2015A&A...579A..63K


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.13CEST07:25:06

2015A&A...579A..63K - Astronomy and Astrophysics, volume 579A, 63-63 (2015/7-1)

XMM-Newton observation of SNR J0533-7202 in the Large Magellanic Cloud.

KAVANAGH P.J., SASAKI M., WHELAN E.T., MAGGI P., HABERL F., BOZZETTO L.M., FILIPOVIC M.D. and CRAWFORD E.J.

Abstract (from CDS):

We present an X-ray study of the supernova remnant SNR J0533-7202 in the Large Magellanic Cloud (LMC) and determine its physical characteristics based on its X-ray emission.We observed SNR J0533-7202 with XMM-Newton (background flare-filtered exposure times of 18ks EPIC-pn and 31ks EPIC-MOS1, EPIC-MOS2). We produced X-ray images of the supernova remnant, performed an X-ray spectral analysis, and compared the results to multi-wavelength studies.The distribution of X-ray emission is highly non-uniform, with the south-west region much brighter than the north-east. The detected X-ray emission is correlated with the radio emission from the remnant. We determine that this morphology is most likely due to the supernova remnant expanding into a non-uniform ambient medium and not an absorption effect. We estimate the remnant size to be 53.9(±3.4)x43.6(±3.4)pc, with the major axis rotated ∼64° east of north. We find no spectral signatures of ejecta emission and infer that the X-ray plasma is dominated by swept up interstellar medium. Using the spectral fit results and the Sedov self-similar solution, we estimate the age of SNR J0533-7202 to be ∼17-27kyr, with an initial explosion energy of (0.09-0.83)x1051erg. We detected an X-ray source located near the centre of the remnant, namely XMMU J053348.2-720233. The source type could not be conclusively determined due to the lack of a multi-wavelength counterpart and low X-ray counts. We found that it is likely either a background active galactic nucleus or a low-mass X-ray binary in the LMC.We detected bright thermal X-ray emission from SNR J0533-7202 and determined that the remnant is in the Sedov phase of its evolution. The lack of ejecta emission prohibits us from typing the remnant with the X-ray data. Therefore, the likely Type Ia classification based on the local stellar population and star formation history reported in the literature cannot be improved upon.

Abstract Copyright:

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

Simbad objects: 7

goto Full paper

goto View the reference in ADS

Number of rows : 7

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 5669 1
2 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 14832 1
3 SNR J053346-720259 SNR 05 33 46.5 -72 02 59           ~ 6 0
4 XMMU J053348.2-720233 X 05 33 48.2 -72 02 33           ~ 1 0
5 1RXS J053353.6-720404 X 05 33 53.602 -72 04 04.51           ~ 8 0
6 NAME LHB X 16 42.0 +02 19           ~ 257 0
7 NAME Local Group GrG ~ ~           ~ 6973 0

    Equat.    Gal    SGal    Ecl

To bookmark this query, right click on this link: simbad:objects in 2015A&A...579A..63K and select 'bookmark this link' or equivalent in the popup menu


2020.07.13-07:25:06

© Université de Strasbourg/CNRS

    • Contact