Star Formation in AEGIS Field Galaxies since z = 1.1: Staged Galaxy Formation and a Model of Mass-dependent Gas Exhaustion

By K. Noeske, S. Faber, B. Weiner, D. Koo, Joel R. Primack, A. Dekel, C. Papovich, Christopher J. Conselice, É. Le Floc'h, G. Rieke and 13 more. 2007

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We analyze star formation (SF) as a function of stellar mass (M*) and redshift z in the All-Wavelength Extended Groth Strip International Survey, for star-forming field galaxies with M* ≳ 1010 M☉ out to z = 1.1. The data indicate that the high specific SF rates (SFRs) of many less massive galaxies do not represent late, irregular or recurrent, starbursts in evolved galaxies. They rather seem to reflect the onset (initial burst) of the dominant SF episode of galaxies, after which SF gradually declines on gigayear timescales to z = 0 and forms the bulk of a galaxy's M*. With decreasing mass, this onset of major SF shifts to decreasing z for an increasing fraction of galaxies (staged galaxy formation). This process may be an important component of the "downsizing" phenomenon. We find that the predominantly gradual decline of SFRs described by Noeske et al. can be reproduced by exponential SF histories (τ models), if less massive galaxies have systematically longer e-folding times τ, and a later onset of SF (zf). Our model can provide a first parameterization of SFR as a function of M* and z, and quantify mass dependences of τ and zf , from direct observations of M* and SFRs up to z > 1. The observed evolution of SF in galaxies can plausibly reflect the dominance of gradual gas exhaustion. The data are also consistent with the history of cosmological accretion onto dark matter halos.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/9fe1918a2767e425566dc7a4ec50fad3e6e37aca

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Citations in the corpus

Galaxy and Mass Assembly (GAMA): the star formation rate dependence of the stellar initial mass function (2011, methodology): “The massdoubling time, used to calculate the td values for the highest SFR sub-group of galaxies, is defined as td = M∗/(0.5 × SFR) (Noeske et al. 2007), and provides a time-scale within which the current SFR would produce the observed stellar mass (M∗).”
Evolution of the dusty infrared luminosity function from z = 0 to z = 2.3 using observations from Spitzer (2011, background): “Atz< 1 the decrease of the SFR density might be driven by a gradual gas exhaustion as suggested by the continuous decrease of the SFR vs M⋆ relation in this redshift range (Noeske et al. 2007; Elbaz et al. 2007).”
Dusty Star Forming Galaxies at High Redshift (2014, background): “…defined in observational terms, several works have claimed that SFGs can be broadly described as sitting on the normal galaxy ‘main sequence’ (Noeske et al., 2007b) and are mostly not made up of secularly evolving, disk galaxies (Shapiro et al., 2008; Förster Schreiber et al., 2009;…”
WHAT DOES A SUBMILLIMETER GALAXY SELECTION ACTUALLY SELECT? THE DEPENDENCE OF SUBMILLIMETER FLUX DENSITY ON STAR FORMATION RATE AND DUST MASS (2010, background): “…onto galaxies at high redshift (e.g., Kereš et al. 2005; Dekel et al. 2009), gas fractions (Erb et al. 2006; Tacconi et al. 2006, 2010; Daddi et al. 2010) and star formation rates (SFRs; Daddi et al. 2007; Noeske et al. 2007a, 2007b) of galaxies at fixed galaxy mass increase rapidly with redshift.”
The origin of the galaxy mass-metallicity relation and implications for galactic outflows (2007, methodology): “It is more likely star formation is delayed in low-mass galaxies by an effect that our model does not account for (Noeske et al. 2007b).”
A survey of molecular gas in luminous sub-millimetre galaxies (2012, background): “Some authors have defined a ‘main sequence’ of star formation (defined as SFR/M∗ ∼ Mα∗ (1 + z)β ; Daddi et al. 2007; Noeske et al. 2007; Schiminovich et al. 2007; Rodighiero et al. 2010).”
IMAGING THE MOLECULAR GAS IN A SUBMILLIMETER GALAXY AT z = 4.05: COLD MODE ACCRETION OR A MAJOR MERGER? (2010, background): “…indicating ‘downsizing’ in galaxy formation, with active star formation being preferentially quenched in more massive galaxies over cosmic time (Noeske et al. 2007, 2009; Zheng et al. 2007; Pannella et al. 2009), as well as the direct observation of old stellar populations in early type…”
THE STAR FORMATION HISTORY OF MASS-SELECTED GALAXIES IN THE COSMOS FIELD (2010, methodology): “As it was claimed (e.g. Noeske et al. 2007b) a tight correlation of SFR and stellar mass disfavors star formation histories (SFHs) of individual normal galaxies that are mainly driven by stochastic processes, such as mergers.”
THE MASS–METALLICITY AND LUMINOSITY–METALLICITY RELATIONS FROM DEEP2 AT z ∼ 0.8 (2010, background): “Noeske et al. (2007b) show that the star formation as a whole was higher at z ∼ 1 and that the star formation rate gradually declines with galaxies spending 67% of their lifetime since z = 1 with SFR that are within a factor 2 of their average and 95% of their time within a factor of 4.”
DEMOGRAPHICS AND PHYSICAL PROPERTIES OF GAS OUTFLOWS/INFLOWS AT 0.4 < z < 1.4 (2012, methodology): “M∗ main sequence (Noeske et al. 2007; Elbaz et al. 2007) fitted to the GALEX-detected subsample of 6102 DEEP2 galaxies with stellar mass measurements.”
Constraining the properties of AGN host galaxies with spectral energy distribution modelling (2015, background): “Addtionally, the slope and redshift evolution of the MS normalization has been discussed in context of feedback processes and gas exhaustion with cosmic time, respectively (e.g. Noeske et al. 2007a; Zheng et al. 2007; Tacconi et al. 2013; Guo et al. 2013).”
THE DEEP2 GALAXY REDSHIFT SURVEY: DESIGN, OBSERVATIONS, DATA REDUCTION, AND REDSHIFTS (2012, methodology): “Most star-formation at z ∼ 1 is taking place in normal galaxies, not in merger-triggered starbursts (Noeske et al. 2007b, Harker 2008).”
Galaxy and Mass Assembly (GAMA): ugriz galaxy luminosity functions (2011, background): “Noeske et al. (2007) have suggested that the first major burst of star formation is delayed to later times for low mass galaxies, contributing to the downsizing phenomenon.”
A Theoretical Interpretation of the Black Hole Fundamental Plane (2007, background): “This is, of course, a nonunique parameterization of the star formation history, butnevertheless appears to be a reasonable description of average stellar populations (e.g., Noeske et al. 2007).”
The galaxy stellar mass-star formation rate relation: evidence for an evolving stellar initial mass function? (2007, methodology): “Another scenario that has been shown to reproduce M∗–SFR evolution is the staged galaxy formation model of Noeske et al. (2007b).”
The effect of gas fraction on the morphology and time-scales of disc galaxy mergers (2009, background): “These galaxies also have higher star-formation rates per unit mass (Noeske et al. 2007) and similar or smaller effective radii (Barden et al. 2005; Melbourne et al. 2007) suggestive of higher gas densities than local disc galaxies.”
Rapid Formation of Exponential Disks and Bulges at High Redshift from the Dynamical Evolution of Clump-Cluster and Chain Galaxies (2007, background): “Noeske et al. (2007) reach a similar conclusion based on the distribution of star formation rates over mass and time.”
The DEEP2 Galaxy Redshift Survey: the role of galaxy environment in the cosmic star formation history (2007, background): “For instance, Bauer et al. (2005) and (Noeske et al. 2007b) find that star–forming galaxies populate a tight sequence in SFR and stellar mass at z < 1.2, with a limited range in SFR at a given stellar mass and redshift (Noeske et al. 2007b).”