Evolution of the dusty infrared luminosity function from z = 0 to z = 2.3 using observations from Spitzer

By B. Magnelli, D. Elbaz, R. Chary, Mark Dickinson, D. L. Borgne, D. Frayer, C. Willmer. 2011

266 citations recorded by the source corpus.

Aims. We derive the evolution of the infrared luminosity function (LF) over the last 4/5ths of cosmic time using deep 24 and 70 μm imaging of the GOODS North and South fields. Methods. We use an extraction technique based on prior source positions at shorter wavelengths to build the 24 and 70 μm source catalogs. The majority (93%) of the sources have a spectroscopic (39%) or a photometric redshift (54%) and, in our redshift range of interest (i.e., 1.3 < z < 2.3) ~20% of the sources have a spectroscopic redshift. To extend our study to lower 70 μm luminosities we perform a stacking analysis and we characterize the observed L_(24/(1 + z)) vs. L_(70/(1 + z)) correlation. Using spectral energy distribution (SED) templates which best fit this correlation, we derive the infrared luminosity of individual sources from their 24 and 70 μm luminosities. We then compute the infrared LF at z ~ 1.55 ± 0.25 and z ~ 2.05 ± 0.25. Results. We observe the break in the infrared LF up to z ~ 2.3. The redshift evolution of the infrared LF from z = 1.3 to z = 2.3 is consistent with a luminosity evolution proportional to (1 + z)^(1.0 ± 0.9) combined with a density evolution proportional to (1 + z)^9−1.1 ± 1.5). At z ~ 2, luminous infrared galaxies (LIRGs: 10^(11)L_⊙ < L_(IR) < 10^(12) L_⊙) are still the main contributors to the total comoving infrared luminosity density of the Universe. At z ~ 2, LIRGs and ultra-luminous infrared galaxies (ULIRGs: 10^(12)L_⊙ < L_(IR)) account for ~49% and ~17% respectively of the total comoving infrared luminosity density of the Universe. Combined with previous results using the same strategy for galaxies at z < 1.3 and assuming a constant conversion between the infrared luminosity and star-formation rate (SFR) of a galaxy, we study the evolution of the SFR density of the Universe from z = 0 to z = 2.3. We find that the SFR density of the Universe strongly increased with redshift from z = 0 to z = 1.3, but is nearly constant at higher redshift out to z = 2.3. As part of the online material accompanying this article, we present source catalogs at 24 μm and 70 μm for both the GOODS-North and -South fields.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

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A UNIFIED EMPIRICAL MODEL FOR INFRARED GALAXY COUNTS BASED ON THE OBSERVED PHYSICAL EVOLUTION OF DISTANT GALAXIES (2012, background): “…increases from z=0 to 1, flattens betweenz = 1 andz = zevo = 2.5 and decreases with redshift atz > zevo, matching the infrared measurements of Magnelli et al. (2011) and Rodighiero et al. (2011), the radio measurements of Karim et al. (2011), and the optical measurements of Bouwens et al.…”
Accreting supermassive black holes in the COSMOS field and the connection to their host galaxies (2012, methodology): “The photometry of the stacked images is measured using the PSF fitting analysis presented by Magnelli et al. (2009, 2011) and using the relevant PSFs and aperture corrections of the COSMOS field (Berta et al. 2011).”
The evolution of the dust temperatures of galaxies in the SFR–M∗ plane up to z ~ 2 (2013, methodology): “S, we used the GOODS MIPS-24 μm catalogue presented in Magnelli et al. (2009, 2011) reaching a 3σ limit of 20 μJy.”
The Herschel* PEP/HerMES luminosity function - I. Probing the evolution of PACS selected Galaxies to z ≃ 4 (2013, methodology): “…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 (Magnelli et al. 2009; Patel et al. 2012) ) – though Magnelli et al. (2011) reached z∼2 through stacking.”
GOODS-HERSCHEL AND CANDELS: THE MORPHOLOGIES OF ULTRALUMINOUS INFRARED GALAXIES AT z ∼ 2 (2011, methodology): “This has been possible for small samples using MIPS 70µm imaging with Spitzer (e.g., Symeonidis et al. 2008; Kartaltepe et al. 2010a), however, MIPS 70µm lacked the sensitivity and resolution to detect anything but the most extreme systems at z ∼ 2, and by z ∼ 2, no longer probes the peak of emissio”
ALMA SPECTROSCOPIC SURVEY IN THE HUBBLE ULTRA DEEP FIELD: THE INFRARED EXCESS OF UV-SELECTED z = 2–10 GALAXIES AS A FUNCTION OF UV-CONTINUUM SLOPE AND STELLAR MASS (2016, methodology): “…energy output from UV - selected galaxies at far-infrared wavelengths is most developed over the redshift range z ∼ 0 to z ∼ 3, with increasing maturity (Reddy et al. 2008; Daddi et al. 2009; Magnelli et al. 2009, 2011, 2013; Karim et al. 2011; Cucciati et al. 2012; Álvarez-Márquez et al. 2016).”
GOODS-HERSCHEL MEASUREMENTS OF THE DUST ATTENUATION OF TYPICAL STAR-FORMING GALAXIES AT HIGH REDSHIFT: OBSERVATIONS OF ULTRAVIOLET-SELECTED GALAXIES AT z ∼ 2 (2011, methodology): “The systematic overestimation of LIR based on L8 alone has been noted before for ultraluminous infrared galaxies studied with Spitzer (Papovich et al. 2007; Daddi et al. 2007; Papovich et al. 2009; Murphy et al. 2011; Magnelli et al. 2011) and Herschel (Nordon et al. 2010; Elbaz et al. 2010).”
Planck 2013 results. XXX. Cosmic infrared background measurements and implications for star formation (2013, background): “Our derived star formation history nicely agrees with the infrared measurements of the dustobscured star-formation rate density of Rodighiero et al. (2010) A30, page 19 of 39 and Magnelli et al. (2011), up to z ∼ 2.”
THE CONTRIBUTION OF STARBURSTS AND NORMAL GALAXIES TO INFRARED LUMINOSITY FUNCTIONS AT z < 2 (2012, methodology): “…SF history has been traced by countless studies, of which we show two recent analyses relying on extinction-free tracers of SFR (Karim et al. 2011, radio continuum; Magnelli et al. 2011, far-IR emission), plus the evolution inferred from extinction-corrected UV data in Reddy & Steidel (2009).”
THE CHARACTERISTIC STAR FORMATION HISTORIES OF GALAXIES AT REDSHIFTS z ∼ 2–7 (2012, background): “…mass end, correcting for them is unlikely to alter significantly the overall slope of the SFR-M∗ relation, given that such high SFR galaxies constitute only a small fraction of the number den- sity of L∗ and fainter galaxies (e.g., Reddy et al. 2008; Reddy & Steidel 2009; Magnelli et al. 2011).”
VALIDATION OF THE EQUILIBRIUM MODEL FOR GALAXY EVOLUTION TO z ∼ 3 THROUGH MOLECULAR GAS AND DUST OBSERVATIONS OF LENSED STAR-FORMING GALAXIES (2013, background): “…this PSF-fitting technique are that it accounts for most of the blending which could be an issue in these typically crowded fields at the longer wavelengths, and allows for photometry on any specific object that is reliable across the different bands (Magnelli et al. 2009, 2011; Lutz et al. 2011).”
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).”
HerMES: deep number counts at 250 μm, 350 μm and 500 μm in the COSMOS and GOODS-N fields and the build-up of the cosmic infrared background (2012, methodology): “In the GOODS-N field, we use the 24µm catalog of Magnelli et al. (2011).”
THE HIDDEN “AGN MAIN SEQUENCE”: EVIDENCE FOR A UNIVERSAL BLACK HOLE ACCRETION TO STAR FORMATION RATE RATIO SINCE z ∼ 2 PRODUCING AN MBH–M* RELATION (2012, methodology): “The 0.5 < z < 2.5 epoch spanned by our samples correspond to the vast majority of both global star (e.g., Dickinson et al. 2003; Magnelli et al. 2011) and SMBH (e.g., Marconi et al. 2004) formation history.”
PACS Evolutionary Probe (PEP) – a Herschel key program (2011, background): “This approach resolv s most of the blending issues encountered in dense fields and allows straightforward multi-wavelength association (Magnelli et al. 2009, 2011; Roseboom et al. 2010).”
REGULARITY UNDERLYING COMPLEXITY: A REDSHIFT-INDEPENDENT DESCRIPTION OF THE CONTINUOUS VARIATION OF GALAXY-SCALE MOLECULAR GAS PROPERTIES IN THE MASS-STAR FORMATION RATE PLANE (2013, unknown): “…et al. 2013) and that the strong decline of the cosmic SFR density since z∼ 2 (e.g., Reddy & Steidel 2009, Rodighiero et al. 2010, Karim et al. 2011, Magnelli et al. 2011, Cucciati et al. 2012; and references therein) reflects the uniform SFR evolution of the majority of the SFG population…”
A Herschel view of the far-infrared properties of submillimetre galaxies (2012, methodology): “…infrared luminosities illustrates the strong evolution with redshift of the infrared galaxy population:i the local Universe such luminous infrared galaxies are very rare but their comoving space density increases by a factor∼400 betweenz∼ 0 and z∼ 2 (Magnelli et al. 2011; Chapman et al. 2005).”
Dusty Star Forming Galaxies at High Redshift (2014, background): “Further Spitzer work was presented in Caputi et al. (2007) and Magnelli et al. (2011), with similar conclusions as Le Floc’h et al. with the first extensions out to z ∼ 2.”