Annu. Rev. Astron. Astrophys. 2001. 39: 249-307
Copyright © 2001 by . All rights reserved

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In this section, we discuss relatively direct implications of the EBL measurements. Models for the origin of the EBL are discussed elsewhere (Section 5).

4.1. Total EBL Energy

Important insights into the nature and evolution of the sources contributing to the EBL can be gained by examining its integrated energy and spectral energy distribution. Examination of Figure 5 suggests that the EBL spectrum has two maxima, with peaks at both optical and far-infrared wavelengths. This supports a picture of a background consisting largely of redshifted primary radiations at optical and near-infrared wavelengths, and reradiated thermal dust emission at far-infrared wavelengths. The existence of the long wavelength peak provides compelling evidence that the dominant luminosity sources are dusty.

We define I ident integ Inu d nu = integ nu Inu d ln nu as the frequency-integrated brightness of the cosmic background radiation. In the following tabulation, we give first the value of the integral (in nWm-2 sr-1) of the nominal EBL shown by the dashed line in Figure 5. We show in parentheses the range of values of the integral obtained using the upper and lower limits defined by the shaded area in Figure 5.

I_{{\rm stellar}} & = & 54 \qquad (19-100),\ \qquad \qquad  \lambda   = 
0.16-3.5~\mu{\rm m} \\
I_{{\rm dust}}    & = & 34 \qquad (11-58),\ \ \qquad \qquad  \lambda   = 
3.5-140~\mu{\rm m} \\
	 	& = & 15\pm2,\ \  \qquad \qquad \qquad  \qquad   \lambda  = 
140-1000~\mu{\rm m} \\
I_{{\rm EBL}}     & = & 100 \qquad (45-170), \qquad \qquad    \lambda  = 
0.16-1000~\mu{\rm m} \\
I_{{\rm CIB}}     & = & 76 \qquad (36-120),\ \qquad \qquad    \lambda  = 
1-1000~\mu{\rm m}.

The quoted uncertainty in the 140-1000 µm integral is 1sigma. In presenting these integrated backgrounds, we have separated out the 3.5 to 140 µm range because there have been no direct detections of the dust emission in this spectral range.

Thermal emission from dust dominates the EBL spectrum at wavelengths longward of ~ 3.5 µm and constitutes about 48% of the nominal EBL. However, values ranging from 20% to 80% are consistent with the measurement uncertainties (Figure 5, shaded area). The nominal percentage is larger than the ~ 30% contribution of dust emission to the local (within ~ 75 h-1 Mpc) luminosity density (Soifer & Neugebauer 1991), which suggests that the relative contribution of dust to the total energy output in the universe was higher in the past than at present. However, given the substantial uncertainty in the EBL measurements, the possibility that this fraction may have been constant or even lower in the past cannot be ruled out.

To compare the integrated EBL energy density with other cosmological energy budgets, it is useful to define the dimensionless radiative energy density, OmegaR, as

\Omega_{R}  =   {4\pi \over c}I /(\rho_c c^2),
\end{equation} (2)

where rhoc is the critical mass density of the universe, with

\rho_c\,c^2  =  1.69 \times\ 10^{-8}\, h^2\, {\rm erg~cm^{-3}}.

The energy density in the EBL is therefore a small fraction of the critical energy density,

\Omega_{EBL} =
2.48 \times\, 10^{-6} h^{-2}\,I_{100},
\end{equation} (3)

where I100 ident IEBL/(100 nW m-2 sr-1) lies in the range 0.45-1.7, as indicated above. The integrated CMB intensity, ICMB, is 1000 nW m-2 sr-1 (Mather et al. 1999), or OmegaCMB = 2.48 × 10-5 h-2. Hence, the total EBL energy is also a small fraction of the radiant energy in the CMB:

\Omega_{EBL} / \Omega_{CMB} = 0.10\,I_{100}.
\end{equation} (4)

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