http://www.cmb-s4.org/wiki/api.php?action=feedcontributions&user=Cbischoff&feedformat=atomCMB-S4 wiki - User contributions [en]2020-02-24T08:20:43ZUser contributionsMediaWiki 1.30.0http://www.cmb-s4.org/wiki/index.php?title=Data_Challenges&diff=10409Data Challenges2020-01-06T22:45:33Z<p>Cbischoff: </p>
<hr />
<div>We separate "experiment definitions" (bands, resolutions, sensitivity level) from "sky models" (LCDM+dust+sync+).<br />
Each of these is designated by a number. The combination of a given experiment definition XX acting on a given sky model YY is designated XX.YY.<br />
<br />
Experiment models, sky models and the datasets obtained by applying for former to the latter are stored at NERSC at <br /><br />
'''/project/projectdirs/cmbs4/{expt_xx, sky_yy, data_xx.yy}'''<br />
<br />
== Experiment Definitions ==<br />
<br />
'''[[Experiment Definitions]]'''<br />
<br />
== Input Sky Components ==<br />
<br />
'''[[Sky Components]]'''<br />
<br />
== Sky Models ==<br />
<br />
'''[[Sky Models]]'''<br />
<br />
<br />
== Sim Data Sets ==<br />
<br />
Many of the possible xx.yy combinations have been generated and are available on NERSC.<br />
<br />
Most of 02.00 through 02.09 exist - these are the "Science Book config".<br />
<br />
Most of 04.00 through 04.06 exist - these are the "CDT report config".<br />
<br />
== NERSC Info ==<br />
<br />
Shared space is available on [http://www.nersc.gov NERSC], where everyone is welcome to [http://crd.lbl.gov/cmb sign-up for an account] under the "Data Analysis for Post-Planck CMB Experiments" allocation (PI Borrill). The files are located in the shared CMB-S4 file space (/project/projectdirs/cmbs4). In order to manage this space, all files stored there should be owned by the cmbs4 project account but accessible to the cmbs4 group. To do this:<br />
* log in to the cmbs4 project account following the instructions [[http://www.nersc.gov/users/accounts/user-accounts/production-project-accounts here]] <br />
* sync the files to an appropriate subdirectory in the project space<br />
* ensure that the permissions are set appropriately (g+rX,o-rwx)<br />
Remember to include a README and to post the details on this wiki page.<br />
<br />
For any NERSC issues, including access to the filegroup and/or project account, please contact [mailto:jdborrill@lbl.gov Julian Borrill].<br />
<br />
=== HPSS Archive ===<br />
<br />
Older data challenge maps are moved to the [https://docs.nersc.gov/filesystems/archive/ High Performance Storage System]. These are stored in the `low_ell_BB` directory in the `cmbs4` user home directory of HPSS. For each Data Challenge, maps are broken up in several different archives to achieve archive file sizes of ~few 100 GB.<br />
<br />
List the data challenge sets that have been archived here:<br />
02.00, 02.01, 02.02, 02.03, 02.04, 02.05, 02.06, 02.09<br />
02b.00, 02b.03<br />
02c.00, 02c.03<br />
03.00, 03.03<br />
03b.00, 03b.03<br />
03c.00, 03c.03</div>Cbischoffhttp://www.cmb-s4.org/wiki/index.php?title=Education_%26_Public_Outreach_Committee&diff=10398Education & Public Outreach Committee2019-12-19T20:37:23Z<p>Cbischoff: </p>
<hr />
<div>Committee members: Colin Bischoff (chair), Amy Lowitz, Benjamin Saliwanchik, Sara Simon, Chris Stoughton, Peter Timbie and Kasey Wagoner.<br />
<br />
* Mailing list: [https://cmb-s4.org/mailman/listinfo/epoc epoc@cmb-s4.org] (new subscribers welcome!)<br />
* Monthly telecon notes: [https://docs.google.com/document/d/1uSJnm8nLwACaFM5zcvg1aZjDMBJjxN9xE_f9DTmsFSU/edit# google doc] (contact Colin for edit access)<br />
* [[EPO_Brainstorming|Brainstorming page]] for outreach projects</div>Cbischoffhttp://www.cmb-s4.org/wiki/index.php?title=Science_Council&diff=10341Science Council2019-11-22T19:16:37Z<p>Cbischoff: /* Low-ell BB */</p>
<hr />
<div>The Science Council consists of two co-Chairs and the co-Coordinators of four Analysis Working Groups (AWGs). We list the working groups here, together with information<br />
about their activities -- such as information about when they meet and links to meeting notes. The co-Chairs are Gil Holder (gil.holder@gmail.com) and Lloyd Knox (lknox@ucdavis.edu).<br />
<br />
===Overview===<br />
Our main focus now is "flowing down" the science to measurement requirements in preparation for CD-1/PDR. <br />
<br />
===Analysis Working Groups===<br />
<br />
====Low-ell BB==== <br />
- Co-Coordinators: Colin Bischoff (bischocn@ucmail.uc.edu) and Kimmy Wu (wlwu_at_kicp_dot_uchicago_dot_edu)<br />
- Meeting Notes: https://docs.google.com/document/d/1886yT1b6QDuWvsbAu5HmVv2Cl4pfH00YpK5Fv8dNzcM<br />
- Shared logbook: [[Simulation_and_Forecasting_Logbook|Simulations and Forecasting Log Book]]<br />
- Data challenge summary pages: [[Data_Challenges|r forecast sim set summary]]<br />
- Project list: [[LowellBB_Project_List | LowellBB_Project List]]<br />
- Meeting Times: Every other Monday at 12:30 eastern / 11:30 central / 9:30 pacific [https://calendar.google.com/calendar/embed?src=t7l87lpt7g2t6a7ak4qh0t72qg%40group.calendar.google.com&ctz=America%2FLos_Angeles[CMB-S4 Google Calendar]]<br />
- Forecast paper draft: [http://spud.spa.umn.edu/~pryke/s4_forecast_paper.pdf auto update pdf]<br />
<br />
====Maps2Cell====<br />
- Co-Coordinators: Marilena Loverde (marilena.loverde@stonybrook.edu) and Christian Reichardt (christian.reichardt@unimelb.edu.au)<br />
- Project list: [[Maps2Cell_Project_List | Maps2CellProject List]]<br />
- Meeting Notes: [https://docs.google.com/document/d/1GevFM9MsQ716W3hobVKcFbP0rJWeff5d2F34jJ1V8c8/edit?usp=sharing[Link]]<br />
- Shared logbook: [[Simulation_and_Forecasting_Logbook|Simulations and Forecasting Log Book]]<br />
- Data challenge summary pages: N/A<br />
- Meeting Times: Look for our meetings on the [https://calendar.google.com/calendar/embed?src=t7l87lpt7g2t6a7ak4qh0t72qg%40group.calendar.google.com&ctz=America%2FLos_Angeles[CMB-S4 Google Calendar]]<br />
<br />
====Maps2OtherStats====<br />
- Co-Coordinators: Blake Sherwin (sherwin@damtp.cam.ac.uk) and Marcelo Alvarez (marcelo.alvarez@berkeley.edu)<br />
- Meeting Notes: [https://docs.google.com/document/d/1uRkComeC4h9pJfWbkq0sK-NwvWp51asDVXny8BTH2YA/edit?usp=sharing[Link]]<br />
- Shared logbook: [[Simulation_and_Forecasting_Logbook|Simulations and Forecasting Log Book]]<br />
- Data challenge summary pages: N/A<br />
- Meeting Times: Look for our meetings on the [https://calendar.google.com/calendar/embed?src=t7l87lpt7g2t6a7ak4qh0t72qg%40group.calendar.google.com&ctz=America%2FLos_Angeles[CMB-S4 Google Calendar]]<br />
<br />
====Sources====<br />
- Co-Coordinators: Joaquin Vieira (jvieira@illinois.edu) and Nick Battaglia (nbatta@astro.cornell.edu)<br />
- Meeting Notes: [https://docs.google.com/document/d/1rImHymDp3tGvd91k-d_bzD3060aejsyOcJ-h4TPKaxY/edit?usp=sharing[Link]]<br />
- Shared logbook: [[Simulation_and_Forecasting_Logbook|Simulations and Forecasting Log Book]]<br />
- Data challenge summary pages: N/A<br />
- Meeting Times: Look for our meetings on the [https://calendar.google.com/calendar/embed?src=t7l87lpt7g2t6a7ak4qh0t72qg%40group.calendar.google.com&ctz=America%2FLos_Angeles[CMB-S4 Google Calendar]]<br />
<br />
===Historical Stuff below here===<br />
<br />
====Science White Papers====<br />
<br />
We are envisioning a series of SWP submitted by the January 2019 deadline. The papers will describe the entirety of science deliverable with observations in CMB frequency bands (loosely defined). The SWPs are common to the entire community; they will not discuss nor highlight any specific project. All interested members of the community are invited to participate in writing and endorsing any of these papers. <br />
<br />
SWP drafts that are ready for comment are available here:<br />
1) Neutrino Mass from Cosmology<br />
Link to the draft: http://dvorkin.physics.harvard.edu/Astro2020_Neutrino_Mass.pdf<br />
Contact person: Cora Dvorkin (cdvorkin@g.harvard.edu)<br />
2) Primordial non-Gaussianity <br />
Link to the draft:https://www.overleaf.com/read/bfsyyxfdqnvq<br />
Contact Person: Daan Meerburg (daanmeerburg@gmail.com) <br />
3) Dark Matter Physics with Cosmological Probes<br />
Link to the draft [PRELIMINARY, incomplete]: https://github.com/veragluscevic/Astro2020-DM-Cosmology<br />
Contact person: Vera Gluscevic (vera.gluscevic@gmail.com)<br />
4) Dark Energy<br />
Link to the draft: https://www.overleaf.com/read/phkpmjbjydwq<br />
Contact person: Anze Slosar (anze@bnl.gov)<br />
5) Features in the primordial power spectrum<br />
Link to the draft: https://www.overleaf.com/read/kyxzvmrbqpgy<br />
Contact person: Anze Slosar (anze@bnl.gov)<br />
6) Messengers from the Early Universe: Cosmic Neutrinos and Other Light Relics <br />
Link to the draft: https://www.overleaf.com/read/ybxqdqnhvtkm<br />
Contact person: Dan Green (drgreen@ucsd.edu)<br />
7) Testing gravity and particle physics with cosmic microwave background constraints on gravitational waves<br />
Link to the draft: https://www.overleaf.com/read/dsfnphrxfgbn<br />
Contact person: Sarah Shandera (shandera@gmail.com)<br />
8) Probing Feedback in Galaxy Formation with Millimeter-wave Observations<br />
Link to the draft: https://www.overleaf.com/read/ypcrxscjwnwr<br />
Contact people: Colin Hill (jch@ias.edu) and Nick Battaglia (nbatta@astro.cornell.edu)<br />
9) Reionization with the CMB <br />
Link to the draft: https://www.overleaf.com/read/bhdvxzqbprkf<br />
Contact people: Marcelo Alvarez (marcelo.alvarez@berkeley.edu) and Cora Dvorkin (cdvorkin@g.harvard.edu)<br />
<br />
<br />
The SWP are limited to 5 pages or fewer each, and we highly recommend that anyone wishing to contribute will read the short National Academies solicitation. Excerpting this key passage from the call may be helpful here:<br />
<br />
White papers should:<br />
- Identify scientific opportunities and compelling scientific themes for the coming decade, particularly those that have arisen from recent advances and accomplishments in astronomy and astrophysics;<br />
- Describe the scientific context of the importance of these opportunities, including connections to other parts of astronomy and astrophysics and, where appropriate, to the advancement of our broader scientific understanding;<br />
- While focusing on science, not specific missions or projects, describe and quantify the key advances in observation, measurement, theory, and/or computation necessary to realize the scientific opportunities within the decade 2020-2030 and beyond.<br />
<br />
To facilitate engagement and coordination of activities, we have created a wiki page (https://zzz.physics.umn.edu/decadal2020/doku.php?id=start) with a (non-comprehensive) list of potential science white papers with relevance to our community. Listed there are titles, and (mostly blank) fields for listing who is actively participating in the creation of the white paper, who has taken on a coordinating role, and links to relevant documentation for that white paper (github repos, online notes, etc.). <br />
<br />
The purpose of the wiki page is to give all of us a comprehensive view of science white paper activity of relevance to the CMB community, make it possible for would-be contributors to join existing efforts, and to allow any of us to spot gaps and work to fill them. The list of paper titles on the wiki now is just to get us started -- we expect it to evolve as, e.g., some topics get split into two or more different white papers, and new topics altogether are added. Anyone wishing to edit the wiki should contact Shaul Hanany (hanany@umn.edu) to get the appropriate permissions.<br />
<br />
====CMB-S4 Decadal Survey Report====<br />
<br />
Each AWG (with some exceptions) is charged with producing a 5-page section, the main elements of the Science Chapter of the DSR, on the science to be done with the CMB-S4 surveys. Our target for completion of a first draft of the DSR is November 2018. <br />
<br />
=====Draft Schedule for Production of Science Chapter sections=====<br />
<br />
- Friday, Sept 28: Long and rough draft completed<br />
- Friday, Oct 19: 5-page rough draft completed<br />
- Friday, Nov 3: cleaned-up draft ready to go out for review and comment<br />
- Wednesday, Nov 21: comments due back to AWGs<br />
- Friday, Dec 7: DSR chapter finalized<br />
- Dec 11 to 13: Internal DSR review in Washington, D.C. Each AWG should have one co-coordinator there<br />
<br />
===Former SC Analysis Working Groups===<br />
<br />
====Primordial Gravitational Waves==== <br />
- Co-Coordinators: Raphael Flauger (flauger@physics.utexas.edu) and Clem Pryke (pryke@physics.umn.edu)<br />
- Meeting Notes: https://docs.google.com/document/d/1886yT1b6QDuWvsbAu5HmVv2Cl4pfH00YpK5Fv8dNzcM<br />
- Shared logbook: [[Simulation_and_Forecasting_Logbook|Simulations and Forecasting Log Book]]<br />
- Data challenge summary pages: [[Data_Challenges|r forecast sim set summary]]<br />
- Meeting Times: Look for our meetings on the [https://calendar.google.com/calendar/embed?src=t7l87lpt7g2t6a7ak4qh0t72qg%40group.calendar.google.com&ctz=America%2FLos_Angeles[CMB-S4 Google Calendar]]<br />
- Forecast paper draft: [http://spud.spa.umn.edu/~pryke/s4_forecast_paper.pdf[auto update pdf]]<br />
<br />
====Primordial Density Perturbations====<br />
- Co-Coordinators: Cora Dvorkin (cdvorkin@g.harvard.edu) & Daan Meerburg (daanmeerburg@gmail.com)<br />
<br />
- Telecons on-needed basis; see [https://calendar.google.com/calendar/embed?src=t7l87lpt7g2t6a7ak4qh0t72qg%40group.calendar.google.com&ctz=America%2FLos_Angeles[CMB-S4 Google Calendar]]<br />
<br />
====Light Relics====<br />
- Co-Coordinators: Daniel Green (drgreen@physics.ucsd.edu) and Joel Meyers (jmeyers@cita.utoronto.ca)<br />
- Forecasting Setup: [[Forecasting|Non-r Forecasting Page]]<br />
- Meeting Times: Look for our meetings on the [https://calendar.google.com/calendar/embed?src=t7l87lpt7g2t6a7ak4qh0t72qg%40group.calendar.google.com&ctz=America%2FLos_Angeles[CMB-S4 Google Calendar]]<br />
<br />
====Neutrino Mass====<br />
- Co-Coordinators: Marilena Loverde (marilena.loverde@stonybrook.edu) and Blake Sherwin (sherwin@damtp.cam.ac.uk)<br />
- Meeting notes: https://cmb-s4.org/wiki/index.php/Neutrino_Mass_WG_Telecon<br />
- Call summaries: https://docs.google.com/document/d/1TWaU75wN1kqbYD1qkwzcJA9fZXGviKSezj3EnlP-ep8/edit?usp=sharing<br />
- Meeting times: will be posted; typically Tuesday 11am ET<br />
====Dark Energy ====<br />
- Co-Coordinators: Anze Slosar (anze@bnl.gov), and David Alonso (David.Alonso@physics.ox.ac.uk)<br />
- Meeting Notes: https://docs.google.com/document/d/13RTNgJNlWd098EPLnQrAAlstqDtyE850P9HnNFqCJZk/edit?usp=sharing<br />
- Meetings organized on as-needed basis.<br />
<br />
====Dark Matter====<br />
- Co-Coordinators: Vera Gluscevic (verag@ias.edu), and Dan Grin (dgrin@haverford.edu)<br />
- DM interactions meeting minutes: https://docs.google.com/document/d/1RxG07ebylnbXqSHFIIujBl6kO-olEUY9XPM4kyy0EXs/edit<br />
- Telecons on-needed basis; see [https://calendar.google.com/calendar/embed?src=t7l87lpt7g2t6a7ak4qh0t72qg%40group.calendar.google.com&ctz=America%2FLos_Angeles[CMB-S4 Google Calendar]]<br />
).<br />
<br />
====Galaxy Formation and Evolution====<br />
- Co-Coordinators: Marcelo Alvarez (marcelo.alvarez@berkeley.edu) and Colin Hill (jcolin.hill@gmail.com)<br />
- Meeting Notes: https://docs.google.com/document/d/11vsmV9fdDd29Kds2WmEh5MddEP7BAO16xMnoxV-MwZY/edit?usp=sharing<br />
- Meeting Times: Look for our meetings on the [https://calendar.google.com/calendar/embed?src=t7l87lpt7g2t6a7ak4qh0t72qg%40group.calendar.google.com&ctz=America%2FLos_Angeles[CMB-S4 Google Calendar]]<br />
<br />
====Legacy Catalogs====<br />
- Co-Coordinators: Lindsey Bleem (lbleem@anl.gov) and Douglas Scott (dscott@phas.ubc.ca)<br />
- Meeting Notes: https://docs.google.com/document/d/169aZRZiqL3uJ2Eg9LY3ytAlR5UPCesJGp4lfVIAFWyA/edit?usp=sharing<br />
- Meeting Times: TBD; will be posted [https://calendar.google.com/calendar/embed?src=t7l87lpt7g2t6a7ak4qh0t72qg%40group.calendar.google.com&ctz=America%2FLos_Angeles[CMB-S4 Google Calendar]]</div>Cbischoffhttp://www.cmb-s4.org/wiki/index.php?title=Science_Council&diff=10340Science Council2019-11-22T19:16:20Z<p>Cbischoff: /* Low-ell BB */</p>
<hr />
<div>The Science Council consists of two co-Chairs and the co-Coordinators of four Analysis Working Groups (AWGs). We list the working groups here, together with information<br />
about their activities -- such as information about when they meet and links to meeting notes. The co-Chairs are Gil Holder (gil.holder@gmail.com) and Lloyd Knox (lknox@ucdavis.edu).<br />
<br />
===Overview===<br />
Our main focus now is "flowing down" the science to measurement requirements in preparation for CD-1/PDR. <br />
<br />
===Analysis Working Groups===<br />
<br />
====Low-ell BB==== <br />
- Co-Coordinators: Colin Bischoff (bischocn@ucmail.uc.edu) and Kimmy Wu (wlwu_at_kicp_dot_uchicago_dot_edu)<br />
- Meeting Notes: https://docs.google.com/document/d/1886yT1b6QDuWvsbAu5HmVv2Cl4pfH00YpK5Fv8dNzcM<br />
- Shared logbook: [[Simulation_and_Forecasting_Logbook|Simulations and Forecasting Log Book]]<br />
- Data challenge summary pages: [[Data_Challenges|r forecast sim set summary]]<br />
- Project list: [[LowellBB_Project_List | LowellBB_Project List]]<br />
- Meeting Times: Every other Monday at 12:30 eastern / 11:30 central / 9:30 pacific. Look for our meetings on the [https://calendar.google.com/calendar/embed?src=t7l87lpt7g2t6a7ak4qh0t72qg%40group.calendar.google.com&ctz=America%2FLos_Angeles[CMB-S4 Google Calendar]]<br />
- Forecast paper draft: [http://spud.spa.umn.edu/~pryke/s4_forecast_paper.pdf auto update pdf]<br />
<br />
====Maps2Cell====<br />
- Co-Coordinators: Marilena Loverde (marilena.loverde@stonybrook.edu) and Christian Reichardt (christian.reichardt@unimelb.edu.au)<br />
- Project list: [[Maps2Cell_Project_List | Maps2CellProject List]]<br />
- Meeting Notes: [https://docs.google.com/document/d/1GevFM9MsQ716W3hobVKcFbP0rJWeff5d2F34jJ1V8c8/edit?usp=sharing[Link]]<br />
- Shared logbook: [[Simulation_and_Forecasting_Logbook|Simulations and Forecasting Log Book]]<br />
- Data challenge summary pages: N/A<br />
- Meeting Times: Look for our meetings on the [https://calendar.google.com/calendar/embed?src=t7l87lpt7g2t6a7ak4qh0t72qg%40group.calendar.google.com&ctz=America%2FLos_Angeles[CMB-S4 Google Calendar]]<br />
<br />
====Maps2OtherStats====<br />
- Co-Coordinators: Blake Sherwin (sherwin@damtp.cam.ac.uk) and Marcelo Alvarez (marcelo.alvarez@berkeley.edu)<br />
- Meeting Notes: [https://docs.google.com/document/d/1uRkComeC4h9pJfWbkq0sK-NwvWp51asDVXny8BTH2YA/edit?usp=sharing[Link]]<br />
- Shared logbook: [[Simulation_and_Forecasting_Logbook|Simulations and Forecasting Log Book]]<br />
- Data challenge summary pages: N/A<br />
- Meeting Times: Look for our meetings on the [https://calendar.google.com/calendar/embed?src=t7l87lpt7g2t6a7ak4qh0t72qg%40group.calendar.google.com&ctz=America%2FLos_Angeles[CMB-S4 Google Calendar]]<br />
<br />
====Sources====<br />
- Co-Coordinators: Joaquin Vieira (jvieira@illinois.edu) and Nick Battaglia (nbatta@astro.cornell.edu)<br />
- Meeting Notes: [https://docs.google.com/document/d/1rImHymDp3tGvd91k-d_bzD3060aejsyOcJ-h4TPKaxY/edit?usp=sharing[Link]]<br />
- Shared logbook: [[Simulation_and_Forecasting_Logbook|Simulations and Forecasting Log Book]]<br />
- Data challenge summary pages: N/A<br />
- Meeting Times: Look for our meetings on the [https://calendar.google.com/calendar/embed?src=t7l87lpt7g2t6a7ak4qh0t72qg%40group.calendar.google.com&ctz=America%2FLos_Angeles[CMB-S4 Google Calendar]]<br />
<br />
===Historical Stuff below here===<br />
<br />
====Science White Papers====<br />
<br />
We are envisioning a series of SWP submitted by the January 2019 deadline. The papers will describe the entirety of science deliverable with observations in CMB frequency bands (loosely defined). The SWPs are common to the entire community; they will not discuss nor highlight any specific project. All interested members of the community are invited to participate in writing and endorsing any of these papers. <br />
<br />
SWP drafts that are ready for comment are available here:<br />
1) Neutrino Mass from Cosmology<br />
Link to the draft: http://dvorkin.physics.harvard.edu/Astro2020_Neutrino_Mass.pdf<br />
Contact person: Cora Dvorkin (cdvorkin@g.harvard.edu)<br />
2) Primordial non-Gaussianity <br />
Link to the draft:https://www.overleaf.com/read/bfsyyxfdqnvq<br />
Contact Person: Daan Meerburg (daanmeerburg@gmail.com) <br />
3) Dark Matter Physics with Cosmological Probes<br />
Link to the draft [PRELIMINARY, incomplete]: https://github.com/veragluscevic/Astro2020-DM-Cosmology<br />
Contact person: Vera Gluscevic (vera.gluscevic@gmail.com)<br />
4) Dark Energy<br />
Link to the draft: https://www.overleaf.com/read/phkpmjbjydwq<br />
Contact person: Anze Slosar (anze@bnl.gov)<br />
5) Features in the primordial power spectrum<br />
Link to the draft: https://www.overleaf.com/read/kyxzvmrbqpgy<br />
Contact person: Anze Slosar (anze@bnl.gov)<br />
6) Messengers from the Early Universe: Cosmic Neutrinos and Other Light Relics <br />
Link to the draft: https://www.overleaf.com/read/ybxqdqnhvtkm<br />
Contact person: Dan Green (drgreen@ucsd.edu)<br />
7) Testing gravity and particle physics with cosmic microwave background constraints on gravitational waves<br />
Link to the draft: https://www.overleaf.com/read/dsfnphrxfgbn<br />
Contact person: Sarah Shandera (shandera@gmail.com)<br />
8) Probing Feedback in Galaxy Formation with Millimeter-wave Observations<br />
Link to the draft: https://www.overleaf.com/read/ypcrxscjwnwr<br />
Contact people: Colin Hill (jch@ias.edu) and Nick Battaglia (nbatta@astro.cornell.edu)<br />
9) Reionization with the CMB <br />
Link to the draft: https://www.overleaf.com/read/bhdvxzqbprkf<br />
Contact people: Marcelo Alvarez (marcelo.alvarez@berkeley.edu) and Cora Dvorkin (cdvorkin@g.harvard.edu)<br />
<br />
<br />
The SWP are limited to 5 pages or fewer each, and we highly recommend that anyone wishing to contribute will read the short National Academies solicitation. Excerpting this key passage from the call may be helpful here:<br />
<br />
White papers should:<br />
- Identify scientific opportunities and compelling scientific themes for the coming decade, particularly those that have arisen from recent advances and accomplishments in astronomy and astrophysics;<br />
- Describe the scientific context of the importance of these opportunities, including connections to other parts of astronomy and astrophysics and, where appropriate, to the advancement of our broader scientific understanding;<br />
- While focusing on science, not specific missions or projects, describe and quantify the key advances in observation, measurement, theory, and/or computation necessary to realize the scientific opportunities within the decade 2020-2030 and beyond.<br />
<br />
To facilitate engagement and coordination of activities, we have created a wiki page (https://zzz.physics.umn.edu/decadal2020/doku.php?id=start) with a (non-comprehensive) list of potential science white papers with relevance to our community. Listed there are titles, and (mostly blank) fields for listing who is actively participating in the creation of the white paper, who has taken on a coordinating role, and links to relevant documentation for that white paper (github repos, online notes, etc.). <br />
<br />
The purpose of the wiki page is to give all of us a comprehensive view of science white paper activity of relevance to the CMB community, make it possible for would-be contributors to join existing efforts, and to allow any of us to spot gaps and work to fill them. The list of paper titles on the wiki now is just to get us started -- we expect it to evolve as, e.g., some topics get split into two or more different white papers, and new topics altogether are added. Anyone wishing to edit the wiki should contact Shaul Hanany (hanany@umn.edu) to get the appropriate permissions.<br />
<br />
====CMB-S4 Decadal Survey Report====<br />
<br />
Each AWG (with some exceptions) is charged with producing a 5-page section, the main elements of the Science Chapter of the DSR, on the science to be done with the CMB-S4 surveys. Our target for completion of a first draft of the DSR is November 2018. <br />
<br />
=====Draft Schedule for Production of Science Chapter sections=====<br />
<br />
- Friday, Sept 28: Long and rough draft completed<br />
- Friday, Oct 19: 5-page rough draft completed<br />
- Friday, Nov 3: cleaned-up draft ready to go out for review and comment<br />
- Wednesday, Nov 21: comments due back to AWGs<br />
- Friday, Dec 7: DSR chapter finalized<br />
- Dec 11 to 13: Internal DSR review in Washington, D.C. Each AWG should have one co-coordinator there<br />
<br />
===Former SC Analysis Working Groups===<br />
<br />
====Primordial Gravitational Waves==== <br />
- Co-Coordinators: Raphael Flauger (flauger@physics.utexas.edu) and Clem Pryke (pryke@physics.umn.edu)<br />
- Meeting Notes: https://docs.google.com/document/d/1886yT1b6QDuWvsbAu5HmVv2Cl4pfH00YpK5Fv8dNzcM<br />
- Shared logbook: [[Simulation_and_Forecasting_Logbook|Simulations and Forecasting Log Book]]<br />
- Data challenge summary pages: [[Data_Challenges|r forecast sim set summary]]<br />
- Meeting Times: Look for our meetings on the [https://calendar.google.com/calendar/embed?src=t7l87lpt7g2t6a7ak4qh0t72qg%40group.calendar.google.com&ctz=America%2FLos_Angeles[CMB-S4 Google Calendar]]<br />
- Forecast paper draft: [http://spud.spa.umn.edu/~pryke/s4_forecast_paper.pdf[auto update pdf]]<br />
<br />
====Primordial Density Perturbations====<br />
- Co-Coordinators: Cora Dvorkin (cdvorkin@g.harvard.edu) & Daan Meerburg (daanmeerburg@gmail.com)<br />
<br />
- Telecons on-needed basis; see [https://calendar.google.com/calendar/embed?src=t7l87lpt7g2t6a7ak4qh0t72qg%40group.calendar.google.com&ctz=America%2FLos_Angeles[CMB-S4 Google Calendar]]<br />
<br />
====Light Relics====<br />
- Co-Coordinators: Daniel Green (drgreen@physics.ucsd.edu) and Joel Meyers (jmeyers@cita.utoronto.ca)<br />
- Forecasting Setup: [[Forecasting|Non-r Forecasting Page]]<br />
- Meeting Times: Look for our meetings on the [https://calendar.google.com/calendar/embed?src=t7l87lpt7g2t6a7ak4qh0t72qg%40group.calendar.google.com&ctz=America%2FLos_Angeles[CMB-S4 Google Calendar]]<br />
<br />
====Neutrino Mass====<br />
- Co-Coordinators: Marilena Loverde (marilena.loverde@stonybrook.edu) and Blake Sherwin (sherwin@damtp.cam.ac.uk)<br />
- Meeting notes: https://cmb-s4.org/wiki/index.php/Neutrino_Mass_WG_Telecon<br />
- Call summaries: https://docs.google.com/document/d/1TWaU75wN1kqbYD1qkwzcJA9fZXGviKSezj3EnlP-ep8/edit?usp=sharing<br />
- Meeting times: will be posted; typically Tuesday 11am ET<br />
====Dark Energy ====<br />
- Co-Coordinators: Anze Slosar (anze@bnl.gov), and David Alonso (David.Alonso@physics.ox.ac.uk)<br />
- Meeting Notes: https://docs.google.com/document/d/13RTNgJNlWd098EPLnQrAAlstqDtyE850P9HnNFqCJZk/edit?usp=sharing<br />
- Meetings organized on as-needed basis.<br />
<br />
====Dark Matter====<br />
- Co-Coordinators: Vera Gluscevic (verag@ias.edu), and Dan Grin (dgrin@haverford.edu)<br />
- DM interactions meeting minutes: https://docs.google.com/document/d/1RxG07ebylnbXqSHFIIujBl6kO-olEUY9XPM4kyy0EXs/edit<br />
- Telecons on-needed basis; see [https://calendar.google.com/calendar/embed?src=t7l87lpt7g2t6a7ak4qh0t72qg%40group.calendar.google.com&ctz=America%2FLos_Angeles[CMB-S4 Google Calendar]]<br />
).<br />
<br />
====Galaxy Formation and Evolution====<br />
- Co-Coordinators: Marcelo Alvarez (marcelo.alvarez@berkeley.edu) and Colin Hill (jcolin.hill@gmail.com)<br />
- Meeting Notes: https://docs.google.com/document/d/11vsmV9fdDd29Kds2WmEh5MddEP7BAO16xMnoxV-MwZY/edit?usp=sharing<br />
- Meeting Times: Look for our meetings on the [https://calendar.google.com/calendar/embed?src=t7l87lpt7g2t6a7ak4qh0t72qg%40group.calendar.google.com&ctz=America%2FLos_Angeles[CMB-S4 Google Calendar]]<br />
<br />
====Legacy Catalogs====<br />
- Co-Coordinators: Lindsey Bleem (lbleem@anl.gov) and Douglas Scott (dscott@phas.ubc.ca)<br />
- Meeting Notes: https://docs.google.com/document/d/169aZRZiqL3uJ2Eg9LY3ytAlR5UPCesJGp4lfVIAFWyA/edit?usp=sharing<br />
- Meeting Times: TBD; will be posted [https://calendar.google.com/calendar/embed?src=t7l87lpt7g2t6a7ak4qh0t72qg%40group.calendar.google.com&ctz=America%2FLos_Angeles[CMB-S4 Google Calendar]]</div>Cbischoffhttp://www.cmb-s4.org/wiki/index.php?title=Simulation_and_Forecasting_Logbook&diff=10295Simulation and Forecasting Logbook2019-11-12T16:30:47Z<p>Cbischoff: /* Logbook Entries (reverse chronological) */</p>
<hr />
<div>This is an index page for logbook-style postings that cover the interconnected topics of sky modeling, simulations, and forecasting for CMB-S4. <br />
<br />
Some guidelines for use:<br />
* '''Postings should include enough context''' so that a reader can jump in and figure out what is going on. It is ''not'' necessary to write an extensive introduction to every posting -- context can be in the form of links to older postings, paper citations, etc.<br />
* Postings should represent a snapshot of work in progress. It's ok to post incomplete results, but recommended that you include notes about what is missing, what you are still planning to work on, etc. <br />
* If you have work that extends or improves an old posting, you should add it as a new posting (that includes links back to the old work as appropriate). Don't update old postings, as they should provide a chronological record of progress.<br />
* On this index page, add a link to your posting with the date, a descriptive posting title, and your full name. This logbook covers a wide range of topics, so titles will be really important to keep it useful. Don't name your posting something like "Forecasting for S4"!<br />
* Links should be added in reverse-chronological order (newest at the top). Your posting can either be written up on another wiki page or it can be a link to some externally hosted webpage (useful if you want to include a javascript plots pager).<br />
<br />
<br />
== Logbook Entries (reverse chronological) ==<br />
<br />
* '''2019 November 12''': [[SAT detector counts, NET, and overall efficiency from DSR]] (C. Bischoff)<br />
* '''2019 November 12''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20191112_bk_scans Actual BK scanning trajectory] (Clem)<br />
* '''2019 November 1''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20191101_dc06_specsmaps DSR Sim Map Set 06 - some spectra and map check plots] (Clem)<br />
* '''2019 October 25''': [[Modulated scan high cadence LAT]] (Reijo)<br />
* '''2019 October 16''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20191016_dc06_dsr DSR Sim Map Set 06 with simple scaling from BK15] (Clem)<br />
* '''2019 September 16''': [[PureB by Messenger Method]] (Michael Ray, Colin Bischoff)<br />
* '''2019 August 29''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190829_noise_params_DSR/ Noise parameters for the DC5 DSR-like data challenge] (Ben Racine)<br />
* '''2019 June 6''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190607_LATSTM/ LAT CDT-STM Noise Levels] (Victor Buza)<br />
* '''2019 May 19''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190519_about_DSR_AppendixA_plots_and_table/ sigma(r) vs r: plots and tables for the DSR] (Ben Racine and Raphael Flauger)<br />
* '''2019 May 17''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190509_b3_obseff Observing efficiency reality check] (Clem)<br />
* '''2019 May 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190511_sigmar_vs_r_galcuts/ sigma(r) vs r: possible figures for the DSR (v4): Galactic cuts added (In progress)] (Ben Racine and Raphael Flauger)<br />
* '''2019 May 11''': [[Update_on_Fisher_forecasts]] (Raphael)<br />
* '''2019 May 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190507_sigmar_vs_r_combined_hits/ sigma(r) vs r: possible figures for the DSR (v3): More realistic combination and fixed 20GHz] (Ben Racine and Raphael Flauger)<br />
* '''2019 May 6''': [[Update_on_Fisher_forecasts]] (Raphael)<br />
* '''2019 April 30''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190430_sigmar_vs_r_forDSR/ sigma(r) vs r: possible figures for the DSR (v2): more optimal weighting] (Ben Racine and Raphael Flauger)<br />
* '''2019 April 29''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190501_obseff Efficiency for Reijo's observation pattern sims] (Clem)<br />
* '''2019 April 29''': [[Fisher forecasts for inverse noise variance weighting]] (Raphael)<br />
* '''2019 April 22''': [[WAFTT results part 3]] (Raphael)<br />
* '''2019 April 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190418_sigmar_vs_r/ sigma(r) vs r: possible figures for the DSR] (Ben Racine)<br />
* '''2019 April 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190410_closedloop_BK15_S4 Zero order closed loop test of performance based scaling - ML search] (Ben Racine)<br />
* '''2019 March 31''': [[Analysis results for configurations 30-33]] (Raphael)<br />
* '''2019 March 30''': [[Characterization of simulations for configurations 30-33]] (Raphael)<br />
* '''2019 March 26''': [[Simulations for configurations with different frequency coverage]] (Raphael)<br />
* '''2019 March 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190326_bkfinal_05 Zero order closed loop test of performance based scaling - BK15 regen power spectra] (Clem)<br />
* '''2019 March 25''': [[Deeper SAT from Chile II]] (Reijo Keskitalo and Julian Borrill)<br />
* '''2019 March 25''': [[Wider SAT from the Pole II]] (Reijo Keskitalo and Julian Borrill)<br />
* '''2019 March 25''': [[Deep SAT from the Pole]] (Reijo Keskitalo and Julian Borrill)<br />
* '''2019 March 18''': [https://cmb-s4.org/wiki/index.php/Optimal_lensing_fermilab Details on optimal lensing Fermilab presentation / 02.xx real delensing] (Marius Millea)<br />
* '''2019 March 18''': [[High cadence LAT from Chile]] (Reijo Keskitalo)<br />
* '''2019 March 18''': [[WAFTT results part 2]] (Raphael)<br />
* '''2019 March 18''': [[Wider SAT from the Pole]] (Reijo Keskitalo)<br />
* '''2019 March 8''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook//20190308_MLsearch_no85no145/ Maximum likelihood search results without 85GHz and 145GHz] (Ben Racine)<br />
* '''2019 March 3''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190303_MLsearch_bpmax_dep/ Maximum likelihood search results: dependence on the multipole range] (Ben Racine)<br />
* '''2019 February 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190220_noiseparams_bk15_forS4/ BK15 noise levels for S4 sims] (Ben Racine) <br />
* '''2019 February 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190220_S4_NET_forecasts_III/ CMB-S4 NET follow-ups II] (Denis Barkats, Ben Racine-updated on Feb 25) <br />
* '''2019 February 18''': [[Correlation of reconstructed lensing template to ideal II]] (Clem Pryke)<br />
* '''2019 February 18''': [[Fisher calcs of 04b/04c for larger value of r]] (Raphael posted by Clem)<br />
* '''2019 February 14''': [[Deeper SAT from Chile]] (Reijo Keskitalo)<br />
* '''2019 January 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190130_Matrix_first_try/ Matrix-based purification analysis: First try] (B.Racine, J.Willmert) ''Updated 2019 Feb 17th''<br />
* '''2019 January 23''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190123_S4_NET_forecasts_II/ CMB-S4 NET follow-ups I] (Denis Barkats, J. Kovac, Ben Racine-updated on Feb 25) <br />
* '''2019 January 15''': [[Correlation of reconstructed lensing template to ideal]] (Clem Pryke)<br />
* '''2019 January 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190120_dc02_ML_LT/ Maximum likelihood search results for Data Challenge 02.00 with two different lensing templates] (C. Umiltà)<br />
* '''2019 January 17''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190117_MLsearch04d/ Maximum likelihood search results for Data Challenge 04d.00, new BK14 mask reanalysis] (Ben Racine)<br />
* '''2019 January 15''': [[Noise models and sky fractions for WAFTT]] (Raphael)<br />
* '''2019 January 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190111_bkfinal_04bcd BK-style power spectra of 04/04b/04c/04d masks (adding BK14 mask)] (Clem)<br />
* '''2018 December 9''': [[Optimal Bayesian delensing progress update]] (Marius Millea) <br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181207_bkfinal_02lt BK-style power spectra of 02 with Carron lensing templates] (Clem)<br />
* '''2018 December 7''': [[Problems with PS2HAT estimator at low ell]] (Clem Pryke)<br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181116_bpbias_study Bandpower bias study] (Ben Racine)<br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181207_expval_input_ML_search Maximum likelihood search with expectation values as input] (C. Umiltà)<br />
* '''2018 November 28''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181128_toy_sims Effective sky fraction] (Clem)<br />
* '''2018 November 21''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181111_dc04_flatpriors/ Maximum likelihood search results for Data Challenge 04, v2] (Ben Racine)<br />
* '''2018 November 21''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181111_dc04_flatpriors/index_abc.html Maximum likelihood search results for Data Challenge 04b and 04c, v2] (Ben Racine)<br />
* '''2018 November 16''': [[Analytic approximation for r likelihood]] (C. Bischoff) ''Updated 2018-11-20''<br />
* '''2018 November 12''': [[Detection significance for r=0.003]] (C. Bischoff)<br />
* '''2018 November 9''': [[Bad realizations in gsync/gdust sims]] (Clem Pryke)<br />
* '''2018 November 8''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181108_dc02_ML_LT Maximum likelihood search results for Data Challenge 02.00 with an ideal lensing template] (C. Umiltà)<br />
* '''2018 November 5''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181105_toy_sims Attempt to understand sigma(r) results with different hit maps] (Clem)<br />
* '''2018 October 29''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181018_1Dmodel_tapering_study Simple 1D model to study the effect of different observation strategies on the bandpower statistics.] (Ben Racine, Victor Buza, John Kovac) ''Updated 2018 Dec 14th''<br />
* '''2018 October 29''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181029_bkfinal_02lt BK-style power spectra of 02 with ideal lensing templates] (Clem)<br />
* '''2018 October 26''': [[Checking BB purity in re-analysis for alternate masks]] (Clem Pryke)<br />
* '''2018 October 23''': [[Estimated observing efficiency for past and current telescopes, version 2]] (C. Bischoff, Y. Chinone, T. Crawford, M. Hasselfield)<br />
* '''2018 October 14''': [[Estimates of delensing efficiency]] (Raphael)<br />
* '''2018 October 14''': [[Analysis of 04, 04b, 04c simulations]] (Raphael) [[Analysis of 04, 04b, 04c simulations comp]] (Ben)<br />
* '''2018 September 30''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180930_dc04_0to9/ Maximum likelihood search results for Data Challenge 04, models 0 to 9] (Ben Racine) ''Updated 2018 Oct 2nd''<br />
* '''2018 September 30''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180930_dc04_abc_model_0123789_ML/ Maximum likelihood search results for Data Challenge 04b and 04c, model 00, 01, 02, 03, 07, 08 and 09] (Ben Racine)<br />
* '''2018 September 30''': [[Ready for delensing use lensing maps 02.00]] (Julien Carron)<br />
* '''2018 September 28''': [[Towards lensing template]] (Clem Pryke)<br />
* '''2018 September 27''': [[Lensing reconstructions 02.00]] (Julien Carron)<br />
* '''2018 September 26''': [[Lensing map reconstruction from 02.00 sims w/ and w/o foreground+inhomogeneous noise]] (Toshiya Namikawa)<br />
* '''2018 September 25''': [[Estimated observing efficiency for past and current telescopes]] (C. Bischoff)<br />
* '''2018 September 25''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180925_bkfinal_04bc BK-style power spectra of 04/04b/04c masks for 00/01/02/03/07/08/09 foreground models] (Clem)<br />
* '''2018 September 12''': [[Low ell noise from past and current telescopes]] (C. Bischoff)<br />
* '''2018 September 5''': [[Phi reconstruction on 02.00 sims III]] (Anton Baleato)<br />
* '''2018 August 31''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180831_dc04_abc_model00_07_ML_proper_bp/ Maximum likelihood search results for Data Challenge 04b and 04c, for sky models 00 and 07] (Ben Racine)<br />
* '''2018 August 31''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180831_dc04_fixed_bp/ Maximum likelihood search results for Data Challenge 04, fixed bandpasses] (Ben Racine)<br />
* '''2018 August 27''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180827_bkfinal_04 Sims with nominal Chile and Pole masks III - BK-style power spectra of 04b.YY and 04c.YY] (Clem)<br />
* '''2018 August 27''': [[Sims with nominal Chile and Pole masks II]] (Clem P.)<br />
* '''2018 August 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180826_dc04_fixed/ Maximum likelihood search results for Data Challenge 04, fixed] (V.Buza, B.Racine)<br />
* '''2018 August 24''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180824_bkfinal_04/ BK-style power spectra of v04.00-06 sims (CDT report config) FIXED] (Caterina Umilta)<br />
* '''2018 August 24''': [[Amplitude modulated Gaussian dust sims]] (Clem P.)<br />
* '''2018 August 17''': [[Sims with nominal Chile and Pole masks]] (Clem P.)<br />
* '''2018 August 10''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180810_noise/ Achieved performance roundup] (C. Bischoff)<br />
* '''2018 August 7''': [[Pre-reference-design noise specifications for large-aperture forecasting]] (Tom Crawford, Matthew Hasselfield, Gil Holder, Lloyd Knox)<br />
* '''2018 August 6''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180805_s4opt/ Performance-based Fisher optimization for CMB-S4, 44cm vs 52cm aperture (w/ high-res/low-res 20 GHz)] (V.Buza)<br />
* '''2018 July 9''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180708_dc04/ Maximum likelihood search results for Data Challenge 04] (V.Buza)<br />
* '''2018 July 6''': [[Phi reconstruction on 02.00 sims II]] (Anton Baleato and Clem Pryke)<br />
* '''2018 June 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180611_s4opt/ Performance-based Fisher optimization for CMB-S4, 44cm aperture] (V.Buza) -- see corrected August 6th Update!<br />
* '''2018 June 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180609_S4_noise_simulation_arbitrary_coverage/ Recipe to generate performance based S4 simulations with arbitrary sky distribution (in progress)] (B.Racine, V.Buza)<br />
* '''2018 April 29''': [[Phi reconstruction on 02.00 sims]] (Anton Baleato)<br />
* '''2018 April 25''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180425_r_equivalent_maps/ Smallfield r-equivalent Maps] (Kenny Lau)<br />
* '''2018 April 4''': [[Sky masks for simulations III]] (Clem P.)<br />
* '''2018 March 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180323_bkfinal_04/ BK-style power spectra of v04.00-06 sims (CDT report config) BROKEN] (Clem)<br />
* '''2018 March 16''': [[ILC noise for large apertures at CDT noise levels]] (Raphael Flauger posted by Clem)<br />
* '''2018 March 16''': [[Sky masks for simulations II]] (Clem P.)<br />
* '''2018 February 19''': [[Sky masks for simulations]] (Clem P.)<br />
* '''2018 February 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180218_s4opt/ Performance-based Fisher optimization for CMB-S4, v3] (Victor Buza)<br />
* '''2018 February 7''': [[Sim map sets to demonstrate "real delensing" (02.00 and 02.09)]] (Clem P.)<br />
* '''2018 February 6''': [[Data Challenge Map Sets 04.YY]] (Clem P.)<br />
* '''2017 December 8''': [[Vansyngel Model]] (Clem P.)<br />
* '''2017 November 6''': [[Bandpass Convention - What does flat mean]] (Clem P.) - followup notes added Nov 20<br />
* '''2017 September 27''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170927_dc02/ Maximum likelihood search results for Data Challenge 02] (Bischoff, Buza, Willmert)<br />
* '''2017 September 13''': [[Bias on r from Band Center Errors]] (Palladino, Willmert, Bischoff)<br />
* '''2017 September 8''': [[Checking dust decorrelation in Raphael MHD based dust sim]] (Clem P.)<br />
* '''2017 September 6''': [[New NET Calculator and Validation]] (Denis Barkats)<br />
* '''2017 September 1''': [[Resolution at 20 GHz]] (Raphael)<br />
* '''2017 August 31''': [[Bias on r from additive systematics]] (Palladino, Willmert, Bischoff)<br />
* '''2017 August 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170818_bkfinal_03.00/ BK-style power spectra for 1000 realizations of v03.00,.03 CMB-S4 simulation maps] (Justin Willmert)<br />
* '''2017 August 18 ''': [[Neff_and_Beam_Calibration| Neff and Beam Calibration]] (Dan)<br />
* '''2017 August 18''': [[Ideal delensing templates from flat-sky QE, first pass]] (Kyle Story)<br />
* '''2017 August 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170818_HR/ High-Res studies for CMB-S4 (draft, v2)] (Victor Buza)<br />
* '''2017 August 18''': [[Comments from Anthony Challinor and Rupert Allison regarding the impact of Galactic Foregrounds on lensing]] (Neelima)<br />
* '''2017 August 11''': [[Joint Synchrotron and Dust Maps from Simulations]] (B. Hensley)<br />
* '''2017 August 9''': [[Dust Emission From Halos]] (Jim & Jean-Baptiste)<br />
* '''2017 August 9''': [[SZ Clusters update]] (Mat & Nick)<br />
* '''2017 August 4''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170804_HR/ High-Res studies for CMB-S4 (preliminary draft)] (Victor Buza); perhaps a reference of interest https://arxiv.org/abs/1707.02259<br />
* '''2017 July 10''': [[Additive systematics for data challenge 03]] (Bischoff, Palladino, Buza, Kovac)<br />
* '''2017 July 6''': [[Detection significance and sky fraction, dust decorrelation]](Raphael)<br />
* '''2017 July 3''': [[Toy highly decorrelated dust model]] (Clem P.)<br />
* '''2017 June 27''': [[Checking dust decorrelation in models d1/d4/d7 and hipdt]] (Clem P.)<br />
* '''2017 June 23''': [[Dust_delensing_firstlook|Dust delensing update]] (Alex)<br />
* '''2017 June 23''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170623_bkfinal_02.00/ BK-style power spectra for 1000 realizations of v02.00–06 CMB-S4 simulation maps] (Justin Willmert) ''Updated 2017 Sep 08''<br />
* '''2017 June 22''': [[Warm-up exercise for delensing]] (Raphael)<br />
* '''2017 June 19''': [[SZ Clusters update]] (Mat, Nick)<br />
* '''2017 June 11''': [[Notes from May 31 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 June 9''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170525_s4syst/ Introducing systematics for CMB-S4] ((Victor Buza), with input from Colin Bischoff, John Kovac)<br />
* '''2017 June 9''': [[Dust_delensing_firstlook]] (Alex)<br />
* '''2017 June 9''': [[r-forecasting: high and low ell coordination|r-forecasting: update on high and low ell coordination]] (Neelima+Colin Hill writing)<br />
* '''2017 June 1''': [[Residuals for DC 01.01 and DC 01.02]] (Raphael)<br />
* '''2017 June 1''': [[Levels of foregrounds in Gaussian and PySM simulations]] (Raphael)<br />
* '''2017 May 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170511_s4dc1/ S4 DC 01.xx analysis, v2] (Victor Buza, Colin Bischoff, Justin Willmert)<br />
* '''2017 May 26 ''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170411_bkfinal_01.00/ Updated v01.02 in "BK-style power spectra for 1000 realizations of v01.00–02 CMB-S4 simulation maps"] (Justin Willmert)<br />
* '''2017 May 15''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170515_chkS4/ N_ell spectra for CMB-S4 DC2.0] (Victor Buza)<br />
* '''2017 May 15''': [[Rev 2 PySM a2d4f1s3 maps]] (Clem P.)<br />
* '''2017 May 12''': [[r-forecasting: high and low ell coordination|r-forecasting: high and low ell coordination]] (lensers writing)<br />
* '''2017 May 8''': [[Checking PySM maps]] (Clem P.)<br />
* '''2017 May 2''': [[Notes from April 26 telecon on science requirements for clusters/high-ell]] (Steve)<br />
* '''2017 May 1''': [[r-forecasting: delensing discussion|r-forecasting delensing discussion]] (Neelima and Blake)<br />
* '''2017 April 28 ''': [[Update_on_Neff_Forecasts| Update on Neff Forecasts]] (Dan)<br />
* '''2017 April 26 ''': [http://www.cosmo.bnl.gov/www/msyriac/web/work/sigma8plots.html Update on cluster number counts forecast including w_a] (Mat and Nick)<br />
* '''2017 April 21 ''': [[lensing-DE|Update on a lensing-based DE forecast]] (Jo, Siddharth)<br />
* '''2017 April 18 ''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170411_bkfinal_01.00/ BK-style power spectra for 1000 realizations of v01.00–02 CMB-S4 simulation maps] (Justin Willmert)<br />
* '''2017 April 18 ''': [[S4-Lensing|S4 measurement requirements for neutrino mass and delensing - first pass]] (Neelima/Blake)<br />
* '''2017 April 17 ''': [[HiDPol|HI-based dust polarization model for r forecasts]] (Tuhin)<br />
* '''2017 April 05 ''': [[lensing-DE|Notes on one path to lensing-based DE forecasts]] (Jo)<br />
* '''2017 April 05 ''': [[Notes from April 5 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 April 05''': [https://cmb-s4.org/CMB-S4workshops/images/Sigma8_z_prep.pdf Sigma8(z) SPT clusters (placeholder) ] (S Bocquet)<br />
* '''2017 April 04''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170404_s4opt/ Updated Performance-based Fisher optimization for CMB-S4 (using bands v1.99)] (Victor Buza, Updated 2017.04.21)<br />
* '''2017 March 31 ''': [[Data Challenge analysis - DC1.0, DC1.1, DC1.2]] (Raphael)<br />
* '''2017 March 30 ''': [[Notes from March 28 telecon on science requirements for clusters/high-ell]] (Jim & Steve)<br />
* '''2017 March 29''': [[CMB-S4 frequency bands v1.99]] (John Kovac, Band-definition working group)<br />
* '''2017 March 28''': [[Adding higher res delensing "band"]] (Clem P.)<br />
* '''2017 March 27''': [[01.01 sim input maps - first try]] (Clem P.)<br />
* '''2017 March 23''': [[01.00 sim input maps]] (Clem P.)<br />
* '''2017 March 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170221_S4_NET_forecasts/ S4 Band sensitivity comparison follow-up] (Denis Barkats, John Kovac)<br />
* '''2017 March 17''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/vbuza/20170317_s4dc1/ S4 DC1.0 analysis] (Victor Buza, Colin Bischoff, Justin Willmert)<br />
* '''2017 March 17 ''': [[Media:Telecon_03172017_optimization_for_CMBS4.pdf]]: Optimization methodology for SO (Josquin)<br />
* '''2017 March 16 ''': [[ P_k_science_case| P(k) science case]] (Colin, Simone, Nick, David)<br />
* '''2017 March 15 ''': [[Notes from March 15 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 March 15 ''': [[CMB halo lensing sensitivity as a function of map sensitivity and resolution]] (Jim & Jean-Baptiste)<br />
* '''2017 March 15 ''': [[w and gamma | w and Delta gamma constraints from sigma_8 (z)]] (Mat & Nick)<br />
* '''2017 March 10 ''': [[Notes from March 8 telecon on science requirements for clusters/high-ell]] (Jim & Steve)<br />
* '''2017 March 8 ''': [[reionization_requirements| Reionization science]] (Simone & Marcelo)<br />
* '''2017 March 8 ''': [[High ell topics | High ell topics ]] (Jim)<br />
* '''2017 March 8 ''': [[SZ_s8_z | sigma 8 of z constraints ]] (Mat, Nick)<br />
* '''2017 March 8 ''': [[Szcounts | Number counts update for 1.0', 1.5', 2.0']] (Nick, Mat)<br />
* '''2017 March 8 ''': [[SZastro | SZ astrophysics with DESI ]](Nick, Simone, Emanuel, David)<br />
* '''2017 February 24''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170224_cmbs4_dc1_final/ BK-style processing of DC1.0 maps to spectra] (Justin Willmert, Colin Bischoff)<br />
* '''2017 February 15 ''': [[Extragalactic lensing sims| Update on extragalactic phase-2 lensing sims]] (Marcelo, George, Dick, others)<br />
* '''2017 February 15 ''': [[Plan for next Galactic Phase-2sims| Plan for next Galactic phase-2 sims]] (Jo, Ben)<br />
* '''2017 February 10 ''': [[Resolution of foreground-cleaned map]] (Mat, Neelima, Blake, Alex, others)<br />
* '''2017 February 10 ''': [[Nongaussian dust in lensing]] (Alex, Mat, Neelima, Blake, others)<br />
* '''2017 January 30''': [[Aliased power in noise maps]] (Bischoff, Updated 2017-02-02)<br />
* '''2017 January 23''': [[CMBS4 Band Sensitivity Comparison]] (Charlie Hill)<br />
* '''2017 January 12''': [http://bicep.rc.fas.harvard.edu/cbischoff/20170112_data_challenge_1/ Maps for CMB-S4 data challenge 1] (Bischoff, Pryke, Buza)<br />
* '''2016 December 21''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/vbuza/20161220_chkS4/ N_ell spectra for the CMB-S4 data challenge, and updated &sigma;(r) checkpoints] (Victor Buza, Updated 2017.02.01)<br />
* '''2016 November 30''': [[First steps to sim input maps]] (Clem P.)<br />
* '''2016 November 4''': [[Tophat bands for Data Challenge]] (Bischoff)<br />
* '''2016 July 8''': [[fsky|Dependence of foregrounds on sky fraction]] (Raphael)<br />
* '''2016 July 8''': [[SciBookPowspecTheoryFig|Three choices for Science Book Figure 5 (theory power spectrum & current BB points)]] (Tom C.)<br />
* '''2016 July 8''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/vbuza/20160707_s4plots/ S4 Inflation Chapter Plot Suggestions, V2] (Victor Buza)<br />
* '''2016 July 6''': [[w_cosntraint|Preliminary w constraint]] (Alessandro)<br />
* '''2016 June 24''': [[nsr|Preliminary ns-r plot for discussion]] (Raphael)<br />
* '''2016 June 16''': [[DelensingImpact| Impact Of Delensing On sigma(r)]] (Neelima/Mat)<br />
* '''2016 June 16''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/vbuza/20160616_s4plots/ S4 Inflation Chapter Plot Suggestions] (Victor Buza)<br />
* '''2016 June 10''': [[MapBasedRb| Map-based &sigma;(r) forecasts V2]] (David/Jo/Ben)<br />
* '''2016 June 3''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/vbuza/20160531_fisher/ &sigma;(r) forecasting checkpoints, V2] (Victor Buza)<br />
* '''2016 June 3''': [[ BTTfixedeffort | Forecasts for fnl BTT beam/fixed effort]] (Daan)<br />
* '''2016 May 31''': [[ForecastPatchyReion| Forecasts for patchy reionization]] (Vera, Alex, Nick)<br />
* '''2016 May 26''': [[Forecasting | Forecasts on neutrino mass]] (Nam, Mat, Neelima)<br />
* '''2016 May 26''': [[ KSZ| Forecasts on kSZ S/N]] (Simone, Emmanuel, Colin)<br />
* '''2016 May 26''': [[ Forecastfiso_planck| Forecast on correlated and anti-correlated CDM isocurvature f_iso]] (Kimmy, Cora, updated with plots 20160602)<br />
* '''2016 May 24''': [[ BTTNoiseBeam | Forecasts on fnl BTT beam/FWHM]] (Daan)<br />
* '''2016 May 22''': [[ ForecastAxions| Update on the axion isocurvature constraints for changing sensitivity and resolution]] (Renee)<br />
* '''2016 May 21''': [[ Forecastpann| Forecast on dark matter annihilation parameter p_ann]] (Kimmy, Cora)<br />
* '''2016 May 20''': [[NeffNoiseBeam| Forecasts on Neff and Yp]] (Joel, Alex)<br />
* '''2016 May 20''': [[ForecastEDE| Forecasts on Early Dark Energy]] (Erminia)<br />
* '''2016 May 20''': [[ForecastCompIsocurv| Forecasts on compensated isocurvature varying sensitivity, resolution and sky coverage]] (Julian, Ely)<br />
* '''2016 May 20''': [[ForecastBirefring| Forecasts on birefringence varying sensitivity and resolution]] (Vera, Alex)<br />
* '''2016 May 20''': [[ForecastStrings| Forecasts on string tension varying sensitivity and resolution]] (Renee)<br />
* '''2016 May 20''': [[RobustForecast| Cosmological forecasts including component separation and iterative delensing]] (Stephen Feeney and Josquin Errard)<br />
* '''2016 May 19''': [[MapBasedR| Map-based &sigma;(r) forecasts]] (David A.)<br />
* '''2016 May 18''': [[Shear_calibration_LSST|LSST shear calibration with CMB S4]] (Emmanuel Schaan)<br />
* '''2016 May 13''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/vbuza/20150505_fisher/ &sigma;(r) forecasting checkpoints] (Victor Buza)<br />
* '''2016 May 13''': [[NonGaussianitiesTTT| CMBS-4 forecasts local and equilateral scalar Ngs using TTT]] (daan)<br />
* '''2016 May 13''': [[ForecastingSims|Simulations for r forecasts]] (Jo/Ben/David)<br />
* '''2016 May 6''': [[DMInteractionsComplementarity|DM interactions: complementarity]] (Vera)<br />
* '''2016 May 6''': [[Scenarios| Scenarios]] (Scott, Vera)<br />
* ''' 2016 May 3''': [[ForecastAxions |Effect of S4 specs on axion density parameters]] (Renee)<br />
* '''2016 April 30''': [[ForecastNu| Effect of S4 specs on neutrino parameters]] (Erminia)<br />
* '''2016 April 28''': [http://web.stanford.edu/~wlwu/posting/20160421_lensres/ Delensing residuals with low-ell foregrounds] (Kimmy Wu)<br />
* '''2016 April 28''': [[NonGaussianities| CMBS-4 forecast for tensor NGs]] (daan)<br />
* '''2016 April 19''': [[ForecastingStep1| Checking basic parameters for nominal case]] (Jo + multiple authors)<br />
* '''2016 April 5''': [[Forecasting|Setting up non-r Fisher-based parameter forecasts]] (Jo + others)<br />
* '''2016 March 31''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/vbuza/20150331_fisher/ Fisher projections for &sigma;(r) based on achieved performance] (Victor Buza)<br />
* '''2016 January 27''': [https://cmb-s4.org/CMB-S4workshops/index.php/File:sptpol_ptsrc_polfrac_500d.pdf Quick estimate of mean-squared polarization fraction for SPTpol sources] (Tom Crawford)</div>Cbischoffhttp://www.cmb-s4.org/wiki/index.php?title=SAT_detector_counts,_NET,_and_overall_efficiency_from_DSR&diff=10294SAT detector counts, NET, and overall efficiency from DSR2019-11-12T16:30:36Z<p>Cbischoff: Created page with "''Colin Bischoff, 2019-11-12'' ---- As an input for time-domain sims, I reproduce below the detector counts and per-detector NET from Table 3-1 of the [https://arxiv.org/abs/..."</p>
<hr />
<div>''Colin Bischoff, 2019-11-12''<br />
----<br />
<br />
As an input for time-domain sims, I reproduce below the detector counts and per-detector NET from Table 3-1 of the [https://arxiv.org/abs/1907.04473 Decadal Survey Report].<br />
<br />
'''IMPORTANT NOTE''': In the arXiv version of the DSR, we accidentally swapped the per-detector NET for 95 and 145 GHz. This has been fixed in the Github repo (thanks Ben!) and it is noted in [https://docs.google.com/document/d/1LJUoq5ORck29tMsdugjEJ3-NJmqlRfm8K3qjD8qDixQ/edit this google doc]. The table below has correct values.<br />
<br />
{| class="wikitable"<br />
! Frequency !! # of optics tubes !! total # of detectors !! NET per-detector [&mu;K sqrt(s)] !! beam FWHM [arcmin]<br />
|-<br />
| 30 GHz || 2 || 576 || 177 || 72.8<br />
|-<br />
| 40 GHz || 2 || 576 || 224 || 72.8<br />
|-<br />
| 85 GHz || 6 || 21144 || 270 || 25.5<br />
|-<br />
| 95 GHz || 6 || 21144 || 238 || 22.7<br />
|-<br />
| 145 GHz || 6 || 21144 || 309 || 25.5<br />
|-<br />
| 155 GHz || 6 || 21144 || 331 || 22.7<br />
|-<br />
| 220 GHz || 4 || 33752 || 747 || 13<br />
|-<br />
| 270 GHz || 4 || 33752 || 1281 || 13<br />
|}<br />
<br />
The DSR also contains Table 2-1 (reproduced below), which lists the map depth and total survey weight (Q and U) for the ultra-deep survey. These are the numbers that are used for parameter forecasts, map-based Data Challenge simulations, etc.<br />
<br />
We can use the detector counts and per-detector NET from the table above to calculate an idealized version of total survey weight (for a seven-year survey):<br />
&tau; = 7 years &times; 365 days / year &times; 86400 seconds / day = 2.2e8 seconds<br />
sw_ideal [&mu;K<sup>-2</sup>] = &tau; &times; Ndet / NET<sup>2</sup><br />
If we take the ratio of the Table 2-1 forecast survey weight to this idealized survey weight, we obtain a value for the end-to-end efficiency that is being assumed in forecasting. The performance-based forecasting method uses the difference between idealized and achieved performance from BICEP/Keck, with SAT 30/40/85/95 GHz efficiency extrapolated from BK 95 GHz, SAT 145/155 GHz efficiency extrapolated from BK 150 GHz, and SAT 220/270 GHz efficiency extrapolated from BK 220 GHz, which accounts for the pattern of efficiency values shown below.<br />
<br />
{| class="wikitable"<br />
! Frequency !! Q/U rms [&mu;K arcmin] !! Total survey weight [&mu;K<sup>-2</sup>] !! End-to-end efficiency<br />
|-<br />
| 30 GHz || 3.5 || 0.69e6 || 17%<br />
|-<br />
| 40 GHz || 4.5 || 0.43e6 || 17%<br />
|-<br />
| 85 GHz || 0.88 || 11.0e6 || 17%<br />
|-<br />
| 95 GHz || 0.78 || 14.1e6 || 17%<br />
|-<br />
| 145 GHz || 1.2 || 5.7e6 || 11.5%<br />
|-<br />
| 155 GHz || 1.3 || 4.8e6 || 11.5%<br />
|- <br />
| 220 GHz || 3.5 || 0.71e6 || 5.3%<br />
|-<br />
| 270 GHz || 6.0 || 0.24e6 || 5.3%<br />
|}</div>Cbischoffhttp://www.cmb-s4.org/wiki/index.php?title=Science_Council&diff=10223Science Council2019-10-21T17:35:43Z<p>Cbischoff: /* Low-ell BB */</p>
<hr />
<div>The Science Council consists of two co-Chairs and the co-Coordinators of four Analysis Working Groups (AWGs). We list the working groups here, together with information<br />
about their activities -- such as information about when they meet and links to meeting notes. The co-Chairs are Gil Holder (gil.holder@gmail.com) and Lloyd Knox (lknox@ucdavis.edu).<br />
<br />
===Overview===<br />
Our main focus now is "flowing down" the science to measurement requirements in preparation for CD-1/PDR. <br />
<br />
===Analysis Working Groups===<br />
<br />
====Low-ell BB==== <br />
- Co-Coordinators: Colin Bischoff (bischocn@ucmail.uc.edu) and Kimmy Wu (wlwu@kicp.uchicago.edu)<br />
- Meeting Notes: https://docs.google.com/document/d/1886yT1b6QDuWvsbAu5HmVv2Cl4pfH00YpK5Fv8dNzcM<br />
- Shared logbook: [[Simulation_and_Forecasting_Logbook|Simulations and Forecasting Log Book]]<br />
- Data challenge summary pages: [[Data_Challenges|r forecast sim set summary]]<br />
- Meeting Times: Look for our meetings on the [https://calendar.google.com/calendar/embed?src=t7l87lpt7g2t6a7ak4qh0t72qg%40group.calendar.google.com&ctz=America%2FLos_Angeles[CMB-S4 Google Calendar]]<br />
- Forecast paper draft: [http://spud.spa.umn.edu/~pryke/s4_forecast_paper.pdf auto update pdf]<br />
<br />
====Maps2Cell====<br />
<br />
====Maps2OtherStats====<br />
<br />
====Sources====<br />
<br />
===Historical Stuff below here===<br />
<br />
====Science White Papers====<br />
<br />
We are envisioning a series of SWP submitted by the January 2019 deadline. The papers will describe the entirety of science deliverable with observations in CMB frequency bands (loosely defined). The SWPs are common to the entire community; they will not discuss nor highlight any specific project. All interested members of the community are invited to participate in writing and endorsing any of these papers. <br />
<br />
SWP drafts that are ready for comment are available here:<br />
1) Neutrino Mass from Cosmology<br />
Link to the draft: http://dvorkin.physics.harvard.edu/Astro2020_Neutrino_Mass.pdf<br />
Contact person: Cora Dvorkin (cdvorkin@g.harvard.edu)<br />
2) Primordial non-Gaussianity <br />
Link to the draft:https://www.overleaf.com/read/bfsyyxfdqnvq<br />
Contact Person: Daan Meerburg (daanmeerburg@gmail.com) <br />
3) Dark Matter Physics with Cosmological Probes<br />
Link to the draft [PRELIMINARY, incomplete]: https://github.com/veragluscevic/Astro2020-DM-Cosmology<br />
Contact person: Vera Gluscevic (vera.gluscevic@gmail.com)<br />
4) Dark Energy<br />
Link to the draft: https://www.overleaf.com/read/phkpmjbjydwq<br />
Contact person: Anze Slosar (anze@bnl.gov)<br />
5) Features in the primordial power spectrum<br />
Link to the draft: https://www.overleaf.com/read/kyxzvmrbqpgy<br />
Contact person: Anze Slosar (anze@bnl.gov)<br />
6) Messengers from the Early Universe: Cosmic Neutrinos and Other Light Relics <br />
Link to the draft: https://www.overleaf.com/read/ybxqdqnhvtkm<br />
Contact person: Dan Green (drgreen@ucsd.edu)<br />
7) Testing gravity and particle physics with cosmic microwave background constraints on gravitational waves<br />
Link to the draft: https://www.overleaf.com/read/dsfnphrxfgbn<br />
Contact person: Sarah Shandera (shandera@gmail.com)<br />
8) Probing Feedback in Galaxy Formation with Millimeter-wave Observations<br />
Link to the draft: https://www.overleaf.com/read/ypcrxscjwnwr<br />
Contact people: Colin Hill (jch@ias.edu) and Nick Battaglia (nbatta@astro.cornell.edu)<br />
9) Reionization with the CMB <br />
Link to the draft: https://www.overleaf.com/read/bhdvxzqbprkf<br />
Contact people: Marcelo Alvarez (marcelo.alvarez@berkeley.edu) and Cora Dvorkin (cdvorkin@g.harvard.edu)<br />
<br />
<br />
The SWP are limited to 5 pages or fewer each, and we highly recommend that anyone wishing to contribute will read the short National Academies solicitation. Excerpting this key passage from the call may be helpful here:<br />
<br />
White papers should:<br />
- Identify scientific opportunities and compelling scientific themes for the coming decade, particularly those that have arisen from recent advances and accomplishments in astronomy and astrophysics;<br />
- Describe the scientific context of the importance of these opportunities, including connections to other parts of astronomy and astrophysics and, where appropriate, to the advancement of our broader scientific understanding;<br />
- While focusing on science, not specific missions or projects, describe and quantify the key advances in observation, measurement, theory, and/or computation necessary to realize the scientific opportunities within the decade 2020-2030 and beyond.<br />
<br />
To facilitate engagement and coordination of activities, we have created a wiki page (https://zzz.physics.umn.edu/decadal2020/doku.php?id=start) with a (non-comprehensive) list of potential science white papers with relevance to our community. Listed there are titles, and (mostly blank) fields for listing who is actively participating in the creation of the white paper, who has taken on a coordinating role, and links to relevant documentation for that white paper (github repos, online notes, etc.). <br />
<br />
The purpose of the wiki page is to give all of us a comprehensive view of science white paper activity of relevance to the CMB community, make it possible for would-be contributors to join existing efforts, and to allow any of us to spot gaps and work to fill them. The list of paper titles on the wiki now is just to get us started -- we expect it to evolve as, e.g., some topics get split into two or more different white papers, and new topics altogether are added. Anyone wishing to edit the wiki should contact Shaul Hanany (hanany@umn.edu) to get the appropriate permissions.<br />
<br />
====CMB-S4 Decadal Survey Report====<br />
<br />
Each AWG (with some exceptions) is charged with producing a 5-page section, the main elements of the Science Chapter of the DSR, on the science to be done with the CMB-S4 surveys. Our target for completion of a first draft of the DSR is November 2018. <br />
<br />
=====Draft Schedule for Production of Science Chapter sections=====<br />
<br />
- Friday, Sept 28: Long and rough draft completed<br />
- Friday, Oct 19: 5-page rough draft completed<br />
- Friday, Nov 3: cleaned-up draft ready to go out for review and comment<br />
- Wednesday, Nov 21: comments due back to AWGs<br />
- Friday, Dec 7: DSR chapter finalized<br />
- Dec 11 to 13: Internal DSR review in Washington, D.C. Each AWG should have one co-coordinator there<br />
<br />
===Analysis Working Groups===<br />
<br />
====Primordial Gravitational Waves==== <br />
- Co-Coordinators: Raphael Flauger (flauger@physics.utexas.edu) and Clem Pryke (pryke@physics.umn.edu)<br />
- Meeting Notes: https://docs.google.com/document/d/1886yT1b6QDuWvsbAu5HmVv2Cl4pfH00YpK5Fv8dNzcM<br />
- Shared logbook: [[Simulation_and_Forecasting_Logbook|Simulations and Forecasting Log Book]]<br />
- Data challenge summary pages: [[Data_Challenges|r forecast sim set summary]]<br />
- Meeting Times: Look for our meetings on the [https://calendar.google.com/calendar/embed?src=t7l87lpt7g2t6a7ak4qh0t72qg%40group.calendar.google.com&ctz=America%2FLos_Angeles[CMB-S4 Google Calendar]]<br />
- Forecast paper draft: [http://spud.spa.umn.edu/~pryke/s4_forecast_paper.pdf[auto update pdf]]<br />
<br />
====Primordial Density Perturbations====<br />
- Co-Coordinators: Cora Dvorkin (cdvorkin@g.harvard.edu) & Daan Meerburg (daanmeerburg@gmail.com)<br />
<br />
- Telecons on-needed basis; see [https://calendar.google.com/calendar/embed?src=t7l87lpt7g2t6a7ak4qh0t72qg%40group.calendar.google.com&ctz=America%2FLos_Angeles[CMB-S4 Google Calendar]]<br />
<br />
====Light Relics====<br />
- Co-Coordinators: Daniel Green (drgreen@physics.ucsd.edu) and Joel Meyers (jmeyers@cita.utoronto.ca)<br />
- Forecasting Setup: [[Forecasting|Non-r Forecasting Page]]<br />
- Meeting Times: Look for our meetings on the [https://calendar.google.com/calendar/embed?src=t7l87lpt7g2t6a7ak4qh0t72qg%40group.calendar.google.com&ctz=America%2FLos_Angeles[CMB-S4 Google Calendar]]<br />
<br />
====Neutrino Mass====<br />
- Co-Coordinators: Marilena Loverde (marilena.loverde@stonybrook.edu) and Blake Sherwin (sherwin@damtp.cam.ac.uk)<br />
- Meeting notes: https://cmb-s4.org/wiki/index.php/Neutrino_Mass_WG_Telecon<br />
- Call summaries: https://docs.google.com/document/d/1TWaU75wN1kqbYD1qkwzcJA9fZXGviKSezj3EnlP-ep8/edit?usp=sharing<br />
- Meeting times: will be posted; typically Tuesday 11am ET<br />
====Dark Energy ====<br />
- Co-Coordinators: Anze Slosar (anze@bnl.gov), and David Alonso (David.Alonso@physics.ox.ac.uk)<br />
- Meeting Notes: https://docs.google.com/document/d/13RTNgJNlWd098EPLnQrAAlstqDtyE850P9HnNFqCJZk/edit?usp=sharing<br />
- Meetings organized on as-needed basis.<br />
<br />
====Dark Matter====<br />
- Co-Coordinators: Vera Gluscevic (verag@ias.edu), and Dan Grin (dgrin@haverford.edu)<br />
- DM interactions meeting minutes: https://docs.google.com/document/d/1RxG07ebylnbXqSHFIIujBl6kO-olEUY9XPM4kyy0EXs/edit<br />
- Telecons on-needed basis; see [https://calendar.google.com/calendar/embed?src=t7l87lpt7g2t6a7ak4qh0t72qg%40group.calendar.google.com&ctz=America%2FLos_Angeles[CMB-S4 Google Calendar]]<br />
).<br />
<br />
====Galaxy Formation and Evolution====<br />
- Co-Coordinators: Marcelo Alvarez (marcelo.alvarez@berkeley.edu) and Colin Hill (jcolin.hill@gmail.com)<br />
- Meeting Notes: https://docs.google.com/document/d/11vsmV9fdDd29Kds2WmEh5MddEP7BAO16xMnoxV-MwZY/edit?usp=sharing<br />
- Meeting Times: Look for our meetings on the [https://calendar.google.com/calendar/embed?src=t7l87lpt7g2t6a7ak4qh0t72qg%40group.calendar.google.com&ctz=America%2FLos_Angeles[CMB-S4 Google Calendar]]<br />
<br />
====Legacy Catalogs====<br />
- Co-Coordinators: Lindsey Bleem (lbleem@anl.gov) and Douglas Scott (dscott@phas.ubc.ca)<br />
- Meeting Notes: https://docs.google.com/document/d/169aZRZiqL3uJ2Eg9LY3ytAlR5UPCesJGp4lfVIAFWyA/edit?usp=sharing<br />
- Meeting Times: TBD; will be posted [https://calendar.google.com/calendar/embed?src=t7l87lpt7g2t6a7ak4qh0t72qg%40group.calendar.google.com&ctz=America%2FLos_Angeles[CMB-S4 Google Calendar]]</div>Cbischoffhttp://www.cmb-s4.org/wiki/index.php?title=UCSD-2019:_Committees:_Education_%26_Public_Outreach&diff=10209UCSD-2019: Committees: Education & Public Outreach2019-10-19T17:30:23Z<p>Cbischoff: /* McMahon: CMB analysis summer school */</p>
<hr />
<div>[https://cmb-s4.org/wiki/index.php/UCSD-2019:_Cosmology_with_CMB-S4#Agenda Link back to agenda]<br />
<br />
== Charge ==<br />
<br />
# Identify key decisions that must be made (and justified) prior to CD-1,<br />
# Make progress on (or actually make) those decisions, <br />
# Lay out a timeline and process for making each decision, consistent with the post-decision work and internal reviews that will be needed to complete preparations for CD-1,<br />
# Ensure that those timelines and processes are understood and supported by the collaboration, and that we (together) believe we can follow them.<br />
<br />
=== Key Issues ===<br />
<br />
* What is the overarching design of the EPO program?<br />
* What is the recording / reporting structure?<br />
* What EPO plan in Chile would we like to propose and how do we coordinate with local resources?<br />
<br />
== Agenda ==<br />
<br />
* Jeff McMahon: [https://sites.google.com/umich.edu/mcmahoncosmology/cmb-school CMB summer school]<br />
* Kirit Karkare: [http://bicep.rc.fas.harvard.edu/student_cmb_lab CMB measurement lab]<br />
* Nick Galitzki: SO education and outreach program<br />
* [https://www.lsst.org/about/epo LSST EPO]<br />
<br />
== Remote Attendance ==<br />
<br />
[https://ucsd.zoom.us/j/424492016 Zoom link]<br />
<br />
== Notes ==<br />
<br />
=== Karkare: CMB Measurement Lab ===<br />
<br />
* Ay191 class for undergrads at Harvard. Experimental lab course for junior or senior physics / astronomy majors. Build experiment from scratch over the course of a semester.<br />
* Recreate Penzias and Wilson CMB discovery by building and operating a CMB telescope.<br />
* Have been able to export this experiment to Wesleyan (professor Meredith Hughes), but it took a lot of effort -- shows that more documentation is needed. Project has run at Harvard several times.<br />
* Cheap TV receiver as detector, but need a cold (LN2) load. Horn and cone forebaffle are both critical for performance -- need machinist help for construction.<br />
* Planning to write up project in American Journal of Physics.<br />
* Are there lower friction versions of this project? If apparatus was already designed / built, students could take the measurement. Experience of building components is still really valuable.<br />
<br />
=== Galitzki: SO outreach ===<br />
<br />
* Got lots of good advice from Rachel Wolf (DES): need to make policies early on, decide that EPO efforts will be funded.<br />
* Kasey has form to log EPO activities across the collaboration. Sprawling collaboration, lots of independent activities.<br />
** Share resources for demos, etc.<br />
* Also have "flagship programs":<br />
** junior member mentoring program<br />
** Chilean program being run by Paolo (site coordinator... now working for CTA). Worked with Chilean artist collective to design prints that illustrate core science concepts. Took these to school for art classes. This evaporated after Paolo left the project, but would be useful to collaborate with other Chilean telescopes (ALMA, CCAT-Prime).<br />
* SO Youtube channel. Videographer Stuart employed to produce interview with SO scientists, other work. Also working with a company to revamp SO website.<br />
* Pontifica Universita Catholica runs astronomy summer school. Jeff McMahon will be down there in January <br />
* Social media: twitter, facebook, youtube. All provide statistics for engagement. This should be helpful for NSF reporting.<br />
** Cycle through a list of collaborators, who are each in charge for a week.<br />
** Haven't done instagram in any official way.<br />
** Tim suggests looking into Hootsuite -- cross-platform management tool that interfaces to twitter, instagram, facebook, etc. Preschedule posts, etc.<br />
** Nick has password for CMB-S4 twitter account. Do we need to acquire / sit on web domains, social media accounts, etc. (What about changing the experiment name?)<br />
* SO does an outreach event with every face-to-face meeting. CMB-S4 should do this. Requires advance planning with someone who is local and enthusiastic.<br />
* Produce a list of contacts at different institutions, so interested people can find a CMB-S4 scientist near them.<br />
<br />
=== McMahon: CMB analysis summer school ===<br />
<br />
* Jupyter notebooks that work through CMB simulation and analysis. Use only numpy/matplotlib, so people can see everything that goes on under the hood.<br />
* Taking this to Chilean astronomy summer school. One outcome will be to get notebooks translated to Spanish.<br />
* These are designed for grad students, etc. Is there a way to do something similar with high school students? <br />
** Need to have different goals with different groups / audiences.<br />
** Darcy suggests look at CUNY Astronomy -- they have materials to get people up to speed who come in with little background.<br />
* HERA has a program where they get REU students from California high schools. <br />
** Is there a way to fund REU students for multiple summers?<br />
<br />
=== Discussion: what should CMB-S4 EPO program do? ===<br />
<br />
* Establish tracking for collaboration member activities<br />
** Encourage collaboration members to work with arts / outreach departments at your own institution.<br />
* Set up social media and improve public-facing website<br />
* Actually do outreach event at next collaboration meeting. Where is the next CMB-S4 meeting?<br />
* Need to pick one or two "flagship projects" -- draft a document describing EPO plan: goals and audiences. Have this ready for next collaboration meeting.<br />
* Create an EPO email list that collaboration members can sign up for (distinct from EPO committee list)<br />
* Create a wiki page for people to brainstorm EPO projects. Lloyd will do this right now.<br />
** Think about existing contacts, i.e. Globetrotters going to South Pole.<br />
* Can we use interest in cosmology to improve general science literacy? "Astronomy is a gateway science"<br />
* Do outreach to audience of informal science education professionals. Set up a booth at a conference to publicize the content we are creating. ASTC is North American conference, held annually.</div>Cbischoffhttp://www.cmb-s4.org/wiki/index.php?title=UCSD-2019:_Committees:_Education_%26_Public_Outreach&diff=10203UCSD-2019: Committees: Education & Public Outreach2019-10-19T17:20:14Z<p>Cbischoff: /* Notes */</p>
<hr />
<div>[https://cmb-s4.org/wiki/index.php/UCSD-2019:_Cosmology_with_CMB-S4#Agenda Link back to agenda]<br />
<br />
== Charge ==<br />
<br />
# Identify key decisions that must be made (and justified) prior to CD-1,<br />
# Make progress on (or actually make) those decisions, <br />
# Lay out a timeline and process for making each decision, consistent with the post-decision work and internal reviews that will be needed to complete preparations for CD-1,<br />
# Ensure that those timelines and processes are understood and supported by the collaboration, and that we (together) believe we can follow them.<br />
<br />
=== Key Issues ===<br />
<br />
* What is the overarching design of the EPO program?<br />
* What is the recording / reporting structure?<br />
* What EPO plan in Chile would we like to propose and how do we coordinate with local resources?<br />
<br />
== Agenda ==<br />
<br />
* Jeff McMahon: [https://sites.google.com/umich.edu/mcmahoncosmology/cmb-school CMB summer school]<br />
* Kirit Karkare: [http://bicep.rc.fas.harvard.edu/student_cmb_lab CMB measurement lab]<br />
* Nick Galitzki: SO education and outreach program<br />
* [https://www.lsst.org/about/epo LSST EPO]<br />
<br />
== Remote Attendance ==<br />
<br />
[https://ucsd.zoom.us/j/424492016 Zoom link]<br />
<br />
== Notes ==<br />
<br />
=== Karkare: CMB Measurement Lab ===<br />
<br />
* Ay191 class for undergrads at Harvard. Experimental lab course for junior or senior physics / astronomy majors. Build experiment from scratch over the course of a semester.<br />
* Recreate Penzias and Wilson CMB discovery by building and operating a CMB telescope.<br />
* Have been able to export this experiment to Wesleyan (professor Meredith Hughes), but it took a lot of effort -- shows that more documentation is needed. Project has run at Harvard several times.<br />
* Cheap TV receiver as detector, but need a cold (LN2) load. Horn and cone forebaffle are both critical for performance -- need machinist help for construction.<br />
* Planning to write up project in American Journal of Physics.<br />
* Are there lower friction versions of this project? If apparatus was already designed / built, students could take the measurement. Experience of building components is still really valuable.<br />
<br />
=== Galitzki: SO outreach ===<br />
<br />
* Got lots of good advice from Rachel Wolf (DES): need to make policies early on, decide that EPO efforts will be funded.<br />
* Kasey has form to log EPO activities across the collaboration. Sprawling collaboration, lots of independent activities.<br />
** Share resources for demos, etc.<br />
* Also have "flagship programs":<br />
** junior member mentoring program<br />
** Chilean program being run by Paolo (site coordinator... now working for CTA). Worked with Chilean artist collective to design prints that illustrate core science concepts. Took these to school for art classes. This evaporated after Paolo left the project, but would be useful to collaborate with other Chilean telescopes (ALMA, CCAT-Prime).<br />
* SO Youtube channel. Videographer Stuart employed to produce interview with SO scientists, other work. Also working with a company to revamp SO website.<br />
* Pontifica Universita Catholica runs astronomy summer school. Jeff McMahon will be down there in January <br />
* Social media: twitter, facebook, youtube. All provide statistics for engagement. This should be helpful for NSF reporting.<br />
** Cycle through a list of collaborators, who are each in charge for a week.<br />
** Haven't done instagram in any official way.<br />
** Tim suggests looking into Hootsuite -- cross-platform management tool that interfaces to twitter, instagram, facebook, etc. Preschedule posts, etc.<br />
** Nick has password for CMB-S4 twitter account. Do we need to acquire / sit on web domains, social media accounts, etc. (What about changing the experiment name?)<br />
* SO does an outreach event with every face-to-face meeting. CMB-S4 should do this. Requires advance planning with someone who is local and enthusiastic.<br />
* Produce a list of contacts at different institutions, so interested people can find a CMB-S4 scientist near them.<br />
<br />
=== McMahon: CMB analysis summer school ===<br />
<br />
* Jupyter notebooks that work through CMB simulation and analysis. Use only numpy/matplotlib, so people can see everything that goes on under the hood.<br />
* Taking this to Chilean astronomy summer school. One outcome will be to get notebooks translated to Spanish.<br />
* These are designed for grad students, etc. Is there a way to do something similar with high school students? <br />
** Need to have different goals with different groups / audiences.<br />
* HERA has a program where they get REU students from California high schools. <br />
** Is there a way to fund REU students for multiple summers?<br />
<br />
=== Discussion: what should CMB-S4 EPO program do? ===<br />
<br />
* Establish tracking for collaboration member activities<br />
** Encourage collaboration members to work with arts / outreach departments at your own institution.<br />
* Set up social media and improve public-facing website<br />
* Actually do outreach event at next collaboration meeting. Where is the next CMB-S4 meeting?<br />
* Need to pick one or two "flagship projects" -- draft a document describing EPO plan: goals and audiences. Have this ready for next collaboration meeting.<br />
* Create an EPO email list that collaboration members can sign up for (distinct from EPO committee list)<br />
* Create a wiki page for people to brainstorm EPO projects. Lloyd will do this right now.<br />
** Think about existing contacts, i.e. Globetrotters going to South Pole.<br />
* Can we use interest in cosmology to improve general science literacy? "Astronomy is a gateway science"<br />
* Do outreach to audience of informal science education professionals. Set up a booth at a conference to publicize the content we are creating. ASTC is North American conference, held annually.</div>Cbischoffhttp://www.cmb-s4.org/wiki/index.php?title=UCSD-2019:_Committees:_Education_%26_Public_Outreach&diff=10193UCSD-2019: Committees: Education & Public Outreach2019-10-19T16:51:28Z<p>Cbischoff: /* Notes */</p>
<hr />
<div>[https://cmb-s4.org/wiki/index.php/UCSD-2019:_Cosmology_with_CMB-S4#Agenda Link back to agenda]<br />
<br />
== Charge ==<br />
<br />
# Identify key decisions that must be made (and justified) prior to CD-1,<br />
# Make progress on (or actually make) those decisions, <br />
# Lay out a timeline and process for making each decision, consistent with the post-decision work and internal reviews that will be needed to complete preparations for CD-1,<br />
# Ensure that those timelines and processes are understood and supported by the collaboration, and that we (together) believe we can follow them.<br />
<br />
=== Key Issues ===<br />
<br />
* What is the overarching design of the EPO program?<br />
* What is the recording / reporting structure?<br />
* What EPO plan in Chile would we like to propose and how do we coordinate with local resources?<br />
<br />
== Agenda ==<br />
<br />
* Jeff McMahon: [https://sites.google.com/umich.edu/mcmahoncosmology/cmb-school CMB summer school]<br />
* Kirit Karkare: [http://bicep.rc.fas.harvard.edu/student_cmb_lab CMB measurement lab]<br />
* Nick Galitzki: SO education and outreach program<br />
* [https://www.lsst.org/about/epo LSST EPO]<br />
<br />
== Remote Attendance ==<br />
<br />
[https://ucsd.zoom.us/j/424492016 Zoom link]<br />
<br />
== Notes ==<br />
<br />
=== Karkare: CMB Measurement Lab ===<br />
<br />
* Ay191 class for undergrads at Harvard. Experimental lab course for junior or senior physics / astronomy majors. Build experiment from scratch over the course of a semester.<br />
* Recreate Penzias and Wilson CMB discovery by building and operating a CMB telescope.<br />
* Have been able to export this experiment to Wesleyan (professor Meredith Hughes), but it took a lot of effort -- shows that more documentation is needed. Project has run at Harvard several times.<br />
* Cheap TV receiver as detector, but need a cold (LN2) load. Horn and cone forebaffle are both critical for performance -- need machinist help for construction.<br />
* Planning to write up project in American Journal of Physics.<br />
* Are there lower friction versions of this project? If apparatus was already designed / built, students could take the measurement. Experience of building components is still really valuable.<br />
<br />
=== Galitzki: SO outreach ===<br />
<br />
* Got lots of good advice from Rachel Wolf (DES): need to make policies early on, decide that EPO efforts will be funded.<br />
* Kasey has form to log EPO activities across the collaboration. Sprawling collaboration, lots of independent activities.<br />
** Share resources for demos, etc.<br />
* Also have "flagship programs":<br />
** junior member mentoring program<br />
** Chilean program being run by Paolo (site coordinator... now working for CTA). Worked with Chilean artist collective to design prints that illustrate core science concepts. Took these to school for art classes. This evaporated after Paolo left the project, but would be useful to collaborate with other Chilean telescopes (ALMA, CCAT-Prime).<br />
* SO Youtube channel. Videographer Stuart employed to produce interview with SO scientists, other work. Also working with a company to revamp SO website.<br />
* Pontifica Universita Catholica runs astronomy summer school. Jeff McMahon will be down there in January <br />
* Social media: twitter, facebook, youtube. All provide statistics for engagement. This should be helpful for NSF reporting.<br />
** Cycle through a list of collaborators, who are each in charge for a week.<br />
** Haven't done instagram in any official way.<br />
** Tim suggests looking into Hootsuite -- cross-platform management tool that interfaces to twitter, instagram, facebook, etc. Preschedule posts, etc.<br />
** Nick has password for CMB-S4 twitter account. Do we need to acquire / sit on web domains, social media accounts, etc. (What about changing the experiment name?)<br />
* SO does an outreach event with every face-to-face meeting. CMB-S4 should do this. Requires advance planning with someone who is local and enthusiastic.<br />
* Produce a list of contacts at different institutions, so interested people can find a CMB-S4 scientist near them.<br />
<br />
=== McMahon: CMB analysis summer school ===<br />
<br />
* Jupyter notebooks that work through CMB simulation and analysis. Use only numpy/matplotlib, so people can see everything that goes on under the hood.<br />
* Taking this to Chilean astronomy summer school. One outcome will be to get notebooks translated to Spanish.<br />
* These are designed for grad students, etc. Is there a way to do something similar with high school students? <br />
** Need to have different goals with different groups / audiences.<br />
* HERA has a program where they get REU students from California high schools. <br />
** Is there a way to fund REU students for multiple summers?</div>Cbischoffhttp://www.cmb-s4.org/wiki/index.php?title=UCSD-2019:_Committees:_Education_%26_Public_Outreach&diff=10188UCSD-2019: Committees: Education & Public Outreach2019-10-19T16:29:09Z<p>Cbischoff: /* Notes */</p>
<hr />
<div>[https://cmb-s4.org/wiki/index.php/UCSD-2019:_Cosmology_with_CMB-S4#Agenda Link back to agenda]<br />
<br />
== Charge ==<br />
<br />
# Identify key decisions that must be made (and justified) prior to CD-1,<br />
# Make progress on (or actually make) those decisions, <br />
# Lay out a timeline and process for making each decision, consistent with the post-decision work and internal reviews that will be needed to complete preparations for CD-1,<br />
# Ensure that those timelines and processes are understood and supported by the collaboration, and that we (together) believe we can follow them.<br />
<br />
=== Key Issues ===<br />
<br />
* What is the overarching design of the EPO program?<br />
* What is the recording / reporting structure?<br />
* What EPO plan in Chile would we like to propose and how do we coordinate with local resources?<br />
<br />
== Agenda ==<br />
<br />
* Jeff McMahon: [https://sites.google.com/umich.edu/mcmahoncosmology/cmb-school CMB summer school]<br />
* Kirit Karkare: [http://bicep.rc.fas.harvard.edu/student_cmb_lab CMB measurement lab]<br />
* Nick Galitzki: SO education and outreach program<br />
* [https://www.lsst.org/about/epo LSST EPO]<br />
<br />
== Remote Attendance ==<br />
<br />
[https://ucsd.zoom.us/j/424492016 Zoom link]<br />
<br />
== Notes ==<br />
<br />
=== Karkare: CMB Measurement Lab ===<br />
<br />
* Ay191 class for undergrads at Harvard. Experimental lab course for junior or senior physics / astronomy majors. Build experiment from scratch over the course of a semester.<br />
* Recreate Penzias and Wilson CMB discovery by building and operating a CMB telescope.<br />
* Have been able to export this experiment to Wesleyan (professor Meredith Hughes), but it took a lot of effort -- shows that more documentation is needed. Project has run at Harvard several times.<br />
* Cheap TV receiver as detector, but need a cold (LN2) load. Horn and cone forebaffle are both critical for performance -- need machinist help for construction.<br />
* Planning to write up project in American Journal of Physics.<br />
* Are there lower friction versions of this project? If apparatus was already designed / built, students could take the measurement. Experience of building components is still really valuable.<br />
<br />
=== Galitzki: SO outreach ===<br />
<br />
* Got lots of good advice from Rachel Wolf (DES): need to make policies early on, decide that EPO efforts will be funded.<br />
* Kasey has form to log EPO activities across the collaboration. Sprawling collaboration, lots of independent activities.<br />
** Share resources for demos, etc.<br />
* Also have "flagship programs":<br />
** junior member mentoring program<br />
** Chilean program being run by Paolo (site coordinator... now working for CTA). Worked with Chilean artist collective to design prints that illustrate core science concepts. Took these to school for art classes. This evaporated after Paolo left the project, but would be useful to collaborate with other Chilean telescopes (ALMA, CCAT-Prime).<br />
* SO Youtube channel. Videographer Stuart employed to produce interview with SO scientists, other work. Also working with a company to revamp SO website.<br />
* Pontifica Universita Catholica runs astronomy summer school. Jeff McMahon will be down there in January <br />
* Social media: twitter, facebook, youtube. All provide statistics for engagement. This should be helpful for NSF reporting.<br />
** Cycle through a list of collaborators, who are each in charge for a week.<br />
** Haven't done instagram in any official way.<br />
** Tim suggests looking into Hootsuite -- cross-platform management tool that interfaces to twitter, instagram, facebook, etc. Preschedule posts, etc.<br />
** Nick has password for CMB-S4 twitter account. Do we need to acquire / sit on web domains, social media accounts, etc. (What about changing the experiment name?)<br />
* SO does an outreach event with every face-to-face meeting. CMB-S4 should do this. Requires advance planning with someone who is local and enthusiastic.<br />
* Produce a list of contacts at different institutions, so interested people can find a CMB-S4 scientist near them.</div>Cbischoffhttp://www.cmb-s4.org/wiki/index.php?title=UCSD-2019:_Committees:_Education_%26_Public_Outreach&diff=10175UCSD-2019: Committees: Education & Public Outreach2019-10-19T15:54:36Z<p>Cbischoff: /* Karkare: CMB Measurement Lab */</p>
<hr />
<div>[https://cmb-s4.org/wiki/index.php/UCSD-2019:_Cosmology_with_CMB-S4#Agenda Link back to agenda]<br />
<br />
== Charge ==<br />
<br />
# Identify key decisions that must be made (and justified) prior to CD-1,<br />
# Make progress on (or actually make) those decisions, <br />
# Lay out a timeline and process for making each decision, consistent with the post-decision work and internal reviews that will be needed to complete preparations for CD-1,<br />
# Ensure that those timelines and processes are understood and supported by the collaboration, and that we (together) believe we can follow them.<br />
<br />
=== Key Issues ===<br />
<br />
* What is the overarching design of the EPO program?<br />
* What is the recording / reporting structure?<br />
* What EPO plan in Chile would we like to propose and how do we coordinate with local resources?<br />
<br />
== Agenda ==<br />
<br />
* Jeff McMahon: [https://sites.google.com/umich.edu/mcmahoncosmology/cmb-school CMB summer school]<br />
* Kirit Karkare: [http://bicep.rc.fas.harvard.edu/student_cmb_lab CMB measurement lab]<br />
* Nick Galitzki: SO education and outreach program<br />
* [https://www.lsst.org/about/epo LSST EPO]<br />
<br />
== Remote Attendance ==<br />
<br />
[https://ucsd.zoom.us/j/424492016 Zoom link]<br />
<br />
== Notes ==<br />
<br />
=== Karkare: CMB Measurement Lab ===<br />
<br />
* Ay191 class for undergrads at Harvard. Experimental lab course for junior or senior physics / astronomy majors. Build experiment from scratch over the course of a semester.<br />
* Recreate Penzias and Wilson CMB discovery by building and operating a CMB telescope.<br />
* Have been able to export this experiment to Wesleyan (professor Meredith Hughes), but it took a lot of effort -- shows that more documentation is needed. Project has run at Harvard several times.<br />
* Cheap TV receiver as detector, but need a cold (LN2) load. Horn and cone forebaffle are both critical for performance -- need machinist help for construction.<br />
* Planning to write up project in American Journal of Physics.<br />
* Are there lower friction versions of this project? If apparatus was already designed / built, students could take the measurement. Experience of building components is still really valuable.</div>Cbischoffhttp://www.cmb-s4.org/wiki/index.php?title=UCSD-2019:_Committees:_Education_%26_Public_Outreach&diff=10174UCSD-2019: Committees: Education & Public Outreach2019-10-19T15:45:00Z<p>Cbischoff: /* Agenda */</p>
<hr />
<div>[https://cmb-s4.org/wiki/index.php/UCSD-2019:_Cosmology_with_CMB-S4#Agenda Link back to agenda]<br />
<br />
== Charge ==<br />
<br />
# Identify key decisions that must be made (and justified) prior to CD-1,<br />
# Make progress on (or actually make) those decisions, <br />
# Lay out a timeline and process for making each decision, consistent with the post-decision work and internal reviews that will be needed to complete preparations for CD-1,<br />
# Ensure that those timelines and processes are understood and supported by the collaboration, and that we (together) believe we can follow them.<br />
<br />
=== Key Issues ===<br />
<br />
* What is the overarching design of the EPO program?<br />
* What is the recording / reporting structure?<br />
* What EPO plan in Chile would we like to propose and how do we coordinate with local resources?<br />
<br />
== Agenda ==<br />
<br />
* Jeff McMahon: [https://sites.google.com/umich.edu/mcmahoncosmology/cmb-school CMB summer school]<br />
* Kirit Karkare: [http://bicep.rc.fas.harvard.edu/student_cmb_lab CMB measurement lab]<br />
* Nick Galitzki: SO education and outreach program<br />
* [https://www.lsst.org/about/epo LSST EPO]<br />
<br />
== Remote Attendance ==<br />
<br />
[https://ucsd.zoom.us/j/424492016 Zoom link]<br />
<br />
== Notes ==<br />
<br />
=== Karkare: CMB Measurement Lab ===<br />
<br />
* Ay191 class for undergrads at Harvard. Experimental lab course for junior or senior physics / astronomy majors. Build experiment from scratch over the course of a semester.<br />
* Recreate Penzias and Wilson CMB discovery by building and operating a CMB telescope.</div>Cbischoffhttp://www.cmb-s4.org/wiki/index.php?title=UCSD-2019:_Committees:_Education_%26_Public_Outreach&diff=10172UCSD-2019: Committees: Education & Public Outreach2019-10-19T15:43:57Z<p>Cbischoff: /* Notes */</p>
<hr />
<div>[https://cmb-s4.org/wiki/index.php/UCSD-2019:_Cosmology_with_CMB-S4#Agenda Link back to agenda]<br />
<br />
== Charge ==<br />
<br />
# Identify key decisions that must be made (and justified) prior to CD-1,<br />
# Make progress on (or actually make) those decisions, <br />
# Lay out a timeline and process for making each decision, consistent with the post-decision work and internal reviews that will be needed to complete preparations for CD-1,<br />
# Ensure that those timelines and processes are understood and supported by the collaboration, and that we (together) believe we can follow them.<br />
<br />
=== Key Issues ===<br />
<br />
* What is the overarching design of the EPO program?<br />
* What is the recording / reporting structure?<br />
* What EPO plan in Chile would we like to propose and how do we coordinate with local resources?<br />
<br />
== Agenda ==<br />
<br />
* Jeff McMahon: [https://sites.google.com/umich.edu/mcmahoncosmology/cmb-school CMB summer school]<br />
* Kirit Karkare: CMB measurement lab<br />
* Nick Galitzki: SO education and outreach program<br />
* [https://www.lsst.org/about/epo LSST EPO]<br />
<br />
== Remote Attendance ==<br />
<br />
[https://ucsd.zoom.us/j/424492016 Zoom link]<br />
<br />
== Notes ==<br />
<br />
=== Karkare: CMB Measurement Lab ===<br />
<br />
* Ay191 class for undergrads at Harvard. Experimental lab course for junior or senior physics / astronomy majors. Build experiment from scratch over the course of a semester.<br />
* Recreate Penzias and Wilson CMB discovery by building and operating a CMB telescope.</div>Cbischoffhttp://www.cmb-s4.org/wiki/index.php?title=UCSD-2019:_Committees:_Education_%26_Public_Outreach&diff=10169UCSD-2019: Committees: Education & Public Outreach2019-10-19T15:36:42Z<p>Cbischoff: /* Agenda */</p>
<hr />
<div>[https://cmb-s4.org/wiki/index.php/UCSD-2019:_Cosmology_with_CMB-S4#Agenda Link back to agenda]<br />
<br />
== Charge ==<br />
<br />
# Identify key decisions that must be made (and justified) prior to CD-1,<br />
# Make progress on (or actually make) those decisions, <br />
# Lay out a timeline and process for making each decision, consistent with the post-decision work and internal reviews that will be needed to complete preparations for CD-1,<br />
# Ensure that those timelines and processes are understood and supported by the collaboration, and that we (together) believe we can follow them.<br />
<br />
=== Key Issues ===<br />
<br />
* What is the overarching design of the EPO program?<br />
* What is the recording / reporting structure?<br />
* What EPO plan in Chile would we like to propose and how do we coordinate with local resources?<br />
<br />
== Agenda ==<br />
<br />
* Jeff McMahon: [https://sites.google.com/umich.edu/mcmahoncosmology/cmb-school CMB summer school]<br />
* Kirit Karkare: CMB measurement lab<br />
* Nick Galitzki: SO education and outreach program<br />
* [https://www.lsst.org/about/epo LSST EPO]<br />
<br />
== Remote Attendance ==<br />
<br />
[https://ucsd.zoom.us/j/424492016 Zoom link]<br />
<br />
== Notes ==</div>Cbischoffhttp://www.cmb-s4.org/wiki/index.php?title=UCSD-2019:_Analysis/Pipeline_Working_Group:_Low-ell_BB&diff=10129UCSD-2019: Analysis/Pipeline Working Group: Low-ell BB2019-10-18T22:46:29Z<p>Cbischoff: /* Notes */</p>
<hr />
<div>[https://cmb-s4.org/wiki/index.php/UCSD-2019:_Cosmology_with_CMB-S4#Agenda Link back to agenda]<br />
<br />
== Charge ==<br />
<br />
# Identify key decisions that must be made (and justified) prior to CD-1,<br />
# Make progress on (or actually make) those decisions, <br />
# Lay out a timeline and process for making each decision, consistent with the post-decision work and internal reviews that will be needed to complete preparations for CD-1,<br />
# Ensure that those timelines and processes are understood and supported by the collaboration, and that we (together) believe we can follow them.<br />
<br />
=== Key Issues ===<br />
<br />
* How do we optimize detector allocation across frequency in the face of uncertainty about foreground properties, for both the SATs and the delensing LAT? <br />
* What are the advantages of split bands? How does performance compare to non-split bands?<br />
* Do we need a 20 GHz channel on delensing LAT (for SAT science)<br />
* How well will de-lensing work in practice? <br />
* What are the necessary analysis tools to answer these questions?<br />
<br />
=== What is CD-1? ===<br />
Blatantly copied from [[UCSD-2019: Analysis/Pipeline Working Group: Maps to C_ell | Analysis/Pipeline Working Group: Maps to C_ell]]:<br />
<br />
Background/clarifying questions:<br />
<br />
* What does “by CD-1” mean, and what are the implications for when tools need to be in place and working?<br />
** According to APC white paper (https://arxiv.org/abs/1908.01062), CD-1 is in Q3 of FY2021 (so June 2021?).<br />
*** But according to project office, "Plan [must be] finalized by start of 2020 for delivering...CD-1"<br />
** Working backward from there, any tool that could reasonably influence a CD-1 decision needs to be in place and working by ... ?<br />
** Give an example timeline for an example decision?<br />
<br />
== Agenda ==<br />
<br />
<br />
# Introduction by everyone in the room: who? where? what aspects of low-ell BB interest you? 5 minutes<br />
# Recap of the plan for this session/CD-1 goals [https://docs.google.com/presentation/d/1Mg1LAUMPJQuLv_Qlk0rXA51KijHwe9BYMAZaLfziE4Y/edit?usp=sharing slides][Wu], 3 minutes<br />
# [https://cmb-s4.org/wiki/images/UCSD_PGW_lowellBB_vbuza.pdf Review of Fisher based S4 forecasting thus far leading to DSR appendix A] [Ben/Victor/Raphael], 15 minutes<br />
# Review of Map based S4 forecasting thus far and ideas for next steps [https://docs.google.com/presentation/d/13WQ7t6cyAfchYjKEGw3iuR1U_8QxEC7pJAHmNUmqjXQ Clem], 10 minutes<br />
# Review of forecasting and simulations for Simons Observatory inflation science [Alonso / Errard / Sherwin], [https://docs.google.com/presentation/d/12m5qjX8jRa1nFZBwdAeFUOQY3CsW43LnMIubRAgG5OQ/edit?usp=sharing slides] [https://drive.google.com/file/d/1XmSwtMbtV0yuqwBngwM-f7IAfgQp6UAB/view?usp=sharing delensing slides] 30 minutes<br />
# Plans for working group [all], ~60 minutes<br />
## Forecasting<br />
##* Quantitative comparison of SO and CMB-S4 DSR forecasts<br />
##* Optimization of delensing effort: update for DSR sensitivity, motivation for frequency coverage, feedback from real delensing efforts<br />
## Data Challenge simulations<br />
##* More / better foreground models<br />
##* Instrumental systematics<br />
##* Other map non-idealities, i.e. filtering / mode loss<br />
##* Coordination with technical groups on instrument configuration, etc<br />
##* What else needs to be demonstrated for CD1?<br />
##* Bottlenecks for sim production<br />
## Analysis of Data Challenges<br />
##* Who plans to participate? How do we get more participation?<br />
##* Delensing<br />
## Specific Data Challenge plan / timeline<br />
##* Experiment config 06: DSR configuration, in progress<br />
##* Update / reoptimization of delensing survey?<br />
##* Inclusion of instrumental systematics -- which ones? how to include?<br />
##* Data Challenges coming out of Data Management group<br />
<br />
== Remote attendance ==<br />
<br />
Join Zoom Meeting<br />
https://zoom.us/j/340796462?pwd=S1o3Q3NQUlFOWkVVUXVrV1laK0JrQT09<br />
<br />
*Meeting ID: 340 796 462<br />
*Password: 654876<br />
<br />
*One tap mobile<br />
*+14086380968,,340796462# US (San Jose)<br />
*+16465588656,,340796462# US (New York)<br />
<br />
*Dial by your location<br />
* +1 408 638 0968 US (San Jose)<br />
* +1 646 558 8656 US (New York)<br />
*Meeting ID: 340 796 462<br />
*Find your local number: https://zoom.us/u/aeGN6VEA3T<br />
<br />
== Notes ==<br />
<br />
=== Buza / Racine: CMB-S4 PGW Forecasting ===<br />
<br />
* Forecasting loop: achieved performance used to forecast CMB-S4 instrument -> generate map-based sims with sky model -> analyze to determine sigma(r) and compare to forecast<br />
* 9 bands spanning 4 atmospheric windows. Using split-bands to guard against unknown foreground complications. (20 GHz channel is on LAT to avoid huge beams)<br />
* Calculate detector NETs for South Pole and Chile. NETs are only used to rescale BICEP/Keck achieved performance -- no ab initio sensitivity calculation.<br />
* Forecast assumes sky model with dust and synchrotron. Foregrounds are allowed to decorrelate -- Fisher calculation assumes 3% dust decorrelation between 217 and 353 GHz.<br />
* Choose distribution of effort across nine frequencies plus delensing (10 channels) to minimize sigma(r). <br />
* Data challenge maps use forecasted noise levels but consider many different foreground models. Validates forecast and also determines bias due to different foreground models.<br />
* Analyze data challenge maps with two pipelines: ILC and parametric likelihood foreground cleaning.<br />
* For DSR, converted optimized distribution into discrete instrument configurations in consultation with SAT and detectors groups. Settled on "configuration 5" -> reference design.<br />
* Using detailed sky coverage maps for Chile (deep and shallow) and Pole (deep or wide). Still rescaling from BICEP/Keck noise, but accounting for change in depth and bandpower degrees of freedom. Also applied a foreground mask, which eliminates some of the Chile coverage. Optionally apply foreground penalty -- assume that we can clean down to 1% of foreground, residual acts as bias.<br />
** End up with variation in sigma(r) as a function of number of SATs in Chile vs Pole. Results are different for r=0 vs r=0.003.<br />
* Lloyd: We don't currently have optimal amount of delensing throughput. Want to know what delensing throughput is needed to hit measurement requirements. See Marius' figure from DSR but need to know what A_L level is threshold.<br />
<br />
=== Sherwin: SO BB pipeline / delensing ===<br />
<br />
* SO is very different limit from S4 -- more noise and more sky, so delensing is less important. SO sigma(r) increases by factor of 2 without delensing.<br />
* Using linearized delensing B-mode template constructed on curved sky. Using Wiener filter to downweight noisy regions, but this isn't much better than just masking. Lensing template treated as virtual frequency band.<br />
* SO in intermediate regime where delensing is needed, but noise isn't quite good enough for internal delensing. Also using LSS (CIB, galaxies) as lensing tracer. Multi-tracer delensing gives significant improvement over CIB or CMB internal alone. Think that they will get to ~70% delensing once LSST data is available.<br />
* Running this in a pipeline. Sims include lensing and LSS.<br />
* Think that LSS calibration will be ok because can do it via cross-spectra with noisy CMB lensing map. Worried about bias due to Galactic dust in CIB maps, but ran some sims and it looks ok.<br />
* Is multi-tracer delensing useful as cross-check for CMB-S4? Very complicated, but could be helpful for wide survey. Important to marginalize over A_lens because lensing residual might be uncertain.<br />
<br />
=== Errard: SO BB + delensing forecasts ===<br />
<br />
* Three different analysis pipelines: power-spectrum based, parametric map-based, and blind ILC. Now working to validate full pipelines on realistic sims.<br />
* Large sky fraction for low-ell survey: 10-20%. Hit regions with higher foregrounds and have to worry about spatial variations of foregrounds.<br />
* Power-spectrum based pipeline: use auto and cross-spectra, model foregrounds, marginalize with Gaussian likelihood. Hard to account for spatially-varying foregrounds. <br />
* Map-based cleaning pipeline: xForecast. Approximate full map likelihood by averaging over CMB and noise fluctuations. Validated against full map-based likelihood (BFoRe) and saw good agreement.<br />
* Analysis of simulated maps produces similar results for all pipelines. Tried some more complicated foreground models.<br />
* Delensing: for power-spectrum-based pipeline, delensing template is a virtual frequency channel. For map-based pipeline, subtract delensing map from foreground-cleaned CMB map.<br />
* We should run these pipelines on CMB-S4 sims and vice versa. SO sims are at NERSC and publicly available.<br />
<br />
=== Pryke: PGW map-based sims ===<br />
<br />
* Most recent set is experiment definition 04 with ten different foreground models. Not up-to-date with DSR experiment design.<br />
* Hope that foreground models span reality, but no guarantee of this.<br />
** Three PySM models<br />
** Tuhin Ghosh model<br />
** Highly-decorrelated dust model, designed to break things (and it does!)<br />
** Flauger / Hensley MHD-based model<br />
** Amplitude-modulated Gaussian, based on Planck<br />
** MKD multilayer model (Delabrouille): SED deviates from greybody even in small pixels -- produces strong bias in analysis (but also fails goodness-of-fit)<br />
** Vansyngel model: extends non-Gaussian structure to small scales<br />
* Map-based sims validate forecast but also allow measurement of bias due to foreground model.<br />
* Recipe to scale noise from achieved performance to map-based sims: <br />
*# Use ratios of ideal NETs to scale from achieved performance to S4 forecast<br />
*# Generate full sky realizations of noise (with tweak needed to recover N_ell)<br />
*# Divide by sqrt of relative hits map. Raphael notes that this causes small bias in results because of mode coupling.<br />
* In addition to BK achieved performance, we have new POLARBEAR results with N_ell and hit pattern.<br />
* Going to make 06 sets of sims using DSR experiment configuration and hits maps.<br />
** Who takes this over when Clem goes to Pole? Caterina volunteers (maybe Victor or Colin too)<br />
* What about data challenge maps from Data Management group?<br />
** We should be ready to analyze those, but keep going on our own sim program.<br />
** Need to talk to Data Management people to make sure that they use good inputs for the sims, especially noise and sky model.<br />
<br />
=== Other discussion ===<br />
<br />
* More / better foreground models: will be discussed in next parallel session<br />
* Instrumental systematics:<br />
** Huge task, but broader responsibility than just this group<br />
** Need to prioritize which systematics are most critical. Can we produce a prioritized list?<br />
** What about just specifying allowable "additive systematics" (which we have already done)? "Measurement requirement" is a spec on additive contamination in the map.<br />
** SO is worried about ground pickup. This is main POLARBEAR systematic for low-ell BB.<br />
* Mukherjee: bias from patchy reionization could be equivalent to 3e-4. Can we add this to simulations?<br />
* Is telecon time still ok? It should work for Europe. Not planning to change. Next telecon will be October 28.</div>Cbischoffhttp://www.cmb-s4.org/wiki/index.php?title=UCSD-2019:_Analysis/Pipeline_Working_Group:_Low-ell_BB&diff=10125UCSD-2019: Analysis/Pipeline Working Group: Low-ell BB2019-10-18T22:30:01Z<p>Cbischoff: /* Notes */</p>
<hr />
<div>[https://cmb-s4.org/wiki/index.php/UCSD-2019:_Cosmology_with_CMB-S4#Agenda Link back to agenda]<br />
<br />
== Charge ==<br />
<br />
# Identify key decisions that must be made (and justified) prior to CD-1,<br />
# Make progress on (or actually make) those decisions, <br />
# Lay out a timeline and process for making each decision, consistent with the post-decision work and internal reviews that will be needed to complete preparations for CD-1,<br />
# Ensure that those timelines and processes are understood and supported by the collaboration, and that we (together) believe we can follow them.<br />
<br />
=== Key Issues ===<br />
<br />
* How do we optimize detector allocation across frequency in the face of uncertainty about foreground properties, for both the SATs and the delensing LAT? <br />
* What are the advantages of split bands? How does performance compare to non-split bands?<br />
* Do we need a 20 GHz channel on delensing LAT (for SAT science)<br />
* How well will de-lensing work in practice? <br />
* What are the necessary analysis tools to answer these questions?<br />
<br />
=== What is CD-1? ===<br />
Blatantly copied from [[UCSD-2019: Analysis/Pipeline Working Group: Maps to C_ell | Analysis/Pipeline Working Group: Maps to C_ell]]:<br />
<br />
Background/clarifying questions:<br />
<br />
* What does “by CD-1” mean, and what are the implications for when tools need to be in place and working?<br />
** According to APC white paper (https://arxiv.org/abs/1908.01062), CD-1 is in Q3 of FY2021 (so June 2021?).<br />
*** But according to project office, "Plan [must be] finalized by start of 2020 for delivering...CD-1"<br />
** Working backward from there, any tool that could reasonably influence a CD-1 decision needs to be in place and working by ... ?<br />
** Give an example timeline for an example decision?<br />
<br />
== Agenda ==<br />
<br />
<br />
# Introduction by everyone in the room: who? where? what aspects of low-ell BB interest you? 5 minutes<br />
# Recap of the plan for this session/CD-1 goals [https://docs.google.com/presentation/d/1Mg1LAUMPJQuLv_Qlk0rXA51KijHwe9BYMAZaLfziE4Y/edit?usp=sharing slides][Wu], 3 minutes<br />
# [https://cmb-s4.org/wiki/images/UCSD_PGW_lowellBB_vbuza.pdf Review of Fisher based S4 forecasting thus far leading to DSR appendix A] [Ben/Victor/Raphael], 15 minutes<br />
# Review of Map based S4 forecasting thus far and ideas for next steps [https://docs.google.com/presentation/d/13WQ7t6cyAfchYjKEGw3iuR1U_8QxEC7pJAHmNUmqjXQ Clem], 10 minutes<br />
# Review of forecasting and simulations for Simons Observatory inflation science [Alonso / Errard / Sherwin], [https://docs.google.com/presentation/d/12m5qjX8jRa1nFZBwdAeFUOQY3CsW43LnMIubRAgG5OQ/edit?usp=sharing slides] [https://drive.google.com/file/d/1XmSwtMbtV0yuqwBngwM-f7IAfgQp6UAB/view?usp=sharing delensing slides] 30 minutes<br />
# Plans for working group [all], ~60 minutes<br />
## Forecasting<br />
##* Quantitative comparison of SO and CMB-S4 DSR forecasts<br />
##* Optimization of delensing effort: update for DSR sensitivity, motivation for frequency coverage, feedback from real delensing efforts<br />
## Data Challenge simulations<br />
##* More / better foreground models<br />
##* Instrumental systematics<br />
##* Other map non-idealities, i.e. filtering / mode loss<br />
##* Coordination with technical groups on instrument configuration, etc<br />
##* What else needs to be demonstrated for CD1?<br />
##* Bottlenecks for sim production<br />
## Analysis of Data Challenges<br />
##* Who plans to participate? How do we get more participation?<br />
##* Delensing<br />
## Specific Data Challenge plan / timeline<br />
##* Experiment config 06: DSR configuration, in progress<br />
##* Update / reoptimization of delensing survey?<br />
##* Inclusion of instrumental systematics -- which ones? how to include?<br />
##* Data Challenges coming out of Data Management group<br />
<br />
== Remote attendance ==<br />
<br />
Join Zoom Meeting<br />
https://zoom.us/j/340796462?pwd=S1o3Q3NQUlFOWkVVUXVrV1laK0JrQT09<br />
<br />
*Meeting ID: 340 796 462<br />
*Password: 654876<br />
<br />
*One tap mobile<br />
*+14086380968,,340796462# US (San Jose)<br />
*+16465588656,,340796462# US (New York)<br />
<br />
*Dial by your location<br />
* +1 408 638 0968 US (San Jose)<br />
* +1 646 558 8656 US (New York)<br />
*Meeting ID: 340 796 462<br />
*Find your local number: https://zoom.us/u/aeGN6VEA3T<br />
<br />
== Notes ==<br />
<br />
=== Buza / Racine: CMB-S4 PGW Forecasting ===<br />
<br />
* Forecasting loop: achieved performance used to forecast CMB-S4 instrument -> generate map-based sims with sky model -> analyze to determine sigma(r) and compare to forecast<br />
* 9 bands spanning 4 atmospheric windows. Using split-bands to guard against unknown foreground complications. (20 GHz channel is on LAT to avoid huge beams)<br />
* Calculate detector NETs for South Pole and Chile. NETs are only used to rescale BICEP/Keck achieved performance -- no ab initio sensitivity calculation.<br />
* Forecast assumes sky model with dust and synchrotron. Foregrounds are allowed to decorrelate -- Fisher calculation assumes 3% dust decorrelation between 217 and 353 GHz.<br />
* Choose distribution of effort across nine frequencies plus delensing (10 channels) to minimize sigma(r). <br />
* Data challenge maps use forecasted noise levels but consider many different foreground models. Validates forecast and also determines bias due to different foreground models.<br />
* Analyze data challenge maps with two pipelines: ILC and parametric likelihood foreground cleaning.<br />
* For DSR, converted optimized distribution into discrete instrument configurations in consultation with SAT and detectors groups. Settled on "configuration 5" -> reference design.<br />
* Using detailed sky coverage maps for Chile (deep and shallow) and Pole (deep or wide). Still rescaling from BICEP/Keck noise, but accounting for change in depth and bandpower degrees of freedom. Also applied a foreground mask, which eliminates some of the Chile coverage. Optionally apply foreground penalty -- assume that we can clean down to 1% of foreground, residual acts as bias.<br />
** End up with variation in sigma(r) as a function of number of SATs in Chile vs Pole. Results are different for r=0 vs r=0.003.<br />
* Lloyd: We don't currently have optimal amount of delensing throughput. Want to know what delensing throughput is needed to hit measurement requirements. See Marius' figure from DSR but need to know what A_L level is threshold.<br />
<br />
=== Sherwin: SO BB pipeline / delensing ===<br />
<br />
* SO is very different limit from S4 -- more noise and more sky, so delensing is less important. SO sigma(r) increases by factor of 2 without delensing.<br />
* Using linearized delensing B-mode template constructed on curved sky. Using Wiener filter to downweight noisy regions, but this isn't much better than just masking. Lensing template treated as virtual frequency band.<br />
* SO in intermediate regime where delensing is needed, but noise isn't quite good enough for internal delensing. Also using LSS (CIB, galaxies) as lensing tracer. Multi-tracer delensing gives significant improvement over CIB or CMB internal alone. Think that they will get to ~70% delensing once LSST data is available.<br />
* Running this in a pipeline. Sims include lensing and LSS.<br />
* Think that LSS calibration will be ok because can do it via cross-spectra with noisy CMB lensing map. Worried about bias due to Galactic dust in CIB maps, but ran some sims and it looks ok.<br />
* Is multi-tracer delensing useful as cross-check for CMB-S4? Very complicated, but could be helpful for wide survey. Important to marginalize over A_lens because lensing residual might be uncertain.<br />
<br />
=== Errard: SO BB + delensing forecasts ===<br />
<br />
* Three different analysis pipelines: power-spectrum based, parametric map-based, and blind ILC. Now working to validate full pipelines on realistic sims.<br />
* Large sky fraction for low-ell survey: 10-20%. Hit regions with higher foregrounds and have to worry about spatial variations of foregrounds.<br />
* Power-spectrum based pipeline: use auto and cross-spectra, model foregrounds, marginalize with Gaussian likelihood. Hard to account for spatially-varying foregrounds. <br />
* Map-based cleaning pipeline: xForecast. Approximate full map likelihood by averaging over CMB and noise fluctuations. Validated against full map-based likelihood (BFoRe) and saw good agreement.<br />
* Analysis of simulated maps produces similar results for all pipelines. Tried some more complicated foreground models.<br />
* Delensing: for power-spectrum-based pipeline, delensing template is a virtual frequency channel. For map-based pipeline, subtract delensing map from foreground-cleaned CMB map.<br />
* We should run these pipelines on CMB-S4 sims and vice versa. SO sims are at NERSC and publicly available.<br />
<br />
=== Pryke: PGW map-based sims ===<br />
<br />
* Most recent set is experiment definition 04 with ten different foreground models. Not up-to-date with DSR experiment design.<br />
* Hope that foreground models span reality, but no guarantee of this.<br />
** Three PySM models<br />
** Tuhin Ghosh model<br />
** Highly-decorrelated dust model, designed to break things (and it does!)<br />
** Flauger / Hensley MHD-based model<br />
** Amplitude-modulated Gaussian, based on Planck<br />
** MKD multilayer model (Delabrouille): SED deviates from greybody even in small pixels -- produces strong bias in analysis (but also fails goodness-of-fit)<br />
** Vansyngel model: extends non-Gaussian structure to small scales<br />
* Map-based sims validate forecast but also allow measurement of bias due to foreground model.<br />
* Recipe to scale noise from achieved performance to map-based sims: <br />
*# Use ratios of ideal NETs to scale from achieved performance to S4 forecast<br />
*# Generate full sky realizations of noise (with tweak needed to recover N_ell)<br />
*# Divide by sqrt of relative hits map. Raphael notes that this causes small bias in results because of mode coupling.<br />
* In addition to BK achieved performance, we have new POLARBEAR results with N_ell and hit pattern.<br />
* Going to make 06 sets of sims using DSR experiment configuration and hits maps.<br />
** Who takes this over when Clem goes to Pole? Caterina volunteers (maybe Victor or Colin too)<br />
* What about data challenge maps from Data Management group?<br />
** We should be ready to analyze those, but keep going on our own sim program.<br />
** Need to talk to Data Management people to make sure that they use good inputs for the sims, especially noise and sky model.</div>Cbischoffhttp://www.cmb-s4.org/wiki/index.php?title=UCSD-2019:_Analysis/Pipeline_Working_Group:_Low-ell_BB&diff=10110UCSD-2019: Analysis/Pipeline Working Group: Low-ell BB2019-10-18T21:46:08Z<p>Cbischoff: /* Notes */</p>
<hr />
<div>[https://cmb-s4.org/wiki/index.php/UCSD-2019:_Cosmology_with_CMB-S4#Agenda Link back to agenda]<br />
<br />
== Charge ==<br />
<br />
# Identify key decisions that must be made (and justified) prior to CD-1,<br />
# Make progress on (or actually make) those decisions, <br />
# Lay out a timeline and process for making each decision, consistent with the post-decision work and internal reviews that will be needed to complete preparations for CD-1,<br />
# Ensure that those timelines and processes are understood and supported by the collaboration, and that we (together) believe we can follow them.<br />
<br />
=== Key Issues ===<br />
<br />
* How do we optimize detector allocation across frequency in the face of uncertainty about foreground properties, for both the SATs and the delensing LAT? <br />
* What are the advantages of split bands? How does performance compare to non-split bands?<br />
* Do we need a 20 GHz channel on delensing LAT (for SAT science)<br />
* How well will de-lensing work in practice? <br />
* What are the necessary analysis tools to answer these questions?<br />
<br />
=== What is CD-1? ===<br />
Blatantly copied from [[UCSD-2019: Analysis/Pipeline Working Group: Maps to C_ell | Analysis/Pipeline Working Group: Maps to C_ell]]:<br />
<br />
Background/clarifying questions:<br />
<br />
* What does “by CD-1” mean, and what are the implications for when tools need to be in place and working?<br />
** According to APC white paper (https://arxiv.org/abs/1908.01062), CD-1 is in Q3 of FY2021 (so June 2021?).<br />
*** But according to project office, "Plan [must be] finalized by start of 2020 for delivering...CD-1"<br />
** Working backward from there, any tool that could reasonably influence a CD-1 decision needs to be in place and working by ... ?<br />
** Give an example timeline for an example decision?<br />
<br />
== Agenda ==<br />
<br />
<br />
# Introduction by everyone in the room: who? where? what aspects of low-ell BB interest you? 5 minutes<br />
# Recap of the plan for this session/CD-1 goals [https://docs.google.com/presentation/d/1Mg1LAUMPJQuLv_Qlk0rXA51KijHwe9BYMAZaLfziE4Y/edit?usp=sharing slides][Wu], 3 minutes<br />
# [https://cmb-s4.org/wiki/images/UCSD_PGW_lowellBB_vbuza.pdf Review of Fisher based S4 forecasting thus far leading to DSR appendix A] [Ben/Victor/Raphael], 15 minutes<br />
# Review of Map based S4 forecasting thus far and ideas for next steps [https://docs.google.com/presentation/d/13WQ7t6cyAfchYjKEGw3iuR1U_8QxEC7pJAHmNUmqjXQ Clem], 10 minutes<br />
# Review of forecasting and simulations for Simons Observatory inflation science [Alonso / Errard / Sherwin], [https://docs.google.com/presentation/d/12m5qjX8jRa1nFZBwdAeFUOQY3CsW43LnMIubRAgG5OQ/edit?usp=sharing slides] [https://drive.google.com/file/d/1XmSwtMbtV0yuqwBngwM-f7IAfgQp6UAB/view?usp=sharing delensing slides] 30 minutes<br />
# Plans for working group [all], ~60 minutes<br />
## Forecasting<br />
##* Quantitative comparison of SO and CMB-S4 DSR forecasts<br />
##* Optimization of delensing effort: update for DSR sensitivity, motivation for frequency coverage, feedback from real delensing efforts<br />
## Data Challenge simulations<br />
##* More / better foreground models<br />
##* Instrumental systematics<br />
##* Other map non-idealities, i.e. filtering / mode loss<br />
##* Coordination with technical groups on instrument configuration, etc<br />
##* What else needs to be demonstrated for CD1?<br />
##* Bottlenecks for sim production<br />
## Analysis of Data Challenges<br />
##* Who plans to participate? How do we get more participation?<br />
##* Delensing<br />
## Specific Data Challenge plan / timeline<br />
##* Experiment config 06: DSR configuration, in progress<br />
##* Update / reoptimization of delensing survey?<br />
##* Inclusion of instrumental systematics -- which ones? how to include?<br />
##* Data Challenges coming out of Data Management group<br />
<br />
== Remote attendance ==<br />
<br />
Join Zoom Meeting<br />
https://zoom.us/j/340796462?pwd=S1o3Q3NQUlFOWkVVUXVrV1laK0JrQT09<br />
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*Meeting ID: 340 796 462<br />
*Password: 654876<br />
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*Meeting ID: 340 796 462<br />
*Find your local number: https://zoom.us/u/aeGN6VEA3T<br />
<br />
== Notes ==<br />
<br />
=== Buza / Racine: CMB-S4 PGW Forecasting ===<br />
<br />
* Forecasting loop: achieved performance used to forecast CMB-S4 instrument -> generate map-based sims with sky model -> analyze to determine sigma(r) and compare to forecast<br />
* 9 bands spanning 4 atmospheric windows. Using split-bands to guard against unknown foreground complications. (20 GHz channel is on LAT to avoid huge beams)<br />
* Calculate detector NETs for South Pole and Chile. NETs are only used to rescale BICEP/Keck achieved performance -- no ab initio sensitivity calculation.<br />
* Forecast assumes sky model with dust and synchrotron. Foregrounds are allowed to decorrelate -- Fisher calculation assumes 3% dust decorrelation between 217 and 353 GHz.<br />
* Choose distribution of effort across nine frequencies plus delensing (10 channels) to minimize sigma(r). <br />
* Data challenge maps use forecasted noise levels but consider many different foreground models. Validates forecast and also determines bias due to different foreground models.<br />
* Analyze data challenge maps with two pipelines: ILC and parametric likelihood foreground cleaning.<br />
* For DSR, converted optimized distribution into discrete instrument configurations in consultation with SAT and detectors groups. Settled on "configuration 5" -> reference design.<br />
* Using detailed sky coverage maps for Chile (deep and shallow) and Pole (deep or wide). Still rescaling from BICEP/Keck noise, but accounting for change in depth and bandpower degrees of freedom. Also applied a foreground mask, which eliminates some of the Chile coverage. Optionally apply foreground penalty -- assume that we can clean down to 1% of foreground, residual acts as bias.<br />
** End up with variation in sigma(r) as a function of number of SATs in Chile vs Pole. Results are different for r=0 vs r=0.003.<br />
* Lloyd: We don't currently have optimal amount of delensing throughput. Want to know what delensing throughput is needed to hit measurement requirements. See Marius' figure from DSR but need to know what A_L level is threshold.<br />
<br />
=== Sherwin: SO BB pipeline / delensing ===<br />
<br />
* SO is very different limit from S4 -- more noise and more sky, so delensing is less important. SO sigma(r) increases by factor of 2 without delensing.<br />
* Using linearized delensing B-mode template constructed on curved sky. Using Wiener filter to downweight noisy regions, but this isn't much better than just masking. Lensing template treated as virtual frequency band.<br />
* SO in intermediate regime where delensing is needed, but noise isn't quite good enough for internal delensing. Also using LSS (CIB, galaxies) as lensing tracer. Multi-tracer delensing gives significant improvement over CIB or CMB internal alone. Think that they will get to ~70% delensing once LSST data is available.<br />
* Running this in a pipeline. Sims include lensing and LSS.<br />
* Think that LSS calibration will be ok because can do it via cross-spectra with noisy CMB lensing map. Worried about bias due to Galactic dust in CIB maps, but ran some sims and it looks ok.<br />
* Is multi-tracer delensing useful as cross-check for CMB-S4? Very complicated, but could be helpful for wide survey. Important to marginalize over A_lens because lensing residual might be uncertain.</div>Cbischoffhttp://www.cmb-s4.org/wiki/index.php?title=UCSD-2019:_Analysis/Pipeline_Working_Group:_Low-ell_BB&diff=9954UCSD-2019: Analysis/Pipeline Working Group: Low-ell BB2019-10-18T15:51:17Z<p>Cbischoff: /* Agenda */</p>
<hr />
<div>[https://cmb-s4.org/wiki/index.php/UCSD-2019:_Cosmology_with_CMB-S4#Agenda Link back to agenda]<br />
<br />
== Charge ==<br />
<br />
# Identify key decisions that must be made (and justified) prior to CD-1,<br />
# Make progress on (or actually make) those decisions, <br />
# Lay out a timeline and process for making each decision, consistent with the post-decision work and internal reviews that will be needed to complete preparations for CD-1,<br />
# Ensure that those timelines and processes are understood and supported by the collaboration, and that we (together) believe we can follow them.<br />
<br />
=== Key Issues ===<br />
<br />
* How do we optimize detector allocation across frequency in the face of uncertainty about foreground properties, for both the SATs and the delensing LAT? <br />
* What are the advantages of split bands? How does performance compare to non-split bands?<br />
* Do we need a 20 GHz channel on delensing LAT (for SAT science)<br />
* How well will de-lensing work in practice? <br />
* What are the necessary analysis tools to answer these questions?<br />
<br />
=== What is CD-1? ===<br />
Blatantly copied from [[UCSD-2019: Analysis/Pipeline Working Group: Maps to C_ell | Analysis/Pipeline Working Group: Maps to C_ell]]:<br />
<br />
Background/clarifying questions:<br />
<br />
* What does “by CD-1” mean, and what are the implications for when tools need to be in place and working?<br />
** According to APC white paper (https://arxiv.org/abs/1908.01062), CD-1 is in Q3 of FY2021 (so June 2021?).<br />
*** But according to project office, "Plan [must be] finalized by start of 2020 for delivering...CD-1"<br />
** Working backward from there, any tool that could reasonably influence a CD-1 decision needs to be in place and working by ... ?<br />
** Give an example timeline for an example decision?<br />
<br />
== Agenda ==<br />
<br />
<br />
# Introduction by everyone in the room: who? where? what aspects of low-ell BB interest you? 5 minutes<br />
# Recap of the plan for this session/CD-1 goals [https://docs.google.com/presentation/d/1Mg1LAUMPJQuLv_Qlk0rXA51KijHwe9BYMAZaLfziE4Y/edit?usp=sharing slides][Wu], 3 minutes<br />
# Review of Fisher based S4 forecasting thus far leading to DSR appendix A [Ben/Victor/Raphael], 15 minutes<br />
# Review of Map based S4 forecasting thus far and ideas for next steps [https://docs.google.com/presentation/d/13WQ7t6cyAfchYjKEGw3iuR1U_8QxEC7pJAHmNUmqjXQ Clem], 10 minutes<br />
# Review of forecasting and simulations for Simons Observatory inflation science [Alonso / Errard / Sherwin], [http://dummylink slides] 30 minutes<br />
# Plans for working group [all], ~60 minutes<br />
## Forecasting<br />
##* Quantitative comparison of SO and CMB-S4 DSR forecasts<br />
##* Optimization of delensing effort: update for DSR sensitivity, motivation for frequency coverage, feedback from real delensing efforts<br />
## Data Challenge simulations<br />
##* More / better foreground models<br />
##* Instrumental systematics<br />
##* Other map non-idealities, i.e. filtering / mode loss<br />
##* Coordination with technical groups on instrument configuration, etc<br />
##* What else needs to be demonstrated for CD1?<br />
##* Bottlenecks for sim production<br />
## Analysis of Data Challenges<br />
##* Who plans to participate? How do we get more participation?<br />
##* Delensing<br />
## Specific Data Challenge plan / timeline<br />
##* Experiment config 06: DSR configuration, in progress<br />
##* Update / reoptimization of delensing survey?<br />
##* Inclusion of instrumental systematics -- which ones? how to include?<br />
##* Data Challenges coming out of Data Management group<br />
<br />
== Remote attendance ==<br />
<br />
[https://ucsd.zoom.us/j/739724358 Zoom link]<br />
<br />
<br />
== Notes ==</div>Cbischoffhttp://www.cmb-s4.org/wiki/index.php?title=UCSD-2019:_Analysis/Pipeline_Working_Group:_Low-ell_BB&diff=9935UCSD-2019: Analysis/Pipeline Working Group: Low-ell BB2019-10-18T06:02:43Z<p>Cbischoff: /* Agenda */</p>
<hr />
<div>[https://cmb-s4.org/wiki/index.php/UCSD-2019:_Cosmology_with_CMB-S4#Agenda Link back to agenda]<br />
<br />
== Charge ==<br />
<br />
# Identify key decisions that must be made (and justified) prior to CD-1,<br />
# Make progress on (or actually make) those decisions, <br />
# Lay out a timeline and process for making each decision, consistent with the post-decision work and internal reviews that will be needed to complete preparations for CD-1,<br />
# Ensure that those timelines and processes are understood and supported by the collaboration, and that we (together) believe we can follow them.<br />
<br />
=== Key Issues ===<br />
<br />
* How do we optimize detector allocation across frequency in the face of uncertainty about foreground properties, for both the SATs and the delensing LAT? <br />
* What are the advantages of split bands? How does performance compare to non-split bands?<br />
* Do we need a 20 GHz channel on delensing LAT (for SAT science)<br />
* How well will de-lensing work in practice? <br />
* What are the necessary analysis tools to answer these questions?<br />
<br />
=== What is CD-1? ===<br />
Blatantly copied from [[UCSD-2019: Analysis/Pipeline Working Group: Maps to C_ell | Analysis/Pipeline Working Group: Maps to C_ell]]:<br />
<br />
Background/clarifying questions:<br />
<br />
* What does “by CD-1” mean, and what are the implications for when tools need to be in place and working?<br />
** According to APC white paper (https://arxiv.org/abs/1908.01062), CD-1 is in Q3 of FY2021 (so June 2021?).<br />
*** But according to project office, "Plan [must be] finalized by start of 2020 for delivering...CD-1"<br />
** Working backward from there, any tool that could reasonably influence a CD-1 decision needs to be in place and working by ... ?<br />
** Give an example timeline for an example decision?<br />
<br />
== Agenda ==<br />
<br />
<br />
# Introduction by everyone in the room: who? where? what aspects of low-ell BB interest you? 5 minutes<br />
# Recap of the plan for this session/CD-1 goals [Wu], 3 minutes<br />
# Review of Fisher based S4 forecasting thus far leading to DSR appendix A [Ben/Victor/Raphael], 15 minutes<br />
# Review of Map based S4 forecasting thus far and ideas for next steps [https://docs.google.com/presentation/d/13WQ7t6cyAfchYjKEGw3iuR1U_8QxEC7pJAHmNUmqjXQ Clem], 10 minutes<br />
# Review of forecasting and simulations for Simons Observatory inflation science [Alonso / Errard / Sherwin], [http://dummylink slides] 30 minutes<br />
# Plans for working group [all], ~60 minutes<br />
## Forecasting<br />
##* Quantitative comparison of SO and CMB-S4 DSR forecasts<br />
##* Optimization of delensing effort: update for DSR sensitivity, motivation for frequency coverage, feedback from real delensing efforts<br />
## Data Challenge simulations<br />
##* More / better foreground models<br />
##* Instrumental systematics<br />
##* Other map non-idealities, i.e. filtering / mode loss<br />
##* Coordination with technical groups on instrument configuration, etc<br />
##* What else needs to be demonstrated for CD1?<br />
## Analysis of Data Challenges<br />
##* Who plans to participate? How do we get more participation?<br />
##* Delensing<br />
<br />
== Remote attendance ==<br />
<br />
[https://ucsd.zoom.us/j/739724358 Zoom link]<br />
<br />
<br />
== Notes ==</div>Cbischoffhttp://www.cmb-s4.org/wiki/index.php?title=UCSD-2019:_Flowdown:_Science_to_Measurement_Requirements&diff=9907UCSD-2019: Flowdown: Science to Measurement Requirements2019-10-18T00:20:41Z<p>Cbischoff: /* Knox */</p>
<hr />
<div>[https://cmb-s4.org/wiki/index.php/UCSD-2019:_Cosmology_with_CMB-S4#Agenda Link back to agenda]<br />
<br />
== Charge ==<br />
===Charge from SOC===<br />
* Define what simulations, and other forecasting tools, are still needed before CD-1, the schedule and plan for these simulations and other forecasting tools, and when any inputs are needed to achieve a complete connection between science and measurement for CD-1.<br />
* Coordinate carefully with science and analysis working groups to understand the assumptions they are making and inputs they are using.<br />
===Additional tips for making this session maximally useful===<br />
* People listed below are being asked to prepare for this discussion by outlining, as well as they can, their response to the charge, and highlighting the questions they have about completing a response to the charge, and more generally, questions they have that will help them have a productive meeting in their Friday afternoon parallel session.<br />
* List systematic effects and suggest plan for writing down appropriate requirements, or questions that may need communication with the Technical Council and coordination with them.<br />
* Read the Science to Measurement Requirements chapter of the DSR in advance to know current state of our art, if you have not already.<br />
<br />
== Agenda ==<br />
<br />
* Overview of flowdown process: what it is and why we do it [Lawrence] [[File:Lawrence_ucsd_2019.pdf]]<br />
* REview of DSR and prompts for discussion [Knox] [[File:Science2Measurement_Knox.key.pdf]]<br />
* General discussion<br />
* Flow down from low-ell BB [Bischoff and Wu] [https://docs.google.com/presentation/d/164NM-vBg0DvYUgGAtbZ1XgIgBNFFloOTWmcewPEsIGQ/edit?usp=sharing slides]<br />
* Flow down from light relics [Loverde and Reichardt]<br />
* Flow down from galaxy clusters goal [Battaglia] [[File:S4_UCSD_Cluster_Flowdown.pdf]]<br />
* Flow down from GRB goal [Vieira]<br />
<br />
== Remote attendance ==<br />
<br />
[https://ucsd.zoom.us/j/973144732 Zoom link]<br />
<br />
== Notes ==<br />
<br />
=== Lawrence ===<br />
* We need requirements specified so people can build without consulting with each other constantly. Too many people for that consultation to be possible.<br />
* "Good enough" is! "Better" costs more.<br />
* science goals --> measurement reqs --> instrument reqs --> mission reqs, plus feasibility and cost loop back.<br />
* Pryke: we've got foregrounds and we don't know what they are. How do we deal with this fundamental degree of uncertainty?<br />
* Lawrence: I'm in complete agreement with that point. We have to make some allowances for the fact we don't know. One way we do that is to have a substantial margin on science requirements: a factor of two in some cases. <br />
* Ed Wollack: It's not a new problem. <br />
* Clem Pryke: but split bands for conservatism was not judged to be a valid argument. We needed to demonstrate it led to improvements, when we don't know what the foregrounds are like!<br />
<br />
=== Knox ===<br />
* Four science goals that drive design: r, light relics, clusters, GRBs. (Other science goals are not design drivers)<br />
* Leads to two surveys: ultra-deep hybrid resolution and deep/wide high resolution<br />
* Worked example of science to measurement flowdown for deep/wide survey. Science goals lead to sky coverage, beam size, map depth, observing cadence. <br />
** Still need to think more about systematics (esp. beams), elevation minimum, margin for science targets.<br />
** Frequency coverage is based on Colin Hill calculations that optimized several science goals... but none of these were actually "galaxy clusters". Is this good enough, or does it need to be revisited?<br />
** Increasing sigma(Delta Neff) requirement from 0.03 to 0.033 makes measurement much easier. Can we do this (but maybe keep a goal of 0.03)?<br />
** Do we need to connect measurement optimizations to cost models? Otherwise, we always want more angular resolution and deeper maps.<br />
* Discussion of beam systematics and the need to simulate them: <br />
** For Neff science goal, planet measurements will measure necessary beam parameters at high significance... so long as they don't vary frequently<br />
** For r / delensing, beam systematics (like far sidelobes) will be important. Still have a problem of how much to believe physical optics models, ground models, etc.<br />
* Example DESI CD-1 requirements document -- Only 19 pages, all flows down from BAO science goal. Sample variance pushes to large sky area, setting errors on D(z) and H(z). This is posted on the wiki (link??)<br />
** Can we get similar document for LSST? [https://arxiv.org/abs/1809.01669 LSST DESC science requirements document on arXiv], [https://docushare.lsstcorp.org/docushare/dsweb/Get/LPM-17 LSST System Science Requirements Document]<br />
* Supposed to have draft baseline requirements document by end of 2020. Lots of work needed by June 2020!</div>Cbischoffhttp://www.cmb-s4.org/wiki/index.php?title=UCSD-2019:_Flowdown:_Science_to_Measurement_Requirements&diff=9906UCSD-2019: Flowdown: Science to Measurement Requirements2019-10-18T00:20:14Z<p>Cbischoff: /* Notes */</p>
<hr />
<div>[https://cmb-s4.org/wiki/index.php/UCSD-2019:_Cosmology_with_CMB-S4#Agenda Link back to agenda]<br />
<br />
== Charge ==<br />
===Charge from SOC===<br />
* Define what simulations, and other forecasting tools, are still needed before CD-1, the schedule and plan for these simulations and other forecasting tools, and when any inputs are needed to achieve a complete connection between science and measurement for CD-1.<br />
* Coordinate carefully with science and analysis working groups to understand the assumptions they are making and inputs they are using.<br />
===Additional tips for making this session maximally useful===<br />
* People listed below are being asked to prepare for this discussion by outlining, as well as they can, their response to the charge, and highlighting the questions they have about completing a response to the charge, and more generally, questions they have that will help them have a productive meeting in their Friday afternoon parallel session.<br />
* List systematic effects and suggest plan for writing down appropriate requirements, or questions that may need communication with the Technical Council and coordination with them.<br />
* Read the Science to Measurement Requirements chapter of the DSR in advance to know current state of our art, if you have not already.<br />
<br />
== Agenda ==<br />
<br />
* Overview of flowdown process: what it is and why we do it [Lawrence] [[File:Lawrence_ucsd_2019.pdf]]<br />
* REview of DSR and prompts for discussion [Knox] [[File:Science2Measurement_Knox.key.pdf]]<br />
* General discussion<br />
* Flow down from low-ell BB [Bischoff and Wu] [https://docs.google.com/presentation/d/164NM-vBg0DvYUgGAtbZ1XgIgBNFFloOTWmcewPEsIGQ/edit?usp=sharing slides]<br />
* Flow down from light relics [Loverde and Reichardt]<br />
* Flow down from galaxy clusters goal [Battaglia] [[File:S4_UCSD_Cluster_Flowdown.pdf]]<br />
* Flow down from GRB goal [Vieira]<br />
<br />
== Remote attendance ==<br />
<br />
[https://ucsd.zoom.us/j/973144732 Zoom link]<br />
<br />
== Notes ==<br />
<br />
=== Lawrence ===<br />
* We need requirements specified so people can build without consulting with each other constantly. Too many people for that consultation to be possible.<br />
* "Good enough" is! "Better" costs more.<br />
* science goals --> measurement reqs --> instrument reqs --> mission reqs, plus feasibility and cost loop back.<br />
* Pryke: we've got foregrounds and we don't know what they are. How do we deal with this fundamental degree of uncertainty?<br />
* Lawrence: I'm in complete agreement with that point. We have to make some allowances for the fact we don't know. One way we do that is to have a substantial margin on science requirements: a factor of two in some cases. <br />
* Ed Wollack: It's not a new problem. <br />
* Clem Pryke: but split bands for conservatism was not judged to be a valid argument. We needed to demonstrate it led to improvements, when we don't know what the foregrounds are like!<br />
<br />
=== Knox ===<br />
* Four science goals that drive design: r, light relics, clusters, GRBs. (Other science goals are not design drivers)<br />
* Leads to two surveys: ultra-deep hybrid resolution and deep/wide high resolution<br />
* Worked example of science to measurement flowdown for deep/wide survey. Science goals lead to sky coverage, beam size, map depth, observing cadence. <br />
** Still need to think more about systematics (esp. beams), elevation minimum, margin for science targets.<br />
** Frequency coverage is based on Colin Hill calculations that optimized several science goals... but none of these were actually "galaxy clusters". Is this good enough, or does it need to be revisited?<br />
** Increasing sigma(Delta Neff) requirement from 0.03 to 0.033 makes measurement much easier. Can we do this (but maybe keep a goal of 0.03)?<br />
** Do we need to connect measurement optimizations to cost models? Otherwise, we always want more angular resolution and deeper maps.<br />
* Discussion of beam systematics and the need to simulate them: <br />
** For Neff science goal, planet measurements will measure necessary beam parameters at high significance... so long as they don't vary frequently<br />
** For r / delensing, beam systematics (like far sidelobes) will be important. Still have a problem of how much to believe physical optics models, ground models, etc.<br />
* Example DESI CD-1 requirements document -- Only 19 pages, all flows down from BAO science goal. Sample variance pushes to large sky area, setting errors on D(z) and H(z).<br />
** This document is posted on wiki (link???).<br />
** Can we get similar document for LSST? [https://arxiv.org/abs/1809.01669 LSST DESC science requirements document on arXiv], [https://docushare.lsstcorp.org/docushare/dsweb/Get/LPM-17 LSST System Science Requirements Document]<br />
* Supposed to have draft baseline requirements document by end of 2020. Lots of work needed by June 2020!</div>Cbischoffhttp://www.cmb-s4.org/wiki/index.php?title=UCSD-2019:_Flowdown:_Science_to_Measurement_Requirements&diff=9905UCSD-2019: Flowdown: Science to Measurement Requirements2019-10-18T00:18:50Z<p>Cbischoff: </p>
<hr />
<div>[https://cmb-s4.org/wiki/index.php/UCSD-2019:_Cosmology_with_CMB-S4#Agenda Link back to agenda]<br />
<br />
== Charge ==<br />
===Charge from SOC===<br />
* Define what simulations, and other forecasting tools, are still needed before CD-1, the schedule and plan for these simulations and other forecasting tools, and when any inputs are needed to achieve a complete connection between science and measurement for CD-1.<br />
* Coordinate carefully with science and analysis working groups to understand the assumptions they are making and inputs they are using.<br />
===Additional tips for making this session maximally useful===<br />
* People listed below are being asked to prepare for this discussion by outlining, as well as they can, their response to the charge, and highlighting the questions they have about completing a response to the charge, and more generally, questions they have that will help them have a productive meeting in their Friday afternoon parallel session.<br />
* List systematic effects and suggest plan for writing down appropriate requirements, or questions that may need communication with the Technical Council and coordination with them.<br />
* Read the Science to Measurement Requirements chapter of the DSR in advance to know current state of our art, if you have not already.<br />
<br />
== Agenda ==<br />
<br />
* Overview of flowdown process: what it is and why we do it [Lawrence] [[File:Lawrence_ucsd_2019.pdf]]<br />
* REview of DSR and prompts for discussion [Knox] [[File:Science2Measurement_Knox.key.pdf]]<br />
* General discussion<br />
* Flow down from low-ell BB [Bischoff and Wu] [https://docs.google.com/presentation/d/164NM-vBg0DvYUgGAtbZ1XgIgBNFFloOTWmcewPEsIGQ/edit?usp=sharing slides]<br />
* Flow down from light relics [Loverde and Reichardt]<br />
* Flow down from galaxy clusters goal [Battaglia] [[File:S4_UCSD_Cluster_Flowdown.pdf]]<br />
* Flow down from GRB goal [Vieira]<br />
<br />
== Remote attendance ==<br />
<br />
[https://ucsd.zoom.us/j/973144732 Zoom link]<br />
<br />
== Notes ==<br />
<br />
=== Lawrence ===<br />
* We need requirements specified so people can build without consulting with each other constantly. Too many people for that consultation to be possible.<br />
* "Good enough" is! "Better" costs more.<br />
* science goals --> measurement reqs --> instrument reqs --> mission reqs, plus feasibility and cost loop back.<br />
* Pryke: we've got foregrounds and we don't know what they are. How do we deal with this fundamental degree of uncertainty?<br />
* Lawrence: I'm in complete agreement with that point. We have to make some allowances for the fact we don't know. One way we do that is to have a substantial margin on science requirements: a factor of two in some cases. <br />
* Ed Wollack: It's not a new problem. <br />
* Clem Pryke: but split bands for conservatism was not judged to be a valid argument. We needed to demonstrate it led to improvements, when we don't know what the foregrounds are like!<br />
<br />
=== Knox ===<br />
* Four science goals that drive design: r, light relics, clusters, GRBs. (Other science goals are not design drivers)<br />
* Leads to two surveys: ultra-deep hybrid resolution and deep/wide high resolution<br />
* Worked example of science to measurement flowdown for deep/wide survey. Science goals lead to sky coverage, beam size, map depth, observing cadence. <br />
** Still need to think more about systematics (esp. beams), elevation minimum, margin for science targets.<br />
** Frequency coverage is based on Colin Hill calculations that optimized several science goals... but none of these were actually "galaxy clusters". Is this good enough, or does it need to be revisited?<br />
** Increasing sigma(Delta Neff) requirement from 0.03 to 0.033 makes measurement much easier. Can we do this (but maybe keep a goal of 0.03)?<br />
** Do we need to connect measurement optimizations to cost models? Otherwise, we always want more angular resolution and deeper maps.<br />
* Discussion of beam systematics and the need to simulate them: <br />
** For Neff science goal, planet measurements will measure necessary beam parameters at high significance... so long as they don't vary frequently<br />
** For r / delensing, beam systematics (like far sidelobes) will be important. Still have a problem of how much to believe physical optics models, ground models, etc.<br />
* Example DESI CD-1 requirements document -- Only 19 pages, all flows down from BAO science goal. Sample variance pushes to large sky area, setting errors on D(z) and H(z).<br />
** This document is posted on wiki (link???).<br />
** Can we get similar document for LSST? [https://arxiv.org/abs/1809.01669 LSST DESC science requirements document on arXiv]<br />
* Supposed to have draft baseline requirements document by end of 2020. Lots of work needed by June 2020!</div>Cbischoffhttp://www.cmb-s4.org/wiki/index.php?title=UCSD-2019:_Flowdown:_Science_to_Measurement_Requirements&diff=9899UCSD-2019: Flowdown: Science to Measurement Requirements2019-10-18T00:07:35Z<p>Cbischoff: /* Notes */</p>
<hr />
<div>[https://cmb-s4.org/wiki/index.php/UCSD-2019:_Cosmology_with_CMB-S4#Agenda Link back to agenda]<br />
<br />
== Charge ==<br />
===Charge from SOC===<br />
* Define what simulations, and other forecasting tools, are still needed before CD-1, the schedule and plan for these simulations and other forecasting tools, and when any inputs are needed to achieve a complete connection between science and measurement for CD-1.<br />
* Coordinate carefully with science and analysis working groups to understand the assumptions they are making and inputs they are using.<br />
===Additional tips for making this session maximally useful===<br />
* People listed below are being asked to prepare for this discussion by outlining, as well as they can, their response to the charge, and highlighting the questions they have about completing a response to the charge, and more generally, questions they have that will help them have a productive meeting in their Friday afternoon parallel session.<br />
* List systematic effects and suggest plan for writing down appropriate requirements, or questions that may need communication with the Technical Council and coordination with them.<br />
* Read the Science to Measurement Requirements chapter of the DSR in advance to know current state of our art, if you have not already.<br />
<br />
== Agenda ==<br />
<br />
* Overview of flowdown process: what it is and why we do it [Lawrence] [[File:Lawrence_ucsd_2019.pdf]]<br />
* REview of DSR and prompts for discussion [Knox] [[File:Science2Measurement_Knox.key.pdf]]<br />
* General discussion<br />
* Flow down from low-ell BB [Bischoff and Wu] [https://docs.google.com/presentation/d/164NM-vBg0DvYUgGAtbZ1XgIgBNFFloOTWmcewPEsIGQ/edit?usp=sharing slides]<br />
* Flow down from light relics [Loverde and Reichardt]<br />
* Flow down from galaxy clusters goal [Battaglia] [[File:S4_UCSD_Cluster_Flowdown.pdf]]<br />
* Flow down from GRB goal [Vieira]<br />
<br />
== Remote attendance ==<br />
<br />
[https://ucsd.zoom.us/j/973144732 Zoom link]<br />
<br />
== Notes ==<br />
<br />
=== Lawrence ===<br />
* We need requirements specified so people can build without consulting with each other constantly. Too many people for that consultation to be possible.<br />
* "Good enough" is! "Better" costs more.<br />
* science goals --> measurement reqs --> instrument reqs --> mission reqs, plus feasibility and cost loop back.<br />
* Pryke: we've got foregrounds and we don't know what they are. How do we deal with this fundamental degree of uncertainty?<br />
* Lawrence: I'm in complete agreement with that point. We have to make some allowances for the fact we don't know. One way we do that is to have a substantial margin on science requirements: a factor of two in some cases. <br />
* Ed Wollack: It's not a new problem. <br />
* Clem Pryke: but split bands for conservatism was not judged to be a valid argument. We needed to demonstrate it led to improvements, when we don't know what the foregrounds are like!<br />
<br />
=== Knox ===<br />
* Four science goals that drive design: r, light relics, clusters, GRBs. (Other science goals are not design drivers)<br />
* Leads to two surveys: ultra-deep hybrid resolution and deep/wide high resolution<br />
* Worked example of science to measurement flowdown for deep/wide survey. Science goals lead to sky coverage, beam size, map depth, observing cadence. <br />
** Still need to think more about systematics (esp. beams), elevation minimum, margin for science targets.<br />
** Frequency coverage is based on Colin Hill calculations that optimized several science goals... but none of these were actually "galaxy clusters". Is this good enough, or does it need to be revisited?<br />
** Increasing sigma(Delta Neff) requirement from 0.03 to 0.033 makes measurement much easier. Can we do this (but maybe keep a goal of 0.03)?<br />
** Do we need to connect measurement optimizations to cost models? Otherwise, we always want more angular resolution and deeper maps.<br />
* Discussion of beam systematics and the need to simulate them: <br />
** For Neff science goal, planet measurements will measure necessary beam parameters at high significance... so long as they don't vary frequently<br />
** For r / delensing, beam systematics (like far sidelobes) will be important. Still have a problem of how much to believe physical optics models, ground models, etc.<br />
* Example DESI CD-1 requirements document -- Only 19 pages, all flows down from BAO science goal. Sample variance pushes to large sky area, setting errors on D(z) and H(z).<br />
** This document is posted on wiki (link???)</div>Cbischoffhttp://www.cmb-s4.org/wiki/index.php?title=UCSD-2019:_Flowdown:_Science_to_Measurement_Requirements&diff=9898UCSD-2019: Flowdown: Science to Measurement Requirements2019-10-18T00:07:09Z<p>Cbischoff: /* Notes */</p>
<hr />
<div>[https://cmb-s4.org/wiki/index.php/UCSD-2019:_Cosmology_with_CMB-S4#Agenda Link back to agenda]<br />
<br />
== Charge ==<br />
===Charge from SOC===<br />
* Define what simulations, and other forecasting tools, are still needed before CD-1, the schedule and plan for these simulations and other forecasting tools, and when any inputs are needed to achieve a complete connection between science and measurement for CD-1.<br />
* Coordinate carefully with science and analysis working groups to understand the assumptions they are making and inputs they are using.<br />
===Additional tips for making this session maximally useful===<br />
* People listed below are being asked to prepare for this discussion by outlining, as well as they can, their response to the charge, and highlighting the questions they have about completing a response to the charge, and more generally, questions they have that will help them have a productive meeting in their Friday afternoon parallel session.<br />
* List systematic effects and suggest plan for writing down appropriate requirements, or questions that may need communication with the Technical Council and coordination with them.<br />
* Read the Science to Measurement Requirements chapter of the DSR in advance to know current state of our art, if you have not already.<br />
<br />
== Agenda ==<br />
<br />
* Overview of flowdown process: what it is and why we do it [Lawrence] [[File:Lawrence_ucsd_2019.pdf]]<br />
* REview of DSR and prompts for discussion [Knox] [[File:Science2Measurement_Knox.key.pdf]]<br />
* General discussion<br />
* Flow down from low-ell BB [Bischoff and Wu] [https://docs.google.com/presentation/d/164NM-vBg0DvYUgGAtbZ1XgIgBNFFloOTWmcewPEsIGQ/edit?usp=sharing slides]<br />
* Flow down from light relics [Loverde and Reichardt]<br />
* Flow down from galaxy clusters goal [Battaglia] [[File:S4_UCSD_Cluster_Flowdown.pdf]]<br />
* Flow down from GRB goal [Vieira]<br />
<br />
== Remote attendance ==<br />
<br />
[https://ucsd.zoom.us/j/973144732 Zoom link]<br />
<br />
== Notes ==<br />
<br />
* Lawrence<br />
** We need requirements specified so people can build without consulting with each other constantly. Too many people for that consultation to be possible.<br />
** "Good enough" is! "Better" costs more.<br />
** science goals --> measurement reqs --> instrument reqs --> mission reqs, plus feasibility and cost loop back.<br />
** Pryke: we've got foregrounds and we don't know what they are. How do we deal with this fundamental degree of uncertainty?<br />
** Lawrence: I'm in complete agreement with that point. We have to make some allowances for the fact we don't know. One way we do that is to have a substantial margin on science requirements: a factor of two in some cases. <br />
** Ed Wollack: It's not a new problem. <br />
** Clem Pryke: but split bands for conservatism was not judged to be a valid argument. We needed to demonstrate it led to improvements, when we don't know what the foregrounds are like!<br />
<br />
* Knox<br />
** Four science goals that drive design: r, light relics, clusters, GRBs. (Other science goals are not design drivers)<br />
** Leads to two surveys: ultra-deep hybrid resolution and deep/wide high resolution<br />
** Worked example of science to measurement flowdown for deep/wide survey. Science goals lead to sky coverage, beam size, map depth, observing cadence. <br />
*** Still need to think more about systematics (esp. beams), elevation minimum, margin for science targets.<br />
*** Frequency coverage is based on Colin Hill calculations that optimized several science goals... but none of these were actually "galaxy clusters". Is this good enough, or does it need to be revisited?<br />
*** Increasing sigma(Delta Neff) requirement from 0.03 to 0.033 makes measurement much easier. Can we do this (but maybe keep a goal of 0.03)?<br />
*** Do we need to connect measurement optimizations to cost models? Otherwise, we always want more angular resolution and deeper maps.<br />
** Discussion of beam systematics and the need to simulate them: <br />
*** For Neff science goal, planet measurements will measure necessary beam parameters at high significance... so long as they don't vary frequently<br />
*** For r / delensing, beam systematics (like far sidelobes) will be important. Still have a problem of how much to believe physical optics models, ground models, etc.<br />
** Example DESI CD-1 requirements document -- Only 19 pages, all flows down from BAO science goal. Sample variance pushes to large sky area, setting errors on D(z) and H(z).<br />
*** This document is posted on wiki (link???)</div>Cbischoffhttp://www.cmb-s4.org/wiki/index.php?title=UCSD-2019:_Analysis/Pipeline_Working_Group:_Low-ell_BB&diff=9545UCSD-2019: Analysis/Pipeline Working Group: Low-ell BB2019-10-14T22:05:32Z<p>Cbischoff: /* Agenda */</p>
<hr />
<div>[https://cmb-s4.org/wiki/index.php/UCSD-2019:_Cosmology_with_CMB-S4#Agenda Link back to agenda]<br />
<br />
== Charge ==<br />
<br />
# Identify key decisions that must be made (and justified) prior to CD-1,<br />
# Make progress on (or actually make) those decisions, <br />
# Lay out a timeline and process for making each decision, consistent with the post-decision work and internal reviews that will be needed to complete preparations for CD-1,<br />
# Ensure that those timelines and processes are understood and supported by the collaboration, and that we (together) believe we can follow them.<br />
<br />
=== Key Issues ===<br />
<br />
* How do we optimize detector allocation across frequency in the face of uncertainty about foreground properties, for both the SATs and the delensing LAT? <br />
* What are the advantages of split bands? How does performance compare to non-split bands?<br />
* Do we need a 20 GHz channel on delensing LAT (for SAT science)<br />
* How well will de-lensing work in practice? <br />
* What are the necessary analysis tools to answer these questions?<br />
<br />
== Agenda ==<br />
<br />
# Needs for CD1 [Wu], 5 minutes<br />
# Review of forecasting and data challenges for DSR [Pryke], 25 minutes<br />
# Review of forecasting and simulations for Simons Observatory inflation science [Alonso / Errard / Sherwin], 30 minutes<br />
# Plans for working group [all], 60 minutes<br />
## Forecasting<br />
##* Quantitative comparison of SO and CMB-S4 DSR forecasts<br />
##* Feedback loop between forecasting and data challenges<br />
## Data Challenge simulations<br />
##* More / better foreground models<br />
##* Instrumental systematics<br />
##* Other map non-idealities, i.e. filtering / mode loss<br />
##* Coordination with technical groups on instrument configuration, etc<br />
##* What else needs to be demonstrated for CD1?<br />
## Analysis of Data Challenges<br />
##* Who plans to participate? How do we get more participation?<br />
##* Delensing<br />
<br />
== Remote attendance ==<br />
<br />
[https://ucsd.zoom.us/j/739724358 Zoom link]<br />
<br />
<br />
== Notes ==</div>Cbischoffhttp://www.cmb-s4.org/wiki/index.php?title=UCSD-2019:_Committees:_Education_%26_Public_Outreach&diff=9471UCSD-2019: Committees: Education & Public Outreach2019-10-10T19:58:37Z<p>Cbischoff: /* Agenda */</p>
<hr />
<div>[https://cmb-s4.org/wiki/index.php/UCSD-2019:_Cosmology_with_CMB-S4#Agenda Link back to agenda]<br />
<br />
== Charge ==<br />
<br />
# Identify key decisions that must be made (and justified) prior to CD-1,<br />
# Make progress on (or actually make) those decisions, <br />
# Lay out a timeline and process for making each decision, consistent with the post-decision work and internal reviews that will be needed to complete preparations for CD-1,<br />
# Ensure that those timelines and processes are understood and supported by the collaboration, and that we (together) believe we can follow them.<br />
<br />
=== Key Issues ===<br />
<br />
* What is the overarching design of the EPO program?<br />
* What is the recording / reporting structure?<br />
* What EPO plan in Chile would we like to propose and how do we coordinate with local resources?<br />
<br />
== Agenda ==<br />
<br />
== Remote Attendance ==<br />
<br />
[https://ucsd.zoom.us/j/462241746 Zoom link]<br />
<br />
== Notes ==</div>Cbischoffhttp://www.cmb-s4.org/wiki/index.php?title=Education_%26_Public_Outreach_Committee&diff=9400Education & Public Outreach Committee2019-10-08T21:56:32Z<p>Cbischoff: </p>
<hr />
<div>Committee members: Colin Bischoff (chair), Amy Lowitz, Benjamin Saliwanchik, Sara Simon, Chris Stoughton, Peter Timbie and Kasey Wagoner.<br />
<br />
* Mailing list: [https://cmb-s4.org/mailman/listinfo/epoc epoc@cmb-s4.org]<br />
* Telecon notes: [https://docs.google.com/document/d/1uSJnm8nLwACaFM5zcvg1aZjDMBJjxN9xE_f9DTmsFSU/edit# google doc] (contact Colin for edit access)</div>Cbischoffhttp://www.cmb-s4.org/wiki/index.php?title=Education_%26_Public_Outreach_Committee&diff=9399Education & Public Outreach Committee2019-10-08T21:55:12Z<p>Cbischoff: </p>
<hr />
<div>Committee members: Colin Bischoff (chair), Amy Lowitz, Benjamin Saliwanchik, Sara Simon, Chris Stoughton, Peter Timbie and Kasey Wagoner.<br />
<br />
* Mailing list: [https://cmb-s4.org/mailman/listinfo/epoc epoc@cmb-s4.org]<br />
* Telecon notes: [https://docs.google.com/document/d/1uSJnm8nLwACaFM5zcvg1aZjDMBJjxN9xE_f9DTmsFSU/edit# google doc]</div>Cbischoffhttp://www.cmb-s4.org/wiki/index.php?title=UCSD-2019:_Cosmology_with_CMB-S4&diff=9398UCSD-2019: Cosmology with CMB-S42019-10-08T20:55:14Z<p>Cbischoff: /* Friday October 18th */</p>
<hr />
<div>== Workshop overview ==<br />
<br />
The San Diego workshop continues a successful series of meetings bringing together the CMB experimental and theoretical community to plan a coordinated, stage-4 ground-based CMB experiment. <br />
<br />
The meeting will be held at UC San Diego, October 17th-19th 2019, starting first thing Thursday morning and ending Saturday lunchtime.<br />
<br />
== Meeting Info & Registration ==<br />
<br />
[http://cmbs4meeting2019.ucsd.edu/index.html Official Workshop Website: Registration, Participants, Hotels, Logistics].<br />
<br />
== Code of Conduct ==<br />
<br />
During the meeting, each participant should adhere at all times to the [https://regents.universityofcalifornia.edu/governance/policies/1111.html UC Standards of Ethical Conduct]. In case of violations, you can contact [https://cmb-s4.org/wiki/index.php/Main_Page#Ombudspeople the CMB-S4 Ombudspeople], Andrea Zonca or any other member of the Local Organizing Committee, or the [http://ophd.ucsd.edu/ UC San Diego Office for the prevention of harassment & discrimination].<br />
<br />
== Attend remotely ==<br />
<br />
We will use Zoom to broadcast all the plenaries from the auditorium, see connection details below.<br />
For the parallel sessions, each physical room has an assigned Zoom link (email zonca@sdsc.edu if you want your account to be a Host so you have admin powers).<br />
<br />
Join Zoom Meeting<br />
https://ucsd.zoom.us/j/424492016<br />
<br />
Meeting ID: 424 492 016<br />
<br />
<nowiki><br />
One tap mobile<br />
+16699006833,,424492016# US (San Jose)<br />
+16465588656,,424492016# US (New York)<br />
<br />
Dial by your location<br />
+1 669 900 6833 US (San Jose)<br />
+1 646 558 8656 US (New York)<br />
Meeting ID: 424 492 016</nowiki><br />
<br />
Find your local number: https://zoom.us/u/adPue3mkc2<br />
<br />
Join by Skype for Business<br />
https://ucsd.zoom.us/skype/424492016<br />
<br />
== About This Wiki==<br />
<br />
As for previous workshops, we will use this wiki to organize the sessions, to capture the input from them, and to develop next steps. Participants are encouraged to edit the wiki directly, including uploading plots or a few slides.<br />
<br />
Hints for formatting this wiki can be found [https://www.mediawiki.org/wiki/Help:Formatting here]<br />
<br />
----<br />
<br />
== Agenda ==<br />
<br />
Draft agenda below.<br />
<br />
If you would like to contribute to a parallel session, please contact the chairs (in brackets).<br />
<br />
Plenary speakers are asked to upload their talks to the wiki, linked to the title.<br />
<br />
=== Thursday October 17th ===<br />
<br />
08:00 - Coffee<br />
<br />
08:30 - Plenary 1, Welcome & Status Reports - Chair: TBD<br />
* 08:30 - Welcome (Mike Norman)<br />
* 08:35 - Logistics (Andrea Zonca)<br />
* 08:40 - Spokespeople (John Carlstrom)<br />
* 08:50 - Membership Committee (John Ruhl)<br />
* 08:55 - Publication & Speakers Committee (Kevin Huffenberger)<br />
* 09:00 - Governing Board (Nils Halverson)<br />
* 09:10 - Project Office + charting the path to CD-1/3a and NSF PDR (Jim Yeck)<br />
* 09:20 - Agency Representatives (Drew Baden, Vladimir Papitashvili)<br />
<br />
9:30 - Plenary 2, Science Themes - Chair: Lloyd Knox<br />
* 09:30 - Primordial Gravitational Waves + Inflation<br />
* 09:45 - Dark Universe<br />
* 10:00 - Matter Mapping<br />
* 10:15 - Transients<br />
<br />
10:30 - Coffee<br />
<br />
11:00 - Plenary 3, Project L2 Elements - Chair: Gil Gilchriese<br />
* 11:00 - Overview + Charge to L2s (Jim Yeck)<br />
* 11:20 - Combined L2 Presentation<br />
** Detectors<br />
** Readout<br />
** Module Assembly + Testing<br />
** Large Aperture Telescopes<br />
** Small Aperture Telescopes<br />
** Data Acquisition + Control<br />
** Data Management<br />
** Site Infrastructure: Atacama<br />
** Site Infrastructure: South Pole<br />
** Integration & Commissioning<br />
<br />
12:30 - Lunch (catering just outside of the Auditorium)<br />
<br />
13:30 - Parallel 1 <br />
* [[UCSD-2019: Technical Working Group: Detectors | Technical Working Group: Detectors]] (Chang/Irwin/Suzuki)<br />
* [[UCSD-2019: Technical Working Group: LATs | Technical Working Group: LATs]] (Carlstrom/Niemack)<br />
* [[UCSD-2019: Technical Working Group: Data Management | Technical Working Group: Data Management]] (Borrill/Crawford)<br />
* [[UCSD-2019: Science Theme: PGW %26 Inflation | Science Theme: PGW & Inflation]] (Pryke/Flauger)<br />
* [[UCSD-2019: Science Theme: Dark Universe | Science Theme: Dark Universe]] (Gluscevic/Green)<br />
* [[UCSD-2019: Science Theme: Matter Mapping | Science Theme: Matter Mapping]] (Bleem/Hill)<br />
* [[UCSD-2019: Science Theme: Transients | Science Theme: Transients]] (Holder/Whitehorn)<br />
<br />
15:30 - Coffee<br />
<br />
15:45 - Parallel 2<br />
* [[UCSD-2019: Technical Working Group: Readout | Technical Working Group: Readout]] (Ahmed/Bender)<br />
* [[UCSD-2019: Technical Working Group: SATs | Technical Working Group: SATs]] (Kovac/Kusaka)<br />
* [[UCSD-2019: Technical Working Group: DAQ | Technical Working Group: DAQ]] (Newburgh/Whitehorn)<br />
* [[UCSD-2019: Flowdown: Science to Measurement Requirements | Flowdown: Science to Measurement Requirements]] (Knox+Lawrence)<br />
<br />
17:45 - [[UCSD 2019 Fireslides 1 | Fireslides 1]]<br />
<br />
18:00 - Posters/Social, appetizers and drinks offered on the patio outside the Auditorium<br />
<br />
[19:00 - Governing Board]<br />
<br />
=== Friday October 18th ===<br />
<br />
08:00 - Coffee<br />
<br />
08:30 - Plenary 4a, Reports Back From Technical Parallels - Chair: Brenna Flaugher<br />
<br />
10:30 - Coffee<br />
<br />
11:00 - Plenary 4b, Reports Back From Science Parallels - Chair: Gil Holder<br />
<br />
12:30 - Lunch (catering just outside of the Auditorium)<br />
<br />
13:30 - Parallel 3<br />
* [[UCSD-2019: Flowdown: Measurement to Technical Requirements | Flowdown: Measurement to Technical Requirements]] (McMahon+Lawrence)<br />
* [[UCSD-2019: Analysis/Pipeline Working Group: Low-ell BB | Analysis/Pipeline Working Group: Low-ell BB]] (Bischoff/Wu)<br />
* [[UCSD-2019: Analysis/Pipeline Working Group: Maps to C_ell | Analysis/Pipeline Working Group: Maps to C_ell]] (Crawford+)<br />
* [[UCSD-2019: Analysis/Pipeline Working Group: Maps to Other Statistics | Analysis/Pipeline Working Group: Maps to Other Statistics]] (Sherwin+)<br />
* [[UCSD-2019: Analysis/Pipeline Working Group: Sources | Analysis/Pipeline Working Group: Sources]] (Holder+)<br />
<br />
15:30 - Coffee<br />
<br />
15:45 - Parallel 4<br />
* [[UCSD-2019: Technical Working Group: Modules %26 Testing | Technical Working Group: Modules & Testing]] (Benson)<br />
* [[UCSD-2019: Cross-Cut: Site Resource Requirements | Cross-Cut: Site Resource Requirements]] (Arnold/Ruhl)<br />
* [[UCSD-2019: Cross-Cut: Cryo-Optics | Cross-Cut: Cryo-Optics]] (Vieira/Vieregg)<br />
* [[UCSD-2019: Cross-Cut: Sidelobes %26 Shielding including Simulation | Cross-Cut: Sidelobes & Shielding including Simulation]] (Keskitalo/Kovac/Niemack)<br />
* [[UCSD-2019: Cross-Cut: Delensing | Cross-Cut: Delensing]] (van Engelen/Wu)<br />
* [[UCSD-2019: Cross-Cut: Sky Modeling | Cross-Cut: Sky Modeling]] (Alvarez/Hensley)<br />
<br />
17:45 - [[UCSD 2019 Fireslides 2 | Fireslides 2]]<br />
<br />
18:00 - No-Host Dinner (TBC)<br />
<br />
=== Saturday October 19th ===<br />
<br />
08:00 - Coffee<br />
<br />
08:30 - Parallel 5<br />
* [[UCSD-2019: Cross-Cut: Pixel Size/f-Number Optimization | Cross-Cut: Pixel Size/f-Number Optimization]] (Vieregg)<br />
* [[UCSD-2019: Cross-Cut: Readout/DAQ/Control Testing | Cross-Cut: Readout/DAQ/Control Testing]] (Newburgh/Whitehorn)<br />
* [[UCSD-2019: Cross-Cut: Simulations for Technical Requirements | Cross-Cut: Simulations for Technical Requirements]] (Simon)<br />
* [[UCSD-2019: Cross-Cut: Joint Probes %26 Cross-Correlations | Cross-Cut: Joint Probes & Cross-Correlations]] (Ferraro)<br />
* [[UCSD-2019: Committees: Education %26 Public Outreach | Committees: Education & Public Outreach]] (Bischoff)<br />
<br />
09:30 - Parallel 6<br />
* [[UCSD-2019: Cross-Cut: Receiver Interfaces | Cross-Cut: Receiver Interfaces]] (Filippini)<br />
* [[UCSD-2019: Cross-Cut: Validation %26 Calibration | Cross-Cut: Validation & Calibration]] (Anderson/Nagy/Simon)<br />
* [[UCSD-2019: Cross-Cut: Component Separation/Foreground Cleaning | Cross-Cut: Component Separation/Foreground Cleaning]] (Dvorkin)<br />
* [[UCSD-2019: Cross-Cut: Simulations for Measurement Requirements | Cross-Cut: Simulations for Measurement Requirements]] (Zonca)<br />
* [[UCSD-2019: Committees: Education %26 Public Outreach | Committees: Education & Public Outreach]] (Bischoff)<br />
<br />
10:30 - Coffee<br />
<br />
11:00 - Plenary 5, Reports Back From Selected Parallels 3-6 - Chair: <br />
<br />
12:15 - Closeout<br />
<br />
12:30 Workshop Ends (no lunch provided)</div>Cbischoffhttp://www.cmb-s4.org/wiki/index.php?title=UCSD-2019:_Analysis/Pipeline_Working_Group:_Low-ell_BB&diff=9392UCSD-2019: Analysis/Pipeline Working Group: Low-ell BB2019-10-08T16:57:44Z<p>Cbischoff: /* Charge */</p>
<hr />
<div>[https://cmb-s4.org/wiki/index.php/UCSD-2019:_Cosmology_with_CMB-S4#Agenda Link back to agenda]<br />
<br />
== Charge ==<br />
<br />
# Identify key decisions that must be made (and justified) prior to CD-1,<br />
# Make progress on (or actually make) those decisions, <br />
# Lay out a timeline and process for making each decision, consistent with the post-decision work and internal reviews that will be needed to complete preparations for CD-1,<br />
# Ensure that those timelines and processes are understood and supported by the collaboration, and that we (together) believe we can follow them.<br />
<br />
=== Key Issues ===<br />
<br />
* How do we optimize detector allocation across frequency in the face of uncertainty about foreground properties, for both the SATs and the delensing LAT? <br />
* What are the advantages of split bands? How does performance compare to non-split bands?<br />
* Do we need a 20 GHz channel on delensing LAT (for SAT science)<br />
* How well will de-lensing work in practice? <br />
* What are the necessary analysis tools to answer these questions?<br />
<br />
== Agenda ==<br />
<br />
<br />
<br />
== Notes ==</div>Cbischoffhttp://www.cmb-s4.org/wiki/index.php?title=UCSD-2019:_Committees:_Education_%26_Public_Outreach&diff=9379UCSD-2019: Committees: Education & Public Outreach2019-10-08T02:49:06Z<p>Cbischoff: /* Charge */</p>
<hr />
<div>[https://cmb-s4.org/wiki/index.php/UCSD-2019:_Cosmology_with_CMB-S4#Agenda Link back to agenda]<br />
<br />
== Charge ==<br />
<br />
# Identify key decisions that must be made (and justified) prior to CD-1,<br />
# Make progress on (or actually make) those decisions, <br />
# Lay out a timeline and process for making each decision, consistent with the post-decision work and internal reviews that will be needed to complete preparations for CD-1,<br />
# Ensure that those timelines and processes are understood and supported by the collaboration, and that we (together) believe we can follow them.<br />
<br />
=== Key Issues ===<br />
<br />
* What is the overarching design of the EPO program?<br />
* What is the recording / reporting structure?<br />
* What EPO plan in Chile would we like to propose and how do we coordinate with local resources?<br />
<br />
== Agenda ==<br />
<br />
<br />
<br />
== Notes ==</div>Cbischoffhttp://www.cmb-s4.org/wiki/index.php?title=Education_%26_Public_Outreach_Committee&diff=9377Education & Public Outreach Committee2019-10-07T14:03:50Z<p>Cbischoff: </p>
<hr />
<div>Committee members: Colin Bischoff (chair), Amy Lowitz, Benjamin Saliwanchik, Sara Simon, Chris Stoughton, Peter Timbie and Kasey Wagoner.<br />
<br />
Mailing list: [https://cmb-s4.org/mailman/listinfo/epoc epoc@cmb-s4.org]</div>Cbischoffhttp://www.cmb-s4.org/wiki/index.php?title=Simulation_and_Forecasting_Logbook&diff=9259Simulation and Forecasting Logbook2019-09-16T14:14:58Z<p>Cbischoff: /* Logbook Entries (reverse chronological) */</p>
<hr />
<div>This is an index page for logbook-style postings that cover the interconnected topics of sky modeling, simulations, and forecasting for CMB-S4. <br />
<br />
Some guidelines for use:<br />
* '''Postings should include enough context''' so that a reader can jump in and figure out what is going on. It is ''not'' necessary to write an extensive introduction to every posting -- context can be in the form of links to older postings, paper citations, etc.<br />
* Postings should represent a snapshot of work in progress. It's ok to post incomplete results, but recommended that you include notes about what is missing, what you are still planning to work on, etc. <br />
* If you have work that extends or improves an old posting, you should add it as a new posting (that includes links back to the old work as appropriate). Don't update old postings, as they should provide a chronological record of progress.<br />
* On this index page, add a link to your posting with the date, a descriptive posting title, and your full name. This logbook covers a wide range of topics, so titles will be really important to keep it useful. Don't name your posting something like "Forecasting for S4"!<br />
* Links should be added in reverse-chronological order (newest at the top). Your posting can either be written up on another wiki page or it can be a link to some externally hosted webpage (useful if you want to include a javascript plots pager).<br />
<br />
<br />
== Logbook Entries (reverse chronological) ==<br />
<br />
* '''2019 September 16''': [[PureB by Messenger Method]] (Michael Ray, Colin Bischoff)<br />
* '''2019 August 29''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190829_noise_params_DSR/ Noise parameters for the DC5 DSR-like data challenge] (Ben Racine)<br />
* '''2019 June 6''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190607_LATSTM/ LAT CDT-STM Noise Levels] (Victor Buza)<br />
* '''2019 May 19''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190519_about_DSR_AppendixA_plots_and_table/ sigma(r) vs r: plots and tables for the DSR] (Ben Racine and Raphael Flauger)<br />
* '''2019 May 17''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190509_b3_obseff Observing efficiency reality check] (Clem)<br />
* '''2019 May 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190511_sigmar_vs_r_galcuts/ sigma(r) vs r: possible figures for the DSR (v4): Galactic cuts added (In progress)] (Ben Racine and Raphael Flauger)<br />
* '''2019 May 11''': [[Update_on_Fisher_forecasts]] (Raphael)<br />
* '''2019 May 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190507_sigmar_vs_r_combined_hits/ sigma(r) vs r: possible figures for the DSR (v3): More realistic combination and fixed 20GHz] (Ben Racine and Raphael Flauger)<br />
* '''2019 May 6''': [[Update_on_Fisher_forecasts]] (Raphael)<br />
* '''2019 April 30''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190430_sigmar_vs_r_forDSR/ sigma(r) vs r: possible figures for the DSR (v2): more optimal weighting] (Ben Racine and Raphael Flauger)<br />
* '''2019 April 29''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190501_obseff Efficiency for Reijo's observation pattern sims] (Clem)<br />
* '''2019 April 29''': [[Fisher forecasts for inverse noise variance weighting]] (Raphael)<br />
* '''2019 April 22''': [[WAFTT results part 3]] (Raphael)<br />
* '''2019 April 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190418_sigmar_vs_r/ sigma(r) vs r: possible figures for the DSR] (Ben Racine)<br />
* '''2019 April 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190410_closedloop_BK15_S4 Zero order closed loop test of performance based scaling - ML search] (Ben Racine)<br />
* '''2019 March 31''': [[Analysis results for configurations 30-33]] (Raphael)<br />
* '''2019 March 30''': [[Characterization of simulations for configurations 30-33]] (Raphael)<br />
* '''2019 March 26''': [[Simulations for configurations with different frequency coverage]] (Raphael)<br />
* '''2019 March 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190326_bkfinal_05 Zero order closed loop test of performance based scaling - BK15 regen power spectra] (Clem)<br />
* '''2019 March 25''': [[Deeper SAT from Chile II]] (Reijo Keskitalo and Julian Borrill)<br />
* '''2019 March 25''': [[Wider SAT from the Pole II]] (Reijo Keskitalo and Julian Borrill)<br />
* '''2019 March 25''': [[Deep SAT from the Pole]] (Reijo Keskitalo and Julian Borrill)<br />
* '''2019 March 18''': [https://cmb-s4.org/wiki/index.php/Optimal_lensing_fermilab Details on optimal lensing Fermilab presentation / 02.xx real delensing] (Marius Millea)<br />
* '''2019 March 18''': [[High cadence LAT from Chile]] (Reijo Keskitalo)<br />
* '''2019 March 18''': [[WAFTT results part 2]] (Raphael)<br />
* '''2019 March 18''': [[Wider SAT from the Pole]] (Reijo Keskitalo)<br />
* '''2019 March 8''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook//20190308_MLsearch_no85no145/ Maximum likelihood search results without 85GHz and 145GHz] (Ben Racine)<br />
* '''2019 March 3''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190303_MLsearch_bpmax_dep/ Maximum likelihood search results: dependence on the multipole range] (Ben Racine)<br />
* '''2019 February 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190220_noiseparams_bk15_forS4/ BK15 noise levels for S4 sims] (Ben Racine) <br />
* '''2019 February 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190220_S4_NET_forecasts_III/ CMB-S4 NET follow-ups II] (Denis Barkats, Ben Racine-updated on Feb 25) <br />
* '''2019 February 18''': [[Correlation of reconstructed lensing template to ideal II]] (Clem Pryke)<br />
* '''2019 February 18''': [[Fisher calcs of 04b/04c for larger value of r]] (Raphael posted by Clem)<br />
* '''2019 February 14''': [[Deeper SAT from Chile]] (Reijo Keskitalo)<br />
* '''2019 January 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190130_Matrix_first_try/ Matrix-based purification analysis: First try] (B.Racine, J.Willmert) ''Updated 2019 Feb 17th''<br />
* '''2019 January 23''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190123_S4_NET_forecasts_II/ CMB-S4 NET follow-ups I] (Denis Barkats, J. Kovac, Ben Racine-updated on Feb 25) <br />
* '''2019 January 15''': [[Correlation of reconstructed lensing template to ideal]] (Clem Pryke)<br />
* '''2019 January 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190120_dc02_ML_LT/ Maximum likelihood search results for Data Challenge 02.00 with two different lensing templates] (C. Umiltà)<br />
* '''2019 January 17''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190117_MLsearch04d/ Maximum likelihood search results for Data Challenge 04d.00, new BK14 mask reanalysis] (Ben Racine)<br />
* '''2019 January 15''': [[Noise models and sky fractions for WAFTT]] (Raphael)<br />
* '''2019 January 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190111_bkfinal_04bcd BK-style power spectra of 04/04b/04c/04d masks (adding BK14 mask)] (Clem)<br />
* '''2018 December 9''': [[Optimal Bayesian delensing progress update]] (Marius Millea) <br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181207_bkfinal_02lt BK-style power spectra of 02 with Carron lensing templates] (Clem)<br />
* '''2018 December 7''': [[Problems with PS2HAT estimator at low ell]] (Clem Pryke)<br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181116_bpbias_study Bandpower bias study] (Ben Racine)<br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181207_expval_input_ML_search Maximum likelihood search with expectation values as input] (C. Umiltà)<br />
* '''2018 November 28''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181128_toy_sims Effective sky fraction] (Clem)<br />
* '''2018 November 21''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181111_dc04_flatpriors/ Maximum likelihood search results for Data Challenge 04, v2] (Ben Racine)<br />
* '''2018 November 21''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181111_dc04_flatpriors/index_abc.html Maximum likelihood search results for Data Challenge 04b and 04c, v2] (Ben Racine)<br />
* '''2018 November 16''': [[Analytic approximation for r likelihood]] (C. Bischoff) ''Updated 2018-11-20''<br />
* '''2018 November 12''': [[Detection significance for r=0.003]] (C. Bischoff)<br />
* '''2018 November 9''': [[Bad realizations in gsync/gdust sims]] (Clem Pryke)<br />
* '''2018 November 8''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181108_dc02_ML_LT Maximum likelihood search results for Data Challenge 02.00 with an ideal lensing template] (C. Umiltà)<br />
* '''2018 November 5''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181105_toy_sims Attempt to understand sigma(r) results with different hit maps] (Clem)<br />
* '''2018 October 29''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181018_1Dmodel_tapering_study Simple 1D model to study the effect of different observation strategies on the bandpower statistics.] (Ben Racine, Victor Buza, John Kovac) ''Updated 2018 Dec 14th''<br />
* '''2018 October 29''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181029_bkfinal_02lt BK-style power spectra of 02 with ideal lensing templates] (Clem)<br />
* '''2018 October 26''': [[Checking BB purity in re-analysis for alternate masks]] (Clem Pryke)<br />
* '''2018 October 23''': [[Estimated observing efficiency for past and current telescopes, version 2]] (C. Bischoff, Y. Chinone, T. Crawford, M. Hasselfield)<br />
* '''2018 October 14''': [[Estimates of delensing efficiency]] (Raphael)<br />
* '''2018 October 14''': [[Analysis of 04, 04b, 04c simulations]] (Raphael) [[Analysis of 04, 04b, 04c simulations comp]] (Ben)<br />
* '''2018 September 30''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180930_dc04_0to9/ Maximum likelihood search results for Data Challenge 04, models 0 to 9] (Ben Racine) ''Updated 2018 Oct 2nd''<br />
* '''2018 September 30''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180930_dc04_abc_model_0123789_ML/ Maximum likelihood search results for Data Challenge 04b and 04c, model 00, 01, 02, 03, 07, 08 and 09] (Ben Racine)<br />
* '''2018 September 30''': [[Ready for delensing use lensing maps 02.00]] (Julien Carron)<br />
* '''2018 September 28''': [[Towards lensing template]] (Clem Pryke)<br />
* '''2018 September 27''': [[Lensing reconstructions 02.00]] (Julien Carron)<br />
* '''2018 September 26''': [[Lensing map reconstruction from 02.00 sims w/ and w/o foreground+inhomogeneous noise]] (Toshiya Namikawa)<br />
* '''2018 September 25''': [[Estimated observing efficiency for past and current telescopes]] (C. Bischoff)<br />
* '''2018 September 25''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180925_bkfinal_04bc BK-style power spectra of 04/04b/04c masks for 00/01/02/03/07/08/09 foreground models] (Clem)<br />
* '''2018 September 12''': [[Low ell noise from past and current telescopes]] (C. Bischoff)<br />
* '''2018 September 5''': [[Phi reconstruction on 02.00 sims III]] (Anton Baleato)<br />
* '''2018 August 31''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180831_dc04_abc_model00_07_ML_proper_bp/ Maximum likelihood search results for Data Challenge 04b and 04c, for sky models 00 and 07] (Ben Racine)<br />
* '''2018 August 31''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180831_dc04_fixed_bp/ Maximum likelihood search results for Data Challenge 04, fixed bandpasses] (Ben Racine)<br />
* '''2018 August 27''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180827_bkfinal_04 Sims with nominal Chile and Pole masks III - BK-style power spectra of 04b.YY and 04c.YY] (Clem)<br />
* '''2018 August 27''': [[Sims with nominal Chile and Pole masks II]] (Clem P.)<br />
* '''2018 August 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180826_dc04_fixed/ Maximum likelihood search results for Data Challenge 04, fixed] (V.Buza, B.Racine)<br />
* '''2018 August 24''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180824_bkfinal_04/ BK-style power spectra of v04.00-06 sims (CDT report config) FIXED] (Caterina Umilta)<br />
* '''2018 August 24''': [[Amplitude modulated Gaussian dust sims]] (Clem P.)<br />
* '''2018 August 17''': [[Sims with nominal Chile and Pole masks]] (Clem P.)<br />
* '''2018 August 10''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180810_noise/ Achieved performance roundup] (C. Bischoff)<br />
* '''2018 August 7''': [[Pre-reference-design noise specifications for large-aperture forecasting]] (Tom Crawford, Matthew Hasselfield, Gil Holder, Lloyd Knox)<br />
* '''2018 August 6''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180805_s4opt/ Performance-based Fisher optimization for CMB-S4, 44cm vs 52cm aperture (w/ high-res/low-res 20 GHz)] (V.Buza)<br />
* '''2018 July 9''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180708_dc04/ Maximum likelihood search results for Data Challenge 04] (V.Buza)<br />
* '''2018 July 6''': [[Phi reconstruction on 02.00 sims II]] (Anton Baleato and Clem Pryke)<br />
* '''2018 June 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180611_s4opt/ Performance-based Fisher optimization for CMB-S4, 44cm aperture] (V.Buza) -- see corrected August 6th Update!<br />
* '''2018 June 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180609_S4_noise_simulation_arbitrary_coverage/ Recipe to generate performance based S4 simulations with arbitrary sky distribution (in progress)] (B.Racine, V.Buza)<br />
* '''2018 April 29''': [[Phi reconstruction on 02.00 sims]] (Anton Baleato)<br />
* '''2018 April 25''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180425_r_equivalent_maps/ Smallfield r-equivalent Maps] (Kenny Lau)<br />
* '''2018 April 4''': [[Sky masks for simulations III]] (Clem P.)<br />
* '''2018 March 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180323_bkfinal_04/ BK-style power spectra of v04.00-06 sims (CDT report config) BROKEN] (Clem)<br />
* '''2018 March 16''': [[ILC noise for large apertures at CDT noise levels]] (Raphael Flauger posted by Clem)<br />
* '''2018 March 16''': [[Sky masks for simulations II]] (Clem P.)<br />
* '''2018 February 19''': [[Sky masks for simulations]] (Clem P.)<br />
* '''2018 February 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180218_s4opt/ Performance-based Fisher optimization for CMB-S4, v3] (Victor Buza)<br />
* '''2018 February 7''': [[Sim map sets to demonstrate "real delensing" (02.00 and 02.09)]] (Clem P.)<br />
* '''2018 February 6''': [[Data Challenge Map Sets 04.YY]] (Clem P.)<br />
* '''2017 December 8''': [[Vansyngel Model]] (Clem P.)<br />
* '''2017 November 6''': [[Bandpass Convention - What does flat mean]] (Clem P.) - followup notes added Nov 20<br />
* '''2017 September 27''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170927_dc02/ Maximum likelihood search results for Data Challenge 02] (Bischoff, Buza, Willmert)<br />
* '''2017 September 13''': [[Bias on r from Band Center Errors]] (Palladino, Willmert, Bischoff)<br />
* '''2017 September 8''': [[Checking dust decorrelation in Raphael MHD based dust sim]] (Clem P.)<br />
* '''2017 September 6''': [[New NET Calculator and Validation]] (Denis Barkats)<br />
* '''2017 September 1''': [[Resolution at 20 GHz]] (Raphael)<br />
* '''2017 August 31''': [[Bias on r from additive systematics]] (Palladino, Willmert, Bischoff)<br />
* '''2017 August 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170818_bkfinal_03.00/ BK-style power spectra for 1000 realizations of v03.00,.03 CMB-S4 simulation maps] (Justin Willmert)<br />
* '''2017 August 18 ''': [[Neff_and_Beam_Calibration| Neff and Beam Calibration]] (Dan)<br />
* '''2017 August 18''': [[Ideal delensing templates from flat-sky QE, first pass]] (Kyle Story)<br />
* '''2017 August 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170818_HR/ High-Res studies for CMB-S4 (draft, v2)] (Victor Buza)<br />
* '''2017 August 18''': [[Comments from Anthony Challinor and Rupert Allison regarding the impact of Galactic Foregrounds on lensing]] (Neelima)<br />
* '''2017 August 11''': [[Joint Synchrotron and Dust Maps from Simulations]] (B. Hensley)<br />
* '''2017 August 9''': [[Dust Emission From Halos]] (Jim & Jean-Baptiste)<br />
* '''2017 August 9''': [[SZ Clusters update]] (Mat & Nick)<br />
* '''2017 August 4''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170804_HR/ High-Res studies for CMB-S4 (preliminary draft)] (Victor Buza); perhaps a reference of interest https://arxiv.org/abs/1707.02259<br />
* '''2017 July 10''': [[Additive systematics for data challenge 03]] (Bischoff, Palladino, Buza, Kovac)<br />
* '''2017 July 6''': [[Detection significance and sky fraction, dust decorrelation]](Raphael)<br />
* '''2017 July 3''': [[Toy highly decorrelated dust model]] (Clem P.)<br />
* '''2017 June 27''': [[Checking dust decorrelation in models d1/d4/d7 and hipdt]] (Clem P.)<br />
* '''2017 June 23''': [[Dust_delensing_firstlook|Dust delensing update]] (Alex)<br />
* '''2017 June 23''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170623_bkfinal_02.00/ BK-style power spectra for 1000 realizations of v02.00–06 CMB-S4 simulation maps] (Justin Willmert) ''Updated 2017 Sep 08''<br />
* '''2017 June 22''': [[Warm-up exercise for delensing]] (Raphael)<br />
* '''2017 June 19''': [[SZ Clusters update]] (Mat, Nick)<br />
* '''2017 June 11''': [[Notes from May 31 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 June 9''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170525_s4syst/ Introducing systematics for CMB-S4] ((Victor Buza), with input from Colin Bischoff, John Kovac)<br />
* '''2017 June 9''': [[Dust_delensing_firstlook]] (Alex)<br />
* '''2017 June 9''': [[r-forecasting: high and low ell coordination|r-forecasting: update on high and low ell coordination]] (Neelima+Colin Hill writing)<br />
* '''2017 June 1''': [[Residuals for DC 01.01 and DC 01.02]] (Raphael)<br />
* '''2017 June 1''': [[Levels of foregrounds in Gaussian and PySM simulations]] (Raphael)<br />
* '''2017 May 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170511_s4dc1/ S4 DC 01.xx analysis, v2] (Victor Buza, Colin Bischoff, Justin Willmert)<br />
* '''2017 May 26 ''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170411_bkfinal_01.00/ Updated v01.02 in "BK-style power spectra for 1000 realizations of v01.00–02 CMB-S4 simulation maps"] (Justin Willmert)<br />
* '''2017 May 15''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170515_chkS4/ N_ell spectra for CMB-S4 DC2.0] (Victor Buza)<br />
* '''2017 May 15''': [[Rev 2 PySM a2d4f1s3 maps]] (Clem P.)<br />
* '''2017 May 12''': [[r-forecasting: high and low ell coordination|r-forecasting: high and low ell coordination]] (lensers writing)<br />
* '''2017 May 8''': [[Checking PySM maps]] (Clem P.)<br />
* '''2017 May 2''': [[Notes from April 26 telecon on science requirements for clusters/high-ell]] (Steve)<br />
* '''2017 May 1''': [[r-forecasting: delensing discussion|r-forecasting delensing discussion]] (Neelima and Blake)<br />
* '''2017 April 28 ''': [[Update_on_Neff_Forecasts| Update on Neff Forecasts]] (Dan)<br />
* '''2017 April 26 ''': [http://www.cosmo.bnl.gov/www/msyriac/web/work/sigma8plots.html Update on cluster number counts forecast including w_a] (Mat and Nick)<br />
* '''2017 April 21 ''': [[lensing-DE|Update on a lensing-based DE forecast]] (Jo, Siddharth)<br />
* '''2017 April 18 ''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170411_bkfinal_01.00/ BK-style power spectra for 1000 realizations of v01.00–02 CMB-S4 simulation maps] (Justin Willmert)<br />
* '''2017 April 18 ''': [[S4-Lensing|S4 measurement requirements for neutrino mass and delensing - first pass]] (Neelima/Blake)<br />
* '''2017 April 17 ''': [[HiDPol|HI-based dust polarization model for r forecasts]] (Tuhin)<br />
* '''2017 April 05 ''': [[lensing-DE|Notes on one path to lensing-based DE forecasts]] (Jo)<br />
* '''2017 April 05 ''': [[Notes from April 5 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 April 05''': [https://cmb-s4.org/CMB-S4workshops/images/Sigma8_z_prep.pdf Sigma8(z) SPT clusters (placeholder) ] (S Bocquet)<br />
* '''2017 April 04''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170404_s4opt/ Updated Performance-based Fisher optimization for CMB-S4 (using bands v1.99)] (Victor Buza, Updated 2017.04.21)<br />
* '''2017 March 31 ''': [[Data Challenge analysis - DC1.0, DC1.1, DC1.2]] (Raphael)<br />
* '''2017 March 30 ''': [[Notes from March 28 telecon on science requirements for clusters/high-ell]] (Jim & Steve)<br />
* '''2017 March 29''': [[CMB-S4 frequency bands v1.99]] (John Kovac, Band-definition working group)<br />
* '''2017 March 28''': [[Adding higher res delensing "band"]] (Clem P.)<br />
* '''2017 March 27''': [[01.01 sim input maps - first try]] (Clem P.)<br />
* '''2017 March 23''': [[01.00 sim input maps]] (Clem P.)<br />
* '''2017 March 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170221_S4_NET_forecasts/ S4 Band sensitivity comparison follow-up] (Denis Barkats, John Kovac)<br />
* '''2017 March 17''': [http://users.physics.harvard.edu/~buza/20170317_s4dc1/ S4 DC1.0 analysis] (Victor Buza, Colin Bischoff, Justin Willmert)<br />
* '''2017 March 17 ''': [[Media:Telecon_03172017_optimization_for_CMBS4.pdf]]: Optimization methodology for SO (Josquin)<br />
* '''2017 March 16 ''': [[ P_k_science_case| P(k) science case]] (Colin, Simone, Nick, David)<br />
* '''2017 March 15 ''': [[Notes from March 15 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 March 15 ''': [[CMB halo lensing sensitivity as a function of map sensitivity and resolution]] (Jim & Jean-Baptiste)<br />
* '''2017 March 15 ''': [[w and gamma | w and Delta gamma constraints from sigma_8 (z)]] (Mat & Nick)<br />
* '''2017 March 10 ''': [[Notes from March 8 telecon on science requirements for clusters/high-ell]] (Jim & Steve)<br />
* '''2017 March 8 ''': [[reionization_requirements| Reionization science]] (Simone & Marcelo)<br />
* '''2017 March 8 ''': [[High ell topics | High ell topics ]] (Jim)<br />
* '''2017 March 8 ''': [[SZ_s8_z | sigma 8 of z constraints ]] (Mat, Nick)<br />
* '''2017 March 8 ''': [[Szcounts | Number counts update for 1.0', 1.5', 2.0']] (Nick, Mat)<br />
* '''2017 March 8 ''': [[SZastro | SZ astrophysics with DESI ]](Nick, Simone, Emanuel, David)<br />
* '''2017 February 24''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170224_cmbs4_dc1_final/ BK-style processing of DC1.0 maps to spectra] (Justin Willmert, Colin Bischoff)<br />
* '''2017 February 15 ''': [[Extragalactic lensing sims| Update on extragalactic phase-2 lensing sims]] (Marcelo, George, Dick, others)<br />
* '''2017 February 15 ''': [[Plan for next Galactic Phase-2sims| Plan for next Galactic phase-2 sims]] (Jo, Ben)<br />
* '''2017 February 10 ''': [[Resolution of foreground-cleaned map]] (Mat, Neelima, Blake, Alex, others)<br />
* '''2017 February 10 ''': [[Nongaussian dust in lensing]] (Alex, Mat, Neelima, Blake, others)<br />
* '''2017 January 30''': [[Aliased power in noise maps]] (Bischoff, Updated 2017-02-02)<br />
* '''2017 January 23''': [[CMBS4 Band Sensitivity Comparison]] (Charlie Hill)<br />
* '''2017 January 12''': [http://bicep.rc.fas.harvard.edu/cbischoff/20170112_data_challenge_1/ Maps for CMB-S4 data challenge 1] (Bischoff, Pryke, Buza)<br />
* '''2016 December 21''': [http://users.physics.harvard.edu/~buza/20161220_chkS4/ N_ell spectra for the CMB-S4 data challenge, and updated &sigma;(r) checkpoints] (Victor Buza, Updated 2017.02.01)<br />
* '''2016 November 30''': [[First steps to sim input maps]] (Clem P.)<br />
* '''2016 November 4''': [[Tophat bands for Data Challenge]] (Bischoff)<br />
* '''2016 July 8''': [[fsky|Dependence of foregrounds on sky fraction]] (Raphael)<br />
* '''2016 July 8''': [[SciBookPowspecTheoryFig|Three choices for Science Book Figure 5 (theory power spectrum & current BB points)]] (Tom C.)<br />
* '''2016 July 8''': [http://users.physics.harvard.edu/~buza/20160707_s4plots/ S4 Inflation Chapter Plot Suggestions, V2] (Victor Buza)<br />
* '''2016 July 6''': [[w_cosntraint|Preliminary w constraint]] (Alessandro)<br />
* '''2016 June 24''': [[nsr|Preliminary ns-r plot for discussion]] (Raphael)<br />
* '''2016 June 16''': [[DelensingImpact| Impact Of Delensing On sigma(r)]] (Neelima/Mat)<br />
* '''2016 June 16''': [http://users.physics.harvard.edu/~buza/20160616_s4plots/ S4 Inflation Chapter Plot Suggestions] (Victor Buza)<br />
* '''2016 June 10''': [[MapBasedRb| Map-based &sigma;(r) forecasts V2]] (David/Jo/Ben)<br />
* '''2016 June 3''': [http://users.physics.harvard.edu/~buza/20160531_fisher/ &sigma;(r) forecasting checkpoints, V2] (Victor Buza)<br />
* '''2016 June 3''': [[ BTTfixedeffort | Forecasts for fnl BTT beam/fixed effort]] (Daan)<br />
* '''2016 May 31''': [[ForecastPatchyReion| Forecasts for patchy reionization]] (Vera, Alex, Nick)<br />
* '''2016 May 26''': [[Forecasting | Forecasts on neutrino mass]] (Nam, Mat, Neelima)<br />
* '''2016 May 26''': [[ KSZ| Forecasts on kSZ S/N]] (Simone, Emmanuel, Colin)<br />
* '''2016 May 26''': [[ Forecastfiso_planck| Forecast on correlated and anti-correlated CDM isocurvature f_iso]] (Kimmy, Cora, updated with plots 20160602)<br />
* '''2016 May 24''': [[ BTTNoiseBeam | Forecasts on fnl BTT beam/FWHM]] (Daan)<br />
* '''2016 May 22''': [[ ForecastAxions| Update on the axion isocurvature constraints for changing sensitivity and resolution]] (Renee)<br />
* '''2016 May 21''': [[ Forecastpann| Forecast on dark matter annihilation parameter p_ann]] (Kimmy, Cora)<br />
* '''2016 May 20''': [[NeffNoiseBeam| Forecasts on Neff and Yp]] (Joel, Alex)<br />
* '''2016 May 20''': [[ForecastEDE| Forecasts on Early Dark Energy]] (Erminia)<br />
* '''2016 May 20''': [[ForecastCompIsocurv| Forecasts on compensated isocurvature varying sensitivity, resolution and sky coverage]] (Julian, Ely)<br />
* '''2016 May 20''': [[ForecastBirefring| Forecasts on birefringence varying sensitivity and resolution]] (Vera, Alex)<br />
* '''2016 May 20''': [[ForecastStrings| Forecasts on string tension varying sensitivity and resolution]] (Renee)<br />
* '''2016 May 20''': [[RobustForecast| Cosmological forecasts including component separation and iterative delensing]] (Stephen Feeney and Josquin Errard)<br />
* '''2016 May 19''': [[MapBasedR| Map-based &sigma;(r) forecasts]] (David A.)<br />
* '''2016 May 18''': [[Shear_calibration_LSST|LSST shear calibration with CMB S4]] (Emmanuel Schaan)<br />
* '''2016 May 13''': [http://users.physics.harvard.edu/~buza/20150505_fisher/ &sigma;(r) forecasting checkpoints] (Victor Buza)<br />
* '''2016 May 13''': [[NonGaussianitiesTTT| CMBS-4 forecasts local and equilateral scalar Ngs using TTT]] (daan)<br />
* '''2016 May 13''': [[ForecastingSims|Simulations for r forecasts]] (Jo/Ben/David)<br />
* '''2016 May 6''': [[DMInteractionsComplementarity|DM interactions: complementarity]] (Vera)<br />
* '''2016 May 6''': [[Scenarios| Scenarios]] (Scott, Vera)<br />
* ''' 2016 May 3''': [[ForecastAxions |Effect of S4 specs on axion density parameters]] (Renee)<br />
* '''2016 April 30''': [[ForecastNu| Effect of S4 specs on neutrino parameters]] (Erminia)<br />
* '''2016 April 28''': [http://web.stanford.edu/~wlwu/posting/20160421_lensres/ Delensing residuals with low-ell foregrounds] (Kimmy Wu)<br />
* '''2016 April 28''': [[NonGaussianities| CMBS-4 forecast for tensor NGs]] (daan)<br />
* '''2016 April 19''': [[ForecastingStep1| Checking basic parameters for nominal case]] (Jo + multiple authors)<br />
* '''2016 April 5''': [[Forecasting|Setting up non-r Fisher-based parameter forecasts]] (Jo + others)<br />
* '''2016 March 31''': [http://users.physics.harvard.edu/~buza/20150331_fisher/ Fisher projections for &sigma;(r) based on achieved performance] (Victor Buza)<br />
* '''2016 January 27''': [https://cmb-s4.org/CMB-S4workshops/index.php/File:sptpol_ptsrc_polfrac_500d.pdf Quick estimate of mean-squared polarization fraction for SPTpol sources] (Tom Crawford)</div>Cbischoffhttp://www.cmb-s4.org/wiki/index.php?title=PureB_by_Messenger_Method&diff=9258PureB by Messenger Method2019-09-16T14:13:20Z<p>Cbischoff: </p>
<hr />
<div>''Michael Ray, Colin Bischoff, 2019-09-16''<br />
----<br />
<br />
This posting describes an alternate pure-B estimator applied to the 95 GHz DC 04.00 maps with ''A<sub>L</sub>''=1. It uses the "messenger method" ([https://ui.adsabs.harvard.edu/abs/2013A%26A...549A.111E/abstract Elsner & Wandelt 2012]) to Wiener filter the maps. We treat the E-mode part of the signal covariance as if it was noise covariance ([https://ui.adsabs.harvard.edu/abs/2017PhRvD..96d3523B/abstract Bunn & Wandelt 2017]), so filter equation becomes:<br />
<br />
map<sub>wf</sub> = (S<sub>B</sub>/(S<sub>B</sub>+S<sub>E</sub>+N)) * map,<br />
<br />
where <tt>S<sub>E,B</sub></tt> are the E-mode and B-mode parts of the signal covariance.<br />
<br />
For these simulations with unfiltered skies, the signal covariance is diagonal in the spherical harmonic basis. We treat the noise covariance as diagonal in the pixel basis (not strictly true because of the white + 1/&#x2113; noise spectrum in the data challenge maps). The messenger method iteratively solves fo the Wiener-filtered map by introducing a messenger field, <tt>t</tt>, with covariance matrix, <tt>T</tt>, that is proportional to the identity matrix, so it can be written easily in any basis. For each step of the algorithm, we transform back and forth between pixel space and spherical harmonic space, with the messenger field carrying information between the two bases.<br />
<br />
As a first demonstration, we applied this technique to the 95 GHz DC 04.00 maps (Gaussian foregrounds, circular 3% fsky mask). The signal covariance matrices (in spherical harmonic space) are set to lensed-LCDM EE and BB spectra (purely diagonal), multiplied by ''B<sub>&#x2113;</sub><sup>2</sup>'' and zeroed for &#x2113; &lt; 30 (this last choice appears to have consequences for the bandpower window functions). We did not include any foreground contribution to the signal covariance. The noise covariance is diagonal in pixel space, with values equal to 0.01 &mu;K<sup>2</sup> times the inverse of the mask (checked against a set of noise maps). For unobserved pixels, the noise covariance is set to a very large but finite value.<br />
<br />
The messenger method includes parameter, &lambda;, which scales the covariance of the messenger field. Convergence proceeds more quickly for large values of &lambda;, but the final solution is obtained for &lambda; = 1. This means that we want to implement a "cooling schedule" for efficient filtering. In our implementation, &lambda; starts at a value of 1300, is decreased to 100 on the second iteration, and then is reduced by factor &eta; = 0.825 on each subsequent iteration. When &lambda; reaches 1, we iterate an additional 5 times. We have experimented fairly extensively with other cooling schedules and found that this method gives good convergence in a reasonable amount of time. (We are able to filter a single set of Q and U maps in 34 minutes on a single processor.)<br />
<br />
Figures 1 and 2 show a map before and after filtering. The input maps is dominated by LCDM E modes. The output map contains B modes from foregrounds and lensing. The output map color scale has been zoomed in so that we can see that the pure-B filtering operation has extended the map into the unobserved region.<br />
<br />
{|<br />
|[[File:Q input map.png|frame|Figure 1: Input Q signal plus noise map. This is zoomed in on the unmasked region of the map.]]<br />
|[[File:Q output map.png|frame|Figure 2: Output Q signal plus noise map. This has been filtered through our pure B estimator. This map is also zoomed in on the unmasked region although the algorithm extends the map into the unmasked region.]]<br />
|}<br />
<br />
After applying the filter, we calculate the BB spectrum with anafast and bin with &Delta;&#x2113;=35, to match the pure-S2hat analysis. Noise bias is measured from 100 noise-only simulations. Bandpower window functions (Figures 4 and 5) and suppression factors are calculated by running &#x2113;-by-&#x2113; simulations (but only 6 realizations per &#x2113; value so far). Figure 3 shows noise-debiased and suppression-factor-corrected power spectra for 100 LCDM+foregrounds+noise simulations. The expectation value line is calculated by applying the bandpower window functions to a LCDM+foregrounds model that matches the sims. <br />
<br />
There is some noticeable bias in the last bin especially. Something is clearly off with the calculations for this bin (see bandpower window functions) and needs to be investigated.<br />
<br />
[[File:Filtered specs mean vs expectation.png|frame|Figure 3: Band powers of 100 filtered signal plus noise simulations. These were filtered using the messenger method estimator. Also shown is the mean and the expectation value calculated using band power window functions and BB theory spectra.|center]]<br />
<br />
Figures 4 and 5 show bandpower window functions for input B modes >> output BB (left) and input E modes >> output BB (right). These were calculated by running just six simulations for each &#x2113; value, and could be made less noisy with additional computation. The purity of the estimator can be seen by comparing the absolute level of the two sets of functions; the first ell bin responds has response to B modes that is ~1000x greater than the response to E modes. Our initial reaction was that this is not an extremely impressive level of purity (though it is better than simply masking and running anafast). However, keep in mind that we are using a Wiener filter that knows about the noise level, so it might choose to keep modes that are slightly ambiguous if they result in a net decrease in bandpower variance.<br />
<br />
The input B >> output BB window functions show a prominent bump for &#x21113; < 30. This is probably due to the choice we made to zero the E and B signal covariance matrices in that range (which does match the sim construction). Our naive expectation based on the Wiener filter equation was that the filter would kill that &#x2113; range because it contains no signal, but clearly this is not happening. We plan to investigate this by calculating window functions without zeroing that part of the covariance matrix.<br />
<br />
The 10th &#x2113; bin shows odd behavior, with no upper end cutoff and very different normalization from other bins. This might just be a bug in the binning code. That bin also showed the largest bias in Figure 3, which might be related.<br />
<br />
{|<br />
|[[File:Messenger bb2bb bpwf.png|frame|Figure 4: BB to BB band power window functions using messenger method pure-B estimator.]]<br />
|[[File:Messenger ee2bb bpwf.png|frame|Figure 5: EE to BB band power window functions using messenger method pure-B estimator.]]<br />
|}<br />
<br />
Figure 6 shows the variance calculated from BB bandpowers of the first 100 signal + noise maps by pure-S2hat and by this estimator. The Wiener filter / messenger method estimator produces lower variance for all bins (but the last bin shouldn't be trusted, for reasons discussed above). We believe that at least part of this improvement is because the Wiener filter considers both signal and noise variance, so it could decide to keep more modes for a signal-dominated case. There results are from sims with ''A<sub>L</sub>'' = 1, which is a pretty large B-mode signal when compared to the CMB-S4 forecasted 95 GHz noise. We expect that the improvement would be much smaller for maps that have been delensed.<br />
<br />
[[File:Variance comparison.png|frame|Figure 6: Comparison of messenger method and S2hat estimator when it comes to the variance in each bin.|center]]<br />
<br />
There are several steps that are still needed before this estimator can be used as part of a full Data Challenge analysis:<br />
* Look into the effect of zeroing signal covariance for &#x2113; < 30. Is this responsible for the low-&#x2113; feature in the bandpower window functions?<br />
* Figure out what is going on with the 10th &#x2113; bin.<br />
* Incorporate this filter into a pipeline infrastructure that can run on all maps, take cross-spectra, calculate TT, EE, TE, EB, TB, etc.</div>Cbischoffhttp://www.cmb-s4.org/wiki/index.php?title=PureB_by_Messenger_Method&diff=9257PureB by Messenger Method2019-09-16T11:56:23Z<p>Cbischoff: </p>
<hr />
<div>''Michael Ray, Colin Bischoff, 2019-09-xx''<br />
----<br />
<br />
This posting describes an alternate pure-B estimator applied to the 95 GHz DC 04.00 maps. It uses the "messenger method" ([https://ui.adsabs.harvard.edu/abs/2013A%26A...549A.111E/abstract Elsner & Wandelt 2012]) to Wiener filter the maps. We treat the E-mode part of the signal covariance as if it was noise covariance ([https://ui.adsabs.harvard.edu/abs/2017PhRvD..96d3523B/abstract Bunn & Wandelt 2017]), so filter equation becomes:<br />
<br />
map<sub>wf</sub> = (S<sub>B</sub>/(S<sub>B</sub>+S<sub>E</sub>+N)) * map,<br />
<br />
where <tt>S<sub>E,B</sub></tt> are the E-mode and B-mode parts of the signal covariance.<br />
<br />
For these simulations with unfiltered skies, the signal covariance is diagonal in the spherical harmonic basis. We treat the noise covariance as diagonal in the pixel basis (not strictly true because of the white + 1/&#x2113; noise spectrum in the data challenge maps). The messenger method iteratively solves fo the Wiener-filtered map by introducing a messenger field, <tt>t</tt>, with covariance matrix, <tt>T</tt>, that is proportional to the identity matrix, so it can be written easily in any basis. For each step of the algorithm, we transform back and forth between pixel space and spherical harmonic space, with the messenger field carrying information between the two bases.<br />
<br />
As a first demonstration, we applied this technique to the 95 GHz DC 04.00 maps (Gaussian foregrounds, circular 3% fsky mask). The signal covariance matrices (in spherical harmonic space) are set to the standard lensed-LCDM E and B-mode spectra (purely diagonal). We did not include any foreground contribution to the signal covariance. The noise covariance is diagonal in pixel space, with values equal to 0.01 &mu;K<sup>2</sup> times the inverse of the mask (checked against a set of noise maps). For unobserved pixels, the noise covariance is set to a very large but finite value.<br />
<br />
The messenger method includes parameter, &lambda;, which scales the covariance of the messenger field. Convergence proceeds more quickly for large values of &lambda;, but the final solution is obtained for &lambda; = 1. This means that we want to implement a "cooling schedule" for efficient filtering. In our implementation, &lambda; starts at a value of 1300, is decreased to 100 on the second iteration, and then is reduced by factor &eta; = 0.825 on each subsequent iteration. When &lambda; reaches 1, we iterate an additional 5 times. We have experimented fairly extensively with other cooling schedules and found that this method gives good convergence in a reasonable amount of time. (We are able to filter a single set of Q and U maps in 34 minutes on a single processor.)<br />
<br />
Figures 1 and 2 show a map before and after filtering. The input maps is dominated by LCDM E modes. The output map contains B modes from foregrounds and lensing. The output map color scale has been zoomed in so that we can see that the pure-B filtering operation has extended the map into the unobserved region.<br />
<br />
{|<br />
|[[File:Q input map.png|frame|Figure 1: Input Q signal plus noise map. This is zoomed in on the unmasked region of the map.]]<br />
|[[File:Q output map.png|frame|Figure 2: Output Q signal plus noise map. This has been filtered through our pure B estimator. This map is also zoomed in on the unmasked region although the algorithm extends the map into the unmasked region.]]<br />
|}<br />
<br />
After applying the filter, we calculate the BB spectrum with anafast and bin with &Delta;&#x2113;=35, to match the pure-S2hat analysis. Noise bias is measured from 100 noise-only simulations. Bandpower window functions (Figures 4 and 5) and suppression factors are calculated by running &#x2113;-by-&#x2113; simulations (but only 6 realizations per &#x2113; value so far). Figure 3 shows noise-debiased and suppression-factor-corrected power spectra for 100 LCDM+foregrounds+noise simulations. The expectation value line is calculated by applying the bandpower window functions to a LCDM+foregrounds model that matches the sims. <br />
<br />
There is some noticeable bias in the last bin especially. Something is clearly off with the calculations for this bin (see bandpower window functions) and needs to be investigated.<br />
<br />
[[File:Filtered specs mean vs expectation.png|frame|Figure 3: Band powers of 100 filtered signal plus noise simulations. These were filtered using the messenger method estimator. Also shown is the mean and the expectation value calculated using band power window functions and BB theory spectra.|center]]<br />
<br />
<br />
As one can see, the expectation value for our estimator runs directly through the middle of our simulations and is very close to our mean. It is worth noting that there is definitely something out of the ordinary happening in our last bin. In this bin, we routinely get results that do not agree with the rest of the data. Because of this, we generally ignore results from the last bin given that we are not too worried with what is happening at that ell range anyway. Shown below are plots of BB to BB and EE to BB band power window functions for both the messenger method estimator and the S2hat estimator. Band power window functions for the messenger estimator were calculated with an input signal C_ell = 1 on the sky. This means that the actual input power for deriving band power window functions is 1 * B_ell squared, where B_ell squared contains the effect of the beam. We also ran 6 simulations at each ell with this input power and then took the mean of the output across these six simulations to get the final band power window functions. Summing the window functions across ell values gives us the total suppression factor.<br />
<br />
Figures 4 and 5 show bandpower window functions for input B modes &rightarrow; output BB <br />
<br />
{|<br />
|[[File:Messenger bb2bb bpwf.png|frame|Figure 4: BB to BB band power window functions using messenger method pure-B estimator.]]<br />
|[[File:Messenger ee2bb bpwf.png|frame|Figure 5: EE to BB band power window functions using messenger method pure-B estimator.]]<br />
|}<br />
<br />
Again, it is visually apparent that there is something odd going on in the last bin for the messenger method estimator.<br />
<br />
Below are plots the variance in each bin across the 100 realizations which were filtered. The exact same simulations were used as input to the two methods compared (signal plus noise simulations at 95 GHz using the 04.00 experiment configuration).<br />
<br />
<br />
[[File:Variance comparison.png|frame|Figure : Comparison of messenger method and S2hat estimator when it comes to the variance in each bin.|center]]<br />
<br />
As shown above, the messenger method beats the S2hat estimator in terms of variance per bin. We believe the main reason for this is that the S2hat estimator uses a simple weighting of 1/N to filter the maps. Since the signal plus noise simulations have a sizeable amount of BB lensing signal contained within them, the fact that we are doing a weiner filter (and thus taking into account the signal covariance) means that we would expect to get a large improvement over an estimator which only knows about noise covariance. For delensed simulations, we would expect to see less of an improvement from the messenger method over the S2hat filtering.</div>Cbischoffhttp://www.cmb-s4.org/wiki/index.php?title=PureB_by_Messenger_Method&diff=9251PureB by Messenger Method2019-09-15T13:15:32Z<p>Cbischoff: </p>
<hr />
<div>''Michael Ray, Colin Bischoff, 2019-09-xx''<br />
----<br />
<br />
This posting describes an alternate pure-B estimator applied to the 95 GHz DC 04.00 maps. It uses the "messenger method" ([https://ui.adsabs.harvard.edu/abs/2013A%26A...549A.111E/abstract Elsner & Wandelt 2012]) to Wiener filter the maps. We treat the E-mode part of the signal covariance as if it was noise covariance ([https://ui.adsabs.harvard.edu/abs/2017PhRvD..96d3523B/abstract Bunn & Wandelt 2017]), so filter equation becomes:<br />
<br />
map<sub>wf</sub> = (S<sub>B</sub>/(S<sub>B</sub>+S<sub>E</sub>+N)) * map,<br />
<br />
where <tt>S<sub>E,B</sub></tt> are the E-mode and B-mode parts of the signal covariance.<br />
<br />
For these simulations with unfiltered skies, the signal covariance is diagonal in the spherical harmonic basis. We treat the noise covariance as diagonal in the pixel basis (not strictly true because of the white + 1/&#x2113; noise spectrum in the data challenge maps). The messenger method iteratively solves fo the Wiener-filtered map by introducing a messenger field, <tt>t</tt>, with covariance matrix, <tt>T</tt>, that is proportional to the identity matrix, so it can be written easily in any basis. For each step of the algorithm, we transform back and forth between pixel space and spherical harmonic space, with the messenger field carrying information between the two bases.<br />
<br />
As a first demonstration, we applied this technique to the 95 GHz DC 04.00 maps (Gaussian foregrounds, circular 3% fsky mask). The signal covariance matrices (in spherical harmonic space) are set to the standard lensed-LCDM E and B-mode spectra (purely diagonal). We did not include any foreground contribution to the signal covariance. The noise covariance is diagonal in pixel space, with values equal to XX &mu;K<sup>2</sup> times the inverse of the mask. For unobserved pixels, the noise covariance is set to a very large but finite value.<br />
<br />
The messenger method includes parameter, &lambda;, which scales the covariance of the messenger field. Convergence proceeds more quickly for large values of &lambda;, but the final solution is obtained for &lambda; = 1. This means that we want to implement a "cooling schedule" for efficient filtering. In our implementation, &lambda; starts at a value of 1300, is decreased to 100 on the second iteration, and then is reduced by factor &eta; = 0.825 on each subsequent iteration. When &lambda; reaches 1, we iterate an additional 5 times. We have experimented fairly extensively with other cooling schedules and found that this method gives good convergence in a reasonable amount of time. (We are able to filter a single set of Q and U maps in 34 minutes on a single processor.)<br />
<br />
Figures 1 and 2 show a map before and after filtering. The input maps is dominated by LCDM E modes. The output map contains B modes from foregrounds and lensing. The output map color scale has been zoomed in so that we can see that the pure-B filtering operation has extended the map into the unobserved region.<br />
<br />
{|<br />
|[[File:Q input map.png|frame|Figure 1: Input Q signal plus noise map. This is zoomed in on the unmasked region of the map.]]<br />
|[[File:Q output map.png|frame|Figure 2: Output Q signal plus noise map. This has been filtered through our pure B estimator. This map is also zoomed in on the unmasked region although the algorithm extends the map into the unmasked region.]]<br />
|}<br />
<br />
The algorithm takes in a set of two maps, corresponding to a Q and U measurement, and outputs a B only weiner filtered set of Q and U maps. One can visually see that although the input map has a defined edge, the algorithm extends the output map into the unobserved region. This is because the code is coming up with a full sky weiner filtered map and thus any power detected at low ell will result in map fluctuations at large angular scales. It is also visually apparent that the input Q map contains mostly E modes (fluctuations that appear straight up and down or straight across), while the output Q map looks like it's all B modes (diagonal fluctuations). This is exactly what we would hope to see from a pure-B estimator. Note that there is a scale difference between the two plots. This is because the input map contains E signal, so the Q map will have a larger amplitude in each pixel for the input map than the output map which contains only B modes.<br />
<br />
There is still some noise bias in the output map, however we can remove that through using monte carlo methods. There is also a suppression factor involved in the output data which is the reason for the scale difference in plots. This factor is corrected for through the use of band power window functions. Both the noise debiasing and suppression factor correction are made at the power spectrum level only. We are not capable of applying noise and suppression factor corrections to maps.<br />
<br />
Shown below is a plot of 100 spectra which are cleaned signal plus noise maps at 95 GHz taken from the 04.00 CMBS4 experiment configuration. The bins used in this analysis began at ell of 20, and went up through ell of 370 with a bin size of 35. So, bin number zero is ell of 20 - 55. Bin 9 (last bin) is ell of 335 - 370. Also included is the mean of these 100 spectra and the expectation value which was calculated using band power window functions and theory BB spectra.<br />
<br />
<br />
[[File:Filtered specs mean vs expectation.png|frame|Figure 3: Band powers of 100 filtered signal plus noise simulations. These were filtered using the messenger method estimator. Also shown is the mean and the expectation value calculated using band power window functions and BB theory spectra.|center]]<br />
<br />
<br />
As one can see, the expectation value for our estimator runs directly through the middle of our simulations and is very close to our mean. It is worth noting that there is definitely something out of the ordinary happening in our last bin. In this bin, we routinely get results that do not agree with the rest of the data. Because of this, we generally ignore results from the last bin given that we are not too worried with what is happening at that ell range anyway. Shown below are plots of BB to BB and EE to BB band power window functions for both the messenger method estimator and the S2hat estimator. Band power window functions for the messenger estimator were calculated with an input signal C_ell = 1 on the sky. This means that the actual input power for deriving band power window functions is 1 * B_ell squared, where B_ell squared contains the effect of the beam. We also ran 6 simulations at each ell with this input power and then took the mean of the output across these six simulations to get the final band power window functions. Summing the window functions across ell values gives us the total suppression factor.<br />
<br />
<br />
[[File:Messenger bb2bb bpwf.png|frame|Figure 4: BB to BB band power window functions using messenger method pure-B estimator.|center]]<br />
[[File:Messenger ee2bb bpwf.png|frame|Figure 5: EE to BB band power window functions using messenger method pure-B estimator.|center]]<br />
[[File:S2hat bb2bb bpwf.png|frame|Figure 6: BB to BB band power window functions using S2hat pure-B estimator|center]]<br />
<br />
<br />
Again, it is visually apparent that there is something odd going on in the last bin for the messenger method estimator.<br />
<br />
Below are plots the variance in each bin across the 100 realizations which were filtered. The exact same simulations were used as input to the two methods compared (signal plus noise simulations at 95 GHz using the 04.00 experiment configuration).<br />
<br />
<br />
[[File:Variance comparison.png|frame|Figure : Comparison of messenger method and S2hat estimator when it comes to the variance in each bin.|center]]<br />
<br />
As shown above, the messenger method beats the S2hat estimator in terms of variance per bin. We believe the main reason for this is that the S2hat estimator uses a simple weighting of 1/N to filter the maps. Since the signal plus noise simulations have a sizeable amount of BB lensing signal contained within them, the fact that we are doing a weiner filter (and thus taking into account the signal covariance) means that we would expect to get a large improvement over an estimator which only knows about noise covariance. For delensed simulations, we would expect to see less of an improvement from the messenger method over the S2hat filtering.</div>Cbischoffhttp://www.cmb-s4.org/wiki/index.php?title=Estimated_observing_efficiency_for_past_and_current_telescopes,_version_2&diff=8936Estimated observing efficiency for past and current telescopes, version 22019-05-09T17:47:25Z<p>Cbischoff: </p>
<hr />
<div>''Colin Bischoff, Yuji Chinone, Tom Crawford, Matt Hasselfield, 2018-10-23''<br />
----<br />
<br />
This posting is an update on a [[Estimated observing efficiency for past and current telescopes|previous posting from 2018-09-25]]. The goal is to try to identify any factors that lead to different observing efficiency between Atacama and South Pole.<br />
<br />
===References===<br />
We assess results from recent CMB polarization experiments that have been published in the following papers:<br />
* [http://adsabs.harvard.edu/abs/2014PhRvL.112x1101A BICEP2 2014] (150 GHz)<br />
* [http://adsabs.harvard.edu/abs/2015ApJ...811..126B BICEP2 + Keck Array 2015] (150 GHz) &mdash; this is the same dataset that was used for BICEP/Keck/Planck joint analysis<br />
* [http://adsabs.harvard.edu/abs/2016PhRvL.116c1302B BICEP2 + Keck Array 2016] (95 and 150 GHz)<br />
* [http://adsabs.harvard.edu/abs/2018arXiv181005216A BICEP2 + Keck Array 2018] (95, 150, and 220 GHz)<br />
* [http://adsabs.harvard.edu/abs/2014JCAP...10..007N ACTpol 2014] (150 GHz)<br />
* [http://adsabs.harvard.edu/abs/2017JCAP...06..031L ACTpol 2017] (150 GHz)<br />
* [http://adsabs.harvard.edu/abs/2011ApJ...741..111Q QUIET 2011] (43 GHz)<br />
* [http://adsabs.harvard.edu/abs/2012ApJ...760..145Q QUIET 2012] (95 GHz)<br />
* [http://adsabs.harvard.edu/abs/2018JCAP...09..005K ABS 2018] (150 GHz)<br />
* [http://adsabs.harvard.edu/abs/2017ApJ...848..121P POLARBEAR 2017] (150 GHz)<br />
* [http://adsabs.harvard.edu/abs/2015ApJ...807..151K SPTpol 2015] (95 and 150 GHz, but only using 150 GHz here)<br />
<br />
===Method===<br />
To investigate observing efficiency, we compare different measures of survey weight, which is defined with units of &mu;K<sup>-2</sup> and accumulates linearly with detector count or integration time.<br />
<br />
The &ldquo;tod weight&rdquo; is calculated from array sensitivity and integration time as<br />
tod_weight = &tau; / NEQ<sup>2</sup><br />
* Note that we use here a convention for NEQ that corresponds to instantaneous sensitivity to whatever combination of Q and U is being measured. By this convention, most experiments should have NEQ that is similar to NET (up to minor factors of polarization efficiency), not a factor of sqrt(2) higher.<br />
* Since survey weight accumulates linearly, we can calculate the total 150 GHz BICEP2/Keck survey weight from the most recent publication as BICEP2 2010&ndash;2012 + Keck 2012&ndash;2013 + Keck 2014 + Keck 2015.<br />
<br />
The &ldquo;bandpower weight&rdquo; is calculated from N<sub>&#x2113;</sub> and effective fsky of the BB bandpowers as<br />
bandpower_weight = 2 * 4&pi; * fsky / N<sub>&#x2113;</sub><br />
* The factor of 2 counts both EE and BB survey weight and is needed to match the NEQ convention discussed above.<br />
* N<sub>&#x2113;</sub> and effective fsky are estimated from the error bars of published bandpowers. This is discussed in more detail in a [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180810_noise/ 2018-08-10 posting]. The bandpower error bars constrain N<sub>&#x2113;</sub> / sqrt(fsky), so for experiments where we weren't able to reliably break this degeneracy it is possible to change the bandpower weight while keeping the bandpower errors fixed. This is noted explicitly on the figure for the case of ABS&mdash;we made a rough estimate of fsky = 3% but added dotted lines that range from 1.5% (lower left end) to 6% (upper right end). This issue affects the QUIET points too, but we haven't added dotted lines there.<br />
<br />
The bandpower weight represents final results after all efficiency hits while the tod weight represents accumulated sensitivity. If we fully understand all of the various efficiency factors, then we should be able to get these numbers to agree.<br />
<br />
===Results===<br />
Figure 1 below shows the bandpower / tod weight ratio vs bandpower weight, color-coded by observing frequency. For each experiment, there are two or three points spaced vertically. These all represent the same bandpowers, but count total observing time differently and arrive at different tod weights.<br />
<br />
[[File:CMB_achieved_efficiency_v2.png|frame|Figure 1: survey weight ratio vs bandpower-derived survey weight|center]]<br />
<br />
* The bottom points uses the most expansive definition of observing time, which is just the duration between when the experiment started operating and when it finished. <br />
** For BICEP2/Keck, this is just calendar years. BICEP2 ran for three years (2010 through 2012). The 2015 paper added two years of Keck Array (2012, 2013). The 2016 paper added Keck data from 2014. The 2018 paper added Keck data from 2015.<br />
** For ACTpol, the 2014 paper was based on just 94 days of operation (2013-09-11 through 2013-12-14). The 2017 paper included an additional 133 days (2014-08-20 through 2014-12-31).<br />
** For QUIET, the 2011 paper was based on 232 days of operation (2008-10-24 through 2009-06-13). The 2012 paper was based on 497 days of operation (2009-08-12 through 2010-12-22).<br />
** For ABS, the 2018 paper was based on 464 days of operation (2012-09-13 through 2013-12-21).<br />
** For POLARBEAR, the 2017 paper was based on 668 days of operation. Season 1 was May 2012 through June 2013 and season 2 was September 2013 through April 2014.<br />
** For SPTpol, the 2015 paper was based on 395 days of operation (April 2012 through April 2013).<br />
* The upper filled points attempt to count just the days spent on normal operations.<br />
** For BICEP2/Keck and SPT, we drop the austral summer deployment season that is typically spent on instrument repairs, upgrades, and calibration. BICEP2 is an expection, as it operated more or less continuously from 2010-02-15 to 2012-11-06 except for a campaign of calibrations from 2011-01-01 to 2011-03-01.<br />
** For ACTpol, we kept only 63% (45%) of the observing time from season 1 (2) to account for night-time only observations.<br />
** For QUIET, the time spent on observations is 3458 hours for 43 GHz and 7426 hours for 95 GHz, taken from the text of the respective papers. These durations include calibrations and Galactic field data, excluding only blocks of downtime due to &ldquo;occasional snow, power outages, and mechanical failures&rdquo;.<br />
** For ABS, the time spent on observations is 6723 hours, taken from the text of the paper.<br />
** For POLARBEAR, the time spent on observations is 4700 hours, taken from the text of the paper.<br />
* In some cases, there is an additional unfilled point that counts only the remaining time after cuts.<br />
** For BICEP2, we used 8.6e9 detector-seconds from Table 7 of BK-II and replaced the array sensitivity with per-detector sensitivity.<br />
** For ABS, we used 461,237 TES-hours from Table 3 of ABS 2018 and replaced the array sensitivity with per-detector sensitivity<br />
** For QUIET, we counted only hours targeting the CMB fields and used 69.4% cut efficiency at 43 GHz (Table 3 of QUIET 2011, pipeline A) and 63.5% cut efficiency at 95 GHz (Table 1 of QUIET 2012, PCL pipeline).<br />
** For POLARBEAR, we used 1400 hours of data after cuts. POLARBEAR 2017 lists 2800 hours of data passing cuts, but 50% of that data is lost from cutting to scan turnarounds.<br />
<br />
===Discussion===<br />
Our interpretation of this figure is as follows:<br />
# If we take the ratio of the two points connected by the line, this is telling us what fraction of the total number of calendar days were spent in standard science observing mode. This ratio is fairly similar for most experiments (60&ndash;65%), but it is notably high for BICEP2 (85%) and low for POLARBEAR (29%). This loss of observing efficiency is not primarily site specific, with much of the downtime due to repairs and upgrades. However, this factor probably does include some downtime due to snowstorms in Atacama while for Pole the summer deployment season conveniently overlaps with the worst observing conditions.<br />
# The next ratio is between the upper filled point and the unfilled point. This represents the loss of observation time due to data cuts (and scheduling). It is quite similar for BICEP2 (33%), ABS (34%), and POLARBEAR (30%). QUIET comes out a bit higher at 43 GHz (54%) and 95 GHz (46%), but is seems reasonable that we would cut less data at low frequencies.<br />
# Finally we can compare the unfilled points, which should include all the efficiency hits from downtime and data cuts with 1, the value that we ought to obtain if all factors are accounted for. We don't have a good explanation for this factor. Potential explanations are that the assumed array sensitivities are a bit too good or that apodized / non-uniform map coverage is inefficient in some way. The values of this factor are 79% for BICEP2, 60% for POLARBEAR, 39% for ABS (or 55%, if we assume ABS fsky=0.06), and 63% (52%) for QUIET 43 (95) GHz (but remember that QUIET could be suffering from similar fsky uncertainty as ABS).<br />
<br />
Of the three factors listed above, only #2 is clearly site-specific, yet it seems to be quite similar between BICEP/Keck, ABS, and POLARBEAR. This survey is obviously imprecise, but it provides some evidence that observing efficiency is not very different between Atacama and Pole, all else being equal. It would be an invaluable exercise if people with deep knowledge of each experiment (and access to data) could produce detailed breakdowns of the factors needed to get agreement between the accumulated tod survey weight and the bandpower-derived version.</div>Cbischoffhttp://www.cmb-s4.org/wiki/index.php?title=Simulation_and_Forecasting_Logbook&diff=8915Simulation and Forecasting Logbook2019-04-29T16:07:59Z<p>Cbischoff: /* Logbook Entries (reverse chronological) */ fixed posting date</p>
<hr />
<div>This is an index page for logbook-style postings that cover the interconnected topics of sky modeling, simulations, and forecasting for CMB-S4. <br />
<br />
Some guidelines for use:<br />
* '''Postings should include enough context''' so that a reader can jump in and figure out what is going on. It is ''not'' necessary to write an extensive introduction to every posting -- context can be in the form of links to older postings, paper citations, etc.<br />
* Postings should represent a snapshot of work in progress. It's ok to post incomplete results, but recommended that you include notes about what is missing, what you are still planning to work on, etc. <br />
* If you have work that extends or improves an old posting, you should add it as a new posting (that includes links back to the old work as appropriate). Don't update old postings, as they should provide a chronological record of progress.<br />
* On this index page, add a link to your posting with the date, a descriptive posting title, and your full name. This logbook covers a wide range of topics, so titles will be really important to keep it useful. Don't name your posting something like "Forecasting for S4"!<br />
* Links should be added in reverse-chronological order (newest at the top). Your posting can either be written up on another wiki page or it can be a link to some externally hosted webpage (useful if you want to include a javascript plots pager).<br />
<br />
<br />
== Logbook Entries (reverse chronological) ==<br />
* '''2019 April 29''': [[Fisher forecasts for inverse noise variance weighting]] (Raphael)<br />
* '''2019 April 22''': [[WAFTT results part 3]] (Raphael)<br />
* '''2019 April 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190410_closedloop_BK15_S4 Zero order closed loop test of performance based scaling - ML search] (Ben Racine)<br />
* '''2019 March 31''': [[Analysis results for configurations 30-33]] (Raphael)<br />
* '''2019 March 30''': [[Characterization of simulations for configurations 30-33]] (Raphael)<br />
* '''2019 March 26''': [[Simulations for configurations with different frequency coverage]] (Raphael)<br />
* '''2019 March 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190326_bkfinal_05 Zero order closed loop test of performance based scaling - BK15 regen power spectra] (Clem)<br />
* '''2019 March 25''': [[Deeper SAT from Chile II]] (Reijo Keskitalo and Julian Borrill)<br />
* '''2019 March 25''': [[Wider SAT from the Pole II]] (Reijo Keskitalo and Julian Borrill)<br />
* '''2019 March 25''': [[Deep SAT from the Pole]] (Reijo Keskitalo and Julian Borrill)<br />
* '''2019 March 18''': [https://cmb-s4.org/wiki/index.php/Optimal_lensing_fermilab Details on optimal lensing Fermilab presentation / 02.xx real delensing] (Marius Millea)<br />
* '''2019 March 18''': [[High cadence LAT from Chile]] (Reijo Keskitalo)<br />
* '''2019 March 18''': [[WAFTT results part 2]] (Raphael)<br />
* '''2019 March 18''': [[Wider SAT from the Pole]] (Reijo Keskitalo)<br />
* '''2019 March 8''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook//20190308_MLsearch_no85no145/ Maximum likelihood search results without 85GHz and 145GHz] (Ben Racine)<br />
* '''2019 March 3''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190303_MLsearch_bpmax_dep/ Maximum likelihood search results: dependence on the multipole range] (Ben Racine)<br />
* '''2019 February 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190220_noiseparams_bk15_forS4/ BK15 noise levels for S4 sims] (Ben Racine) <br />
* '''2019 February 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190220_S4_NET_forecasts_III/ CMB-S4 NET follow-ups II] (Denis Barkats, Ben Racine-updated on Feb 25) <br />
* '''2019 February 18''': [[Correlation of reconstructed lensing template to ideal II]] (Clem Pryke)<br />
* '''2019 February 18''': [[Fisher calcs of 04b/04c for larger value of r]] (Raphael posted by Clem)<br />
* '''2019 February 14''': [[Deeper SAT from Chile]] (Reijo Keskitalo)<br />
* '''2019 January 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190130_Matrix_first_try/ Matrix-based purification analysis: First try] (B.Racine, J.Willmert) ''Updated 2019 Feb 17th''<br />
* '''2019 January 23''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190123_S4_NET_forecasts_II/ CMB-S4 NET follow-ups I] (Denis Barkats, J. Kovac, Ben Racine-updated on Feb 25) <br />
* '''2019 January 15''': [[Correlation of reconstructed lensing template to ideal]] (Clem Pryke)<br />
* '''2019 January 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190120_dc02_ML_LT/ Maximum likelihood search results for Data Challenge 02.00 with two different lensing templates] (C. Umiltà)<br />
* '''2019 January 17''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190117_MLsearch04d/ Maximum likelihood search results for Data Challenge 04d.00, new BK14 mask reanalysis] (Ben Racine)<br />
* '''2019 January 15''': [[Noise models and sky fractions for WAFTT]] (Raphael)<br />
* '''2019 January 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190111_bkfinal_04bcd BK-style power spectra of 04/04b/04c/04d masks (adding BK14 mask)] (Clem)<br />
* '''2018 December 9''': [[Optimal Bayesian delensing progress update]] (Marius Millea) <br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181207_bkfinal_02lt BK-style power spectra of 02 with Carron lensing templates] (Clem)<br />
* '''2018 December 7''': [[Problems with PS2HAT estimator at low ell]] (Clem Pryke)<br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181116_bpbias_study Bandpower bias study] (Ben Racine)<br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181207_expval_input_ML_search Maximum likelihood search with expectation values as input] (C. Umiltà)<br />
* '''2018 November 28''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181128_toy_sims Effective sky fraction] (Clem)<br />
* '''2018 November 21''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181111_dc04_flatpriors/ Maximum likelihood search results for Data Challenge 04, v2] (Ben Racine)<br />
* '''2018 November 21''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181111_dc04_flatpriors/index_abc.html Maximum likelihood search results for Data Challenge 04b and 04c, v2] (Ben Racine)<br />
* '''2018 November 16''': [[Analytic approximation for r likelihood]] (C. Bischoff) ''Updated 2018-11-20''<br />
* '''2018 November 12''': [[Detection significance for r=0.003]] (C. Bischoff)<br />
* '''2018 November 9''': [[Bad realizations in gsync/gdust sims]] (Clem Pryke)<br />
* '''2018 November 8''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181108_dc02_ML_LT Maximum likelihood search results for Data Challenge 02.00 with an ideal lensing template] (C. Umiltà)<br />
* '''2018 November 5''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181105_toy_sims Attempt to understand sigma(r) results with different hit maps] (Clem)<br />
* '''2018 October 29''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181018_1Dmodel_tapering_study Simple 1D model to study the effect of different observation strategies on the bandpower statistics.] (Ben Racine, Victor Buza, John Kovac) ''Updated 2018 Dec 14th''<br />
* '''2018 October 29''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181029_bkfinal_02lt BK-style power spectra of 02 with ideal lensing templates] (Clem)<br />
* '''2018 October 26''': [[Checking BB purity in re-analysis for alternate masks]] (Clem Pryke)<br />
* '''2018 October 23''': [[Estimated observing efficiency for past and current telescopes, version 2]] (C. Bischoff, Y. Chinone, T. Crawford, M. Hasselfield)<br />
* '''2018 October 14''': [[Estimates of delensing efficiency]] (Raphael)<br />
* '''2018 October 14''': [[Analysis of 04, 04b, 04c simulations]] (Raphael) [[Analysis of 04, 04b, 04c simulations comp]] (Ben)<br />
* '''2018 September 30''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180930_dc04_0to9/ Maximum likelihood search results for Data Challenge 04, models 0 to 9] (Ben Racine) ''Updated 2018 Oct 2nd''<br />
* '''2018 September 30''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180930_dc04_abc_model_0123789_ML/ Maximum likelihood search results for Data Challenge 04b and 04c, model 00, 01, 02, 03, 07, 08 and 09] (Ben Racine)<br />
* '''2018 September 30''': [[Ready for delensing use lensing maps 02.00]] (Julien Carron)<br />
* '''2018 September 28''': [[Towards lensing template]] (Clem Pryke)<br />
* '''2018 September 27''': [[Lensing reconstructions 02.00]] (Julien Carron)<br />
* '''2018 September 26''': [[Lensing map reconstruction from 02.00 sims w/ and w/o foreground+inhomogeneous noise]] (Toshiya Namikawa)<br />
* '''2018 September 25''': [[Estimated observing efficiency for past and current telescopes]] (C. Bischoff)<br />
* '''2018 September 25''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180925_bkfinal_04bc BK-style power spectra of 04/04b/04c masks for 00/01/02/03/07/08/09 foreground models] (Clem)<br />
* '''2018 September 12''': [[Low ell noise from past and current telescopes]] (C. Bischoff)<br />
* '''2018 September 5''': [[Phi reconstruction on 02.00 sims III]] (Anton Baleato)<br />
* '''2018 August 31''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180831_dc04_abc_model00_07_ML_proper_bp/ Maximum likelihood search results for Data Challenge 04b and 04c, for sky models 00 and 07] (Ben Racine)<br />
* '''2018 August 31''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180831_dc04_fixed_bp/ Maximum likelihood search results for Data Challenge 04, fixed bandpasses] (Ben Racine)<br />
* '''2018 August 27''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180827_bkfinal_04 Sims with nominal Chile and Pole masks III - BK-style power spectra of 04b.YY and 04c.YY] (Clem)<br />
* '''2018 August 27''': [[Sims with nominal Chile and Pole masks II]] (Clem P.)<br />
* '''2018 August 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180826_dc04_fixed/ Maximum likelihood search results for Data Challenge 04, fixed] (V.Buza, B.Racine)<br />
* '''2018 August 24''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180824_bkfinal_04/ BK-style power spectra of v04.00-06 sims (CDT report config) FIXED] (Caterina Umilta)<br />
* '''2018 August 24''': [[Amplitude modulated Gaussian dust sims]] (Clem P.)<br />
* '''2018 August 17''': [[Sims with nominal Chile and Pole masks]] (Clem P.)<br />
* '''2018 August 10''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180810_noise/ Achieved performance roundup] (C. Bischoff)<br />
* '''2018 August 7''': [[Pre-reference-design noise specifications for large-aperture forecasting]] (Tom Crawford, Matthew Hasselfield, Gil Holder, Lloyd Knox)<br />
* '''2018 August 6''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180805_s4opt/ Performance-based Fisher optimization for CMB-S4, 44cm vs 52cm aperture (w/ high-res/low-res 20 GHz)] (V.Buza)<br />
* '''2018 July 9''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180708_dc04/ Maximum likelihood search results for Data Challenge 04] (V.Buza)<br />
* '''2018 July 6''': [[Phi reconstruction on 02.00 sims II]] (Anton Baleato and Clem Pryke)<br />
* '''2018 June 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180611_s4opt/ Performance-based Fisher optimization for CMB-S4, 44cm aperture] (V.Buza) -- see corrected August 6th Update!<br />
* '''2018 June 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180609_S4_noise_simulation_arbitrary_coverage/ Recipe to generate performance based S4 simulations with arbitrary sky distribution (in progress)] (B.Racine, V.Buza)<br />
* '''2018 April 29''': [[Phi reconstruction on 02.00 sims]] (Anton Baleato)<br />
* '''2018 April 25''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180425_r_equivalent_maps/ Smallfield r-equivalent Maps] (Kenny Lau)<br />
* '''2018 April 4''': [[Sky masks for simulations III]] (Clem P.)<br />
* '''2018 March 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180323_bkfinal_04/ BK-style power spectra of v04.00-06 sims (CDT report config) BROKEN] (Clem)<br />
* '''2018 March 16''': [[ILC noise for large apertures at CDT noise levels]] (Raphael Flauger posted by Clem)<br />
* '''2018 March 16''': [[Sky masks for simulations II]] (Clem P.)<br />
* '''2018 February 19''': [[Sky masks for simulations]] (Clem P.)<br />
* '''2018 February 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180218_s4opt/ Performance-based Fisher optimization for CMB-S4, v3] (Victor Buza)<br />
* '''2018 February 7''': [[Sim map sets to demonstrate "real delensing" (02.00 and 02.09)]] (Clem P.)<br />
* '''2018 February 6''': [[Data Challenge Map Sets 04.YY]] (Clem P.)<br />
* '''2017 December 8''': [[Vansyngel Model]] (Clem P.)<br />
* '''2017 November 6''': [[Bandpass Convention - What does flat mean]] (Clem P.) - followup notes added Nov 20<br />
* '''2017 September 27''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170927_dc02/ Maximum likelihood search results for Data Challenge 02] (Bischoff, Buza, Willmert)<br />
* '''2017 September 13''': [[Bias on r from Band Center Errors]] (Palladino, Willmert, Bischoff)<br />
* '''2017 September 8''': [[Checking dust decorrelation in Raphael MHD based dust sim]] (Clem P.)<br />
* '''2017 September 6''': [[New NET Calculator and Validation]] (Denis Barkats)<br />
* '''2017 September 1''': [[Resolution at 20 GHz]] (Raphael)<br />
* '''2017 August 31''': [[Bias on r from additive systematics]] (Palladino, Willmert, Bischoff)<br />
* '''2017 August 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170818_bkfinal_03.00/ BK-style power spectra for 1000 realizations of v03.00,.03 CMB-S4 simulation maps] (Justin Willmert)<br />
* '''2017 August 18 ''': [[Neff_and_Beam_Calibration| Neff and Beam Calibration]] (Dan)<br />
* '''2017 August 18''': [[Ideal delensing templates from flat-sky QE, first pass]] (Kyle Story)<br />
* '''2017 August 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170818_HR/ High-Res studies for CMB-S4 (draft, v2)] (Victor Buza)<br />
* '''2017 August 18''': [[Comments from Anthony Challinor and Rupert Allison regarding the impact of Galactic Foregrounds on lensing]] (Neelima)<br />
* '''2017 August 11''': [[Joint Synchrotron and Dust Maps from Simulations]] (B. Hensley)<br />
* '''2017 August 9''': [[Dust Emission From Halos]] (Jim & Jean-Baptiste)<br />
* '''2017 August 9''': [[SZ Clusters update]] (Mat & Nick)<br />
* '''2017 August 4''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170804_HR/ High-Res studies for CMB-S4 (preliminary draft)] (Victor Buza); perhaps a reference of interest https://arxiv.org/abs/1707.02259<br />
* '''2017 July 10''': [[Additive systematics for data challenge 03]] (Bischoff, Palladino, Buza, Kovac)<br />
* '''2017 July 6''': [[Detection significance and sky fraction, dust decorrelation]](Raphael)<br />
* '''2017 July 3''': [[Toy highly decorrelated dust model]] (Clem P.)<br />
* '''2017 June 27''': [[Checking dust decorrelation in models d1/d4/d7 and hipdt]] (Clem P.)<br />
* '''2017 June 23''': [[Dust_delensing_firstlook|Dust delensing update]] (Alex)<br />
* '''2017 June 23''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170623_bkfinal_02.00/ BK-style power spectra for 1000 realizations of v02.00–06 CMB-S4 simulation maps] (Justin Willmert) ''Updated 2017 Sep 08''<br />
* '''2017 June 22''': [[Warm-up exercise for delensing]] (Raphael)<br />
* '''2017 June 19''': [[SZ Clusters update]] (Mat, Nick)<br />
* '''2017 June 11''': [[Notes from May 31 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 June 9''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170525_s4syst/ Introducing systematics for CMB-S4] ((Victor Buza), with input from Colin Bischoff, John Kovac)<br />
* '''2017 June 9''': [[Dust_delensing_firstlook]] (Alex)<br />
* '''2017 June 9''': [[r-forecasting: high and low ell coordination|r-forecasting: update on high and low ell coordination]] (Neelima+Colin Hill writing)<br />
* '''2017 June 1''': [[Residuals for DC 01.01 and DC 01.02]] (Raphael)<br />
* '''2017 June 1''': [[Levels of foregrounds in Gaussian and PySM simulations]] (Raphael)<br />
* '''2017 May 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170511_s4dc1/ S4 DC 01.xx analysis, v2] (Victor Buza, Colin Bischoff, Justin Willmert)<br />
* '''2017 May 26 ''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170411_bkfinal_01.00/ Updated v01.02 in "BK-style power spectra for 1000 realizations of v01.00–02 CMB-S4 simulation maps"] (Justin Willmert)<br />
* '''2017 May 15''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170515_chkS4/ N_ell spectra for CMB-S4 DC2.0] (Victor Buza)<br />
* '''2017 May 15''': [[Rev 2 PySM a2d4f1s3 maps]] (Clem P.)<br />
* '''2017 May 12''': [[r-forecasting: high and low ell coordination|r-forecasting: high and low ell coordination]] (lensers writing)<br />
* '''2017 May 8''': [[Checking PySM maps]] (Clem P.)<br />
* '''2017 May 2''': [[Notes from April 26 telecon on science requirements for clusters/high-ell]] (Steve)<br />
* '''2017 May 1''': [[r-forecasting: delensing discussion|r-forecasting delensing discussion]] (Neelima and Blake)<br />
* '''2017 April 28 ''': [[Update_on_Neff_Forecasts| Update on Neff Forecasts]] (Dan)<br />
* '''2017 April 26 ''': [http://www.cosmo.bnl.gov/www/msyriac/web/work/sigma8plots.html Update on cluster number counts forecast including w_a] (Mat and Nick)<br />
* '''2017 April 21 ''': [[lensing-DE|Update on a lensing-based DE forecast]] (Jo, Siddharth)<br />
* '''2017 April 18 ''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170411_bkfinal_01.00/ BK-style power spectra for 1000 realizations of v01.00–02 CMB-S4 simulation maps] (Justin Willmert)<br />
* '''2017 April 18 ''': [[S4-Lensing|S4 measurement requirements for neutrino mass and delensing - first pass]] (Neelima/Blake)<br />
* '''2017 April 17 ''': [[HiDPol|HI-based dust polarization model for r forecasts]] (Tuhin)<br />
* '''2017 April 05 ''': [[lensing-DE|Notes on one path to lensing-based DE forecasts]] (Jo)<br />
* '''2017 April 05 ''': [[Notes from April 5 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 April 05''': [https://cmb-s4.org/CMB-S4workshops/images/Sigma8_z_prep.pdf Sigma8(z) SPT clusters (placeholder) ] (S Bocquet)<br />
* '''2017 April 04''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170404_s4opt/ Updated Performance-based Fisher optimization for CMB-S4 (using bands v1.99)] (Victor Buza, Updated 2017.04.21)<br />
* '''2017 March 31 ''': [[Data Challenge analysis - DC1.0, DC1.1, DC1.2]] (Raphael)<br />
* '''2017 March 30 ''': [[Notes from March 28 telecon on science requirements for clusters/high-ell]] (Jim & Steve)<br />
* '''2017 March 29''': [[CMB-S4 frequency bands v1.99]] (John Kovac, Band-definition working group)<br />
* '''2017 March 28''': [[Adding higher res delensing "band"]] (Clem P.)<br />
* '''2017 March 27''': [[01.01 sim input maps - first try]] (Clem P.)<br />
* '''2017 March 23''': [[01.00 sim input maps]] (Clem P.)<br />
* '''2017 March 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170221_S4_NET_forecasts/ S4 Band sensitivity comparison follow-up] (Denis Barkats, John Kovac)<br />
* '''2017 March 17''': [http://users.physics.harvard.edu/~buza/20170317_s4dc1/ S4 DC1.0 analysis] (Victor Buza, Colin Bischoff, Justin Willmert)<br />
* '''2017 March 17 ''': [[Media:Telecon_03172017_optimization_for_CMBS4.pdf]]: Optimization methodology for SO (Josquin)<br />
* '''2017 March 16 ''': [[ P_k_science_case| P(k) science case]] (Colin, Simone, Nick, David)<br />
* '''2017 March 15 ''': [[Notes from March 15 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 March 15 ''': [[CMB halo lensing sensitivity as a function of map sensitivity and resolution]] (Jim & Jean-Baptiste)<br />
* '''2017 March 15 ''': [[w and gamma | w and Delta gamma constraints from sigma_8 (z)]] (Mat & Nick)<br />
* '''2017 March 10 ''': [[Notes from March 8 telecon on science requirements for clusters/high-ell]] (Jim & Steve)<br />
* '''2017 March 8 ''': [[reionization_requirements| Reionization science]] (Simone & Marcelo)<br />
* '''2017 March 8 ''': [[High ell topics | High ell topics ]] (Jim)<br />
* '''2017 March 8 ''': [[SZ_s8_z | sigma 8 of z constraints ]] (Mat, Nick)<br />
* '''2017 March 8 ''': [[Szcounts | Number counts update for 1.0', 1.5', 2.0']] (Nick, Mat)<br />
* '''2017 March 8 ''': [[SZastro | SZ astrophysics with DESI ]](Nick, Simone, Emanuel, David)<br />
* '''2017 February 24''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170224_cmbs4_dc1_final/ BK-style processing of DC1.0 maps to spectra] (Justin Willmert, Colin Bischoff)<br />
* '''2017 February 15 ''': [[Extragalactic lensing sims| Update on extragalactic phase-2 lensing sims]] (Marcelo, George, Dick, others)<br />
* '''2017 February 15 ''': [[Plan for next Galactic Phase-2sims| Plan for next Galactic phase-2 sims]] (Jo, Ben)<br />
* '''2017 February 10 ''': [[Resolution of foreground-cleaned map]] (Mat, Neelima, Blake, Alex, others)<br />
* '''2017 February 10 ''': [[Nongaussian dust in lensing]] (Alex, Mat, Neelima, Blake, others)<br />
* '''2017 January 30''': [[Aliased power in noise maps]] (Bischoff, Updated 2017-02-02)<br />
* '''2017 January 23''': [[CMBS4 Band Sensitivity Comparison]] (Charlie Hill)<br />
* '''2017 January 12''': [http://bicep.rc.fas.harvard.edu/cbischoff/20170112_data_challenge_1/ Maps for CMB-S4 data challenge 1] (Bischoff, Pryke, Buza)<br />
* '''2016 December 21''': [http://users.physics.harvard.edu/~buza/20161220_chkS4/ N_ell spectra for the CMB-S4 data challenge, and updated &sigma;(r) checkpoints] (Victor Buza, Updated 2017.02.01)<br />
* '''2016 November 30''': [[First steps to sim input maps]] (Clem P.)<br />
* '''2016 November 4''': [[Tophat bands for Data Challenge]] (Bischoff)<br />
* '''2016 July 8''': [[fsky|Dependence of foregrounds on sky fraction]] (Raphael)<br />
* '''2016 July 8''': [[SciBookPowspecTheoryFig|Three choices for Science Book Figure 5 (theory power spectrum & current BB points)]] (Tom C.)<br />
* '''2016 July 8''': [http://users.physics.harvard.edu/~buza/20160707_s4plots/ S4 Inflation Chapter Plot Suggestions, V2] (Victor Buza)<br />
* '''2016 July 6''': [[w_cosntraint|Preliminary w constraint]] (Alessandro)<br />
* '''2016 June 24''': [[nsr|Preliminary ns-r plot for discussion]] (Raphael)<br />
* '''2016 June 16''': [[DelensingImpact| Impact Of Delensing On sigma(r)]] (Neelima/Mat)<br />
* '''2016 June 16''': [http://users.physics.harvard.edu/~buza/20160616_s4plots/ S4 Inflation Chapter Plot Suggestions] (Victor Buza)<br />
* '''2016 June 10''': [[MapBasedRb| Map-based &sigma;(r) forecasts V2]] (David/Jo/Ben)<br />
* '''2016 June 3''': [http://users.physics.harvard.edu/~buza/20160531_fisher/ &sigma;(r) forecasting checkpoints, V2] (Victor Buza)<br />
* '''2016 June 3''': [[ BTTfixedeffort | Forecasts for fnl BTT beam/fixed effort]] (Daan)<br />
* '''2016 May 31''': [[ForecastPatchyReion| Forecasts for patchy reionization]] (Vera, Alex, Nick)<br />
* '''2016 May 26''': [[Forecasting | Forecasts on neutrino mass]] (Nam, Mat, Neelima)<br />
* '''2016 May 26''': [[ KSZ| Forecasts on kSZ S/N]] (Simone, Emmanuel, Colin)<br />
* '''2016 May 26''': [[ Forecastfiso_planck| Forecast on correlated and anti-correlated CDM isocurvature f_iso]] (Kimmy, Cora, updated with plots 20160602)<br />
* '''2016 May 24''': [[ BTTNoiseBeam | Forecasts on fnl BTT beam/FWHM]] (Daan)<br />
* '''2016 May 22''': [[ ForecastAxions| Update on the axion isocurvature constraints for changing sensitivity and resolution]] (Renee)<br />
* '''2016 May 21''': [[ Forecastpann| Forecast on dark matter annihilation parameter p_ann]] (Kimmy, Cora)<br />
* '''2016 May 20''': [[NeffNoiseBeam| Forecasts on Neff and Yp]] (Joel, Alex)<br />
* '''2016 May 20''': [[ForecastEDE| Forecasts on Early Dark Energy]] (Erminia)<br />
* '''2016 May 20''': [[ForecastCompIsocurv| Forecasts on compensated isocurvature varying sensitivity, resolution and sky coverage]] (Julian, Ely)<br />
* '''2016 May 20''': [[ForecastBirefring| Forecasts on birefringence varying sensitivity and resolution]] (Vera, Alex)<br />
* '''2016 May 20''': [[ForecastStrings| Forecasts on string tension varying sensitivity and resolution]] (Renee)<br />
* '''2016 May 20''': [[RobustForecast| Cosmological forecasts including component separation and iterative delensing]] (Stephen Feeney and Josquin Errard)<br />
* '''2016 May 19''': [[MapBasedR| Map-based &sigma;(r) forecasts]] (David A.)<br />
* '''2016 May 18''': [[Shear_calibration_LSST|LSST shear calibration with CMB S4]] (Emmanuel Schaan)<br />
* '''2016 May 13''': [http://users.physics.harvard.edu/~buza/20150505_fisher/ &sigma;(r) forecasting checkpoints] (Victor Buza)<br />
* '''2016 May 13''': [[NonGaussianitiesTTT| CMBS-4 forecasts local and equilateral scalar Ngs using TTT]] (daan)<br />
* '''2016 May 13''': [[ForecastingSims|Simulations for r forecasts]] (Jo/Ben/David)<br />
* '''2016 May 6''': [[DMInteractionsComplementarity|DM interactions: complementarity]] (Vera)<br />
* '''2016 May 6''': [[Scenarios| Scenarios]] (Scott, Vera)<br />
* ''' 2016 May 3''': [[ForecastAxions |Effect of S4 specs on axion density parameters]] (Renee)<br />
* '''2016 April 30''': [[ForecastNu| Effect of S4 specs on neutrino parameters]] (Erminia)<br />
* '''2016 April 28''': [http://web.stanford.edu/~wlwu/posting/20160421_lensres/ Delensing residuals with low-ell foregrounds] (Kimmy Wu)<br />
* '''2016 April 28''': [[NonGaussianities| CMBS-4 forecast for tensor NGs]] (daan)<br />
* '''2016 April 19''': [[ForecastingStep1| Checking basic parameters for nominal case]] (Jo + multiple authors)<br />
* '''2016 April 5''': [[Forecasting|Setting up non-r Fisher-based parameter forecasts]] (Jo + others)<br />
* '''2016 March 31''': [http://users.physics.harvard.edu/~buza/20150331_fisher/ Fisher projections for &sigma;(r) based on achieved performance] (Victor Buza)<br />
* '''2016 January 27''': [https://cmb-s4.org/CMB-S4workshops/index.php/File:sptpol_ptsrc_polfrac_500d.pdf Quick estimate of mean-squared polarization fraction for SPTpol sources] (Tom Crawford)</div>Cbischoffhttp://www.cmb-s4.org/wiki/index.php?title=Fermilab-2019:_Cosmology_with_CMB-S4&diff=8566Fermilab-2019: Cosmology with CMB-S42019-03-14T16:51:02Z<p>Cbischoff: /* Thursday March 14th */</p>
<hr />
<div><br />
== Workshop overview ==<br />
<br />
The Fermilab workshop continues a successful series of meetings bringing together the CMB experimental and theoretical community to plan a coordinated, stage-4 ground-based CMB experiment. <br />
<br />
The meeting will be held at Fermilab, March 13-15, 2019. The first 2 days will be a collaboration meeting and the 3rd will be our first project meeting; everyone is welcome to all 3 days.<br />
<br />
== Meeting Info & Registration ==<br />
<br />
[http://indico.fnal.gov/e/cmbs4collaboration2019 Official Workshop Website: Registration, Participants, Hotels, Logistics].<br />
<br />
'''Location: IARC Building at Fermilab''' http://iarc.fnal.gov/<br />
<br />
'''Remote Connection Information: '''<br />
<br />
'''Zoom link: https://fnal.zoom.us/j/356003665'''<br />
<br />
One tap mobile:<br><br />
+16465588656,,356003665# US (New York)<br><br />
+16699006833,,356003665# US (San Jose)<br />
<br />
Dial by your location: <br />
+1 669 900 6833 US (San Jose)<br><br />
Meeting ID: 356 003 665<br><br />
Find your local number: https://zoom.us/u/acu5oQsITY<br />
<br />
Slack channel #fermilab2019 on the CMB-S4 workspace, or use https://cmb-s4.slack.com/messages/CCMNTUDC1<br />
<br />
== About This Wiki==<br />
<br />
As for previous workshops, we will use this wiki to organize the sessions, to capture the input from them, and to develop next steps. Participants are encouraged to edit the wiki directly, including uploading plots or a few slides.<br />
<br />
Hints for formatting this wiki can be found [https://www.mediawiki.org/wiki/Help:Formatting here]<br />
<br />
----<br />
<br />
== Agenda ==<br />
<br />
=== Wednesday March 13th ===<br />
<br />
'''Morning Sessions Chair: Brad Benson'''<br />
<br />
'''08:30 Welcome and Spokesperson Update'''<br />
* '''08:30''' FNAL Welcome (Nigel Lockyer) and Meeting Logistics (Brad Benson) [[Media:2019_03_CMBS4_Fermilab_Welcome.pdf]]<br />
* '''08:45''' Spokesperson update (Julian Borrill, John Carlstrom) [https://docs.google.com/presentation/d/1Hjsw0zmFjQRpRM52sC1lbfgH1FfZV1ntN9Bp_ofR9zE Slides]<br />
* '''09:15''' Agency update (Drew Baden, Nigel Sharp)<br />
<br />
'''09:30 Collaboration Update '''<br />
* '''09:30''' Governing Board (Nils Halverson) [[Media:CMB-S4_GB_Activities_Fermilab_Meeting_2019-03-12.pdf]]<br />
* '''09:45''' Membership (John Ruhl) [https://docs.google.com/presentation/d/1_OzqTXBoGqSZn2BYjpDAt0gx6ZLfKaxGyr0wa4Q9w24/edit?usp=sharing Slides]<br />
* '''10:00''' - Publication and Speakers (Kevin Huffenberger) [https://docs.google.com/presentation/d/1gt12BffbFeRXJL9J9h7bX7_Pf8jLi3Erry2MSxCVpyk/edit?usp=sharing Slides]<br />
<br />
'''10:15''' ''Coffee Break''<br />
<br />
'''10:45''' DSR Review and Science'''<br />
* '''10:45''' Summary of DSR review and planned response (Julian Borrill) [https://docs.google.com/presentation/d/1vgqQwN9Q54XiBUzB42H2Hlq6cE7BO6UGLnKGc-z70N0 Slides]<br />
* '''11:05''' r (Clem Pryke) [https://docs.google.com/presentation/d/18UsMRhIHlk8mrWkIuoSwpLPfTPXZbwceW0EhQ4ixGQ8 Slides]<br />
* '''11:15''' Neff (Joel Meyers) [[Media:Light_Relics_Fermilab_2019.pdf]]<br />
* '''11:25''' Mass mapping (Lindsey Bleem) [https://cmb-s4.org/wiki/images/Mass_mapping_31919_v1.pdf Slides]<br />
* '''11:35''' Gas mapping (Nick Battaglia) [[Media:CMBS4GasMappingFNAL19.pdf]]<br />
* '''11:45''' Transients (Nathan Whitehorn) [[Media:CMBS4TransientsFNAL19.pdf]]<br />
* '''11:55''' Science case to measurements requirements (Gil Holder) [https://docs.google.com/presentation/d/1bRtYR_Od-lI_xwKaR5RKCabj6jCCt-3zV8XkFkQIkBs/edit?usp=sharing Slides][https://drive.google.com/open?id=1HPBnf098ErUUdqQjXpCddColre0iHXhP pdf]<br />
* '''12:15''' Measurement requirements to technical requirements (Jeff McMahon) [https://docs.google.com/presentation/d/1w60FJp0fabUBF_OLFIbEaDntlPBx7K3DeDq_0GfGTZo/edit#slide=id.g51c952aeca_1_28 Slides]<br />
<br />
'''12:30 Lunch & JSAC (Junior Scientist) Event'''<br />
<br />
* Junior Scientist Event - register here: https://goo.gl/forms/wdQ0wl5hEh2cLUVl1 <br />
<br />
'''Afternoon Sessions Chair: Abby Vieregg'''<br />
<br />
'''1:30 DSR Reference Design'''<br />
* '''1:30''' Reference design overview (Steve Padin) [[Media:CMBS4RefDesignOverview.pdf]]<br />
* '''1:50''' SATs (John Kovac) [https://docs.google.com/presentation/d/1pLFNJIJPVincoF-KPp2jQBPfDkcxcgY9SQAoGyPXgAI/edit#slide=id.p1 Slides]<br />
* '''2:05''' LATs (Mike Niemack) [[Media:LATs_20190313.pdf]]<br />
* '''2:20''' Detectors and readout (Clarence Chang) [[Media:CMB-S4_FNAL_DSR_DR.pdf]]<br />
* '''2:35''' SItes and Integration & commissioning (Brad Benson, Sara Simon) [https://docs.google.com/presentation/d/1gIkb_21oy1SM__cBeLmZmZnlhNUzowRRV6h8TJu3m08/edit?usp=sharing Slides]<br />
* '''2:50''' SAT siting decision tree (John Ruhl) [https://docs.google.com/presentation/d/1NL06LQ2te-bo3LF350T9Lf2D8lTcWqV_AVqjGNqB-Sk/edit?usp=sharing Slides]<br />
* '''3:10''' Budget and schedule (Brenna Flaugher) [[Media:BF-March-Collab-schedule-slides-1.pdf]]<br />
'''3:30''' ''Coffee Break''<br />
<br />
'''4:00 NSF MSRI Proposals'''<br />
* '''4:00''' CMB-S4 MSRI-1 (5+5) (John Carlstrom) [[Media:MSRI-R1-Carlstrom.pdf]]<br />
* '''4:10''' SO MSRI-1 (5+5) (Mark Devlin/Kam Arnold) [[Media:MSRI1-for-S4.pdf]]<br />
* '''4:20''' SPO MSRI-1 (5+5) (John Kovac) [[Media:SPO_MSRI_scope_LNAL_Mar2019.pdf]]<br />
* '''4:30''' CCAT-prime MSRI-1 (5+5) (Mike Niemack) [[Media:CCATprime_CMBS4_20190313r.pdf]]<br />
<br />
'''4:40 Fireslides (Chair: Sasha Rahlin) [[Media:fireslides.pdf]]'''<br />
<br />
'''5:30 Group photo at Wilson Hall'''<br />
<br />
'''5:45 Poster Session at Wilson Hall'''<br />
<br />
'''6:00-8:00 Social event and food at Wilson Hall'''<br />
<br />
----<br />
<br />
=== Thursday March 14th ===<br />
<br />
'''08:30 Path to CD-1 / PDR'''<br />
* '''8:30''' Path to CD-1 / PDR (John Carlstrom, Julian Borrill)[[Media:Path_To_CD-1_PDR.pdf]]<br />
** Reference Material: [[File:DOE_Order_413-3B.pdf]]<br />
** Reference Material: [[File:LargeFacilitiesManual_nsf17066.pdf]]<br />
** Reference Material: [[File:CMB-S4_DesignDecisionPrinciples-v190228.pdf]]<br />
* '''9:15''' Project Perspectives (Charles Lawrence) [[Media:TheProjectPerspective.pdf]]<br />
* '''9:30''' Questions and Discussion<br />
<br />
'''10:00''' ''Coffee Break''<br />
<br />
* '''10:30''' Interactive Session: Path to Baseline Design (Chairs: Jeff McMahon, Abigail Vieregg) [https://docs.google.com/presentation/d/1P2AsQkPJPP_2y6clK11aPDemBu0jRV4cyYtfQlQ4edo/edit#slide=id.g51c90b7fcc_0_0 Slides], [https://docs.google.com/presentation/d/1OOaYpTe9e4XSfV3fMlobDwlTSsLOnQkVJQ7imFTwhP8 Julian slides]<br />
** [https://docs.google.com/document/d/1m1gj34O_8ve9GJ2i1oaYAyAD-N18TzNaCIQ0S3H0z9M/edit Notes]<br />
** Working group leads present timeline for decision making <br />
** Collated current list of R&D priorities (Technical Coordinators)<br />
** Discuss list of R&D items that funding was requested from DOE in February (Brenna Flaugher) [[Media:BF-March-Collab-R&D.pdf]]<br />
<br />
'''12:30 Lunch'''<br />
<br />
'''1:30 Submitted Talks (Chair: Adam Anderson)'''<br />
*'''1:30''' Modulations of the CMB (Daniel Grin)[[File:S4_modulation_2019_grin.pdf]]<br />
* '''1:50''' Non-Gaussian information in the small-scale CMB: from lensing to galaxy velocities (Simone Ferraro)<br />
* '''2:10''' CMB-S4 Delensing (Marius Milea)<br />
* '''2:30''' Update on uMUX R&D towards CMB-S4 (Zeesh Ahmed)<br />
* '''2:50''' Recent Advances in Next-Generation Frequency-Multiplexed TES readout (Tijmen de Haan) <br />
* '''3:10''' Demonstration of the low-l performance and control of systematic errors for Polarbear-1 (Neil Goeckner-Wald) [[Media:S4_March_Polarbear.pdf]]<br />
<br />
'''3:30''' ''Coffee Break''<br />
<br />
* '''4:00''' Update on European coordination for ground-based CMB experiments (Carlo Baccigalupi)<br />
<br />
'''4:30''' ''Collaboration Wrap-up (Spokespeople)''<br />
<br />
----<br />
<br />
=== Friday March 15th ===<br />
<br />
'''8:30 Project Day'''<br />
* '''8:30''' Integrated project plan (Jim Yeck)<br />
* '''9:00''' Preparations for DOE/CD-1 and NSF PDR (Mark Reichanadter)<br />
* '''9:30''' Critical path, technical decision timeline, design reviews (Brenna Flaugher)<br />
* '''10:00''' Cost, schedule, contingency overview (Kathy Bailey)<br />
<br />
'''10:30''' ''Coffee Break''<br />
<br />
* '''10:45''' preliminary Project Execution Plan (pPEP) Session (Jim Yeck)<br />
** '''11:00''' pPEP Project Governance & Project Office (Jim Yeck)<br />
** '''11:15''' pPEP Agency Scope & Responsibilities (Jim Yeck)<br />
** '''11:30''' Institutional Roles (Jim Yeck)<br />
* '''11:45''' Systems engineering and risk status (Zeesh Ahmed, Nadine Kurita)<br />
<br />
'''12:15''' '''Lunch and Sidet Tours'''<br />
<br />
'''1:30''' <br />
* '''1:30''' R&D plan and priorities (Brenna Flaugher)<br />
* '''2:00''' Interm Integrated project office (JIm Yeck)<br />
* '''2:15''' Technical coordination plans (Jeff McMahon, Abigail Vieregg)<br />
* '''2:45''' In-kind contributions (Julian Borrill)<br />
* '''3:00''' Detectors and readout - Discussion of next steps<br />
* '''3:15''' Site infrastructure - Discussion of critical path and next steps (Brad Benson)<br />
<br />
* '''3:45''' Project wrap-up<br />
<br />
'''17:00''' End of meeting</div>Cbischoffhttp://www.cmb-s4.org/wiki/index.php?title=Speakers_bureau_talks_list&diff=8169Speakers bureau talks list2019-01-11T19:04:47Z<p>Cbischoff: /* Past talks */</p>
<hr />
<div>===Proposed talks===<br />
<br />
{|class="wikitable"<br />
! Announced !! Date !! Venue !! Speaker !! Title/Topic !! Abstract !! Slides<br />
<!-- Generic Template <br />
|- <br />
| 01 Jan 2021 <br />
| Fancypants Conference <br />
| Postdoc McSpeaker <br />
| CMB-S4 strikes back<br />
| In this talk I will present many, many wonderful things about CMB-S4, and the many, many wonderful people who contribute. <br />
| [[Media:myslides.pdf]]<br />
--><br />
|}<br />
<br />
===Approved talks===<br />
<br />
{|class="wikitable"<br />
! Announced !! Date !! Venue !! Speaker !! Title/Topic !! Abstract !! Slides<br />
<!-- Generic Template <br />
|- <br />
| 25 May 2018<br />
| 4-11 July 2018<br />
| ICHEP 2018, Seoul<br />
| Plenary <br />
| Masashi Hazumi <br />
| Plenary talk on CMB cosmology<br />
| <br />
| [[Media:myslides.pdf]]<br />
--> <br />
<br />
<br />
|- <br />
| <br />
| 29 November - 1 December 2018 <br />
| Novel Instrumentation for Fundamental Physics Workshop, Puerto Rico<br />
https://indico.cern.ch/event/748721/<br />
| Clarence Chang<br />
| Update on the ongoing activities<br />
| <br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
|}<br />
<br />
===Past talks===<br />
<br />
{|class="wikitable"<br />
! Announced !! Date !! Venue !! Speaker !! Title/Topic !! Abstract !! Slides<br />
<br />
|-<br />
|<br />
| 7 December 2019<br />
| AAS 223, Seattle<br />
| Colin Bischoff<br />
| The search for primordial gravitational waves with CMB polarization<br />
| Observations of Cosmic Microwave Background B-mode polarization at large angular scales are a uniquely powerful method to search for primordial gravitational waves, such as those predicted by theories of inflation. A major milestone would be to either detect this signature of gravitational waves or else to set an upper limit on the tensor-to-scalar ratio, r < 0.001, which would rule out the most compelling models of large-field inflation. This goal will be met by Stage-3 experiments currently coming online, the CMB Stage-4 project planned for next decade, as well as new balloon-borne and satellite telescopes. Galactic foregrounds and gravitational lensing of E-mode polarization pose major challenges for these measurements, but are already being addressed by current projects. I will discuss the goals and common design features of experiments targeting the primordial gravitational wave signal, as well as forecasts developed for CMB Stage-4.<br />
| [[Media:20190107_bischoff_aas.pdf]]<br />
<br />
|- <br />
| <br />
| 22-24 September 2018<br />
| International Symposium on Cosmology and Ali CMB Polarization Telescope, Shanghai<br />
https://indico.leeinst.sjtu.edu.cn/event/44/overview<br />
| Peter Timbie<br />
| CMB-S4 overview and a general discussion of detector development<br />
| <br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
|- <br />
|<br />
| 15-18 October 2018<br />
| CMB Foregrounds, Tenerife <br />
http://www.iac.es/congreso/cmbforegrounds18/<br />
| Julian Borrill <br />
| CMB-S4 overview<br />
| <br />
| [[Media:myslides.pdf]]<br />
<br />
|- <br />
|<br />
| 4-9 November 2018<br />
| 8th KIAS Workshop on Cosmology and Structure Formation<br />
http://home.kias.re.kr/cosmology2018/<br />
| Francois Bouchet <br />
| CMB-S4 overview<br />
| <br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
<br />
<br />
<br />
|- <br />
| <br />
| <br />
| Recontres Du Vietnam <br />
| Raphael Flauger<br />
| Plenary talk, including CMB-S4 <br />
| <br />
| [[Media:myslides.pdf]]<br />
|- <br />
|<br />
| 14-21 July, 2018<br />
| COSPAR, Pasadena<br />
| John Carlstrom<br />
| The Next Generation Ground-Based Cosmic Microwave Background Experiment, CMB-S4<br />
| <br />
Measurements of the CMB have driven our understanding of the universe and the physics that govern its evolution from primordial quantum fluctuations to its present state. They provide the foundation for the remarkable 6-parameter cosmological model, ΛCDM, which fits all cosmological data, although there are some tensions that may possibly hint at new physics. Far from being the last word in cosmology, the model raises deep questions: Is Inflation correct? What is its energy scale? What is the dark matter? What is the nature of dark energy? Are there light sterile neutrinos, or other light relics? This talk will describe progress on the next generation ground-based CMB experiment, CMB-S4, that is being designed to have sufficient sensitivity and control of systematics to make breakthroughs in many of these areas, i.e., to cross critical thresholds in parameter values or show that ΛCDM is incomplete.<br />
| [[Media:E1-2-0023-18-Carlstrom-Posted.pdf]]<br />
<br />
<br />
<br />
<br />
|- <br />
| <br />
| 4-11 July 2018<br />
| ICHEP 2018, Seoul<br />
| Masashi Hazumi <br />
| Plenary talk on CMB cosmology<br />
|<br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
<br />
<br />
|- <br />
| 1 Jun 2018<br />
| 1-7 July 2018 <br />
| Marcel Grossman Meeting <br />
| Carlo Baccigalupi<br />
| The Status of the CMB Stage IV Experiment<br />
| Abstract: The 'Stage-4' ground-based cosmic microwave background (CMB) experiment, CMB-S4, consists of dedicated telescopes equipped with highly sensitive superconducting cameras operating at the South Pole, the high Chilean Atacama plateau, and possibly northern hemisphere sites. CMB-S4 will be designed to cross critical thresholds in testing inflation, determining the number and masses of the neutrinos, constraining possible new light relic particles, providing precise constraints on the nature of dark energy, and testing general relativity on large scales. In this contribution, we review the status of the project.<br />
| [[Media:Carlo_Baccigalupi_S4_MGM15.pdf]]<br />
[[Media:Carlo_Baccigalupi_S4_MGM15.odp]]<br />
<br />
<br />
<br />
<br />
|- <br />
| <br />
| 19 Jun 2018 <br />
| POLAR2018<br />
| John Carlstrom <br />
| Status and Future of Cosmic Microwave Background Measurements from Antarctica <br />
| <br />
| [[Media:E1-2-0023-18-Carlstrom-Posted.pdf]]<br />
<br />
<br />
<br />
|- <br />
| <br />
| 17-22 June 2018<br />
| Workshop: WHIM and Cluster Outskirts: Lost and Found Baryons in the Local Universe, UA-Huntsville<br />
| Jim Bartlett <br />
| Gas Feedback<br />
|<br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
|- <br />
| 25 May 2018<br />
| 04-08 Jun 2018 <br />
| PASCO, Case Western <br />
| John Ruhl <br />
| Plenary talk on CMB-S4 <br />
| <br />
| [[Media:ruhl_pascos_final.pdf]] <br />
[[Media:Ruhl_pascos_final.key]]<br />
<br />
<br />
<br />
<br />
|- <br />
|<br />
| 15 April 2018 <br />
| AAS<br />
| Brad Benson<br />
| CMB-S4 excerpt from "The Hubble Constant from the Cosmic Microwave Background"<br />
| <br />
| [[media:2018_04_15_Benson_CMB_Hubble_CMBS4_slides.pdf]]<br />
<br />
<br />
<br />
|- <br />
|<br />
| 17-24 March 2018 <br />
| Rencontres de Moriond: Cosmology<br />
| Victor Buza <br />
| CMB-S4 Performance-Based Constraints On Primordial Gravitational Waves<br />
| <br />
The next-generation ground-based cosmic microwave background experiment, CMB-S4, will achieve new thresholds in the search for the B-mode polarization signature of primordial gravitational waves. To quantify these thresholds, as well as to propose an informed experimental configuration that will reach them, the CMB-S4 forecasting working group has developed a Fisher forecasting machinery targeted towards optimizing tensor-to-scalar parameter constraints in the presence of galactic foregrounds and gravitational lensing of the CMB. In this talk I will describe this framework and explain the uniqueness of this particular approach in basing the forecasts on scalings from actual analyses and multi-year achieved performances of the currently deployed BICEP/Keck series of experiments. In addition, I will detail our work on developing map-level noise simulations, and using various sky models, models of instrumental systematics, and analysis methods to explore the robustness of our findings, which most recently appeared in the CMB-S4 CDT report. Finally, I will talk about employing the Fisher framework in tandem with the simulations work to arrive at the currently proposed CMB-S4 strawman configuration. <br />
<br />
| [[Media:Moriond2018_Buza.pdf]]<br />
<br />
<br />
|- <br />
| 22 Jan 2018<br />
| 18-23 March 2018<br />
| Snowcluster<br />
| Nick Battaglia<br />
| On Cluster Profiles with CMB-S4<br />
| <br />
The next generation cosmic microwave background (CMB) experiment, CMB-S4, will make unprecedented measurements of secondary anisotropies in the CMB. I will focus on observations of the thermal and kinetic<br />
Sunyaev-Zel’dovich (SZ) effects, which will provide new windows into the thermodynamic properties of galaxy groups and clusters. I will<br />
show how we can constrain important baryonic processes, like feedback, that govern group and cluster formation through the high fidelity SZ<br />
profile measurements from CMB-S4. Additionally, I will describe the prospects to constrain fundamental physics from SZ observations and<br />
how to mitigate the modeling uncertainties associated with the baryonic processes that currently limit these constraints.<br />
| [[Media:Battaglia_Snowcluster_2018.pdf]]<br />
<br />
<br />
<br />
<br />
|- <br />
|<br />
| 31 Jan 2018 <br />
| CMB in Germany<br />
| John Carlstrom<br />
| CMB-S4 update<br />
| <br />
| [[Media:]]<br />
<br />
|- <br />
|<br />
| 2 Aug 2017 <br />
| NRAO Futures 2017<br />
| Zeesh Ahmed<br />
| <br />
| <br />
| [[File:AhmedFutures2017CMB-S4.pdf]]<br />
<br />
|- <br />
|<br />
| 6 Jan 2017 <br />
| B modes from space workshop<br />
| Lloyd Knox<br />
| CMB-S4 update<br />
| <br />
| [[Media:]]<br />
<br />
<br />
|- <br />
|<br />
| 2 Mar 2017 <br />
| SLAC Colloquium<br />
| Suzanne Staggs<br />
| Update following Feb 2017 CMB-S4 meeting<br />
|<br />
| [[file:CMB-and-S4-Staggs-SLAC-20170302-final.pptx]] <br />
<br />
|- <br />
|<br />
| 5 Aug 2016 <br />
| NRAO Futures 2016<br />
| Zeesh Ahmed<br />
| <br />
| <br />
| [[file:AhmedFuturesCMBsummary.pdf]]<br />
<br />
|- <br />
|<br />
| July 2016 <br />
| ICHEP 2016<br />
| Jeff McMahon<br />
| <br />
| <br />
| [[media:McMahon_ICHEP2016.pdf]]<br />
<br />
<br />
<br />
|- <br />
|<br />
| 28 Jan 2016 <br />
| Astronomy and Astrophysics Advisory Committee (AAAC)<br />
| John Carlstrom<br />
| CMB-S4 update<br />
| <br />
| [[file:CarlstromCMB-S4_AAAC_160128.pdf]]<br />
<br />
<br />
<br />
|}</div>Cbischoffhttp://www.cmb-s4.org/wiki/index.php?title=File:20190107_bischoff_aas.pdf&diff=8168File:20190107 bischoff aas.pdf2019-01-11T19:02:50Z<p>Cbischoff: Slides for Colin Bischoff talk at AAS 223</p>
<hr />
<div>Slides for Colin Bischoff talk at AAS 223</div>Cbischoffhttp://www.cmb-s4.org/wiki/index.php?title=Simulation_and_Forecasting_Logbook&diff=8153Simulation and Forecasting Logbook2018-12-10T18:09:10Z<p>Cbischoff: Copied Marius' posting link from deprecated r Forecasting Logbook</p>
<hr />
<div>This is an index page for logbook-style postings that cover the interconnected topics of sky modeling, simulations, and forecasting for CMB-S4. <br />
<br />
Some guidelines for use:<br />
* '''Postings should include enough context''' so that a reader can jump in and figure out what is going on. It is ''not'' necessary to write an extensive introduction to every posting -- context can be in the form of links to older postings, paper citations, etc.<br />
* Postings should represent a snapshot of work in progress. It's ok to post incomplete results, but recommended that you include notes about what is missing, what you are still planning to work on, etc. <br />
* If you have work that extends or improves an old posting, you should add it as a new posting (that includes links back to the old work as appropriate). Don't update old postings, as they should provide a chronological record of progress.<br />
* On this index page, add a link to your posting with the date, a descriptive posting title, and your full name. This logbook covers a wide range of topics, so titles will be really important to keep it useful. Don't name your posting something like "Forecasting for S4"!<br />
* Links should be added in reverse-chronological order (newest at the top). Your posting can either be written up on another wiki page or it can be a link to some externally hosted webpage (useful if you want to include a javascript plots pager).<br />
<br />
<br />
== Logbook Entries (reverse chronological) ==<br />
* '''2018 December 9''': [[Optimal Bayesian delensing progress update]] (Marius Millea) ''Updated 2018 Oct 2nd''<br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181207_bkfinal_02lt BK-style power spectra of 02 with Carron lensing templates] (Clem)<br />
* '''2018 December 7''': [[Problems with PS2HAT estimator at low ell]] (Clem Pryke)<br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181116_bpbias_study Bandpower bias study] (Ben Racine)<br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181207_expval_input_ML_search Maximum likelihood search with expectation values as input] (C. Umiltà)<br />
* '''2018 November 28''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181128_toy_sims Effective sky fraction] (Clem)<br />
* '''2018 November 21''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181111_dc04_flatpriors/ Maximum likelihood search results for Data Challenge 04, v2] (Ben Racine)<br />
* '''2018 November 21''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181111_dc04_flatpriors/index_abc.html Maximum likelihood search results for Data Challenge 04b and 04c, v2] (Ben Racine)<br />
* '''2018 November 16''': [[Analytic approximation for r likelihood]] (C. Bischoff) ''Updated 2018-11-20''<br />
* '''2018 November 12''': [[Detection significance for r=0.003]] (C. Bischoff)<br />
* '''2018 November 9''': [[Bad realizations in gsync/gdust sims]] (Clem Pryke)<br />
* '''2018 November 8''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181108_dc02_ML_LT Maximum likelihood search results for Data Challenge 02.00 with an ideal lensing template] (C. Umiltà)<br />
* '''2018 November 5''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181105_toy_sims Attempt to understand sigma(r) results with different hit maps] (Clem)<br />
* '''2018 October 29''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181018_1Dmodel_tapering_study Simple 1D model to study the effect of different observation strategies on the bandpower statistics.] (Ben Racine, Victor Buza, John Kovac)<br />
* '''2018 October 29''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181029_bkfinal_02lt BK-style power spectra of 02 with ideal lensing templates] (Clem)<br />
* '''2018 October 26''': [[Checking BB purity in re-analysis for alternate masks]] (Clem Pryke)<br />
* '''2018 October 23''': [[Estimated observing efficiency for past and current telescopes, version 2]] (C. Bischoff, Y. Chinone, T. Crawford, M. Hasselfield)<br />
* '''2018 October 14''': [[Estimates of delensing efficiency]] (Raphael)<br />
* '''2018 October 14''': [[Analysis of 04, 04b, 04c simulations]] (Raphael) [[Analysis of 04, 04b, 04c simulations comp]] (Ben)<br />
* '''2018 September 30''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180930_dc04_0to9/ Maximum likelihood search results for Data Challenge 04, models 0 to 9] (Ben Racine) ''Updated 2018 Oct 2nd''<br />
* '''2018 September 30''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180930_dc04_abc_model_0123789_ML/ Maximum likelihood search results for Data Challenge 04b and 04c, model 00, 01, 02, 03, 07, 08 and 09] (Ben Racine)<br />
* '''2018 September 30''': [[Ready for delensing use lensing maps 02.00]] (Julien Carron)<br />
* '''2018 September 28''': [[Towards lensing template]] (Clem Pryke)<br />
* '''2018 September 27''': [[Lensing reconstructions 02.00]] (Julien Carron)<br />
* '''2018 September 26''': [[Lensing map reconstruction from 02.00 sims w/ and w/o foreground+inhomogeneous noise]] (Toshiya Namikawa)<br />
* '''2018 September 25''': [[Estimated observing efficiency for past and current telescopes]] (C. Bischoff)<br />
* '''2018 September 25''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180925_bkfinal_04bc BK-style power spectra of 04/04b/04c masks for 00/01/02/03/07/08/09 foreground models] (Clem)<br />
* '''2018 September 12''': [[Low ell noise from past and current telescopes]] (C. Bischoff)<br />
* '''2018 September 5''': [[Phi reconstruction on 02.00 sims III]] (Anton Baleato)<br />
* '''2018 August 31''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180831_dc04_abc_model00_07_ML_proper_bp/ Maximum likelihood search results for Data Challenge 04b and 04c, for sky models 00 and 07] (Ben Racine)<br />
* '''2018 August 31''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180831_dc04_fixed_bp/ Maximum likelihood search results for Data Challenge 04, fixed bandpasses] (Ben Racine)<br />
* '''2018 August 27''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180827_bkfinal_04 Sims with nominal Chile and Pole masks III - BK-style power spectra of 04b.YY and 04c.YY] (Clem)<br />
* '''2018 August 27''': [[Sims with nominal Chile and Pole masks II]] (Clem P.)<br />
* '''2018 August 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180826_dc04_fixed/ Maximum likelihood search results for Data Challenge 04, fixed] (V.Buza, B.Racine)<br />
* '''2018 August 24''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180824_bkfinal_04/ BK-style power spectra of v04.00-06 sims (CDT report config) FIXED] (Caterina Umilta)<br />
* '''2018 August 24''': [[Amplitude modulated Gaussian dust sims]] (Clem P.)<br />
* '''2018 August 17''': [[Sims with nominal Chile and Pole masks]] (Clem P.)<br />
* '''2018 August 10''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180810_noise/ Achieved performance roundup] (C. Bischoff)<br />
* '''2018 August 7''': [[Pre-reference-design noise specifications for large-aperture forecasting]] (Tom Crawford, Matthew Hasselfield, Gil Holder, Lloyd Knox)<br />
* '''2018 August 6''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180805_s4opt/ Performance-based Fisher optimization for CMB-S4, 44cm vs 52cm aperture (w/ high-res/low-res 20 GHz)] (V.Buza)<br />
* '''2018 July 9''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180708_dc04/ Maximum likelihood search results for Data Challenge 04] (V.Buza)<br />
* '''2018 July 6''': [[Phi reconstruction on 02.00 sims II]] (Anton Baleato and Clem Pryke)<br />
* '''2018 June 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180611_s4opt/ Performance-based Fisher optimization for CMB-S4, 44cm aperture] (V.Buza) -- see corrected August 6th Update!<br />
* '''2018 June 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180609_S4_noise_simulation_arbitrary_coverage/ Recipe to generate performance based S4 simulations with arbitrary sky distribution (in progress)] (B.Racine, V.Buza)<br />
* '''2018 April 29''': [[Phi reconstruction on 02.00 sims]] (Anton Baleato)<br />
* '''2018 April 25''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180425_r_equivalent_maps/ Smallfield r-equivalent Maps] (Kenny Lau)<br />
* '''2018 April 4''': [[Sky masks for simulations III]] (Clem P.)<br />
* '''2018 March 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180323_bkfinal_04/ BK-style power spectra of v04.00-06 sims (CDT report config) BROKEN] (Clem)<br />
* '''2018 March 16''': [[ILC noise for large apertures at CDT noise levels]] (Raphael Flauger posted by Clem)<br />
* '''2018 March 16''': [[Sky masks for simulations II]] (Clem P.)<br />
* '''2018 February 19''': [[Sky masks for simulations]] (Clem P.)<br />
* '''2018 February 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180218_s4opt/ Performance-based Fisher optimization for CMB-S4, v3] (Victor Buza)<br />
* '''2018 February 7''': [[Sim map sets to demonstrate "real delensing" (02.00 and 02.09)]] (Clem P.)<br />
* '''2018 February 6''': [[Data Challenge Map Sets 04.YY]] (Clem P.)<br />
* '''2017 December 8''': [[Vansyngel Model]] (Clem P.)<br />
* '''2017 November 6''': [[Bandpass Convention - What does flat mean]] (Clem P.) - followup notes added Nov 20<br />
* '''2017 September 27''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170927_dc02/ Maximum likelihood search results for Data Challenge 02] (Bischoff, Buza, Willmert)<br />
* '''2017 September 13''': [[Bias on r from Band Center Errors]] (Palladino, Willmert, Bischoff)<br />
* '''2017 September 8''': [[Checking dust decorrelation in Raphael MHD based dust sim]] (Clem P.)<br />
* '''2017 September 6''': [[New NET Calculator and Validation]] (Denis Barkats)<br />
* '''2017 September 1''': [[Resolution at 20 GHz]] (Raphael)<br />
* '''2017 August 31''': [[Bias on r from additive systematics]] (Palladino, Willmert, Bischoff)<br />
* '''2017 August 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170818_bkfinal_03.00/ BK-style power spectra for 1000 realizations of v03.00,.03 CMB-S4 simulation maps] (Justin Willmert)<br />
* '''2017 August 18 ''': [[Neff_and_Beam_Calibration| Neff and Beam Calibration]] (Dan)<br />
* '''2017 August 18''': [[Ideal delensing templates from flat-sky QE, first pass]] (Kyle Story)<br />
* '''2017 August 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170818_HR/ High-Res studies for CMB-S4 (draft, v2)] (Victor Buza)<br />
* '''2017 August 18''': [[Comments from Anthony Challinor and Rupert Allison regarding the impact of Galactic Foregrounds on lensing]] (Neelima)<br />
* '''2017 August 11''': [[Joint Synchrotron and Dust Maps from Simulations]] (B. Hensley)<br />
* '''2017 August 9''': [[Dust Emission From Halos]] (Jim & Jean-Baptiste)<br />
* '''2017 August 9''': [[SZ Clusters update]] (Mat & Nick)<br />
* '''2017 August 4''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170804_HR/ High-Res studies for CMB-S4 (preliminary draft)] (Victor Buza); perhaps a reference of interest https://arxiv.org/abs/1707.02259<br />
* '''2017 July 10''': [[Additive systematics for data challenge 03]] (Bischoff, Palladino, Buza, Kovac)<br />
* '''2017 July 6''': [[Detection significance and sky fraction, dust decorrelation]](Raphael)<br />
* '''2017 July 3''': [[Toy highly decorrelated dust model]] (Clem P.)<br />
* '''2017 June 27''': [[Checking dust decorrelation in models d1/d4/d7 and hipdt]] (Clem P.)<br />
* '''2017 June 23''': [[Dust_delensing_firstlook|Dust delensing update]] (Alex)<br />
* '''2017 June 23''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170623_bkfinal_02.00/ BK-style power spectra for 1000 realizations of v02.00–06 CMB-S4 simulation maps] (Justin Willmert) ''Updated 2017 Sep 08''<br />
* '''2017 June 22''': [[Warm-up exercise for delensing]] (Raphael)<br />
* '''2017 June 19''': [[SZ Clusters update]] (Mat, Nick)<br />
* '''2017 June 11''': [[Notes from May 31 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 June 9''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170525_s4syst/ Introducing systematics for CMB-S4] ((Victor Buza), with input from Colin Bischoff, John Kovac)<br />
* '''2017 June 9''': [[Dust_delensing_firstlook]] (Alex)<br />
* '''2017 June 9''': [[r-forecasting: high and low ell coordination|r-forecasting: update on high and low ell coordination]] (Neelima+Colin Hill writing)<br />
* '''2017 June 1''': [[Residuals for DC 01.01 and DC 01.02]] (Raphael)<br />
* '''2017 June 1''': [[Levels of foregrounds in Gaussian and PySM simulations]] (Raphael)<br />
* '''2017 May 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170511_s4dc1/ S4 DC 01.xx analysis, v2] (Victor Buza, Colin Bischoff, Justin Willmert)<br />
* '''2017 May 26 ''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170411_bkfinal_01.00/ Updated v01.02 in "BK-style power spectra for 1000 realizations of v01.00–02 CMB-S4 simulation maps"] (Justin Willmert)<br />
* '''2017 May 15''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170515_chkS4/ N_ell spectra for CMB-S4 DC2.0] (Victor Buza)<br />
* '''2017 May 15''': [[Rev 2 PySM a2d4f1s3 maps]] (Clem P.)<br />
* '''2017 May 12''': [[r-forecasting: high and low ell coordination|r-forecasting: high and low ell coordination]] (lensers writing)<br />
* '''2017 May 8''': [[Checking PySM maps]] (Clem P.)<br />
* '''2017 May 2''': [[Notes from April 26 telecon on science requirements for clusters/high-ell]] (Steve)<br />
* '''2017 May 1''': [[r-forecasting: delensing discussion|r-forecasting delensing discussion]] (Neelima and Blake)<br />
* '''2017 April 28 ''': [[Update_on_Neff_Forecasts| Update on Neff Forecasts]] (Dan)<br />
* '''2017 April 26 ''': [http://www.cosmo.bnl.gov/www/msyriac/web/work/sigma8plots.html Update on cluster number counts forecast including w_a] (Mat and Nick)<br />
* '''2017 April 21 ''': [[lensing-DE|Update on a lensing-based DE forecast]] (Jo, Siddharth)<br />
* '''2017 April 18 ''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170411_bkfinal_01.00/ BK-style power spectra for 1000 realizations of v01.00–02 CMB-S4 simulation maps] (Justin Willmert)<br />
* '''2017 April 18 ''': [[S4-Lensing|S4 measurement requirements for neutrino mass and delensing - first pass]] (Neelima/Blake)<br />
* '''2017 April 17 ''': [[HiDPol|HI-based dust polarization model for r forecasts]] (Tuhin)<br />
* '''2017 April 05 ''': [[lensing-DE|Notes on one path to lensing-based DE forecasts]] (Jo)<br />
* '''2017 April 05 ''': [[Notes from April 5 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 April 05''': [https://cmb-s4.org/CMB-S4workshops/images/Sigma8_z_prep.pdf Sigma8(z) SPT clusters (placeholder) ] (S Bocquet)<br />
* '''2017 April 04''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170404_s4opt/ Updated Performance-based Fisher optimization for CMB-S4 (using bands v1.99)] (Victor Buza, Updated 2017.04.21)<br />
* '''2017 March 31 ''': [[Data Challenge analysis - DC1.0, DC1.1, DC1.2]] (Raphael)<br />
* '''2017 March 30 ''': [[Notes from March 28 telecon on science requirements for clusters/high-ell]] (Jim & Steve)<br />
* '''2017 March 29''': [[CMB-S4 frequency bands v1.99]] (John Kovac, Band-definition working group)<br />
* '''2017 March 28''': [[Adding higher res delensing "band"]] (Clem P.)<br />
* '''2017 March 27''': [[01.01 sim input maps - first try]] (Clem P.)<br />
* '''2017 March 23''': [[01.00 sim input maps]] (Clem P.)<br />
* '''2017 March 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170221_S4_NET_forecasts/ S4 Band sensitivity comparison follow-up] (Denis Barkats, John Kovac)<br />
* '''2017 March 17''': [http://users.physics.harvard.edu/~buza/20170317_s4dc1/ S4 DC1.0 analysis] (Victor Buza, Colin Bischoff, Justin Willmert)<br />
* '''2017 March 17 ''': [[Media:Telecon_03172017_optimization_for_CMBS4.pdf]]: Optimization methodology for SO (Josquin)<br />
* '''2017 March 16 ''': [[ P_k_science_case| P(k) science case]] (Colin, Simone, Nick, David)<br />
* '''2017 March 15 ''': [[Notes from March 15 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 March 15 ''': [[CMB halo lensing sensitivity as a function of map sensitivity and resolution]] (Jim & Jean-Baptiste)<br />
* '''2017 March 15 ''': [[w and gamma | w and Delta gamma constraints from sigma_8 (z)]] (Mat & Nick)<br />
* '''2017 March 10 ''': [[Notes from March 8 telecon on science requirements for clusters/high-ell]] (Jim & Steve)<br />
* '''2017 March 8 ''': [[reionization_requirements| Reionization science]] (Simone & Marcelo)<br />
* '''2017 March 8 ''': [[High ell topics | High ell topics ]] (Jim)<br />
* '''2017 March 8 ''': [[SZ_s8_z | sigma 8 of z constraints ]] (Mat, Nick)<br />
* '''2017 March 8 ''': [[Szcounts | Number counts update for 1.0', 1.5', 2.0']] (Nick, Mat)<br />
* '''2017 March 8 ''': [[SZastro | SZ astrophysics with DESI ]](Nick, Simone, Emanuel, David)<br />
* '''2017 February 24''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170224_cmbs4_dc1_final/ BK-style processing of DC1.0 maps to spectra] (Justin Willmert, Colin Bischoff)<br />
* '''2017 February 15 ''': [[Extragalactic lensing sims| Update on extragalactic phase-2 lensing sims]] (Marcelo, George, Dick, others)<br />
* '''2017 February 15 ''': [[Plan for next Galactic Phase-2sims| Plan for next Galactic phase-2 sims]] (Jo, Ben)<br />
* '''2017 February 10 ''': [[Resolution of foreground-cleaned map]] (Mat, Neelima, Blake, Alex, others)<br />
* '''2017 February 10 ''': [[Nongaussian dust in lensing]] (Alex, Mat, Neelima, Blake, others)<br />
* '''2017 January 30''': [[Aliased power in noise maps]] (Bischoff, Updated 2017-02-02)<br />
* '''2017 January 23''': [[CMBS4 Band Sensitivity Comparison]] (Charlie Hill)<br />
* '''2017 January 12''': [http://bicep.rc.fas.harvard.edu/cbischoff/20170112_data_challenge_1/ Maps for CMB-S4 data challenge 1] (Bischoff, Pryke, Buza)<br />
* '''2016 December 21''': [http://users.physics.harvard.edu/~buza/20161220_chkS4/ N_ell spectra for the CMB-S4 data challenge, and updated &sigma;(r) checkpoints] (Victor Buza, Updated 2017.02.01)<br />
* '''2016 November 30''': [[First steps to sim input maps]] (Clem P.)<br />
* '''2016 November 4''': [[Tophat bands for Data Challenge]] (Bischoff)<br />
* '''2016 July 8''': [[fsky|Dependence of foregrounds on sky fraction]] (Raphael)<br />
* '''2016 July 8''': [[SciBookPowspecTheoryFig|Three choices for Science Book Figure 5 (theory power spectrum & current BB points)]] (Tom C.)<br />
* '''2016 July 8''': [http://users.physics.harvard.edu/~buza/20160707_s4plots/ S4 Inflation Chapter Plot Suggestions, V2] (Victor Buza)<br />
* '''2016 July 6''': [[w_cosntraint|Preliminary w constraint]] (Alessandro)<br />
* '''2016 June 24''': [[nsr|Preliminary ns-r plot for discussion]] (Raphael)<br />
* '''2016 June 16''': [[DelensingImpact| Impact Of Delensing On sigma(r)]] (Neelima/Mat)<br />
* '''2016 June 16''': [http://users.physics.harvard.edu/~buza/20160616_s4plots/ S4 Inflation Chapter Plot Suggestions] (Victor Buza)<br />
* '''2016 June 10''': [[MapBasedRb| Map-based &sigma;(r) forecasts V2]] (David/Jo/Ben)<br />
* '''2016 June 3''': [http://users.physics.harvard.edu/~buza/20160531_fisher/ &sigma;(r) forecasting checkpoints, V2] (Victor Buza)<br />
* '''2016 June 3''': [[ BTTfixedeffort | Forecasts for fnl BTT beam/fixed effort]] (Daan)<br />
* '''2016 May 31''': [[ForecastPatchyReion| Forecasts for patchy reionization]] (Vera, Alex, Nick)<br />
* '''2016 May 26''': [[Forecasting | Forecasts on neutrino mass]] (Nam, Mat, Neelima)<br />
* '''2016 May 26''': [[ KSZ| Forecasts on kSZ S/N]] (Simone, Emmanuel, Colin)<br />
* '''2016 May 26''': [[ Forecastfiso_planck| Forecast on correlated and anti-correlated CDM isocurvature f_iso]] (Kimmy, Cora, updated with plots 20160602)<br />
* '''2016 May 24''': [[ BTTNoiseBeam | Forecasts on fnl BTT beam/FWHM]] (Daan)<br />
* '''2016 May 22''': [[ ForecastAxions| Update on the axion isocurvature constraints for changing sensitivity and resolution]] (Renee)<br />
* '''2016 May 21''': [[ Forecastpann| Forecast on dark matter annihilation parameter p_ann]] (Kimmy, Cora)<br />
* '''2016 May 20''': [[NeffNoiseBeam| Forecasts on Neff and Yp]] (Joel, Alex)<br />
* '''2016 May 20''': [[ForecastEDE| Forecasts on Early Dark Energy]] (Erminia)<br />
* '''2016 May 20''': [[ForecastCompIsocurv| Forecasts on compensated isocurvature varying sensitivity, resolution and sky coverage]] (Julian, Ely)<br />
* '''2016 May 20''': [[ForecastBirefring| Forecasts on birefringence varying sensitivity and resolution]] (Vera, Alex)<br />
* '''2016 May 20''': [[ForecastStrings| Forecasts on string tension varying sensitivity and resolution]] (Renee)<br />
* '''2016 May 20''': [[RobustForecast| Cosmological forecasts including component separation and iterative delensing]] (Stephen Feeney and Josquin Errard)<br />
* '''2016 May 19''': [[MapBasedR| Map-based &sigma;(r) forecasts]] (David A.)<br />
* '''2016 May 18''': [[Shear_calibration_LSST|LSST shear calibration with CMB S4]] (Emmanuel Schaan)<br />
* '''2016 May 13''': [http://users.physics.harvard.edu/~buza/20150505_fisher/ &sigma;(r) forecasting checkpoints] (Victor Buza)<br />
* '''2016 May 13''': [[NonGaussianitiesTTT| CMBS-4 forecasts local and equilateral scalar Ngs using TTT]] (daan)<br />
* '''2016 May 13''': [[ForecastingSims|Simulations for r forecasts]] (Jo/Ben/David)<br />
* '''2016 May 6''': [[DMInteractionsComplementarity|DM interactions: complementarity]] (Vera)<br />
* '''2016 May 6''': [[Scenarios| Scenarios]] (Scott, Vera)<br />
* ''' 2016 May 3''': [[ForecastAxions |Effect of S4 specs on axion density parameters]] (Renee)<br />
* '''2016 April 30''': [[ForecastNu| Effect of S4 specs on neutrino parameters]] (Erminia)<br />
* '''2016 April 28''': [http://web.stanford.edu/~wlwu/posting/20160421_lensres/ Delensing residuals with low-ell foregrounds] (Kimmy Wu)<br />
* '''2016 April 28''': [[NonGaussianities| CMBS-4 forecast for tensor NGs]] (daan)<br />
* '''2016 April 19''': [[ForecastingStep1| Checking basic parameters for nominal case]] (Jo + multiple authors)<br />
* '''2016 April 5''': [[Forecasting|Setting up non-r Fisher-based parameter forecasts]] (Jo + others)<br />
* '''2016 March 31''': [http://users.physics.harvard.edu/~buza/20150331_fisher/ Fisher projections for &sigma;(r) based on achieved performance] (Victor Buza)<br />
* '''2016 January 27''': [https://cmb-s4.org/CMB-S4workshops/index.php/File:sptpol_ptsrc_polfrac_500d.pdf Quick estimate of mean-squared polarization fraction for SPTpol sources] (Tom Crawford)</div>Cbischoffhttp://www.cmb-s4.org/wiki/index.php?title=Simulation_and_Forecasting_Logbook&diff=8081Simulation and Forecasting Logbook2018-11-20T16:04:05Z<p>Cbischoff: /* Logbook Entries (reverse chronological) */</p>
<hr />
<div>This is an index page for logbook-style postings that cover the interconnected topics of sky modeling, simulations, and forecasting for CMB-S4. <br />
<br />
Some guidelines for use:<br />
* '''Postings should include enough context''' so that a reader can jump in and figure out what is going on. It is ''not'' necessary to write an extensive introduction to every posting -- context can be in the form of links to older postings, paper citations, etc.<br />
* Postings should represent a snapshot of work in progress. It's ok to post incomplete results, but recommended that you include notes about what is missing, what you are still planning to work on, etc. <br />
* If you have work that extends or improves an old posting, you should add it as a new posting (that includes links back to the old work as appropriate). Don't update old postings, as they should provide a chronological record of progress.<br />
* On this index page, add a link to your posting with the date, a descriptive posting title, and your full name. This logbook covers a wide range of topics, so titles will be really important to keep it useful. Don't name your posting something like "Forecasting for S4"!<br />
* Links should be added in reverse-chronological order (newest at the top). Your posting can either be written up on another wiki page or it can be a link to some externally hosted webpage (useful if you want to include a javascript plots pager).<br />
<br />
<br />
== Logbook Entries (reverse chronological) ==<br />
* '''2018 November 16''': [[Analytic approximation for r likelihood]] (C. Bischoff) ''Updated 2018-11-20''<br />
* '''2018 November 12''': [[Detection significance for r=0.003]] (C. Bischoff)<br />
* '''2018 November 9''': [[Bad realizations in gsync/gdust sims]] (Clem Pryke)<br />
* '''2018 November 8''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181108_dc02_ML_LT Maximum likelihood search results for Data Challenge 02.00 with an ideal lensing template] (C. Umiltà)<br />
* '''2018 November 5''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181105_toy_sims Attempt to understand sigma(r) results with different hit maps] (Clem)<br />
* '''2018 October 29''': [http://bicep2.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181018_1Dmodel_tapering_study Simple 1D model to study the effect of different observation strategies on the bandpower statistics.] (Ben Racine, Victor Buza, John Kovac)<br />
* '''2018 October 29''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181029_bkfinal_02lt BK-style power spectra of 02 with lensing templates] (Clem)<br />
* '''2018 October 26''': [[Checking BB purity in re-analysis for alternate masks]] (Clem Pryke)<br />
* '''2018 October 23''': [[Estimated observing efficiency for past and current telescopes, version 2]] (C. Bischoff, Y. Chinone, T. Crawford, M. Hasselfield)<br />
* '''2018 October 14''': [[Estimates of delensing efficiency]] (Raphael)<br />
* '''2018 October 14''': [[Analysis of 04, 04b, 04c simulations]] (Raphael) [[Analysis of 04, 04b, 04c simulations comp]] (Ben)<br />
* '''2018 September 30''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180930_dc04_0to9/ Maximum likelihood search results for Data Challenge 04, models 0 to 9] (Ben Racine) ''Updated 2018 Oct 2nd''<br />
* '''2018 September 30''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180930_dc04_abc_model_0123789_ML/ Maximum likelihood search results for Data Challenge 04b and 04c, model 00, 01, 02, 03, 07, 08 and 09] (Ben Racine)<br />
* '''2018 September 30''': [[Ready for delensing use lensing maps 02.00]] (Julien Carron)<br />
* '''2018 September 28''': [[Towards lensing template]] (Clem Pryke)<br />
* '''2018 September 27''': [[Lensing reconstructions 02.00]] (Julien Carron)<br />
* '''2018 September 26''': [[Lensing map reconstruction from 02.00 sims w/ and w/o foreground+inhomogeneous noise]] (Toshiya Namikawa)<br />
* '''2018 September 25''': [[Estimated observing efficiency for past and current telescopes]] (C. Bischoff)<br />
* '''2018 August 27''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180925_bkfinal_04bc BK-style power spectra of 04/04b/04c masks for 00/01/02/03/07/08/09 foreground models] (Clem)<br />
* '''2018 September 12''': [[Low ell noise from past and current telescopes]] (C. Bischoff)<br />
* '''2018 September 5''': [[Phi reconstruction on 02.00 sims III]] (Anton Baleato)<br />
* '''2018 August 31''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180831_dc04_abc_model00_07_ML_proper_bp/ Maximum likelihood search results for Data Challenge 04b and 04c, for sky models 00 and 07] (Ben Racine)<br />
* '''2018 August 31''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180831_dc04_fixed_bp/ Maximum likelihood search results for Data Challenge 04, fixed bandpasses] (Ben Racine)<br />
* '''2018 August 27''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180827_bkfinal_04 Sims with nominal Chile and Pole masks III - BK-style power spectra of 04b.YY and 04c.YY] (Clem)<br />
* '''2018 August 27''': [[Sims with nominal Chile and Pole masks II]] (Clem P.)<br />
* '''2018 August 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180826_dc04_fixed/ Maximum likelihood search results for Data Challenge 04, fixed] (V.Buza, B.Racine)<br />
* '''2018 August 24''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180824_bkfinal_04/ BK-style power spectra of v04.00-06 sims (CDT report config) FIXED] (Caterina Umilta)<br />
* '''2018 August 24''': [[Amplitude modulated Gaussian dust sims]] (Clem P.)<br />
* '''2018 August 17''': [[Sims with nominal Chile and Pole masks]] (Clem P.)<br />
* '''2018 August 10''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180810_noise/ Achieved performance roundup] (C. Bischoff)<br />
* '''2018 August 7''': [[Pre-reference-design noise specifications for large-aperture forecasting]] (Tom Crawford, Matthew Hasselfield, Gil Holder, Lloyd Knox)<br />
* '''2018 August 6''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180805_s4opt/ Performance-based Fisher optimization for CMB-S4, 44cm vs 52cm aperture (w/ high-res/low-res 20 GHz)] (V.Buza)<br />
* '''2018 July 9''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180708_dc04/ Maximum likelihood search results for Data Challenge 04] (V.Buza)<br />
* '''2018 July 6''': [[Phi reconstruction on 02.00 sims II]] (Anton Baleato and Clem Pryke)<br />
* '''2018 June 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180611_s4opt/ Performance-based Fisher optimization for CMB-S4, 44cm aperture] (V.Buza) -- see corrected August 6th Update!<br />
* '''2018 June 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180609_S4_noise_simulation_arbitrary_coverage/ Recipe to generate performance based S4 simulations with arbitrary sky distribution (in progress)] (B.Racine, V.Buza)<br />
* '''2018 April 29''': [[Phi reconstruction on 02.00 sims]] (Anton Baleato)<br />
* '''2018 April 25''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180425_r_equivalent_maps/ Smallfield r-equivalent Maps] (Kenny Lau)<br />
* '''2018 April 4''': [[Sky masks for simulations III]] (Clem P.)<br />
* '''2018 March 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180323_bkfinal_04/ BK-style power spectra of v04.00-06 sims (CDT report config) BROKEN] (Clem)<br />
* '''2018 March 16''': [[ILC noise for large apertures at CDT noise levels]] (Raphael Flauger posted by Clem)<br />
* '''2018 March 16''': [[Sky masks for simulations II]] (Clem P.)<br />
* '''2018 February 19''': [[Sky masks for simulations]] (Clem P.)<br />
* '''2018 February 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180218_s4opt/ Performance-based Fisher optimization for CMB-S4, v3] (Victor Buza)<br />
* '''2018 February 7''': [[Sim map sets to demonstrate "real delensing" (02.00 and 02.09)]] (Clem P.)<br />
* '''2018 February 6''': [[Data Challenge Map Sets 04.YY]] (Clem P.)<br />
* '''2017 December 8''': [[Vansyngel Model]] (Clem P.)<br />
* '''2017 November 6''': [[Bandpass Convention - What does flat mean]] (Clem P.) - followup notes added Nov 20<br />
* '''2017 September 27''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170927_dc02/ Maximum likelihood search results for Data Challenge 02] (Bischoff, Buza, Willmert)<br />
* '''2017 September 13''': [[Bias on r from Band Center Errors]] (Palladino, Willmert, Bischoff)<br />
* '''2017 September 8''': [[Checking dust decorrelation in Raphael MHD based dust sim]] (Clem P.)<br />
* '''2017 September 6''': [[New NET Calculator and Validation]] (Denis Barkats)<br />
* '''2017 September 1''': [[Resolution at 20 GHz]] (Raphael)<br />
* '''2017 August 31''': [[Bias on r from additive systematics]] (Palladino, Willmert, Bischoff)<br />
* '''2017 August 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170818_bkfinal_03.00/ BK-style power spectra for 1000 realizations of v03.00,.03 CMB-S4 simulation maps] (Justin Willmert)<br />
* '''2017 August 18 ''': [[Neff_and_Beam_Calibration| Neff and Beam Calibration]] (Dan)<br />
* '''2017 August 18''': [[Ideal delensing templates from flat-sky QE, first pass]] (Kyle Story)<br />
* '''2017 August 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170818_HR/ High-Res studies for CMB-S4 (draft, v2)] (Victor Buza)<br />
* '''2017 August 18''': [[Comments from Anthony Challinor and Rupert Allison regarding the impact of Galactic Foregrounds on lensing]] (Neelima)<br />
* '''2017 August 11''': [[Joint Synchrotron and Dust Maps from Simulations]] (B. Hensley)<br />
* '''2017 August 9''': [[Dust Emission From Halos]] (Jim & Jean-Baptiste)<br />
* '''2017 August 9''': [[SZ Clusters update]] (Mat & Nick)<br />
* '''2017 August 4''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170804_HR/ High-Res studies for CMB-S4 (preliminary draft)] (Victor Buza); perhaps a reference of interest https://arxiv.org/abs/1707.02259<br />
* '''2017 July 10''': [[Additive systematics for data challenge 03]] (Bischoff, Palladino, Buza, Kovac)<br />
* '''2017 July 6''': [[Detection significance and sky fraction, dust decorrelation]](Raphael)<br />
* '''2017 July 3''': [[Toy highly decorrelated dust model]] (Clem P.)<br />
* '''2017 June 27''': [[Checking dust decorrelation in models d1/d4/d7 and hipdt]] (Clem P.)<br />
* '''2017 June 23''': [[Dust_delensing_firstlook|Dust delensing update]] (Alex)<br />
* '''2017 June 23''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170623_bkfinal_02.00/ BK-style power spectra for 1000 realizations of v02.00–06 CMB-S4 simulation maps] (Justin Willmert) ''Updated 2017 Sep 08''<br />
* '''2017 June 22''': [[Warm-up exercise for delensing]] (Raphael)<br />
* '''2017 June 19''': [[SZ Clusters update]] (Mat, Nick)<br />
* '''2017 June 11''': [[Notes from May 31 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 June 9''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170525_s4syst/ Introducing systematics for CMB-S4] ((Victor Buza), with input from Colin Bischoff, John Kovac)<br />
* '''2017 June 9''': [[Dust_delensing_firstlook]] (Alex)<br />
* '''2017 June 9''': [[r-forecasting: high and low ell coordination|r-forecasting: update on high and low ell coordination]] (Neelima+Colin Hill writing)<br />
* '''2017 June 1''': [[Residuals for DC 01.01 and DC 01.02]] (Raphael)<br />
* '''2017 June 1''': [[Levels of foregrounds in Gaussian and PySM simulations]] (Raphael)<br />
* '''2017 May 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170511_s4dc1/ S4 DC 01.xx analysis, v2] (Victor Buza, Colin Bischoff, Justin Willmert)<br />
* '''2017 May 26 ''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170411_bkfinal_01.00/ Updated v01.02 in "BK-style power spectra for 1000 realizations of v01.00–02 CMB-S4 simulation maps"] (Justin Willmert)<br />
* '''2017 May 15''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170515_chkS4/ N_ell spectra for CMB-S4 DC2.0] (Victor Buza)<br />
* '''2017 May 15''': [[Rev 2 PySM a2d4f1s3 maps]] (Clem P.)<br />
* '''2017 May 12''': [[r-forecasting: high and low ell coordination|r-forecasting: high and low ell coordination]] (lensers writing)<br />
* '''2017 May 8''': [[Checking PySM maps]] (Clem P.)<br />
* '''2017 May 2''': [[Notes from April 26 telecon on science requirements for clusters/high-ell]] (Steve)<br />
* '''2017 May 1''': [[r-forecasting: delensing discussion|r-forecasting delensing discussion]] (Neelima and Blake)<br />
* '''2017 April 28 ''': [[Update_on_Neff_Forecasts| Update on Neff Forecasts]] (Dan)<br />
* '''2017 April 26 ''': [http://www.cosmo.bnl.gov/www/msyriac/web/work/sigma8plots.html Update on cluster number counts forecast including w_a] (Mat and Nick)<br />
* '''2017 April 21 ''': [[lensing-DE|Update on a lensing-based DE forecast]] (Jo, Siddharth)<br />
* '''2017 April 18 ''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170411_bkfinal_01.00/ BK-style power spectra for 1000 realizations of v01.00–02 CMB-S4 simulation maps] (Justin Willmert)<br />
* '''2017 April 18 ''': [[S4-Lensing|S4 measurement requirements for neutrino mass and delensing - first pass]] (Neelima/Blake)<br />
* '''2017 April 17 ''': [[HiDPol|HI-based dust polarization model for r forecasts]] (Tuhin)<br />
* '''2017 April 05 ''': [[lensing-DE|Notes on one path to lensing-based DE forecasts]] (Jo)<br />
* '''2017 April 05 ''': [[Notes from April 5 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 April 05''': [https://cmb-s4.org/CMB-S4workshops/images/Sigma8_z_prep.pdf Sigma8(z) SPT clusters (placeholder) ] (S Bocquet)<br />
* '''2017 April 04''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170404_s4opt/ Updated Performance-based Fisher optimization for CMB-S4 (using bands v1.99)] (Victor Buza, Updated 2017.04.21)<br />
* '''2017 March 31 ''': [[Data Challenge analysis - DC1.0, DC1.1, DC1.2]] (Raphael)<br />
* '''2017 March 30 ''': [[Notes from March 28 telecon on science requirements for clusters/high-ell]] (Jim & Steve)<br />
* '''2017 March 29''': [[CMB-S4 frequency bands v1.99]] (John Kovac, Band-definition working group)<br />
* '''2017 March 28''': [[Adding higher res delensing "band"]] (Clem P.)<br />
* '''2017 March 27''': [[01.01 sim input maps - first try]] (Clem P.)<br />
* '''2017 March 23''': [[01.00 sim input maps]] (Clem P.)<br />
* '''2017 March 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170221_S4_NET_forecasts/ S4 Band sensitivity comparison follow-up] (Denis Barkats, John Kovac)<br />
* '''2017 March 17''': [http://users.physics.harvard.edu/~buza/20170317_s4dc1/ S4 DC1.0 analysis] (Victor Buza, Colin Bischoff, Justin Willmert)<br />
* '''2017 March 17 ''': [[Media:Telecon_03172017_optimization_for_CMBS4.pdf]]: Optimization methodology for SO (Josquin)<br />
* '''2017 March 16 ''': [[ P_k_science_case| P(k) science case]] (Colin, Simone, Nick, David)<br />
* '''2017 March 15 ''': [[Notes from March 15 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 March 15 ''': [[CMB halo lensing sensitivity as a function of map sensitivity and resolution]] (Jim & Jean-Baptiste)<br />
* '''2017 March 15 ''': [[w and gamma | w and Delta gamma constraints from sigma_8 (z)]] (Mat & Nick)<br />
* '''2017 March 10 ''': [[Notes from March 8 telecon on science requirements for clusters/high-ell]] (Jim & Steve)<br />
* '''2017 March 8 ''': [[reionization_requirements| Reionization science]] (Simone & Marcelo)<br />
* '''2017 March 8 ''': [[High ell topics | High ell topics ]] (Jim)<br />
* '''2017 March 8 ''': [[SZ_s8_z | sigma 8 of z constraints ]] (Mat, Nick)<br />
* '''2017 March 8 ''': [[Szcounts | Number counts update for 1.0', 1.5', 2.0']] (Nick, Mat)<br />
* '''2017 March 8 ''': [[SZastro | SZ astrophysics with DESI ]](Nick, Simone, Emanuel, David)<br />
* '''2017 February 24''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170224_cmbs4_dc1_final/ BK-style processing of DC1.0 maps to spectra] (Justin Willmert, Colin Bischoff)<br />
* '''2017 February 15 ''': [[Extragalactic lensing sims| Update on extragalactic phase-2 lensing sims]] (Marcelo, George, Dick, others)<br />
* '''2017 February 15 ''': [[Plan for next Galactic Phase-2sims| Plan for next Galactic phase-2 sims]] (Jo, Ben)<br />
* '''2017 February 10 ''': [[Resolution of foreground-cleaned map]] (Mat, Neelima, Blake, Alex, others)<br />
* '''2017 February 10 ''': [[Nongaussian dust in lensing]] (Alex, Mat, Neelima, Blake, others)<br />
* '''2017 January 30''': [[Aliased power in noise maps]] (Bischoff, Updated 2017-02-02)<br />
* '''2017 January 23''': [[CMBS4 Band Sensitivity Comparison]] (Charlie Hill)<br />
* '''2017 January 12''': [http://bicep.rc.fas.harvard.edu/cbischoff/20170112_data_challenge_1/ Maps for CMB-S4 data challenge 1] (Bischoff, Pryke, Buza)<br />
* '''2016 December 21''': [http://users.physics.harvard.edu/~buza/20161220_chkS4/ N_ell spectra for the CMB-S4 data challenge, and updated &sigma;(r) checkpoints] (Victor Buza, Updated 2017.02.01)<br />
* '''2016 November 30''': [[First steps to sim input maps]] (Clem P.)<br />
* '''2016 November 4''': [[Tophat bands for Data Challenge]] (Bischoff)<br />
* '''2016 July 8''': [[fsky|Dependence of foregrounds on sky fraction]] (Raphael)<br />
* '''2016 July 8''': [[SciBookPowspecTheoryFig|Three choices for Science Book Figure 5 (theory power spectrum & current BB points)]] (Tom C.)<br />
* '''2016 July 8''': [http://users.physics.harvard.edu/~buza/20160707_s4plots/ S4 Inflation Chapter Plot Suggestions, V2] (Victor Buza)<br />
* '''2016 July 6''': [[w_cosntraint|Preliminary w constraint]] (Alessandro)<br />
* '''2016 June 24''': [[nsr|Preliminary ns-r plot for discussion]] (Raphael)<br />
* '''2016 June 16''': [[DelensingImpact| Impact Of Delensing On sigma(r)]] (Neelima/Mat)<br />
* '''2016 June 16''': [http://users.physics.harvard.edu/~buza/20160616_s4plots/ S4 Inflation Chapter Plot Suggestions] (Victor Buza)<br />
* '''2016 June 10''': [[MapBasedRb| Map-based &sigma;(r) forecasts V2]] (David/Jo/Ben)<br />
* '''2016 June 3''': [http://users.physics.harvard.edu/~buza/20160531_fisher/ &sigma;(r) forecasting checkpoints, V2] (Victor Buza)<br />
* '''2016 June 3''': [[ BTTfixedeffort | Forecasts for fnl BTT beam/fixed effort]] (Daan)<br />
* '''2016 May 31''': [[ForecastPatchyReion| Forecasts for patchy reionization]] (Vera, Alex, Nick)<br />
* '''2016 May 26''': [[Forecasting | Forecasts on neutrino mass]] (Nam, Mat, Neelima)<br />
* '''2016 May 26''': [[ KSZ| Forecasts on kSZ S/N]] (Simone, Emmanuel, Colin)<br />
* '''2016 May 26''': [[ Forecastfiso_planck| Forecast on correlated and anti-correlated CDM isocurvature f_iso]] (Kimmy, Cora, updated with plots 20160602)<br />
* '''2016 May 24''': [[ BTTNoiseBeam | Forecasts on fnl BTT beam/FWHM]] (Daan)<br />
* '''2016 May 22''': [[ ForecastAxions| Update on the axion isocurvature constraints for changing sensitivity and resolution]] (Renee)<br />
* '''2016 May 21''': [[ Forecastpann| Forecast on dark matter annihilation parameter p_ann]] (Kimmy, Cora)<br />
* '''2016 May 20''': [[NeffNoiseBeam| Forecasts on Neff and Yp]] (Joel, Alex)<br />
* '''2016 May 20''': [[ForecastEDE| Forecasts on Early Dark Energy]] (Erminia)<br />
* '''2016 May 20''': [[ForecastCompIsocurv| Forecasts on compensated isocurvature varying sensitivity, resolution and sky coverage]] (Julian, Ely)<br />
* '''2016 May 20''': [[ForecastBirefring| Forecasts on birefringence varying sensitivity and resolution]] (Vera, Alex)<br />
* '''2016 May 20''': [[ForecastStrings| Forecasts on string tension varying sensitivity and resolution]] (Renee)<br />
* '''2016 May 20''': [[RobustForecast| Cosmological forecasts including component separation and iterative delensing]] (Stephen Feeney and Josquin Errard)<br />
* '''2016 May 19''': [[MapBasedR| Map-based &sigma;(r) forecasts]] (David A.)<br />
* '''2016 May 18''': [[Shear_calibration_LSST|LSST shear calibration with CMB S4]] (Emmanuel Schaan)<br />
* '''2016 May 13''': [http://users.physics.harvard.edu/~buza/20150505_fisher/ &sigma;(r) forecasting checkpoints] (Victor Buza)<br />
* '''2016 May 13''': [[NonGaussianitiesTTT| CMBS-4 forecasts local and equilateral scalar Ngs using TTT]] (daan)<br />
* '''2016 May 13''': [[ForecastingSims|Simulations for r forecasts]] (Jo/Ben/David)<br />
* '''2016 May 6''': [[DMInteractionsComplementarity|DM interactions: complementarity]] (Vera)<br />
* '''2016 May 6''': [[Scenarios| Scenarios]] (Scott, Vera)<br />
* ''' 2016 May 3''': [[ForecastAxions |Effect of S4 specs on axion density parameters]] (Renee)<br />
* '''2016 April 30''': [[ForecastNu| Effect of S4 specs on neutrino parameters]] (Erminia)<br />
* '''2016 April 28''': [http://web.stanford.edu/~wlwu/posting/20160421_lensres/ Delensing residuals with low-ell foregrounds] (Kimmy Wu)<br />
* '''2016 April 28''': [[NonGaussianities| CMBS-4 forecast for tensor NGs]] (daan)<br />
* '''2016 April 19''': [[ForecastingStep1| Checking basic parameters for nominal case]] (Jo + multiple authors)<br />
* '''2016 April 5''': [[Forecasting|Setting up non-r Fisher-based parameter forecasts]] (Jo + others)<br />
* '''2016 March 31''': [http://users.physics.harvard.edu/~buza/20150331_fisher/ Fisher projections for &sigma;(r) based on achieved performance] (Victor Buza)<br />
* '''2016 January 27''': [https://cmb-s4.org/CMB-S4workshops/index.php/File:sptpol_ptsrc_polfrac_500d.pdf Quick estimate of mean-squared polarization fraction for SPTpol sources] (Tom Crawford)</div>Cbischoffhttp://www.cmb-s4.org/wiki/index.php?title=File:04c_AL106.png&diff=8080File:04c AL106.png2018-11-20T16:02:31Z<p>Cbischoff: Cbischoff uploaded a new version of File:04c AL106.png</p>
<hr />
<div>Marginalized r likelihood for experiment config 04c and AL=0.106</div>Cbischoffhttp://www.cmb-s4.org/wiki/index.php?title=File:04c_AL106.png&diff=8079File:04c AL106.png2018-11-20T16:02:17Z<p>Cbischoff: Cbischoff uploaded a new version of File:04c AL106.png</p>
<hr />
<div>Marginalized r likelihood for experiment config 04c and AL=0.106</div>Cbischoffhttp://www.cmb-s4.org/wiki/index.php?title=Analytic_approximation_for_r_likelihood&diff=8078Analytic approximation for r likelihood2018-11-20T15:59:30Z<p>Cbischoff: </p>
<hr />
<div>''Colin Bischoff, 2018-11-16'' // ''updated 2018-11-20''<br />
----<br />
<br />
In a [[Detection_significance_for_r=0.003|previous posting]], I ran BICEP/Keck-style CosmoMC likelihood analysis for bandpowers corresponding to the model expectation value for r=0.003 + foregrounds + lensing residual. This allowed me to calculate the detection significance for r in those particular scenarios: experiment config 04b (Chile sky coverage) with residual A<sub>L</sub>=0.27 or 0.337 and experiment config 04c (Pole sky coverage) with residual A<sub>L</sub>=0.081 or 0.106. Victor's Fisher analysis allows us to calculate &sigma;(r) for other scenarios, but we would like to estimate statistics like detection significance which rely on the non-Gaussian shape of the likelihood.<br />
<br />
My ansatz is that the shape of the r likelihood can be well described with the H-L likelihood ([http://adsabs.harvard.edu/abs/2008PhRvD..77j3013H Hamimeche & Lewis; PRD 77, 10, 103013; 2008]). That likelihood is meant to describe CMB power spectra, but the BB spectrum is linear in r (more or less) so we might expect this choice to work well. For a one-dimensional likelihood with r as the only parameter, the form of the H-L likelihood simplifies (scalar multiplication commutes) and we can write it as<br />
<br />
-log(L) = ( x - log x - 1 ) * ( r<sub>f</sub> + N )<sup>2</sup> / &sigma;<sup>2</sup><br />
x = ( r<sub>ML</sub> + N ) / ( r + N )<br />
<br />
where <br />
* <tt>r</tt> is the likelihood parameter, <br />
* <tt>r<sub>ML</sub></tt> is the maximum-likelihood r value, <br />
* <tt>&sigma;</tt> is &sigma;(r) calculated assuming a fiducial model with r = <tt>r<sub>f</sub></tt>,<br />
* <tt>N</tt> is a "noise bias" that contains contributions from instrumental noise, residual foregrounds, and residual lensing.<br />
<br />
In practice, if we want a representative likelihood curve for a particular value of r, we can use a Fisher code to calculate &sigma;(r) then set <tt>r<sub>ML</sub></tt> = <tt>r<sub>f</sub></tt> = r and <tt>&sigma;</tt> = &sigma;(r). However, we still need to get an estimate of parameter <tt>N</tt> from the CosmoMC-derived likelihoods.<br />
<br />
For the four scenarios shown in my previous posting, I reran the CosmoMC likelihood with somewhat tighter convergence criteria and at a higher temperature to get a better measurement in the tails of the distribution. Then I fit each curve to the model by minimizing a K-S statistic. The results are shown in the following table, along with detection significance calculated both from the CosmoMC likelihood and from the analytic fit. <br />
<br />
The table also includes a degrees of freedom statistic calculated as <br />
<br />
k = 2 * ( r<sub>ML</sub> + N )<sup>2</sup> / &sigma;<sup>2</sup><br />
<br />
We might expect that this parameter should come out with a common value for the two Chile scenarios and a common value for the two Pole scenarios, with a ratio that corresponds to the relative sky area. I do find that both Pole scenarios correspond to <tt>k</tt> ~ 525 but I find very high and inconsistent values of <tt>k</tt> for the two Chile scenarios. I think the reason is that parameter <tt>N</tt> mostly affects the skewness of the distribution. The Pole likelihoods have significant skewness and I get a reliable fit. The Chile likelihoods have less skewness, so there is equal preference for any large value of <tt>N</tt>. Perhaps the best estimate of <tt>k</tt> for the Chile mask would be to start from the Pole mask value of <tt>k</tt>, then multiply by some map-derived estimate of the relative sky areas.<br />
<br />
<blockquote><br />
'''UPDATE 2018-11-20''': I added new columns to the table and new lines to the figures showing how the likelihood shape and detection significance change if we fix <tt>k</tt> to 525 for Pole and 10000 for Chile. <br />
</blockquote><br />
<br />
Using the degrees of freedom parameter, we can write down an analytic model for the r likelihood by picking r, doing a Fisher calculation for &sigma;(r), and then calculating <tt>N</tt> from the above equation.<br />
<br />
{| class="wikitable"<br />
! Site !! A<sub>L</sub> !! !! <tt>r<sub>ML</sub></tt> !! <tt>&sigma;</tt> !! <tt>N</tt> !! <tt>k</tt> !! significance (original) !! significance (fit) !! <tt>k*</tt> !! significance (fix <tt>k=k*</tt>)<br />
|-<br />
| Chile || 0.270 || || 0.00256 || 0.00102 || 0.195 || 28446 || 2.5 &sigma; || 2.5 &sigma; || 10000 || 2.6<br />
|-<br />
| Chile || 0.337 || || 0.00255 || 0.00112 || 0.076 || 9803 || 2.3 &sigma; || 2.3 &sigma; || 10000 || 2.3 <br />
|-<br />
| Pole || 0.081 || || 0.00268 || 0.00080 || 0.010 || 492 || 3.8 &sigma; || 4.0 &sigma; || 525 || 3.9<br />
|-<br />
| Pole || 0.106 || || 0.00269 || 0.00088 || 0.012 || 569 || 3.5 &sigma; || 3.5 &sigma; || 525 || 3.5<br />
|}<br />
<br />
The figures below show the CosmoMC likelihood (blue) and the analytic model (orange) for the four scenarios that I used. The lower panels of each figure shows the fractional difference between the original likelihood and the model, which does increase out in the tails.<br />
<br />
[[File:04b_AL270.png|frame|Figure 1: Marginalized r likelihood for experiment config 04b and A<sub>L</sub>=0.270|center]]<br />
<br />
[[File:04b_AL337.png|frame|Figure 2: Marginalized r likelihood for experiment config 04b and A<sub>L</sub>=0.337|center]]<br />
<br />
[[File:04c_AL081.png|frame|Figure 3: Marginalized r likelihood for experiment config 04c and A<sub>L</sub>=0.081|center]]<br />
<br />
[[File:04c_AL106.png|frame|Figure 4: Marginalized r likelihood for experiment config 04c and A<sub>L</sub>=0.106|center]]</div>Cbischoffhttp://www.cmb-s4.org/wiki/index.php?title=File:04c_AL106.png&diff=8077File:04c AL106.png2018-11-20T15:57:41Z<p>Cbischoff: Cbischoff uploaded a new version of File:04c AL106.png</p>
<hr />
<div>Marginalized r likelihood for experiment config 04c and AL=0.106</div>Cbischoffhttp://www.cmb-s4.org/wiki/index.php?title=File:04c_AL081.png&diff=8076File:04c AL081.png2018-11-20T15:57:19Z<p>Cbischoff: Cbischoff uploaded a new version of File:04c AL081.png</p>
<hr />
<div>Marginalized r likelihood for experiment config 04c and AL=0.081</div>Cbischoffhttp://www.cmb-s4.org/wiki/index.php?title=File:04b_AL337.png&diff=8075File:04b AL337.png2018-11-20T15:56:55Z<p>Cbischoff: Cbischoff uploaded a new version of File:04b AL337.png</p>
<hr />
<div>Marginalized r likelihood for experiment config 04b and AL=0.337</div>Cbischoff