Issue |
A&A
Volume 648, April 2021
|
|
---|---|---|
Article Number | A90 | |
Number of page(s) | 20 | |
Section | Interstellar and circumstellar matter | |
DOI | https://doi.org/10.1051/0004-6361/202038488 | |
Published online | 16 April 2021 |
Multiwavelength analysis of the X-ray spur and southeast of the Large Magellanic Cloud
1
Dr. Karl Remeis Observatory and ECAP, Universität Erlangen-Nürnberg,
Sternwartstraße 7,
96049
Bamberg, Germany
e-mail: jonathan.knies@fau.de
2
Department of Physics, Nagoya University,
Furo-cho, Chikusa-ku,
Nagoya
464-8601, Japan
3
Max-Planck-Institut für extraterrestrische Physik,
Gießenbachstraße 1,
85741
Garching, Germany
4
Cerro Tololo Inter-American Observatory,
Casilla 603,
La Serena, Chile
5
School of Cosmic Physics, Dublin Institute for Advanced Studies,
31 Fitzwilliam Place,
Dublin 2, Ireland
6
Western Sydney University,
Locked Bag 1797,
Penrith South DC,
NSW 2751, Australia
Received:
25
May
2020
Accepted:
26
January
2021
Aims. The giant H II region 30 Doradus (30 Dor) located in the eastern part of the Large Magellanic Cloud is one of the most active star-forming regions in the Local Group. Studies of H I data have revealed two large gas structures which must have collided with each other in the region around 30 Dor. In X-rays there is extended emission (~1 kpc) south of 30 Dor called the X-ray spur, which appears to be anticorrelated with the H I gas. We study the properties of the hot interstellar medium (ISM) in the X-ray spur and investigate its origin including related interactions in the ISM.
Methods. We analyzed new and archival XMM-Newton data of the X-ray spur and its surroundings to determine the properties of the hot diffuse plasma. We created detailed plasma property maps by utilizing the Voronoi tessellation algorithm. We also studied H I and CO data, as well as optical line emission data of Hα and [S II], and compared them to the results of the X-ray spectral analysis.
Results. We find evidence of two hot plasma components with temperatures of kT1 ~ 0.2 keV and kT2 ~ 0.5−0.9 keV, with the hotter component being much more pronounced near 30 Dor and the X-ray spur. In 30 Dor, the plasma has most likely been heated by massive stellar winds and supernova remnants. In the X-ray spur, we find no evidence of heating by stars. Instead, the X-ray spur must have been compressed and heated by the collision of the H I gas.
Key words: ISM: general / ISM: structure / galaxies: ISM / Magellanic Clouds / X-rays: ISM / radio lines: ISM
© ESO 2021
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