A long-wavelength view on galaxy evolution from deep surveys by the Infrared Space Observatory

By A. Franceschini, H. Aussel, C. Cesarsky, D. Elbaz, D. Fadda. 2001

172 citations recorded by the source corpus.

We discuss the constraints set on galaxy evolution by a variety of data from deep extragalactic surveys performed in the mid-IR and far-IR with the Infrared Space Observatory and with millimetric telescopes at longer wavelengths. These observations indicate extremely high rates of evolution for IR galaxies, exceeding those measured for galaxies at other wavelengths and comparable or larger than the rates observed for quasars. We also match the modelled integrated emission by IR galaxies at any redshifts with the observed spectral intensity of the extragalactic IR background (CIRB), as a further constraint. The multi-wavelength statistics on IR galaxies can be reconciled with each other by assuming for the bulk of the population spectral energy distributions (SED) as typical for starbursts, which we take as an indication that stellar (rather than AGN, see also Fadda et al. [CITE]) activity powers IR emission by faint galaxies. According to our model and following the analysis of Elbaz et al. ([CITE]), the deep ISO surveys at 15 μ m may have already resolved more than 50% of the bolometric CIRB intensity: the faint ISO 15 μ m source samples, relatively easy to identify in deep optical images (Aussel et al. [CITE]), can then allow to investigate the origin of the CIRB background. From our fits to the observed optical-IR SEDs, these objects appear to mostly involve massive galaxies hosting luminous starbursts ($SFR\sim 100$ $M_\odot$/yr). The evolutionary scheme we infer from these data considers a bimodal star formation (SF), including a phase of long-lived quiescent SF, and enhanced SF taking place during transient events recurrently triggered by interactions and merging. We interpret the strong observed evolution as an increase with z of the rate of interactions between galaxies ( density evolution ) and an increase of their IR luminosity due to the more abundant fuel available in the past ( luminosity evolution ): both factors enhance the probability to detect a galaxy during the "active" phase at higher z . Very schematically, we associate the origin of the bulk of the optical/NIR background to the quiescent evolution, while the CIRB is interpreted as mostly due the dusty starburst phase. The latter possibly leads to the formation of galaxy spheroids, when the dynamical events triggering the starburst re-distribute already present stellar populations. The large energy contents in the CIRB and optical backgrounds are not easily explained, considering the moderate efficiency of energy generation by stars: a top-heavy stellar IMF associated with the starburst phase (and compared with a more standard IMF during the quiescent SF) would alleviate the problem. The evolution of the IR emissivity of galaxies from the present time to $z\sim 1$ is so strong that the combined set of constraints by the observed z -distributions and the CIRB spectrum impose it to turn-over at $z> 1$: scenarios in which a dominant fraction of stellar formation occurs at very high- z are not supported by our analysis.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/9b94c44296b7f189eeceb15d1b2527b34de9028e

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In Astronomy and Astrophysics

1. D. M. Alexander
2. L. Hernquist
3. P. Hopkins
4. E. Daddi
5. D. Elbaz
6. Mark Dickinson
7. R. Somerville
8. C. Conroy

In Instrumentation

1. E. Daddi
2. Mark Dickinson
3. A. Renzini
4. D. Elbaz
5. C. Conroy
6. P. Hopkins
7. L. Hernquist
8. R. Dav'e

Citations in the corpus

• DUSTY INFRARED GALAXIES: Sources of the Cosmic Infrared Background (2005, background): “…several empirical approaches have been proposed to model the high evolution of the infrared output with redshift (e.g., Chary & Elbaz 2001; Franceschini et al. 2001; Rowan-Robinson 2001; Takeuchi et al. 2001; Xu et al. 2001; Lagache et al. 2004) that fit source counts, redshift…”
• Spitzer View on the Evolution of Star-forming Galaxies from z = 0 to z ~ 3 (2005, methodology): “The Infrared Space Observatory (ISO) showed that dustenshrouded starbursts have undergone strong evolution from z 1 to z ¼ 0 (Franceschini et al. 2001).”
• The 0.4 < z < 1.3 star formation history of the Universe as viewed in the far-infrared (2009, background): “…Space Observatory(ISO), several teams have confirmed the importance of infrared galaxies for the understanding of SFR evolution (Elbaz et al. 1999; Aussel et al. 1999; Chary & Elbaz 2001; Franceschini et al. 2001; Xu et al. 2001; Elbaz et al. 2002; Metcalfe et al. 2003; Lagache et al. 2004).”
• Infrared Luminosity Functions from the Chandra Deep Field-South: The Spitzer View on the History of Dusty Star Formation at 0 ≲ z ≲ 1* (2005, background): “In the past few years, deep observations performed in the infrared by ISO and in the submillimeter by the SCUBA camera have revealed strong evolution of these luminous sources with lookback time (Smail et al. 1997; Blain et al. 1999a; Elbaz et al. 1999; Serjeant et al. 2001; Dole et al. 2001), that ”
• SWIRE: The SIRTF Wide‐Area Infrared Extragalactic Survey (2001, background): “…redshift, the form of the initial mass fucntion (IMF) in starbursts (an IMF truncated at the low mass end would reduce conflicts between the observed luminosities and the conversion rate of gas to stars (Franceschini et al. 2001)), and the contribution to the IR luminosities of dust-enshrouded AGN.”
• Modelling infrared galaxy evolution using a phenomenological approach (2002, background): “…have been proposed to model the high rate of evolution of IR galaxies (e.g. Devriendt & Guiderdoni 2000; Wang & Biermann 2000; Charry & Elbaz 2001; Franceschini et al. 2001; Malkan & Stecker 2001; Pearson 2001; Rowan-Robinson 2001; Takeuchi et al. 2001; Xu et al. 2001; Balland, Devriendt & Silk…”
• Quasars: the characteristic spectrum and the induced radiative heating (2003, background): “(iii) The CIB at 15 µm: EIE(15 µm, total) ≈ 3 nW m−2 sr−1 (Franceschini et al. 2001; Elbaz, Cesarsky & Chanial 2002), and ≈ 17% of this intensity is due to AGN that make up ∼ 85% of the 2–10 keV background, as inferred from the cross-correlation of XMM-Newton and Chandra deep X-ray surveys with…”
• Evolution of the dusty infrared luminosity function from z = 0 to z = 2.3 using observations from Spitzer (2011, background): “…ULIRGs 1012L⊙ < LIR) in the evolution of the star-formation rate (SFR) history of the Universe is now well established up toz ∼ 1 (Chary & Elbaz 2001; Franceschini et al. 2001; Xu et al. 2001; Elbaz et al. 2002; Metcalfe et al. 2003; Lagache et al. 2004; Le Floc’h et al. 2005; Magnelli et al.…”
• Extragalactic optical-infrared background radiation, its time evolution and the cosmic photon-photon opacity (2008, methodology): “…have performed extensive explorations of high-redshift galaxies thanks to the extremely high sensitivity allowed by the very low background noise (Elbazet al. 1999, 2002 and Franceschini et al. 2001 for the main ISO results; Le Floc’h et al. 2005, Prez-Gonzlez et al. 2005, for Spitzer results).”
• THE CONTRIBUTION OF STARBURSTS AND NORMAL GALAXIES TO INFRARED LUMINOSITY FUNCTIONS AT z < 2 (2012, background): “The evolving shape of IR LFs hence implicitly contains information on the relative importance of the two modes of SF in the past (e.g., Franceschini et al. 2001, Béthermin et al. 2011).”
• THE SPITZER–WISE SURVEY OF THE ECLIPTIC POLES (2011, background): “The rising counts were first discovered with deep ISOCAM 15 μm source counts, attributed to populations at z ∼ 0.8 (arising from the redshifted 7.7 μm PAH) and extending to z= 2 (Franceschini et al. 2001).”
• A New Photometric Technique for the Joint Selection of Star-forming and Passive Galaxies at 1.4 ≲ z ≲ 2.5 (2004, background): “…dust-enshrouded high redshift star-forming objectsinclude detecting them from their far-IR or sub-mm emission 2 E. Daddi et al. due to cold dust (Franceschini et al. 2001; Smail et al. 2002; Champan et al. 2003), observing the emission at X-ray or radio wavelengths that are not extincted by…”
• Mid- and far-infrared luminosity functions and galaxy evolution from multiwavelength Spitzer observations up to z ~ 2.5 (2009, methodology): “Compared to previous analyses essentially based on preSpitzer surveys (e.g. Franceschini et al. 2001), an important addition in AF09 was the introduction of an evolutionary component of very luminous IR galaxies dominating the cosmic IR emissivity atz ∼2, and essentially absent or very rare…”
• A semi-empirical simulation of the extragalactic radio continuum sky for next generation radio telescopes (2008, background): “11 of Franceschini et al. 2001) is completelydifferent from the one we assume, with the starbursts comprising a decreasing fraction of the whole forL60 > 1010 L⊙.”
• The extragalactic background light revisited and the cosmic photon–photon opacity (Corrigendum) (2017, background): “…galaxy M82 (see e.g., Polletta et al. 2007): while in the range from 5 to 18 µm they are fixed to the mid-IR spectrum of M82 observed by ISOCAM (Franceschini et al. 2001), at longer wavelengths the two spectra have been modified so as to best-fit all the multi-wavelength data reported in…”
• A Significant Population of Very Luminous Dust-Obscured Galaxies at Redshift z ~ 2 (2008, background): “…was derived from studies of a handful of the most extreme IRAS sources, constraints on the redshift evolution out to z ∼ 1 (largely due to ISO; e.g., Franceschini et al. 2001; Chary & Elbaz 2001; Lagache et al. 2003), small samples of galaxies discovered at sub-millimeter wavelengths (e.g., Smail…”
• 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): “Franceschini et al. (2001) made an attempt to account for this starburst phase in a backwards evolution model.”
• Deep Spitzer 24 μm COSMOS Imaging. I. The Evolution of Luminous Dusty Galaxies—Confronting the Models (2009, methodology): “…of the counts below 80µJy it is again consistent with the picture suggested by phenomenological models of IR galaxy evolution (e.g. Chary & Elbaz 2001; Franceschini et al. 2001) and by the analysis of the history of the CIB recently performed with other methods (e.g., Dole et al. 2006).”