RESOLVE and ECO: The Halo Mass-Dependent Shape of Galaxy Stellar and
  Baryonic Mass Functions
  In this work, we present galaxy stellar and baryonic (stars plus cold gas)
mass functions (SMF and BMF) and their halo mass dependence for two
volume-limited data sets. The first, RESOLVE-B, coincides with the Stripe 82
footprint and is extremely complete down to baryonic mass Mbary ~ 10^9.1 Msun,
probing the gas-rich dwarf regime below Mbary ~ 10^10 Msun. The second, ECO,
covers a ~40 times larger volume (containing RESOLVE-A) and is complete to
Mbary ~ 10^9.4 Msun. To construct the SMF and BMF we implement a new "cross-bin
sampling" technique with Monte Carlo sampling from the full likelihood
distributions of stellar or baryonic mass. Our SMFs exhibit the "plateau"
feature starting below Mstar ~ 10^10 Msun that has been described in prior
work. However, the BMF fills in this feature and rises as a straight power law
below ~10^10 Msun, as gas-dominated galaxies become the majority of the
population. Nonetheless, the low-mass slope of the BMF is not as steep as that
of the theoretical dark matter halo MF. Moreover, we assign group halo masses
by abundance matching, finding that the SMF and BMF separated into four
physically motivated halo mass regimes reveal complex structure underlying the
simple shape of the overall MFs. In particular, the satellite MFs are depressed
below the central galaxy MF "humps" in groups with mass <10^13.5 Msun yet rise
steeply in clusters. Our results suggest that satellite destruction and/or
stripping are active from the point of nascent group formation. We show that
the key role of groups in shaping MFs enables reconstruction of a given
survey's SMF or BMF based on its group halo mass distribution.
