Interpreting the Cosmic Infrared Background: Constraints on the Evolution of the Dust-enshrouded Star Formation Rate

By R. Chary, D. Elbaz. 2001

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The mid-infrared local luminosity function is evolved with redshift to fit the spectrum of the cosmic infrared background (CIRB) at λ > 5 μm and the galaxy counts from various surveys at mid-infrared, far-infrared, and submillimeter wavelengths. A variety of evolutionary models provide satisfactory fits to the CIRB and the number counts. The degeneracy in the range of models cannot be broken by current observations. However, the different evolutionary models yield approximately the same comoving number density of infrared luminous galaxies as a function of redshift. Since the spectrum of the cosmic background at λ > 200 μm is quite sensitive to the evolution at high redshift, i.e., z > 1, all models that fit the counts require a flattening at z ~ 0.8 to avoid overproducing the CIRB. About 80% of the 140 μm CIRB is produced at 0 < z < 1.5, while only about 30% of the 850 μm background is produced within the same redshift range. The nature of the evolution is then translated into a measure of the dust-enshrouded star formation rate (SFR) density as a function of redshift and compared with estimates from rest-frame optical/ultraviolet surveys. The dust-enshrouded SFR density appears to peak at z = 0.8 ± 0.1, much sooner than previously thought, with a value of 0.25 M☉ yr-1 Mpc-3, and remains almost constant up to z ~ 2. At least 70% of this star formation takes place in infrared luminous galaxies with LIR > 1011 L☉. The long-wavelength observations that constrain our evolutionary models do not strongly trace the evolution at z > 2 and a drop-off in the dust-enshrouded SFR density is consistent with both the CIRB spectrum and the number counts. However, a comparison with the infrared luminosity function derived from extinction-corrected rest-frame optical/ultraviolet observations of the Lyman break galaxy population at z ~ 3 suggests that the almost flat comoving SFR density seen between redshifts of 0.8 and 2 extends up to a redshift of z ~ 4.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/4025526f43dda1f7427c4be2aa97a619e87fed3e

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Citations in the corpus

Dust in the Reionization Era: ALMA Observations of a z = 8.38 Gravitationally Lensed Galaxy (2017, methodology): “Firstly, we used an updated version of Hyperz (Bolzonella et al. 2000) with a template library drawn from Bruzual & Charlot (2003), Chary & Elbaz (2001), Coleman et al. (1980), and Leitherer et al. (1999) including nebular emission lines as described by Schaerer & de Barros (2009).”
Star formation and mass assembly in high-redshift galaxies (2009, methodology): “In Appendix A, we compare these values with the corresponding LIR predicted by different model libraries (Chary & Elbaz 2001; Polletta et al. 2007).”
The 0.4 < z < 1.3 star formation history of the Universe as viewed in the far-infrared (2009, methodology): “The thin and the thick solid lines correspond to thek-correction obtained using the Chary & Elbaz (2001) 1011 L⊙ and 1012 L⊙ templates respectively.”
AN ATLAS OF GALAXY SPECTRAL ENERGY DISTRIBUTIONS FROM THE ULTRAVIOLET TO THE MID-INFRARED (2013, methodology): “In Figure 12 we plot our spectrum of IC 4553 (Arp 220), along with other IC 4553 templates from the recent literature (Chary & Elbaz 2001; Donley et al. 2007; Polletta et al. 2007; Rieke et al. 2009).”
A PUBLIC Ks-SELECTED CATALOG IN THE COSMOS/UltraVISTA FIELD: PHOTOMETRY, PHOTOMETRIC REDSHIFTS, AND STELLAR POPULATION PARAMETERS, (2013, methodology): “We use the log-average of the Dale & Helou (2002) templates for this computation (see, Wuyts et al. 2008), but note that using the log-average of the Chary & Elbaz (2001) templates would provide very similar results (Muzzin et al. 2010).”
Spitzer Observations of Massive, Red Galaxies at High Redshift (2005, methodology): “…the redshifts of the DRGs, z 1 3:5, the Spitzer 24 m probes the rest-framemid-IR, which broadly correlates with the total thermal IR luminosity, LIR L(8 1000 m) (e.g., Spinoglio et al. 1995; Roussel et al. 2001; Chary & Elbaz 2001; Dale et al. 2001; Elbaz et al. 2002; Papovich & Bell 2002).”
Fitting the integrated spectral energy distributions of galaxies (2010, background): “Well known examples of templates include those of Chary and Elbaz (2001), Dale and Helou (2002), Lagache et al. (2004), and, more recently, Rieke et al. (2009).”
A lower-limit flux for the extragalactic background light (2010, background): “…(back- wards evolution) extrapolates present day data or templatespectra to high redshift in a certain wavelength range (for the most recent ones: Chary & Elbaz 2001; Malkan & Stecker 2001; Totani & Takeuchi 2002; Lagache et al., 2003, 2004; Xu et al., 2003; King et al., 2003, Stecker et…”
Local supermassive black holes, relics of active galactic nuclei and the X-ray background (2003, methodology): “9 we plot the cosmic accretion history of BH’s (computed using the Ueda et al. (2003) luminosity function, ǫ = 0.1 and λ = 1) and we compare it with the estimate by Barger et al. (2001) and with the cosmic star formation rate by Chary & Elbaz (2001).”
GMASS ultradeep spectroscopy of galaxies at $z$ ~ 2 - II. Superdense passive galaxies: how did they form and evolve? (2008, methodology): “If the 24µm emission is real and due to star formation activity, and extrapolating from the 24µm measurements using the spectral templates of Chary & Elbaz (2001) (see for instance Daddi et al. 2007a, Daddi et al. 2007b, the implied infrared (bolometric) luminosity is≈ 1.4×1011 L⊙.”
On the evolution and environmental dependence of the star formation rate versus stellar mass relation since z ∼ 2 (2013, methodology): “We derive the total infrared luminosity (LIR) from the stacked 24µm photometry using the Chary & Elbaz (2001) SED templates, and then compute the SFR using the combined Hα andLIR approach suggested by Kennicutt et al. (2009); SFR= 7.9× 10−42[L(Hα)obs +0.0024× LIR] (erg s−1).”
The far-infrared/radio correlation as probed by Herschel (2010, methodology): “…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 using the models of Chary & Elbaz (2001).”
Bolometric luminosities and Eddington ratios of X-ray selected active galactic nuclei in the XMM-COSMOS survey (2012, methodology): “The code is based on a large set of star-burst templat s from Chary & Elbaz (2001) and Dale & Helou (2002), and galaxy templates from the Bruzual & Charlot (2003) code for spectral synthesis models, while AGN templates are taken from Silva et al. (2004).”
THE SFR–M* RELATION AND EMPIRICAL STAR FORMATION HISTORIES FROM ZFOURGE AT 0.5 < z < 4 (2015, background): “The longer wavelength data from Spitzer and Herschel allow for robust SFR measurements (e.g. Kennicutt 1998; Chary & Elbaz 2001; Papovich et al. 2007; Elbaz et al. 2011).”
A TURNOVER IN THE GALAXY MAIN SEQUENCE OF STAR FORMATION AT M* ∼ 1010 M☉ FOR REDSHIFTS z < 1.3 (2015, neutral): “It has been shown that measuring the LIR from fitting the farinfrared data to libraries of SED (e.g. Chary & Elbaz 2001; Dale & Helou 2002) gives roughly the same results as the modified blackbody plus power-law model (Casey 2012; U et al. 2012; Lee et al. 2013).”
The incidence of obscuration in active galactic nuclei (2013, methodology): “We then derive the SFR of each redshift, luminosity and obscuration-class bin using their stacked PACS flux densities and the Chary & Elbaz (2001) SED library.”
SPECTRAL ENERGY DISTRIBUTIONS OF LOCAL LUMINOUS AND ULTRALUMINOUS INFRARED GALAXIES (2012, methodology): “…new total infrared luminosity, LIR = 8 − 1000µm, by using χ 2 minimization to fit the MIR-FIR-submm portion (14 data points) of the SEDs with different dust models and a modified black body fit (CE,DH,SK,mBB: Chary & Elbaz 2001; Dale & Helou 2002; Siebenmorgen & Krügel 2007; Casey 2012, Table 9).”
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): “To interprete these fluxes, we consider a variety of dust templates, including those of Elbaz et al. (2011), Chary & Elbaz (2001), Dale & Helou (2002), and Rieke et al. (2009), as well as the 24µm-LIR and radioinfrared correlations of Reddy et al. (2010) and Bell (2003), respectively.”
The HDUV Survey: A Revised Assessment of the Relationship between UV Slope and Dust Attenuation for High-redshift Galaxies (2017, neutral): “7/LIR〉 = 0.18 ± 0.03, where the latter has been corrected for the difference in this ratio when assuming the Elbaz et al. (2011) dust template rather than those of Chary & Elbaz (2001).”