2025A&A...700A.137M


Query : 2025A&A...700A.137M

2025A&A...700A.137M - Astronomy and Astrophysics, volume 700A137 (2025/8-1)

Studying the multiphase interstellar medium in the Large Magellanic Cloud with SRG/eROSITA I. Analysis of diffuse X-ray emission.

MAYER M.G.F., SASAKI M., HABERL F., TSUGE K., FUKUI Y., MAITRA C., FILIPOVIC M.D., SMEATON Z.J., STAVELEY-SMITH L., KORIBALSKI B., POINTS S. and KAVANAGH P.

Abstract (from CDS):

Context. The Large Magellanic Cloud (LMC), being a nearby and actively star-forming satellite galaxy of the Milky Way, is an ideal site to observe the multiphase interstellar medium (ISM) of a galaxy across the electromagnetic spectrum.
Aims. We aimed to exploit the available SRG/eROSITA all-sky survey data to study the distribution, composition and properties of the diffuse X-ray emitting hot gas in the LMC.
Methods. We constructed multiband X-ray images of the LMC, reflecting the morphology and temperatures of the diffuse hot gas. By performing spatially resolved X-ray spectroscopy of 175 independent regions, we constrained the distribution, temperature, mass, energetics and composition of the hot ISM phase throughout the galaxy, while also testing for the presence of X-ray synchrotron emission. We combined our constraints with multiwavelength data to obtain a comprehensive view of the different ISM phases.
Results. We measure a total X-ray luminosity of the hot ISM phase of 1.9 × 1038 erg s–1 (0.2-5.0 keV band), and constrain its thermal energy to around 9 × 1054 erg. The typical density and temperature of the X-ray emitting plasma are around 5 × 10–3 cm–3 and 0.25 keV, respectively, with both exhibiting broad peaks in the southeast of the LMC. The observed degree of X-ray absorption correlates strongly with the distribution of foreground H I gas, whereas a spatial anticorrelation between the hot and cold ISM phases is visible on sub-kpc scales within the disk. The abundances of light metals show a strong gradient throughout the LMC, with the north and east exhibiting a strong α-enhancement, as expected from observed massive stellar populations there. In contrast, the enigmatic “X-ray spur” exhibits a local deficit in α-elements, and a peak in hot-gas pressure at P/k ∼ 105 K cm–3, consistent with a dominant energy input through tidally driven gas collisions. Finally, we tentatively identify spectroscopic signatures of nonthermal X-ray emission from the supergiant shell LMC 2, although contamination by straylight cannot be excluded.

Abstract Copyright: © The Authors 2025

Journal keyword(s): ISM: abundances - ISM: structure - X-rays: ISM

Simbad objects: 22

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Number of rows : 22
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026
#notes
1 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 12317 1
2 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 7988 0
3 NAME Magellanic Bridge HI 03 11 -77.5           ~ 522 1
4 LHA 120-N 11 HII 04 56 51.4 -66 24 24           ~ 275 0
5 X LMC X-2 LXB 05 20 29.0 -71 57 33 17.20 18.00 18.0     ~ 189 0
6 NAME LMC Bar PoG 05 22 08 -69 23.5           ~ 343 0
7 NAME LMC 5 Supergiant Shell sh 05 22 42 -66 05.6           ~ 56 0
8 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 19090 0
9 MCSNR J0525-6938 SNR 05 25 02.3 -69 38 39           ~ 446 1
10 SNR B0525-66.0 SNR 05 25 27.1 -65 59 11           ~ 111 1
11 SNR J052559-660453 SNR 05 26 00.4 -66 05 02     12.71     ~ 456 2
12 NAME LMC 4 Supergiant Shell sh 05 31 33 -66 40.5           ~ 183 0
13 SNR B0535-66.0 SNR 05 35 43.1 -66 01 59           ~ 193 1
14 NAME 30 Dor C Rad 05 36 07.70 -69 11 52.6           ~ 87 1
15 NGC 2044 As* 05 36 11 -69 11.8   10.69 10.59     ~ 89 0
16 NAME 30 Dor Region reg 05 38.0 -69 06           ~ 261 0
17 NAME 30 Dor Nebula SFR 05 38 36.0 -69 05 11           ~ 1276 2
18 RMC 136 Cl* 05 38 42.396 -69 06 03.36   5.81 5.40     ~ 2236 2
19 X LMC X-1 HXB 05 39 38.8284304464 -69 44 35.531553624   14.8 14.5 14.924   O8(f)p 700 0
20 [KDS99] SGS 17 sh 05 40 26 -68 19.0           ~ 9 0
21 NAME LMC 2 Supergiant Shell sh 05 41 27 -69 22.4           ~ 200 0
22 M 51 Sy2 13 29 52.698 +47 11 42.93   9.26 8.36 8.40   ~ 4565 4

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