TY - JOUR
T1 - Multiwavelength analysis of the X-ray spur and southeast of the Large Magellanic Cloud
AU - Knies, J. R.
AU - Sasaki, M.
AU - Fukui, Y.
AU - Tsuge, K.
AU - Haberl, F.
AU - Points, S.
AU - Kavanagh, P. J.
AU - Filipovic, M. D.
PY - 2021
Y1 - 2021
N2 - 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.
AB - 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.
UR - https://hdl.handle.net/1959.7/uws:63209
U2 - 10.1051/0004-6361/202038488
DO - 10.1051/0004-6361/202038488
M3 - Article
SN - 0004-6361
VL - 648
JO - Astronomy and Astrophysics
JF - Astronomy and Astrophysics
M1 - A90
ER -