Polarized near-infrared light of the Dusty S-cluster Object (DSO/G2) at the Galactic Center

TL;DR

This study uses near-infrared polarimetric imaging to analyze the Dusty S-cluster Object (DSO/G2) near the Galactic Center, revealing it as a polarized, dust-enshrouded young star with a bow shock, whose polarization properties vary as it approaches Sgr A*.

Contribution

First polarimetric analysis of DSO/G2 providing insights into its nature and structure, suggesting it is a young star with a bow shock and modeling its polarization behavior.

Findings

DSO is an intrinsically polarized source with >20% polarization degree.

The polarization angle varies as the source approaches Sgr A*.

The source likely has a non-spherical geometry modeled as a bow shock with bipolar wind.

Abstract

We investigate an infrared-excess source called G2 or Dusty S-cluster Object (DSO) moving on a highly eccentric orbit around the Galaxy's central black hole, Sgr A*. We use, for the first time, near-infrared polarimetric imaging data to determine the nature and the properties of the DSO, and obtain an improved K_s-band identification of this source in median polarimetry images of different observing years. The source starts to deviate from the stellar confusion in 2008, and it does not show any flux density variability over the years we analyzed it. We measure the polarization degree and angle of the DSO between 2008 and 2012 and conclude, based on the significance analysis on polarization parameters, that it is an intrinsically polarized source (>20%) with a varying polarization angle as it approaches Sgr A* position. DSO shows a near-infrared excess of K_s-L' > 3 that remains compact close to the pericenter of its orbit. Its observed parameters and the significant polarization obtained in this work show that the DSO might be a dust-enshrouded young star, forming a bow shock as it approaches the super massive black hole. The significantly high measured polarization degree indicates that it has a non-spherical geometry and it can be modelled as a combination of a bow shock with a bipolar wind of the star. We use a 3D radiative transfer model that can reproduce the observed properties of the source such as the total flux density and the polarization degree. We obtain that the change of the polarization angle can be due to an intrinsic change in the source structure. Accretion disc precession of the young star in the gravitational field of the black hole can lead to the change of the bipolar outflow and therefore the polarization angle variation. It might also be the result of the source interaction with the ambient medium.