A spectroscopic measurement of galaxy formation time‐scales with the Redshift One LDSS3 Emission line Survey
We present measurements of the specific star formation rate (SSFR)–stellar mass relation for star-forming galaxies. Our deep spectroscopic samples are based on the Redshift One LDSS3 Emission line Survey (ROLES) and European Southern Observatory (ESO) public spectroscopy at z= 1, and on the Sloan Digital Sky Survey (SDSS) at z= 0.1. These data sets cover an equally deep mass range of 8.5 ≲ log(M*/M⊙) ≲ 11 at both epochs. We find that the SSFR–mass relation evolves in a way which is remarkably independent of stellar mass, as we previously found for the SFR density (SFRD)–mass relation. However, we see a subtle upturn in SSFR–mass for the lowest mass galaxies (which may at least partly be driven by mass-incompleteness in the K-selected sample). This upturn is suggestive of greater evolution for lower mass galaxies, which may be explained by less massive galaxies forming their stars later and on longer time-scales than higher mass galaxies, as implied by the ‘cosmic downsizing’ scenario. Parametrizing the e-folding time-scale and formation redshift as simple functions of baryonic mass gives best-fitting parametrizations of τ(Mb) ∝M−1.01b and 1 +zf(Mb) ∝M0.30b. This subtle upturn is also seen in the SFRD as a function of stellar mass. At higher masses, such as those probed by previous surveys, the evolution in SSFR–mass is almost independent of stellar mass. At higher masses [log(M*/M⊙) > 10] the shapes of the cumulative cosmic SFRDs are very similar at both z= 0.1 and 1.0, both showing 70 per cent of the total SFRD above a mass of log(M*/M⊙) > 10. Mass functions are constructed for star-forming galaxies and found to evolve by only <35 per cent between z= 1 and 0.1 over the whole mass range. The evolution is such that the mass function decreases with increasing cosmic time, confirming that galaxies are leaving the star-forming sequence/blue cloud. The observational results are extended to z∼ 2 by adding two recent Lyman break galaxy samples, and data at these three epochs (z= 0.1, 1, 2) are compared with the GALFORM semi-analytic model of galaxy formation. GALFORM predicts an overall SFRD as a function of stellar mass in reasonable agreement with the observations. The star formation time-scales inferred from 1/SSFR also give reasonable overall agreement, with the agreement becoming worse at the lowest and highest masses. The models do not reproduce the SSFR upturn seen in our data at low masses, where the effects of extinction and active galactic nuclei feedback should be minimal and the comparison should be most robust.
Available from: Vladimir Avila-Reese
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ABSTRACT: (Abridged) By means of high-resolution cosmological simulations in the
context of the LCDM scenario, the specific star formation rate (SSFR=SFR/Ms, Ms
is the stellar mass)--Ms and stellar mass fraction (Fs=Ms/Mh, Mh is the halo
mass)--Ms relations of low-mass galaxies (2.5< Mh/10^10 Msun <50 at redshift
z=0) at different epochs are predicted. The Hydrodynamics ART code was used and
some variations of the sub-grid parameters were explored. Most of simulated
galaxies, specially those with the highest resolutions, have significant disk
components and their structural and dynamical properties are in reasonable
agreement with observations of sub-M* field galaxies. However, the SSFRs are
5-10 times smaller than the averages of several (compiled and homogenized here)
observational determinations for field blue/star-forming galaxies at z<0.3 (at
low masses, most of observed field galaxies are actually blue/star-forming).
This inconsistency seems to remain even at z~1.5 though less drastic. The Fs of
simulated galaxies increases with Mh as semi-empirical inferences show, but in
absolute values the former are ~5-10 times larger than the latter at z=0; this
difference increases probably to larger factors at z~1-1.5. The inconsistencies
reported here imply that simulated low-mass galaxies (0.2<Ms/10^9 Msun <30 at
z=0) assembled their stellar masses much earlier than observations suggest.
This confirms the predictions previously found by means of LCDM-based models of
disk galaxy formation and evolution for isolated low-mass galaxies (Firmani &
Avila-Reese 2010), and highlight that our implementation of astrophysics into
simulations and models are still lacking vital ingredients.
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ABSTRACT: We compare the galaxy population in the Virgo, Fornax, Coma and Perseus cluster to a state-of-the-art semi-analytic model,
focusing on the regime of dwarf galaxies with luminosities from approximately 108 to 109 L⊙. We find that the number density profiles of dwarfs in observed clusters are reproduced reasonably well, and that the red
fractions of model clusters provide a good match to Coma and Perseus. On the other hand, the red fraction among dwarf galaxies
in Virgo is clearly lower than in model clusters. We argue that this is mainly caused by the treatment of environmental effects
in the model. This explanation is supported by our finding that the colours of central (‘field’) dwarf galaxies are reproduced
well, in contrast to previous claims. Finally, we find that the dwarf-to-giant ratio in model clusters is too high. This may
indicate that the current model prescription for tidal disruption of faint galaxies is still not efficient enough.
Available from: Simon P. Driver
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ABSTRACT: We determine the low-redshift field galaxy stellar mass function (GSMF) using an area of 143 deg2 from the first three years of the Galaxy And Mass Assembly (GAMA) survey. The magnitude limits of this redshift survey are
r < 19.4 mag over two-thirds and 19.8 mag over one-third of the area. The GSMF is determined from a sample of 5210 galaxies
using a density-corrected maximum volume method. This efficiently overcomes the issue of fluctuations in the number density
versus redshift. With H0= 70 km s−1 Mpc−1, the GSMF is well described between 108 and 1011.5 M⊙ using a double Schechter function with , , α1=−0.35, and α2=−1.47. This result is more robust to uncertainties in the flow-model corrected redshifts than from the shallower Sloan Digital
Sky Survey main sample (r < 17.8 mag). The upturn in the GSMF is also seen directly in the i-band and K-band galaxy luminosity functions. Accurately measuring the GSMF below 108 M⊙ is possible within the GAMA survey volume but as expected requires deeper imaging data to address the contribution from low
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