The contribution of known galaxies to the optical EBL can be calculated
directly by integrating the emitted flux times the differential number counts
down to the detection threshold. The results for 0.35
2.2 µm are listed in Table 1, along
with the
magnitude range of integration and the estimated 1
error bars, which
arise mostly from field-to-field variations in the numbers of relatively
bright galaxies.
![]() | AB (range) | ![]() ![]() | ![]() | ![]() |
3600 | 18.0-28.0 | 2.87 | 0.58 | 0.42 |
4500 | 15.0-29.0 | 4.57 | 0.73 | 0.47 |
6700 | 15.0-30.5 | 6.74 | 1.25 | 0.94 |
8100 | 12.0-29.0 | 8.04 | 1.62 | 0.92 |
11000 | 10.0-29.0 | 9.71 | 3.00 | 1.90 |
16000 | 10.0-29.0 | 9.02 | 2.62 | 1.68 |
22000 | 12.0-25.5 | 7.92 | 2.04 | 1.21 |
In all seven bands, the slope of the differential number-magnitude relation is
flatter than 0.4 above mAB ~ 20 (25) at near-IR (optical)
wavelengths, and this flattening appears to be more pronounced at the shorter
wavelengths. (1)
The leveling off of the counts is clearly seen in
Figure 1, where the function
i =
10-0.4(mAB+48.6) N(m) is plotted
against apparent magnitude in
all bands. While counts having a logarithmic slope d log
N/dmAB =
0.40 continue to add to the EBL at the faintest magnitudes, it
appears that the HDF survey has achieved the sensitivity to capture
the bulk of the near-ultraviolet, optical, and near-IR extragalactic light
from discrete sources. The flattening at faint
apparent magnitudes cannot be due to the reddening of distant sources as
their Lyman break gets redshifted into the blue passband, since the fraction
of Lyman-break galaxies at (say) B
25 is small
(Steidel et al. 1996;
Pozzetti et al. 1998).
Moreover, an absorption-induced loss of sources cannot explain the similar
change of slope of the galaxy counts observed in the V,I,J,H, and
K bands.
While this suggests that the surface density of
optically luminous galaxies is leveling off beyond z ~ 1.5, we are
worried that a significant amount of light may actually be missed at faint
magnitudes because of systematic errors.
The spectrum of the optical EBL
is shown in Figure 2, together with the recent
results from COBE.
The value derived by integrating the galaxy counts down to very
faint magnitude levels (because of the flattening of the number-magnitude
relation most of the contribution to the
optical EBL comes from relatively bright galaxies)
implies a lower limit to the EBL intensity in the 0.2-2.2 µm
interval of Iopt 15 n W m-2sr-1. Including the tentative
detection at 3.5 µm by Dwek & Arendt (1999) would boost
Iopt to
19 n W m-2sr-1.
Recent direct measurements of the optical EBL at 3000, 5500, and 8000 Å
from absolute surface photometry by
Bernstein et al. (1999)
lie between a
factor of 2.5 to 3 higher than the integrated light from galaxy counts, with
an uncertainty that is largely due to systematic rather than
statistical error. Applying this correction factor to the range
3000-8000 Å gives a total optical EBL intensity in the range 25-30
n W m-2sr-1. This could become ~ 45 n W
m-2sr-1 if the same correction
holds also in the near-IR. The COBE / FIRAS
(Fixsen et al. 1998)
measurements yield IFIR
14 n W m-2sr-1 in the 125-2000
µm range. When combined with the DIRBE
(Hauser et al. 1998;
Schlegel et al. 1998)
points at 140 and 240 µm, one gets a far-IR
background intensity of IFIR (140-2000 µm)
20 n W m-2sr-1.
The residual emission in the 3.5 to 140 µm region is poorly
known, but it is likely to exceed 10 n W m-2sr-1
(Dwek et al. 1998).
Additional constraints
- provided by statistical analyses of the source-subtracted sky - on the EBL
have been discussed by, e.g.
Martin & Bowyer (1989),
Kashlinsky et
al. (1996),
and Vogeley (1997).
![]() |
Figure 2. Spectrum of the optical
extragalactic background light from resolved sources
as derived from a compilation of ground-based and space-based galaxy counts
in the UBVIJHK bands (filled dots), together with the FIRAS
125-5000 µm (dashed line) and DIRBE 140 and
240 µm (filled squares) detections
(Hauser et al. 1998;
Fixsen et al. 1998).
The empty squares show the DIRBE points after correction
for WIM dust emission
(Lagache et al. 1999).
Also plotted (filled
triangle) is a FOCA-UV point at 2000 Å
from Armand et
al. (1994),
and a tentative detection at 3.5 µm (empty dot) from
COBE / DIRBE observations
(Dwek & Arendt 1999).
The empty pentagons at 3000, 5500, and 8000 Å are
Bernstein et al. (1999)
measurements of the EBL from resolved and unresolved galaxies fainter
than V = 23 mag (the error bars showing 2 |
A ``best-guess'' estimate of the total EBL intensity observed today appears to be
In the following, we will adopt a reference value for the background light
associated with star formation activity
over the entire history of the universe of IEBL = 50
I50 n W m-2sr-1.
1 A fluctuation analysis by
Pozzetti et al. (1998)
has shown
that the turnover observed in the U band is likely due to the
``reddening''
of high redshift galaxies caused by neutral hydrogen along the line of
sight. Back.