Gemini spectroscopy of the outer disk star cluster BH176

TL;DR

This study uses spectroscopic and photometric data to determine the properties and origin of the old, metal-rich star cluster BH176, suggesting it belongs to the thick disk and may have formed through a high-velocity gas cloud encounter or as a satellite dwarf galaxy.

Contribution

First detailed spectroscopic analysis of BH176 combining multiple methods to determine its properties and origin.

Findings

BH176 has a metallicity of [Fe/H] = -0.1±0.1.

Age of BH176 is approximately 7±0.5 Gyr.

BH176 is likely part of the thick disk and may have formed from a high-velocity gas cloud encounter.

Abstract

BH176 is an old metal-rich star cluster. It is spatially and kinematically consistent with belonging to the Monoceros Ring. It is larger in size and more distant from the Galactic plane than typical open clusters, and it does not belong to the Galactic bulge. Our aim is to determine the origin of this unique object by accurately determining its distance, metallicity, and age. The best way to reach this goal is to combine spectroscopic and photometric methods. We present medium-resolution observations of red clump and red giant branch stars in BH176 obtained with the Gemini South Multi-Object Spectrograph.We derive radial velocities, metallicities, effective temperatures, and surface gravities of the observed stars and use these parameters to distinguish member stars from field objects. We determine the following parameters for BH176: $V_h= 0\pm 15$ km/s, $[Fe/H]=-0.1\pm 0.1$, age $7\pm 0.5$ Gyr, $E(V-I)=0.79\pm 0.03$, distance $ 15.2\pm 0.2$ kpc, $\alpha$-element abundance $[\alpha/Fe] \sim 0.25$ dex (the mean of [Mg/Fe], and [Ca/Fe]). BH176 is a member of old Galactic open clusters that presumably belong to the thick disk. It may have originated as a massive star cluster after the encounter of the forming thin disk with a high-velocity gas cloud or as a satellite dwarf galaxy.