APEX stuff – 4 Feb 2003. Martin White Department of Physics Department of Astronomy UC Berkeley Lawrence Berkeley National Lab. Some points. CMB confusion is quite an issue – two frequencies are better than one. dN/dz curves are smooth, for most cosmology don’t need very accurate z’s.
Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author.While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server.
Department of Physics
Department of Astronomy
Lawrence Berkeley National Lab
Linear color scale: -100mK to +100mK
Effects of beam
MHW~ l2 e- l2
When sources are well separated and/or the background does not contribute much power on the scales of interest, filtering is relatively easy. In our situation …
… plus foregrounds!
Cluster counts are most sensitive to the matter density and the normalization of the power spectrum.
Local abundance not held fixed!
Derivatives are smooth over Dz~0.1 – don’t need good redshifts!
IRAS 100mm map (mK)
The sun is not “in” this field in Jan ’04.
30 minute drift scans for 50 days
(~400 hours total)
On line, late 2004
25% of telescope time will be dedicated to SZ survey
… with Volker Springel & Lars Hernquist
Sources found with Sextractor
Y~M x T
Effect is indep.
c.f. optical richness
Heating or cooling alone
can cause big shifts, but
when combined in a self-
consistent model …
Atacama is at –23o so only sky with d<-67o can be observed
Plus lost time for sun, moon, …