The 0.4 < z < 1.3 star formation history of the Universe as viewed in the far-infrared

By B. Magnelli, D. Elbaz, R. Chary, M. Dickinson, D. L. Borgne, D. Frayer, C. Willmer. 2009

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Aims. We use the deepest existing mid- and far-infrared observations (reaching ∼3 mJy at 70 μm) obtained with Spitzer in the Great Observatories Origins Deep Survey (GOODS) and Far Infrared Deep Extragalactic Legacy survey (FIDEL) fields to derive the evolution of the rest-frame 15 μm, 35 μm, and total infrared luminosity functions of galaxies spanning z < 1.3. We thereby quantify the fractional contribution of infrared luminous galaxies to the comoving star formation rate density over this redshift range. In comparison with previous studies, the present one takes advantage of deep 70 μm observations that provide a more robust infrared luminosity indicator than 24 μm affected by the emission of PAHs at high redshift (z ∼ 1), and we use several independent fields to control cosmic variance. Methods. We used a new extraction technique based on the well-determined positions of galaxies at shorter wavelengths to extract the 24 and 70 μm flux densities of galaxies. It is found that sources separated by a minimum of 0.5 x FWHM are deblended by this technique, which facilitates multi-wavelength associations of counterparts. Using a combination of photometric and spectroscopic redshifts that exist for ∼80% of the sources in our sample, we are able to estimate the rest-frame luminosities of galaxies at 15 μm and 35 μm. By complementing direct detections with a careful stacking analysis, we measured the mid- and far-infrared luminosity functions of galaxies over a factor ∼100 in luminosity (1011 L ⊙ <∼ L IR <∼ 10 13 L ⊙ ) at z < 1.3. A stacking analysis was performed to validate the bolometric corrections and to compute comoving star-formation rate densities in three redshift bins 0.4 < z < 0.7, 0.7 < z < 1.0 and, 1.0 < z < 1.3. Results. We find that the average infrared spectral energy distribution of galaxies over the last 2/3 of the cosmic time is consistent with that of local galaxies, although individual sources do present significant scatter. We also measured both the bright and faint ends of the infrared luminosity functions and find no evidence for a change in the slope of the double power law used to characterize the luminosity function. The redshift evolution of infrared luminous galaxies is consistent with pure luminosity evolution proportional to (1 + z ) 3.6±0.4 up to z ∼ 1.3. We do not find evidence of differential evolution between LIRGs and ULIRGs up to z ∼ 1.3, in contrast with previous claims. The comoving number density of infrared luminous galaxies has increased by a factor of ∼100 between 0 < z < 1. By z ∼ 1.0, LIRGs produce half of the total comoving infrared luminosity density.

Subfields: Astronomy and Astrophysics, Instrumentation, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/1cb1180457de07a7f4b5dfdad3cd50ded270d1b9

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Citations in the corpus

A Herschel view of the far-infrared properties of submillimetre galaxies (2012, methodology): “In PEP, prior source extraction was performed using the method presented in Magnelli et al. (2009), while in HerMES it was performed using the method presented in Roseboom et al. (2010), both consortia using consistent MIPS-24µm catalogues.”
The deepest Herschel-PACS far-infrared survey: number counts and infrared luminosity functions from combined PEP/GOODS-H observations (2013, methodology): “At z< 1.8, we find good agreement with the Spitzer analysis of Magnelli et al. (2009, 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).”
The far-infrared/radio correlation as probed by Herschel (2010, background): “…with photometric redshifts (〈z〉 = 0.94; interquartile z, 0.56–1.76); 3. a LIR-matched sample of 652 sources spanning z = 0−2, selected initially at 24 μm (Magnelli et al. 2009; Berta et al. 2010) then filtered to cover only the decade of LIR between 1011 → 1012 L (LIRGs), where LIR is determined…”
The VISTA deep extragalactic observations (VIDEO) survey (2012, background): “However, these techniques are only sensitive to relatively unobscured systems, and are known to miss much of the luminosity density arising from galaxies at z 1 (e.g. Schiminovich et al. 2005; Magnelli et al. 2009).”
Herschel unveils a puzzling uniformity of distant dusty galaxies (2010, methodology): “…al. 2005; Magnelli et al. 2009), while submm and Spitzer data demonstrate that ultra-luminous IR galaxies (ULIRGs, LIR ≥ 10 12 L⊙) are equally important at z ∼ 2 (Papovich et al. 2007; Caputi et al. 2007; Daddi et al. 2007; Article published by EDP Sciences Page 1 of 5 Magnelli et al. 2009, 2010).”
Modeling the evolution of infrared galaxies: a parametric backward evolution model (2010, result): “We compared our results with the measurements of Caputi et al. (2007) performed from MIPS 24 μm observations and the measurement of Magnelli et al. (2009) obtained using MIPS 70 μm observations.”
Tracing the cosmic growth of supermassive black holes to z ∼ 3 with Herschel (2014, methodology): “In this inner GOODS-S area, the Spitzer-MIPS 24 µm selected catalogue (Magnelli et al. 2009) is linked to Spitzer-IRAC 3.6 µm positions through prior extraction.”
MID-INFRARED PROPERTIES OF NEARBY LUMINOUS INFRARED GALAXIES. I. SPITZER INFRARED SPECTROGRAPH SPECTRA FOR THE GOALS SAMPLE (2013, background): “…rare in the local 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…”
Dusty Star Forming Galaxies at High Redshift (2014, background): “…have a clear advantage over previous Spitzer work since Herschel probes the peak of infrared emission directly rather than indirectly; work from Magnelli et al. (2009), Casey et al. (2012a,b), Magnelli et al. (2013), and Gruppioni et al. (2013) have all published integrated luminosity…”
The evolution of the dust temperatures of galaxies in the SFR–M∗ plane up to z ~ 2 (2013, methodology): “In PEP, prior source extraction was performed using the method presented in Magnelli et al. (2009), while in HerMES it was performed using the method presented in Roseboom et al. (2010), both consortia using consistent MIPS-24 μm catalogues.”
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).”
The Herschel view of the dominant mode of galaxy growth from z = 4 to the present day (2014, methodology): “Detected and stacked sources are then combined using a weighted average (as in, e.g., Magnelli et al. 2009).”
MODELING THE EXTRAGALACTIC BACKGROUND LIGHT FROM STARS AND DUST (2009, unknown): “…Sawicki & Thompson (2006); filled rightward-pointing triangles: Dahlen et al. (2007); star: Smith et al. (2008); empty upward-pointing triangles: Magnelli et al. (2009); empty diamonds: Takeuchi et al. (2006); empty downward-pointing triangles: Babbedge et al. (2006); empty leftward-pointing…”
ON STAR FORMATION RATES AND STAR FORMATION HISTORIES OF GALAXIES OUT TO z ∼ 3 (2011, methodology): “Briefly, the PACS photometry used in this paper was obtained by PSF-fitting using the positions of MIPS 24 µm detected sources from Magnelli et al. (2009) as prior.”
Panchromatic spectral energy distributions of Herschel sources (2013, methodology): “…et al. 1984), Infrared Space Observatory (ISO, e.g. ELAIS, Rowan-Robinson et al. 2004), Spitzer (e.g. Frayer et al. 2009; Le Floc’h et al. 2009; Magnelli et al. 2009; Lonsdale et al. 2003, 2004, Dickinson et al. 2001) and AKARI (e.g. Matsuura et al. 2009; Matsuhara et al. 2006) revealed the…”