Difference between revisions of "Expected Survey Performance for Science Forecasting"

From CMB-S4 wiki
Jump to: navigation, search
(Observation Definition)
(Observation Definition)
Line 17: Line 17:
 
'''Deep and Wide Field (Hi-res)'''
 
'''Deep and Wide Field (Hi-res)'''
  
[Caution... these numbers will be updated shortly.]
+
[Caution... these uK-arcmin numbers will be updated shortly.]
  
 
{| class="wikitable" style="text-align: right; margin-left: 51px;"
 
{| class="wikitable" style="text-align: right; margin-left: 51px;"

Revision as of 13:18, 30 May 2019

The most up-to-date expected survey performances (previously called "experiment definitions"), and all the historical ones used for iterating, for both large-area survey and small-area survey, can be found at Survey Performance Expectations.

Expected Survey Performances (a result of instrument performance and observations) below are the converged result at each epoch (or will be once someone fills them in).


Reference Design

Instrument Definition

LAT

SAT

Observation Definition

Deep and Wide Field (Hi-res)

[Caution... these uK-arcmin numbers will be updated shortly.]

Galactic cut (in %) 0 10 20 30
Sky fraction (in %) 75.8 69.3 61.6 53.9
Effective sky fraction for noise (in %) 70.9 64.8 57.3 50.1
Effective sky fraction for signal (in %) 66.2 60.6 53.3 46.5


Frequency (GHz) 30 40 95 145 220 270
white noise level TT (uK-arcmin) 9.5 11.5 1.5 2.1 7.9 13.8
ell knee TT 433 395 1315 4651 4511 4525
1/f exponent TT (uK-arcmin) -3.5 -3.4 -3.1 -2.3 -3.4 -3.4
white noise level E/B (uK-arcmin) 13.4 16.3 2.2 2.9 11.2 19.6
ell knee E/B 467 467 467 467 467 467
1/f exponent E/B (uK-arcmin) -1.1 -1.1 -1.1 -1.1 -1.1 -1.1
Penalty (relative to f_sky scaling) 1.04 1.08 1.06 1.06 1.07 1.09

Hi-res Ultra-deep Field

All numbers are defined for v1 of the pole deep survey described here, which has and effective sky fraction for noise of 2.88%

Frequency (GHz) 20 30 40 95 145 220 270
Beam FWHM (arcmin) 11.0 7.3 5.5 2.3 1.5 1.0 0.8
white noise level E/B (uK-arcmin) 8.44 5.03 4.51 0.68 0.96 5.72 9.80
ell knee E/B 200 200 200 200 200 200 200
1/f exponent E/B -2.0 -2.0 -2.0 -2.0 -3.0 -3.0 -3.0
ell min 30 30 30 30 30 30 30
nside 512 512 512 512 512 512 512


Lo-Res Ultra-Deep Field

All numbers are defined for v1 of the pole deep survey described here, which has and effective sky fraction for noise of 2.88%

Frequency (GHz) 30 40 85 95 145 155 220 270
Bandwidth (GHz) 9.0 12.0 20.4 22.8 31.9 34.1 48.4 59.4
Beam FWHM (arcmin) 72.8 72.8 25.5 25.5 22.7 22.7 13.0 13.0
white noise level TT (uK-arcmin) 5.64 7.14 1.41 1.24 2.71 2.90 7.50 12.85
ell knee TT 150 150 150 150 230 230 230 230
1/f exponent TT -4.4 -4.4 -4.4 -4.4 -3.8 -3.8 -3.8 -3.8
white noise level EE (uK-arcmin) 3.74 4.73 0.93 0.82 1.25 1.34 3.48 8.08
ell knee EE 60 60 60 60 65 65 65 65
1/f exponent EE -2.2 -2.2 -2.2 -2.2 -3.1 -3.1 -3.1 -3.1
white noise level BB (uK-arcmin) 3.53 4.46 0.88 0.78 1.23 1.34 3.48 5.97
ell knee BB 60 60 60 60 60 60 60 60
1/f exponent BB -1.7 -1.7 -1.7 -1.7 -3.0 -3.0 -3.0 -3.0
ell min 30 30 30 30 30 30 30 30
nside 512 512 512 512 512 512 512 512



CDT Design

Instrument Definition

LAT

SAT

Observation Definition

Delensing LAT

Wide-Area LAT

Pole SAT

Atacama SAT