THE COSMIC INFRARED BACKGROUND: Measurements and Implications ⁄

By M. Hauser, E. D. S. T. S. Institute, NASAGoddard Space Flight Center. 2001

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▪ Abstract The cosmic infrared background records much of the radiant energy released by processes of structure formation that have occurred since the decoupling of matter and radiation following the Big Bang. In the past few years, data from the Cosmic Background Explorer (COBE) mission provided the first measurements of this background, with additional constraints coming from studies of the attenuation of TeV γ-rays. At the same time, there has been rapid progress in resolving a significant fraction of this background with the deep galaxy counts at infrared wavelengths from the Infrared Space Observatory (ISO) instruments and at submillimeter wavelengths from the Submillimeter Common User Bolometer Array (SCUBA) instrument. This article reviews the measurements of the infrared background and sources contributing to it and discusses the implications for past and present cosmic processes.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/b55ffe15b9c681dc437672d5477585e074b76b4c

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Citations in the corpus

Measurement of the extragalactic background light imprint on the spectra of the brightest blazars observed with H.E.S.S. (2012, background): “The former is mainly due to the radiation emitted by stellar nucleosynthesis in the optical (O) to near infrared (IR), while the latter stems from UV-optical light absorbed and re-radiated by dust in the IR domain (for a review, see Hauser & Dwek 2001).”
The extragalactic background light revisited and the cosmic photon–photon opacity (Corrigendum) (2017, methodology): “…various published measurements of the total-light EBL in the near-IR based on COBE (Gorjian et al. 2000, Wright & Reese 2000, Cambresy et al. 2001, Hauser & Dwek 2001, Dwek & Krennrich 2005, 2013), and IRTS (Matsumoto et al. 2005; Kashlinsky 2006) observations, and rocket experiments (Zemkov et…”
THE COSMIC CORE-COLLAPSE SUPERNOVA RATE DOES NOT MATCH THE MASSIVE-STAR FORMATION RATE (2011, methodology): “Thus, to explain the supernova rate problem by lowering the SFR, one would require almost no dust at these distances, which is inconsistent with our understanding of the FIR universe (Hauser & Dwek 2001; Lagache et al. 2005).”
Number Counts at 3 μm < λ < 10 μm from the Spitzer Space Telescope (2004, background): “For example, normal galaxies alone cannot explain the cosmic infrared background (Hauser & Dwek 2001); instead, it is necessary to invoke a population of dusty, starbursting galaxies (e.g., M82) which re-radiate a substantial portion of their bolometric luminosity in the far-infrared.”
GeV gamma-ray attenuation and the high-redshift UV background (2009, background): “…the present-day EBL through absolute photometry in the optical and IR portion of the spectrum are hampered by the bright foregrounds of the Milky Way and zodiacal light from dust in ∗ E-mail:rgilmore@physics.ucsc.edu the solar system, as well as calibration uncertainties (Hauser & Dwek 2001).”
A lower-limit flux for the extragalactic background light (2010, methodology): “While it is possible to measure extragalactic diffuse emission in the sub-mm range, (Puget et al., 1996; Hauser et al., 1998; Hauser & Dwek 2001), the EBL isdifficult to measure directly in the infrared because of strong foreground contamination.”
2FHL: THE SECOND CATALOG OF HARD FERMI-LAT SOURCES (2015, background): “These photons from significantly attenuated sources provide information about the EBL, which in turn carries fundamental information about galaxy evolution and cosmology (e.g., Hauser & Dwek 2001; Domínguez & Prada 2013; Biteau & Williams 2015).”
HERSCHEL-ATLAS GALAXY COUNTS AND HIGH-REDSHIFT LUMINOSITY FUNCTIONS: THE FORMATION OF MASSIVE EARLY-TYPE GALAXIES (2011, background): “19 we illustrate the contribution of proto- spheroids to the extragalactic infrared background intensity (Lagache et al. 1999; Hauser & Dwek 2001) according to our physical model.”
Reionization and the Cosmic Dawn with the Square Kilometre Array (2012, background): “Although expected and searched for since at least the 1960s (see Hauser & Dwek 2001, for a review), it was first measured in this wavelength range in the year 2000 by a combination of IRTS and COBE data (Gorjian et al. 2000; Matsumoto et al. 2000; Wright & Reese 2000).”
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.”
Building the cosmic infrared background brick by brick with Herschel/PEP. ⋆ (2011, background): “Its energy density di tribution is characterized by two primary peaks: the first atλ ∼ 1 µm produced by starlight, and a second peak at∼ 100− 200 µm mainly due to starlight absorbed and reprocessed by dust in galaxies (e.g. Hauser & Dwek 2001).”
SWIRE: The SIRTF Wide‐Area Infrared Extragalactic Survey (2001, positive): “The COBE detection of the Cosmic Infrared Background (CIB) has illustrated that >50% of the total luminous energy density of the Universe emerges longward of ∼1µm (Hauser & Dwek 2001).”
Electron-positron pairs in physics and astrophysics: from heavy nuclei to black holes (2009, neutral): “[287, 288].”
Dust in the Early Universe: Dust Formation in the Ejecta of Population III Supernovae (2003, background): “Furthermore, dust grains residing in interstellar space in galaxies and in the intergalactic medium cause obscuration and reddening of starlight, and the thermal radiation from the dust grains distorts the cosmic background radiation (see Hauser & Dwek 2001 for details).”
Star-forming galaxies as the origin of diffuse high-energy backgrounds: gamma-ray and neutrino connections, and implications for starburst history (2014, methodology): “Surveys of dust emission performed with former satellites exploring the Universe in the mid- and far-IR domain (IRAS, ISO, and Spitzer) allowed the first studies of the IR-galaxy luminosity function (comoving number density of galaxies per unit luminosity range) up to z ∼ 2 [23–26].”