The COSMOS ACS Catalog
COSMOS measurements of the integrated stellar content as a function of halo mass.
To access the HOD measurement of f* as a function of halo mass (either M200b or M500c) and redshift please here. For more details on these measurements, please look xxxx. Note that if you compare the contribution from central galaxies to f* in these files to the SHMR for central galaxies you will find a small difference between the two curves. This is because the former represents the mean value of P(M*|Mh) whereas the later represents the median value of P(M*|Mh). The two estimates differ because of scatter in the SHMR. In this work, P(M*|Mh) is assumed to be a log-normal.
Stellar Mass Completeness of BOSS Galaxy Samples
In <a href=”http://adsabs.harvard.edu/abs/2015arXiv150704752L”>Leauthaud et al. 2015 </a> I quantified the stellar mass completeness of the BOSS galaxy samples. Please <a href=”http://member.ipmu.jp/alexie.leauthaud/boss_completeness/”>CLICK
HERE</a> to access files for these completeness estimates.</p>
<p class=”para3″ align=”justify”> Details can also be found at the <a href=”http://www.massivegalaxies.com/”>Massive Galaxies
COSMOS measurements of the Pivot masses
The pivot masses describe the masses for which the ratio Mhalo/M* reaches a minimum. This minimum is noteworthy for models of galaxy formation because it marks the mass at which the accumulated stellar growth of the central galaxy has been the most efficient. This minimum can be described in terms of the ‘pivot stellar mass’, M*piv , the ‘pivot halo mass’, Mhpiv, and the ‘pivot ratio’, (Mh/M*)piv (see xxx). Please click HERE to access files for the COSMOS pivot masses.
COSMOS galaxies in X-ray groups to z=1
With former Berkeley graduate student Matt George, we have produced a group membership catalog for a sample of 160 X-ray selected groups in COSMOS. This catalog has been made
public and you can find the details in xxx.
Compilation of low-z data used to plot the stellar-to-halo mass relation (SHMR) in Leauthaud et al. 2011b (Figure 10)
CLICK HERE</a> to access a tarfile containing a compilation of data points for the low z (z<0.4) SHMR. This file should allow you to reproduce most of the data points from Leauthaud et al. 2011b (see figure below). Please note that all data points have been converted to represent P(M*|Mh). h=0.72 is assumed. Stellar masses have been converted to a Chabrier IMF. Halo mass is defined as M200b (defined wrsp 200*background density). Halo masses have been converted to M200b assuming a NFW profile and a Munoz-Cuartas et al. (2010) mass-concentration relation for a WMAP5 cosmology when necessary.
For further details on the data points (and associated uncertainties), please read <a href=”http://adsabs.harvard.edu/abs/2011arXiv1104.0928L”>Leauthaud et al. 2011b.</a> Please also make sure to quote the original source of each measurement (described in the file header and in the Figure below).
Please make sure that you
familiarize yourself with the various uncertainties related
to each of these measurements. Errors quoted here only
represent statistical uncertainty (68% confidence level), it
is YOUR responsibility to make sure you understand the
possible systematic uncertainties in each of these
The results in these files have been
converted from the original measurement to a common halo mass
definition (M200b) and value of h=0.72. Please make the necessary
sanity checks and if you find any errors, please do let me know so
that I can fix them.