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<title>Extragalactic background light</title>

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Extragalactic background light

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The diffuse extragalactic background light (EBL) is all the accumulated radiation in the <a href="Universe" title="Universe">universe</a> due to <a href="Star_formation" title="Star formation">star formation</a> processes, plus a contribution from <a href="Active_galactic_nuclei" class="mw-redirect" title="Active galactic nuclei">active galactic nuclei</a> (AGNs).<a href="#cite_note-NYT-20181203-1">[1]</a> This radiation covers almost all wavelengths of the <a href="Electromagnetic_spectrum" title="Electromagnetic spectrum">electromagnetic spectrum</a>, except the microwave, which is dominated by the primordial <a href="Cosmic_microwave_background" title="Cosmic microwave background">cosmic microwave background</a>. The EBL is part of the <a href="Diffuse_extragalactic_background_radiation" title="Diffuse extragalactic background radiation">diffuse extragalactic background radiation</a> (DEBRA), which by definition covers the entire electromagnetic spectrum. After the <a href="Cosmic_microwave_background" title="Cosmic microwave background">cosmic microwave background</a>, the EBL produces the second-most energetic diffuse background, thus being essential for understanding the full energy balance of the universe.

The understanding of the EBL is also fundamental for extragalactic very-high-energy (VHE, 30 GeV-30 TeV) astronomy.<a href="#cite_note-2">[2]</a> VHE <a href="Photon" title="Photon">photons</a> coming from cosmological distances are attenuated by <a href="Pair_production" title="Pair production">pair production</a> with EBL photons. This interaction is dependent on the <a href="Spectral_energy_distribution" title="Spectral energy distribution">spectral energy distribution</a> (SED) of the EBL. Therefore, it is necessary to know the SED of the EBL in order to study intrinsic properties of the emission in the VHE sources.

<div class="mw-heading mw-heading2"><h2 id="Observations">Observations</h2></div>

The direct measurement of the EBL is difficult mainly due to the contribution of <a href="Zodiacal_light" title="Zodiacal light">zodiacal light</a> that is orders of magnitude higher than the EBL. Different groups have claimed the detection of the EBL in the optical<a href="#cite_note-3">[3]</a> and near-infrared.<a href="#cite_note-4">[4]</a><a href="#cite_note-5">[5]</a> However, it has been proposed that these analyses have been contaminated by zodiacal light.<a href="#cite_note-6">[6]</a> Recently, two independent groups using different technique have claimed the detection of the EBL in the optical with no contamination from zodiacal light.<a href="#cite_note-7">[7]</a><a href="#cite_note-8">[8]</a><a href="#cite_note-9">[9]</a>

There are also other techniques that set limits to the background. It is possible to set lower limits from deep galaxy surveys.<a href="#cite_note-10">[10]</a><a href="#cite_note-11">[11]</a> On the other hand, VHE observations of extragalactic sources set upper limits to the EBL.<a href="#cite_note-12">[12]</a><a href="#cite_note-13">[13]</a><a href="#cite_note-14">[14]</a>

In November 2018, astronomers reported that the EBL amounted to 4 x 1084 <a href="Photon" title="Photon">photons</a>.<a href="#cite_note-NYT-20181203-1">[1]</a><a href="#cite_note-SCI-20181130-15">[15]</a>

<div class="mw-heading mw-heading2"><h2 id="Empirical_modelings">Empirical modelings</h2></div>

There are empirical approaches that predict the overall SED of the EBL in the local universe as well as its evolution over time. These types of modeling can be divided in four different categories according to:<a href="#cite_note-Domínguez_2011-16">[16]</a>

(i) Forward evolution, which begins with cosmological initial conditions and follows a forward evolution with time by means of semi-analytical models of galaxy formation.<a href="#cite_note-17">[17]</a><a href="#cite_note-18">[18]</a><a href="#cite_note-19">[19]</a>

(ii) Backward evolution, which begins with existing galaxy populations and extrapolates them backwards in time.<a href="#cite_note-20">[20]</a><a href="#cite_note-21">[21]</a><a href="#cite_note-22">[22]</a>

(iii) Evolution of the galaxy populations that is inferred over a range of <a href="Redshift" title="Redshift">redshifts</a>. The galaxy evolution is inferred here using some quantity derived from observations such as the star formation rate density of the universe.<a href="#cite_note-23">[23]</a><a href="#cite_note-24">[24]</a><a href="#cite_note-25">[25]</a><a href="#cite_note-26">[26]</a>

(iv) Evolution of the galaxy populations that is directly observed over the range of redshifts that contribute significantly to the EBL.<a href="#cite_note-Domínguez_2011-16">[16]</a>

<ul><li><a href="Cosmic_infrared_background" title="Cosmic infrared background">Cosmic infrared background</a></li>

<li><a href="Cosmic_microwave_background" title="Cosmic microwave background">Cosmic microwave background</a> (CMB) radiation</li>

<li><a href="Diffuse_extragalactic_background_radiation" title="Diffuse extragalactic background radiation">Diffuse extragalactic background radiation</a></li></ul>

<div class="mw-heading mw-heading2"><h2 id="References">References</h2></div>

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