LAT Frequency Flowdown

From CMB-S4 wiki
Revision as of 12:23, 22 April 2019 by Jch (talk | contribs)
Jump to navigationJump to search


(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 the CMB-S4 LATs.

Setup and Assumptions

I use the noise calculator for the CMB-S4 LATs posted at

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.

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.

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.


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 . These maps are also available at

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

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.

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.