On the Evolution of Star-forming Galaxies

By Andrew M. Hopkins. 2004

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The evolution in the comoving space density of the global average galaxy star formation rate (SFR) out to a redshift around unity is well established. Beyond z ≈ 1 there is growing evidence that this evolution is flat or even increasing, contrary to early indications of a turnover. Some recent analyses of z ≈ 6 photometric dropouts are suggestive of a decline from z = 3 to z ≈ 6, but there is still very little constraint on the extent of dust obscuration at such high redshifts. In less than a decade, numerous measurements of galaxy SFR density spanning z = 0 to as high as z ≈ 6 have rapidly broadened our understanding of galaxy evolution, and a summary of existing SFR density measurements is presented here. This global star formation history compilation is found to be consistent to within factors of about 3 over essentially the entire range 0 < z ≲ 6, and it can be used to constrain the evolution of the luminosity function (LF) for star-forming galaxies. The LF evolution for star-forming galaxies has been previously explored using optical source counts, as well as radio source counts at 1.4 GHz, and a well-known degeneracy between luminosity evolution [L ∝ (1 + z)Q] and density evolution [ϕ ∝ (1 + z)P] is found. Combining the constraints from the global SFR density evolution with those from the 1.4 GHz radio source counts at submillijansky levels allows this degeneracy to be broken and a best-fitting evolutionary form to be established. The preferred evolution in a H0 = 70, ΩM = 0.3, ΩΛ = 0.7 cosmology from these combined constraints is Q = 2.70 ± 0.60, P = 0.15 ± 0.60.

Subfields: Astronomy and Astrophysics, Instrumentation

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Citations in the corpus

The evolution of massive black holes and their spins in their galactic hosts (2012, background): “More specifically, emission from massive stars, which are short-lived compared to the typical star-formation timescales, can be used to extrapolate the IMF and obtain theSFR (see Hopkins (2004, 2007); Hopkins & Beacom (2006, 2008) for compilations of recent data).”
A semi-empirical simulation of the extragalactic radio continuum sky for next generation radio telescopes (2008, background): “More recent determinations of the evolution of the radio luminosity function of star-forming galaxies are consistent with this, mostly finding luminosity evolution of the form(1 + z)Q (Q = 2 − 3) and negligible density evolution (e.g. Seymour et al. 2004;Hopkins 2004).”
The evolution of stellar mass and the implied star formation history (2008, methodology): “Using the compilation of HB06 (an updated version of Hopkins 2004) we compare a range of instantaneous measurements to our SFH, shown in Fig.”
THE HUBBLE SPACE TELESCOPE WIDE FIELD CAMERA 3 EARLY RELEASE SCIENCE DATA: PANCHROMATIC FAINT OBJECT COUNTS FOR 0.2–2 μm WAVELENGTH (2010, background): “The critical epoch for the assembly of massive galaxies appears to be the ∼4 Gyr span from redshift z'3 to z'1, where also the cosmic star-formation history seems to have peaked (Madau, Pozzetti, & Dickinson 1998; Hopkins 2004; Hopkins & Beacom 2006).”
Gaseous Galaxy Halos (2012, background): “The sources discussed below will provide additional fuel, but low redshift spiral galaxies may also gradually decrease their SFR’s (e.g., Madau et al., 1998; Hopkins, 2004).”
Star Formation and the Growth of Stellar Mass (2007, background): “…evolution of cosmic star formation rate (e.g., Madau et al. 1996; Lilly et al. 1996; Steidel et al. 1999; Flores et al. 1999; Haarsma et al. 2000; Hopkins 2004; Le Floc’h et al. 2005) and the buildup of stellar mass (e.g., Brinchmann& Ellis 2000; Cole et al. 2001; Dickinson et al. 2003; Rudnick…”
Cosmological simulations of intergalactic medium enrichment from galactic outflows (2006, background): “Data points shown are from a compilation by Hopkins (2004).”
Star Formation in AEGIS Field Galaxies since z = 1.1: The Dominance of Gradually Declining Star Formation, and the Main Sequence of Star-forming Galaxies (2007, background): “Theglobal SFR density has also11M p 10 M∗ , decreased by a factor of 3 over this same interval (Hopkins 2004, eq.”
On the Normalization of the Cosmic Star Formation History (2006, methodology): “These data are reproduced from Figure 1 of Hopkins (2004), and use their “common” obscuration correction where necessary.”
ON THE STELLAR POPULATIONS AND EVOLUTION OF STAR-FORMING GALAXIES AT 6.3 < z ⩽ 8.6 (2009, background): “…the integrated galaxy star–formation rate (SFR) density, which increases by roughly an order of magnitude over the redshift rangez∼ 0 to 1, and reaches a peak at some point between 1.5. z. 3 (e.g., Lilly et al. 1996; Steidel et al. 1999; Dickinson et al. 2003; Hopkins 2004; Reddy & Steidel 2009).”
The galaxy stellar mass-star formation rate relation: evidence for an evolving stellar initial mass function? (2007, methodology): “5 shows the cosmic SFH with data points compiled by Hopkins (2004), and the fit by Hopkins & Beacom (2006).”
UV CONTINUUM SLOPE AND DUST OBSCURATION FROM z ∼ 6 TO z ∼ 2: THE STAR FORMATION RATE DENSITY AT HIGH REDSHIFT (2009, background): “20 These dust corrections are much more modest than have occasionally been assumed to calculate the total star formation rate density at early times, e.g., the factor of ∼ 8 adopted by Giavalisco et al. (2004b) or the factor of ∼3 adopted by Hopkins (2004) for their common obscuration correction.”
The Calibration of Mid-Infrared Star Formation Rate Indicators (2007, background): “…to find general tools to mitigate the effects of dust on this important SFR indicator (e.g., Calzetti, Kinney & Storchi–Bergmann 1994; Kennicutt 1998a; Meurer, Heckman & Calzetti 1999; Hopkins et al. 2001; Sullivan et al. 2001; Buat et al. 2002, 2005; Bell 2003; Hopkins 2004; Salim et al. 2007).”
Cosmic Star Formation History and Its Dependence on Galaxy Stellar Mass (2004, unknown): “Despite these challenges Hopkins (2004) recently compiled results from 33 studies over the rangez = 0 to z ≈ 6.”
Galaxy and Mass Assembly (GAMA): ugriz galaxy luminosity functions (2011, methodology): “Looking back in time with increasing redshift, the star formation rate appears to peak at redshift z ' 1, above which it plateaus and slowly declines towards z ' 6 (Cole et al. 2000; Hopkins 2004; Hopkins & Beacom 2006; Yuksel et al. 2008; Kistler et al. 2009).”