Dynamics and Stellar Content of the Giant Southern Stream in M31. I. Keck Spectroscopy of Red Giant Stars

Abstract

This paper presents the first results from a large spectroscopic survey of red giant branch ( RGB) stars in M31 using DEIMOS on the Keck 10 m telescope. A photometric prescreening method, based on the intermediate-width DDO51 band centered on the Mg b/MgH absorption feature, was used to select spectroscopic targets. RGB candidates were targeted in a small section of M31's giant southern tidal stream at a projected distance of 31 kpc from the galaxy's center. We isolate a clean sample of 68 RGB stars by removing contaminants (foreground Milky Way dwarf stars and background galaxies) using a combination of spectroscopic, imaging, and photometric methods: radial velocity and the surface gravity-sensitive Na i doublet are particularly useful in this regard. About 65% of the M31 stars are found to be members of the giant southern stream, while the rest appear to be members of the general spheroid population. The mean (heliocentric) radial velocity of the stream in our field is À458 km s À1 , blueshifted by À158 km s À1 relative to M31's systemic velocity, in good agreement with recent velocity measurements at other points along the stream. The intrinsic velocity dispersion of the stream is found to be 15 þ8 À15 km s À1 (90% confidence limit). A companion paper by Font and coworkers discusses possible orbits, implications of the coldness of the stream, and properties of the progenitor satellite galaxy. The kinematics, and possibly the metallicity distribution, of the general spheroid (i.e., nonstream) population in this region of M31 indicate that it is significantly different from samples drawn from other parts of the M31 spheroid; this is probably an indication of substructure in the bulge and halo. The stream appears to have a higher mean metallicity than the general spheroid, h½Fe/H i $ À0:54 versus À0.74, and a smaller metallicity spread. The relatively high metallicity of the stream implies that its progenitor must have been a luminous dwarf galaxy. The Ca ii triplet line strengths of the M31 RGB stars are generally consistent with photometric estimates of their metallicity (derived by fitting RGB fiducials in the color-magnitude diagram). There is indirect evidence of a population of intermediate-age stars in the stream.

Substructure and Tidal Streams in the Andromeda Galaxy and its Satellites

“…Roughly 50% of the stellar mass in the GSS fields was in place ∼ 9 Gyr ago, and the metallicity had reached the solar value by 5 Gyr ago, consistent with direct spectroscopy constraints from RGB stars (e.g. Guhathakurta et al, 2006;Kalirai et al, 2006;Gilbert et al, 2009). In addition, all the GSS fields probed thus far reveal a large spread in metallicity (≥ 1.5 dex).…”

Constraints on the Formation of M31’s Stellar Halo from the SPLASH Survey

“…The velocity distributions of spectroscopically confirmed M31 stars in individual fields have been analyzed to identify and characterize tidal debris features, including measurements along the giant southern stream (GSS)-the most prominent tidal stream in M31's stellar halo [25][26][27]35,40,41].…”

Collision Tomography: Physical Properties of Possible Progenitors of the Andromeda Stellar Stream

“…This hypothesis is supported by the discovery of tidal features such as the Sagittarius stream and the giant stellar stream in M31. Furthermore, photometric and spectroscopic observations of the spatial distribution and radial velocity distribution of red giant stars and of the metallicity distribution near these galaxies have revealed other substructures (Ferguson et al 2002;Ibata et al 2004Ibata et al , 2005Ibata et al , 2007Guhathakurta et al 2006;Koch et al 2008).…”

“…Recent observations of red giant stars near M31 have revealed a giant stellar stream to its south as well as giant stellar shells to the east and west of its center (Ibata et al 2001(Ibata et al , 2004Ferguson et al 2002;McConnachie et al 2003;Guhathakurta et al 2006;Koch et al 2008). The giant stellar stream extends out to over 100 kpc from M31ʼs center (McConnachie et al 2003).…”