Issue |
A&A
Volume 401, Number 2, April II 2003
|
|
---|---|---|
Page(s) | 625 - 630 | |
Section | Stellar structure and evolution | |
DOI | https://doi.org/10.1051/0004-6361:20021871 | |
Published online | 21 March 2003 |
Point X-ray sources in the SNR G 315.4-2.30 (MSH 14-63, RCW 86)
1
Sternberg Astronomical Institute, Moscow State University, Universitetskij Pr. 13, Moscow 119992, Russia
2
E.K.Kharadze Abastumani Astrophysical Observatory, Georgian Academy of Sciences, A.Kazbegi ave. 2-a, Tbilisi 380060, Georgia
3
Abdus Salam International Centre for Theoretical Physics, Strada Costiera 11, PO Box 586, 34100 Trieste, Italy
4
Space Research Institute, Russian Academy of Sciences, Profsoyuznaya 84/32, Moscow 117997, Russia
Corresponding author: V. V. Gvaramadze, vgvaram@sai.msu.ru
Received:
1
August
2002
Accepted:
28
October
2002
We report the results of a search for a point X-ray
source (stellar remnant) in the southwest protrusion of the
supernova remnant G 315.4-2.30 (MSH 14-63, RCW 86)
using the archival data of the Chandra X-ray Observatory.
The search was motivated by a hypothesis that G 315.4-2.30 is
the result of an off-centered cavity supernova explosion of a
moving massive star, which ended its evolution just near the edge
of the main-sequence wind-driven bubble. This hypothesis implies
that the southwest protrusion in G 315.4-2.30 is the remainder
of a pre-existing bow shock-like structure created by the
interaction of the supernova progenitor's wind with the
interstellar medium and that the actual location of the supernova
blast center is near the center of this hemispherical structure.
We have discovered two point X-ray sources in the “proper" place.
One of the sources has an optical counterpart with the
photographic magnitude , while the spectrum of the
source can be fitted with an optically thin plasma model. We
interpret this source as a foreground active star of late spectral
type. The second source has no optical counterpart to a limiting
magnitude ~21. The spectrum of this source can be fitted
almost equally well with several simple models (power law: photon
index
; two-temperature blackbody:
keV,
km and
keV,
km; blackbody plus
power law:
keV, photon index
). We interpret this
source as a candidate stellar remnant (neutron star), while the
photon index and non-thermal luminosity of the source (almost the
same as those of the Vela pulsar and the recently discovered
pulsar PSR J 0205+6449 in the supernova remnant 3C 58) suggest
that it can be a young “ordinary" pulsar.
Key words: stars: neutron / ISM: bubbles / ISM: individual objects: G 315.4-2.30 (MSH 14-63, RCW 86) / ISM: supernova remnants / X-ray: stars
© ESO, 2003
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