Global Properties of M31's Stellar Halo from the SPLASH Survey. I. Surface Brightness Profile

TL;DR

This study maps the surface brightness profile of M31's stellar halo out to 175 kpc using spectroscopic data, revealing a power-law distribution, halo shape, and evidence of accreted substructures, enhancing understanding of galaxy halos.

Contribution

First detailed spectroscopic surface brightness profile of M31's halo extending to large radii, identifying substructure and halo shape with improved contamination rejection.

Findings

Halo follows a power-law with index -2.2 +/- 0.2

Halo is likely prolate or spherical, aligned with M31's minor axis

Outer halo shows significant substructure from accreted stars

Abstract

We present the surface brightness profile of M31's stellar halo out to a projected radius of 175 kpc. The surface brightness estimates are based on confirmed samples of M31 red giant branch stars derived from Keck/DEIMOS spectroscopic observations. A set of empirical spectroscopic and photometric M31 membership diagnostics is used to identify and reject foreground and background contaminants. This enables us to trace the stellar halo of M31 to larger projected distances and fainter surface brightnesses than previous photometric studies. The surface brightness profile of M31's halo follows a power-law with index -2.2 +/- 0.2 and extends to a projected distance of at least ~175 kpc (~ 2/3 of M31's virial radius), with no evidence of a downward break at large radii. The best-fit elliptical isophotes have b/a=0.94 with the major axis of the halo aligned along the minor axis of M31's disk, consistent with a prolate halo, although the data are also consistent with M31's halo having spherical symmetry. The fact that tidal debris features are kinematically cold is used to identify substructure in the spectroscopic fields out to projected radii of 90 kpc, and investigate the effect of this substructure on the surface brightness profile. The scatter in the surface brightness profile is reduced when kinematically identified tidal debris features in M31 are statistically subtracted; the remaining profile indicates a comparatively diffuse stellar component to M31's stellar halo exists to large distances. Beyond 90 kpc, kinematically cold tidal debris features can not be identified due to small number statistics; nevertheless, the significant field-to-field variation in surface brightness beyond 90 kpc suggests that the outermost region of M31's halo is also comprised to a significant degree of stars stripped from accreted objects.