The Infrared Luminosity Function of Galaxies at Redshifts z = 1 and z ~ 2 in the GOODS Fields

By K. Caputi, G. Lagache, Lin Yan, H. Dole, N. Bavouzet, É. Le Floc'h, P. Choi, G. Helou, Naveen A. Reddy. 2007

267 citations recorded by the source corpus.

We present the rest-frame 8 μm LF at redshifts z = 1 and ~2, computed from Spitzer 24 μm-selected galaxies in the GOODS fields over an area of 291 arcmin2. Using classification criteria based on X-ray data and IRAC colors, we identify the AGNs in our sample. The rest-frame 8 μm LFs for star-forming galaxies at redshifts z = 1 and ~2 have the same shape as at z ~ 0, but with a strong positive luminosity evolution. The number density of star-forming galaxies with log10(νL) > 11 increases by a factor >250 from redshift z ~ 0 to 1 and is basically the same at z = 1 and ~2. The resulting rest-frame 8 μm luminosity densities associated with star formation at z = 1 and ~2 are more than 4 and 2 times larger than at z ~ 0, respectively. We also compute the total rest-frame 8 μm LF for star-forming galaxies and AGNs at z ~ 2 and show that AGNs dominate its bright end, which is well described by a power law. Using a new calibration based on Spitzer star-forming galaxies at 0 < z < 0.6 and validated at higher redshifts through stacking analysis, we compute the bolometric IR LF for star-forming galaxies at z = 1 and ~2. We find that the respective bolometric IR luminosity densities are (1.2 ± 0.2) × 109 and (6.6) × 108 L☉ Mpc-3, in agreement with previous studies within the error bars. At z ~ 2, around 90% of the IR luminosity density associated with star formation is produced by luminous and ultraluminous IR galaxies, with the two populations contributing in roughly similar amounts. Finally, we discuss the consistency of our findings with other existing observational results on galaxy evolution.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/c7c922530103170f1f0c7e519a3f5a68fa68aa1a

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In Astronomy and Astrophysics

1. P. Hopkins
2. L. Hernquist
3. R. Dav'e
4. R. Somerville
5. D. M. Alexander
6. P. V. van Dokkum
7. A. Dekel
8. C. Conroy

In Instrumentation

1. P. Hopkins
2. L. Hernquist
3. P. V. van Dokkum
4. R. Dav'e
5. C. Conroy
6. M. Franx
7. A. Dekel
8. R. Somerville

Citations in the corpus

• Evolution of the dusty infrared luminosity function from z = 0 to z = 2.3 using observations from Spitzer (2011, methodology): “Empty triangles represent the rest-frame 8µm LF derived by Caputi et al. (2007) atz ∼ 2.”
• Short-Duration Gamma-Ray Bursts (2013, background): “The expected U/LIRG fraction for a progenitor population that tracks stellar mass alone is∼ 1% (Caputi et al. 2006), while for progenitors that track only star formation it is∼ 25% (Le Floc’h et al. 2005, Caputi et al. 2007).”
• Galaxy luminosities, stellar masses, sizes, velocity dispersions as a function of morphological type (2009, methodology): “…the SFR over the range 2 <z < 6 using deep optical and infrared data from Advanced Camera for Surveys (ACS)/Near Infrared Camera and Multi-Object Spectrometer (NICMOS) in the GOODS fields, UBVi dropout Lyman break galaxies and ultraluminous infrared galaxies (ULIRGs) data from Caputi et al. (2007).”
• EXTRAGALACTIC MILLIMETER-WAVE SOURCES IN SOUTH POLE TELESCOPE SURVEY DATA: SOURCE COUNTS, CATALOG, AND STATISTICS FOR AN 87 SQUARE-DEGREE FIELD (2009, background): “IRAS, however, detected mostly low-redshift (z < 1) objects, and these relatively rare and nearby sources contributed only a small fraction of the CIB (Le Floc’h et al. 2005; Caputi et al. 2007), indicating that the bulk of CIB sources are at high redshift.”
• Semi-analytic modelling of the extragalactic background light and consequences for extragalactic gamma-ray spectra: Modelling of the EBL and gamma-ray spectra (2012, background): “Total IR luminosity: observational estimates of the IR emissivity are from Caputi et al. (2007) (open blue pentagons), Reddy et al. (2008) (green circles), Rodighiero et al. (2010) (purple stars) and Le Floc’h et al. (2005) (red crosses). not affected by any further interactions except for…”
• Characterization of Scuba-2 450 μm and 850 μm selected galaxies in the COSMOS field (2013, methodology): “We then assume an underlying distribution or density of galaxies in z–LIR–λpeak space, as given by integratedinfrared luminosity functions (Le Floc’h et al. 2005; Caputi et al. 2007; Magnelli et al. 2011; Casey et al. 2012a; Gruppioni et al. 2013).”
• GOODS–Herschel: an infrared main sequence for star-forming galaxies (2011, background): “…revealed that the contribution to the cosmic SFR density of even more active objects, the ultraluminous IR galaxies (ULIRGs,LIR≥1012 L⊙), was as important as for LIRGs (Chapman et al. 2005, Papovich et al. 2007, Caputi et al. 2007, Daddi et al. 2007a, Magnelli et al. 2009, 2011).”
• Cosmic evolution of submillimeter galaxies and their contribution to stellar mass assembly (2009, unknown): “…0.400 0.2091 0.0357 0.0357 mid-IR Reddy et al. (2008) 3.050 0.350 0.1124 0.0211 0.0211 mid-IR Reddy et al. (2008) 1.000 0.100 0.2000 0.0300 0.0300 mid-IR Caputi et al. (2007) 2.000 0.300 0.1100 0.0200 0.0200 mid-IR Caputi et al. (2007) 0.450 0.150 0.2750 0.0220 0.0220 mid-IR Santini et al.…”
• THE SINS SURVEY: MODELING THE DYNAMICS OF z ∼ 2 GALAXIES AND THE HIGH-z TULLY–FISHER RELATION (2009, background): “These represent the bulk of the cosmic star formation activity and stellar mass density at these redshifts (Reddy et al. 2005; Rudnick et al. 2006; Grazian et al. 2007, Caputi et al. 2007).”
• The HDUV Survey: A Revised Assessment of the Relationship between UV Slope and Dust Attenuation for High-redshift Galaxies (2017, background): “…of highly dust-obscured galaxies compared to intrinsically faint galaxies (e.g., as inferred from the shapes of the UV and IR luminosity functions; Caputi et al. 2007; Reddy et al. 2008; Reddy & Steidel 2009; Magnelli et al. 2013) implies that in a numberweighted sense, the mean bolometric…”
• MID-INFRARED PROPERTIES OF NEARBY LUMINOUS INFRARED GALAXIES. I. SPITZER INFRARED SPECTROGRAPH SPECTRA FOR THE GOALS SAMPLE (2013, background): “…universe, their comoving number density increases by more than 100 times from the current epoch to z∼1, (Le Floc’h et al. 2005; Magnelli et al. 2009) until LIRGs dominate the total IR energy density at redshifts of z∼1-2 when star formation in the universe was at its peak (Caputi et al. 2007).”
• A physical model for z∼ 2 dust-obscured galaxies (2009, background): “…infrared galaxies (ULIRGs; LIR > 1012 L ) at z ∼ 2 appear to contribute substantially to the infrared luminosity density (Pérez-Gonzélez et al. 2005; Caputi et al. 2007; Reddy et al. 2008; Hopkins et al. 2010; Hopkins & Hernquist 2010), and the , and the z > 0.7 SFR density (Le Floc’h et al.…”
• DUST OBSCURATION AND METALLICITY AT HIGH REDSHIFT: NEW INFERENCES FROM UV, Hα, AND 8 μm OBSERVATIONS OF z ∼ 2 STAR-FORMING GALAXIES (2010, methodology): “Excepting our present determination and that of Rigby et al. (2008), all the relations shown in Figure 5 were calibrated on galaxies at z < 0.7.12 The calibration presented by Caputi et al. (2007) is in rough agreement with our relationship within the rms dispersion of the latter.”
• UV-CONTINUUM SLOPES AT z  ∼  4–7 FROM THE HUDF09+ERS+CANDELS OBSERVATIONS: DISCOVERY OF A WELL-DEFINED UV COLOR–MAGNITUDE RELATIONSHIP FOR z ⩾ 4 STAR-FORMING GALAXIES (2011, methodology): “Since the 70µm and 24µm data that Magnelli et al. (2011) utilise are significantly deeper than that used by Caputi et al. (2007) and allow for a self-consistent correction to the total bolometric luminosity, the Magnelli et al. (2011) SFR density estimate represents a noteworthy improvement on the…”
• A Significant Population of Very Luminous Dust-Obscured Galaxies at Redshift z ~ 2 (2008, methodology): “Converting from observed 24µm flux densities to restframe far-infrared or bolometric luminosities is notoriously uncertain and has a checkered history (e.g., see §6 of Caputi et al. 2007, for a recent summary).”
• GeV OBSERVATIONS OF STAR-FORMING GALAXIES WITH THE FERMI LARGE AREA TELESCOPE (2012, result): “…et al. (2010) integrated over IR luminosity and redshift are consistent with the cosmic SFR history estimated from analyses of IR observations by Pérez-González et al. (2005), Le Floc’h et al. (2005), and Caputi et al. (2007), and that estimated with far-ultraviolet data (Tresse et al. 2007).”
• The Herschel* PEP/HerMES luminosity function - I. Probing the evolution of PACS selected Galaxies to z ≃ 4 (2013, methodology): “With Spitzer 24-µm data, it was possible to study the evolution of the mid-IR LF up to z∼2 (e.g. Le Floc’h et al. 2005, Caputi et al. 2007, Rodighiero et al. 2010a), while, even with the deepest Spitzer Space Telescope (Werner et al. 2004) 70-µm data, only z∼1–1.2 could be reached in the far-IR…”
• GOODS-HERSCHEL AND CANDELS: THE MORPHOLOGIES OF ULTRALUMINOUS INFRARED GALAXIES AT z ∼ 2 (2011, background): “…with Spitzer and now Herschel have shown that while rare locally, (U)LIRGs were once much more common and even dominated the cosmic star formation rate at z > 1 (e.g., Floc’h et al. 2005; Caputi et al. 2007; Magnelli et al. 2009; Magnelli et al. 2011; Béthermin et al. 2011; Murphy et al. 2011).”
• EXPLAINING THE [C ii]157.7 μm DEFICIT IN LUMINOUS INFRARED GALAXIES—FIRST RESULTS FROM A HERSCHEL/PACS STUDY OF THE GOALS SAMPLE (2013, background): “…holes since (1) IR-luminous galaxies comprise the bulk of the cosmic infrared background and dominate star-formation activity between 0.5 < z < 2 (Caputi et al. 2007; Magnelli et al. 2011; Murphy et al. 2011; Berta et al. 2011) and (2) AGN activity may preferentially occur during episodes of…”