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

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'''Hi-res Ultra-deep Field ''' | '''Hi-res Ultra-deep Field ''' | ||

− | All numbers are defined for v1 of the pole deep survey described here, which has | + | All numbers are defined for v1 of the pole deep survey described here, which has an effective sky fraction for noise of 2.88%. |

+ | Please see [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190607_LATSTM/ this posting] for a source of the white noise levels given here. | ||

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'''Lo-Res Ultra-Deep Field''' | '''Lo-Res Ultra-Deep Field''' | ||

− | All numbers are defined for v1 of the pole deep survey described here, which has | + | All numbers are defined for v1 of the pole deep survey described here, which has an effective sky fraction for noise of 2.88%. |

+ | To obtain the white noise levels given below, one should take the numbers in the first table under [https://cmb-s4.org/wiki/index.php/Survey_Performance_Expectations "Small-area Survey Performance Expectation 05"] (scaled from achieved BK performance and to a 3% patch), which are given for a 1-4-4-3 tube configuration and 7 yrs of observation, scale to 2-6-6-4 tubes (i.e. divide by factors of sqrt(2/1), sqrt(6/4) and sqrt(4/3)), then further scale down by sqrt(3)/sqrt(2.88)*sqrt(1.32). This last factor comes from dividing out the initial scaling to 3%, and applying an extra ratio of (noise) f_sky for BK and the survey of interest (the 2.88 and 1.32 numbers can be found [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190511_sigmar_vs_r_galcuts/?&obseff=full&decorr=decorr_&decorr2=lineardecorr_&linlog=loglog&linlog2=loglog&maskname=mask_iwcov_tot_pole_deep_v1_&plots=plots&nmask2=5mask&fg=without&weight=optweight_v1&ntube=18&stat=AL&band=&minpole=&r=0&galmask=&morechilefg=_morechilefg&dustsync=Dust&galcut=58#permalink_fig7 in this posting] by clicking "Pole Deep (v1)" and "04d") | ||

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## Revision as of 14:57, 7 June 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).

## Contents

## DSR Reference Design

### Instrument Definition

**LAT**

**SAT**

### Observation Definition

**Deep and Wide Field (Hi-res)**

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) | 21.8 | 12.4 | 2.0 | 2.0 | 6.9 | 16.7 |

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) | 30.8 | 17.6 | 2.9 | 2.8 | 9.8 | 23.6 |

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 |

**Hi-res Ultra-deep Field **

All numbers are defined for v1 of the pole deep survey described here, which has an effective sky fraction for noise of 2.88%. Please see this posting for a source of the white noise levels given here.

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 an effective sky fraction for noise of 2.88%. To obtain the white noise levels given below, one should take the numbers in the first table under "Small-area Survey Performance Expectation 05" (scaled from achieved BK performance and to a 3% patch), which are given for a 1-4-4-3 tube configuration and 7 yrs of observation, scale to 2-6-6-4 tubes (i.e. divide by factors of sqrt(2/1), sqrt(6/4) and sqrt(4/3)), then further scale down by sqrt(3)/sqrt(2.88)*sqrt(1.32). This last factor comes from dividing out the initial scaling to 3%, and applying an extra ratio of (noise) f_sky for BK and the survey of interest (the 2.88 and 1.32 numbers can be found in this posting by clicking "Pole Deep (v1)" and "04d")

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**