... MAXIMA-1

http://cosmology.berkeley.edu/group/cmb/

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... Boomerang

http://cmb.phys.cwru.edu/boomerang/

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... WMAP

http://map.gsfc.nasa.gov

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... VSA

http://www.mrao.cam.ac.uk/telescopes/vsa/

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... CBI

http://www.astro.caltech.edu/tjp/CBI/

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... SCP

http://panisse.lbl.gov

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... search

http://cfa-www.harvard.edu/cfa/oir/Research/supernova/HighZ.html

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... SDSS

http://www.sdss.org/

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... 2dF

http://www.aao.gov.au/2df

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... APEX

http://bolo.berkeley.edu/apexsz/

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... SZA

http://astro.uchicago.edu/sza/

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... AMI

http://www.mrao.cam.ac.uk/telescopes/ami/

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... ACT

http://www.hep.upenn.edu/act

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... Surveyor

http://astro.estec.esa.nl/Planck

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... Telescope

http://astro.uchicago.edu/spt

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... Consortium

http://www.mpa-garching.mpg.de/Virgo/

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... catalogs

For the exact description of these catalogs see Evrard et al. (2002).

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... CMB

http://cmb.as.arizona.edu/~eisenste/acousticpeak/

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... freedom

One also has to consider the steepness of the luminosity function of those objects.

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... K.A.O.S.

http://www.noao.edu/kaos/

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... avoided

This is only true when we have enough galaxy redshifts per cluster, so that one can average down to something close to the center of mass velocity. One might also try to exploit the fact that the bright central cD galaxies have small velocities with respect to the rest of the cluster (see the simulation results by Berlind et al. 2003). Even if one is able to find a good estimate for the center of mass velocity for each cluster in the sample, the redshift space distortions on reasonably large scales would still deviate from the simple linear prediction (Scoccimarro 2004).

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... mission

Using the spectral dependence of thermal SZ effect (see Eq. (23)) we see that the 30 mJy sensitivity of PLANCK's 353 GHz channel corresponds to 17 mJy at 153 GHz.

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...(Eisenstein et al. 2005)

The detection has also been claimed using the 2dF redshift survey (Cole et al. 2005).

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...=0)

The light-cone bias parameters calculated this way are 5.0, 4.7, 4.3 for the PLANCK and 4.4, 4.1, 3.9 for the SPT with the number of clusters 15 000, 25 000 and 350 000, respectively.

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... sight

The Alcock-Paczynski test (Alcock & Paczynski 1979) is based on these cosmological distortions.

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... functions

In the calculations we use the FKP weight function.

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... 353 GHz

http://astro.estec.esa.nl/Planck

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