TY  - JOUR
A1  - Henault-Brunet, V.
A1  - Oskinova, Lida
A1  - Guerrero, M. A.
A1  - Sun, W.
A1  - Chu, Y.-H.
A1  - Evans, C. J.
A1  - Gallagher, J. S.
A1  - Gruendl, R. A.
A1  - Reyes-Iturbide, J.
T1  - Discovery of a Be/X-ray pulsar binary and associated supernova remnant in the wing of the small magellanic cloud
JF  - Monthly notices of the Royal Astronomical Society
N2  - We report on a new Be/X-ray pulsar binary located in the Wing of the Small Magellanic Cloud (SMC). The strong pulsed X-ray source was discovered with the Chandra and XMM-Newton X-ray observatories. The X-ray pulse period of 1062 s is consistently determined from both Chandra and XMM-Newton observations, revealing one of the slowest rotating X-ray pulsars known in the SMC. The optical counterpart of the X-ray source is the emission-line star 2dFS 3831. Its B0-0.5(III)e+ spectral type is determined from VLT-FLAMES and 2dF optical spectroscopy, establishing the system as a Be/X-ray binary (Be-XRB). The hard X-ray spectrum is well fitted by a power law with additional thermal and blackbody components, the latter reminiscent of persistent Be-XRBs. This system is the first evidence of a recent supernova in the low-density surroundings of NGC602. We detect a shell nebula around 2dFS 3831 in H alpha and [OIII] images and conclude that it is most likely a supernova remnant. If it is linked to the supernova explosion that created this new X-ray pulsar, its kinematic age of (2-4) x 10(4) yr provides a constraint on the age of the pulsar.
KW  - stars: emission-line, Be
KW  - ISM: supernova remnants
KW  - Magellanic Clouds
KW  - X-rays: binaries
Y1  - 2012
U6  - https://doi.org/10.1111/j.1745-3933.2011.01183.x
SN  - 0035-8711
VL  - 420
IS  - 1
SP  - L13
EP  - L17
PB  - Wiley-Blackwell
CY  - Malden
ER  -