Clustering of the IR Background Light with Spitzer: Contribution from Resolved Sources

Details Clustering of the IR Background Light with Spitzer: Contribution from Resolved Sources Clustering of the IR Background Light with Spitzer: Contribution from Resolved Sources

2006-09-15

arxiv.org/abs/astro-ph/0609451v3

Astrophys.J.657:37-50,2007

Astronomy and Astrophysics

Astrophysics

12 pages, 11 figures. Accepted version in press with ApJ. Revised version includes conditional luminosity function models for

Scientific paper

10.1086/511293

We describe the angular power spectrum of resolved sources at 3.6 microns (L-band) in Spitzer imaging data of the GOODS HDF-N, the GOODS CDF-S, and the NDWFS Bootes field in several source magnitude bins. We also measure angular power spectra of resolved sources in the Bootes field at K_S and J-bands using ground-based IR imaging data. In the three bands, J, K_S, and L, we detect the clustering of galaxies on top of the shot-noise power spectrum at multipoles between ell ~ 10^2 and 10^5. The angular power spectra range from the large, linear scales to small, non-linear scales of galaxy clustering, and in some magnitude ranges, show departure from a power-law clustering spectrum. We consider a halo model to describe clustering measurements and to establish the halo occup ation number parameters of IR bright galaxies at redshifts around one. We also extend our clustering results and completeness-corrected faint source number counts in GOODS fields to understand the underlying nature of unresolved sources responsible for IR background (IRB) anisotropies that were detected in deep Spitzer images. While these unresolved fluctuations were measured at sub-arcminute angular scales, if a high-redshift diffuse component associated with first galaxies exists in the IRB, then it's clustering properties are best studied with shallow, wide-field images that allow a measurement of the clustering spectrum from a few degrees to arcminute angular scales.

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