We describe the angular power spectrum of resolved sources at 3.6 \mu m ( L -band ) in Spitzer imaging data of the GOODS HDF-N , the GOODS CDF-S , and the NDWFS Boötes field in several source magnitude bins .
We also measure angular power spectra of resolved sources in the Boötes 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 \sim 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 occupation number parameters of IR bright galaxies at redshifts around one .
The typical halo mass scale at which two or more IR galaxies with L -band Vega magnitude between 17 and 19 are found in the same halo is between 9 \times 10 ^ { 11 } M _ { \sun } and 7 \times 10 ^ { 12 } M _ { \sun } at the 1 \sigma confidence level ; this is consistent with the previous halo mass estimates for bright , red galaxies at z \sim 1 .
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 .