2022A&A...661A..37S


Query : 2022A&A...661A..37S

2022A&A...661A..37S - Astronomy and Astrophysics, volume 661A, 37-37 (2022/5-1)

First studies of the diffuse X-ray emission in the Large Magellanic Cloud with eROSITA.

SASAKI M., KNIES J., HABERL F., MAITRA C., KERP J., BYKOV A.M., DENNERL K., FILIPOVIC M.D., FREYBERG M., KORIBALSKI B.S., POINTS S. and STAVELEY-SMITH L.

Abstract (from CDS):


Context. In the first months after its launch in July 2019, the extended Roentgen Survey with an Imaging Telescope Array (eROSITA) on board Spektrum-Roentgen-Gamma performed long-exposure observations in the regions around supernova (SN) 1987A and super-nova remnant (SNR) N132D in the Large Magellanic Cloud (LMC).
Aims. We analysed the distribution and the spectrum of the diffuse X-ray emission in the observed fields to determine the physical properties of the hot phase of the interstellar medium (ISM).
Methods. Spectral extraction regions were defined using the Voronoi tessellation method. The spectra were fit with a combination of thermal and non-thermal emission models. The eROSITA data are complemented by newly derived column density maps for the Milky Way and the LMC, 888 MHz radio continuum map from the Australian Square Kilometer Array Pathfinder, and optical images of the Magellanic Cloud Emission Line Survey.
Results. We detect significant emission from thermal plasma with kT = 0.2 keV in all the regions. There is also an additional higher- temperature emission component from a plasma with kT ~= 0.7 keV. The surface brightness of this component is one order of magnitude lower than that of the lower-temperature component. In addition, non-thermal X-ray emission is significantly detected in the superbubble 30 Dor C. The absorbing column density NH in the LMC derived from the analysis of the X-ray spectra taken with eROSITA is consistent with the NH obtained from the emission of the cold medium over the entire area. Neon abundance is enhanced in the regions in and around 30 Dor and SN 1987A, indicating that the ISM has been chemically enriched by the young stellar population. In the centre of 30 Dor, there are two bright extended X-ray sources, which coincide with the stellar cluster RMC 136 and the Wolf-Rayet stars RMC 139 and RMC 140. For both regions the emission is best modelled with a high-temperature (kT > 1 keV) non-equilibrium ionisation plasma emission and a non-thermal component with a photon index of Γ = 1.3. In addition, we detect an extended X-ray source at the position of the optical SNR candidate J0529-7004 with thermal emission, and thus confirm its classification as an SNR.
Conclusions. Using data from the early observations of the regions around SN 1987A and SNR N132D with eROSITA we confirm that there is thermal interstellar plasma in the entire observed field. eROSITA with its large field of view and high sensitivity at lower X-ray energies allows us for the first time to carry out a detailed study of the ISM at high energies consistently over a large region in the LMC. We thus measure the properties of the interstellar plasma and the distribution of non-thermal particles and derive the column density of the cold matter on the line of sight.

Abstract Copyright: © ESO 2022

Journal keyword(s): Magellanic Clouds - X-rays: ISM - ISM: structure - ISM: bubbles - ISM: supernova remnants - ISM: abundances

Status at CDS : Examining the need for a new acronym.

Simbad objects: 29

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Number of rows : 29
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 NGC 104 GlC 00 24 05.359 -72 04 53.20   5.78 4.09     ~ 3736 0
2 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 10314 1
3 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 6371 1
4 ACO 3158 ClG 03 42 39.6 -53 37 50           ~ 283 0
5 NGC 1918 SNR 05 19 04.50 -69 38 56.0           ~ 97 0
6 SNR B0519-69.0 SNR 05 19 35.14 -69 02 00.5           ~ 145 0
7 SNR J051945-692600 SNR 05 19 45.00 -69 26 00.0           ~ 44 0
8 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 16153 1
9 SNR J052501-693842 SNR 05 25 02.20 -69 38 39.0           ~ 380 1
10 SNR J052741-691207 SNR 05 27 39.00 -69 12 12.0           ~ 36 0
11 SN 1987A SN* 05 35 28.020 -69 16 11.07           SNIIpec 4721 2
12 NAME Honeycomb Nebula SNR 05 35 46 -69 18.0           ~ 46 0
13 NAME 30 Dor C Superbubble Rad 05 35 50.8 -69 12 22           ~ 46 1
14 NAME 30 Dor C Rad 05 36 07.70 -69 11 52.6           ~ 71 1
15 MCSNR J0536-6913 SNR 05 36 17.0 -69 13 28           ~ 10 0
16 NGC 2060 SNR 05 37 51.4466169456 -69 10 23.947092084   9.69 9.59     ~ 339 2
17 MCSNR J0538-6921 SR? 05 38 12.9 -69 21 41           ~ 2 0
18 NAME 30 Dor Nebula SFR 05 38 36.0 -69 05 11           ~ 1114 2
19 RMC 140 WR* 05 38 41.62 -69 05 14.0   11.213 11.616     WN7+WC4/5pec 78 0
20 RMC 139 WR* 05 38 42.3537501576 -69 04 58.196699796   12.04 11.94     O6.5Iafc+O6Iaf 88 0
21 RMC 136 Cl* 05 38 42.396 -69 06 03.36           ~ 1872 1
22 BAT99 108 WR* 05 38 42.43 -69 06 02.2   12.78 12.77     WN5h 72 0
23 X LMC X-1 HXB 05 39 38.8284304464 -69 44 35.531553624   14.8 14.5     O8(f)p 602 2
24 PSR B0540-69 Psr 05 40 10.84 -69 19 54.2           ~ 849 3
25 NAME LMC 2 Supergiant Shell sh 05 41 27 -69 22.4           ~ 180 0
26 SNR B0543-68.9 SNR 05 43 08 -68 58.3           ~ 55 0
27 NAME LHB X 16 42.0 +02 19           ~ 296 0
28 Cl Westerlund 1 OpC 16 47 04.00 -45 51 04.9           ~ 511 0
29 NAME Local Group GrG ~ ~           ~ 7717 0

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2022.08.09-16:47:01

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