The late-type stellar density profile in the Galactic Center: A statistical approach

TL;DR

This paper introduces a statistical method leveraging new astrometric data to better determine the three-dimensional density profile of late-type stars in the Galactic Center, addressing previous projection correction uncertainties.

Contribution

It develops a novel statistical approach that utilizes measured projected accelerations to directly infer the line-of-sight distances, improving the accuracy of the stellar density profile.

Findings

Six new projected radial accelerations measured

Enhanced constraints on the stellar density profile

Evidence supporting a relaxed cusp in the Galactic Center

Abstract

The late-type stellar population in the Galactic Center was first predicted to reside in a dynamically relaxed cusp (power law slope ranging from 3/2 to 7/4). However, observations - which rely on models to correct for projection effects - have suggested a flat distribution instead. The need for this correction is due to the lack of information regarding the line-of-sight distances. With a two decade long baseline in astrometric measurements, we are now able to measure significant projected radial accelerations, six of which are newly reported here, that directly constrain line-of-sight distances. Here we present a statistical approach to take advantage of this information and more accurately constrain the shape of the radial density profile of the late-type stellar population in the Galactic Center.