eROSITA (eRASS1) study of the Canis Major overdensity: Developing a multi-wavelength algorithm for classifying faint X-ray sources

TL;DR

This study uses eROSITA X-ray data to classify faint sources in the Canis Major overdensity, developing a multi-wavelength algorithm that distinguishes between Galactic and extragalactic objects, revealing diverse stellar populations and potential members of the overdensity.

Contribution

The paper introduces a novel multi-wavelength classification algorithm for faint X-ray sources in dense regions, applied to the first eROSITA survey of the Canis Major overdensity.

Findings

Classified over 8,000 X-ray sources into Galactic and extragalactic categories.

Identified 34 symbiotic star candidates and M-giant counterparts in CMa OD.

Detected potential members of CMa OD, including X-ray binaries and quiescent sources.

Abstract

Using the data of eROSITA (extended Roentgen Survey with an Imaging Telescope Array) on board Spektrum-Roentgen-Gamma (Spektr-RG, SRG) taken during the first eROSITA all-sky survey (eRASS1), we perform the first X-ray classification and population study in the field of Canis Major overdensity (CMa OD), which is an elliptical-shaped stellar overdensity located at l = -240, b = -80. The study aims to identify the X-ray sources in CMa OD. For this purpose, we developed a classification algorithm using multi-wavelength criteria as a preliminary method for the classification of faint X-ray sources, specifically in regions with a high source number density. Out of a total number of 8311 X-ray sources, we have classified 1029 sources as Galactic stars and binaries in the foreground, 946 sources as active galactic nuclei (AGN) and galaxies in the background, and 435 sources with stellar counterparts, which can belong to either the MW or CMa OD. Among the sources with a stellar counterpart, we have identified 34 symbiotic star candidates, plus 335 sources, of which the infrared counterparts have properties of M-giants in CMa OD. Moreover, there is a known high-mass X-ray binary (HMXB, 4U 0728-25) in the field of our study, which, according to the Gaia parallax of its companion, seems to be a member of CMa OD. There is also a recently detected transient low-mass X-ray binary (LMXB, SRGt J071522.1-191609), which can be a member of CMa OD based on its companion that is most likely highly absorbed and is thus located behind the Galactic disk. In addition, we present the X-ray luminosity function (XLF) of members and candidate members of CMa OD. It is dominated by sources with luminosities of < 2*10^32-10^33 erg/s in the energy range of 0.2-2.3 keV, which are expected to be either accreting white dwarfs or quiescent LMXBs.