Leo V: Spectroscopy of a Distant and Disturbed Satellite

TL;DR

This study spectroscopically analyzes Leo V, a distant Milky Way satellite, revealing its velocity dispersion, mass, metallicity, and potential tidal disruption, with implications for its dark matter content and orbital history.

Contribution

First spectroscopic analysis of Leo V revealing its velocity dispersion, mass, metallicity, and potential tidal disruption features.

Findings

Leo V has a velocity dispersion of ~2.4 km/s in the core.

Estimated dynamical mass of Leo V is ~3.3 x 10^5 solar masses.

Leo V shows signs of mass loss and possible tidal disruption.

Abstract

We present a spectroscopic study of Leo V, a recently discovered satellite of the Milky Way (MW). From stellar spectra obtained with the MMT/Hectochelle spectrograph we identify seven likely members of Leo V. Five cluster near the Leo V center (R < 3 arcmin) and have velocity dispersion 2.4_{-1.4}^{+2.4} km/s. The other two likely members lie near each other but far from the center (R~13 arcmin ~ 700 pc) and inflate the global velocity dispersion to 3.7_{-1.4}^{+2.3} km/s. Assuming the five central members are bound, we obtain a dynamical mass of M=3.3_{-2.5}^{+9.1} x 10^5M_{sun} (M/L_V=75_{-58}^{+230}[M/L_V]_{sun}). From the stacked spectrum of the five central members we estimate a mean metallicity of [Fe/H]=-2.0\pm 0.2 dex. Thus with respect to dwarf spheroidals of similar luminosity, Leo V is slightly less massive and slightly more metal-rich. Since we resolve the central velocity dispersion only marginally, we do not rule out the possibility that Leo V is a diffuse star cluster devoid of dark matter. The wide separation of its two outer members implies Leo V is losing mass; however, its large distance (D ~ 180 kpc) is difficult to reconcile with MW tidal stripping unless the orbit is very radial.