RT Journal Article
T1 A comprehensive study of NGC 2023 with XMM-Newton and Spitzer*
A1 López García, M. A.
A1 López Santiago, J.
A1 Albacete Colombo, J. F.
A1 Pérez González, Pablo Guillermo
A1 Castro Rubio, Elisa De
AB 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 to 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 and the presence of accretion discs) of the stars detected in an XMM-Newton observation. This study has allowed us to analyse 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.
PB Wiley
SN 0035-8711
YR 2013
FD 2013-02
LK https://hdl.handle.net/20.500.14352/34699
UL https://hdl.handle.net/20.500.14352/34699
LA eng
NO This article has been accepted for publication in Monthly notices of the Royal Astronomical Society © 2013 MNRAS. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved. MAL-G and JL-S acknowledge support by the Spanish Ministerio de Ciencía e Innovación under grant AYA2008-06423-C03-03. JFA-C is a researcher of the CONICET and acknowledges support by grant PICT 2007-02177 (SecyT). PGP-G acknowledges support from the Spanish Programa Nacional de Astronomía y Astrofísica under grants AYA2009-10368 and AYA2009-07723-E. We would like to acknowledge the anonymous referee for a fruitful discussion about the results of this work. His/her comments on the text content have allowed us to notoriously improve this manuscript.
NO Spanish Ministerio de Ciencía e Innovación
NO SecyT
NO Spanish Programa Nacional de Astronomía y Astrofísica
DS Docta Complutense
RD 10 abr 2025