A comprehensive study of NGC 2023 with XMM-Newton and Spitzer

TL;DR

This study combines X-ray, optical, and infrared data to analyze the properties and evolutionary stages of stars in NGC 2023, revealing similarities with other star-forming regions like Taurus-Auriga.

Contribution

It provides the first spectral energy distribution analysis of X-ray emitting stars in NGC 2023, enhancing understanding of their physical properties and evolutionary stages.

Findings

Stars in NGC 2023 share physical characteristics with those in Taurus-Auriga.

Spectral energy distributions enable determination of stellar evolutionary stages.

X-ray plasma properties are comparable to other nearby star-forming regions.

Abstract

Nearby star-forming regions are ideal laboratories to study high-energy emission of different stellar populations, from very massive stars to brown dwarfs. NGC 2023 is a reflection nebula situated on the south of the Flame Nebula (NGC 2024) and at the edge of the H ii region IC 434, which also contains the Horsehead Nebula (Barnard 33). NGC 2023, NGC 2024, Barnard 33 and the surroundings of the O-type supergiant star {\zeta} Ori constitute the south part of the Orion B molecular complex. In this work, we present a comprehensive study of X-ray emitters in the region of NGC 2023 and its ?surroundings. We combine optical and infrared data to determine physical properties (mass, temperature, luminosity, presence of accretion disks) of the stars detected in an XMM-Newton observation. This study has allowed us to analyze spectral energy distribution of these stars for the first time and determine their evolutionary stage. Properties of the X-ray emitting plasma of these stars are compared to those found in other nearby star-forming regions. The results indicate that the stars that are being formed in this region have characteristics, in terms of physical properties and luminosity function, similar to those found in the Taurus-Auriga molecular complex.