http://www.cmb-s4.org/wiki/api.php?action=feedcontributions&user=Jch&feedformat=atomCMB-S4 wiki - User contributions [en]2020-04-03T04:25:45ZUser contributionsMediaWiki 1.30.0http://www.cmb-s4.org/wiki/index.php?title=UCSD-2019:_Analysis/Pipeline_Working_Group:_Maps_to_C_ell&diff=10143UCSD-2019: Analysis/Pipeline Working Group: Maps to C ell2019-10-19T00:07:24Z<p>Jch: /* 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 />
'''Note that "Maps to Cl" is actually shorthand for "Maps to Cl to Parameters" or "Maps to Parameters from (non-low-ell-BB) Power Spectra." This is important for understanding the charge and defining the responsibilities of this group.'''<br />
<br />
The charge from the meeting SOC is twofold (see https://docs.google.com/document/d/1KtRif7_BPi3gACMkIA7__AWK63iUJiljN6UlKI41MS0 for the exact charge). One part is a set of general instructions for all analysis working groups:<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 />
The other part is a set of specific questions to support other working groups / WBSs as we move to the next level of design. Our questions are:<br />
<br />
* How are we calibrating beams to meet high-ell science requirements? Can we use high S/N point sources alone?<br />
* How does the galaxy impact Neff inference? <br />
* Does this drive frequency coverage? <br />
* Is there a path to realistically achieve both the necessary cadence for transients and the necessary sky coverage for light relics goals?<br />
* What are the necessary analysis tools to answer these questions?<br />
<br />
== Agenda ==<br />
<br />
<br />
'''Reminder: What are the science targets, and what was previously identified as important decisions / questions by the forecasters? (30 minutes total)'''<br />
<br />
''1. Light relics summary'' (Ben Wallisch, on behalf of Dan Green and Joel Meyers and others) [[:File:UCSD2019_LightRelicsSummary.pdf|slides]]<br />
<br />
''2. Dark matter science summary'' (Vera Gluscevic) [[:File:Gluscevic-dark-matter-UCSD2019.pdf|slides]]<br />
<br />
<br />
'''General charge (45 minutes total)'''<br />
<br />
''1. Identify key decisions that must be made (and justified) prior to CD-1'' (open discussion with some structure and example questions from organizers)<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 />
Some possible key decisions/questions:<br />
<br />
* Start with known high-priority things<br />
** Which instrumental effects are important, what requirements can we put on them, and are they relevant for decisions being made on the timescale of CD-1?<br />
*** Beams<br />
*** T -> P leakage<br />
*** Time constants<br />
*** Gain / gain drift / elevation-dependent gain<br />
** What limits how much sky we can observe?<br />
** What science goals beyond Neff potentially drive measurement and instrument requirements for non-BB power spectra? Are we missing something by concentrating on Neff?<br />
** What level of sims to maps to Cell to parameters pipeline do we need for CD-1? Should a tool be developed to be used by the whole collaboration?<br />
*** Do we need to include delensing in near-term forecasting tools?<br />
** Should Maps to Cell and low-ell BB groups have a common set of simulations and analysis tools to be addressing “non-idealities” by CD-1?<br />
*** This is happening in DM / Simulations, though other groups will have input on the nature of these tools.<br />
** Should we be setting up data challenges (e.g., make a CMB sky with beam properties varying across the field and have people analyze it and get unbiased Neff)?<br />
<br />
''2. Make progress on (or actually make) those decisions''<br />
<br />
''3. 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 />
<br />
* Summary of decisions identified as most important, possible tasking and timelines.<br />
<br />
''4. Ensure that those timelines and processes are understood and supported by the collaboration, and that we (together) believe we can follow them.''<br />
<br />
* We can talk in the session about the best ways to ensure this. <br />
<br />
<br />
'''Individual charge questions (45 minutes total)'''<br />
<br />
''Questions regarding how much sky we could possibly observe without hitting some systematic or noise floor? (what is limiting fsky?)''<br />
<br />
''1. How does the galaxy impact Neff inference and does this drive frequency coverage?'' (Colin Hill) [[File:JCH_Gal_Neff_v2.pdf]]<br />
* also think about ground pickup?<br />
<br />
''2. Is there a path to realistically achieve both the necessary cadence for transients and the necessary sky coverage for light relics goals?'' (Reijo Keskitalo) [https://cmb-s4.org/wiki/index.php/File:LAT_scanning_slides_for_CMBS4_San_Diego_2019.pdf slides] [https://cmb-s4.org/wiki/index.php/Chile_Scanning_Movie animation] [https://cmb-s4.org/wiki/index.php/High_cadence_LAT_from_Chile wiki post] [https://cmb-s4.org/wiki/index.php/WAFTT_results_part_3 WAFFT results part 3]<br />
<br />
<br />
''Questions regarding systematics:''<br />
<br />
''3. How are we calibrating beams to meet high-ell science requirements? Can we use high S/N point sources alone?'' (Tom Crawford [https://docs.google.com/presentation/d/1l_ZdHL0HcZ18EKbFRljPI_j-08oF7zDlZoefJnYg1R4 slides])<br />
* What about T -> P leakage for Neff? (incl higher-order terms)<br />
<br />
<br />
''General questions'''<br />
<br />
''4. What are the necessary analysis tools to answer these questions?'' (all, discussion)<br />
<br />
== Remote attendance ==<br />
<br />
[https://fnal.zoom.us/j/9554120728 Zoom link]<br />
<br />
== Notes ==<br />
<br />
'''Early notes on planning/agenda are here:''' https://docs.google.com/document/d/1uxn1AedOzWAObeG59aS7WPfctV_GC6kDbDw0KgdR_Ow<br />
<br />
'''Note further "charge" from Lloyd's flowdown parallel summary:<br />
* Working groups need to develop (or gather) software needed for reduction of simulated maps to science results.<br />
* Working groups need to think about development of analyses for rapid exploration of different measurement properties (e.g., frequency distribution, angular resolution, levels of systematic effects).<br />
* Flowdown from Science to Meas will be done with a hybrid approach of semi-analytic (or otherwise “fast”) methods, map-based sims, and occasional time-domain sims.<br />
<br />
'''Brainstorming on key decisions on the path to CD-1'''<br />
<br />
Some possible key decisions/questions:<br />
<br />
Start with known high-priority things<br />
Which instrumental effects are important, what requirements can we put on them, and are they relevant for decisions being made on the timescale of CD-1?<br />
Beams<br />
T -> P leakage<br />
Time constants<br />
Gain / gain drift / elevation-dependent gain<br />
cross-talk?<br />
- if you have xtalk in pixel partners, it is just a reduction in polarization efficiency, and there's nothing you can do about it. someone should just declare a limit on that.<br />
polarization-dependent beams?<br />
- is this different from just beam mismatches between polarization partners?<br />
- can we measure polarized beams? how?<br />
- is it hopeless to do this off of astronomical sources? do we absolutely need a terrestrial source? how to set this requirement?<br />
<br />
What limits how much sky we can observe?<br />
What science goals beyond Neff potentially drive measurement and instrument requirements for non-BB power spectra? Are we missing something by concentrating on Neff?<br />
What level of sims to maps to Cell to parameters pipeline do we need for CD-1? Should a tool be developed to be used by the whole collaboration?<br />
Do we need to include delensing in near-term forecasting tools?<br />
- we think this was included in Science Book forecasts.<br />
- and in DSR<br />
- if you just include 7 parameters (LCDM+Neff), the difference between doing forecasts on unlensed spectra and real delensing is not that important. <br />
- but if you include Yp, it starts to matter (like 0.3 sigma)<br />
- confirm with Dan & Joel, but probably already done<br />
Should Maps to Cell and low-ell BB groups have a common set of simulations and analysis tools to be addressing “non-idealities” by CD-1?<br />
- This is happening in DM / Simulations, though other groups will have input on the nature of these tools.<br />
- well, the simulation side is definitely happening, but what about the tools? Do we need to produce a unified set of maps to C_ell tools?<br />
- general consensus is yes.<br />
- Who maintains and develops these tools?<br />
- this working group (not Data Management, not TOASTers)<br />
- needs to be a schedule for delivery of these tools, and they need to be ready for the first Mock Data Challenge<br />
<br />
Should we be setting up data challenges (e.g., make a CMB sky with beam properties varying across the field and have people analyze it and get unbiased Neff)?</div>Jchhttp://www.cmb-s4.org/wiki/index.php?title=File:JCH_Gal_Neff_v2.pdf&diff=10142File:JCH Gal Neff v2.pdf2019-10-19T00:06:50Z<p>Jch: </p>
<hr />
<div></div>Jchhttp://www.cmb-s4.org/wiki/index.php?title=UCSD-2019:_Analysis/Pipeline_Working_Group:_Maps_to_Other_Statistics&diff=10061UCSD-2019: Analysis/Pipeline Working Group: Maps to Other Statistics2019-10-18T19:25:39Z<p>Jch: /* Agenda */</p>
<hr />
<div>[https://cmb-s4.org/wiki/index.php/UCSD-2019:_Cosmology_with_CMB-S4#Agenda Link back to agenda]<br />
<br />
Background: this working group covers a remarkably broad area of science targets and topics, although none of them are design-driving, primary science goals. Scientifically, it can cover science topics including neutrino mass, structure growth and dark energy / modified gravity, reionization, baryonic physics, and other topics. In terms of measurements covered by this group, they include lensing power spectra and cross-correlations, cluster cosmology, SZ cross-correlations and higher point functions, CMB bispectra, and several others.<br />
<br />
In light of this, major goals of our group are to identify and prioritize several key science targets and analyses, and, with our work as part of this group, strengthen and sharpen these S4 science cases. Our work should also inform the efforts of other working groups (for example by exploring mass calibration for the sources group and lensing systematics for BB-delensing).<br />
<br />
To start, an idea is to focus on a few of the key science targets: neutrino mass (e.g. from lensing), baryonic physics and reionization. However, we will have a broader discussion on priorities and science targets at the end of the session.<br />
<br />
<br />
== Official Charge Question ==<br />
<br />
* Given plausible CIB models (and galactic foregrounds) at high ell, what frequency coverage (and associated sensitivity) is sufficient to reduce CIB residuals below statistical errors on tSZ and kSZ measurements?<br />
* How severe is the impact of small-scale polarized foregrounds on lensing? (If important, how can we mitigate them?)<br />
* What is the optimal strategy for mitigating temperature lensing foregrounds?<br />
* What are requirements on beam and pointing for sub-percent lensing spectra?<br />
* What are the necessary analysis tools to answer these questions?<br />
<br />
== Agenda ==<br />
<br />
Introductory remarks (Marcelo and Blake)<br />
<br />
<br />
'''Lensing'''<br />
<br />
Foregrounds:<br />
<br />
Emmanuel Schaan: temperature foregrounds in lensing (20+10 mins) [[File:Talk_lensing_foregrounds_cmbs4_schaan.pdf]]<br />
<br />
Kevin Huffenberger: modeling of small-scale non-Gaussian Galactic foregrounds (to characterize lensing bias) (10+5 mins) [[File:Smallscale_foregrounds.pdf]]<br />
<br />
Srini Raghunathan: foregrounds for cluster lensing reconstruction (10+5 mins)<br />
<br />
<br />
Theory:<br />
<br />
Alex van Engelen: baryonic effects for CMB lensing and neutrino mass (10+5 mins) [[File:baryons_CMBS4.key.pdf]]<br />
<br />
<br />
'''SZ'''<br />
<br />
Marcelo Alvarez: constraints on patchy reionization from kSZ (10+5 mins) [[File:Mapsother_reionization.pdf]]<br />
<br />
Colin Hill (discussion): CIB cleaning requirements for SZ (10 mins) [[File:JCH_CIB_Cleaning.pdf]]<br />
<br />
<br />
'''Discussion'''<br />
<br />
Key targets and analyses<br />
<br />
== Remote attendance ==<br />
<br />
[https://ucsd.zoom.us/j/973144732 Zoom link]<br />
<br />
<br />
== Notes ==</div>Jchhttp://www.cmb-s4.org/wiki/index.php?title=File:JCH_CIB_Cleaning.pdf&diff=10059File:JCH CIB Cleaning.pdf2019-10-18T19:24:59Z<p>Jch: </p>
<hr />
<div></div>Jchhttp://www.cmb-s4.org/wiki/index.php?title=UCSD-2019:_Analysis/Pipeline_Working_Group:_Maps_to_C_ell&diff=10048UCSD-2019: Analysis/Pipeline Working Group: Maps to C ell2019-10-18T19:06:45Z<p>Jch: /* 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 />
'''Note that "Maps to Cl" is actually shorthand for "Maps to Cl to Parameters" or "Maps to Parameters from (non-low-ell-BB) Power Spectra." This is important for understanding the charge and defining the responsibilities of this group.'''<br />
<br />
The charge from the meeting SOC is twofold (see https://docs.google.com/document/d/1KtRif7_BPi3gACMkIA7__AWK63iUJiljN6UlKI41MS0 for the exact charge). One part is a set of general instructions for all analysis working groups:<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 />
The other part is a set of specific questions to support other working groups / WBSs as we move to the next level of design. Our questions are:<br />
<br />
* How are we calibrating beams to meet high-ell science requirements? Can we use high S/N point sources alone?<br />
* How does the galaxy impact Neff inference? <br />
* Does this drive frequency coverage? <br />
* Is there a path to realistically achieve both the necessary cadence for transients and the necessary sky coverage for light relics goals?<br />
* What are the necessary analysis tools to answer these questions?<br />
<br />
== Agenda ==<br />
<br />
<br />
'''Reminder: What are the science targets, and what was previously identified as important decisions / questions by the forecasters? (30 minutes total)'''<br />
<br />
''1. Light relics summary'' (Ben Wallisch, on behalf of Dan Green and Joel Meyers and others) [https://dummylink slides]<br />
<br />
''2. Dark matter science summary'' (Vera Gluscevic) [[:File:Gluscevic-dark-matter-UCSD2019.pdf|slides]]<br />
<br />
<br />
'''General charge (45 minutes total)'''<br />
<br />
''1. Identify key decisions that must be made (and justified) prior to CD-1'' (open discussion with some structure and example questions from organizers)<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 />
Some possible key decisions/questions:<br />
<br />
* Start with known high-priority things<br />
** Which instrumental effects are important, what requirements can we put on them, and are they relevant for decisions being made on the timescale of CD-1?<br />
*** Beams<br />
*** T -> P leakage<br />
*** Time constants<br />
*** Gain / gain drift / elevation-dependent gain<br />
** What limits how much sky we can observe?<br />
** What science goals beyond Neff potentially drive measurement and instrument requirements for non-BB power spectra? Are we missing something by concentrating on Neff?<br />
** What level of sims to maps to Cell to parameters pipeline do we need for CD-1? Should a tool be developed to be used by the whole collaboration?<br />
*** Do we need to include delensing in near-term forecasting tools?<br />
** Should Maps to Cell and low-ell BB groups have a common set of simulations and analysis tools to be addressing “non-idealities” by CD-1?<br />
*** This is happening in DM / Simulations, though other groups will have input on the nature of these tools.<br />
** Should we be setting up data challenges (e.g., make a CMB sky with beam properties varying across the field and have people analyze it and get unbiased Neff)?<br />
<br />
''2. Make progress on (or actually make) those decisions''<br />
<br />
''3. 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 />
<br />
* Summary of decisions identified as most important, possible tasking and timelines.<br />
<br />
''4. Ensure that those timelines and processes are understood and supported by the collaboration, and that we (together) believe we can follow them.''<br />
<br />
* We can talk in the session about the best ways to ensure this. <br />
<br />
<br />
'''Individual charge questions (45 minutes total)'''<br />
<br />
''Questions regarding how much sky we could possibly observe without hitting some systematic or noise floor? (what is limiting fsky?)''<br />
<br />
''1. How does the galaxy impact Neff inference and does this drive frequency coverage?'' (Colin Hill) [[File:JCH_Gal_Neff.pdf]]<br />
* also think about ground pickup?<br />
<br />
''2. Is there a path to realistically achieve both the necessary cadence for transients and the necessary sky coverage for light relics goals?'' (Reijo Keskitalo) [https://cmb-s4.org/wiki/index.php/File:LAT_scanning_slides_for_CMBS4_San_Diego_2019.pdf slides] [https://cmb-s4.org/wiki/index.php/Chile_Scanning_Movie animation] [https://cmb-s4.org/wiki/index.php/High_cadence_LAT_from_Chile wiki post]<br />
<br />
<br />
''Questions regarding systematics:''<br />
<br />
''3. How are we calibrating beams to meet high-ell science requirements? Can we use high S/N point sources alone?''<br />
* TC (I did an early study on this and can resurrect it for discussion) [https://cmb-s4.org/wiki/images/Neff_beams_v1.pdf slides]<br />
* What about T -> P leakage for Neff? (incl higher-order terms)<br />
<br />
<br />
''General questions'''<br />
<br />
''4. What are the necessary analysis tools to answer these questions?'' (all, discussion)<br />
<br />
== Remote attendance ==<br />
<br />
[https://ucsd.zoom.us/j/605467322 Zoom link]<br />
<br />
<br />
== Notes ==<br />
<br />
'''Early notes on planning/agenda are here:''' https://docs.google.com/document/d/1uxn1AedOzWAObeG59aS7WPfctV_GC6kDbDw0KgdR_Ow</div>Jchhttp://www.cmb-s4.org/wiki/index.php?title=File:JCH_Gal_Neff.pdf&diff=10047File:JCH Gal Neff.pdf2019-10-18T19:05:28Z<p>Jch: </p>
<hr />
<div></div>Jchhttp://www.cmb-s4.org/wiki/index.php?title=UCSD-2019:_Science_Theme:_Matter_Mapping&diff=9799UCSD-2019: Science Theme: Matter Mapping2019-10-17T20:44:18Z<p>Jch: /* 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 />
Review science goals <br><br />
Review/update/prioritize questions to be answered regarding measurement requirements <br><br />
Identify priorities for science case development, if any<br />
<br />
== Agenda ==<br />
<br />
- Presentations on additional science and new ideas [7+3 min each]<br />
* Srini Raghunathan: CMB-cluster lensing and tSZ counts [[File:SRaghunathan_matter_mapping_session.pdf]]<br />
* Siavash Yasini: Birkinshaw-Gull effect<br />
* Selim Hotinli: Rees-Sciama and/or moving lens effect<br />
* Giulio Fabbian [remote]: NG lensing biases [[File:Fabbian_cmbs4_2019ucsd.pdf]]<br />
* Alex van Engelen: thermal-kinetic SZ (tkSZ) [https://cmb-s4.org/wiki/index.php/File:Tksz_vanengelen_S4_oct2019.key.pdf Slides]<br />
* Nick Battaglia: SZ systematics [[File:S4_SZ_systematics.pdf]]<br />
* (If time, late contribution) Blake Sherwin + Simone Ferraro [[File:smallScalesS4.pdf]]<br />
<br />
- Focused discussions: [~1 hr]<br />
* Further developing science cases: deep survey at the Pole -- e.g., overlap with deep satellite observations, possibilities for cross-correlations<br />
* Galactic Science <br />
* Review/update/prioritize questions to be answered regarding measurement requirements -- what needs to be done for CD-1? what needs to be done better than it was in the DSR?<br />
<br />
== Remote attendance ==<br />
<br />
[https://ucsd.zoom.us/j/988412674 Zoom link]<br />
<br />
== Notes ==<br />
Please comment as you see fit. [https://docs.google.com/presentation/d/1-JnkuklosNzJwkc_yZEYxhN5o430xvyhK7MimDXzEC4/edit?usp=sharing here]</div>Jchhttp://www.cmb-s4.org/wiki/index.php?title=File:Fabbian_cmbs4_2019ucsd.pdf&diff=9795File:Fabbian cmbs4 2019ucsd.pdf2019-10-17T20:42:13Z<p>Jch: </p>
<hr />
<div></div>Jchhttp://www.cmb-s4.org/wiki/index.php?title=UCSD-2019:_Science_Theme:_Matter_Mapping&diff=9783UCSD-2019: Science Theme: Matter Mapping2019-10-17T19:22:27Z<p>Jch: </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 />
Review science goals <br><br />
Review/update/prioritize questions to be answered regarding measurement requirements <br><br />
Identify priorities for science case development, if any<br />
<br />
== Agenda ==<br />
<br />
- Presentations on additional science and new ideas [7+3 min each]<br />
* Srini Raghunathan: CMB-cluster lensing and tSZ counts [[File:SRaghunathan_matter_mapping_session.pdf]]<br />
* Siavash Yasini: Birkinshaw-Gull effect<br />
* Selim Hotinli: Rees-Sciama and/or moving lens effect<br />
* Giulio Fabbian [remote]: NG lensing biases<br />
* Alex van Engelen: thermal-kinetic SZ (tkSZ) [https://cmb-s4.org/wiki/index.php/File:Tksz_vanengelen_S4_oct2019.key.pdf Slides]<br />
* Nick Battaglia: SZ systematics [[File:S4_SZ_systematics.pdf]]<br />
<br />
- Focused discussions: [~1 hr]<br />
* Further developing science cases: deep survey at the Pole -- e.g., overlap with deep satellite observations, possibilities for cross-correlations<br />
* Galactic Science <br />
* Review/update/prioritize questions to be answered regarding measurement requirements -- what needs to be done for CD-1? what needs to be done better than it was in the DSR?<br />
<br />
== Remote attendance ==<br />
<br />
[https://ucsd.zoom.us/j/988412674 Zoom link]<br />
<br />
== Notes ==<br />
Please comment as you see fit. [https://docs.google.com/presentation/d/1-JnkuklosNzJwkc_yZEYxhN5o430xvyhK7MimDXzEC4/edit?usp=sharing here]</div>Jchhttp://www.cmb-s4.org/wiki/index.php?title=File:SRaghunathan_matter_mapping_session.pdf&diff=9774File:SRaghunathan matter mapping session.pdf2019-10-17T18:45:50Z<p>Jch: Jch uploaded a new version of File:SRaghunathan matter mapping session.pdf</p>
<hr />
<div></div>Jchhttp://www.cmb-s4.org/wiki/index.php?title=UCSD-2019:_Cosmology_with_CMB-S4&diff=9681UCSD-2019: Cosmology with CMB-S42019-10-17T15:49:24Z<p>Jch: /* Thursday October 17th */</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 session has a Zoom link assigned, see the dedicated pages on the wiki linked from the agenda (email zonca@sdsc.edu if you want your account to be a Host so you have admin permissions).<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 />
== Slack channel ==<br />
<br />
Please join the <code>#ucsd2019</code> channel on CMB-S4 organization on Slack.<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 />
== Posters, Fire slides and Randomized Coffee Trial ==<br />
<br />
Attendees can introduce themselves or a new project/concept/idea with a one-minute, one-slide "fire slide." Two fire slide sessions will be held, end of the day on Thursday and Friday.<br />
Poster session is on Thursday evening right outside the Auditorium, you are very welcome to introduce your poster with a "fire slide".<br />
Please sign up for both using [https://forms.gle/yG2ZGraJXWqskJDH7 this form] by the end of the day October 11th.<br />
<br />
The Junior Scientist Advancement Committee is running a Randomized Coffee Trial as a way to create new connections for our junior members. Each junior member will be randomly paired with a senior member who they do not already know well. The only obligation is to meet and have at least a 10 minute conversation about your work over one of the coffee breaks.<br />
We encourage everyone (junior and senior) to [https://forms.gle/nvnyyouWs1DAwdHd7 sign up using this link] by 5pm PDT on Tuesday, October 15.<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 />
=== Rooms ===<br />
<br />
Plenaries: SDSC Full Auditorium<br />
<br />
Parallels, sorted from larger to smaller:<br />
<br />
* Auditorium: larger split<br />
* Auditorium: smaller split<br />
* East Wing: Synthesis Center E-143<br />
* Central Wing: Conf room 408<br />
* East Wing: Conf room E-330 (Thu) East Wing: E-145 (Fri-Sat)<br />
* Central Wing: Conf 567<br />
* Central Wing: Conf room 575<br />
<br />
Small meeting room for telecons: East Wing: Conf room E-322<br />
or any of the other rooms when not used.<br />
<br />
=== Thursday October 17th ===<br />
<br />
08:00 - Coffee and breakfast<br />
<br />
08:30 - Plenary 1, Welcome & Status Reports - Chair: Julian Borrill<br />
* 08:30 - Welcome (Mike Norman)<br />
* 08:35 - [[UCSD-2019: Logistics | Logistics]] (Andrea Zonca)<br />
* 08:40 - Executive Committee & Governing Board Update [https://docs.google.com/presentation/d/1FW3BBDiMZ9p36JN1AtP-z_HAVAXacGWFbLVFl_EXbOY slides]<br />
* 09:10 - Project Office + charting the path to CD-1/3a and NSF PDR (Jim Yeck) [[File:Plenary_Yeck.pptx]]<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 (Raphael Flauger)[[File:Flauger_191017_PGW.pdf|Flauger_191017_PGW.pdf]]<br />
* 09:45 - Dark Universe (Daniel Green) [[File:Green_dark_universe_plenary.pdf|Green_dark_universe_plenary.pdf]]<br />
* 10:00 - Matter Mapping (Colin Hill) [[File:JCH_Matter_Mapping.pdf|JCH_Matter_Mapping.pdf]]<br />
<br />
10:15 - Coffee (at 10:17 the alarm siren will go off for [https://blink.ucsd.edu/safety/emergencies/preparedness/get-ready/shakeout.html Earthquake preparedness drill], we can stay inside the auditorium)<br />
<br />
10:45 - Plenary 2 - continue<br />
* 10:45 - Transients (Nathan Whitehorn)<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 - Show of hands to assign rooms for the 2 afternoon parallel sessions and update the agenda accordingly<br />
<br />
12:35 - Lunch (catering just outside of the Auditorium)<br />
<br />
We have some attendees with severe allergy to nuts. Corner Bakery will serve no food containing nuts, '''do not bring peanuts / peanut butter / tree nuts''' into the meeting rooms)<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 />
18:15 - Posters/Social, please remember to sign up for a poster (see above). We will also have a "Job board" where people can tack ads. Appetizers and soda offered on the patio outside the Auditorium (no food containing nuts, no alcoholic drinks)<br />
<br />
[19:00 - Governing Board in Room E-145]<br />
<br />
=== Friday October 18th ===<br />
<br />
08:00 - Coffee and breakfast<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 - Show of hands to assign rooms for the 2 afternoon parallel sessions and update the agenda accordingly<br />
<br />
12:35 - 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+Loverde+Reichardt)<br />
* [[UCSD-2019: Analysis/Pipeline Working Group: Maps to Other Statistics | Analysis/Pipeline Working Group: Maps to Other Statistics]] (Sherwin+Alvarez)<br />
* [[UCSD-2019: Analysis/Pipeline Working Group: Sources | Analysis/Pipeline Working Group: Sources]] (Holder+Battaglia+Vieira)<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 />
18:15 - A few options for dinners below:<br />
<br />
* Walking distance from the Auditorium: [https://sodaandswine.com/ Soda&Swine],[https://rockbottom.com/locations/la-jolla/ Rock Bottom], [https://www.bellavistacaffe.com/menus Bella Vista Cafe]<br />
* 5 min drive from campus: [https://www.cohnrestaurants.com/draftrepublic/menu Draft Republic], [https://www.westfield.com/utc/entertainment/dining Westfield UTC mall]<br />
* Around San Diego based on neighborhood: Prepkitchen (Del Mar), Karl Strauss (La Jolla), Galaxy Tacos (La Jolla Shores), Ballast Point (Miramar)<br />
* Close to the airport: [https://libertystation.com/directory/eat Liberty Station]<br />
<br />
=== Saturday October 19th ===<br />
<br />
08:00 - Coffee and breakfast<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: Knox/Ruhl/Arnold<br />
<br />
12:15 - Closeout (Spokespeople)<br />
<br />
12:30 Workshop Ends (no lunch provided)</div>Jchhttp://www.cmb-s4.org/wiki/index.php?title=File:JCH_Matter_Mapping.pdf&diff=9680File:JCH Matter Mapping.pdf2019-10-17T15:48:55Z<p>Jch: </p>
<hr />
<div></div>Jchhttp://www.cmb-s4.org/wiki/index.php?title=UCSD-2019:_Science_Theme:_Matter_Mapping&diff=9565UCSD-2019: Science Theme: Matter Mapping2019-10-15T22:03:47Z<p>Jch: /* 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 />
<br />
<br />
== Agenda ==<br />
<br />
- Review of previous work and science case(s) [10 min]<br />
<br />
- Presentations on additional science and new ideas [5+2 min each]<br />
* Srini Raghunathan: CMB-cluster lensing and tSZ counts<br />
* Siavash Yasini: Birkinshaw-Gull effect<br />
* Selim Hotinli: Rees-Sciama and/or moving lens effect<br />
* Giulio Fabbian [remote]: NG lensing biases<br />
* Alex van Engelen: thermal correction to kSZ<br />
* Nick Battaglia: SZ systematics<br />
<br />
- Focused discussions: [~1 hr]<br />
* Further developing science cases: deep survey at the Pole -- e.g., overlap with deep satellite observations, possibilities for cross-correlations<br />
* Review/update/prioritize questions to be answered regarding measurement requirements -- what needs to be done for CD-1? what needs to be done better than it was in the DSR?<br />
<br />
== Remote attendance ==<br />
<br />
[https://ucsd.zoom.us/j/988412674 Zoom link]<br />
<br />
== Notes ==</div>Jchhttp://www.cmb-s4.org/wiki/index.php?title=UCSD-2019:_Science_Theme:_Matter_Mapping&diff=9564UCSD-2019: Science Theme: Matter Mapping2019-10-15T22:03:32Z<p>Jch: /* 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 />
<br />
<br />
== Agenda ==<br />
<br />
- Review of previous work and science case(s) [10 min]<br />
<br />
- Presentations on additional science and new ideas [5+2 min each]<br />
* Srini Raghunathan: CMB-cluster lensing and tSZ counts<br />
* Siavash Yasini: Birkinshaw-Gull effect<br />
* Selim Hotinli: Rees-Sciama and/or moving lens effect<br />
* Giulio Fabbian [remote]: NG lensing biases<br />
* Alex van Engelen: thermal correction to kSZ<br />
* Nick Battaglia: SZ systematics<br />
<br />
- Focused discussions: (~1 hr)<br />
* Further developing science cases: deep survey at the Pole -- e.g., overlap with deep satellite observations, possibilities for cross-correlations<br />
* Review/update/prioritize questions to be answered regarding measurement requirements -- what needs to be done for CD-1? what needs to be done better than it was in the DSR?<br />
<br />
== Remote attendance ==<br />
<br />
[https://ucsd.zoom.us/j/988412674 Zoom link]<br />
<br />
== Notes ==</div>Jchhttp://www.cmb-s4.org/wiki/index.php?title=UCSD-2019:_Science_Theme:_Matter_Mapping&diff=9563UCSD-2019: Science Theme: Matter Mapping2019-10-15T22:03:10Z<p>Jch: /* 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 />
<br />
<br />
== Agenda ==<br />
<br />
- Review of previous work and science case(s) [10 min]<br />
<br />
- Presentations on additional science and new ideas [5+2 min each]<br />
* Srini Raghunathan: CMB-cluster lensing and tSZ counts<br />
* Siavash Yasini: Birkinshaw-Gull effect<br />
* Selim Hotinli: Rees-Sciama and/or moving lens effect<br />
* Giulio Fabbian [remote]: NG lensing biases<br />
* Alex van Engelen: thermal correction to kSZ<br />
* Nick Battaglia: SZ systematics<br />
<br />
- Focused discussions: (~1 hr)<br />
* Further developing science cases: deep survey at the Pole -- e.g., overlap with deep satellite observations, possibilities for cross-correlations<br />
* Review/update/prioritize questions to be answered regarding measurement requirements -- what needs to be done for CD-1? what needs to be done better than it was in the DSR?<br />
<br />
== Remote attendance ==<br />
<br />
[https://ucsd.zoom.us/j/988412674 Zoom link]<br />
<br />
== Notes ==</div>Jchhttp://www.cmb-s4.org/wiki/index.php?title=Survey_Performance_Expectations&diff=9034Survey Performance Expectations2019-06-10T22:39:43Z<p>Jch: added 190604d noise curves</p>
<hr />
<div>This page summarizes the various survey performance expectations (previously called "experiment definitions.")<br />
The data products referred to are located on the NERSC system under '''/project/projectdirs/cmbs4/expt_xx'''<br />
<br />
===Large-area Survey Performance Expectation 01===<br />
The NTT should fill in here what they can, with input from large-area forecasters where needed. <br />
Ideally there would be separate specifications of instrument capabilities, and assumed sky coverage, rather than<br />
having these lumped together.<br />
<br />
The numbers below are based on the Noise Tiger Team code lat-noise-181002.py (but 181016 yields the same numbers), run assuming the default settings and fsky=0.4. The default settings include 2 LATs, each equipped with 1 ULF tube, 2 LF tubes, 12 MF tubes, and 4 UHF tubes. Note that the EE and BB noise levels are sqrt(2) higher than the TT noise levels and are omitted from the table below for brevity. The atmospheric treatment and other details are described in the code and in the lat-noise-*.pdf document linked below.<br />
<br />
{| class="wikitable" style="text-align: right; margin-left: 51px;"<br />
! Frequency (GHz) !! 20 !! 27 !! 39 !! 93 !! 145 !! 225 !! 280<br />
|-<br />
| Bandwidth (GHz) || n/a || n/a || n/a || n/a || n/a || n/a || n/a<br />
|-<br />
| # of optics tubes || 1 || colspan="2"| 2 || colspan="2"| 12 || colspan="2"| 4<br />
|-<br />
| Beam FWHM (arcmin) || 10. || 7.4 || 5.1 || 2.2 || 1.4 || 1.0 || 0.9<br />
|-<br />
| white noise level TT (uK-arcmin) || 45.9 || 15.5 || 8.7 || 1.5 || 1.5 || 4.8|| 11.5<br />
|-<br />
|}<br />
<br />
Full noise model:<br />
* 190311 (latest): [[File:lat-noise-190311-py.txt]], [[File:lat-noise-190311.pdf]]<br />
** Significant change to white noise dependence on elevation. (Still no change to elev=50 results.)<br />
* 181121: [[File:lat-noise-181121-py.txt]], [[File:lat-noise-181121.pdf]]<br />
** This should be almost identical to 181016, if elevation=50 deg (the default) is used.<br />
* 181016: [[File:lat-noise-181016-py.txt]], [[File:lat-noise-181016.pdf]]<br />
* 181002: [[File:lat-noise-181002-py.txt]], [[File:lat-noise-181002.pdf]]<br />
<br />
Updated post-component-separation noise curves from Colin H. (190604d LAT noise model):<br />
http://sns.ias.edu/~jch/S4_190604d_2LAT_Tpol_default_noisecurves.tgz<br />
N.B. if you use these in a S/N or Fisher calculation, the effective fsky values to use are fsky_signal = 0.42 and fsky_noise = 0.45.<br />
File name conventions are described in detail below.<br />
<br />
(Out of date: Post-component-separation (harmonic-space ILC) noise curves from Colin H.: http://sns.ias.edu/~jch/S4_2LAT_Tpol_default_noisecurves.tgz )<br />
<br />
The file name conventions are very similar to those from the Simons Observatory noise files located at https://simonsobservatory.org/assets/supplements/20180822_SO_Noise_Public.tgz . In the S4 case, there is only one sensitivity option (labeled "SENS0", but this doesn't mean anything, it's just the default S4 setup). There is also only one fsky option (16000 deg^2, i.e., 40%). <br />
<br />
I include results for both temperature and polarization observables. Each temperature file contains three columns:<br />
[ell] [N(ell)^TT in uK^2] [N(ell)^yy]<br />
<br />
Each polarization file also contains three columns:<br />
[ell] [N(ell)^EE in uK^2] [N(ell)^BB in uK^2]<br />
<br />
The "deproj" conventions are identical to what is described in the SO science paper (deproj0 = standard ILC, deproj1 = tSZ or CMB deprojected for CMB or tSZ reconstruction, etc) -- see Sec. 2 of https://arxiv.org/abs/1808.07445 . Contact jch 'at' ias.edu if anything is unclear, and/or please refer to Sec. 2 of the SO paper.<br />
<br />
IMPORTANT: these noise curves should not necessarily be used naively down to the lowest multipoles. They do not include the effects of ground pickup or other systematics that generate significant additional large-scale noise. A reasonable lower limit (which matches the SO forecasting) is to use ell_min = 30. Planck data can be used on larger scales. See Sec. 2.6 of the SO paper for details on how this was done in that work.<br />
<br />
I also include pure inverse-covariance-weighted noise curves for both TT and EE/BB (i.e., with zero foregrounds).<br />
<br />
I also include the CMB lensing reconstruction noise for the TT and EB estimators (for each of the deproj options), but people should probably re-compute this using their codes (I just used the standard QE, which is of course sub-optimal here, and I also only went down to L ~ 40).<br />
<br />
====Alternative Large-area Survey Performance Expectations====<br />
Scaling from the the Expectation 01 table above, other frequency combinations (including 350 GHz) are explored by Mike Niemack and Steve Choi below. <br />
<br />
=====Large-area Survey 02=====<br />
with emphasis on foreground channels<br />
{| class="wikitable" style="text-align: right; margin-left: 51px;"<br />
! Frequency (GHz) !! 20 !! 27 !! 39 !! 93 !! 145 !! 225 !! 280 !! 350<br />
|-<br />
| # of optics tubes || 0 || colspan="2"| 4 || colspan="2"| 9 || colspan="2"| 4|| 2<br />
|-<br />
| Beam FWHM (arcmin) || 10. || 7.4 || 5.1 || 2.2 || 1.4 || 1.0 || 0.9 || 0.7 <br />
|-<br />
| white noise level TT (uK-arcmin) || n/a || 11.0 || 6.2 || 1.73 || 1.73 || 4.8 || 11.5 || 58.9<br />
|-<br />
|}<br />
<br />
=====Large-area Survey 03=====<br />
with emphasis on 350 GHz<br />
{| class="wikitable" style="text-align: right; margin-left: 51px;"<br />
! Frequency (GHz) !! 20 !! 27 !! 39 !! 93 !! 145 !! 225 !! 280 !! 350<br />
|-<br />
| # of optics tubes || 0 || colspan="2"| 2 || colspan="2"| 12 || colspan="2"| 2 || 3<br />
|-<br />
| Beam FWHM (arcmin) || 10. || 7.4 || 5.1 || 2.2 || 1.4 || 1.0 || 0.9 || 0.7 <br />
|-<br />
| white noise level TT (uK-arcmin) || n/a || 15.5 || 8.7 || 1.50 || 1.50 || 6.8 || 16.3 || 48.1<br />
|-<br />
|}<br />
<br />
=====Large-area Survey 04=====<br />
with minor shift towards higher frequencies compared to nominal configuration 01<br />
{| class="wikitable" style="text-align: right; margin-left: 51px;"<br />
! Frequency (GHz) !! 20 !! 27 !! 39 !! 93 !! 145 !! 225 !! 280 !! 350<br />
|-<br />
| # of optics tubes || 0 || colspan="2"| 2 || colspan="2"| 13 || colspan="2"| 3 || 1<br />
|-<br />
| Beam FWHM (arcmin) || 10. || 7.4 || 5.1 || 2.2 || 1.4 || 1.0 || 0.9 || 0.7 <br />
|-<br />
| white noise level TT (uK-arcmin) || n/a || 15.5 || 8.7 || 1.44 || 1.44 || 5.5 || 13.3 || 83.2<br />
|-<br />
|}<br />
<br />
=====Large-area Survey 05=====<br />
with emphasis on 90/150 GHz<br />
{| class="wikitable" style="text-align: right; margin-left: 51px;"<br />
! Frequency (GHz) !! 20 !! 27 !! 39 !! 93 !! 145 !! 225 !! 280 !! 350<br />
|-<br />
| # of optics tubes || 0 || colspan="2"| 2 || colspan="2"| 15 || colspan="2"| 2 || 0<br />
|-<br />
| Beam FWHM (arcmin) || 10. || 7.4 || 5.1 || 2.2 || 1.4 || 1.0 || 0.9 || 0.7 <br />
|-<br />
| white noise level TT (uK-arcmin) || n/a || 15.5 || 8.7 || 1.34 || 1.34 || 6.8 || 16.3 || n/a<br />
|-<br />
|}<br />
<br />
=====Large-area Survey 06=====<br />
with emphasis on low frequencies<br />
{| class="wikitable" style="text-align: right; margin-left: 51px;"<br />
! Frequency (GHz) !! 20 !! 27 !! 39 !! 93 !! 145 !! 225 !! 280 !! 350<br />
|-<br />
| # of optics tubes || 2 || colspan="2"| 3 || colspan="2"| 11 || colspan="2"| 3 || 0<br />
|-<br />
| Beam FWHM (arcmin) || 10. || 7.4 || 5.1 || 2.2 || 1.4 || 1.0 || 0.9 || 0.7 <br />
|-<br />
| white noise level TT (uK-arcmin) || 32.5 || 12.7 || 7.1 || 1.57 || 1.57 || 5.5 || 13.3 || n/a<br />
|-<br />
|}<br />
<br />
===Small-area Survey Performance Expectation 05===<br />
<br />
Victor provided the tables below 11/27/18 scaled from BK14 published bandpower covariance matrix.<br />
They are designed to be apples-to-apples comparable<br />
to the 04 tables below.<br />
They assume 3% nominal sky coverage, as did the previous table, even though the Chile coverage<br />
will of course be much larger.<br />
When we run map based sim using the numbers below the scaling to Pole and Chile coverage will be done in the same way as to was for 04 sets (04b and 04c)<br />
(see [[Sims_with_nominal_Chile_and_Pole_masks]]) to ensure apples-to-apples comparison.<br />
<br />
The appropriate delensing factors to use for 7 years are apparently 0.081 and 0.27 for Pole/Chile taken from<br />
[https://docs.google.com/spreadsheets/d/1i_GU6hZKhxmBb64vhgr4rkRrERvl8Lz5YaZO0-dWjn0 this spreadsheet]<br />
<br />
S4 Pole — 7 years with 12 tubes of Config 5 [https://docs.google.com/spreadsheets/d/1B9A5-IYr1wAbOUgFDcnYv7q0_WXgXNU7EhlfBRqavm Link] over nominal 3% sky<br />
<br />
{| class="wikitable" style="text-align: right; margin-left: 51px;"<br />
! Frequency (GHz) !! 20 !! 30 !! 40 !! 85 !! 95 !! 145 !! 155 !! 220 !! 270<br />
|-<br />
| Bandwidth (GHz) || 5.0 || 9.0 || 12.0 || 20.4 || 22.8 || 31.9 || 34.1 || 48.4 || 59.4<br />
|-<br />
| Beam FWHM (arcmin) || 11.0 || 72.8 || 72.8 || 25.5 || 25.5 || 22.7 || 22.7 || 13.0 || 13.0<br />
|-<br />
| white noise level TT (uK-arcmin) || 16.55 || 9.36 || 11.85 || 2.02 || 1.78 || 3.89 || 4.16 || 10.15 || 17.40<br />
|-<br />
| ell knee TT || 500 || 150 || 150 || 150 || 150 || 230 || 230 || 230 || 230<br />
|-<br />
| 1/f exponent TT || -4.4 || -4.4 || -4.4 || -4.4 || -4.4 || -3.8 || -3.8 || -3.8 || -3.8<br />
|-<br />
| white noise level EE (uK-arcmin) || 10.87 || 6.20 || 7.85 || 1.34 || 1.18 || 1.80 || 1.93 || 4.71 || 8.08 <br />
|-<br />
| ell knee EE || 200 || 60 || 60 || 60 || 60 || 65 || 65 || 65 || 65<br />
|-<br />
| 1/f exponent EE || -2.2 || -2.2 || -2.2 || -2.2 || -2.2 || -3.1 || -3.1 || -3.1 || -3.1<br />
|-<br />
| white noise level BB (uK-arcmin) || 10.23 || 5.85 || 7.40 || 1.27 || 1.12 || 1.76 || 1.89 || 4.60 || 7.89<br />
|-<br />
| ell knee BB || 200 || 60 || 60 || 60 || 60 || 60 || 60 || 60 || 60<br />
|-<br />
| 1/f exponent BB || -1.7 || -1.7 || -1.7 || -1.7 || -1.7 || -3.0 || -3.0 || -3.0 || -3.0<br />
|-<br />
| ell min || 30 || 30 || 30 || 30 || 30 || 30 || 30 || 30 || 30 <br />
|-<br />
| nside || 512 || 512 || 512 || 512 || 512 || 512 || 512 || 512 || 512<br />
|}<br />
<br />
S4 Chile — 7 years with 6 tubes of Config 9 [https://docs.google.com/spreadsheets/d/1B9A5-IYr1wAbOUgFDcnYv7q0_WXgXNU7EhlfBRqavm Link] over nominal 3% sky and assuming same<br />
observing efficiency as Pole.<br />
<br />
{| class="wikitable" style="text-align: right; margin-left: 51px;"<br />
! Frequency (GHz) !! 20 !! 30 !! 40 !! 85 !! 95 !! 145 !! 155 !! 220 !! 270<br />
|-<br />
| Bandwidth (GHz) || 5.0 || 9.0 || 12.0 || 20.4 || 22.8 || 31.9 || 34.1 || 48.4 || 59.4<br />
|-<br />
| Beam FWHM (arcmin) || 11.0 || 72.8 || 72.8 || 31.9 || 31.9 || 28.4 || 28.4 || 13.0 || 13.0<br />
|-<br />
| white noise level TT (uK-arcmin) || 16.55 || 7.44 || 9.42 || 3.08 || 2.72 || 5.92 || 6.34 || 17.58 || 30.14<br />
|-<br />
| ell knee TT || 500 || 150 || 150 || 150 || 150 || 230 || 230 || 230 || 230<br />
|-<br />
| 1/f exponent TT || -4.4 || -4.4 || -4.4 || -4.4 || -4.4 || -3.8 || -3.8 || -3.8 || -3.8<br />
|-<br />
| white noise level EE (uK-arcmin) || 10.87 || 4.93 || 6.24 || 2.04 || 1.80 || 2.74 || 2.94 || 8.16 || 14.00 <br />
|-<br />
| ell knee EE || 200 || 60 || 60 || 60 || 60 || 65 || 65 || 65 || 65<br />
|-<br />
| 1/f exponent EE || -2.2 || -2.2 || -2.2 || -2.2 || -2.2 || -3.1 || -3.1 || -3.1 || -3.1<br />
|-<br />
| white noise level BB (uK-arcmin) || 10.23 || 4.65 || 5.88 || 1.93 || 1.71 || 2.68 || 2.88 || 7.97 || 13.67<br />
|-<br />
| ell knee BB || 200 || 60 || 60 || 60 || 60 || 60 || 60 || 60 || 60<br />
|-<br />
| 1/f exponent BB || -1.7 || -1.7 || -1.7 || -1.7 || -1.7 || -3.0 || -3.0 || -3.0 || -3.0<br />
|-<br />
| ell min || 30 || 30 || 30 || 30 || 30 || 30 || 30 || 30 || 30 <br />
|-<br />
| nside || 512 || 512 || 512 || 512 || 512 || 512 || 512 || 512 || 512<br />
|}<br />
<br />
The effort at 20 GHz is constant and assumes 135 det per year for 7 years regardless of site<br />
<br />
The numbers in the second table were determined using the following scaling of the first table: <br />
<br />
- det counts at pole (7 years * nr_tubes * nr of det per tube) = [2016,2016,98784,98784,98784,98784,177282,177282] at [30,40,85,95,145,155,220,270]GHz<br />
<br />
x1 = 7.*[1,1,4,4,4,4,3,3].*[288, 288, 3528, 3528, 3528, 3528, 8442, 8442]<br />
<br />
- det counts in chile (7 years * nr_tubes * nr of det per tube) = [3192,3192,42588,42588,42588,42588,59094,59094]<br />
<br />
x2 = 7.*[1,1,2,2,2,2,1,1].*[456, 456, 3042, 3042, 3042, 3042, 8442, 8442]<br />
<br />
- sqrt of det count ratios to scale the Pole numbers by<br />
<br />
sqrt(x1./x2) = 0.7947 0.7947 1.5230 1.5230 1.5230 1.5230 1.7321 1.7321<br />
<br />
=== Experiment Definition 04 ===<br />
This is very similar to 02 but with the noise levels tweaked down by sqrt(7/6) to try and get sigma(r)=1e-4 as per science requirement.<br />
(The noise map generator has also been tweaked such that the level quoted in the params.dat table will be reproduced exactly when the power spectra of the maps is taken with the provided mask - i.e. the actual noise level will slightly lower in the center of the mask.)<br />
A 20GHz band has been added which is assumed to be on a large aperture telescope (and hence has higher resolution and ell knee).<br />
Below is the contents of the params.dat file. The noise levels and resolutions are copied from the [https://www.nsf.gov/mps/ast/aaac/cmb_s4/report/CMBS4_final_report_NL.pdf CDT report] "Science Traceability Matrix".<br />
Specs for the high res bands exist but have not been added yet. <br />
<br />
Set 04 is the same idealized circular 3% sky patch as set 02.<br />
We also add 04b which is a for a nominal Chile realistic mask<br />
and 04c which is a realistic Pole mask (actually the BICEP3 2017 as observed mask). See [[Sims_with_nominal_Chile_and_Pole_masks | this logbook posting]] for details.<br />
<br />
{| class="wikitable" style="text-align: right; margin-left: 51px;"<br />
! Frequency (GHz) !! 20 !! 30 !! 40 !! 85 !! 95 !! 145 !! 155 !! 220 !! 270<br />
|-<br />
| Bandwidth (GHz) || 5.0 || 9.0 || 12.0 || 20.4 || 22.8 || 31.9 || 34.1 || 48.4 || 59.4<br />
|-<br />
| Beam FWHM (arcmin) || 11.0 || 76.6 || 57.5 || 27.0 || 24.2 || 15.9 || 14.8 || 10.7 || 8.5<br />
|-<br />
| white noise level TT (uK-arcmin) || 16.66 || 10.62 || 10.07 || 2.01 || 1.59 || 4.53 || 4.53 || 11.61 || 15.84<br />
|-<br />
| ell knee TT || 500 || 175 || 175 || 175 || 175 || 230 || 230 || 230 || 230<br />
|-<br />
| 1/f exponent TT || -4.1 || -4.1 || -4.1 || -4.1 || -4.1 || -3.8 || -3.8 || -3.8 || -3.8<br />
|-<br />
| white noise level EE (uK-arcmin) || 13.94 || 8.88 || 8.42 || 1.67 || 1.32 || 2.12 || 2.12 || 5.43 || 7.42 <br />
|-<br />
| ell knee EE || 200 || 50 || 50 || 50 || 50 || 65 || 65 || 65 || 65<br />
|-<br />
| 1/f exponent EE || -2.0 || -2.0 || -2.0 || -2.0 || -2.0 || -3.0 || -3.0 || -3.0 || -3.0<br />
|-<br />
| white noise level BB (uK-arcmin) || 13.6 || 8.67 || 8.22 || 1.64 || 1.30 || 2.03 || 2.03 || 5.19 || 7.08<br />
|-<br />
| ell knee BB || 200 || 50 || 50 || 50 || 50 || 60 || 60 || 60 || 60<br />
|-<br />
| 1/f exponent BB || -2.0 || -2.0 || -2.0 || -2.0 || -2.0 || -3.0 || -3.0 || -3.0 || -3.0<br />
|-<br />
| ell min || 30 || 30 || 30 || 30 || 30 || 30 || 30 || 30 || 30 <br />
|-<br />
| nside || 512 || 512 || 512 || 512 || 512 || 512 || 512 || 512 || 512<br />
|}<br />
<br />
=== Experiment Definition 03, 03b, 03c ===<br />
These sims are nearly identical to experiment definition 02, 02b, 02c, and even use the same noise realizations. The one change is the inclusion of additive systematics, following the prescription described in this [[Additive_systematics_for_data_challenge_03|2017-07-10 posting]]. Blocks of realizations contain different versions of the additive systematic, as shown below. For all cases, the level of the systematic is chosen to yield bias on ''r'' of 1e-4 (by the analysis of the 2017-07-10 posting). The first block of realizations, 0000&ndash;0124, contains no systematic and should be completely identical to the 02/02b/02c realizations.<br />
<br />
{| class="wikitable"<br />
|-<br />
! realizations !! A<sub>uncorr</sub> !! B<sub>uncorr</sub> !! A<sub>corr</sub> !! B<sub>corr</sub> !! Description<br />
|-<br />
| 0000&ndash;0124 || 0 || 0 || 0 || 0 || No systematics<br />
|-<br />
| 0125&ndash;0249 || 0.0328 || 0 || 0 || 0 || Uncorrelated systematic with white spectrum<br />
|-<br />
| 0250&ndash;0374 || 0 || 0.0689 || 0 || 0 || Uncorrelated systematic with 1/ell spectrum<br />
|-<br />
| 0375&ndash;0499 || 0 || 0 || 0.0584 || 0 || Correlated systematic with white spectrum<br />
|-<br />
| 0500&ndash;0624 || 0 || 0 || 0 || 0.1049 || Correlated systematic with 1/ell spectrum<br />
|-<br />
| 0625&ndash;0749 || 0.0164 || 0.0345 || 0 || 0 || Uncorrelated systematic with white + 1/ell spectrum<br />
|-<br />
| 0750&ndash;0874 || 0 || 0 || 0.0292 || 0.0525 || Correlated systematic with white + 1/ell spectrum<br />
|-<br />
| 0875&ndash;0999 || 0.0082 || 0.0172 || 0.0146 || 0.0262 || Uncorrelated + correlated systematic with white + 1/ell spectrum<br />
|}<br />
<br />
Combined maps for analysis can be found on NERSC in '''/project/projectdirs/cmbs4/data_xx.yy/03''' etc.<br />
<br />
Parameters and ingredients for the combined maps can be found in '''/project/projectdirs/cmbs4/expt_xx/03''' etc. Note that noise, rhits, and wfunc are actually symlinks to those directories under experiment configs 02, 02b, 02c.<br />
<br />
=== Experiment Definition 02, 02b, 02c ===<br />
This is an update from 01 which differs in the following ways:<br />
<br />
1) Addition of 20GHz band and (slight) changes to the band/detector optimization as per<br />
[[http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170515_chkS4 Victor's May 15 posting in the logbook]].<br />
<br />
2) Addition of 3 delensing bands 95/145/220GHz with same number of detectors as the low res equivalent bands<br />
but beam size 4x higher. This adds up to approximately the same number of detectors but clearly one should reoptimize<br />
once they are not all at the same freq. Since we are still quite far from having real lensing reconstruction and realistic<br />
(non-Gaussian) high ell foregrounds this probably is OK for this round.<br />
<br />
3) Addition of tensors - even number realizations have r=0.003, odd number have r=0.<br />
<br />
4) Set 02 is the same nominal 3% sky patch as set 01. We now add 02b which is 1% round patch with center<br />
the same as the BICEP/Keck patch (RA=0, Dec=-57.5), and 02c which is 10% round patch centered on RA=15deg, Dec=-35.<br />
<br />
These products appear on NERSC under '''/project/projectdirs/cmbs4/expt_xx/02''' etc.<br />
<br />
=== Experiment Definition 01 ===<br />
This is intended to be basically the same as the assumptions made for the Fisher calculations done for the Science Book.<br />
The parameters come from [[http://users.physics.harvard.edu/~buza/20161220_chkS4 Victor's Dec 21 posting in the logbook]] with the addition of bandwidths from<br />
[[Tophat_bands_for_Data_Challenge|Colin's Nov 4 posting]] and are summarized in the following table:<br />
<br />
{| class="wikitable" style="text-align: right; margin-left: 51px;"<br />
! Frequency (GHz) !! 30 !! 40 !! 85 !! 95 !! 145 !! 155 !! 220 !! 270 !! 155 HR<br />
|-<br />
| Bandwidth (GHz) || 9.0 || 12.0 || 20.4 || 22.8 || 31.9 || 34.1 || 48.4 || 59.4 || 34.1<br />
|-<br />
| Beam FWHM (arcmin) || 76.6 || 57.5 || 27.0 || 24.2 || 15.9 || 14.8 || 10.7 || 8.5 || 4.0<br />
|-<br />
| white noise level TT (uK-arcmin) || 12.97 || 13.22 || 2.30 || 1.89 || 5.31 || 5.48 || 11.86 || 17.72 || 5.48<br />
|-<br />
| ell knee TT || 175 || 175 || 175 || 175 || 230 || 230 || 230 || 230 || 500<br />
|-<br />
| 1/f exponent TT || -4.1 || -4.1 || -4.1 || -4.1 || -3.8 || -3.8 || -3.8 || -3.8 || -3.8<br />
|-<br />
| white noise level EE (uK-arcmin) || 10.85 || 11.06 || 1.93 || 1.58 || 2.49 || 2.56 || 5.55 || 8.30 || 2.56 <br />
|-<br />
| ell knee EE || 50 || 50 || 50 || 50 || 65 || 65 || 65 || 65 || 200<br />
|-<br />
| 1/f exponent EE || -2.0 || -2.0 || -2.0 || -2.0 || -3.0 || -3.0 || -3.0 || -3.0 || -3.0<br />
|-<br />
| white noise level BB (uK-arcmin) || 10.59 || 10.79 || 1.88 || 1.54 || 2.38 || 2.45 || 5.30 || 7.93 || 2.45<br />
|-<br />
| ell knee BB || 50 || 50 || 50 || 50 || 60 || 60 || 60 || 60 || 200<br />
|-<br />
| 1/f exponent BB || -2.0 || -2.0 || -2.0 || -2.0 || -3.0 || -3.0 || -3.0 || -3.0 || -3.0<br />
|-<br />
| ell min || 30 || 30 || 30 || 30 || 30 || 30 || 30 || 30 || 100<br />
|-<br />
| nside || 512 || 512 || 512 || 512 || 512 || 512 || 512 || 512 || 2048<br />
|}<br />
<br />
These parameters are in the file '''expt_xx/01/params.dat''' and give rise to the window functions in '''expt_xx/01/wfunc''' and the noise spectra in '''expt_xx/01/noise/cls'''.<br />
The intent of the low ell cutoff is to approximate the effect of the timestream filtering which is commonly done in ground based experiments (and as some kind of acknowledgement that<br />
the largest angular scales may anyway be corrupted by systematic effects).<br />
<br />
Additionally '''expt_xx/01/rhits/fsky03bk_n0512.fits''' is supposed to represent the "relative hits" with which the sky has been observed.<br />
This is a circular pattern centred at RA=0, Dec=-45 (a bit below the BICEP/Keck patch) which is flat at one out to r=12deg and then rolls down to zero as cosine squared over an<br />
additional 15 deg.<br />
This is some kind of approximation as to what small apertures might deliver (given their large instantaneous field of view).<br />
<br />
From the noise spectra sets of alms are generated (with nlmax=4096) with names like '''expt_xx/01/noise/alm/noise_f155_b15_ellmin30_alm_mc_0000.fits''' where 155 is the frequency, 15 is the beam size (in arcmin), and 0000 is the realization number. <br />
<br />
From these full sky maps are rendered at nside=512 and nlmax=1024. No beam smoothing is applied as is appropriate for noise.<br />
The maps have names like '''expt_xx/01/noise/map/noise_f155_b15_ellmin30_map_0512_mc_0000.fits'''.<br />
<br />
The full sky noise is then divided by the square-root of the rhits mask and the result stored in files like '''data_xx.yy/01.YY/cmbs4_01_noise_f155_b15_ellmin30_map_0512_mc_0000.fits''' - these are the noise realizations that one would have access to in a real experiment - the noise blows up around the edge.<br />
<br />
These masked noise realizations are then added to the sky model (LCDM+dust+sync+) and stored in names like '''data_xx.yy/01.YY/cmbs4_01pYY_comb_f155_b15_ellmin30_map_0512_mc_0000.fits'''.<br />
As a crude simulation of delensing these combined maps are also provided with the lensing effect reduced to 30, 10 and 3% of reality by combining lensed and unlensed LCDM - look for files<br />
with names like '''data_xx.yy/01.YY/cmbs4_01pYY_comb_AL0p3_f155_b15_ellmin30_map_0512_mc_0000.fits'''.<br />
Maps with partial lensing are constructed by the following combination: partially_lensed_map = sqrt(A_L) * lensed_map + (1 - sqrt(A_L)) * unlensed_map.<br />
<br />
To analyze these maps one should use only the '''expt_xx/01/params.dat''' file and the maps under '''data_xx.yy/01.YY'''.<br />
A thousand realizations are present.<br />
We can see these maps [[01.00 sim input maps | in this posting]]<br />
<br />
The last column of the table above shows one additional tweak - a second 155GHz band with a higher 1/f knee and smaller beam size - this is supposed to<br />
represent the maps made by higher resolution telescopes running in concert with small apertures in a hybrid approach.<br />
These maps can in principle be used to reconstruct the lensing potential and delens explicitly - instead of cheating by using<br />
the AL0p3 files etc.<br />
At the moment the noise spectrum in these maps is provisional.<br />
Additionally we may wish to add additional frequency bands at higher resolution so foreground cleaning<br />
before delensing can be done.<br />
We can see these maps [[Adding higher res delensing "band" | in this posting]].<br />
<br />
(The filtered LLCDM realizations are also copied in '''data_xx.yy/01.YY''' as these are needed to build the bandpower covariance matrix in the multi-component cross spectrum approach used by the BK group.<br />
It seems reasonable that one would always have realizations of a known spectrum signal passed through an experimental simulation.)</div>Jchhttp://www.cmb-s4.org/wiki/index.php?title=Requirements_Flowdown&diff=8889Requirements Flowdown2019-04-22T18:28:26Z<p>Jch: /* Materials */</p>
<hr />
<div>This page tracks work towards refining the links and traceability between Science requirements, measurement requirements and system/instrument requirements. The immediate goal is to converge on a Science Traceability Matrix (see CDT STM linked below for example) in time for the Decadal Survey Review in mid 2019. The STM needs to be backed by clear, crisp evidence explaining our choices in survey and instrument strategy.<br />
<br />
===Meetings===<br />
<br />
''Science Collaboration Flowdown meeting (coordinated by J3)''<br />
* Membership: ET, SC, TC, Project team<br />
* Biweekly starting Feb 11, 11am pacific/2pm eastern<br />
* [http://uberconference.com/cmbs4a Uberconference cmbs4a]<br />
* (866-578-4799 or 480-999-2448)<br />
* [https://docs.google.com/document/d/1H0cKBe9BNCRVk5HK-dqXzKXUs4z0ivcfRTYlROeQE_E/edit?usp=sharing Notes for Julian's flowdown call]<br />
<br />
''Project Flowdown Assessment working group (coordinated by Natalie and Zeesh)''<br />
* Membership: Darcy Barron, Chris Sheehy, Chris Bebek, Nadine Kurita, Martin Nordby, Natalie Roe, Zeesh Ahmed<br />
* Searching for a new meeting time..<br />
* [https://docs.google.com/document/d/1fOuWPfW84Imj-_Dmhf9P2I2eI3VpfTKuOR7cC1JCm_M/edit# Notes for project system engineering]<br />
<br />
===Materials===<br />
As a first step, we will use the following spreadsheet to make sure we have links to basis documentation backing the various requirements that the collaboration has already identified. This tool will also help us identify holes in the flowdown that need to be filled.<br />
<br />
* [https://docs.google.com/spreadsheets/d/1EE25NskNqN5B7pOK0IPGbLkZopcRuhLDwssE1r56pkQ/edit?usp=sharing CMB-S4 requirements traceability spreadsheet]<br />
* [https://docs.google.com/document/d/1SlsVKL-bHGR7tp7x_c1zB8AdgrqxWjOpbO3r3hDLSs8/edit?usp=sharing Elements of Flowdown to be completed before FNAL meeting]<br />
* [https://docs.google.com/document/d/1Gb0dgVC-TCo7YWeEfP1fSo2HtQ2S0HIXrf0Mg_z6Tpk/edit Link to PGW flowdown notes]<br />
* Link to Neff flowdown notes<br />
* Link to Legacy Survey: Mass Mapping flowdown wiki to be placed here. [https://docs.google.com/document/d/1-duNRqdsYLABtVh_Alx-tFPaNQL3PySbonj0UN4CD94/edit?usp=sharing Draft page here.]<br />
* Link to Legacy Survey: Baryon Mapping flowdown wiki to be placed here. [https://docs.google.com/document/d/1yi1GNXpk_-rZXQLflZNvQc9BRupbw3F7O-oFtZWibzQ/edit?usp=sharing Draft page here.]<br />
* Link to Legacy Survey: Time Domain flowdown wiki to be placed here [[Transients]]<br />
* LAT (non-Neff) frequency channel flowdown (Colin H.): [[LAT Frequency Flowdown]]<br />
<br />
===Reference documents===<br />
* CDT Science traceability matrix [[file:CDT_STM.pdf]]<br />
* DESI requirements tracker and SRD [[File:DESI_L123_driver.pdf]]</div>Jchhttp://www.cmb-s4.org/wiki/index.php?title=LAT_Frequency_Flowdown&diff=8888LAT Frequency Flowdown2019-04-22T18:27:24Z<p>Jch: </p>
<hr />
<div>=== Summary ===<br />
(Colin Hill writing 4-22-19)<br />
<br />
In this posting I present the results of "flowdown" (i.e., optimization) calculations for the frequency channel distribution of the CMB-S4 LATs.<br />
<br />
=== Setup and Assumptions ===<br />
<br />
I use the noise calculator for the CMB-S4 LATs posted at https://cmb-s4.org/wiki/images/Lat-noise-190311-py.txt<br />
<br />
This noise calculator allows one to vary the sky fraction surveyed (fsky) and the number of optics tubes of each type (LF, MF, UHF). For reference, LF = 27 and 39 GHz, MF = 93 and 145 GHz, UHF = 225 and 280 GHz. I do not consider the 20 GHz channel (ULF) in this work, as its resolution is low enough as to likely be irrelevant for LAT science. I consider fsky = 0.1, 0.2, and 0.4, and all possible optics tube configurations with 18 total tubes (assuming there is 19th tube used for the ULF). I also impose a constraint that there is at least one MF tube, since these are clearly the main 'science frequencies'. This yields a total of 3420 possible configurations. Note that I assume two identical copies of the LAT, in order to reduce the computational complexity. If desired, one could run a full optimization of all 36 optics tubes.<br />
<br />
I also run calculations using a modified version of the S4 noise calculator (via Matthew Hasselfield) that allows for the possibility of "XHF" optics tubes, where XHF = 281 and 350 GHz. The atmosphere for these tubes is assumed to match CCAT site specifications.<br />
<br />
I include Planck data (30 - 353 GHz) in all calculations, as these channels are useful on large angular scales where the S4 atmospheric noise is large.<br />
<br />
=== Methodology ===<br />
<br />
I focus on temperature-based observables in the following: thermal SZ, kinematic SZ, CMB lensing via the TT quadratic estimator, and the CMB TT power spectrum. I model the temperature sky at all frequencies from 27 to 353 GHz (13 channels, or 15 when including XHF tubes) using the simulated sky maps described in Sec. 2 of https://arxiv.org/abs/1808.07445 . These maps are also available at https://lambda.gsfc.nasa.gov/toolbox/tb_cmbsim_ov.cfm<br />
<br />
I use simple Galactic-emission-thresholded sky masks that leave the cleanest 10%, 20%, or 40% of the sky that is visible from Chile. These are identical to the sky masks used in https://arxiv.org/abs/1808.07445<br />
<br />
For each fsky and optics tube configuration option, I use a harmonic-space ILC code to obtain "post-component-separation" noise power spectra for the blackbody CMB temperature and Compton-y fields, using the modeled sky power spectra and the per-frequency noise power spectra computed using the S4 calculator (as well as Planck noise, assumed to be white). I consider the option of explicitly "deprojecting" some contaminants using a constrained ILC, which is a robust way to conservatively assess the frequency coverage that may be needed to sufficiently remove these foregrounds. I consider three deprojection options: no deprojection, deprojection of tSZ (for CMB reconstruction) or CMB (for tSZ reconstruction), and deprojection of a fiducial CIB spectrum (for CMB and tSZ reconstruction). The total number of fsky/configuration/deprojection options is thus 10260.<br />
<br />
For each fsky and optics tube configuration option (and deprojection option), I then compute the S/N on four observables: tSZ power spectrum, kSZ power spectrum (conservatively considering only ell>3000), CMB lensing power spectrum via the TT estimator (effectively also a proxy for CMB halo lensing, which is dominated by TT), and the CMB TT power spectrum. These S/N values are used as the 'optimization metric' for 'flowdown', i.e., I seek configurations that maximize these S/N values.<br />
<br />
=== Results ===<br />
<br />
General result, valid for all observables and all deprojection options: going wide (fsky=0.4) is always optimal for the S/N of all these observables. Even for the kSZ power spectrum, the S4 noise is sufficiently low (i.e., we are close enough to hitting sample variance on a range of modes) that going wide is preferred over going deep. I do not list fsky in the optimal configurations below because it is always 0.4.<br />
<br />
I also explicitly highlight below the performance of the fiducial configuration used in all previous calculations (fsky=0.4, LF=2, MF=12, UHF=4).<br />
<br />
'''No deprojection''', aka 'standard ILC':<br />
<br />
There are many joint-optimal configurations that yield S/N values within 93% of maximum for all observables. Reasonable-looking ones include:<br />
<br />
LF=1, MF=10, UHF=7<br />
<br />
LF=1, MF=11, UHF=6<br />
<br />
LF=1, MF=12, UHF=5<br />
<br />
LF=1, MF=13, UHF=4<br />
<br />
LF=1, MF=14, UHF=3<br />
<br />
LF=2, MF=10, UHF=6<br />
<br />
LF=2, MF=11, UHF=5<br />
<br />
LF=2, MF=12, UHF=4<br />
<br />
LF=2, MF=13, UHF=3<br />
<br />
LF=2, MF=14, UHF=2<br />
<br />
<br />
If XHF tubes are considered, the joint-optimal configurations are<br />
<br />
LF=1, MF=9, UHF=5, XHF=3<br />
<br />
LF=1, MF=10, UHF=3, XHF=4<br />
<br />
LF=1, MF=10, UHF=4, XHF=3<br />
<br />
LF=1, MF=11, UHF=2, XHF=4<br />
<br />
LF=1, MF=11, UHF=3, XHF=3<br />
<br />
LF=2, MF=10, UHF=3, XHF=3<br />
<br />
which all yield S/N values within 99% of maximum for all observables.<br />
<br />
''The performance of the fiducial configuration is good for everything here, yielding S/N > 93% of maximum for kSZ, lensing, and CMB, and S/N ~ 88% of maximum for tSZ. I think this would serve as a reasonable baseline 'flowdown' justification for the fiducial choice of bands. Note that the S/N maxima are computed when allowing XHF tubes, so the upshot is that allowing XHF tubes would yield ~10% gains in S/N (for the no-deprojection case; gains are larger in other cases below).''<br />
<br />
<br />
'''Deprojection of tSZ (for CMB) or of CMB (for tSZ)''': <br />
<br />
The joint-optimal configurations are<br />
<br />
LF=1, MF=4, UHF=13<br />
<br />
LF=1, MF=5, UHF=12<br />
<br />
LF=1, MF=6, UHF=11<br />
<br />
LF=1, MF=7, UHF=10<br />
<br />
yielding S/N values within 92% of maximum for all observables.<br />
<br />
<br />
If XHF tubes are considered, there are many configurations with S/N values > 95% of maximum for all observables. Reasonable looking ones include:<br />
<br />
LF=1, MF=8, UHF=4, XHF=5<br />
<br />
LF=1, MF=8, UHF=5, XHF=4<br />
<br />
LF=1, MF=8, UHF=6, XHF=3<br />
<br />
LF=2, MF=5, UHF=6, XHF=5<br />
<br />
''The performance of the fiducial configuration is good for everything except kSZ, yielding S/N > 94% of maximum for tSZ, lensing, and CMB, but S/N ~ 84% of maximum for kSZ (still not too bad).<br />
''<br />
<br />
<br />
'''Deprojection of CIB (for both CMB and tSZ)''':<br />
<br />
The joint-optimal configuration is<br />
<br />
LF=1, MF=6, UHF=11<br />
<br />
yielding S/N values within 93% of maximum for all observables.<br />
<br />
<br />
If XHF tubes are considered, there are many configurations with S/N values > 95% of maximum for all observables. Reasonable looking ones include:<br />
<br />
LF=1, MF=10, UHF=0, XHF=7<br />
<br />
LF=1, MF=10, UHF=1, XHF=6<br />
<br />
LF=1, MF=10, UHF=2, XHF=5<br />
<br />
LF=1, MF=9, UHF=0, XHF=8<br />
<br />
LF=1, MF=9, UHF=1, XHF=7<br />
<br />
LF=1, MF=9, UHF=2, XHF=6<br />
<br />
LF=1, MF=9, UHF=3, XHF=5<br />
<br />
LF=1, MF=9, UHF=4, XHF=4<br />
<br />
''The performance of the fiducial configuration is good for everything except kSZ, yielding S/N > 96% of maximum for tSZ, lensing, and CMB, but S/N ~ 82% of maximum for kSZ (still not too bad).<br />
''<br />
<br />
<br />
=== Conclusions ===<br />
The fiducial configuration performs acceptably well in all cases considered here (generally within ~10% of global optimized configurations). If one considers the possibility of XHF tubes, we could gain up to ~20% in S/N, specifically for cases when imposing deprojection constraints on various foreground contaminants.</div>Jchhttp://www.cmb-s4.org/wiki/index.php?title=LAT_Frequency_Flowdown&diff=8887LAT Frequency Flowdown2019-04-22T18:24:38Z<p>Jch: </p>
<hr />
<div>=== Summary ===<br />
(Colin Hill writing 4-22-19)<br />
<br />
In this posting I present the results of "flowdown" (i.e., optimization) calculations for the frequency channel distribution of the CMB-S4 LATs.<br />
<br />
=== Setup and Assumptions ===<br />
<br />
I use the noise calculator for the CMB-S4 LATs posted at https://cmb-s4.org/wiki/images/Lat-noise-190311-py.txt<br />
<br />
This noise calculator allows one to vary the sky fraction surveyed (fsky) and the number of optics tubes of each type (LF, MF, UHF). For reference, LF = 27 and 39 GHz, MF = 93 and 145 GHz, UHF = 225 and 280 GHz. I do not consider the 20 GHz channel (ULF) in this work, as its resolution is low enough as to likely be irrelevant for LAT science. I consider fsky = 0.1, 0.2, and 0.4, and all possible optics tube configurations with 18 total tubes (assuming there is 19th tube used for the ULF). I also impose a constraint that there is at least one MF tube, since these are clearly the main 'science frequencies'. This yields a total of 3420 possible configurations. Note that I assume two identical copies of the LAT, in order to reduce the computational complexity. If desired, one could run a full optimization of all 36 optics tubes.<br />
<br />
I also run calculations using a modified version of the S4 noise calculator (via Matthew Hasselfield) that allows for the possibility of "XHF" optics tubes, where XHF = 281 and 350 GHz. The atmosphere for these tubes is assumed to match CCAT site specifications.<br />
<br />
I include Planck data (30 - 353 GHz) in all calculations, as these channels are useful on large angular scales where the S4 atmospheric noise is large.<br />
<br />
=== Methodology ===<br />
<br />
I focus on temperature-based observables in the following: thermal SZ, kinematic SZ, CMB lensing via the TT quadratic estimator, and the CMB TT power spectrum. I model the temperature sky at all frequencies from 27 to 353 GHz (13 channels, or 15 when including XHF tubes) using the simulated sky maps described in Sec. 2 of https://arxiv.org/abs/1808.07445 . These maps are also available at https://lambda.gsfc.nasa.gov/toolbox/tb_cmbsim_ov.cfm<br />
<br />
I use simple Galactic-emission-thresholded sky masks that leave the cleanest 10%, 20%, or 40% of the sky that is visible from Chile. These are identical to the sky masks used in https://arxiv.org/abs/1808.07445<br />
<br />
For each fsky and optics tube configuration option, I use a harmonic-space ILC code to obtain "post-component-separation" noise power spectra for the blackbody CMB temperature and Compton-y fields, using the modeled sky power spectra and the per-frequency noise power spectra computed using the S4 calculator (as well as Planck noise, assumed to be white). I consider the option of explicitly "deprojecting" some contaminants using a constrained ILC, which is a robust way to conservatively assess the frequency coverage that may be needed to sufficiently remove these foregrounds. I consider three deprojection options: no deprojection, deprojection of tSZ (for CMB reconstruction) or CMB (for tSZ reconstruction), and deprojection of a fiducial CIB spectrum (for CMB and tSZ reconstruction). The total number of fsky/configuration/deprojection options is thus 10260.<br />
<br />
For each fsky and optics tube configuration option (and deprojection option), I then compute the S/N on four observables: tSZ power spectrum, kSZ power spectrum (conservatively considering only ell>3000), CMB lensing power spectrum via the TT estimator (effectively also a proxy for CMB halo lensing, which is dominated by TT), and the CMB TT power spectrum. These S/N values are used as the 'optimization metric' for 'flowdown', i.e., I seek configurations that maximize these S/N values.<br />
<br />
=== Results ===<br />
<br />
General result, valid for all observables and all deprojection options: going wide (fsky=0.4) is always optimal for the S/N of all these observables. Even for the kSZ power spectrum, the S4 noise is sufficiently low (i.e., we are close enough to hitting sample variance on a range of modes) that going wide is preferred over going deep. I do not list fsky in the optimal configurations below because it is always 0.4.<br />
<br />
I also explicitly highlight below the performance of the fiducial configuration used in all previous calculations (fsky=0.4, LF=2, MF=12, UHF=4).<br />
<br />
'''No deprojection''', aka 'standard ILC':<br />
<br />
There are many joint-optimal configurations that yield S/N values within 93% of maximum for all observables. Reasonable-looking ones include:<br />
<br />
LF=1, MF=10, UHF=7<br />
<br />
LF=1, MF=11, UHF=6<br />
<br />
LF=1, MF=12, UHF=5<br />
<br />
LF=1, MF=13, UHF=4<br />
<br />
LF=1, MF=14, UHF=3<br />
<br />
LF=2, MF=10, UHF=6<br />
<br />
LF=2, MF=11, UHF=5<br />
<br />
LF=2, MF=12, UHF=4<br />
<br />
LF=2, MF=13, UHF=3<br />
<br />
LF=2, MF=14, UHF=2<br />
<br />
<br />
If XHF tubes are considered, the joint-optimal configurations are<br />
<br />
LF=1, MF=9, UHF=5, XHF=3<br />
<br />
LF=1, MF=10, UHF=3, XHF=4<br />
<br />
LF=1, MF=10, UHF=4, XHF=3<br />
<br />
LF=1, MF=11, UHF=2, XHF=4<br />
<br />
LF=1, MF=11, UHF=3, XHF=3<br />
<br />
LF=2, MF=10, UHF=3, XHF=3<br />
<br />
which all yield S/N values within 99% of maximum for all observables.<br />
<br />
''The performance of the fiducial configuration is good for everything here, yielding S/N > 93% of maximum for kSZ, lensing, and CMB, and S/N ~ 88% of maximum for tSZ. I think this would serve as a reasonable baseline 'flowdown' justification for the fiducial choice of bands. Note that the S/N maxima are computed when allowing XHF tubes, so the upshot is that allowing XHF tubes would yield ~10% gains in S/N (for the no-deprojection case; gains are larger in other cases below).''<br />
<br />
<br />
'''Deprojection of tSZ (for CMB) or of CMB (for tSZ)''': <br />
<br />
The joint-optimal configurations are<br />
<br />
LF=1, MF=4, UHF=13<br />
<br />
LF=1, MF=5, UHF=12<br />
<br />
LF=1, MF=6, UHF=11<br />
<br />
LF=1, MF=7, UHF=10<br />
<br />
yielding S/N values within 92% of maximum for all observables.<br />
<br />
<br />
If XHF tubes are considered, there are many configurations with S/N values > 95% of maximum for all observables. Reasonable looking ones include:<br />
<br />
LF=1, MF=8, UHF=4, XHF=5<br />
<br />
LF=1, MF=8, UHF=5, XHF=4<br />
<br />
LF=1, MF=8, UHF=6, XHF=3<br />
<br />
LF=2, MF=5, UHF=6, XHF=5<br />
<br />
''The performance of the fiducial configuration is good for everything except kSZ, yielding S/N > 94% of maximum for tSZ, lensing, and CMB, but S/N ~ 84% of maximum for kSZ (still not too bad).<br />
''<br />
<br />
'''Deprojection of CIB (for both CMB and tSZ)''':<br />
<br />
The joint-optimal configuration is<br />
<br />
LF=1, MF=6, UHF=11<br />
<br />
yielding S/N values within 93% of maximum for all observables.<br />
<br />
<br />
If XHF tubes are considered, there are many configurations with S/N values > 95% of maximum for all observables. Reasonable looking ones include:<br />
<br />
LF=1, MF=10, UHF=0, XHF=7<br />
<br />
LF=1, MF=10, UHF=1, XHF=6<br />
<br />
LF=1, MF=10, UHF=2, XHF=5<br />
<br />
LF=1, MF=9, UHF=0, XHF=8<br />
<br />
LF=1, MF=9, UHF=1, XHF=7<br />
<br />
LF=1, MF=9, UHF=2, XHF=6<br />
<br />
LF=1, MF=9, UHF=3, XHF=5<br />
<br />
LF=1, MF=9, UHF=4, XHF=4<br />
<br />
''The performance of the fiducial configuration is good for everything except kSZ, yielding S/N > 96% of maximum for tSZ, lensing, and CMB, but S/N ~ 82% of maximum for kSZ (still not too bad).<br />
''</div>Jchhttp://www.cmb-s4.org/wiki/index.php?title=LAT_Frequency_Flowdown&diff=8886LAT Frequency Flowdown2019-04-22T18:22:43Z<p>Jch: </p>
<hr />
<div>=== Summary ===<br />
(Colin Hill writing 4-22-19)<br />
<br />
In this posting I present the results of "flowdown" (i.e., optimization) calculations for the frequency channel distribution of the CMB-S4 LATs.<br />
<br />
=== Setup and Assumptions ===<br />
<br />
I use the noise calculator for the CMB-S4 LATs posted at https://cmb-s4.org/wiki/images/Lat-noise-190311-py.txt<br />
<br />
This noise calculator allows one to vary the sky fraction surveyed (fsky) and the number of optics tubes of each type (LF, MF, UHF). For reference, LF = 27 and 39 GHz, MF = 93 and 145 GHz, UHF = 225 and 280 GHz. I do not consider the 20 GHz channel (ULF) in this work, as its resolution is low enough as to likely be irrelevant for LAT science. I consider fsky = 0.1, 0.2, and 0.4, and all possible optics tube configurations with 18 total tubes (assuming there is 19th tube used for the ULF). I also impose a constraint that there is at least one MF tube, since these are clearly the main 'science frequencies'. This yields a total of 3420 possible configurations. Note that I assume two identical copies of the LAT, in order to reduce the computational complexity. If desired, one could run a full optimization of all 36 optics tubes.<br />
<br />
I also run calculations using a modified version of the S4 noise calculator (via Matthew Hasselfield) that allows for the possibility of "XHF" optics tubes, where XHF = 281 and 350 GHz. The atmosphere for these tubes is assumed to match CCAT site specifications.<br />
<br />
I include Planck data (30 - 353 GHz) in all calculations, as these channels are useful on large angular scales where the S4 atmospheric noise is large.<br />
<br />
=== Methodology ===<br />
<br />
I focus on temperature-based observables in the following: thermal SZ, kinematic SZ, CMB lensing via the TT quadratic estimator, and the CMB TT power spectrum. I model the temperature sky at all frequencies from 27 to 353 GHz (13 channels, or 15 when including XHF tubes) using the simulated sky maps described in Sec. 2 of https://arxiv.org/abs/1808.07445 . These maps are also available at https://lambda.gsfc.nasa.gov/toolbox/tb_cmbsim_ov.cfm<br />
<br />
I use simple Galactic-emission-thresholded sky masks that leave the cleanest 10%, 20%, or 40% of the sky that is visible from Chile. These are identical to the sky masks used in https://arxiv.org/abs/1808.07445<br />
<br />
For each fsky and optics tube configuration option, I use a harmonic-space ILC code to obtain "post-component-separation" noise power spectra for the blackbody CMB temperature and Compton-y fields, using the modeled sky power spectra and the per-frequency noise power spectra computed using the S4 calculator (as well as Planck noise, assumed to be white). I consider the option of explicitly "deprojecting" some contaminants using a constrained ILC, which is a robust way to conservatively assess the frequency coverage that may be needed to sufficiently remove these foregrounds. I consider three deprojection options: no deprojection, deprojection of tSZ (for CMB reconstruction) or CMB (for tSZ reconstruction), and deprojection of a fiducial CIB spectrum (for CMB and tSZ reconstruction). The total number of fsky/configuration/deprojection options is thus 10260.<br />
<br />
For each fsky and optics tube configuration option (and deprojection option), I then compute the S/N on four observables: tSZ power spectrum, kSZ power spectrum (conservatively considering only ell>3000), CMB lensing power spectrum via the TT estimator (effectively also a proxy for CMB halo lensing, which is dominated by TT), and the CMB TT power spectrum. These S/N values are used as the 'optimization metric' for 'flowdown', i.e., I seek configurations that maximize these S/N values.<br />
<br />
=== Results ===<br />
<br />
General result, valid for all observables and all deprojection options: going wide (fsky=0.4) is always optimal for the S/N of all these observables. Even for the kSZ power spectrum, the S4 noise is sufficiently low (i.e., we are close enough to hitting sample variance on a range of modes) that going wide is preferred over going deep. I do not list fsky in the optimal configurations below because it is always 0.4.<br />
<br />
I also explicitly highlight below the performance of the fiducial configuration used in all previous calculations (fsky=0.4, LF=2, MF=12, UHF=4).<br />
<br />
'''No deprojection''', aka 'standard ILC':<br />
<br />
There are many joint-optimal configurations that yield S/N values within 93% of maximum for all observables. Reasonable-looking ones include:<br />
LF=1, MF=10, UHF=7<br />
LF=1, MF=11, UHF=6<br />
LF=1, MF=12, UHF=5<br />
LF=1, MF=13, UHF=4<br />
LF=1, MF=14, UHF=3<br />
LF=2, MF=10, UHF=6<br />
LF=2, MF=11, UHF=5<br />
LF=2, MF=12, UHF=4<br />
LF=2, MF=13, UHF=3<br />
LF=2, MF=14, UHF=2<br />
<br />
If XHF tubes are considered, the joint-optimal configurations are<br />
LF=1, MF=9, UHF=5, XHF=3<br />
LF=1, MF=10, UHF=3, XHF=4<br />
LF=1, MF=10, UHF=4, XHF=3<br />
LF=1, MF=11, UHF=2, XHF=4<br />
LF=1, MF=11, UHF=3, XHF=3<br />
LF=2, MF=10, UHF=3, XHF=3<br />
which all yield S/N values within 99% of maximum for all observables.<br />
<br />
''The performance of the fiducial configuration is good for everything here, yielding S/N > 93% of maximum for kSZ, lensing, and CMB, and S/N ~ 88% of maximum for tSZ. I think this would serve as a reasonable baseline 'flowdown' justification for the fiducial choice of bands. Note that the S/N maxima are computed when allowing XHF tubes, so the upshot is that allowing XHF tubes would yield ~10% gains in S/N (for the no-deprojection case; gains are larger in other cases below).''<br />
<br />
<br />
'''Deprojection of tSZ (for CMB) or of CMB (for tSZ)''': <br />
<br />
The joint-optimal configurations are<br />
LF=1, MF=4, UHF=13<br />
LF=1, MF=5, UHF=12<br />
LF=1, MF=6, UHF=11<br />
LF=1, MF=7, UHF=10<br />
yielding S/N values within 92% of maximum for all observables.<br />
<br />
If XHF tubes are considered, there are many configurations with S/N values > 95% of maximum for all observables. Reasonable looking ones include:<br />
LF=1, MF=8, UHF=4, XHF=5<br />
LF=1, MF=8, UHF=5, XHF=4<br />
LF=1, MF=8, UHF=6, XHF=3<br />
LF=2, MF=5, UHF=6, XHF=5<br />
<br />
''The performance of the fiducial configuration is good for everything except kSZ, yielding S/N > 94% of maximum for tSZ, lensing, and CMB, but S/N ~ 84% of maximum for kSZ (still not too bad).<br />
''<br />
<br />
'''Deprojection of CIB (for both CMB and tSZ)''':<br />
<br />
The joint-optimal configuration is<br />
LF=1, MF=6, UHF=11<br />
yielding S/N values within 93% of maximum for all observables.<br />
<br />
If XHF tubes are considered, there are many configurations with S/N values > 95% of maximum for all observables. Reasonable looking ones include:<br />
LF=1, MF=10, UHF=0, XHF=7<br />
LF=1, MF=10, UHF=1, XHF=6<br />
LF=1, MF=10, UHF=2, XHF=5<br />
LF=1, MF=9, UHF=0, XHF=8<br />
LF=1, MF=9, UHF=1, XHF=7<br />
LF=1, MF=9, UHF=2, XHF=6<br />
LF=1, MF=9, UHF=3, XHF=5<br />
LF=1, MF=9, UHF=4, XHF=4<br />
<br />
''The performance of the fiducial configuration is good for everything except kSZ, yielding S/N > 96% of maximum for tSZ, lensing, and CMB, but S/N ~ 82% of maximum for kSZ (still not too bad).<br />
''</div>Jchhttp://www.cmb-s4.org/wiki/index.php?title=LAT_Frequency_Flowdown&diff=8885LAT Frequency Flowdown2019-04-22T18:05:06Z<p>Jch: </p>
<hr />
<div>=== Summary ===<br />
(Colin Hill writing 4-22-19)<br />
<br />
In this posting I present the results of "flowdown" (i.e., optimization) calculations for the frequency channel distribution of the CMB-S4 LATs.<br />
<br />
=== Setup and Assumptions ===<br />
<br />
I use the noise calculator for the CMB-S4 LATs posted at https://cmb-s4.org/wiki/images/Lat-noise-190311-py.txt<br />
<br />
This noise calculator allows one to vary the sky fraction surveyed (fsky) and the number of optics tubes of each type (LF, MF, UHF). For reference, LF = 27 and 39 GHz, MF = 93 and 145 GHz, UHF = 225 and 280 GHz. I do not consider the 20 GHz channel (ULF) in this work, as its resolution is low enough as to likely be irrelevant for LAT science. I consider fsky = 0.1, 0.2, and 0.4, and all possible optics tube configurations with 18 total tubes (assuming there is 19th tube used for the ULF). I also impose a constraint that there is at least one MF tube, since these are clearly the main 'science frequencies'. This yields a total of 3420 possible configurations. Note that I assume two identical copies of the LAT, in order to reduce the computational complexity. If desired, one could run a full optimization of all 36 optics tubes.<br />
<br />
I also run calculations using a modified version of the S4 noise calculator (via Matthew Hasselfield) that allows for the possibility of "XHF" optics tubes, where XHF = 281 and 350 GHz. The atmosphere for these tubes is assumed to match CCAT site specifications.<br />
<br />
I include Planck data (30 - 353 GHz) in all calculations, as these channels are useful on large angular scales where the S4 atmospheric noise is large.<br />
<br />
=== Methodology ===<br />
<br />
I focus on temperature-based observables in the following: thermal SZ, kinematic SZ, CMB lensing via the TT quadratic estimator, and the CMB TT power spectrum. I model the temperature sky at all frequencies from 27 to 353 GHz (13 channels, or 15 when including XHF tubes) using the simulated sky maps described in Sec. 2 of https://arxiv.org/abs/1808.07445 . These maps are also available at https://lambda.gsfc.nasa.gov/toolbox/tb_cmbsim_ov.cfm<br />
<br />
I use simple Galactic-emission-thresholded sky masks that leave the cleanest 10%, 20%, or 40% of the sky that is visible from Chile. These are identical to the sky masks used in https://arxiv.org/abs/1808.07445<br />
<br />
For each fsky and optics tube configuration option, I use a harmonic-space ILC code to obtain "post-component-separation" noise power spectra for the blackbody CMB temperature and Compton-y fields, using the modeled sky power spectra and the per-frequency noise power spectra computed using the S4 calculator (as well as Planck noise, assumed to be white). I consider the option of explicitly "deprojecting" some contaminants using a constrained ILC, which is a robust way to conservatively assess the frequency coverage that may be needed to sufficiently remove these foregrounds. I consider three deprojection options: no deprojection, deprojection of tSZ (for CMB reconstruction) or CMB (for tSZ reconstruction), and deprojection of a fiducial CIB spectrum (for CMB and tSZ reconstruction). The total number of fsky/configuration/deprojection options is thus 10260.<br />
<br />
For each fsky and optics tube configuration option (and deprojection option), I then compute the S/N on four observables: tSZ power spectrum, kSZ power spectrum (conservatively considering only ell>3000), CMB lensing power spectrum via the TT estimator (effectively also a proxy for CMB halo lensing, which is dominated by TT), and the CMB TT power spectrum. These S/N values are used as the 'optimization metric' for 'flowdown', i.e., I seek configurations that maximize these S/N values.<br />
<br />
=== Results ===<br />
<br />
General result, valid for all observables and all deprojection options: going wide (fsky=0.4) is always optimal for the S/N of all these observables. Even for the kSZ power spectrum, the S4 noise is sufficiently low (i.e., we are close enough to hitting sample variance on a range of modes) that going wide is preferred over going deep. I do not list fsky in the optimal configurations below because it is always 0.4.<br />
<br />
I also explicitly highlight below the performance of the fiducial configuration used in all previous calculations (fsky=0.4, LF=2, MF=12, UHF=4).<br />
<br />
'''No deprojection''', aka 'standard ILC':<br />
<br />
The joint-optimal configuration is<br />
<br />
<br />
yielding S/N values within XX% of maximum for all observables.<br />
<br />
<br />
<br />
'''Deprojection of tSZ (for CMB) or of CMB (for tSZ)''': <br />
<br />
The joint-optimal configurations are<br />
LF=1, MF=4, UHF=13<br />
LF=1, MF=5, UHF=12<br />
LF=1, MF=6, UHF=11<br />
LF=1, MF=7, UHF=10<br />
yielding S/N values within 92% of maximum for all observables.<br />
<br />
If XHF tubes are considered, there are many configurations with S/N values > 95% of maximum for all observables. Reasonable looking ones include:<br />
LF=1, MF=8, UHF=4, XHF=5<br />
LF=1, MF=8, UHF=5, XHF=4<br />
LF=1, MF=8, UHF=6, XHF=3<br />
LF=2, MF=5, UHF=6, XHF=5<br />
<br />
The performance of the fiducial configuration is good for everything except kSZ, yielding S/N > 94% of maximum for tSZ, lensing, and CMB, but S/N ~ 84% of maximum for kSZ (still not too bad).<br />
<br />
<br />
'''Deprojection of CIB (for both CMB and tSZ)''':<br />
<br />
The joint-optimal configuration is<br />
LF=1, MF=6, UHF=11<br />
yielding S/N values within 93% of maximum for all observables.<br />
<br />
If XHF tubes are considered, there are many configurations with S/N values > 95% of maximum for all observables. Reasonable looking ones include:<br />
LF=1, MF=10, UHF=0, XHF=7<br />
LF=1, MF=10, UHF=1, XHF=6<br />
LF=1, MF=10, UHF=2, XHF=5<br />
LF=1, MF=9, UHF=0, XHF=8<br />
LF=1, MF=9, UHF=1, XHF=7<br />
LF=1, MF=9, UHF=2, XHF=6<br />
LF=1, MF=9, UHF=3, XHF=5<br />
LF=1, MF=9, UHF=4, XHF=4<br />
<br />
The performance of the fiducial configuration is good for everything except kSZ, yielding S/N > 96% of maximum for tSZ, lensing, and CMB, but S/N ~ 82% of maximum for kSZ (still not too bad).</div>Jchhttp://www.cmb-s4.org/wiki/index.php?title=LAT_Frequency_Flowdown&diff=8883LAT Frequency Flowdown2019-04-22T17:53:48Z<p>Jch: </p>
<hr />
<div>=== Summary ===<br />
(Colin Hill writing 4-22-19)<br />
<br />
In this posting I present the results of "flowdown" (i.e., optimization) calculations for the frequency channel distribution of the CMB-S4 LATs.<br />
<br />
=== Setup and Assumptions ===<br />
<br />
I use the noise calculator for the CMB-S4 LATs posted at https://cmb-s4.org/wiki/images/Lat-noise-190311-py.txt<br />
<br />
This noise calculator allows one to vary the sky fraction surveyed (fsky) and the number of optics tubes of each type (LF, MF, UHF). For reference, LF = 27 and 39 GHz, MF = 93 and 145 GHz, UHF = 225 and 280 GHz. I do not consider the 20 GHz channel (ULF) in this work, as its resolution is low enough as to likely be irrelevant for LAT science. I consider fsky = 0.1, 0.2, and 0.4, and all possible optics tube configurations with 18 total tubes (assuming there is 19th tube used for the ULF). I also impose a constraint that there is at least one MF tube, since these are clearly the main 'science frequencies'. This yields a total of 3420 possible configurations. Note that I assume two identical copies of the LAT, in order to reduce the computational complexity. If desired, one could run a full optimization of all 36 optics tubes.<br />
<br />
I also run calculations using a modified version of the S4 noise calculator (via Matthew Hasselfield) that allows for the possibility of "XHF" optics tubes, where XHF = 281 and 350 GHz. The atmosphere for these tubes is assumed to match CCAT site specifications.<br />
<br />
I include Planck data (30 - 353 GHz) in all calculations, as these channels are useful on large angular scales where the S4 atmospheric noise is large.<br />
<br />
=== Methodology ===<br />
<br />
I focus on temperature-based observables in the following: thermal SZ, kinematic SZ, CMB lensing via the TT quadratic estimator, and the CMB TT power spectrum. I model the temperature sky at all frequencies from 27 to 353 GHz (13 channels, or 15 when including XHF tubes) using the simulated sky maps described in Sec. 2 of https://arxiv.org/abs/1808.07445 . These maps are also available at https://lambda.gsfc.nasa.gov/toolbox/tb_cmbsim_ov.cfm<br />
<br />
I use simple Galactic-emission-thresholded sky masks that leave the cleanest 10%, 20%, or 40% of the sky that is visible from Chile. These are identical to the sky masks used in https://arxiv.org/abs/1808.07445<br />
<br />
For each fsky and optics tube configuration option, I use a harmonic-space ILC code to obtain "post-component-separation" noise power spectra for the blackbody CMB temperature and Compton-y fields, using the modeled sky power spectra and the per-frequency noise power spectra computed using the S4 calculator (as well as Planck noise, assumed to be white). I consider the option of explicitly "deprojecting" some contaminants using a constrained ILC, which is a robust way to conservatively assess the frequency coverage that may be needed to sufficiently remove these foregrounds. I consider three deprojection options: no deprojection, deprojection of tSZ (for CMB reconstruction) or CMB (for tSZ reconstruction), and deprojection of a fiducial CIB spectrum (for CMB and tSZ reconstruction). The total number of fsky/configuration/deprojection options is thus 10260.<br />
<br />
For each fsky and optics tube configuration option (and deprojection option), I then compute the S/N on four observables: tSZ power spectrum, kSZ power spectrum (conservatively considering only ell>3000), CMB lensing power spectrum via the TT estimator (effectively also a proxy for CMB halo lensing, which is dominated by TT), and the CMB TT power spectrum. These S/N values are used as the 'optimization metric' for 'flowdown', i.e., I seek configurations that maximize these S/N values.<br />
<br />
=== Results ===<br />
<br />
General result, valid for all observables and all deprojection options: going wide (fsky=0.4) is always optimal for the S/N of all these observables. Even for the kSZ power spectrum, the S4 noise is sufficiently low (i.e., we are close enough to hitting sample variance on a range of modes) that going wide is preferred over going deep. I do not list fsky in the optimal configurations below because it is always 0.4.<br />
<br />
I also explicitly highlight below the performance of the fiducial configuration used in all previous calculations (fsky=0.4, LF=2, MF=12, UHF=4).<br />
<br />
'''No deprojection''', aka 'standard ILC': The following configurations all <br />
<br />
<br />
Fiducial configuration yields S/N values <br />
<br />
<br />
'''Deprojection of tSZ (for CMB) or of CMB (for tSZ)''': <br />
<br />
<br />
<br />
'''Deprojection of CIB (for both CMB and tSZ)''':<br />
The joint-optimal configuration is<br />
LF=1, MF=6, UHF=11<br />
yielding S/N values within 93% of maximum for all observables.<br />
<br />
If XHF tubes are considered, there are many configurations with S/N values > 95% of maximum for all observables. Reasonable looking ones include:<br />
LF=1, MF=10, UHF=0, XHF=7<br />
LF=1, MF=10, UHF=1, XHF=6<br />
LF=1, MF=10, UHF=2, XHF=5<br />
LF=1, MF=9, UHF=0, XHF=8<br />
LF=1, MF=9, UHF=1, XHF=7<br />
LF=1, MF=9, UHF=2, XHF=6<br />
LF=1, MF=9, UHF=3, XHF=5<br />
LF=1, MF=9, UHF=4, XHF=4<br />
<br />
The performance of the fiducial configuration is good for everything except kSZ, yielding S/N > 96% of maximum for tSZ, lensing, and CMB, but S/N ~ 82% of maximum for kSZ (still not too bad).</div>Jchhttp://www.cmb-s4.org/wiki/index.php?title=LAT_Frequency_Flowdown&diff=8880LAT Frequency Flowdown2019-04-22T17:23:23Z<p>Jch: </p>
<hr />
<div>=== Summary ===<br />
(Colin Hill writing 4-22-19)<br />
<br />
In this posting I present the results of "flowdown" (i.e., optimization) calculations for the frequency channel distribution of the CMB-S4 LATs.<br />
<br />
=== Setup and Assumptions ===<br />
<br />
I use the noise calculator for the CMB-S4 LATs posted at https://cmb-s4.org/wiki/images/Lat-noise-190311-py.txt<br />
<br />
This noise calculator allows one to vary the sky fraction surveyed (fsky) and the number of optics tubes of each type (LF, MF, UHF). For reference, LF = 27 and 39 GHz, MF = 93 and 145 GHz, UHF = 225 and 280 GHz. I do not consider the 20 GHz channel (ULF) in this work, as its resolution is low enough as to likely be irrelevant for LAT science. I consider fsky = 0.1, 0.2, and 0.4, and all possible optics tube configurations with 18 total tubes (assuming there is 19th tube used for the ULF). I also impose a constraint that there is at least one MF tube, since these are clearly the main 'science frequencies'. This yields a total of 3420 possible configurations. Note that I assume two identical copies of the LAT, in order to reduce the computational complexity. If desired, one could run a full optimization of all 36 optics tubes.<br />
<br />
I also run calculations using a modified version of the S4 noise calculator (via Matthew Hasselfield) that allows for the possibility of "XHF" optics tubes, where XHF = 281 and 350 GHz. The atmosphere for these tubes is assumed to match CCAT site specifications.<br />
<br />
I include Planck data (30 - 353 GHz) in all calculations, as these channels are useful on large angular scales where the S4 atmospheric noise is large.<br />
<br />
=== Methodology ===<br />
<br />
I focus on temperature-based observables in the following: thermal SZ, kinematic SZ, CMB lensing via the TT quadratic estimator, and the CMB TT power spectrum. I model the temperature sky at all frequencies from 27 to 353 GHz (13 channels, or 15 when including XHF tubes) using the simulated sky maps described in Sec. 2 of https://arxiv.org/abs/1808.07445 . These maps are also available at https://lambda.gsfc.nasa.gov/toolbox/tb_cmbsim_ov.cfm<br />
<br />
I use simple Galactic-emission-thresholded sky masks that leave the cleanest 10%, 20%, or 40% of the sky that is visible from Chile. These are identical to the sky masks used in https://arxiv.org/abs/1808.07445<br />
<br />
For each fsky and optics tube configuration option, I use a harmonic-space ILC code to obtain "post-component-separation" noise power spectra for the blackbody CMB temperature and Compton-y fields, using the modeled sky power spectra and the per-frequency noise power spectra computed using the S4 calculator (as well as Planck noise, assumed to be white). I consider the option of explicitly "deprojecting" some contaminants using a constrained ILC, which is a robust way to conservatively assess the frequency coverage that may be needed to sufficiently remove these foregrounds. I consider three deprojection options: no deprojection, deprojection of tSZ (for CMB reconstruction) or CMB (for tSZ reconstruction), and deprojection of a fiducial CIB spectrum (for CMB and tSZ reconstruction). The total number of fsky/configuration/deprojection options is thus 10260.<br />
<br />
For each fsky and optics tube configuration option (and deprojection option), I then compute the S/N on four observables: tSZ power spectrum, kSZ power spectrum (conservatively considering only ell>3000), CMB lensing power spectrum via the TT estimator (effectively also a proxy for CMB halo lensing, which is dominated by TT), and the CMB TT power spectrum. These S/N values are used as the 'optimization metric' for 'flowdown', i.e., I seek configurations that maximize these S/N values.<br />
<br />
=== Results ===</div>Jchhttp://www.cmb-s4.org/wiki/index.php?title=LAT_Frequency_Flowdown&diff=8879LAT Frequency Flowdown2019-04-22T17:16:55Z<p>Jch: Created page with "=== Summary === (Colin Hill writing 4-22-19) In this posting I present the results of "flowdown" (i.e., optimization) calculations for the frequency channel distribution of t..."</p>
<hr />
<div>=== Summary ===<br />
(Colin Hill writing 4-22-19)<br />
<br />
In this posting I present the results of "flowdown" (i.e., optimization) calculations for the frequency channel distribution of the CMB-S4 LATs.<br />
<br />
=== Setup and Assumptions ===<br />
<br />
I use the noise calculator for the CMB-S4 LATs posted at https://cmb-s4.org/wiki/images/Lat-noise-190311-py.txt<br />
<br />
This noise calculator allows one to vary the sky fraction surveyed (fsky) and the number of optics tubes of each type (LF, MF, UHF). For reference, LF = 27 and 39 GHz, MF = 93 and 145 GHz, UHF = 225 and 280 GHz. I do not consider the 20 GHz channel (ULF) in this work, as its resolution is low enough as to likely be irrelevant for LAT science. I consider fsky = 0.1, 0.2, and 0.4, and all possible optics tube configurations with 18 total tubes (assuming there is 19th tube used for the ULF). I also impose a constraint that there is at least one MF tube, since these are clearly the main 'science frequencies'. This yields a total of 3420 possible configurations. Note that I assume two identical copies of the LAT, in order to reduce the computational complexity. If desired, one could run a full optimization of all 36 optics tubes.<br />
<br />
I also run calculations using a modified version of the S4 noise calculator (via Matthew Hasselfield) that allows for the possibility of "XHF" optics tubes, where XHF = 281 and 350 GHz. The atmosphere for these tubes is assumed to match CCAT site specifications.<br />
<br />
I include Planck data (30 - 353 GHz) in all calculations, as these channels are useful on large angular scales where the S4 atmospheric noise is large.<br />
<br />
=== Methodology ===<br />
<br />
I focus on temperature-based observables in the following: thermal SZ, kinematic SZ, CMB lensing via the TT quadratic estimator, and the CMB TT power spectrum. I model the temperature sky at all frequencies from 27 to 353 GHz (13 channels, or 15 when including XHF tubes) using the simulated sky maps described in Sec. 2 of https://arxiv.org/abs/1808.07445 . These maps are also available at https://lambda.gsfc.nasa.gov/toolbox/tb_cmbsim_ov.cfm<br />
<br />
I use simple Galactic-emission-thresholded sky masks that leave the cleanest 10%, 20%, or 40% of the sky that is visible from Chile. These are identical to the sky masks used in https://arxiv.org/abs/1808.07445<br />
<br />
For each fsky and optics tube configuration option, I use a harmonic-space ILC code to obtain "post-component-separation" noise power spectra for either the blackbody CMB temperature or Compton-y fields, using the modeled sky power spectra and the per-frequency noise power spectra computed using the S4 calculator (as well as Planck noise, assumed to be white).</div>Jchhttp://www.cmb-s4.org/wiki/index.php?title=Speakers_bureau_talks_list&diff=8178Speakers bureau talks list2019-01-13T22:07:30Z<p>Jch: /* 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 />
| Masashi Hazumi <br />
| Plenary talk on CMB cosmology<br />
| <br />
| [[Media:myslides.pdf]]<br />
--> <br />
<br />
|- <br />
| 12 Jan 2019<br />
| 13-16 April 2019<br />
| APS April Meeting, Devner<br />
| Nils Halverson <br />
| 12 minutes on CMB-S4<br />
| <br />
| [[Media:myslides.pdf]]<br />
<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 Hill<br />
| Constraining Feedback in Galaxy Formation with Next-Generation CMB Experiments<br />
| The cosmic microwave background (CMB) radiation is a powerful backlight with which to illuminate structure throughout cosmic history. The thermal (tSZ) and kinematic Sunyaev-Zel'dovich (kSZ) effects, sourced by the scattering of CMB photons off free electrons, directly probe the thermal pressure and density of ionized gas, while gravitational lensing of the CMB directly measures the line-of-sight matter density. Measurements of these effects, which have only been robustly detected within the past decade, will transform our understanding of galaxy formation and evolution in upcoming CMB surveys. I will present predictions for the tSZ and kSZ signals of galaxy and cluster populations at various redshifts derived from state-of-the-art cosmological hydrodynamics simulations, with differing implementations of sub-grid feedback physics due to active galactic nuclei and supernovae. While multiple feedback implementations are able to reproduce the stellar properties of galaxies, their predictions for the tSZ and kSZ signals can be distinguished at high significance by upcoming experiments, including CMB-S4. Next-generation CMB surveys will thus provide crucial input to our understanding of galaxy formation, particularly at high redshift, where other probes have limited signal-to-noise. I will conclude by discussing implications of these measurements for the modeling of baryonic effects on the matter power spectrum, which is amongst the largest systematic uncertainties in cosmological constraints derived from weak gravitational lensing data.<br />
| [[https://cmb-s4.org/wiki/images/JCH_AAS_S4.pdf]]<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 />
| 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:]]<br />
<br />
<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:]]<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:]]<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:]]<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:]]<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>Jchhttp://www.cmb-s4.org/wiki/index.php?title=File:JCH_AAS_S4.pdf&diff=8177File:JCH AAS S4.pdf2019-01-13T22:03:55Z<p>Jch: </p>
<hr />
<div></div>Jchhttp://www.cmb-s4.org/wiki/index.php?title=Speakers_bureau_talks_list&diff=8176Speakers bureau talks list2019-01-13T22:03:13Z<p>Jch: /* 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 />
| Masashi Hazumi <br />
| Plenary talk on CMB cosmology<br />
| <br />
| [[Media:myslides.pdf]]<br />
--> <br />
<br />
|- <br />
| 12 Jan 2019<br />
| 13-16 April 2019<br />
| APS April Meeting, Devner<br />
| Nils Halverson <br />
| 12 minutes on CMB-S4<br />
| <br />
| [[Media:myslides.pdf]]<br />
<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 Hill<br />
| Constraining Feedback in Galaxy Formation with Next-Generation CMB Experiments<br />
| The cosmic microwave background (CMB) radiation is a powerful backlight with which to illuminate structure throughout cosmic history. The thermal (tSZ) and kinematic Sunyaev-Zel'dovich (kSZ) effects, sourced by the scattering of CMB photons off free electrons, directly probe the thermal pressure and density of ionized gas, while gravitational lensing of the CMB directly measures the line-of-sight matter density. Measurements of these effects, which have only been robustly detected within the past decade, will transform our understanding of galaxy formation and evolution in upcoming CMB surveys. I will present predictions for the tSZ and kSZ signals of galaxy and cluster populations at various redshifts derived from state-of-the-art cosmological hydrodynamics simulations, with differing implementations of sub-grid feedback physics due to active galactic nuclei and supernovae. While multiple feedback implementations are able to reproduce the stellar properties of galaxies, their predictions for the tSZ and kSZ signals can be distinguished at high significance by upcoming experiments, including CMB-S4. Next-generation CMB surveys will thus provide crucial input to our understanding of galaxy formation, particularly at high redshift, where other probes have limited signal-to-noise. I will conclude by discussing implications of these measurements for the modeling of baryonic effects on the matter power spectrum, which is amongst the largest systematic uncertainties in cosmological constraints derived from weak gravitational lensing data.<br />
| [[Media:JCH_AAS_S4.pdf]]<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 />
| 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:]]<br />
<br />
<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:]]<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:]]<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:]]<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:]]<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>Jchhttp://www.cmb-s4.org/wiki/index.php?title=Survey_Performance_Expectations&diff=8000Survey Performance Expectations2018-10-25T18:23:28Z<p>Jch: /* Large-area Survey Performance Expectation 01 */</p>
<hr />
<div>This page summarizes the various survey performance expectations (previously called "experiment definitions.")<br />
The data products referred to are located on the NERSC system under '''/project/projectdirs/cmbs4/expt_xx'''<br />
<br />
===Large-area Survey Performance Expectation 01===<br />
The NTT should fill in here what they can, with input from large-area forecasters where needed. <br />
Ideally there would be separate specifications of instrument capabilities, and assumed sky coverage, rather than<br />
having these lumped together.<br />
<br />
The numbers below are based on the Noise Tiger Team code lat-noise-181002.py (but 181016 yields the same numbers), run assuming the default settings and fsky=0.4. The default settings include 2 LATs, each equipped with 1 ULF tube, 2 LF tubes, 12 MF tubes, and 4 UHF tubes. Note that the EE and BB noise levels are sqrt(2) higher than the TT noise levels and are omitted from the table below for brevity. The atmospheric treatment and other details are described in the code and in the lat-noise-*.pdf document linked below.<br />
<br />
{| class="wikitable" style="text-align: right; margin-left: 51px;"<br />
! Frequency (GHz) !! 20 !! 27 !! 39 !! 93 !! 145 !! 225 !! 280<br />
|-<br />
| Bandwidth (GHz) || n/a || n/a || n/a || n/a || n/a || n/a || n/a<br />
|-<br />
| Beam FWHM (arcmin) || 10. || 7.4 || 5.1 || 2.2 || 1.4 || 1.0 || 0.9<br />
|-<br />
| white noise level TT (uK-arcmin) || 45.9 || 15.5 || 8.7 || 1.5 || 1.5 || 4.8|| 11.5<br />
|-<br />
|}<br />
<br />
Full noise model:<br />
* 181016 (latest): [[File:lat-noise-181016-py.txt]], [[File:lat-noise-181016.pdf]]<br />
* 181002: [[File:lat-noise-181002-py.txt]], [[File:lat-noise-181002.pdf]]<br />
<br />
Post-component-separation (harmonic-space ILC) noise curves from Colin H.:<br />
http://sns.ias.edu/~jch/S4_2LAT_Tpol_default_noisecurves.tgz<br />
<br />
The file name conventions are very similar to those from the Simons Observatory noise files located at https://simonsobservatory.org/assets/supplements/20180822_SO_Noise_Public.tgz . In the S4 case, there is only one sensitivity option (labeled "SENS0", but this doesn't mean anything, it's just the default S4 setup). There is also only one fsky option (16000 deg^2, i.e., 40%). <br />
<br />
I include results for both temperature and polarization observables. Each temperature file contains three columns:<br />
[ell] [N(ell)^TT in uK^2] [N(ell)^yy]<br />
<br />
Each polarization file also contains three columns:<br />
[ell] [N(ell)^EE in uK^2] [N(ell)^BB in uK^2]<br />
<br />
The "deproj" conventions are identical to what is described in the SO science paper (deproj0 = standard ILC, etc) -- see Sec. 2 of https://arxiv.org/abs/1808.07445 . Contact jch 'at' ias.edu if anything is unclear, and/or please refer to Sec. 2 of the SO paper.<br />
<br />
IMPORTANT: these noise curves should not necessarily be used naively down to the lowest multipoles. They do not include the effects of ground pickup or other systematics that generate significant additional large-scale noise. A reasonable lower limit (which matches the SO forecasting) is to use ell_min = 30. Planck data can be used on larger scales. See Sec. 2.6 of the SO paper for details on how this was done in that work.<br />
<br />
I also include pure inverse-covariance-weighted noise curves for both TT and EE/BB (i.e., with zero foregrounds).<br />
<br />
I also include the CMB lensing reconstruction noise for the TT and EB estimators (for each of the deproj options), but people should probably re-compute this using their codes (I just used the standard QE, which is of course sub-optimal here, and I also only went down to L ~ 40).<br />
<br />
===Small-area Survey Performance Expectation 05===<br />
What we have here in "Small-area Survey Performance Expectation 05" does not fit the intended mold. But it seems practical. Here we are not specifying the map noise performance of a single instrument and survey. Instead, we are specifying some assumptions for a trade study among different instrument configurations.<br />
<br />
The SAT group is currently using the Fisher forecasting machinery used for the Science Book and validated with map-based exercises in the CDT process, to make r forecasts for a great number of configurations, for both Chile and Pole. The plan is to adjust the number of optics tubes for each configuration, and distribution over sites, to hit the target sigma(r). Then the configurations can be compared for cost and risk at fixed sigma(r). <br />
<br />
NTT prescription for these forecasts:<br />
does not exist yet.<br />
<br />
De-lensing procedure for these forecasts:<br />
Adopt A_L = 0.13 for the Pole survey, and A_L = 0.27 for the Chile survey, based on this [post|https://cmb-s4.org/wiki/index.php/Survey_Performance_Expectations].<br />
<br />
=== Experiment Definition 04 ===<br />
This is very similar to 02 but with the noise levels tweaked down by sqrt(7/6) to try and get sigma(r)=1e-4 as per science requirement.<br />
(The noise map generator has also been tweaked such that the level quoted in the params.dat table will be reproduced exactly when the power spectra of the maps is taken with the provided mask - i.e. the actual noise level will slightly lower in the center of the mask.)<br />
A 20GHz band has been added which is assumed to be on a large aperture telescope (and hence has higher resolution and ell knee).<br />
Below is the contents of the params.dat file. The noise levels and resolutions are copied from the [https://www.nsf.gov/mps/ast/aaac/cmb_s4/report/CMBS4_final_report_NL.pdf CDT report] "Science Traceability Matrix".<br />
Specs for the high res bands exist but have not been added yet. <br />
<br />
Set 04 is the same idealized circular 3% sky patch as set 02.<br />
We also add 04b which is a for a nominal Chile realistic mask<br />
and 04c which is a realistic Pole mask (actually the BICEP3 2017 as observed mask). See [[Sims_with_nominal_Chile_and_Pole_masks | this logbook posting]] for details.<br />
<br />
{| class="wikitable" style="text-align: right; margin-left: 51px;"<br />
! Frequency (GHz) !! 20 !! 30 !! 40 !! 85 !! 95 !! 145 !! 155 !! 220 !! 270<br />
|-<br />
| Bandwidth (GHz) || 5.0 || 9.0 || 12.0 || 20.4 || 22.8 || 31.9 || 34.1 || 48.4 || 59.4<br />
|-<br />
| Beam FWHM (arcmin) || 11.0 || 76.6 || 57.5 || 27.0 || 24.2 || 15.9 || 14.8 || 10.7 || 8.5<br />
|-<br />
| white noise level TT (uK-arcmin) || 16.66 || 10.62 || 10.07 || 2.01 || 1.59 || 4.53 || 4.53 || 11.61 || 15.84<br />
|-<br />
| ell knee TT || 500 || 175 || 175 || 175 || 175 || 230 || 230 || 230 || 230<br />
|-<br />
| 1/f exponent TT || -4.1 || -4.1 || -4.1 || -4.1 || -4.1 || -3.8 || -3.8 || -3.8 || -3.8<br />
|-<br />
| white noise level EE (uK-arcmin) || 13.94 || 8.88 || 8.42 || 1.67 || 1.32 || 2.12 || 2.12 || 5.43 || 7.42 <br />
|-<br />
| ell knee EE || 200 || 50 || 50 || 50 || 50 || 65 || 65 || 65 || 65<br />
|-<br />
| 1/f exponent EE || -2.0 || -2.0 || -2.0 || -2.0 || -2.0 || -3.0 || -3.0 || -3.0 || -3.0<br />
|-<br />
| white noise level BB (uK-arcmin) || 13.6 || 8.67 || 8.22 || 1.64 || 1.30 || 2.03 || 2.03 || 5.19 || 7.08<br />
|-<br />
| ell knee BB || 200 || 50 || 50 || 50 || 50 || 60 || 60 || 60 || 60<br />
|-<br />
| 1/f exponent BB || -2.0 || -2.0 || -2.0 || -2.0 || -2.0 || -3.0 || -3.0 || -3.0 || -3.0<br />
|-<br />
| ell min || 30 || 30 || 30 || 30 || 30 || 30 || 30 || 30 || 30 <br />
|-<br />
| nside || 512 || 512 || 512 || 512 || 512 || 512 || 512 || 512 || 512<br />
|}<br />
<br />
=== Experiment Definition 03, 03b, 03c ===<br />
These sims are nearly identical to experiment definition 02, 02b, 02c, and even use the same noise realizations. The one change is the inclusion of additive systematics, following the prescription described in this [[Additive_systematics_for_data_challenge_03|2017-07-10 posting]]. Blocks of realizations contain different versions of the additive systematic, as shown below. For all cases, the level of the systematic is chosen to yield bias on ''r'' of 1e-4 (by the analysis of the 2017-07-10 posting). The first block of realizations, 0000&ndash;0124, contains no systematic and should be completely identical to the 02/02b/02c realizations.<br />
<br />
{| class="wikitable"<br />
|-<br />
! realizations !! A<sub>uncorr</sub> !! B<sub>uncorr</sub> !! A<sub>corr</sub> !! B<sub>corr</sub> !! Description<br />
|-<br />
| 0000&ndash;0124 || 0 || 0 || 0 || 0 || No systematics<br />
|-<br />
| 0125&ndash;0249 || 0.0328 || 0 || 0 || 0 || Uncorrelated systematic with white spectrum<br />
|-<br />
| 0250&ndash;0374 || 0 || 0.0689 || 0 || 0 || Uncorrelated systematic with 1/ell spectrum<br />
|-<br />
| 0375&ndash;0499 || 0 || 0 || 0.0584 || 0 || Correlated systematic with white spectrum<br />
|-<br />
| 0500&ndash;0624 || 0 || 0 || 0 || 0.1049 || Correlated systematic with 1/ell spectrum<br />
|-<br />
| 0625&ndash;0749 || 0.0164 || 0.0345 || 0 || 0 || Uncorrelated systematic with white + 1/ell spectrum<br />
|-<br />
| 0750&ndash;0874 || 0 || 0 || 0.0292 || 0.0525 || Correlated systematic with white + 1/ell spectrum<br />
|-<br />
| 0875&ndash;0999 || 0.0082 || 0.0172 || 0.0146 || 0.0262 || Uncorrelated + correlated systematic with white + 1/ell spectrum<br />
|}<br />
<br />
Combined maps for analysis can be found on NERSC in '''/project/projectdirs/cmbs4/data_xx.yy/03''' etc.<br />
<br />
Parameters and ingredients for the combined maps can be found in '''/project/projectdirs/cmbs4/expt_xx/03''' etc. Note that noise, rhits, and wfunc are actually symlinks to those directories under experiment configs 02, 02b, 02c.<br />
<br />
=== Experiment Definition 02, 02b, 02c ===<br />
This is an update from 01 which differs in the following ways:<br />
<br />
1) Addition of 20GHz band and (slight) changes to the band/detector optimization as per<br />
[[http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170515_chkS4 Victor's May 15 posting in the logbook]].<br />
<br />
2) Addition of 3 delensing bands 95/155/220GHz with same number of detectors as the low res equivalent bands<br />
but beam size 4x higher. This adds up to approximately the same number of detectors but clearly one should reoptimize<br />
once they are not all at the same freq. Since we are still quite far from having real lensing reconstruction and realistic<br />
(non-Gaussian) high ell foregrounds this probably is OK for this round.<br />
<br />
3) Addition of tensors - even number realizations have r=0.003, odd number have r=0.<br />
<br />
4) Set 02 is the same nominal 3% sky patch as set 01. We now add 02b which is 1% round patch with center<br />
the same as the BICEP/Keck patch (RA=0, Dec=-57.5), and 02c which is 10% round patch centered on RA=15deg, Dec=-35.<br />
<br />
These products appear on NERSC under '''/project/projectdirs/cmbs4/expt_xx/02''' etc.<br />
<br />
=== Experiment Definition 01 ===<br />
This is intended to be basically the same as the assumptions made for the Fisher calculations done for the Science Book.<br />
The parameters come from [[http://users.physics.harvard.edu/~buza/20161220_chkS4 Victor's Dec 21 posting in the logbook]] with the addition of bandwidths from<br />
[[Tophat_bands_for_Data_Challenge|Colin's Nov 4 posting]] and are summarized in the following table:<br />
<br />
{| class="wikitable" style="text-align: right; margin-left: 51px;"<br />
! Frequency (GHz) !! 30 !! 40 !! 85 !! 95 !! 145 !! 155 !! 220 !! 270 !! 155 HR<br />
|-<br />
| Bandwidth (GHz) || 9.0 || 12.0 || 20.4 || 22.8 || 31.9 || 34.1 || 48.4 || 59.4 || 34.1<br />
|-<br />
| Beam FWHM (arcmin) || 76.6 || 57.5 || 27.0 || 24.2 || 15.9 || 14.8 || 10.7 || 8.5 || 4.0<br />
|-<br />
| white noise level TT (uK-arcmin) || 12.97 || 13.22 || 2.30 || 1.89 || 5.31 || 5.48 || 11.86 || 17.72 || 5.48<br />
|-<br />
| ell knee TT || 175 || 175 || 175 || 175 || 230 || 230 || 230 || 230 || 500<br />
|-<br />
| 1/f exponent TT || -4.1 || -4.1 || -4.1 || -4.1 || -3.8 || -3.8 || -3.8 || -3.8 || -3.8<br />
|-<br />
| white noise level EE (uK-arcmin) || 10.85 || 11.06 || 1.93 || 1.58 || 2.49 || 2.56 || 5.55 || 8.30 || 2.56 <br />
|-<br />
| ell knee EE || 50 || 50 || 50 || 50 || 65 || 65 || 65 || 65 || 200<br />
|-<br />
| 1/f exponent EE || -2.0 || -2.0 || -2.0 || -2.0 || -3.0 || -3.0 || -3.0 || -3.0 || -3.0<br />
|-<br />
| white noise level BB (uK-arcmin) || 10.59 || 10.79 || 1.88 || 1.54 || 2.38 || 2.45 || 5.30 || 7.93 || 2.45<br />
|-<br />
| ell knee BB || 50 || 50 || 50 || 50 || 60 || 60 || 60 || 60 || 200<br />
|-<br />
| 1/f exponent BB || -2.0 || -2.0 || -2.0 || -2.0 || -3.0 || -3.0 || -3.0 || -3.0 || -3.0<br />
|-<br />
| ell min || 30 || 30 || 30 || 30 || 30 || 30 || 30 || 30 || 100<br />
|-<br />
| nside || 512 || 512 || 512 || 512 || 512 || 512 || 512 || 512 || 2048<br />
|}<br />
<br />
These parameters are in the file '''expt_xx/01/params.dat''' and give rise to the window functions in '''expt_xx/01/wfunc''' and the noise spectra in '''expt_xx/01/noise/cls'''.<br />
The intent of the low ell cutoff is to approximate the effect of the timestream filtering which is commonly done in ground based experiments (and as some kind of acknowledgement that<br />
the largest angular scales may anyway be corrupted by systematic effects).<br />
<br />
Additionally '''expt_xx/01/rhits/fsky03bk_n0512.fits''' is supposed to represent the "relative hits" with which the sky has been observed.<br />
This is a circular pattern centred at RA=0, Dec=-45 (a bit below the BICEP/Keck patch) which is flat at one out to r=12deg and then rolls down to zero as cosine squared over an<br />
additional 15 deg.<br />
This is some kind of approximation as to what small apertures might deliver (given their large instantaneous field of view).<br />
<br />
From the noise spectra sets of alms are generated (with nlmax=4096) with names like '''expt_xx/01/noise/alm/noise_f155_b15_ellmin30_alm_mc_0000.fits''' where 155 is the frequency, 15 is the beam size (in arcmin), and 0000 is the realization number. <br />
<br />
From these full sky maps are rendered at nside=512 and nlmax=1024. No beam smoothing is applied as is appropriate for noise.<br />
The maps have names like '''expt_xx/01/noise/map/noise_f155_b15_ellmin30_map_0512_mc_0000.fits'''.<br />
<br />
The full sky noise is then divided by the square-root of the rhits mask and the result stored in files like '''data_xx.yy/01.YY/cmbs4_01_noise_f155_b15_ellmin30_map_0512_mc_0000.fits''' - these are the noise realizations that one would have access to in a real experiment - the noise blows up around the edge.<br />
<br />
These masked noise realizations are then added to the sky model (LCDM+dust+sync+) and stored in names like '''data_xx.yy/01.YY/cmbs4_01pYY_comb_f155_b15_ellmin30_map_0512_mc_0000.fits'''.<br />
As a crude simulation of delensing these combined maps are also provided with the lensing effect reduced to 30, 10 and 3% of reality by combining lensed and unlensed LCDM - look for files<br />
with names like '''data_xx.yy/01.YY/cmbs4_01pYY_comb_AL0p3_f155_b15_ellmin30_map_0512_mc_0000.fits'''.<br />
Maps with partial lensing are constructed by the following combination: partially_lensed_map = sqrt(A_L) * lensed_map + (1 - sqrt(A_L)) * unlensed_map.<br />
<br />
To analyze these maps one should use only the '''expt_xx/01/params.dat''' file and the maps under '''data_xx.yy/01.YY'''.<br />
A thousand realizations are present.<br />
We can see these maps [[01.00 sim input maps | in this posting]]<br />
<br />
The last column of the table above shows one additional tweak - a second 155GHz band with a higher 1/f knee and smaller beam size - this is supposed to<br />
represent the maps made by higher resolution telescopes running in concert with small apertures in a hybrid approach.<br />
These maps can in principle be used to reconstruct the lensing potential and delens explicitly - instead of cheating by using<br />
the AL0p3 files etc.<br />
At the moment the noise spectrum in these maps is provisional.<br />
Additionally we may wish to add additional frequency bands at higher resolution so foreground cleaning<br />
before delensing can be done.<br />
We can see these maps [[Adding higher res delensing "band" | in this posting]].<br />
<br />
(The filtered LLCDM realizations are also copied in '''data_xx.yy/01.YY''' as these are needed to build the bandpower covariance matrix in the multi-component cross spectrum approach used by the BK group.<br />
It seems reasonable that one would always have realizations of a known spectrum signal passed through an experimental simulation.)</div>Jchhttp://www.cmb-s4.org/wiki/index.php?title=Survey_Performance_Expectations&diff=7999Survey Performance Expectations2018-10-25T16:07:19Z<p>Jch: /* Large-area Survey Performance Expectation 01 */</p>
<hr />
<div>This page summarizes the various survey performance expectations (previously called "experiment definitions.")<br />
The data products referred to are located on the NERSC system under '''/project/projectdirs/cmbs4/expt_xx'''<br />
<br />
===Large-area Survey Performance Expectation 01===<br />
The NTT should fill in here what they can, with input from large-area forecasters where needed. <br />
Ideally there would be separate specifications of instrument capabilities, and assumed sky coverage, rather than<br />
having these lumped together.<br />
<br />
The numbers below are based on the Noise Tiger Team code lat-noise-181002.py (but 181016 yields the same numbers), run assuming the default settings and fsky=0.4. The default settings include 2 LATs, each equipped with 1 ULF tube, 2 LF tubes, 12 MF tubes, and 4 UHF tubes. Note that the EE and BB noise levels are sqrt(2) higher than the TT noise levels and are omitted from the table below for brevity. The atmospheric treatment and other details are described in the code and in the lat-noise-*.pdf document linked below.<br />
<br />
{| class="wikitable" style="text-align: right; margin-left: 51px;"<br />
! Frequency (GHz) !! 20 !! 27 !! 39 !! 93 !! 145 !! 225 !! 280<br />
|-<br />
| Bandwidth (GHz) || n/a || n/a || n/a || n/a || n/a || n/a || n/a<br />
|-<br />
| Beam FWHM (arcmin) || 10. || 7.4 || 5.1 || 2.2 || 1.4 || 1.0 || 0.9<br />
|-<br />
| white noise level TT (uK-arcmin) || 45.9 || 15.5 || 8.7 || 1.5 || 1.5 || 4.8|| 11.5<br />
|-<br />
|}<br />
<br />
Full noise model:<br />
* 181016 (latest): [[File:lat-noise-181016-py.txt]], [[File:lat-noise-181016.pdf]]<br />
* 181002: [[File:lat-noise-181002-py.txt]], [[File:lat-noise-181002.pdf]]<br />
<br />
Post-component-separation (harmonic-space ILC) noise curves from Colin H.:<br />
http://sns.ias.edu/~jch/S4_2LAT_Tpol_default_noisecurves.tgz<br />
<br />
The file name conventions are very similar to those from the Simons Observatory noise files located at https://simonsobservatory.org/assets/supplements/20180822_SO_Noise_Public.tgz . In the S4 case, there is only one sensitivity option (labeled "SENS0", but this doesn't mean anything, it's just the default S4 setup). There is also only one fsky option (16000 deg^2, i.e., 40%). <br />
<br />
I include results for both temperature and polarization observables. Each temperature file contains three columns:<br />
[ell] [N(ell)^TT in uK^2] [N(ell)^yy]<br />
<br />
Each polarization file also contains three columns:<br />
[ell] [N(ell)^EE in uK^2] [N(ell)^BB in uK^2]<br />
<br />
The "deproj" conventions are identical to what is described in the SO science paper (deproj0 = standard ILC, etc) -- see Sec. 2 of https://arxiv.org/abs/1808.07445 . Contact jch 'at' ias.edu if anything is unclear, and/or please refer to Sec. 2 of the SO paper.<br />
<br />
I also include pure inverse-covariance-weighted noise curves for both TT and EE/BB (i.e., with zero foregrounds).<br />
<br />
I also include the CMB lensing reconstruction noise for the TT and EB estimators (for each of the deproj options), but people should probably re-compute this using their codes (I just used the standard QE, which is of course sub-optimal here, and I also only went down to L ~ 40).<br />
<br />
===Small-area Survey Performance Expectation 05===<br />
What we have here in "Small-area Survey Performance Expectation 05" does not fit the intended mold. But it seems practical. Here we are not specifying the map noise performance of a single instrument and survey. Instead, we are specifying some assumptions for a trade study among different instrument configurations.<br />
<br />
The SAT group is currently using the Fisher forecasting machinery used for the Science Book and validated with map-based exercises in the CDT process, to make r forecasts for a great number of configurations, for both Chile and Pole. The plan is to adjust the number of optics tubes for each configuration, and distribution over sites, to hit the target sigma(r). Then the configurations can be compared for cost and risk at fixed sigma(r). <br />
<br />
NTT prescription for these forecasts:<br />
does not exist yet.<br />
<br />
De-lensing procedure for these forecasts:<br />
Adopt A_L = 0.13 for the Pole survey, and A_L = 0.27 for the Chile survey, based on this [post|https://cmb-s4.org/wiki/index.php/Survey_Performance_Expectations].<br />
<br />
=== Experiment Definition 04 ===<br />
This is very similar to 02 but with the noise levels tweaked down by sqrt(7/6) to try and get sigma(r)=1e-4 as per science requirement.<br />
(The noise map generator has also been tweaked such that the level quoted in the params.dat table will be reproduced exactly when the power spectra of the maps is taken with the provided mask - i.e. the actual noise level will slightly lower in the center of the mask.)<br />
A 20GHz band has been added which is assumed to be on a large aperture telescope (and hence has higher resolution and ell knee).<br />
Below is the contents of the params.dat file. The noise levels and resolutions are copied from the [https://www.nsf.gov/mps/ast/aaac/cmb_s4/report/CMBS4_final_report_NL.pdf CDT report] "Science Traceability Matrix".<br />
Specs for the high res bands exist but have not been added yet. <br />
<br />
Set 04 is the same idealized circular 3% sky patch as set 02.<br />
We also add 04b which is a for a nominal Chile realistic mask<br />
and 04c which is a realistic Pole mask (actually the BICEP3 2017 as observed mask). See [[Sims_with_nominal_Chile_and_Pole_masks | this logbook posting]] for details.<br />
<br />
{| class="wikitable" style="text-align: right; margin-left: 51px;"<br />
! Frequency (GHz) !! 20 !! 30 !! 40 !! 85 !! 95 !! 145 !! 155 !! 220 !! 270<br />
|-<br />
| Bandwidth (GHz) || 5.0 || 9.0 || 12.0 || 20.4 || 22.8 || 31.9 || 34.1 || 48.4 || 59.4<br />
|-<br />
| Beam FWHM (arcmin) || 11.0 || 76.6 || 57.5 || 27.0 || 24.2 || 15.9 || 14.8 || 10.7 || 8.5<br />
|-<br />
| white noise level TT (uK-arcmin) || 16.66 || 10.62 || 10.07 || 2.01 || 1.59 || 4.53 || 4.53 || 11.61 || 15.84<br />
|-<br />
| ell knee TT || 500 || 175 || 175 || 175 || 175 || 230 || 230 || 230 || 230<br />
|-<br />
| 1/f exponent TT || -4.1 || -4.1 || -4.1 || -4.1 || -4.1 || -3.8 || -3.8 || -3.8 || -3.8<br />
|-<br />
| white noise level EE (uK-arcmin) || 13.94 || 8.88 || 8.42 || 1.67 || 1.32 || 2.12 || 2.12 || 5.43 || 7.42 <br />
|-<br />
| ell knee EE || 200 || 50 || 50 || 50 || 50 || 65 || 65 || 65 || 65<br />
|-<br />
| 1/f exponent EE || -2.0 || -2.0 || -2.0 || -2.0 || -2.0 || -3.0 || -3.0 || -3.0 || -3.0<br />
|-<br />
| white noise level BB (uK-arcmin) || 13.6 || 8.67 || 8.22 || 1.64 || 1.30 || 2.03 || 2.03 || 5.19 || 7.08<br />
|-<br />
| ell knee BB || 200 || 50 || 50 || 50 || 50 || 60 || 60 || 60 || 60<br />
|-<br />
| 1/f exponent BB || -2.0 || -2.0 || -2.0 || -2.0 || -2.0 || -3.0 || -3.0 || -3.0 || -3.0<br />
|-<br />
| ell min || 30 || 30 || 30 || 30 || 30 || 30 || 30 || 30 || 30 <br />
|-<br />
| nside || 512 || 512 || 512 || 512 || 512 || 512 || 512 || 512 || 512<br />
|}<br />
<br />
=== Experiment Definition 03, 03b, 03c ===<br />
These sims are nearly identical to experiment definition 02, 02b, 02c, and even use the same noise realizations. The one change is the inclusion of additive systematics, following the prescription described in this [[Additive_systematics_for_data_challenge_03|2017-07-10 posting]]. Blocks of realizations contain different versions of the additive systematic, as shown below. For all cases, the level of the systematic is chosen to yield bias on ''r'' of 1e-4 (by the analysis of the 2017-07-10 posting). The first block of realizations, 0000&ndash;0124, contains no systematic and should be completely identical to the 02/02b/02c realizations.<br />
<br />
{| class="wikitable"<br />
|-<br />
! realizations !! A<sub>uncorr</sub> !! B<sub>uncorr</sub> !! A<sub>corr</sub> !! B<sub>corr</sub> !! Description<br />
|-<br />
| 0000&ndash;0124 || 0 || 0 || 0 || 0 || No systematics<br />
|-<br />
| 0125&ndash;0249 || 0.0328 || 0 || 0 || 0 || Uncorrelated systematic with white spectrum<br />
|-<br />
| 0250&ndash;0374 || 0 || 0.0689 || 0 || 0 || Uncorrelated systematic with 1/ell spectrum<br />
|-<br />
| 0375&ndash;0499 || 0 || 0 || 0.0584 || 0 || Correlated systematic with white spectrum<br />
|-<br />
| 0500&ndash;0624 || 0 || 0 || 0 || 0.1049 || Correlated systematic with 1/ell spectrum<br />
|-<br />
| 0625&ndash;0749 || 0.0164 || 0.0345 || 0 || 0 || Uncorrelated systematic with white + 1/ell spectrum<br />
|-<br />
| 0750&ndash;0874 || 0 || 0 || 0.0292 || 0.0525 || Correlated systematic with white + 1/ell spectrum<br />
|-<br />
| 0875&ndash;0999 || 0.0082 || 0.0172 || 0.0146 || 0.0262 || Uncorrelated + correlated systematic with white + 1/ell spectrum<br />
|}<br />
<br />
Combined maps for analysis can be found on NERSC in '''/project/projectdirs/cmbs4/data_xx.yy/03''' etc.<br />
<br />
Parameters and ingredients for the combined maps can be found in '''/project/projectdirs/cmbs4/expt_xx/03''' etc. Note that noise, rhits, and wfunc are actually symlinks to those directories under experiment configs 02, 02b, 02c.<br />
<br />
=== Experiment Definition 02, 02b, 02c ===<br />
This is an update from 01 which differs in the following ways:<br />
<br />
1) Addition of 20GHz band and (slight) changes to the band/detector optimization as per<br />
[[http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170515_chkS4 Victor's May 15 posting in the logbook]].<br />
<br />
2) Addition of 3 delensing bands 95/155/220GHz with same number of detectors as the low res equivalent bands<br />
but beam size 4x higher. This adds up to approximately the same number of detectors but clearly one should reoptimize<br />
once they are not all at the same freq. Since we are still quite far from having real lensing reconstruction and realistic<br />
(non-Gaussian) high ell foregrounds this probably is OK for this round.<br />
<br />
3) Addition of tensors - even number realizations have r=0.003, odd number have r=0.<br />
<br />
4) Set 02 is the same nominal 3% sky patch as set 01. We now add 02b which is 1% round patch with center<br />
the same as the BICEP/Keck patch (RA=0, Dec=-57.5), and 02c which is 10% round patch centered on RA=15deg, Dec=-35.<br />
<br />
These products appear on NERSC under '''/project/projectdirs/cmbs4/expt_xx/02''' etc.<br />
<br />
=== Experiment Definition 01 ===<br />
This is intended to be basically the same as the assumptions made for the Fisher calculations done for the Science Book.<br />
The parameters come from [[http://users.physics.harvard.edu/~buza/20161220_chkS4 Victor's Dec 21 posting in the logbook]] with the addition of bandwidths from<br />
[[Tophat_bands_for_Data_Challenge|Colin's Nov 4 posting]] and are summarized in the following table:<br />
<br />
{| class="wikitable" style="text-align: right; margin-left: 51px;"<br />
! Frequency (GHz) !! 30 !! 40 !! 85 !! 95 !! 145 !! 155 !! 220 !! 270 !! 155 HR<br />
|-<br />
| Bandwidth (GHz) || 9.0 || 12.0 || 20.4 || 22.8 || 31.9 || 34.1 || 48.4 || 59.4 || 34.1<br />
|-<br />
| Beam FWHM (arcmin) || 76.6 || 57.5 || 27.0 || 24.2 || 15.9 || 14.8 || 10.7 || 8.5 || 4.0<br />
|-<br />
| white noise level TT (uK-arcmin) || 12.97 || 13.22 || 2.30 || 1.89 || 5.31 || 5.48 || 11.86 || 17.72 || 5.48<br />
|-<br />
| ell knee TT || 175 || 175 || 175 || 175 || 230 || 230 || 230 || 230 || 500<br />
|-<br />
| 1/f exponent TT || -4.1 || -4.1 || -4.1 || -4.1 || -3.8 || -3.8 || -3.8 || -3.8 || -3.8<br />
|-<br />
| white noise level EE (uK-arcmin) || 10.85 || 11.06 || 1.93 || 1.58 || 2.49 || 2.56 || 5.55 || 8.30 || 2.56 <br />
|-<br />
| ell knee EE || 50 || 50 || 50 || 50 || 65 || 65 || 65 || 65 || 200<br />
|-<br />
| 1/f exponent EE || -2.0 || -2.0 || -2.0 || -2.0 || -3.0 || -3.0 || -3.0 || -3.0 || -3.0<br />
|-<br />
| white noise level BB (uK-arcmin) || 10.59 || 10.79 || 1.88 || 1.54 || 2.38 || 2.45 || 5.30 || 7.93 || 2.45<br />
|-<br />
| ell knee BB || 50 || 50 || 50 || 50 || 60 || 60 || 60 || 60 || 200<br />
|-<br />
| 1/f exponent BB || -2.0 || -2.0 || -2.0 || -2.0 || -3.0 || -3.0 || -3.0 || -3.0 || -3.0<br />
|-<br />
| ell min || 30 || 30 || 30 || 30 || 30 || 30 || 30 || 30 || 100<br />
|-<br />
| nside || 512 || 512 || 512 || 512 || 512 || 512 || 512 || 512 || 2048<br />
|}<br />
<br />
These parameters are in the file '''expt_xx/01/params.dat''' and give rise to the window functions in '''expt_xx/01/wfunc''' and the noise spectra in '''expt_xx/01/noise/cls'''.<br />
The intent of the low ell cutoff is to approximate the effect of the timestream filtering which is commonly done in ground based experiments (and as some kind of acknowledgement that<br />
the largest angular scales may anyway be corrupted by systematic effects).<br />
<br />
Additionally '''expt_xx/01/rhits/fsky03bk_n0512.fits''' is supposed to represent the "relative hits" with which the sky has been observed.<br />
This is a circular pattern centred at RA=0, Dec=-45 (a bit below the BICEP/Keck patch) which is flat at one out to r=12deg and then rolls down to zero as cosine squared over an<br />
additional 15 deg.<br />
This is some kind of approximation as to what small apertures might deliver (given their large instantaneous field of view).<br />
<br />
From the noise spectra sets of alms are generated (with nlmax=4096) with names like '''expt_xx/01/noise/alm/noise_f155_b15_ellmin30_alm_mc_0000.fits''' where 155 is the frequency, 15 is the beam size (in arcmin), and 0000 is the realization number. <br />
<br />
From these full sky maps are rendered at nside=512 and nlmax=1024. No beam smoothing is applied as is appropriate for noise.<br />
The maps have names like '''expt_xx/01/noise/map/noise_f155_b15_ellmin30_map_0512_mc_0000.fits'''.<br />
<br />
The full sky noise is then divided by the square-root of the rhits mask and the result stored in files like '''data_xx.yy/01.YY/cmbs4_01_noise_f155_b15_ellmin30_map_0512_mc_0000.fits''' - these are the noise realizations that one would have access to in a real experiment - the noise blows up around the edge.<br />
<br />
These masked noise realizations are then added to the sky model (LCDM+dust+sync+) and stored in names like '''data_xx.yy/01.YY/cmbs4_01pYY_comb_f155_b15_ellmin30_map_0512_mc_0000.fits'''.<br />
As a crude simulation of delensing these combined maps are also provided with the lensing effect reduced to 30, 10 and 3% of reality by combining lensed and unlensed LCDM - look for files<br />
with names like '''data_xx.yy/01.YY/cmbs4_01pYY_comb_AL0p3_f155_b15_ellmin30_map_0512_mc_0000.fits'''.<br />
Maps with partial lensing are constructed by the following combination: partially_lensed_map = sqrt(A_L) * lensed_map + (1 - sqrt(A_L)) * unlensed_map.<br />
<br />
To analyze these maps one should use only the '''expt_xx/01/params.dat''' file and the maps under '''data_xx.yy/01.YY'''.<br />
A thousand realizations are present.<br />
We can see these maps [[01.00 sim input maps | in this posting]]<br />
<br />
The last column of the table above shows one additional tweak - a second 155GHz band with a higher 1/f knee and smaller beam size - this is supposed to<br />
represent the maps made by higher resolution telescopes running in concert with small apertures in a hybrid approach.<br />
These maps can in principle be used to reconstruct the lensing potential and delens explicitly - instead of cheating by using<br />
the AL0p3 files etc.<br />
At the moment the noise spectrum in these maps is provisional.<br />
Additionally we may wish to add additional frequency bands at higher resolution so foreground cleaning<br />
before delensing can be done.<br />
We can see these maps [[Adding higher res delensing "band" | in this posting]].<br />
<br />
(The filtered LLCDM realizations are also copied in '''data_xx.yy/01.YY''' as these are needed to build the bandpower covariance matrix in the multi-component cross spectrum approach used by the BK group.<br />
It seems reasonable that one would always have realizations of a known spectrum signal passed through an experimental simulation.)</div>Jchhttp://www.cmb-s4.org/wiki/index.php?title=Survey_Performance_Expectations&diff=7904Survey Performance Expectations2018-10-09T20:54:33Z<p>Jch: /* Large-area Experiment Definition 01 */</p>
<hr />
<div>This page summarizes the various experiment definitions.<br />
The data products referred to are located on the NERSC system under '''/project/projectdirs/cmbs4/expt_xx'''<br />
<br />
===Large-area Experiment Definition 01===<br />
The NTT should fill in here what they can, with input from large-area forecasters where needed. <br />
Ideally there would be separate specifications of instrument capabilities, and assumed sky coverage, rather than<br />
having these lumped together.<br />
<br />
The numbers below are based on the Noise Tiger Team product lat-noise-181002.py , run assuming the default settings and fsky=0.4. The default settings include 2 LATs, each equipped with 1 ULF tube, 2 LF tubes, 12 MF tubes, and 4 UHF tubes. Note that the EE and BB noise levels are sqrt(2) higher than the TT noise levels and are omitted from the table below for brevity. The atmospheric treatment and other details are described in the code and in this PDF document:<br />
[[File:lat-noise-181002.pdf]]<br />
<br />
{| class="wikitable" style="text-align: right; margin-left: 51px;"<br />
! Frequency (GHz) !! 20 !! 27 !! 39 !! 93 !! 145 !! 225 !! 280<br />
|-<br />
| Bandwidth (GHz) || n/a || n/a || n/a || n/a || n/a || n/a || n/a<br />
|-<br />
| Beam FWHM (arcmin) || 10. || 7.4 || 5.1 || 2.2 || 1.4 || 1.0 || 0.9<br />
|-<br />
| white noise level TT (uK-arcmin) || 45.9 || 15.5 || 8.7 || 1.5 || 1.5 || 4.8|| 11.5<br />
|-<br />
|}<br />
<br />
===Small-area Experiment Definition 05===<br />
The NTT should fill in here what they can, with input from small-area forecasters (r forecasters) where needed. Ideally instrument capabilities are distinct from specification of survey coverage, so coverage can be iterated without changing the instrument. For LAT instrument capability, it would make sense to refer to the appropriate Large-area Experiment Definition rather than reproduce a description of the LATs here.<br />
<br />
=== Experiment Definition 04 ===<br />
This is very similar to 02 but with the noise levels tweaked down by sqrt(7/6) to try and get sigma(r)=1e-4 as per science requirement.<br />
(The noise map generator has also been tweaked such that the level quoted in the params.dat table will be reproduced exactly when the power spectra of the maps is taken with the provided mask - i.e. the actual noise level will slightly lower in the center of the mask.)<br />
A 20GHz band has been added which is assumed to be on a large aperture telescope (and hence has higher resolution and ell knee).<br />
Below is the contents of the params.dat file. The noise levels and resolutions are copied from the [https://www.nsf.gov/mps/ast/aaac/cmb_s4/report/CMBS4_final_report_NL.pdf CDT report] "Science Traceability Matrix".<br />
Specs for the high res bands exist but have not been added yet. <br />
<br />
{| class="wikitable" style="text-align: right; margin-left: 51px;"<br />
! Frequency (GHz) !! 20 !! 30 !! 40 !! 85 !! 95 !! 145 !! 155 !! 220 !! 270<br />
|-<br />
| Bandwidth (GHz) || 5.0 || 9.0 || 12.0 || 20.4 || 22.8 || 31.9 || 34.1 || 48.4 || 59.4<br />
|-<br />
| Beam FWHM (arcmin) || 11.0 || 76.6 || 57.5 || 27.0 || 24.2 || 15.9 || 14.8 || 10.7 || 8.5<br />
|-<br />
| white noise level TT (uK-arcmin) || 16.66 || 10.62 || 10.07 || 2.01 || 1.59 || 4.53 || 4.53 || 11.61 || 15.84<br />
|-<br />
| ell knee TT || 500 || 175 || 175 || 175 || 175 || 230 || 230 || 230 || 230<br />
|-<br />
| 1/f exponent TT || -4.1 || -4.1 || -4.1 || -4.1 || -4.1 || -3.8 || -3.8 || -3.8 || -3.8<br />
|-<br />
| white noise level EE (uK-arcmin) || 13.94 || 8.88 || 8.42 || 1.67 || 1.32 || 2.12 || 2.12 || 5.43 || 7.42 <br />
|-<br />
| ell knee EE || 200 || 50 || 50 || 50 || 50 || 65 || 65 || 65 || 65<br />
|-<br />
| 1/f exponent EE || -2.0 || -2.0 || -2.0 || -2.0 || -2.0 || -3.0 || -3.0 || -3.0 || -3.0<br />
|-<br />
| white noise level BB (uK-arcmin) || 13.6 || 8.67 || 8.22 || 1.64 || 1.30 || 2.03 || 2.03 || 5.19 || 7.08<br />
|-<br />
| ell knee BB || 200 || 50 || 50 || 50 || 50 || 60 || 60 || 60 || 60<br />
|-<br />
| 1/f exponent BB || -2.0 || -2.0 || -2.0 || -2.0 || -2.0 || -3.0 || -3.0 || -3.0 || -3.0<br />
|-<br />
| ell min || 30 || 30 || 30 || 30 || 30 || 30 || 30 || 30 || 30 <br />
|-<br />
| nside || 512 || 512 || 512 || 512 || 512 || 512 || 512 || 512 || 512<br />
|}<br />
<br />
=== Experiment Definition 03, 03b, 03c ===<br />
These sims are nearly identical to experiment definition 02, 02b, 02c, and even use the same noise realizations. The one change is the inclusion of additive systematics, following the prescription described in this [[Additive_systematics_for_data_challenge_03|2017-07-10 posting]]. Blocks of realizations contain different versions of the additive systematic, as shown below. For all cases, the level of the systematic is chosen to yield bias on ''r'' of 1e-4 (by the analysis of the 2017-07-10 posting). The first block of realizations, 0000&ndash;0124, contains no systematic and should be completely identical to the 02/02b/02c realizations.<br />
<br />
{| class="wikitable"<br />
|-<br />
! realizations !! A<sub>uncorr</sub> !! B<sub>uncorr</sub> !! A<sub>corr</sub> !! B<sub>corr</sub> !! Description<br />
|-<br />
| 0000&ndash;0124 || 0 || 0 || 0 || 0 || No systematics<br />
|-<br />
| 0125&ndash;0249 || 0.0328 || 0 || 0 || 0 || Uncorrelated systematic with white spectrum<br />
|-<br />
| 0250&ndash;0374 || 0 || 0.0689 || 0 || 0 || Uncorrelated systematic with 1/ell spectrum<br />
|-<br />
| 0375&ndash;0499 || 0 || 0 || 0.0584 || 0 || Correlated systematic with white spectrum<br />
|-<br />
| 0500&ndash;0624 || 0 || 0 || 0 || 0.1049 || Correlated systematic with 1/ell spectrum<br />
|-<br />
| 0625&ndash;0749 || 0.0164 || 0.0345 || 0 || 0 || Uncorrelated systematic with white + 1/ell spectrum<br />
|-<br />
| 0750&ndash;0874 || 0 || 0 || 0.0292 || 0.0525 || Correlated systematic with white + 1/ell spectrum<br />
|-<br />
| 0875&ndash;0999 || 0.0082 || 0.0172 || 0.0146 || 0.0262 || Uncorrelated + correlated systematic with white + 1/ell spectrum<br />
|}<br />
<br />
Combined maps for analysis can be found on NERSC in '''/project/projectdirs/cmbs4/data_xx.yy/03''' etc.<br />
<br />
Parameters and ingredients for the combined maps can be found in '''/project/projectdirs/cmbs4/expt_xx/03''' etc. Note that noise, rhits, and wfunc are actually symlinks to those directories under experiment configs 02, 02b, 02c.<br />
<br />
=== Experiment Definition 02, 02b, 02c ===<br />
This is an update from 01 which differs in the following ways:<br />
<br />
1) Addition of 20GHz band and (slight) changes to the band/detector optimization as per<br />
[[http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170515_chkS4 Victor's May 15 posting in the logbook]].<br />
<br />
2) Addition of 3 delensing bands 95/155/220GHz with same number of detectors as the low res equivalent bands<br />
but beam size 4x higher. This adds up to approximately the same number of detectors but clearly one should reoptimize<br />
once they are not all at the same freq. Since we are still quite far from having real lensing reconstruction and realistic<br />
(non-Gaussian) high ell foregrounds this probably is OK for this round.<br />
<br />
3) Addition of tensors - even number realizations have r=0.003, odd number have r=0.<br />
<br />
4) Set 02 is the same nominal 3% sky patch as set 01. We now add 02b which is 1% round patch with center<br />
the same as the BICEP/Keck patch (RA=0, Dec=-57.5), and 02c which is 10% round patch centered on RA=15deg, Dec=-35.<br />
<br />
These products appear on NERSC under '''/project/projectdirs/cmbs4/expt_xx/02''' etc.<br />
<br />
=== Experiment Definition 01 ===<br />
This is intended to be basically the same as the assumptions made for the Fisher calculations done for the Science Book.<br />
The parameters come from [[http://users.physics.harvard.edu/~buza/20161220_chkS4 Victor's Dec 21 posting in the logbook]] with the addition of bandwidths from<br />
[[Tophat_bands_for_Data_Challenge|Colin's Nov 4 posting]] and are summarized in the following table:<br />
<br />
{| class="wikitable" style="text-align: right; margin-left: 51px;"<br />
! Frequency (GHz) !! 30 !! 40 !! 85 !! 95 !! 145 !! 155 !! 220 !! 270 !! 155 HR<br />
|-<br />
| Bandwidth (GHz) || 9.0 || 12.0 || 20.4 || 22.8 || 31.9 || 34.1 || 48.4 || 59.4 || 34.1<br />
|-<br />
| Beam FWHM (arcmin) || 76.6 || 57.5 || 27.0 || 24.2 || 15.9 || 14.8 || 10.7 || 8.5 || 4.0<br />
|-<br />
| white noise level TT (uK-arcmin) || 12.97 || 13.22 || 2.30 || 1.89 || 5.31 || 5.48 || 11.86 || 17.72 || 5.48<br />
|-<br />
| ell knee TT || 175 || 175 || 175 || 175 || 230 || 230 || 230 || 230 || 500<br />
|-<br />
| 1/f exponent TT || -4.1 || -4.1 || -4.1 || -4.1 || -3.8 || -3.8 || -3.8 || -3.8 || -3.8<br />
|-<br />
| white noise level EE (uK-arcmin) || 10.85 || 11.06 || 1.93 || 1.58 || 2.49 || 2.56 || 5.55 || 8.30 || 2.56 <br />
|-<br />
| ell knee EE || 50 || 50 || 50 || 50 || 65 || 65 || 65 || 65 || 200<br />
|-<br />
| 1/f exponent EE || -2.0 || -2.0 || -2.0 || -2.0 || -3.0 || -3.0 || -3.0 || -3.0 || -3.0<br />
|-<br />
| white noise level BB (uK-arcmin) || 10.59 || 10.79 || 1.88 || 1.54 || 2.38 || 2.45 || 5.30 || 7.93 || 2.45<br />
|-<br />
| ell knee BB || 50 || 50 || 50 || 50 || 60 || 60 || 60 || 60 || 200<br />
|-<br />
| 1/f exponent BB || -2.0 || -2.0 || -2.0 || -2.0 || -3.0 || -3.0 || -3.0 || -3.0 || -3.0<br />
|-<br />
| ell min || 30 || 30 || 30 || 30 || 30 || 30 || 30 || 30 || 100<br />
|-<br />
| nside || 512 || 512 || 512 || 512 || 512 || 512 || 512 || 512 || 2048<br />
|}<br />
<br />
These parameters are in the file '''expt_xx/01/params.dat''' and give rise to the window functions in '''expt_xx/01/wfunc''' and the noise spectra in '''expt_xx/01/noise/cls'''.<br />
The intent of the low ell cutoff is to approximate the effect of the timestream filtering which is commonly done in ground based experiments (and as some kind of acknowledgement that<br />
the largest angular scales may anyway be corrupted by systematic effects).<br />
<br />
Additionally '''expt_xx/01/rhits/fsky03bk_n0512.fits''' is supposed to represent the "relative hits" with which the sky has been observed.<br />
This is a circular pattern centred at RA=0, Dec=-45 (a bit below the BICEP/Keck patch) which is flat at one out to r=12deg and then rolls down to zero as cosine squared over an<br />
additional 15 deg.<br />
This is some kind of approximation as to what small apertures might deliver (given their large instantaneous field of view).<br />
<br />
From the noise spectra sets of alms are generated (with nlmax=4096) with names like '''expt_xx/01/noise/alm/noise_f155_b15_ellmin30_alm_mc_0000.fits''' where 155 is the frequency, 15 is the beam size (in arcmin), and 0000 is the realization number. <br />
<br />
From these full sky maps are rendered at nside=512 and nlmax=1024. No beam smoothing is applied as is appropriate for noise.<br />
The maps have names like '''expt_xx/01/noise/map/noise_f155_b15_ellmin30_map_0512_mc_0000.fits'''.<br />
<br />
The full sky noise is then divided by the square-root of the rhits mask and the result stored in files like '''data_xx.yy/01.YY/cmbs4_01_noise_f155_b15_ellmin30_map_0512_mc_0000.fits''' - these are the noise realizations that one would have access to in a real experiment - the noise blows up around the edge.<br />
<br />
These masked noise realizations are then added to the sky model (LCDM+dust+sync+) and stored in names like '''data_xx.yy/01.YY/cmbs4_01pYY_comb_f155_b15_ellmin30_map_0512_mc_0000.fits'''.<br />
As a crude simulation of delensing these combined maps are also provided with the lensing effect reduced to 30, 10 and 3% of reality by combining lensed and unlensed LCDM - look for files<br />
with names like '''data_xx.yy/01.YY/cmbs4_01pYY_comb_AL0p3_f155_b15_ellmin30_map_0512_mc_0000.fits'''.<br />
Maps with partial lensing are constructed by the following combination: partially_lensed_map = sqrt(A_L) * lensed_map + (1 - sqrt(A_L)) * unlensed_map.<br />
<br />
To analyze these maps one should use only the '''expt_xx/01/params.dat''' file and the maps under '''data_xx.yy/01.YY'''.<br />
A thousand realizations are present.<br />
We can see these maps [[01.00 sim input maps | in this posting]]<br />
<br />
The last column of the table above shows one additional tweak - a second 155GHz band with a higher 1/f knee and smaller beam size - this is supposed to<br />
represent the maps made by higher resolution telescopes running in concert with small apertures in a hybrid approach.<br />
These maps can in principle be used to reconstruct the lensing potential and delens explicitly - instead of cheating by using<br />
the AL0p3 files etc.<br />
At the moment the noise spectrum in these maps is provisional.<br />
Additionally we may wish to add additional frequency bands at higher resolution so foreground cleaning<br />
before delensing can be done.<br />
We can see these maps [[Adding higher res delensing "band" | in this posting]].<br />
<br />
(The filtered LLCDM realizations are also copied in '''data_xx.yy/01.YY''' as these are needed to build the bandpower covariance matrix in the multi-component cross spectrum approach used by the BK group.<br />
It seems reasonable that one would always have realizations of a known spectrum signal passed through an experimental simulation.)</div>Jchhttp://www.cmb-s4.org/wiki/index.php?title=File:Lat-noise-181002.pdf&diff=7903File:Lat-noise-181002.pdf2018-10-09T20:53:06Z<p>Jch: </p>
<hr />
<div></div>Jchhttp://www.cmb-s4.org/wiki/index.php?title=Survey_Performance_Expectations&diff=7902Survey Performance Expectations2018-10-09T20:50:22Z<p>Jch: /* Large-area Experiment Definition 01 */</p>
<hr />
<div>This page summarizes the various experiment definitions.<br />
The data products referred to are located on the NERSC system under '''/project/projectdirs/cmbs4/expt_xx'''<br />
<br />
===Large-area Experiment Definition 01===<br />
The NTT should fill in here what they can, with input from large-area forecasters where needed. <br />
Ideally there would be separate specifications of instrument capabilities, and assumed sky coverage, rather than<br />
having these lumped together.<br />
<br />
The numbers below are based on the Noise Tiger Team product lat-noise-181002.py , run assuming the default settings and fsky=0.4. The default settings include 2 LATs, each equipped with 1 ULF tube, 2 LF tubes, 12 MF tubes, and 4 UHF tubes. Note that the EE and BB noise levels are sqrt(2) higher than the TT noise levels and are omitted from the table below for brevity. The atmospheric treatment is described in the code.<br />
<br />
{| class="wikitable" style="text-align: right; margin-left: 51px;"<br />
! Frequency (GHz) !! 20 !! 27 !! 39 !! 93 !! 145 !! 225 !! 280<br />
|-<br />
| Bandwidth (GHz) || n/a || n/a || n/a || n/a || n/a || n/a || n/a<br />
|-<br />
| Beam FWHM (arcmin) || 10. || 7.4 || 5.1 || 2.2 || 1.4 || 1.0 || 0.9<br />
|-<br />
| white noise level TT (uK-arcmin) || 45.9 || 15.5 || 8.7 || 1.5 || 1.5 || 4.8|| 11.5<br />
|-<br />
|}<br />
<br />
===Small-area Experiment Definition 05===<br />
The NTT should fill in here what they can, with input from small-area forecasters (r forecasters) where needed. Ideally instrument capabilities are distinct from specification of survey coverage, so coverage can be iterated without changing the instrument. For LAT instrument capability, it would make sense to refer to the appropriate Large-area Experiment Definition rather than reproduce a description of the LATs here.<br />
<br />
=== Experiment Definition 04 ===<br />
This is very similar to 02 but with the noise levels tweaked down by sqrt(7/6) to try and get sigma(r)=1e-4 as per science requirement.<br />
(The noise map generator has also been tweaked such that the level quoted in the params.dat table will be reproduced exactly when the power spectra of the maps is taken with the provided mask - i.e. the actual noise level will slightly lower in the center of the mask.)<br />
A 20GHz band has been added which is assumed to be on a large aperture telescope (and hence has higher resolution and ell knee).<br />
Below is the contents of the params.dat file. The noise levels and resolutions are copied from the [https://www.nsf.gov/mps/ast/aaac/cmb_s4/report/CMBS4_final_report_NL.pdf CDT report] "Science Traceability Matrix".<br />
Specs for the high res bands exist but have not been added yet. <br />
<br />
{| class="wikitable" style="text-align: right; margin-left: 51px;"<br />
! Frequency (GHz) !! 20 !! 30 !! 40 !! 85 !! 95 !! 145 !! 155 !! 220 !! 270<br />
|-<br />
| Bandwidth (GHz) || 5.0 || 9.0 || 12.0 || 20.4 || 22.8 || 31.9 || 34.1 || 48.4 || 59.4<br />
|-<br />
| Beam FWHM (arcmin) || 11.0 || 76.6 || 57.5 || 27.0 || 24.2 || 15.9 || 14.8 || 10.7 || 8.5<br />
|-<br />
| white noise level TT (uK-arcmin) || 16.66 || 10.62 || 10.07 || 2.01 || 1.59 || 4.53 || 4.53 || 11.61 || 15.84<br />
|-<br />
| ell knee TT || 500 || 175 || 175 || 175 || 175 || 230 || 230 || 230 || 230<br />
|-<br />
| 1/f exponent TT || -4.1 || -4.1 || -4.1 || -4.1 || -4.1 || -3.8 || -3.8 || -3.8 || -3.8<br />
|-<br />
| white noise level EE (uK-arcmin) || 13.94 || 8.88 || 8.42 || 1.67 || 1.32 || 2.12 || 2.12 || 5.43 || 7.42 <br />
|-<br />
| ell knee EE || 200 || 50 || 50 || 50 || 50 || 65 || 65 || 65 || 65<br />
|-<br />
| 1/f exponent EE || -2.0 || -2.0 || -2.0 || -2.0 || -2.0 || -3.0 || -3.0 || -3.0 || -3.0<br />
|-<br />
| white noise level BB (uK-arcmin) || 13.6 || 8.67 || 8.22 || 1.64 || 1.30 || 2.03 || 2.03 || 5.19 || 7.08<br />
|-<br />
| ell knee BB || 200 || 50 || 50 || 50 || 50 || 60 || 60 || 60 || 60<br />
|-<br />
| 1/f exponent BB || -2.0 || -2.0 || -2.0 || -2.0 || -2.0 || -3.0 || -3.0 || -3.0 || -3.0<br />
|-<br />
| ell min || 30 || 30 || 30 || 30 || 30 || 30 || 30 || 30 || 30 <br />
|-<br />
| nside || 512 || 512 || 512 || 512 || 512 || 512 || 512 || 512 || 512<br />
|}<br />
<br />
=== Experiment Definition 03, 03b, 03c ===<br />
These sims are nearly identical to experiment definition 02, 02b, 02c, and even use the same noise realizations. The one change is the inclusion of additive systematics, following the prescription described in this [[Additive_systematics_for_data_challenge_03|2017-07-10 posting]]. Blocks of realizations contain different versions of the additive systematic, as shown below. For all cases, the level of the systematic is chosen to yield bias on ''r'' of 1e-4 (by the analysis of the 2017-07-10 posting). The first block of realizations, 0000&ndash;0124, contains no systematic and should be completely identical to the 02/02b/02c realizations.<br />
<br />
{| class="wikitable"<br />
|-<br />
! realizations !! A<sub>uncorr</sub> !! B<sub>uncorr</sub> !! A<sub>corr</sub> !! B<sub>corr</sub> !! Description<br />
|-<br />
| 0000&ndash;0124 || 0 || 0 || 0 || 0 || No systematics<br />
|-<br />
| 0125&ndash;0249 || 0.0328 || 0 || 0 || 0 || Uncorrelated systematic with white spectrum<br />
|-<br />
| 0250&ndash;0374 || 0 || 0.0689 || 0 || 0 || Uncorrelated systematic with 1/ell spectrum<br />
|-<br />
| 0375&ndash;0499 || 0 || 0 || 0.0584 || 0 || Correlated systematic with white spectrum<br />
|-<br />
| 0500&ndash;0624 || 0 || 0 || 0 || 0.1049 || Correlated systematic with 1/ell spectrum<br />
|-<br />
| 0625&ndash;0749 || 0.0164 || 0.0345 || 0 || 0 || Uncorrelated systematic with white + 1/ell spectrum<br />
|-<br />
| 0750&ndash;0874 || 0 || 0 || 0.0292 || 0.0525 || Correlated systematic with white + 1/ell spectrum<br />
|-<br />
| 0875&ndash;0999 || 0.0082 || 0.0172 || 0.0146 || 0.0262 || Uncorrelated + correlated systematic with white + 1/ell spectrum<br />
|}<br />
<br />
Combined maps for analysis can be found on NERSC in '''/project/projectdirs/cmbs4/data_xx.yy/03''' etc.<br />
<br />
Parameters and ingredients for the combined maps can be found in '''/project/projectdirs/cmbs4/expt_xx/03''' etc. Note that noise, rhits, and wfunc are actually symlinks to those directories under experiment configs 02, 02b, 02c.<br />
<br />
=== Experiment Definition 02, 02b, 02c ===<br />
This is an update from 01 which differs in the following ways:<br />
<br />
1) Addition of 20GHz band and (slight) changes to the band/detector optimization as per<br />
[[http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170515_chkS4 Victor's May 15 posting in the logbook]].<br />
<br />
2) Addition of 3 delensing bands 95/155/220GHz with same number of detectors as the low res equivalent bands<br />
but beam size 4x higher. This adds up to approximately the same number of detectors but clearly one should reoptimize<br />
once they are not all at the same freq. Since we are still quite far from having real lensing reconstruction and realistic<br />
(non-Gaussian) high ell foregrounds this probably is OK for this round.<br />
<br />
3) Addition of tensors - even number realizations have r=0.003, odd number have r=0.<br />
<br />
4) Set 02 is the same nominal 3% sky patch as set 01. We now add 02b which is 1% round patch with center<br />
the same as the BICEP/Keck patch (RA=0, Dec=-57.5), and 02c which is 10% round patch centered on RA=15deg, Dec=-35.<br />
<br />
These products appear on NERSC under '''/project/projectdirs/cmbs4/expt_xx/02''' etc.<br />
<br />
=== Experiment Definition 01 ===<br />
This is intended to be basically the same as the assumptions made for the Fisher calculations done for the Science Book.<br />
The parameters come from [[http://users.physics.harvard.edu/~buza/20161220_chkS4 Victor's Dec 21 posting in the logbook]] with the addition of bandwidths from<br />
[[Tophat_bands_for_Data_Challenge|Colin's Nov 4 posting]] and are summarized in the following table:<br />
<br />
{| class="wikitable" style="text-align: right; margin-left: 51px;"<br />
! Frequency (GHz) !! 30 !! 40 !! 85 !! 95 !! 145 !! 155 !! 220 !! 270 !! 155 HR<br />
|-<br />
| Bandwidth (GHz) || 9.0 || 12.0 || 20.4 || 22.8 || 31.9 || 34.1 || 48.4 || 59.4 || 34.1<br />
|-<br />
| Beam FWHM (arcmin) || 76.6 || 57.5 || 27.0 || 24.2 || 15.9 || 14.8 || 10.7 || 8.5 || 4.0<br />
|-<br />
| white noise level TT (uK-arcmin) || 12.97 || 13.22 || 2.30 || 1.89 || 5.31 || 5.48 || 11.86 || 17.72 || 5.48<br />
|-<br />
| ell knee TT || 175 || 175 || 175 || 175 || 230 || 230 || 230 || 230 || 500<br />
|-<br />
| 1/f exponent TT || -4.1 || -4.1 || -4.1 || -4.1 || -3.8 || -3.8 || -3.8 || -3.8 || -3.8<br />
|-<br />
| white noise level EE (uK-arcmin) || 10.85 || 11.06 || 1.93 || 1.58 || 2.49 || 2.56 || 5.55 || 8.30 || 2.56 <br />
|-<br />
| ell knee EE || 50 || 50 || 50 || 50 || 65 || 65 || 65 || 65 || 200<br />
|-<br />
| 1/f exponent EE || -2.0 || -2.0 || -2.0 || -2.0 || -3.0 || -3.0 || -3.0 || -3.0 || -3.0<br />
|-<br />
| white noise level BB (uK-arcmin) || 10.59 || 10.79 || 1.88 || 1.54 || 2.38 || 2.45 || 5.30 || 7.93 || 2.45<br />
|-<br />
| ell knee BB || 50 || 50 || 50 || 50 || 60 || 60 || 60 || 60 || 200<br />
|-<br />
| 1/f exponent BB || -2.0 || -2.0 || -2.0 || -2.0 || -3.0 || -3.0 || -3.0 || -3.0 || -3.0<br />
|-<br />
| ell min || 30 || 30 || 30 || 30 || 30 || 30 || 30 || 30 || 100<br />
|-<br />
| nside || 512 || 512 || 512 || 512 || 512 || 512 || 512 || 512 || 2048<br />
|}<br />
<br />
These parameters are in the file '''expt_xx/01/params.dat''' and give rise to the window functions in '''expt_xx/01/wfunc''' and the noise spectra in '''expt_xx/01/noise/cls'''.<br />
The intent of the low ell cutoff is to approximate the effect of the timestream filtering which is commonly done in ground based experiments (and as some kind of acknowledgement that<br />
the largest angular scales may anyway be corrupted by systematic effects).<br />
<br />
Additionally '''expt_xx/01/rhits/fsky03bk_n0512.fits''' is supposed to represent the "relative hits" with which the sky has been observed.<br />
This is a circular pattern centred at RA=0, Dec=-45 (a bit below the BICEP/Keck patch) which is flat at one out to r=12deg and then rolls down to zero as cosine squared over an<br />
additional 15 deg.<br />
This is some kind of approximation as to what small apertures might deliver (given their large instantaneous field of view).<br />
<br />
From the noise spectra sets of alms are generated (with nlmax=4096) with names like '''expt_xx/01/noise/alm/noise_f155_b15_ellmin30_alm_mc_0000.fits''' where 155 is the frequency, 15 is the beam size (in arcmin), and 0000 is the realization number. <br />
<br />
From these full sky maps are rendered at nside=512 and nlmax=1024. No beam smoothing is applied as is appropriate for noise.<br />
The maps have names like '''expt_xx/01/noise/map/noise_f155_b15_ellmin30_map_0512_mc_0000.fits'''.<br />
<br />
The full sky noise is then divided by the square-root of the rhits mask and the result stored in files like '''data_xx.yy/01.YY/cmbs4_01_noise_f155_b15_ellmin30_map_0512_mc_0000.fits''' - these are the noise realizations that one would have access to in a real experiment - the noise blows up around the edge.<br />
<br />
These masked noise realizations are then added to the sky model (LCDM+dust+sync+) and stored in names like '''data_xx.yy/01.YY/cmbs4_01pYY_comb_f155_b15_ellmin30_map_0512_mc_0000.fits'''.<br />
As a crude simulation of delensing these combined maps are also provided with the lensing effect reduced to 30, 10 and 3% of reality by combining lensed and unlensed LCDM - look for files<br />
with names like '''data_xx.yy/01.YY/cmbs4_01pYY_comb_AL0p3_f155_b15_ellmin30_map_0512_mc_0000.fits'''.<br />
Maps with partial lensing are constructed by the following combination: partially_lensed_map = sqrt(A_L) * lensed_map + (1 - sqrt(A_L)) * unlensed_map.<br />
<br />
To analyze these maps one should use only the '''expt_xx/01/params.dat''' file and the maps under '''data_xx.yy/01.YY'''.<br />
A thousand realizations are present.<br />
We can see these maps [[01.00 sim input maps | in this posting]]<br />
<br />
The last column of the table above shows one additional tweak - a second 155GHz band with a higher 1/f knee and smaller beam size - this is supposed to<br />
represent the maps made by higher resolution telescopes running in concert with small apertures in a hybrid approach.<br />
These maps can in principle be used to reconstruct the lensing potential and delens explicitly - instead of cheating by using<br />
the AL0p3 files etc.<br />
At the moment the noise spectrum in these maps is provisional.<br />
Additionally we may wish to add additional frequency bands at higher resolution so foreground cleaning<br />
before delensing can be done.<br />
We can see these maps [[Adding higher res delensing "band" | in this posting]].<br />
<br />
(The filtered LLCDM realizations are also copied in '''data_xx.yy/01.YY''' as these are needed to build the bandpower covariance matrix in the multi-component cross spectrum approach used by the BK group.<br />
It seems reasonable that one would always have realizations of a known spectrum signal passed through an experimental simulation.)</div>Jchhttp://www.cmb-s4.org/wiki/index.php?title=Survey_Performance_Expectations&diff=7901Survey Performance Expectations2018-10-09T20:48:18Z<p>Jch: /* Large-area Experiment Definition 01 */</p>
<hr />
<div>This page summarizes the various experiment definitions.<br />
The data products referred to are located on the NERSC system under '''/project/projectdirs/cmbs4/expt_xx'''<br />
<br />
===Large-area Experiment Definition 01===<br />
The NTT should fill in here what they can, with input from large-area forecasters where needed. <br />
Ideally there would be separate specifications of instrument capabilities, and assumed sky coverage, rather than<br />
having these lumped together.<br />
<br />
The numbers below are based on the Noise Tiger Team product lat-noise-181002.py , run assuming the default settings and fsky=0.4. The EE and BB noise levels are sqrt(2) higher than the TT noise levels. The atmospheric treatment is described in the code.<br />
<br />
{| class="wikitable" style="text-align: right; margin-left: 51px;"<br />
! Frequency (GHz) !! 20 !! 27 !! 39 !! 93 !! 145 !! 225 !! 280<br />
|-<br />
| Bandwidth (GHz) || n/a || n/a || n/a || n/a || n/a || n/a || n/a<br />
|-<br />
| Beam FWHM (arcmin) || 10. || 7.4 || 5.1 || 2.2 || 1.4 || 1.0 || 0.9<br />
|-<br />
| white noise level TT (uK-arcmin) || 45.9 || 15.5 || 8.7 || 1.5 || 1.5 || 4.8|| 11.5<br />
|-<br />
|}<br />
<br />
===Small-area Experiment Definition 05===<br />
The NTT should fill in here what they can, with input from small-area forecasters (r forecasters) where needed. Ideally instrument capabilities are distinct from specification of survey coverage, so coverage can be iterated without changing the instrument. For LAT instrument capability, it would make sense to refer to the appropriate Large-area Experiment Definition rather than reproduce a description of the LATs here.<br />
<br />
=== Experiment Definition 04 ===<br />
This is very similar to 02 but with the noise levels tweaked down by sqrt(7/6) to try and get sigma(r)=1e-4 as per science requirement.<br />
(The noise map generator has also been tweaked such that the level quoted in the params.dat table will be reproduced exactly when the power spectra of the maps is taken with the provided mask - i.e. the actual noise level will slightly lower in the center of the mask.)<br />
A 20GHz band has been added which is assumed to be on a large aperture telescope (and hence has higher resolution and ell knee).<br />
Below is the contents of the params.dat file. The noise levels and resolutions are copied from the [https://www.nsf.gov/mps/ast/aaac/cmb_s4/report/CMBS4_final_report_NL.pdf CDT report] "Science Traceability Matrix".<br />
Specs for the high res bands exist but have not been added yet. <br />
<br />
{| class="wikitable" style="text-align: right; margin-left: 51px;"<br />
! Frequency (GHz) !! 20 !! 30 !! 40 !! 85 !! 95 !! 145 !! 155 !! 220 !! 270<br />
|-<br />
| Bandwidth (GHz) || 5.0 || 9.0 || 12.0 || 20.4 || 22.8 || 31.9 || 34.1 || 48.4 || 59.4<br />
|-<br />
| Beam FWHM (arcmin) || 11.0 || 76.6 || 57.5 || 27.0 || 24.2 || 15.9 || 14.8 || 10.7 || 8.5<br />
|-<br />
| white noise level TT (uK-arcmin) || 16.66 || 10.62 || 10.07 || 2.01 || 1.59 || 4.53 || 4.53 || 11.61 || 15.84<br />
|-<br />
| ell knee TT || 500 || 175 || 175 || 175 || 175 || 230 || 230 || 230 || 230<br />
|-<br />
| 1/f exponent TT || -4.1 || -4.1 || -4.1 || -4.1 || -4.1 || -3.8 || -3.8 || -3.8 || -3.8<br />
|-<br />
| white noise level EE (uK-arcmin) || 13.94 || 8.88 || 8.42 || 1.67 || 1.32 || 2.12 || 2.12 || 5.43 || 7.42 <br />
|-<br />
| ell knee EE || 200 || 50 || 50 || 50 || 50 || 65 || 65 || 65 || 65<br />
|-<br />
| 1/f exponent EE || -2.0 || -2.0 || -2.0 || -2.0 || -2.0 || -3.0 || -3.0 || -3.0 || -3.0<br />
|-<br />
| white noise level BB (uK-arcmin) || 13.6 || 8.67 || 8.22 || 1.64 || 1.30 || 2.03 || 2.03 || 5.19 || 7.08<br />
|-<br />
| ell knee BB || 200 || 50 || 50 || 50 || 50 || 60 || 60 || 60 || 60<br />
|-<br />
| 1/f exponent BB || -2.0 || -2.0 || -2.0 || -2.0 || -2.0 || -3.0 || -3.0 || -3.0 || -3.0<br />
|-<br />
| ell min || 30 || 30 || 30 || 30 || 30 || 30 || 30 || 30 || 30 <br />
|-<br />
| nside || 512 || 512 || 512 || 512 || 512 || 512 || 512 || 512 || 512<br />
|}<br />
<br />
=== Experiment Definition 03, 03b, 03c ===<br />
These sims are nearly identical to experiment definition 02, 02b, 02c, and even use the same noise realizations. The one change is the inclusion of additive systematics, following the prescription described in this [[Additive_systematics_for_data_challenge_03|2017-07-10 posting]]. Blocks of realizations contain different versions of the additive systematic, as shown below. For all cases, the level of the systematic is chosen to yield bias on ''r'' of 1e-4 (by the analysis of the 2017-07-10 posting). The first block of realizations, 0000&ndash;0124, contains no systematic and should be completely identical to the 02/02b/02c realizations.<br />
<br />
{| class="wikitable"<br />
|-<br />
! realizations !! A<sub>uncorr</sub> !! B<sub>uncorr</sub> !! A<sub>corr</sub> !! B<sub>corr</sub> !! Description<br />
|-<br />
| 0000&ndash;0124 || 0 || 0 || 0 || 0 || No systematics<br />
|-<br />
| 0125&ndash;0249 || 0.0328 || 0 || 0 || 0 || Uncorrelated systematic with white spectrum<br />
|-<br />
| 0250&ndash;0374 || 0 || 0.0689 || 0 || 0 || Uncorrelated systematic with 1/ell spectrum<br />
|-<br />
| 0375&ndash;0499 || 0 || 0 || 0.0584 || 0 || Correlated systematic with white spectrum<br />
|-<br />
| 0500&ndash;0624 || 0 || 0 || 0 || 0.1049 || Correlated systematic with 1/ell spectrum<br />
|-<br />
| 0625&ndash;0749 || 0.0164 || 0.0345 || 0 || 0 || Uncorrelated systematic with white + 1/ell spectrum<br />
|-<br />
| 0750&ndash;0874 || 0 || 0 || 0.0292 || 0.0525 || Correlated systematic with white + 1/ell spectrum<br />
|-<br />
| 0875&ndash;0999 || 0.0082 || 0.0172 || 0.0146 || 0.0262 || Uncorrelated + correlated systematic with white + 1/ell spectrum<br />
|}<br />
<br />
Combined maps for analysis can be found on NERSC in '''/project/projectdirs/cmbs4/data_xx.yy/03''' etc.<br />
<br />
Parameters and ingredients for the combined maps can be found in '''/project/projectdirs/cmbs4/expt_xx/03''' etc. Note that noise, rhits, and wfunc are actually symlinks to those directories under experiment configs 02, 02b, 02c.<br />
<br />
=== Experiment Definition 02, 02b, 02c ===<br />
This is an update from 01 which differs in the following ways:<br />
<br />
1) Addition of 20GHz band and (slight) changes to the band/detector optimization as per<br />
[[http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170515_chkS4 Victor's May 15 posting in the logbook]].<br />
<br />
2) Addition of 3 delensing bands 95/155/220GHz with same number of detectors as the low res equivalent bands<br />
but beam size 4x higher. This adds up to approximately the same number of detectors but clearly one should reoptimize<br />
once they are not all at the same freq. Since we are still quite far from having real lensing reconstruction and realistic<br />
(non-Gaussian) high ell foregrounds this probably is OK for this round.<br />
<br />
3) Addition of tensors - even number realizations have r=0.003, odd number have r=0.<br />
<br />
4) Set 02 is the same nominal 3% sky patch as set 01. We now add 02b which is 1% round patch with center<br />
the same as the BICEP/Keck patch (RA=0, Dec=-57.5), and 02c which is 10% round patch centered on RA=15deg, Dec=-35.<br />
<br />
These products appear on NERSC under '''/project/projectdirs/cmbs4/expt_xx/02''' etc.<br />
<br />
=== Experiment Definition 01 ===<br />
This is intended to be basically the same as the assumptions made for the Fisher calculations done for the Science Book.<br />
The parameters come from [[http://users.physics.harvard.edu/~buza/20161220_chkS4 Victor's Dec 21 posting in the logbook]] with the addition of bandwidths from<br />
[[Tophat_bands_for_Data_Challenge|Colin's Nov 4 posting]] and are summarized in the following table:<br />
<br />
{| class="wikitable" style="text-align: right; margin-left: 51px;"<br />
! Frequency (GHz) !! 30 !! 40 !! 85 !! 95 !! 145 !! 155 !! 220 !! 270 !! 155 HR<br />
|-<br />
| Bandwidth (GHz) || 9.0 || 12.0 || 20.4 || 22.8 || 31.9 || 34.1 || 48.4 || 59.4 || 34.1<br />
|-<br />
| Beam FWHM (arcmin) || 76.6 || 57.5 || 27.0 || 24.2 || 15.9 || 14.8 || 10.7 || 8.5 || 4.0<br />
|-<br />
| white noise level TT (uK-arcmin) || 12.97 || 13.22 || 2.30 || 1.89 || 5.31 || 5.48 || 11.86 || 17.72 || 5.48<br />
|-<br />
| ell knee TT || 175 || 175 || 175 || 175 || 230 || 230 || 230 || 230 || 500<br />
|-<br />
| 1/f exponent TT || -4.1 || -4.1 || -4.1 || -4.1 || -3.8 || -3.8 || -3.8 || -3.8 || -3.8<br />
|-<br />
| white noise level EE (uK-arcmin) || 10.85 || 11.06 || 1.93 || 1.58 || 2.49 || 2.56 || 5.55 || 8.30 || 2.56 <br />
|-<br />
| ell knee EE || 50 || 50 || 50 || 50 || 65 || 65 || 65 || 65 || 200<br />
|-<br />
| 1/f exponent EE || -2.0 || -2.0 || -2.0 || -2.0 || -3.0 || -3.0 || -3.0 || -3.0 || -3.0<br />
|-<br />
| white noise level BB (uK-arcmin) || 10.59 || 10.79 || 1.88 || 1.54 || 2.38 || 2.45 || 5.30 || 7.93 || 2.45<br />
|-<br />
| ell knee BB || 50 || 50 || 50 || 50 || 60 || 60 || 60 || 60 || 200<br />
|-<br />
| 1/f exponent BB || -2.0 || -2.0 || -2.0 || -2.0 || -3.0 || -3.0 || -3.0 || -3.0 || -3.0<br />
|-<br />
| ell min || 30 || 30 || 30 || 30 || 30 || 30 || 30 || 30 || 100<br />
|-<br />
| nside || 512 || 512 || 512 || 512 || 512 || 512 || 512 || 512 || 2048<br />
|}<br />
<br />
These parameters are in the file '''expt_xx/01/params.dat''' and give rise to the window functions in '''expt_xx/01/wfunc''' and the noise spectra in '''expt_xx/01/noise/cls'''.<br />
The intent of the low ell cutoff is to approximate the effect of the timestream filtering which is commonly done in ground based experiments (and as some kind of acknowledgement that<br />
the largest angular scales may anyway be corrupted by systematic effects).<br />
<br />
Additionally '''expt_xx/01/rhits/fsky03bk_n0512.fits''' is supposed to represent the "relative hits" with which the sky has been observed.<br />
This is a circular pattern centred at RA=0, Dec=-45 (a bit below the BICEP/Keck patch) which is flat at one out to r=12deg and then rolls down to zero as cosine squared over an<br />
additional 15 deg.<br />
This is some kind of approximation as to what small apertures might deliver (given their large instantaneous field of view).<br />
<br />
From the noise spectra sets of alms are generated (with nlmax=4096) with names like '''expt_xx/01/noise/alm/noise_f155_b15_ellmin30_alm_mc_0000.fits''' where 155 is the frequency, 15 is the beam size (in arcmin), and 0000 is the realization number. <br />
<br />
From these full sky maps are rendered at nside=512 and nlmax=1024. No beam smoothing is applied as is appropriate for noise.<br />
The maps have names like '''expt_xx/01/noise/map/noise_f155_b15_ellmin30_map_0512_mc_0000.fits'''.<br />
<br />
The full sky noise is then divided by the square-root of the rhits mask and the result stored in files like '''data_xx.yy/01.YY/cmbs4_01_noise_f155_b15_ellmin30_map_0512_mc_0000.fits''' - these are the noise realizations that one would have access to in a real experiment - the noise blows up around the edge.<br />
<br />
These masked noise realizations are then added to the sky model (LCDM+dust+sync+) and stored in names like '''data_xx.yy/01.YY/cmbs4_01pYY_comb_f155_b15_ellmin30_map_0512_mc_0000.fits'''.<br />
As a crude simulation of delensing these combined maps are also provided with the lensing effect reduced to 30, 10 and 3% of reality by combining lensed and unlensed LCDM - look for files<br />
with names like '''data_xx.yy/01.YY/cmbs4_01pYY_comb_AL0p3_f155_b15_ellmin30_map_0512_mc_0000.fits'''.<br />
Maps with partial lensing are constructed by the following combination: partially_lensed_map = sqrt(A_L) * lensed_map + (1 - sqrt(A_L)) * unlensed_map.<br />
<br />
To analyze these maps one should use only the '''expt_xx/01/params.dat''' file and the maps under '''data_xx.yy/01.YY'''.<br />
A thousand realizations are present.<br />
We can see these maps [[01.00 sim input maps | in this posting]]<br />
<br />
The last column of the table above shows one additional tweak - a second 155GHz band with a higher 1/f knee and smaller beam size - this is supposed to<br />
represent the maps made by higher resolution telescopes running in concert with small apertures in a hybrid approach.<br />
These maps can in principle be used to reconstruct the lensing potential and delens explicitly - instead of cheating by using<br />
the AL0p3 files etc.<br />
At the moment the noise spectrum in these maps is provisional.<br />
Additionally we may wish to add additional frequency bands at higher resolution so foreground cleaning<br />
before delensing can be done.<br />
We can see these maps [[Adding higher res delensing "band" | in this posting]].<br />
<br />
(The filtered LLCDM realizations are also copied in '''data_xx.yy/01.YY''' as these are needed to build the bandpower covariance matrix in the multi-component cross spectrum approach used by the BK group.<br />
It seems reasonable that one would always have realizations of a known spectrum signal passed through an experimental simulation.)</div>Jchhttp://www.cmb-s4.org/wiki/index.php?title=Survey_Performance_Expectations&diff=7900Survey Performance Expectations2018-10-09T20:48:07Z<p>Jch: /* Large-area Experiment Definition 01 */</p>
<hr />
<div>This page summarizes the various experiment definitions.<br />
The data products referred to are located on the NERSC system under '''/project/projectdirs/cmbs4/expt_xx'''<br />
<br />
===Large-area Experiment Definition 01===<br />
The NTT should fill in here what they can, with input from large-area forecasters where needed. <br />
Ideally there would be separate specifications of instrument capabilities, and assumed sky coverage, rather than<br />
having these lumped together.<br />
<br />
The numbers below are based on the Noise Tiger Team product lat-noise-181002.py , run assuming the default settings and fsky=0.4. The EE and BB noise levels are sqrt(2) higher than the TT noise levels. The atmospheric treatment is described in the code.<br />
<br />
{| class="wikitable" style="text-align: right; margin-left: 51px;"<br />
! Frequency (GHz) !! 20 !! 27 !! 39 !! 93 !! 145 !! 225 !! 280<br />
|-<br />
| Bandwidth (GHz) || n/a || n/a || n/a || n/a || n/a || n/a || n/a || n/a<br />
|-<br />
| Beam FWHM (arcmin) || 10. || 7.4 || 5.1 || 2.2 || 1.4 || 1.0 || 0.9<br />
|-<br />
| white noise level TT (uK-arcmin) || 45.9 || 15.5 || 8.7 || 1.5 || 1.5 || 4.8|| 11.5<br />
|-<br />
|}<br />
<br />
===Small-area Experiment Definition 05===<br />
The NTT should fill in here what they can, with input from small-area forecasters (r forecasters) where needed. Ideally instrument capabilities are distinct from specification of survey coverage, so coverage can be iterated without changing the instrument. For LAT instrument capability, it would make sense to refer to the appropriate Large-area Experiment Definition rather than reproduce a description of the LATs here.<br />
<br />
=== Experiment Definition 04 ===<br />
This is very similar to 02 but with the noise levels tweaked down by sqrt(7/6) to try and get sigma(r)=1e-4 as per science requirement.<br />
(The noise map generator has also been tweaked such that the level quoted in the params.dat table will be reproduced exactly when the power spectra of the maps is taken with the provided mask - i.e. the actual noise level will slightly lower in the center of the mask.)<br />
A 20GHz band has been added which is assumed to be on a large aperture telescope (and hence has higher resolution and ell knee).<br />
Below is the contents of the params.dat file. The noise levels and resolutions are copied from the [https://www.nsf.gov/mps/ast/aaac/cmb_s4/report/CMBS4_final_report_NL.pdf CDT report] "Science Traceability Matrix".<br />
Specs for the high res bands exist but have not been added yet. <br />
<br />
{| class="wikitable" style="text-align: right; margin-left: 51px;"<br />
! Frequency (GHz) !! 20 !! 30 !! 40 !! 85 !! 95 !! 145 !! 155 !! 220 !! 270<br />
|-<br />
| Bandwidth (GHz) || 5.0 || 9.0 || 12.0 || 20.4 || 22.8 || 31.9 || 34.1 || 48.4 || 59.4<br />
|-<br />
| Beam FWHM (arcmin) || 11.0 || 76.6 || 57.5 || 27.0 || 24.2 || 15.9 || 14.8 || 10.7 || 8.5<br />
|-<br />
| white noise level TT (uK-arcmin) || 16.66 || 10.62 || 10.07 || 2.01 || 1.59 || 4.53 || 4.53 || 11.61 || 15.84<br />
|-<br />
| ell knee TT || 500 || 175 || 175 || 175 || 175 || 230 || 230 || 230 || 230<br />
|-<br />
| 1/f exponent TT || -4.1 || -4.1 || -4.1 || -4.1 || -4.1 || -3.8 || -3.8 || -3.8 || -3.8<br />
|-<br />
| white noise level EE (uK-arcmin) || 13.94 || 8.88 || 8.42 || 1.67 || 1.32 || 2.12 || 2.12 || 5.43 || 7.42 <br />
|-<br />
| ell knee EE || 200 || 50 || 50 || 50 || 50 || 65 || 65 || 65 || 65<br />
|-<br />
| 1/f exponent EE || -2.0 || -2.0 || -2.0 || -2.0 || -2.0 || -3.0 || -3.0 || -3.0 || -3.0<br />
|-<br />
| white noise level BB (uK-arcmin) || 13.6 || 8.67 || 8.22 || 1.64 || 1.30 || 2.03 || 2.03 || 5.19 || 7.08<br />
|-<br />
| ell knee BB || 200 || 50 || 50 || 50 || 50 || 60 || 60 || 60 || 60<br />
|-<br />
| 1/f exponent BB || -2.0 || -2.0 || -2.0 || -2.0 || -2.0 || -3.0 || -3.0 || -3.0 || -3.0<br />
|-<br />
| ell min || 30 || 30 || 30 || 30 || 30 || 30 || 30 || 30 || 30 <br />
|-<br />
| nside || 512 || 512 || 512 || 512 || 512 || 512 || 512 || 512 || 512<br />
|}<br />
<br />
=== Experiment Definition 03, 03b, 03c ===<br />
These sims are nearly identical to experiment definition 02, 02b, 02c, and even use the same noise realizations. The one change is the inclusion of additive systematics, following the prescription described in this [[Additive_systematics_for_data_challenge_03|2017-07-10 posting]]. Blocks of realizations contain different versions of the additive systematic, as shown below. For all cases, the level of the systematic is chosen to yield bias on ''r'' of 1e-4 (by the analysis of the 2017-07-10 posting). The first block of realizations, 0000&ndash;0124, contains no systematic and should be completely identical to the 02/02b/02c realizations.<br />
<br />
{| class="wikitable"<br />
|-<br />
! realizations !! A<sub>uncorr</sub> !! B<sub>uncorr</sub> !! A<sub>corr</sub> !! B<sub>corr</sub> !! Description<br />
|-<br />
| 0000&ndash;0124 || 0 || 0 || 0 || 0 || No systematics<br />
|-<br />
| 0125&ndash;0249 || 0.0328 || 0 || 0 || 0 || Uncorrelated systematic with white spectrum<br />
|-<br />
| 0250&ndash;0374 || 0 || 0.0689 || 0 || 0 || Uncorrelated systematic with 1/ell spectrum<br />
|-<br />
| 0375&ndash;0499 || 0 || 0 || 0.0584 || 0 || Correlated systematic with white spectrum<br />
|-<br />
| 0500&ndash;0624 || 0 || 0 || 0 || 0.1049 || Correlated systematic with 1/ell spectrum<br />
|-<br />
| 0625&ndash;0749 || 0.0164 || 0.0345 || 0 || 0 || Uncorrelated systematic with white + 1/ell spectrum<br />
|-<br />
| 0750&ndash;0874 || 0 || 0 || 0.0292 || 0.0525 || Correlated systematic with white + 1/ell spectrum<br />
|-<br />
| 0875&ndash;0999 || 0.0082 || 0.0172 || 0.0146 || 0.0262 || Uncorrelated + correlated systematic with white + 1/ell spectrum<br />
|}<br />
<br />
Combined maps for analysis can be found on NERSC in '''/project/projectdirs/cmbs4/data_xx.yy/03''' etc.<br />
<br />
Parameters and ingredients for the combined maps can be found in '''/project/projectdirs/cmbs4/expt_xx/03''' etc. Note that noise, rhits, and wfunc are actually symlinks to those directories under experiment configs 02, 02b, 02c.<br />
<br />
=== Experiment Definition 02, 02b, 02c ===<br />
This is an update from 01 which differs in the following ways:<br />
<br />
1) Addition of 20GHz band and (slight) changes to the band/detector optimization as per<br />
[[http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170515_chkS4 Victor's May 15 posting in the logbook]].<br />
<br />
2) Addition of 3 delensing bands 95/155/220GHz with same number of detectors as the low res equivalent bands<br />
but beam size 4x higher. This adds up to approximately the same number of detectors but clearly one should reoptimize<br />
once they are not all at the same freq. Since we are still quite far from having real lensing reconstruction and realistic<br />
(non-Gaussian) high ell foregrounds this probably is OK for this round.<br />
<br />
3) Addition of tensors - even number realizations have r=0.003, odd number have r=0.<br />
<br />
4) Set 02 is the same nominal 3% sky patch as set 01. We now add 02b which is 1% round patch with center<br />
the same as the BICEP/Keck patch (RA=0, Dec=-57.5), and 02c which is 10% round patch centered on RA=15deg, Dec=-35.<br />
<br />
These products appear on NERSC under '''/project/projectdirs/cmbs4/expt_xx/02''' etc.<br />
<br />
=== Experiment Definition 01 ===<br />
This is intended to be basically the same as the assumptions made for the Fisher calculations done for the Science Book.<br />
The parameters come from [[http://users.physics.harvard.edu/~buza/20161220_chkS4 Victor's Dec 21 posting in the logbook]] with the addition of bandwidths from<br />
[[Tophat_bands_for_Data_Challenge|Colin's Nov 4 posting]] and are summarized in the following table:<br />
<br />
{| class="wikitable" style="text-align: right; margin-left: 51px;"<br />
! Frequency (GHz) !! 30 !! 40 !! 85 !! 95 !! 145 !! 155 !! 220 !! 270 !! 155 HR<br />
|-<br />
| Bandwidth (GHz) || 9.0 || 12.0 || 20.4 || 22.8 || 31.9 || 34.1 || 48.4 || 59.4 || 34.1<br />
|-<br />
| Beam FWHM (arcmin) || 76.6 || 57.5 || 27.0 || 24.2 || 15.9 || 14.8 || 10.7 || 8.5 || 4.0<br />
|-<br />
| white noise level TT (uK-arcmin) || 12.97 || 13.22 || 2.30 || 1.89 || 5.31 || 5.48 || 11.86 || 17.72 || 5.48<br />
|-<br />
| ell knee TT || 175 || 175 || 175 || 175 || 230 || 230 || 230 || 230 || 500<br />
|-<br />
| 1/f exponent TT || -4.1 || -4.1 || -4.1 || -4.1 || -3.8 || -3.8 || -3.8 || -3.8 || -3.8<br />
|-<br />
| white noise level EE (uK-arcmin) || 10.85 || 11.06 || 1.93 || 1.58 || 2.49 || 2.56 || 5.55 || 8.30 || 2.56 <br />
|-<br />
| ell knee EE || 50 || 50 || 50 || 50 || 65 || 65 || 65 || 65 || 200<br />
|-<br />
| 1/f exponent EE || -2.0 || -2.0 || -2.0 || -2.0 || -3.0 || -3.0 || -3.0 || -3.0 || -3.0<br />
|-<br />
| white noise level BB (uK-arcmin) || 10.59 || 10.79 || 1.88 || 1.54 || 2.38 || 2.45 || 5.30 || 7.93 || 2.45<br />
|-<br />
| ell knee BB || 50 || 50 || 50 || 50 || 60 || 60 || 60 || 60 || 200<br />
|-<br />
| 1/f exponent BB || -2.0 || -2.0 || -2.0 || -2.0 || -3.0 || -3.0 || -3.0 || -3.0 || -3.0<br />
|-<br />
| ell min || 30 || 30 || 30 || 30 || 30 || 30 || 30 || 30 || 100<br />
|-<br />
| nside || 512 || 512 || 512 || 512 || 512 || 512 || 512 || 512 || 2048<br />
|}<br />
<br />
These parameters are in the file '''expt_xx/01/params.dat''' and give rise to the window functions in '''expt_xx/01/wfunc''' and the noise spectra in '''expt_xx/01/noise/cls'''.<br />
The intent of the low ell cutoff is to approximate the effect of the timestream filtering which is commonly done in ground based experiments (and as some kind of acknowledgement that<br />
the largest angular scales may anyway be corrupted by systematic effects).<br />
<br />
Additionally '''expt_xx/01/rhits/fsky03bk_n0512.fits''' is supposed to represent the "relative hits" with which the sky has been observed.<br />
This is a circular pattern centred at RA=0, Dec=-45 (a bit below the BICEP/Keck patch) which is flat at one out to r=12deg and then rolls down to zero as cosine squared over an<br />
additional 15 deg.<br />
This is some kind of approximation as to what small apertures might deliver (given their large instantaneous field of view).<br />
<br />
From the noise spectra sets of alms are generated (with nlmax=4096) with names like '''expt_xx/01/noise/alm/noise_f155_b15_ellmin30_alm_mc_0000.fits''' where 155 is the frequency, 15 is the beam size (in arcmin), and 0000 is the realization number. <br />
<br />
From these full sky maps are rendered at nside=512 and nlmax=1024. No beam smoothing is applied as is appropriate for noise.<br />
The maps have names like '''expt_xx/01/noise/map/noise_f155_b15_ellmin30_map_0512_mc_0000.fits'''.<br />
<br />
The full sky noise is then divided by the square-root of the rhits mask and the result stored in files like '''data_xx.yy/01.YY/cmbs4_01_noise_f155_b15_ellmin30_map_0512_mc_0000.fits''' - these are the noise realizations that one would have access to in a real experiment - the noise blows up around the edge.<br />
<br />
These masked noise realizations are then added to the sky model (LCDM+dust+sync+) and stored in names like '''data_xx.yy/01.YY/cmbs4_01pYY_comb_f155_b15_ellmin30_map_0512_mc_0000.fits'''.<br />
As a crude simulation of delensing these combined maps are also provided with the lensing effect reduced to 30, 10 and 3% of reality by combining lensed and unlensed LCDM - look for files<br />
with names like '''data_xx.yy/01.YY/cmbs4_01pYY_comb_AL0p3_f155_b15_ellmin30_map_0512_mc_0000.fits'''.<br />
Maps with partial lensing are constructed by the following combination: partially_lensed_map = sqrt(A_L) * lensed_map + (1 - sqrt(A_L)) * unlensed_map.<br />
<br />
To analyze these maps one should use only the '''expt_xx/01/params.dat''' file and the maps under '''data_xx.yy/01.YY'''.<br />
A thousand realizations are present.<br />
We can see these maps [[01.00 sim input maps | in this posting]]<br />
<br />
The last column of the table above shows one additional tweak - a second 155GHz band with a higher 1/f knee and smaller beam size - this is supposed to<br />
represent the maps made by higher resolution telescopes running in concert with small apertures in a hybrid approach.<br />
These maps can in principle be used to reconstruct the lensing potential and delens explicitly - instead of cheating by using<br />
the AL0p3 files etc.<br />
At the moment the noise spectrum in these maps is provisional.<br />
Additionally we may wish to add additional frequency bands at higher resolution so foreground cleaning<br />
before delensing can be done.<br />
We can see these maps [[Adding higher res delensing "band" | in this posting]].<br />
<br />
(The filtered LLCDM realizations are also copied in '''data_xx.yy/01.YY''' as these are needed to build the bandpower covariance matrix in the multi-component cross spectrum approach used by the BK group.<br />
It seems reasonable that one would always have realizations of a known spectrum signal passed through an experimental simulation.)</div>Jchhttp://www.cmb-s4.org/wiki/index.php?title=File:JCH_SO.pdf&diff=7591File:JCH SO.pdf2018-09-08T12:19:37Z<p>Jch: </p>
<hr />
<div></div>Jchhttp://www.cmb-s4.org/wiki/index.php?title=Princeton-2018:_Cosmology_with_CMB-S4&diff=7590Princeton-2018: Cosmology with CMB-S42018-09-08T12:19:18Z<p>Jch: </p>
<hr />
<div>== Workshop overview ==<br />
<br />
<br />
<br />
'''Workshop Photo:<br />
''' <br /><br />
[[File:CMB-S4_2018-1-photo.jpg|600px]]<br />
<br/><br />
<br />
The Princeton 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 />
The workshop is supported by Princeton University with a generous contribution from the Kavli Institute for Cosmological Physics.<br />
<br />
This meeting will focus on moving us towards the Decadal Survey and project formation. Each day will have a different flavor:<br />
* Thursday - Collaboration, Project and Decadal Survey Report updates and discussion<br />
* Friday - Broader community building ahead of the Decadal Process<br />
* Saturday - Parallel Science & Technical Council sessions<br />
<br />
== Meeting Info & Registration ==<br />
<br />
[http://phyindico.princeton.edu/indico/event/12/page/0 Official Workshop Website: Registration, Participants, Hotels, Logistics].<br />
<br />
[[File:workshop-map-venue.png]] <br /><br />
Registration begins outside McDonnell A02 at 8 am on Thursday, 6 Sept 2018. <br />
Parking is in lot 21 (see map). <br />
<br />
'''Remote Connection Information:'''<br />
<br />
https://bluejeans.com/ <br /><br />
Meeting ID: 211 655 218<br /><br />
*1.888.240.2560 (US Toll Free)<br />
*1.408.317.9253 (US (Primary, San Jose)) <br />
*1.408.740.7256 (US (San Jose)) <br /><br />
*Global Numbers: https://www.bluejeans.com/numbers<br />
<br />
Slack channel #princeton2018 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 />
== Agenda ==<br />
<br />
<br />
=== Thursday September 6th ===<br />
<br />
'''08:00''' ''Breakfast'' <br />
<br />
'''08:30''' Welcome & Logistics (Suzanne Staggs Herman Verlinde, chair of the Physics Department) [[File:Logistics-pton-20180906.pdf]]<br />
<br />
''' Status & Context'''<br /><br />
'''08:45''' Introduction & Collaboration Update (Julian Borrill) [[File:Cmbs4_collaboration.pdf]]<br /> <br />
'''09:05''' DSR Update (John Carlstrom) [[File:DSR-Carlstrom.pdf]]<br /><br />
'''09:25''' Project Update (Jim Yeck) [[File:S4 Princeton Workshop Yeck.pdf]]<br /><br />
'''09:45''' Q&A<br />
<br />
'''DSR - Science Council''' <br /><br />
'''10:00''' Introduction (Lloyd Knox) [[File:DSR_ScienceCouncil_Princeton2018.pdf]]<br /> <br />
'''10:15''' Gravitational Waves & Inflation (Raphael Flauger) [[File: GWPrinceton.pdf]]<br /><br />
<br />
'''10:30''' ''Coffee Break''<br />
<br />
'''11:00''' Light Relics (Daniel Green & Joel Meyers) [[File:LightRelics_Meyers_Princeton_S4.pdf]] <br /><br />
'''11:15''' Neutrino Mass (Marilena Loverde & Blake Sherwin) [[File:S4WGNeutrinoMassReport.pdf]]<br /><br />
'''11:30''' Dark Energy & Dark Matter (Vera Gluscevic & Nick Battaglia) [[File:DMDE CMBS4 Princeton2018.pdf]]<br /><br />
'''11:45''' Galaxy Formation & Evolution (Marcelo Alvarez & Colin Hill) [[File:CMB-S4 Galaxy Formation and Evolution (Princeton).pdf]] <br /><br />
'''12:00''' Legacy Catalogs (Lindsey Bleem) [[https://cmb-s4.org/wiki/images/Legacy_catalog_update_princeton_9_6_18.pdf here]]<br /><br />
'''12:15''' Q&A<br />
<br />
'''12:30''' ''Lunch & JSAC Event''<br />
<br />
'''DSR - Technical Council'''<br /><br />
'''13:30''' Introduction (McMahon/Vieregg) [[File:TechCouncilPrinceton2018.pdf]] <br /><br />
'''13:45''' Sites & Infrastructure (Kam Arnold, Brad Benson) [https://drive.google.com/file/d/1XB3Kt80dbh9qoyvvnppN6RYispp_XFrB/view?usp=sharing Site Presentation PDF]<br /><br />
'''14:00''' Large Telescopes (Mike Niemack, Steve Padin) [[File:LargeTelescopesLargeCryostatsStatusPrincetonV2.pdf]] <br /><br />
'''14:15''' Small Telescopes (John Kovac, Chao-Lin Kuo, Aikito Kusaka) [[File:SmallTelescopes_Princeton_Thursday_slides.pdf]]<br /><br />
'''14:30''' Detectors & Readout (Clarence Chang, Kent Irwin, Adrian Lee) [[File:DetectorsReadout.pdf]]<br /><br />
'''14:45''' Data Acquisition & Control (Laura Newburgh, Nathan Whitehorn) [[File:S4_DAQ.pdf]] <br /><br />
'''15:00''' Data Management (Matthew Hasselfield) [[File:Data_management_20180906_v1.pdf]] <br /><br />
'''15:15''' Integration & Commissioning (Kam Arnold, Bradford Benson) [[File:IntegrationCommissioningPrinceton2018.pdf]] <br /><br />
'''15:30''' Options (Steve Padin) [[File:OptionsPrincetonV1.pdf]] <br /><br />
'''15:45''' Q&A<br />
<br />
'''16:00''' Fireslides 1 [[File:FireSlides_Thursday_post.pdf]]<br />
<br />
'''16:30''' Poster Session, Cocktails & Light Dinner<br />
<br />
------<br />
<br />
=== Friday September 7th ===<br />
<br />
'''08:00''' ''Breakfast''<br />
<br />
'''The CMB Circa September 2018'''<br />
<br />
'''08:30''' Harmonic Overtones (Marc Kamionkowski) [[File:Morningmarc.pdf]] <br /><br />
'''08:55''' On-sky performance of the CLASS Q-band telescope (John Appel) [[File:CLASS_S4_20180907_final.pdf]]<br /><br />
'''09:05''' SPIDER: an update, with foregrounds. Lots of them. [[File:Cmbs4_aug2018.red.mini.pdf]] (Bill Jones) <br /><br />
'''09:15''' Current state of the BICEP/Keck instrument, data and analysis (Clem Pryke) [[File:BK2018.pdf]] <br /><br />
'''09:25''' Planck 2018 and setting the stage for Stage-4 (Marius Millea) [[File:Planck2018.pdf]] <br /><br />
'''09:35''' Ground, Balloon, Space Complementarity (Shaul Hanany) [[File:PrincetonS4_2018V2.pdf]] <br /><br />
'''09:50''' BK-SPT3G forward plans (John Kovac) [[File:BK-SPT3G_forward.pdf]] <br /><br />
'''10:05''' Simons Observatory forward plans (Jo Dunkley) [[File:SO_plans.pdf]] <br /><br />
'''10:20''' The Big Step Up to CMB-S4 (Gil Holder) [[File:S4_Princeton_holder.pdf]] <br />
<br />
'''10:35''' ''Coffee Break''<br />
<br />
'''Adjacent Science & Emerging Ideas'''<br />
<br />
'''11:15''' Millimeter/Submillimeter Large Telescopes and Instruments (Phil Mauskopf) [[File:mauskopf_princeton_cmbs4.pdf]] <br /><br />
'''11:30''' Intensity mapping meets the CMB: Complementary Cosmology across the radio spectrum (Laura Newburgh) [[File:2018_09_S4_IntensityMappingCMB.pdf]] <br /><br />
'''11:45''' SPHERE-X (Jamie Bock) [[File:Spherex_cmbs4_2018.pdf]] <br /><br />
'''12:00''' Weak Lensing (Elisabeth Krause) [[https://cmb-s4.org/wiki/images/Krause_LSSTxS4_2018.pdf slides_here]]<br />
<br />
'''12:15''' '' Group Photo & Lunch''<br />
<br />
'''13:15''' Reionization Studies in the CMB-S4 Era (Adam Lidz) [[File:cmbs4_sep7_18_lidz.pdf]] <br /><br />
'''13:30''' A biased view of open questions in galaxy formation (Norm Murray) [[File:CMB-S4_Murray.pdf]]<br /><br />
'''13:45''' Polarized dust foreground models from HI data (Susan Clark) [[File:Clark_S4_ForegroundModels.pdf]] <br /><br />
'''14:00''' Properties of the magnetized dusty interstellar medium with Planck [[File:Aumont_Princeton_CMB-S4_090718.pdf]] (Jonathan Aumont)<br />
<br />
'''Talks From Collaboration Members'''<br />
<br />
'''14:15''' Inflationary vs. Reionization Features from Current and Future Data (Cora Dvorkin) [[File:DvorkinCMBS4.pdf]]<br /><br />
'''14:25''' Stress-testing nonstandard neutrino physics with CMB-S4 (Francis-Yan Cyr-Racine) [[File:CMB-S4_princeton18_cyr-racine.pdf]]<br /><br />
'''14:35''' Searching for Dark Matter Interactions in the CMB (Kimberly Boddy) [[File:Boddy.pdf]] <br /><br />
'''14:45''' Foreground immune CMB lensing with shear-only reconstruction (Emmanuel Schaan) [[https://cmb-s4.org/wiki/images/Cmb_shear_schaan.pdf slides]]<br /><br />
'''14:55''' Cosmology from cross correlating S4 lensing with photometric galaxy counts (Blake Sherwin) [[File:NeutrinoXCorrs.pdf]] <br /><br />
'''15:05''' Higher order corrections to CMB lensing cross correlations (Vanessa Boehm) [[https://cmb-s4.org/wiki/images/HighOrderCorr.pdf slides]]<br /><br />
'''15:15''' CMB lensing on small scales (Simone Ferraro) [[File:Ferraro_s4_princeton.pdf]] <br /><br />
'''15:25''' kSZ cosmology without the cluster optical depth degeneracy (Mathew Madhavacheril) [[File:Madhavacheril_S4kSZ_v1.pdf]] <br /><br />
'''15:35''' Q&A<br />
<br />
'''15:50''' ''Coffee Break''<br />
<br />
'''16:05''' Fireslides 2 [[File:FireSlides_Friday_post.pdf]]<br />
<br />
'''16:30''' Wrap-Up Panel - Roger Blandford, Chris Carilli, Bonnie Fleming, George Fuller, Risa Wechsler, (Matias Zaldarriaga was called away)<br /><br />
<br />
Contributed material for panel discussion by panelists and audience:<br /><br />
*(Charge) [[File:Panel-slide.pdf]]<br />
*From George Fuller: [[File:Fuller-CMB-S4.Princeton.pdf]]<br /><br />
*From Roger Blandford:[[File:Cmbs4rdb.pdf]]<br /><br />
*From Chris Carilli: [[File:Carilli-CMBS4.pdf]]<br/><br />
<br />
'''17:45''' Next Steps & Action Items<br />
<br />
'''Parallel Afternoon Session for Project Team'''<br />
<br />
'''15:00''' Charge for Decadal Survey Report Review on 12/11-13 in DC <br /><br />
'''15:30''' Possible DSR Review Committee and Planning Details <br /><br />
'''16:00''' Review of Overall Timeline and Boundary Conditions <br /><br />
'''16:30''' Critical Issues Identified in Project Planning <br /><br />
'''17:00''' Preparations/Guidance for Saturday Sessions <br /><br />
<br />
------<br />
<br />
=== Saturday September 8th ===<br />
<br />
'''PLEASE REMEMBER TO COMPLETE THE MEMBERSHIP SURVEY [[https://goo.gl/forms/GjFla4oPdLnVjugp2 HERE]]'''<br />
<br />
'''08:30''' ''Breakfast''<br />
<br />
'''09:00''' Parallel Sessions<br />
* Science Council:<br />
** 09:00 Noise & Forecasting (70 min)<br />
*** 09:00 r Forecasting Update (Clem Pryke)<br />
*** 09:10 small-area survey report from Noise Tiger Team (NTT) (Colin Bischoff)<br />
*** 09:20 Discussion<br />
*** 09:40 Report from NTT on large-area survey forecasting (Matthew Hasselfield)<br />
*** 09:50 Simons Observatory approach to TT, TE, EE, phi phi, tSZ, kSZ forecasting (Colin Hill) [[File:JCH_SO.pdf]]<br />
*** 10:00 Discussion<br />
** 10:10 White Paper Organization (50 min)<br />
** 11:00 Coffee Break<br />
** 11:30 Science Council AWG Breakout Sessions<br />
<br />
* Technical Council:<br />
** 09:00 Project Planning<br />
** 11:00 Coffee Break<br />
** 11:30 Project Planning (continued)<br />
<br />
'''13:00''' ''Lunch (on your own)''<br />
<br />
'''14:00 onwards''' Rooms available for breakout sessions as required</div>Jchhttp://www.cmb-s4.org/wiki/index.php?title=File:Clark_S4_ForegroundModels.pdf&diff=7523File:Clark S4 ForegroundModels.pdf2018-09-07T14:01:22Z<p>Jch: </p>
<hr />
<div></div>Jchhttp://www.cmb-s4.org/wiki/index.php?title=Princeton-2018:_Cosmology_with_CMB-S4&diff=7522Princeton-2018: Cosmology with CMB-S42018-09-07T14:00:41Z<p>Jch: </p>
<hr />
<div>== Workshop overview ==<br />
<br />
The Princeton 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 />
The workshop is supported by Princeton University with a generous contribution from the Kavli Institute for Cosmological Physics.<br />
<br />
This meeting will focus on moving us towards the Decadal Survey and project formation. Each day will have a different flavor:<br />
* Thursday - Collaboration, Project and Decadal Survey Report updates and discussion<br />
* Friday - Broader community building ahead of the Decadal Process<br />
* Saturday - Parallel Science & Technical Council sessions<br />
<br />
== Meeting Info & Registration ==<br />
<br />
[http://phyindico.princeton.edu/indico/event/12/page/0 Official Workshop Website: Registration, Participants, Hotels, Logistics].<br />
<br />
[[File:workshop-map-venue.png]] <br /><br />
Registration begins outside McDonnell A02 at 8 am on Thursday, 6 Sept 2018. <br />
Parking is in lot 21 (see map). <br />
<br />
'''Remote Connection Information:'''<br />
<br />
https://bluejeans.com/ <br /><br />
Meeting ID: 211 655 218<br /><br />
*1.888.240.2560 (US Toll Free)<br />
*1.408.317.9253 (US (Primary, San Jose)) <br />
*1.408.740.7256 (US (San Jose)) <br /><br />
*Global Numbers: https://www.bluejeans.com/numbers<br />
<br />
Slack channel #princeton2018 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 />
== Agenda ==<br />
<br />
<br />
=== Thursday September 6th ===<br />
<br />
'''08:00''' ''Breakfast'' <br />
<br />
'''08:30''' Welcome & Logistics (Suzanne Staggs Herman Verlinde, chair of the Physics Department) [[File:Logistics-pton-20180906.pdf]]<br />
<br />
''' Status & Context'''<br /><br />
'''08:45''' Introduction & Collaboration Update (Julian Borrill) [[File:Cmbs4_collaboration.pdf]]<br /> <br />
'''09:05''' DSR Update (John Carlstrom) [[File:DSR-Carlstrom.pdf]]<br /><br />
'''09:25''' Project Update (Jim Yeck) [[File:S4 Princeton Workshop Yeck.pdf]]<br /><br />
'''09:45''' Q&A<br />
<br />
'''DSR - Science Council''' <br /><br />
'''10:00''' Introduction (Lloyd Knox) [[File:DSR_ScienceCouncil_Princeton2018.pdf]]<br /> <br />
'''10:15''' Gravitational Waves & Inflation (Raphael Flauger) [[File: GWPrinceton.pdf]]<br /><br />
<br />
'''10:30''' ''Coffee Break''<br />
<br />
'''11:00''' Light Relics (Daniel Green & Joel Meyers) [[File:LightRelics_Meyers_Princeton_S4.pdf]] <br /><br />
'''11:15''' Neutrino Mass (Marilena Loverde & Blake Sherwin) [[File:S4WGNeutrinoMassReport.pdf]]<br /><br />
'''11:30''' Dark Energy & Dark Matter (Vera Gluscevic & Nick Battaglia) [[File:DMDE CMBS4 Princeton2018.pdf]]<br /><br />
'''11:45''' Galaxy Formation & Evolution (Marcelo Alvarez & Colin Hill) [[File:CMB-S4 Galaxy Formation and Evolution (Princeton).pdf]] <br /><br />
'''12:00''' Legacy Catalogs (Lindsey Bleem) [[https://cmb-s4.org/wiki/images/Legacy_catalog_update_princeton_9_6_18.pdf here]]<br /><br />
'''12:15''' Q&A<br />
<br />
'''12:30''' ''Lunch & JSAC Event''<br />
<br />
'''DSR - Technical Council'''<br /><br />
'''13:30''' Introduction (McMahon/Vieregg) [[File:TechCouncilPrinceton2018.pdf]] <br /><br />
'''13:45''' Sites & Infrastructure (Kam Arnold, Brad Benson) [https://drive.google.com/file/d/1XB3Kt80dbh9qoyvvnppN6RYispp_XFrB/view?usp=sharing Site Presentation PDF]<br /><br />
'''14:00''' Large Telescopes (Mike Niemack, Steve Padin) [[File:LargeTelescopesLargeCryostatsStatusPrincetonV2.pdf]] <br /><br />
'''14:15''' Small Telescopes (John Kovac, Chao-Lin Kuo, Aikito Kusaka) [[File:SmallTelescopes_Princeton_Thursday_slides.pdf]]<br /><br />
'''14:30''' Detectors & Readout (Clarence Chang, Kent Irwin, Adrian Lee) [[File:DetectorsReadout.pdf]]<br /><br />
'''14:45''' Data Acquisition & Control (Laura Newburgh, Nathan Whitehorn) [[File:S4_DAQ.pdf]] <br /><br />
'''15:00''' Data Management (Matthew Hasselfield) [[File:Data_management_20180906_v1.pdf]] <br /><br />
'''15:15''' Integration & Commissioning (Kam Arnold, Bradford Benson) [[File:IntegrationCommissioningPrinceton2018.pdf]] <br /><br />
'''15:30''' Options (Steve Padin) [[File:OptionsPrincetonV1.pdf]] <br /><br />
'''15:45''' Q&A<br />
<br />
'''16:00''' Fireslides 1 [[File:FireSlides_Thursday_post.pdf]]<br />
<br />
'''16:30''' Poster Session, Cocktails & Light Dinner<br />
<br />
------<br />
<br />
=== Friday September 7th ===<br />
<br />
'''08:00''' ''Breakfast''<br />
<br />
'''The CMB Circa September 2018'''<br />
<br />
'''08:30''' Harmonic Overtones (Marc Kamionkowski) [[File:Morningmarc.pdf]] <br /><br />
'''08:55''' On-sky performance of the CLASS Q-band telescope (John Appel) [[File:CLASS_S4_20180907_final.pdf]]<br /><br />
'''09:05''' SPIDER: an update, with foregrounds. Lots of them. (Bill Jones) <br /><br />
'''09:15''' Current state of the BICEP/Keck instrument, data and analysis (Clem Pryke) [[File:BK2018.pdf]] <br /><br />
'''09:25''' Planck 2018 and setting the stage for Stage-4 (Marius Millea) [[File:Planck2018.pdf]] <br /><br />
'''09:35''' Ground, Balloon, Space Complementarity (Shaul Hanany) [[File:PrincetonS4_2018V2.pdf]] <br /><br />
'''09:50''' BK-SPT3G forward plans (John Kovac) [[File:BK-SPT3G_forward.pdf]] <br /><br />
'''10:05''' Simons Observatory forward plans (Jo Dunkley) [[File:SO_plans.pdf]] <br /><br />
'''10:20''' The Big Step Up to CMB-S4 (Gil Holder) [[File:S4_Princeton_holder.pdf]] <br />
<br />
'''10:35''' ''Coffee Break''<br />
<br />
'''Adjacent Science & Emerging Ideas'''<br />
<br />
'''11:15''' Millimeter/Submillimeter Large Telescopes and Instruments (Phil Mauskopf) [[File:Mauskopf_princeton_cmbs4.pdf]]<br /><br />
'''11:30''' Intensity mapping meets the CMB: Complementary Cosmology across the radio spectrum (Laura Newburgh) [[File:2018_09_S4_IntensityMappingCMB.pdf]] <br /><br />
'''11:45''' SPHERE-X (Jamie Bock) [[File:Spherex_cmbs4_2018.pdf]] <br /><br />
'''12:00''' Weak Lensing (Elisabeth Krause) [[https://cmb-s4.org/wiki/images/Krause_LSSTxS4_2018.pdf slides_here]]<br />
<br />
'''12:15''' '' Group Photo & Lunch''<br />
<br />
'''13:15''' Reionization Studies in the CMB-S4 Era (Adam Lidz) <br /><br />
'''13:30''' A biased view of open questions in galaxy formation (Norm Murray) <br /><br />
'''13:45''' Polarized dust foreground models from HI data (Susan Clark) [[File:Clark_S4_ForegroundModels.pdf]] <br /><br />
'''14:00''' Properties of the magnetized dusty interstellar medium with Planck (Jonathan Aumont)<br />
<br />
'''Talks From Collaboration Members'''<br />
<br />
'''14:15''' Inflationary vs. Reionization Features from Current and Future Data (Cora Dvorkin) <br /><br />
'''14:25''' Stress-testing nonstandard neutrino physics with CMB-S4 (Francis-Yan Cyr-Racine) <br /><br />
'''14:35''' Searching for Dark Matter Interactions in the CMB (Kimberly Boddy) <br /><br />
'''14:45''' Foreground immune CMB lensing with shear-only reconstruction (Emmanuel Schaan) <br /><br />
'''14:55''' Cosmology from cross correlating S4 lensing with photometric galaxy counts (Blake Sherwin) [[File:NeutrinoXCorrs.pdf]] <br /><br />
'''15:05''' Higher order corrections to CMB lensing cross correlations (Vanessa Boehm) <br /><br />
'''15:15''' CMB lensing on small scales (Simone Ferraro) <br /><br />
'''15:25''' kSZ cosmology without the optical depth degeneracy (Mathew Madhavacheril) <br /><br />
'''15:35''' Q&A<br />
<br />
'''15:50''' ''Coffee Break''<br />
<br />
'''16:05''' Fireslides 2<br />
<br />
'''16:30''' Wrap-Up Panel - Roger Blandford, Chris Carilli, Bonnie Fleming, George Fuller, Risa Wechsler, Matias Zaldarriaga<br /><br />
Contributed material for panel discussion by panelists and audience:<br /><br />
*From George Fuller: [[File:Fuller-CMB-S4-Princeton.pdf]]<br /><br />
<br />
'''17:45''' Next Steps & Action Items<br />
<br />
'''Parallel Afternoon Session for Project Team'''<br />
<br />
'''15:00''' Charge for Decadal Survey Report Review on 12/11-13 in DC <br /><br />
'''15:30''' Possible DSR Review Committee and Planning Details <br /><br />
'''16:00''' Review of Overall Timeline and Boundary Conditions <br /><br />
'''16:30''' Critical Issues Identified in Project Planning <br /><br />
'''17:00''' Preparations/Guidance for Saturday Sessions <br /><br />
<br />
------<br />
<br />
=== Saturday September 8th ===<br />
<br />
'''08:30''' ''Breakfast''<br />
<br />
'''09:00''' Parallel Sessions<br />
* Science Council:<br />
** Noise & Forecasting (60 min)<br />
** White Paper Organization (45 min)<br />
* Technical Council:<br />
** Project Planning<br />
<br />
'''10:45''' ''Coffee Break''<br />
<br />
'''11:15''' Parallel Sessions<br />
*Science Council<br />
** AWG Working Meetings<br />
* Technical Council<br />
** Project Planning (continued)<br />
<br />
'''12:45''' ''Lunch (on your own)''<br />
<br />
'''13:45 onwards''' Rooms available for breakout sessions as required</div>Jchhttp://www.cmb-s4.org/wiki/index.php?title=Princeton-2018:_Cosmology_with_CMB-S4&diff=7439Princeton-2018: Cosmology with CMB-S42018-09-06T13:58:29Z<p>Jch: </p>
<hr />
<div>== Workshop overview ==<br />
<br />
The Princeton 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 />
The workshop is supported by Princeton University with a generous contribution from the Kavli Institute for Cosmological Physics.<br />
<br />
This meeting will focus on moving us towards the Decadal Survey and project formation. Each day will have a different flavor:<br />
* Thursday - Collaboration, Project and Decadal Survey Report updates and discussion<br />
* Friday - Broader community building ahead of the Decadal Process<br />
* Saturday - Parallel Science & Technical Council sessions<br />
<br />
== Meeting Info & Registration ==<br />
<br />
[http://phyindico.princeton.edu/indico/event/12/page/0 Official Workshop Website: Registration, Participants, Hotels, Logistics].<br />
<br />
[[File:workshop-map-venue.png]] <br /><br />
Registration begins outside McDonnell A02 at 8 am on Thursday, 6 Sept 2018. <br />
Parking is in lot 21 (see map). <br />
<br />
'''Remote Connection Information:'''<br />
<br />
https://bluejeans.com/ <br /><br />
Meeting ID: 350 694 048 <br /><br />
*1.888.240.2560 (US Toll Free)<br />
*1.408.317.9253 (US (Primary, San Jose)) <br />
*1.408.740.7256 (US (San Jose)) <br /><br />
*Global Numbers: https://www.bluejeans.com/numbers<br />
<br />
Slack channel #princeton2018 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 />
== Agenda ==<br />
<br />
<br />
=== Thursday September 6th ===<br />
<br />
'''08:00''' ''Breakfast'' <br />
<br />
'''08:30''' Welcome & Logistics (Suzanne Staggs Herman Verlinde, chair of the Physics Department) [[File:Logistics-pton-20180906.pdf]]<br />
<br />
''' Status & Context'''<br /><br />
'''08:45''' Introduction & Collaboration Update (Julian Borrill) [[File:Cmbs4_collaboration.pdf]]<br /> <br />
'''09:05''' DSR Update (John Carlstrom) [[File:DSR-Carlstrom.pdf]]<br /><br />
'''09:25''' Project Update (Jim Yeck) [[File:S4 Princeton Workshop Yeck.pdf]]<br /><br />
'''09:45''' Q&A<br />
<br />
'''DSR - Science Council''' <br /><br />
'''10:00''' Introduction (Lloyd Knox) [[File:DSR_ScienceCouncil_Princeton2018.pdf]]<br /> <br />
'''10:15''' Gravitational Waves & Inflation (Raphael Flauger) [[File: GWPrinceton.pdf]]<br /><br />
<br />
'''10:30''' ''Coffee Break''<br />
<br />
'''11:00''' Light Relics (Daniel Green & Joel Meyers) [[File:LightRelics_Meyers_Princeton_S4.pdf]] <br /><br />
'''11:15''' Neutrino Mass (Marilena Loverde & Blake Sherwin) [[File:S4WGNeutrinoMassReport.pdf]]<br /><br />
'''11:30''' Dark Energy & Dark Matter (Vera Gluscevic & Nick Battaglia) [[File:DMDE CMBS4 Princeton2018.pdf]]<br /><br />
'''11:45''' Galaxy Formation & Evolution (Marcelo Alvarez & Colin Hill) [[File:CMB-S4 Galaxy Formation and Evolution (Princeton).pdf]] <br /><br />
'''12:00''' Legacy Catalogs (Lindsey Bleem) [[https://cmb-s4.org/wiki/images/Legacy_catalog_update_princeton_9_6_18.pdf here]]<br /><br />
'''12:15''' Q&A<br />
<br />
'''12:30''' ''Lunch & JSAC Event''<br />
<br />
'''DSR - Technical Council'''<br /><br />
'''13:30''' Introduction (McMahon/Vieregg) [[File:TechCouncilPrinceton2018.pdf]] <br /><br />
'''13:45''' Sites & Infrastructure (Kam Arnold, Brad Benson) <br /><br />
'''14:00''' Large Telescopes (Mike Niemack, Steve Padin) [[File:LargeTelescopesLargeCryostatsStatusPrincetonV2.pdf]] <br /><br />
'''14:15''' Small Telescopes (John Kovac, Chao-Lin Kuo, Aikito Kusaka) <br /><br />
'''14:30''' Detectors & Readout (Clarence Chang, Kent Irwin, Adrian Lee) [[File:DetectorsReadout.pdf]]<br /><br />
'''14:45''' Data Acquisition & Control (Laura Newburgh, Nathan Whitehorn) <br /><br />
'''15:00''' Data Management (Matthew Hasselfield) <br /><br />
'''15:15''' Integration & Commissioning (Kam Arnold, Brad Benson) <br /><br />
'''15:30''' Options (Steve Padin) [[File:OptionsPrincetonV1.pdf]] <br /><br />
'''15:45''' Q&A<br />
<br />
'''16:00''' Fireslides 1<br />
<br />
'''16:30''' Poster Session, Cocktails & Light Dinner<br />
<br />
------<br />
<br />
=== Friday September 7th ===<br />
<br />
'''08:00''' ''Breakfast''<br />
<br />
'''The CMB Circa September 2018'''<br />
<br />
'''08:30''' Harmonic Overtones (Marc Kamionkowski) <br /><br />
'''08:55''' On-sky performance of the CLASS Q-band telescope (John Appel) <br /><br />
'''09:05''' SPIDER: an update, with foregrounds. Lots of them. (Bill Jones) <br /><br />
'''09:15''' Current state of the BICEP/Keck instrument, data and analysis (Clem Pryke) <br /><br />
'''09:25''' Planck 2018 and setting the stage for Stage-4 (Marius Millea) <br /><br />
'''09:35''' Ground, Balloon, Space Complementarity (Shaul Hanany) <br /><br />
'''09:50''' BK-SPT3G forward plans (John Kovac) <br /><br />
'''10:05''' Simons Observatory forward plans (Jo Dunkley) <br /><br />
'''10:20''' The Big Step Up to CMB-S4 (Gil Holder)<br />
<br />
'''10:35''' ''Coffee Break''<br />
<br />
'''Adjacent Science & Emerging Ideas'''<br />
<br />
'''11:15''' Millimeter/Submillimeter Large Telescopes and Instruments (Phil Mauskopf) <br /><br />
'''11:30''' Intensity mapping meets the CMB: Complementary Cosmology across the radio spectrum (Laura Newburgh) <br /><br />
'''11:45''' SPHERE-X (Jamie Bock) <br /><br />
'''12:00''' Weak Lensing (Elisabeth Krause)<br />
<br />
'''12:15''' '' Group Photo & Lunch''<br />
<br />
'''13:15''' Reionization Studies in the CMB-S4 Era (Adam Lidz) <br /><br />
'''13:30''' A biased view of open questions in galaxy formation (Norm Murray) <br /><br />
'''13:45''' Polarized dust foreground models from HI data (Susan Clark) <br /><br />
'''14:00''' Properties of the magnetized dusty interstellar medium with Planck (Jonathan Aumont)<br />
<br />
'''Talks From Collaboration Members'''<br />
<br />
'''14:15''' Inflationary vs. Reionization Features from Current and Future Data (Cora Dvorkin) <br /><br />
'''14:25''' Stress-testing nonstandard neutrino physics with CMB-S4 (Francis-Yan Cyr-Racine) <br /><br />
'''14:35''' Searching for Dark Matter Interactions in the CMB (Kimberly Boddy) <br /><br />
'''14:45''' Foreground immune CMB lensing with shear-only reconstruction (Emmanuel Schaan) <br /><br />
'''14:55''' Cosmology from cross correlating S4 lensing with photometric galaxy counts (Blake Sherwin) <br /><br />
'''15:05''' Higher order corrections to CMB lensing cross correlations (Vanessa Boehm) <br /><br />
'''15:15''' CMB lensing on small scales (Simone Ferraro) <br /><br />
'''15:25''' kSZ cosmology without the optical depth degeneracy (Mathew Madhavacheril) <br /><br />
'''15:35''' Q&A<br />
<br />
'''15:50''' ''Coffee Break''<br />
<br />
'''16:05''' Fireslides 2<br />
<br />
'''16:30''' Wrap-Up Panel - Roger Blandford, Chris Carilli, Bonnie Fleming, George Fuller, Risa Wechsler, Matias Zaldarriaga<br />
<br />
'''17:45''' Next Steps & Action Items<br />
<br />
'''Parallel Afternoon Session for Project Team'''<br />
<br />
'''15:00''' Charge for Decadal Survey Report Review on 12/11-13 in DC <br /><br />
'''15:30''' Possible DSR Review Committee and Planning Details <br /><br />
'''16:00''' Review of Overall Timeline and Boundary Conditions <br /><br />
'''16:30''' Critical Issues Identified in Project Planning <br /><br />
'''17:00''' Preparations/Guidance for Saturday Sessions <br /><br />
<br />
------<br />
<br />
=== Saturday September 8th ===<br />
<br />
'''08:30''' ''Breakfast''<br />
<br />
'''09:00''' Parallel Sessions<br />
* Science Council:<br />
** Noise & Forecasting (60 min)<br />
** White Paper Organization (45 min)<br />
* Technical Council:<br />
** Project Planning<br />
<br />
'''10:45''' ''Coffee Break''<br />
<br />
'''11:15''' Parallel Sessions<br />
*Science Council<br />
** AWG Working Meetings<br />
* Technical Council<br />
** Project Planning (continued)<br />
<br />
'''12:45''' ''Lunch (on your own)''<br />
<br />
'''13:45 onwards''' Rooms available for breakout sessions as required</div>Jchhttp://www.cmb-s4.org/wiki/index.php?title=File:CMB-S4_Galaxy_Formation_and_Evolution_(Princeton).pdf&diff=7438File:CMB-S4 Galaxy Formation and Evolution (Princeton).pdf2018-09-06T13:56:40Z<p>Jch: </p>
<hr />
<div></div>Jchhttp://www.cmb-s4.org/wiki/index.php?title=Princeton-2018:_Cosmology_with_CMB-S4&diff=7437Princeton-2018: Cosmology with CMB-S42018-09-06T13:56:17Z<p>Jch: </p>
<hr />
<div>== Workshop overview ==<br />
<br />
The Princeton 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 />
The workshop is supported by Princeton University with a generous contribution from the Kavli Institute for Cosmological Physics.<br />
<br />
This meeting will focus on moving us towards the Decadal Survey and project formation. Each day will have a different flavor:<br />
* Thursday - Collaboration, Project and Decadal Survey Report updates and discussion<br />
* Friday - Broader community building ahead of the Decadal Process<br />
* Saturday - Parallel Science & Technical Council sessions<br />
<br />
== Meeting Info & Registration ==<br />
<br />
[http://phyindico.princeton.edu/indico/event/12/page/0 Official Workshop Website: Registration, Participants, Hotels, Logistics].<br />
<br />
[[File:workshop-map-venue.png]] <br /><br />
Registration begins outside McDonnell A02 at 8 am on Thursday, 6 Sept 2018. <br />
Parking is in lot 21 (see map). <br />
<br />
'''Remote Connection Information:'''<br />
<br />
https://bluejeans.com/ <br /><br />
Meeting ID: 350 694 048 <br /><br />
*1.888.240.2560 (US Toll Free)<br />
*1.408.317.9253 (US (Primary, San Jose)) <br />
*1.408.740.7256 (US (San Jose)) <br /><br />
*Global Numbers: https://www.bluejeans.com/numbers<br />
<br />
Slack channel #princeton2018 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 />
== Agenda ==<br />
<br />
<br />
=== Thursday September 6th ===<br />
<br />
'''08:00''' ''Breakfast'' <br />
<br />
'''08:30''' Welcome & Logistics (Suzanne Staggs Herman Verlinde, chair of the Physics Department) [[File:Logistics-pton-20180906.pdf]]<br />
<br />
''' Status & Context'''<br /><br />
'''08:45''' Introduction & Collaboration Update (Julian Borrill) [[File:Cmbs4_collaboration.pdf]]<br /> <br />
'''09:05''' DSR Update (John Carlstrom) [[File:DSR-Carlstrom.pdf]]<br /><br />
'''09:25''' Project Update (Jim Yeck) [[File:S4 Princeton Workshop Yeck.pdf]]<br /><br />
'''09:45''' Q&A<br />
<br />
'''DSR - Science Council''' <br /><br />
'''10:00''' Introduction (Lloyd Knox) [[File:DSR_ScienceCouncil_Princeton2018.pdf]]<br /> <br />
'''10:15''' Gravitational Waves & Inflation (Raphael Flauger) [[File: GWPrinceton.pdf]]<br /><br />
<br />
'''10:30''' ''Coffee Break''<br />
<br />
'''11:00''' Light Relics (Daniel Green & Joel Meyers) [[File:LightRelics_Meyers_Princeton_S4.pdf]] <br /><br />
'''11:15''' Neutrino Mass (Marilena Loverde & Blake Sherwin) [[File:S4WGNeutrinoMassReport.pdf]]<br /><br />
'''11:30''' Dark Energy & Dark Matter (Vera Gluscevic & Nick Battaglia) [[File:DMDE CMBS4 Princeton2018.pdf]]<br /><br />
'''11:45''' Galaxy Formation & Evolution (Marcelo Alvarez & Colin Hill) [[File:CMB-S4_Galaxy Formation and Evolution (Princeton).pdf]] <br /><br />
'''12:00''' Legacy Catalogs (Lindsey Bleem) [[https://cmb-s4.org/wiki/images/Legacy_catalog_update_princeton_9_6_18.pdf here]]<br /><br />
'''12:15''' Q&A<br />
<br />
'''12:30''' ''Lunch & JSAC Event''<br />
<br />
'''DSR - Technical Council'''<br /><br />
'''13:30''' Introduction (McMahon/Vieregg) [[File:TechCouncilPrinceton2018.pdf]] <br /><br />
'''13:45''' Sites & Infrastructure (Kam Arnold, Brad Benson) <br /><br />
'''14:00''' Large Telescopes (Mike Niemack, Steve Padin) [[File:LargeTelescopesLargeCryostatsStatusPrincetonV2.pdf]] <br /><br />
'''14:15''' Small Telescopes (John Kovac, Chao-Lin Kuo, Aikito Kusaka) <br /><br />
'''14:30''' Detectors & Readout (Clarence Chang, Kent Irwin, Adrian Lee) [[File:DetectorsReadout.pdf]]<br /><br />
'''14:45''' Data Acquisition & Control (Laura Newburgh, Nathan Whitehorn) <br /><br />
'''15:00''' Data Management (Matthew Hasselfield) <br /><br />
'''15:15''' Integration & Commissioning (Kam Arnold, Brad Benson) <br /><br />
'''15:30''' Options (Steve Padin) [[File:OptionsPrincetonV1.pdf]] <br /><br />
'''15:45''' Q&A<br />
<br />
'''16:00''' Fireslides 1<br />
<br />
'''16:30''' Poster Session, Cocktails & Light Dinner<br />
<br />
------<br />
<br />
=== Friday September 7th ===<br />
<br />
'''08:00''' ''Breakfast''<br />
<br />
'''The CMB Circa September 2018'''<br />
<br />
'''08:30''' Harmonic Overtones (Marc Kamionkowski) <br /><br />
'''08:55''' On-sky performance of the CLASS Q-band telescope (John Appel) <br /><br />
'''09:05''' SPIDER: an update, with foregrounds. Lots of them. (Bill Jones) <br /><br />
'''09:15''' Current state of the BICEP/Keck instrument, data and analysis (Clem Pryke) <br /><br />
'''09:25''' Planck 2018 and setting the stage for Stage-4 (Marius Millea) <br /><br />
'''09:35''' Ground, Balloon, Space Complementarity (Shaul Hanany) <br /><br />
'''09:50''' BK-SPT3G forward plans (John Kovac) <br /><br />
'''10:05''' Simons Observatory forward plans (Jo Dunkley) <br /><br />
'''10:20''' The Big Step Up to CMB-S4 (Gil Holder)<br />
<br />
'''10:35''' ''Coffee Break''<br />
<br />
'''Adjacent Science & Emerging Ideas'''<br />
<br />
'''11:15''' Millimeter/Submillimeter Large Telescopes and Instruments (Phil Mauskopf) <br /><br />
'''11:30''' Intensity mapping meets the CMB: Complementary Cosmology across the radio spectrum (Laura Newburgh) <br /><br />
'''11:45''' SPHERE-X (Jamie Bock) <br /><br />
'''12:00''' Weak Lensing (Elisabeth Krause)<br />
<br />
'''12:15''' '' Group Photo & Lunch''<br />
<br />
'''13:15''' Reionization Studies in the CMB-S4 Era (Adam Lidz) <br /><br />
'''13:30''' A biased view of open questions in galaxy formation (Norm Murray) <br /><br />
'''13:45''' Polarized dust foreground models from HI data (Susan Clark) <br /><br />
'''14:00''' Properties of the magnetized dusty interstellar medium with Planck (Jonathan Aumont)<br />
<br />
'''Talks From Collaboration Members'''<br />
<br />
'''14:15''' Inflationary vs. Reionization Features from Current and Future Data (Cora Dvorkin) <br /><br />
'''14:25''' Stress-testing nonstandard neutrino physics with CMB-S4 (Francis-Yan Cyr-Racine) <br /><br />
'''14:35''' Searching for Dark Matter Interactions in the CMB (Kimberly Boddy) <br /><br />
'''14:45''' Foreground immune CMB lensing with shear-only reconstruction (Emmanuel Schaan) <br /><br />
'''14:55''' Cosmology from cross correlating S4 lensing with photometric galaxy counts (Blake Sherwin) <br /><br />
'''15:05''' Higher order corrections to CMB lensing cross correlations (Vanessa Boehm) <br /><br />
'''15:15''' CMB lensing on small scales (Simone Ferraro) <br /><br />
'''15:25''' kSZ cosmology without the optical depth degeneracy (Mathew Madhavacheril) <br /><br />
'''15:35''' Q&A<br />
<br />
'''15:50''' ''Coffee Break''<br />
<br />
'''16:05''' Fireslides 2<br />
<br />
'''16:30''' Wrap-Up Panel - Roger Blandford, Chris Carilli, Bonnie Fleming, George Fuller, Risa Wechsler, Matias Zaldarriaga<br />
<br />
'''17:45''' Next Steps & Action Items<br />
<br />
'''Parallel Afternoon Session for Project Team'''<br />
<br />
'''15:00''' Charge for Decadal Survey Report Review on 12/11-13 in DC <br /><br />
'''15:30''' Possible DSR Review Committee and Planning Details <br /><br />
'''16:00''' Review of Overall Timeline and Boundary Conditions <br /><br />
'''16:30''' Critical Issues Identified in Project Planning <br /><br />
'''17:00''' Preparations/Guidance for Saturday Sessions <br /><br />
<br />
------<br />
<br />
=== Saturday September 8th ===<br />
<br />
'''08:30''' ''Breakfast''<br />
<br />
'''09:00''' Parallel Sessions<br />
* Science Council:<br />
** Noise & Forecasting (60 min)<br />
** White Paper Organization (45 min)<br />
* Technical Council:<br />
** Project Planning<br />
<br />
'''10:45''' ''Coffee Break''<br />
<br />
'''11:15''' Parallel Sessions<br />
*Science Council<br />
** AWG Working Meetings<br />
* Technical Council<br />
** Project Planning (continued)<br />
<br />
'''12:45''' ''Lunch (on your own)''<br />
<br />
'''13:45 onwards''' Rooms available for breakout sessions as required</div>Jchhttp://www.cmb-s4.org/wiki/index.php?title=Princeton-2018:_Cosmology_with_CMB-S4&diff=7355Princeton-2018: Cosmology with CMB-S42018-09-05T17:46:37Z<p>Jch: /* Thursday September 6th */</p>
<hr />
<div>== Workshop overview ==<br />
<br />
The Princeton 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 />
The workshop is supported by Princeton University with a generous contribution from the Kavli Institute for Cosmological Physics.<br />
<br />
This meeting will focus on moving us towards the Decadal Survey and project formation. Each day will have a different flavor:<br />
* Thursday - Collaboration, Project and Decadal Survey Report updates and discussion<br />
* Friday - Broader community building ahead of the Decadal Process<br />
* Saturday - Parallel Science & Technical Council sessions<br />
<br />
== Meeting Info & Registration ==<br />
<br />
[http://phyindico.princeton.edu/indico/event/12/page/0 Official Workshop Website: Registration, Participants, Hotels, Logistics].<br />
<br />
[[File:workshop-map-venue.png]] <br /><br />
Registration begins outside McDonnell A02 at 8 am on Thursday, 6 Sept 2018. <br />
Parking is in lot 21 (see map). <br />
<br />
'''Remote Connection Information:'''<br />
<br />
https://bluejeans.com/ <br /><br />
Meeting ID: 350 694 048 <br /><br />
*1.888.240.2560 (US Toll Free)<br />
*1.408.317.9253 (US (Primary, San Jose)) <br />
*1.408.740.7256 (US (San Jose)) <br /><br />
*Global Numbers: https://www.bluejeans.com/numbers<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 />
== Agenda ==<br />
<br />
Work in progress:<br />
<br />
=== Thursday September 6th ===<br />
<br />
'''08:00''' ''Breakfast'' <br />
<br />
'''08:30''' Welcome & Logistics (Suzanne Staggs Herman Verlinde, chair of the Physics Department) <br />
<br />
''' Status & Context'''<br /><br />
'''08:45''' Introduction & Collaboration Update (Julian Borrill) <br /><br />
'''09:05''' Project Update (Jim Yeck) <br /><br />
'''09:25''' DSR Update (John Carlstrom) <br /><br />
'''09:45''' Q&A<br />
<br />
'''DSR - Science Council''' <br /><br />
'''10:00''' Introduction (Holder/Knox) <br /><br />
'''10:15''' Gravitational Waves & Inflation ()<br />
<br />
'''10:30''' ''Coffee Break''<br />
<br />
'''11:00''' Light Relics () <br /><br />
'''11:15''' Neutrino Mass () <br /><br />
'''11:30''' Dark Energy & Dark Matter () <br /><br />
'''11:45''' Galaxy Formation & Evolution (Marcelo Alvarez & Colin Hill) <br /><br />
'''12:00''' Legacy Catalogs () <br /><br />
'''12:15''' Q&A<br />
<br />
'''12:30''' ''Lunch & JSAC Event''<br />
<br />
'''DSR - Technical Council'''<br /><br />
'''13:30''' Introduction (McMahon/Vieregg) <br /><br />
'''13:45''' Sites & Infrastructure (Kam Arnold, Brad Benson) <br /><br />
'''14:00''' Large Telescopes (Mike Niemack, Steve Padin) <br /><br />
'''14:15''' Small Telescopes (John Kovac, Chao-Lin Kuo, Aikito Kusaka) <br /><br />
'''14:30''' Detectors & Readout (Clarence Chang, Kent Irwin, Adrian Lee) <br /><br />
'''14:45''' Data Acquisition & Control (Laura Newburgh, Nathan Whitehorn) <br /><br />
'''15:00''' Data Management (Matthew Hasselfield) <br /><br />
'''15:15''' Integration & Commissioning (Kam Arnold, Brad Benson) <br /><br />
'''15:30''' Options (Steve Padin) <br /><br />
'''15:45''' Q&A<br />
<br />
'''16:00''' Fireslides 1<br />
<br />
'''16:30''' Poster Session, Cocktails & Light Dinner<br />
<br />
------<br />
<br />
=== Friday September 7th ===<br />
<br />
'''08:00''' ''Breakfast''<br />
<br />
'''The CMB Circa September 2018'''<br />
<br />
'''08:30''' Harmonic Overtones (Marc Kamionkowski) <br /><br />
'''08:55''' Update on CLASS (John Appel) <br /><br />
'''09:05''' SPIDER update/new results () <br /><br />
'''09:15''' Current state of the BICEP/Keck instrument, data and analysis (Clem Pryke) <br /><br />
'''09:25''' Planck 2018 and setting the stage for Stage-4 (Marius Millea) <br /><br />
'''09:35''' Ground, Balloon, Space Complementarity (Shaul Hanany) <br /><br />
'''09:50''' BK-SPT3G forward plans (John Kovac) <br /><br />
'''10:05''' Simons Observatory forward plans (Jo Dunkley) <br /><br />
'''10:20''' The Big Step Up to CMB-S4 (Gil Holder)<br />
<br />
'''10:35''' ''Coffee Break''<br />
<br />
'''Adjacent Science & Emerging Ideas'''<br />
<br />
'''11:15''' Millimeter/Submillimeter Large Telescopes and Instruments (Phil Mauskopf) <br /><br />
'''11:30''' Intensity mapping meets the CMB: Complementary Cosmology across the radio spectrum (Laura Newburgh) <br /><br />
'''11:45''' SPHERE-X (Jamie Bock) <br /><br />
'''12:00''' Weak Lensing (Elisabeth Krause)<br />
<br />
'''12:15''' '' Group Photo & Lunch''<br />
<br />
'''13:15''' Reionization Studies in the CMB-S4 Era (Adam Lidz) <br /><br />
'''13:30''' A biased view of open questions in galaxy formation (Norm Murray) <br /><br />
'''13:45''' Polarized dust foreground models from HI data (Susan Clark) <br /><br />
'''14:00''' Properties of the magnetized dusty interstellar medium with Planck (Jonathan Aumont)<br />
<br />
'''Talks From Collaboration Members'''<br />
<br />
'''14:15''' Inflationary vs. Reionization Features from Current and Future Data (Cora Dvorkin) <br /><br />
'''14:25''' Stress-testing nonstandard neutrino physics with CMB-S4 (Francis-Yan Cyr-Racine) <br /><br />
'''14:35''' Searching for Dark Matter Interactions in the CMB (Kimberly Boddy) <br /><br />
'''14:45''' Foreground immune CMB lensing with shear-only reconstruction (Emmanuel Schaan) <br /><br />
'''14:55''' Cosmology from cross correlating S4 lensing with photometric galaxy counts (Blake Sherwin) <br /><br />
'''15:05''' Higher order corrections to CMB lensing cross correlations (Vanessa Boehm) <br /><br />
'''15:15''' CMB lensing on small scales (Simone Ferraro) <br /><br />
'''15:25''' kSZ cosmology without the optical depth degeneracy (Mathew Madhavacheril) <br /><br />
'''15:35''' Q&A<br />
<br />
'''15:50''' ''Coffee Break''<br />
<br />
'''16:05''' Fireslides 2<br />
<br />
'''16:30''' Wrap-Up Panel - Roger Blandford, Chris Carilli, Bonnie Fleming, George Fuller, Risa Wechsler, Matias Zaldarriaga<br />
<br />
'''17:45''' Next Steps & Action Items<br />
<br />
'''Parallel Afternoon Session for Project Team'''<br />
<br />
'''15:00''' Charge for Decadal Survey Report Review on 12/11-13 in DC <br /><br />
'''15:30''' Possible DSR Review Committee and Planning Details <br /><br />
'''16:00''' Review of Overall Timeline and Boundary Conditions <br /><br />
'''16:30''' Critical Issues Identified in Project Planning <br /><br />
'''17:00''' Preparations/Guidance for Saturday Sessions <br /><br />
<br />
------<br />
<br />
=== Saturday September 8th ===<br />
<br />
'''08:30''' ''Breakfast''<br />
<br />
'''09:00''' Parallel Sessions<br />
* Science Council:<br />
** Noise & Forecasting (60 min)<br />
** White Paper Organization (45 min)<br />
* Technical Council:<br />
** Project Planning<br />
<br />
'''10:45''' ''Coffee Break''<br />
<br />
'''11:15''' Parallel Sessions<br />
*Science Council<br />
** AWG Working Meetings<br />
* Technical Council<br />
** Project Planning (continued)<br />
<br />
'''12:45''' ''Lunch (on your own)''<br />
<br />
'''13:45 onwards''' Rooms available for breakout sessions as required</div>Jchhttp://www.cmb-s4.org/wiki/index.php?title=Science_Council&diff=7058Science Council2018-08-17T03:08:05Z<p>Jch: /* Galaxy Formation and Evolution */</p>
<hr />
<div>The Science Council consists of two co-Chairs and the co-Coordinators of six 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 />
====Gravitational Waves and Inflation====<br />
- Co-Coordinators: Raphael Flauger (flauger@physics.utexas.edu) and Clem Pryke (pryke@physics.umn.edu)<br />
- Meeting Notes: ??<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 />
<br />
====Light Relics====<br />
<br />
====Neutrino Mass====<br />
<br />
====Dark Energy and Dark Matter====<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====</div>Jchhttp://www.cmb-s4.org/wiki/index.php?title=Argonne-2018:P3-3&diff=6509Argonne-2018:P3-32018-03-06T16:07:49Z<p>Jch: /* Parallel session P3-3: Forecasting - Sky Modeling (chair: R. Flauger) */</p>
<hr />
<div>Back to [[Argonne-2018: Cosmology with CMB-S4|Argonne 2018 main page]]<br />
<br />
== Parallel session P3-3: Forecasting - Sky Modeling (chair: R. Flauger) ==<br />
<br />
* Introduction<br />
*[[File:slides|Carlo Baccigalupi]]<br />
*[[File:slides|Kevin Huffenberger]]<br />
*[[:File:Argonne_P33_Marcelo.pdf|Marcelo Alvarez]]<br />
*[[File:slides|Alex van Engelen]]<br />
*[[File:JCH.pdf|Colin Hill]]<br />
*[[File:slides|Blake Sherwin]]<br />
* Discussion<br />
<br />
== Notes from session (Tuesday, March 6, 11:15-12:45) ==</div>Jchhttp://www.cmb-s4.org/wiki/index.php?title=File:JCH.pdf&diff=6508File:JCH.pdf2018-03-06T16:05:16Z<p>Jch: Jch uploaded a new version of File:JCH.pdf</p>
<hr />
<div></div>Jchhttp://www.cmb-s4.org/wiki/index.php?title=Argonne-2018:P1-3&diff=6480Argonne-2018:P1-32018-03-06T14:18:53Z<p>Jch: /* Parallel session P1-3: Extending the Science case for the Decadal CDR (chair: Simone Ferraro) */</p>
<hr />
<div>Back to [[Argonne-2018: Cosmology with CMB-S4|Argonne 2018 main page]]<br />
<br />
== Parallel session P1-3: Extending the Science case for the Decadal CDR (chair: Simone Ferraro) ==<br />
<br />
*[[:File:slides|Intro]]<br />
*[[:File:schaan_ksz.pdf|Emmanuel]]<br />
*[[:File:Elena_SZpol.pdf|Elena]]<br />
*[[:File:Alvarez-eor.pdf|Marcelo]]<br />
*[[:File:TSZ.pdf|Colin]]<br />
*[[:File:Rahul_Sources.pdf|Rahul]]<br />
<br />
== Notes from session (Tuesday, March 6, 08:45-09:45) ==</div>Jchhttp://www.cmb-s4.org/wiki/index.php?title=File:TSZ.pdf&diff=6479File:TSZ.pdf2018-03-06T14:18:25Z<p>Jch: </p>
<hr />
<div></div>Jchhttp://www.cmb-s4.org/wiki/index.php?title=File:LSS_summary_JCH.pdf&diff=5198File:LSS summary JCH.pdf2017-08-25T18:25:05Z<p>Jch: </p>
<hr />
<div></div>Jchhttp://www.cmb-s4.org/wiki/index.php?title=Harvard-2017:Science_Case_and_Preparing_for_the_Decadal_Review&diff=5197Harvard-2017:Science Case and Preparing for the Decadal Review2017-08-25T18:23:51Z<p>Jch: /* Plenary Session: Science Case & Preparing for the Decadal Review (Chair: Cora Dvorkin ) [Jefferson 250] */</p>
<hr />
<div>Back to [[Harvard-2017:_Cosmology_with_CMB-S4#Friday.2C_25_August| Harvard-2017 main page]]<br />
==Plenary Session: Science Case & Preparing for the Decadal Review (Chair: Cora Dvorkin ) [Jefferson 250]==<br />
<br />
Post talks here.<br />
* Mechanics of decadal review process and timeline -- John Carlstrom [[File:CMB-S4andDecadalProcess.pdf]]<br />
* Reports from parallels II here w/ emphasis on synergy (e.g. LSS + S4) -- Session II chairs:<br />
<br />
Space and Balloons [[File:SpaceComplementarity.pdf]]<br />
<br />
E-mode Cosmology [[File:Report_from_E-modes_session_Dvorkin.pdf]]<br />
<br />
High-ell / Large-Scale Structure [[File:LSS_summary_JCH.pdf]]<br />
<br />
* Organizing outreach (White papers, conferences, ...) -- Lloyd Knox [[File: ]]<br />
<br />
== Notes from session ==<br />
<br />
<br />
== Action items/Next steps ==<br />
<br />
Summarize action items here</div>Jchhttp://www.cmb-s4.org/wiki/index.php?title=File:LSS_summary.pdf&diff=5196File:LSS summary.pdf2017-08-25T18:22:23Z<p>Jch: </p>
<hr />
<div></div>Jch