2022A&A...657A..26M


Query : 2022A&A...657A..26M

2022A&A...657A..26M - Astronomy and Astrophysics, volume 657A, 26-26 (2022/1-1)

Discovery of four super-soft X-ray sources in XMM-Newton observations of the Large Magellanic Cloud.

MAITRA C. and HABERL F.

Abstract (from CDS):

Context. Super-soft X-ray sources were established as a heterogeneous class of objects from observations of the Large Magellanic Cloud (LMC). Aims. We have searched for new sources of this class in the X-ray images obtained from the XMM-Newton survey of the LMC and additional archival observations. Methods. We first selected candidates by visual inspection of the image and screened out the artefacts that can mimic super-soft X-ray sources as well as the bright foreground stars that create optical loading in the detectors. We obtained four new super-soft X-ray sources for which we performed detailed X-ray timing and spectral analyses and searched for possible optical counterparts to identify their nature. We also looked at archival ROSAT and Swift observations to investigate the long-term behaviour of the sources. Results. XMMU J050452.0-683909 is identified as the central star of the planetary nebula SMP LMC 21 in the LMC. We suggest XMMU J051854.8-695601 and XMMU J050815.1-691832 as new soft intermediate polars based on the nature of their X-ray spectrum. Their estimated absorption-corrected luminosities and the blackbody radii indicate that they are located in our Galaxy, rather than the LMC. We discovered coherent pulsations of 497 s from XMMU J044626.6-692011, which indicates a magnetic cataclysmic variable nature of the source. The location of XMMU J044626.6-692011 in the LMC or our Galaxy is less clear. It could either be a white dwarf in the LMC with nuclear burning on its surface near the Eddington limit or another soft intermediate polar in our Galaxy. Conclusions. The discovery of new super-soft X-ray sources makes a significant contribution to the known population in our Galaxy. An observed higher density of sources in the direction of the Magellanic Clouds can likely be explained by the relatively low Galactic column density in their direction as well as a large number of existing observations sensitive at low X-ray energies.

Abstract Copyright: © C. Maitra and F. Haberl 2021

Journal keyword(s): novae - cataclysmic variables - white dwarfs - binaries: close - galaxies: individual: LMC - X-rays: stars

Simbad objects: 23

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Number of rows : 23
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 M 31 G 00 42 44.330 +41 16 07.50 4.86 4.36 3.44     ~ 12097 1
2 RX J004253.0+411533 X 00 42 52.528 +41 15 40.20           ~ 29 0
3 NAME M31PSS CV* 00 43 19.59 +41 17 56.9           ~ 25 0
4 2XMMi J004319.9+411346 No* 00 43 20.00 +41 13 46.0       17.0   ~ 29 0
5 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 10530 1
6 LHA 115-N 67 PN 00 58 37.095 -71 35 48.80   16.3 16.4 15.27 17.66 ~ 90 0
7 RX J0059.4-7118 N* 00 59 27.179 -71 18 27.68           ~ 4 0
8 LIN 357 PN 00 59 40.5128319264 -71 38 15.143769276   17.48 17.856   18.581 ~ 33 0
9 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 6555 1
10 XMMU J044626.6-692011 X 04 46 26.62 -69 20 11.9           ~ 1 0
11 HD 268622 * 04 47 24.7078863480 -69 26 06.430336692   12.000 11.282 11.217   G5 9 0
12 SSTISAGEMC J050451.97-683909.7 pA? 05 04 51.9929947440 -68 39 09.696052080 15.517 16.420 15.531 15.11 16.976 ~ 51 0
13 1RXS J050526.3-684628 X 05 05 20.9 -68 45 47           ~ 4 0
14 LHA 120-N 102 PN 05 08 03.3523991256 -68 40 16.560238548 15.580 16.298 15.406 14.86 16.653 ~ 48 0
15 2RXS J050813.5-691831 X 05 08 23.1 -69 18 00           ~ 3 0
16 3XMM J051034.6-670353 CV? 05 10 34.78 -67 03 54.2           ~ 3 0
17 V* UU Col CV* 05 12 13.2335083440 -32 41 39.743719692   17.72       ~ 44 0
18 XMMU J051854.8-695601 X 05 18 55.3 -69 56 01           ~ 2 0
19 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 16509 1
20 V* V405 Aur CV* 05 57 59.2934496792 +53 53 44.926489464           ~ 125 0
21 V* PQ Gem CV* 07 51 17.3280306912 +14 44 23.874868716           ~ 219 0
22 V* WX Pyx XB* 08 33 05.7636304080 -22 48 31.980809016   18.0       ~ 37 0
23 V* NY Lup XB* 15 48 14.5961459448 -45 28 39.918848376     14.50 14.42   K0/3Ve 95 1

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2023.01.30-22:20:29

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