Dusty Infrared Galaxies: Sources of the Cosmic Infrared Background

Lagache, G.; Puget, J.‐L.; Dole, H.

doi:10.1146/annurev.astro.43.072103.150606

Cited by 286 publications

(298 citation statements)

References 148 publications

(177 reference statements)

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“…This behavior is expected because of the redshifted peak in the galaxy spectral energy distributions, or k-correction (e.g. Lagache et al 2004;Lagache et al 2005) (Le Floch et al 2009) 70μm (this work) 100μm (Berta et al 2010) 160μm (this work) 160μm (Berta et al 2010) Fig. 9.…”

Section: The 24 70 100 and 160 μM Backgroundsmentioning

confidence: 71%

“…Lagache et al 2005;Bethermin et al 2010c). The 24 μm background contains, however, a significant contribution from galaxies at z > 1 (30%, according to Le Floc'h et al 2009).…”

Section: The 24 70 100 and 160 μM Backgroundsmentioning

confidence: 99%

“…Thus, the peak and the structure in redshift observed with the S 24 > 80 μJy cut is not significantly affected by this selection, and our conclusions based on this cut can be extended to the whole CIB buildup, at least for z < 2.5. However, the S 24 > 80 μJy cut might cause a problem of strong incompleteness at Herschel SPIRE wavelengths, made-up by higher-redshift sources (Lagache et al 2005;Marsden et al 2009). A need to use fainter 24 μm flux densities is thus required at submm wavelengths.…”

Section: The Modelsmentioning

confidence: 99%

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The cosmic far-infrared background buildup since redshift 2 at 70 and 160 microns in the COSMOS and GOODS fields

Jauzac

Dole

Floc’h

et al. 2010

A&A

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Context. The cosmic far-infrared background (CIB) at wavelengths around 160 μm corresponds to the peak intensity of the whole extragalactic background light, which is being measured with increasing accuracy. However, the build up of the CIB emission as a function of redshift is still not well known. Aims. Our goal is to measure the CIB history at 70 μm and 160 μm at different redshifts, and provide constraints for infrared galaxy evolution models. Methods. We used deep Spitzer 24 μm catalogs complete to about 80 μJy with spectroscopic and photometric redshift identifications, derived using the GOODS and COSMOS deep infrared surveys covering 2 square degrees total. After cleaning the Spitzer/MIPS 70 μm and 160 μm maps of detected sources, we stacked the far-IR images at the positions of the 24 μm sources in different redshift bins. We measured the contribution of each stacked source to the total 70 and 160 μm light, and compared with model predictions and far-IR measurements obtained for Herschel/PACS data of smaller fields. Results. We detect components of the 70 and 160 μm backgrounds in different redshift bins up to z ∼ 2. The contribution to the CIB reaches a maximum at 0.3 ≤ z ≤ 0.9 at 160 μm (and z ≤ 0.5 at 70 μm). A total of 81% (74%) of the 70 (160) μm background was emitted at z < 1. We estimate that the AGN contribution to the far-IR CIB is less than about 10% at z < 1.5. We provide a comprehensive view of the CIB buildup at 24, 70, 100 and 160 μm. Conclusions. We find that IR galaxy models predicting a major contribution to the CIB from sources at z < 1 agree with our measurements, while our results exclude other models that predict a peak of the background at higher redshifts. The consistency of our results with those obtained by the direct study of Herschel far-IR data at 160 μm confirms that the stacking analysis method is a valid approach to estimate the components of the far-IR background using prior information about resolved mid-IR sources.

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Section: The 24 70 100 and 160 μM Backgroundsmentioning

confidence: 71%

“…Lagache et al 2005;Bethermin et al 2010c). The 24 μm background contains, however, a significant contribution from galaxies at z > 1 (30%, according to Le Floc'h et al 2009).…”

Section: The 24 70 100 and 160 μM Backgroundsmentioning

confidence: 99%

Section: The Modelsmentioning

confidence: 99%

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The cosmic far-infrared background buildup since redshift 2 at 70 and 160 microns in the COSMOS and GOODS fields

Jauzac

Dole

Floc’h

et al. 2010

A&A

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“…Negrello et al predict a redshift distribution for S 350 > 100 mJy galaxies peaking at z ≈ 2 (red line on Figure 19). In contrast, earlier predictive work by Lagache et al (2005) addresses the overall redshift distribution for the underlying 350µm population, which peaks at substantially lower redshift, z ≈ 1, with a long tail out to high redshifts. Another phenomenological approach described in Béthermin et al (2011), working backwards from constrained luminosity functions to redshift distributions and number counts predicts a peak at very low redshifts with a secondary peak 10 at z ∼ 2.…”

Section: Redshift Distributions Of 250µm-500 Mm-selected Dsfg Populatmentioning

confidence: 91%

Dusty star-forming galaxies at high redshift

2014

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Far-infrared and submillimeter wavelength surveys have now established the important role of dusty, star-forming galaxies (DSFGs) in the assembly of stellar mass and the evolution of massive galaxies in the Universe. The brightest of these galaxies have infrared luminosities in excess of 10 13 L with implied star-formation rates of thousands of solar masses per year. They represent the most intense starbursts in the Universe, yet many are completely optically obscured. Their easy detection at submm wavelengths is due to dust heated by ultraviolet radiation of newly forming stars. When summed up, all of the dusty, star-forming galaxies in the Universe produce an infrared radiation field that has an equal energy density as the direct starlight emission from all galaxies visible at ultraviolet and optical wavelengths. The bulk of this infrared extragalactic background light emanates from galaxies as diverse as gas-rich disks to mergers of intense starbursting galaxies. Major advances in far-infrared instrumentation in recent years, both spacebased and ground-based, has led to the detection of nearly a million DSFGs, yet our understanding of the underlying astrophysics that govern the start and end of the dusty starburst phase is still in nascent stage. This review is aimed at summarizing the current status of DSFG studies, focusing especially on the detailed characterization of the bestunderstood subset (submillimeter galaxies, who were summarized in the last review of this field over a decade ago, Blain et al. 2002), but also the selection and characterization of more recently discovered DSFG populations. We review DSFG population statistics, their physical properties including dust, gas and stellar contents, their environments, and current theoretical models related to the formation and evolution of these galaxies.

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“…The cosmic IR background (CIB, Puget et al 1996;Hauser et al 1998) accounts for roughly half of the total extragalactic background light (EBL, Hauser & Dwek 2001;Lagache et al 2005), i.e., half of the energy radiated by all galaxies, at all cosmic epochs, at any wavelength (Dole et al 2006). It is therefore a crucial constraint on modes and times of galaxy formation.…”

Section: Introductionmentioning

confidence: 99%

Dissecting the cosmic infra-red background withHerschel/PEP

Berta

Magnelli

Lutz

et al. 2010

A&A

112

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The constituents of the cosmic IR background (CIB) are studied at its peak wavelengths (100 and 160 μm) by exploiting Herschel/PACS observations of the GOODS-N, Lockman Hole, and COSMOS fields in the PACS evolutionary probe (PEP) guaranteed-time survey. The GOODS-N data reach 3σ depths of ∼3.0 mJy at 100 μm and ∼5.7 mJy at 160 μm. At these levels, source densities are 40 and 18 beams/source, respectively, thus hitting the confusion limit at 160 μm. Differential number counts extend from a few mJy up to 100-200 mJy, and are approximated as a double power law, with the break lying between 5 and 10 mJy. The available ancillary information allows us to split number counts into redshift bins. At z ≤ 0.5 we isolate a class of luminous sources (L IR ∼ 10 11 L ), whose SEDs resemble late-spiral galaxies, peaking at ∼130 μm restframe and significantly colder than what is expected on the basis of pre-Herschel models. By integrating number counts over the whole covered flux range, we obtain a surface brightness of 6.36± 1.67 and 6.58± 1.62 [nW m −2 sr −1 ] at 100 and 160 μm, resolving ∼45% and ∼52% of the CIB, respectively. When stacking 24 μm sources, the inferred CIB lies within 1.1σ and 0.5σ from direct measurements in the two bands, and fractions increase to 50% and 75%. Most of this resolved CIB fraction was radiated at z ≤ 1.0, with 160 μm sources found at higher redshift than 100 μm ones.

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Dusty Infrared Galaxies: Sources of the Cosmic Infrared Background

Cited by 286 publications

References 148 publications

The cosmic far-infrared background buildup since redshift 2 at 70 and 160 microns in the COSMOS and GOODS fields

The cosmic far-infrared background buildup since redshift 2 at 70 and 160 microns in the COSMOS and GOODS fields

Dusty star-forming galaxies at high redshift

Dissecting the cosmic infra-red background withHerschel/PEP

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