Other
Scientific paper
May 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21840303d&link_type=abstract
American Astronomical Society, AAS Meeting #218, #403.03; Bulletin of the American Astronomical Society, Vol. 43, 2011
Other
Scientific paper
The sum total of the energy released by the earliest era of star formation should show up today within the diffuse extragalactic background light (EBL), its signature peaking in the near-infrared. There is considerable controversy over estimates of the average EBL per steradian at wavelengths longward of 1µm, over measurements of background fluctuations, and over the interpretation of the measurements. Resolving this controversy is important because the EBL constrains the history of galaxy evolution, and because the near-infrared fluctuations may contain important information about Population III stars and the earliest era of star formation. We compare number counts from recent galaxy surveys, correcting for their differing passbands. With some assumptions about galaxy sizes and surface-brightness profiles, we account for the light missed in standard photometric estimates, integrating the resulting corrected counts to estimate the total EBL due to resolved galaxies. We then present an analysis of background fluctuations in observations of the HUDF, the GOODS field, and the CANDELS fields obtained with WFC3. The fluctuation signal provides a constraint on the slope of galaxy counts fainter than the levels of individual detection. The color dependence of the fluctuations provides a constraint on the redshift distribution of these very faint sources. Fluctuations of the near-infrared EBL due to undetected sources help also constrain the nature of galaxies below current detection levels in other deep fields. The spatial and spectral information of these anisotropies provide valuable information about the EoR, as well as new populations of faint objects at lower redshifts. Via various analysis tools such as power spectra, P(D) fitting, and cross-correlations, best-fit models to faint sources can be obtained.
Chary Ranga Ram
Cooray Asantha R.
Dolch Timothy
Ferguson Henry C.
Koekemoer Anton M.
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