Spitzer View on the Evolution of Star-forming Galaxies from z = 0 to z ~ 3

By P. Pérez-González, G. Rieke, E. Egami, A. Alonso-Herrero, H. Dole, C. Papovich, M. Blaylock, J. Jones, M. Rieke, J. Rigby and 4 more. 2005

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We use a 24 μm-selected sample containing more than 8000 sources to study the evolution of star-forming galaxies in the redshift range from z = 0 to z ~ 3. We obtain photometric redshifts for most of the sources in our survey using a method based on empirically built templates spanning from ultraviolet to mid-infrared wavelengths. The accuracy of these redshifts is better than 10% for 80% of the sample. The derived redshift distribution of the sources detected by our survey peaks at around z = 0.6-1.0 (the location of the peak being affected by cosmic variance) and decays monotonically from z ~ 1 to z ~ 3. We have fitted infrared luminosity functions in several redshift bins in the range 0 < z ≲ 3. Our results constrain the density and/or luminosity evolution of infrared-bright star-forming galaxies. The typical infrared luminosity (L*) decreases by an order of magnitude from z ~ 2 to the present. The cosmic star formation rate (SFR) density goes as (1 + z)4.0±0.2 from z = 0 to 0.8. From z = 0.8 to z ~ 1.2, the SFR density continues rising with a smaller slope. At 1.2 < z ≲ 3, the cosmic SFR density remains roughly constant. The SFR density is dominated at low redshift (z ≲ 0.5) by galaxies that are not very luminous in the infrared (LTIR < 1011 L☉, where LTIR is the total infrared luminosity, integrated from 8 to 1000 μm). The contribution from luminous and ultraluminous infrared galaxies (LTIR > 1011 L☉) to the total SFR density increases steadily from z ~ 0 up to z ~ 2.5, forming at least half of the newly born stars by z ~ 1.5. Ultraluminous infrared galaxies (LTIR > 1012 L☉) play a rapidly increasing role for z ≳ 1.3.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/f658663774209a4aca05e4ab8c9500205459655a

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Citations in the corpus

Herschel PEP/HerMES: the redshift evolution (0 ≤ z ≤ 4) of dust attenuation and of the total (UV+IR) star formation rate density (2013, background): “4 suggests a flattening of the total SFRD up to z ∼ 3 (Chary & Elbaz(2001), Perez-Gonzalez et al.(2005), Le Floc’h et al.(2005), Franceschini et al.(2010)) where the UV data favour a peak followed by a decrease.”
FIREWORKS U38-to-24 μm Photometry of the GOODS Chandra Deep Field-South: Multiwavelength Catalog and Total Infrared Properties of Distant Ks-selected Galaxies (2008, methodology): “We note that several other authors developed similar algorithms to reduce the effects of confusion (Pérez-González et al. 2005, 2008; G06a).”
Mass, metal, and energy feedback in cosmological simulations (2007, methodology): “The typical mass outflow rate reduces with time for two reasons: First, the star formation rates are lower owing to lower accretion rates from the IGM, as discussed in SH03b and OD06 and as observed by Pérez-González et al. (2005); Caputi et al. (2006); Papovich et al. (2006).”
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): “…(SF) occurring earlier in massive galaxies than in less massive systems (e.g., Guzma´n et al. 1997; Brinchmann & Ellis 2000; Juneau et al. 2005; Bauer et al. 2005; Bell et al. 2005; Pérez-Gonza´lez et al. 2005; Feulner et al. 2005; Papovich et al. 2006; Caputi et al. 2006; Reddy et al. 2006).”
The Infrared Luminosity Function of Galaxies at Redshifts z = 1 and z ~ 2 in the GOODS Fields (2007, methodology): “…literature, and based on different datasets: ISO mid-IR (Flores et al. 1999; left-hand-pointing triangles), Spitzer mid-IR (Le Floc’h et al. 2005 and Pérez-González et al. 2005; right-hand-pointing triangle and asterisks, respectively), sub-millimetre (Barger et al. 2000 and Chapman et al. 2005;…”
The evolution of stellar mass and the implied star formation history (2008, neutral): “Radio/submillimetre/FIR (red): Flores et al. (1999), Barger, Cowie & Richards (2000), Condon, Cotton & Broderick (2002), Sadler et al. (2002), Serjeant, Gruppioni & Oliver (2002), Machalski & Godlowski (2000), Haarsma et al. (2000), Condon (1989), Pérez-González et al. (2005).”
Outflows in Infrared-Luminous Starbursts at z < 0.5. I. Sample, Na I D Spectra, and Profile Fitting (2005, background): “Early results from Spitzer indicate that ULIRGs may contain half of the forming stars at z ¼ 2 (Perez-Gonzalez et al. 2005).”
The Cosmic Infrared Background Resolved by Spitzer. Contributions of Mid-Infrared Galaxies to the Far-Infrared Background. (2006, background): “Our 24 µm sample is almost complete in flux (80% completeness down to S24 = 80µJy and 50% at 60µJy), and the physical properties of S24 ≥ 80µJy galaxies have been extensively studied (Le Floc’h et al., 2004; Pérez-González et al., 2005; Le Floc’h et al., 2005; Caputi et al., 2006).”
HISTORY OF GALAXY INTERACTIONS AND THEIR IMPACT ON STAR FORMATION OVER THE LAST 7 Gyr FROM GEMS (2009, background): “…since z < 1 is of great astrophysical interest, given that the cosmic SFR density is claimed to decline by a factor of 4 to 10 since z ∼ 1 (e.g., Lilly et al. 1996; Ellis et al 1996; Flores et al. 1999; Haarsma et al. 2000; Hopkins 2004; Pérez-González et al. 2005; Le Floc’h et al. 2005).”
A POPULATION OF MASSIVE, LUMINOUS GALAXIES HOSTING HEAVILY DUST-OBSCURED GAMMA-RAY BURSTS: IMPLICATIONS FOR THE USE OF GRBs AS TRACERS OF COSMIC STAR FORMATION (2013, background): “…10 12 L⊙) or submillimeter galaxies (SMGs) are known (Berger et al. 2003; Tanvir et al. 2004), even though these systems contribute substantially to, and may dominate, the cosmic SFR at higher redshifts (z & 1.5; e.g., Smolčić et al. 2009; Pérez-González et al. 2005; Micha lowski et al. 2010).”
Mid-Infrared Spectral Diagnosis of Submillimeter Galaxies (2007, background): “…with the Infrared Space Observatory (ISO) and the Spitzer Space Telescope (hereafter Spitzer) have shown that about 70% of the comoving star formation rate density (SFRD) at 0:5 < z < 3 is obscured by dust (Chary & Elbaz 2001, hereafter CE01; Le Floc’h et al. 2005; Pérez-González et al. 2005).”
VLT/VIMOS integral field spectroscopy of luminous and ultraluminous infrared galaxies: 2D kinematic properties (2013, neutral): “Although (U)LIRGs are rare in the local universe (e.g., Lagache et al. 2005), they are much more numerous at high-z and are relevant contributors to the whole past star formation beyond z∼ 1 (e.g., Le Floc’h et al. 2005; Pérez-González et al. 2005, 2008).”
Astrophysical and cosmological information from large-scale submillimetre surveys of extragalactic sources (2007, result): “2 of Pérez-González et al. 2005 and Fig.”
CONNECTING THE GAMMA RAY BURST RATE AND THE COSMIC STAR FORMATION HISTORY: IMPLICATIONS FOR REIONIZATION AND GALAXY EVOLUTION (2011, neutral): “…and observations by Wolf et al. (2003), Bouwens et al. (2003a,b), Bunker et al. (2004), Ouchi et al. (2004), Arnouts et al. (2005), Le Floc’h et al. (2005), Pérez-González et al. (2005), Schiminovich et al. (2005), Bouwens & Illingworth (2006), Hanish et al. (2006), and Thompson et al. (2006).”
The Star Formation Rate Density and Dust Attenuation Evolution over 12 Gyr with the VVDS Surveys (2011, background): “Conversely, Tresse et al. (2007) derived them by comparing the dust corrected 12µm (Pérez-González et al. 2005) and Hα (Tresse & Maddox 1998; Tresse et al. 2002) SFRDs to their uncorrected FUV-derived VVDS Deep SFRDs.”