The Cosmic Infrared Background Resolved by Spitzer. Contributions of Mid-Infrared Galaxies to the Far-Infrared Background.

By H. Dole, G. Lagache, J. Puget, K. Caputi, N. Fernández-Conde, É. Le Floc'h, C. Papovich, P. Pérez-González, G. Rieke, M. Blaylock. 2006

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Aims. We quantify the contributions of 24 mu m galaxies to the Far-Infrared ( FIR) Background at 70 and 160 mu m. We provide new estimates of the Cosmic Infrared Background ( CIB), and compare it with the Cosmic Optical Background ( COB). Methods. Using Spitzer data at 24, 70 and 160 mu m in three deep fields, we stacked more than 19000 MIPS 24 mu m sources with S-24 >= 60 mu Jy at 70 and 160 mu m, and measured the resulting FIR flux densities. Results. This method allows a gain up to one order of magnitude in depth in the FIR. We find that the Mid-Infrared ( MIR) 24 mu m selected sources contribute to more than 70% of the Cosmic Infrared Background ( CIB) at 70 and 160 mu m. This is the first direct measurement of the contribution of MIR-selected galaxies to the FIR CIB. Galaxies contributing the most to the total CIB are thus z similar to 1 luminous infrared galaxies, which have intermediate stellar masses. We estimate that the CIB will be resolved at 0.9 mJy at 70 and 3 mJy at 160 mu m. By combining the extrapolation of the 24 mu m source counts below analysis, we obtain lower limits of 7.1 +/- 1.0 and 13.4 +/- 1.7 nW m(-2) sr(-1) for the CIB at 70 and 160 mu m, respectively. Conclusions. The MIPS surveys have resolved more than three quarters of the MIR and FIR CIB. By carefully integrating the Extragalactic Background Light ( EBL) SED, we also find that the CIB has the same brightness as the COB, around 24 nW m(-2) sr(-1). The EBL is produced on average by 115 infrared photons for one visible photon. Finally, the galaxy formation and evolution processes emitted a brightness equivalent to 5% of the primordial electromagnetic background ( CMB).

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/74fab1e3aa3cb4ed2d3fe92b7ca8d193a9f65efa

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Citations in the corpus

BLAST: RESOLVING THE COSMIC SUBMILLIMETER BACKGROUND (2009, methodology): “In particular, Dole et al. (2006) performed aperture photometry on their stacked maps, effectively subtracting a local background.”
The Herschel census of infrared SEDs through cosmic time (2013, background): “…but exhibit a strong increase in number density at earlier epochs (e.g. Takeuchi, Buat & Burgarella 2005), being responsible for about half the total light emitted from all galaxies integrated through cosmic time (e.g. Gispert, Lagache & Puget 2000; Lagache, Puget & Dole 2005; Dole et al. 2006).”
Deep ATLAS Radio Observations of the Chandra Deep Field-South/Spitzer Wide-Area Infrared Extragalactic Field (2006, background): “Spitzer surveys have shown that the cosmic infrared background is dominated by luminous infrared galaxies at around z 1 (Dole et al. 2006), while Chapman et al. (2003a) suggest that a large population of highly obscured but very active galaxies at z ¼ 1 5 may be the dominant location of massive…”
Intergalactic Photon Spectra from the Far-IR to the UV Lyman Limit for 0 < z < 6 and the Optical Depth of the Universe to High-Energy Gamma Rays (2005, neutral): “The new lower limits in the far-IR log ν = 12.63 (70 µm ) and log ν = 12.27 (160 µm ) are from Dole et al. (2006).”
New limits on the density of the extragalactic background light in the optical to the far-infrared from the spectra of all known TeV blazars (2007, methodology): “Solid lower limits for the EBL level have been derived from source counts (e.g. Madau & Pozzetti 2000; Fazio et al. 2004; Frayer et al. 2006; Dole et al. 2006).”
THE SDSS-III BARYON OSCILLATION SPECTROSCOPIC SURVEY: THE QUASAR LUMINOSITY FUNCTION FROM DATA RELEASE NINE (2012, background): “…and nature of various cosmic backgrounds, including the buildup of the cosmic X-ray (Shanks et al. 1991; Comastri et al. 1995; Ueda et al. 2003; Brandt & Hasinger 2005; Hickox & Markevitch 2006), ultraviolet (Henry 1991) and infrared (IR) (Hauser & Dwek 2001; Dole et al. 2006) backgrounds.”
The Herschel view of the dominant mode of galaxy growth from z = 4 to the present day (2014, methodology): “Stacking is a powerful and routinely used technique that combines the signal of multiple sources at various positions on the images, known from deeper surveys (see, e.g., Dole et al. 2006, where it was first applied to FIR images).”
Modeling the evolution of infrared galaxies: a parametric backward evolution model (2010, background): “We found a CIB integrated value (over the 8−1000 μm range) of 23.7 ± 0.9 nW m−2 sr−1, which agrees with the 24−27.5 nW m−2 sr−1 range of Dole et al. (2006).”
The Starburst Contribution to the Extragalactic γ-Ray Background (2006, background): “For example, the strong evolution of the IR luminosity function with redshift indicates thatF TIR is dominated by luminous infrared galaxies at z 1 (Dole et al. 2006); these systems are typical of thosewe expect to be proton calorimeters, in which case f (z) 1 at z 1.”
THE SPITZER LOCAL VOLUME LEGACY: SURVEY DESCRIPTION AND INFRARED PHOTOMETRY (2009, methodology): “A stacking analysis (e.g., Dole et al. 2006) will be employed to obtain a better statistical understanding of the fainter galaxy population at long wavelengths, in particular with respect to the H I emission.”
Measurement of the extragalactic background light imprint on the spectra of the brightest blazars observed with H.E.S.S. (2012, background): “Strict lower limits Article published by EDP Sciences A4, page 1 of 11 have been derived from integrated galaxy counts (see, e.g., Madau & Pozzetti 2000; Fazio et al. 2004; Dole et al. 2006, for more details).”
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): “Several methods can be used (e.g. Dole et al. 2006, Marsden et al. 2009, see the discussion in Vieira et al. in prep.).”
Deep Spitzer 24 μm COSMOS Imaging. I. The Evolution of Luminous Dusty Galaxies—Confronting the Models (2009, methodology): “This result has already been infered from previously-published studies (e.g., Elbaz et al. 2002; Dole et al. 2006) but our data provide for the first time a large enough statistics to explore with good accuracy the build-up of the mid-IR background as a function of cosmic time.”
PACS Evolutionary Probe (PEP) – a Herschel key program (2011, methodology): “The CIB peaks at roughly 150 µm (e.g. Dole et al. 2006), making Herschel/PACS excellently suited to characterise the sources of its bulk energyoutput.”
The extragalactic background light and the gamma-ray opacity of the universe (2012, background): “Stacking of astronomical images of sources detected at one wavelength enhances their signal relative to the random background fluctuations at some other wavelength (e.g. Dole et al., 2006).”
A lower-limit flux for the extragalactic background light (2010, methodology): “To overcome the poor constraints at far-infrared wavelengths, a stacking analysis of near- and mid-infraredsources is used (e.g. Dole et al., 2006), to significantly resolve the cosmic infrared background (CIB), leading to constraining lower limits.”
THE EXTRAGALACTIC BACKGROUND LIGHT, THE HUBBLE CONSTANT, AND ANOMALIES: CONCLUSIONS FROM 20 YEARS OF TeV GAMMA-RAY OBSERVATIONS (2015, methodology): “This is compatible at the 1σ level with previous estimations based on galaxy counts (Dole et al. 2006) and on models (see e.g., Table 1 in G12, Table 4 in D11, and Table 2 in F10).”