Measurements of the spectral energy distribution of the cosmic infrared background

TL;DR

This paper reviews various measurements of the cosmic infrared background's spectral energy distribution, highlighting their methods, strengths, limitations, and recent progress in understanding the universe's star formation history.

Contribution

It provides a comprehensive overview of the different measurement techniques for the CIB SED and discusses recent advances and future prospects in the field.

Findings

Absolute SED measurements limited by foreground subtraction.

Stringent lower limits from galaxy counts up to 100 microns.

Upper limits from high-energy spectra constrain IR emission.

Abstract

The extragalactic background light (EBL) is the relic emission of all processes of structure formation in the Universe. About half of this background, called the Cosmic Infrared Background (CIB) is emitted in the 8-1000 microns range, and peaks around 150 microns. It is due to the dust reemission from star formation processes and AGN emission. The CIB spectral energy distribution (SED) constraints the models of star formation in the Universe. It is also useful to compute the opacity of the Universe to the TeV photons. We present the different types of measurements of the CIB and discuss their strengths and weaknesses. 1. The absolute SED was measured by COBE, and by other experiments. These measurements are limited by the accuracy of the component separation, i.e. the foreground subtraction. 2. Robust lower limits are determined from the extragalactic number counts of infrared galaxies. These lower limits are very stringent up to 100 microns. At larger wavelengths, the rather low angular resolution of the instruments limits strongly the depth of the number counts. The "stacking" method determines the flux emitted at a given wavelength by a population detected at another wavelength, and provides stringent lower limits in the sub-mm range. It is complementary with other methods based on the statistical analysis of the map properties like the P(D) analysis. 3. Finally, upper limits can be derived from the high energy spectra of extragalactic sources. These upper limits give currently good constraints in the near- and mid-IR. Progress have been amazing since the CIB discovery about 15 years ago: the SED is much better known, and most of it can be accounted for by galaxies (directly or indirectly). Prospects are also exciting, with fluctuation analysis with Planck&Herschel, and forthcoming missions.