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SHAM Beyond Clustering: New Tests of Galaxy-Halo Abundance Matching with Galaxy Groups | | Andrew P. Hearin
; Andrew R. Zentner
; Andreas A. Berlind
; Jeffrey A. Newman
; | | Date: |
17 Oct 2012 | | Abstract: | We construct mock catalogs of galaxy groups using subhalo abundance matching
(SHAM) and undertake several new tests of the SHAM prescription for the
galaxy-dark matter connection. All SHAM models we studied exhibit significant
tension with galaxy groups observed in the Sloan Digital Sky Survey (SDSS). The
SHAM prediction for the field galaxy luminosity function is systematically too
dim, and the group galaxy luminosity function systematically too bright,
regardless of the details of the SHAM prescription. SHAM models connecting
r-band luminosity, Mr, to Vacc, the maximum circular velocity of a subhalo at
the time of accretion onto the host, faithfully reproduce galaxy group
abundance as a function of richness, g(N). However, SHAM models connecting Mr
with Vpeak, the peak value of Vmax over the entire merger history of the halo,
over-predict the abundance of galaxy groups. Our results suggest that no SHAM
model can simultaneously reproduce the observed group multiplicity function and
two-point projected galaxy clustering. Nevertheless, we also report a new
success of SHAM: an accurate prediction for Phi(m12), the abundance of galaxy
groups as a function of magnitude gap m12, defined as the difference between
the r-band absolute magnitude of the two brightest group members. We show that
it may be possible to use joint measurements of g(N) and Phi(m12) to tightly
constrain the details of the SHAM implementation. Additionally, we show that
the hypothesis that the luminosity gap is constructed via random draws from a
universal luminosity function provides a poor description of the data,
contradicting recent claims in the literature. Finally, we test a common
assumption of the Conditional Luminosity Function (CLF) formalism, that the
satellite LF need only be conditioned by the brightness of the central galaxy.
We find this assumption to be well-supported by the observed Phi(m12). | | Source: | arXiv, 1210.4927 | | Services: | Forum | Review | PDF | Favorites | |
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