132 research outputs found
Marked Statistics and the Environmental Dependence of Galaxy Formation
Many have used the two-point correlation function to study the clustering of galaxies as a function of their properties, such as luminosity, color, and stellar mass. We explore the technique of `marked' correlations, in which clustering is measured with galaxies weighted by a particular property or `mark'. Marked clustering statistics identify and quantify how galaxy properties are correlated with their environment. We present marked correlation analyses in the framework of the dark matter halo model, in which all environmental correlations are due to the correlation of the masses and formation histories of halos with their environment. We perform marked correlation analyses of galaxy luminosity, color, stellar mass, metallicity, and star formation rate in the Sloan Digital Sky Survey and the Millennium Run Simulation. We also analyze luminosity-marked correlations of galaxies in groups and clusters. Our measurements show that luminous, red, massive, metal-rich, and passively star forming galaxies tend to be located in denser environments than fainter, bluer, less massive, metal-poor, and actively star forming galaxies. Our marked correlation measurements also show how these environmental correlations vary as a function of scale. Our halo-model analyses show that the environmental dependence of luminosity and stellar mass of SDSS galaxies is primarily driven by the environmental dependence of halo mass
Galaxy formation with cold gas accretion and evolving stellar initial mass function
The evolution of the galaxy stellar mass function is especially useful to
test the current model of galaxy formation. Observational data have revealed a
few inconsistencies with predictions from the model. For
example, most massive galaxies have already been observed at very high
redshifts, and they have experienced only mild evolution since then. In
conflict with this, semi-analytical models of galaxy formation predict an
insufficient number of massive galaxies at high redshift and a rapid evolution
between redshift 1 and 0 . In addition, there is a strong correlation between
star formation rate and stellar mass for star-forming galaxies, which can be
roughly reproduced with the model, but with a normalization that is too low at
high redshift. Furthermore, the stellar mass density obtained from the integral
of the cosmic star formation history is higher than the measured one by a
factor of 2. In this paper, we study these issues using a semi-analytical model
that includes: 1) cold gas accretion in massive halos at high redshift; 2)
tidal stripping of stellar mass from satellite galaxies; and 3) an evolving
stellar initial mass function (bottom-light) with a higher gas recycle
fraction. Our results show that the combined effects from 1) and 2) can predict
sufficiently massive galaxies at high redshifts and reproduce their mild
evolution at low redshift, While the combined effects of 1) and 3) can
reproduce the correlation between star formation rate and stellar mass for
star-forming galaxies across wide range of redshifts. A bottom-light/top-heavy
stellar IMF could partly resolve the conflict between the stellar mass density
and cosmic star formation history.Comment: 9 pages, 7 figures. Accepted for publication in Ap
Satellite Luminosities in Galaxy Groups
Halo model interpretations of the luminosity dependence of galaxy clustering
assume that there is a central galaxy in every sufficiently massive halo, and
that this central galaxy is very different from all the others in the halo. The
halo model decomposition makes the remarkable prediction that the mean
luminosity of the non-central galaxies in a halo should be almost independent
of halo mass: the predicted increase is about 20% while the halo mass increases
by a factor of more than 20. In contrast, the luminosity of the central object
is predicted to increase approximately linearly with halo mass at low to
intermediate masses, and logarithmically at high masses. We show that this
weak, almost non-existent mass-dependence of the satellites is in excellent
agreement with the satellite population in group catalogs constructed by two
different collaborations. This is remarkable, because the halo model prediction
was made without ever identifying groups and clusters. The halo model also
predicts that the number of satellites in a halo is drawn from a Poisson
distribution with mean which depends on halo mass. This, combined with the weak
dependence of satellite luminosity on halo mass, suggests that the Scott
effect, such that the luminosities of very bright galaxies are merely the
statistically extreme values of a general luminosity distribution, may better
apply to the most luminous satellite galaxy in a halo than to BCGs. If galaxies
are identified with halo substructure at the present time, then central
galaxies should be about 4 times more massive than satellite galaxies of the
same luminosity, whereas the differences between the stellar M/L ratios should
be smaller. Therefore, a comparison of the weak lensing signal from central and
satellite galaxies should provide useful constraints. [abridged]Comment: 8 pages, 3 figures. Matches version accepted by MNRA
Central and Satellite Colors in Galaxy Groups: A Comparison of the Halo Model and SDSS Group Catalogs
Current analytic and semi-analytic dark matter halo models distinguish
between the central galaxy in a halo and the satellite galaxies in halo
substructures. Using a recent halo-model description of the color dependence of
galaxy clustering (Skibba & Sheth 2008), we investigate the colors of central
and satellite galaxies predicted by the model and compare them to those of two
galaxy group catalogs constructed from the Sloan Digital Sky Survey (Yang et
al. 2007, Berlind et al. 2006a). In the model, the environmental dependence of
galaxy color is determined by that of halo mass, and the predicted color mark
correlations were shown to be consistent with SDSS measurements. The model
assumes that satellites tend to follow a color-magnitude sequence that
approaches the red sequence at bright luminosities; the model's success
suggests that bright satellites tend to be `red and dead' while the star
formation in fainter ones is in the process of being quenched. In both the
model and the SDSS group catalogs, we find that at fixed luminosity or stellar
mass, central galaxies tend to be bluer than satellites. In contrast, at fixed
group richness or halo mass, central galaxies tend to be redder than
satellites, and galaxy colors become redder with increasing mass. We also
compare the central and satellite galaxy color distributions, as a function of
luminosity and as a function of richness, in the model and in the two group
catalogs. Except for faint galaxies and small groups, the model and both group
catalogs are in very good agreement.Comment: 9 pages, 7 figures, revised version submitted to MNRAS. Significant
revisions were made, and figures were added showing the color distributions.
Important correction: the model and both group catalogs now have consistent
satellite colors--almost independent of group richnes
Evaluating and Improving Semi-analytic modelling of Dust in Galaxies based on Radiative Transfer Calculations
The treatment of dust attenuation is crucial in order to compare the
predictions of galaxy formation models with multiwavelength observations. Most
past studies have either used simple analytic prescriptions or else full
radiative transfer (RT) calculations. Here, we couple star formation histories
and morphologies predicted by the semi-analytic galaxy formation model MORGANA
with RT calculations from the spectrophotometric and dust code GRASIL to create
a library of galaxy SEDs from the UV/optical through the far Infrared, and
compare the predictions of the RT calculations with analytic prescriptions. We
consider a low and high redshift sample, as well as an additional library
constructed with empirical, non-cosmological star formation histories and
simple (pure bulge or disc) morphologies. Based on these libraries, we derive
fitting formulae for the effective dust optical depth as a function of galaxy
physical properties such as metallicity, gas mass, and radius. We show that
such fitting formulae can predict the V-band optical depth with a scatter
smaller than 0.4 dex for both the low and high redshift samples, but that there
is a large galaxy-to-galaxy scatter in the shapes of attenuation curves,
probably due to geometrical variations, which our simple recipe does not
capture well. However, our new recipe provides a better approximation to the
GRASIL results at optical wavelength than standard analytic prescriptions from
the literature, particularly at high redshift.Comment: 20 pages, 13 figures, 4 tables; accepted for publication by MNRA
PRIMUS: The Effect of Physical Scale on the Luminosity-Dependence of Galaxy Clustering via Cross-Correlations
We report small-scale clustering measurements from the PRIMUS spectroscopic
redshift survey as a function of color and luminosity. We measure the
real-space cross-correlations between 62,106 primary galaxies with PRIMUS
redshifts and a tracer population of 545,000 photometric galaxies over
redshifts from z=0.2 to z=1. We separately fit a power-law model in redshift
and luminosity to each of three independent color-selected samples of galaxies.
We report clustering amplitudes at fiducial values of z=0.5 and L=1.5 L*. The
clustering of the red galaxies is ~3 times as strong as that of the blue
galaxies and ~1.5 as strong as that of the green galaxies. We also find that
the luminosity dependence of the clustering is strongly dependent on physical
scale, with greater luminosity dependence being found between r=0.0625 Mpc/h
and r=0.25 Mpc/h, compared to the r=0.5 Mpc/h to r=2 Mpc/h range. Moreover,
over a range of two orders of magnitude in luminosity, a single power-law fit
to the luminosity dependence is not sufficient to explain the increase in
clustering at both the bright and faint ends at the smaller scales. We argue
that luminosity-dependent clustering at small scales is a necessary component
of galaxy-halo occupation models for blue, star-forming galaxies as well as for
red, quenched galaxies.Comment: 13 pages, 6 figures, 5 tables; published in ApJ (revised to match
published version
Dark Matter Halo Models of Stellar Mass-Dependent Galaxy Clustering in PRIMUS+DEEP2 at 0.2<z<1.2
We utilize CDM halo occupation models of galaxy clustering to
investigate the evolving stellar mass dependent clustering of galaxies in the
PRIsm MUlti-object Survey (PRIMUS) and DEEP2 Redshift Survey over the past
eight billion years of cosmic time, between . These clustering
measurements provide new constraints on the connections between dark matter
halo properties and galaxy properties in the context of the evolving
large-scale structure of the universe. Using both an analytic model and a set
of mock galaxy catalogs, we find a strong correlation between central galaxy
stellar mass and dark matter halo mass over the range
-, approximately consistent
with previous observations and theoretical predictions. However, the
stellar-to-halo mass relation (SHMR) and the mass scale where star formation
efficiency reaches a maximum appear to evolve more strongly than predicted by
other models, including models based primarily on abundance-matching
constraints. We find that the fraction of satellite galaxies in haloes of a
given mass decreases significantly from to , partly due to
the fact that haloes at fixed mass are rarer at higher redshift and have lower
abundances. We also find that the ratio, a model parameter
that quantifies the critical mass above which haloes host at least one
satellite, decreases from at to at .
Considering the evolution of the subhalo mass function vis-\`{a}-vis satellite
abundances, this trend has implications for relations between satellite
galaxies and halo substructures and for intracluster mass, which we argue has
grown due to stripped and disrupted satellites between and
.Comment: 17 pages, 9 figures and 4 tables; Astrophysical Journal, publishe
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