Stellar masses calibrated with micro-lensed quasars

Abstract

We measure the stellar mass surface densities of early type galaxies by observing the micro-lensing of macro-lensed quasars caused by individual stars, including stellar remnants, brown dwarfs and red dwarfs too faint to produce photometric or spectroscopic signatures. Our method measures the graininess of the gravitational potential, in contrast to methods that decompose a smooth total gravitational potential into two smooth components, one stellar and one dark. We find the median likelihood value for the calibration factor F by which Salpeter stellar masses (with a low mass cutoff of 0.1 solar masses) must be multiplied is 1.23, with a one sigma confidence range of 0.77 < F < 2.10.Comment: To be published in IAU Symposium 311, Galaxy Masses as Constraints of Formation Models, ed. M. Cappellari & S. Courteau, Cambridge Univ. Press, in press (2014). This article draws heavily upon the very much longer arXiv:1405.003