Probing the galaxy-halo connection with total satellite luminosity

We demonstrate how the total luminosity in satellite galaxies is a powerful probe of dark matter haloes around central galaxies. The method cross-correlates central galaxies in spectroscopic galaxy samples with fainter galaxies detected in photometric surveys. Using models, we show that the total galaxy luminosity, L-sat, scales linearly with host halo mass, making L-sat an excellent proxy for M-h. L-sat is also sensitive to the formation time of the halo. We demonstrate that probes of galaxy large-scale environment can break this degeneracy. Although this is an indirect probe of the halo, it yields a high signal-to-noise ratio measurement for galaxies expected to occupy haloes at <10(12) M-circle dot, where other methods suffer from larger errors. In this paper, we focus on observational and theoretical systematics in the L-sat method. We test the robustness of our method of finding central galaxies and our methods of estimating the number of background galaxies. We implement this method on galaxies in the Sloan Digital Sky Survey (SDSS) data, with satellites identified in fainter imaging data. We find excellent agreement between our theoretical predictions and the observational measurements. Finally, we compare our L-sat measurements to weak lensing estimates of M-h for red and blue subsamples. In the stellar mass range where the measurements overlap, we find consistent results, where red galaxies live in larger haloes. However, the L-sat approach allows us to probe significantly lower mass galaxies. At these masses, the L-sat values are equivalent. This example shows the potential of L-sat as a probe of dark haloes.

Automated summary

The total luminosity in satellite galaxies can effectively probe dark matter haloes around central galaxies, as it scales linearly with host halo mass and is sensitive to halo formation time. Probes of galaxy large-scale environment can break the degeneracy, and lower mass galaxies show equivalent L-sat values. This method provides a high signal-to-noise ratio measurement for galaxies expected to occupy haloes at <10^12 M⊙.