Difference between revisions of "ForecastingStep1"
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*White noise, no FG inflation | *White noise, no FG inflation | ||
− | *S4 | + | *S4 T/E/B/k over 40% of sky, 30<ell < lmax |
*Planck TT/TE/EE from 30<l<2500 over additional 20% of sky. Can use these 'Planck-pol' specs for noise:[[File:planck_pol.pdf|500px]] | *Planck TT/TE/EE from 30<l<2500 over additional 20% of sky. Can use these 'Planck-pol' specs for noise:[[File:planck_pol.pdf|500px]] | ||
*Planck TT at l<30 over 80% of sky | *Planck TT at l<30 over 80% of sky |
Revision as of 04:23, 19 April 2016
Checking forecasting outputs
This should be run for the test case for S4+Planck. This is T/E/kappa. No clusters or BAO at this point (can be posted in other entries though). Settings described here and here:
- S4 = single channel (e.g. 150 GHz) at 1 uK/amin in T and 1.4uK/amin in P, 3 arcmin resolution.
- White noise, no FG inflation
- S4 T/E/B/k over 40% of sky, 30<ell < lmax
- Planck TT/TE/EE from 30<l<2500 over additional 20% of sky. Can use these 'Planck-pol' specs for noise:File:Planck pol.pdf
- Planck TT at l<30 over 80% of sky
- Tau prior 0.06+-0.01
- lmax(TT)=3000 unless explicit foreground cleaning is done in code for kSZ etc
- lmax(TE,EE)=5000 unless explicit foreground cleaning done in code
- kk reconstructed from 30<l<lmax using MV estimate
- quadratic estimator for lensing, ideally with iterative delensing
- Gaussian likelihood neglecting T/E/k covariance is ok, but non-Gaussian better
- non-linear power spectrum for kk, e.g. ok to use halofit in CAMB
- if easy to do, use pivot k=0.05
obh2 | och2 | theta | As | ns | tau | |
Stephen/Josquin | ||||||
Alex/Joel/Dan | ||||||
Mat/Neelima/Nam | ||||||
Add your name here |
obh2 | och2 | theta | As | ns | tau | mnu (meV) | |
Stephen/Josquin | |||||||
Alex/Joel/Dan | |||||||
Mat/Neelima/Nam | |||||||
Add your name here |