Photometric mass estimation and the stellar mass–halo mass relation for low mass galaxies

We present a photometric halo mass estimation technique for local galaxies that enables us to establish the stellar mass-halo (SMHM) relation down masses of 10$^5$ M$_\odot$. find no detectable differences among SMHM relations four galaxy clusters or between cluster and field we agreement with extrapolations previous derived using abundance matching approaches. fit power law our empirical adopted NFW dark matter profiles M$_* < 10^9$ M$_\odot$, is M$_h = 10^{10.35\pm0.02}({\rm M}_*/10^8 {\rm M}_\odot)^{0.63\pm0.02}$. The normalisation this susceptible systematic modelling errors depend on potential quoted uncertainties refer in median relation. For 10^{9}$ M$_\odot$ satisfy selection criteria, scatter about $M_h$, including arising from methodology, 0.3 dex. Finally, place lower luminosity Local Group relationship same technique, extending it \sim 10^3$ suggest some these show evidence additional interior effective radius beyond provided by standard profile. If form central black hole, hole are range intermediate holes, $10^{(5.7\pm0.6)}$ which corresponds few percent M$_h$, well above values extrapolated relationships describing more massive galaxies.