An X-ray study of supernova remnant N49 and soft gamma-ray repeater 0526-66 in the Large Magellanic Cloud

Sangwook Park, John P. Hughes, Patrick O. Slane, David N. Burrows, Jae Joon Lee, Koji Mori

Research output: Contribution to journalArticle

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Abstract

We report on the results from our deep Chandra observation (120ks) of the supernova remnant (SNR) N49 and soft gamma-ray repeater (SGR) 0526-66 in the Large Magellanic Cloud. We firmly establish the detection of an ejecta "bullet" beyond the southwestern boundary of N49. The X-ray spectrum of the bullet is distinguished from that of the main SNR shell, showing significantly enhanced Si and S abundances. We also detect an ejecta feature in the eastern shell, which shows metal overabundances similar to those of the bullet. If N49 was produced by a core-collapse explosion of a massive star, the detected Si-rich ejecta may represent explosive O-burning or incomplete Si-burning products from deep interior of the SN. On the other hand, the observed Si/S abundance ratio in the ejecta may favor Type Ia origin for N49. We refine the Sedov age of N49, τSed 4800yr, with the explosion energy E 0 1.8 × 1051erg. Our blackbody (BB) + power law (PL) model for the quiescent X-ray emission from SGR 0526-66 indicates that the PL photon index (Γ 2.5) is identical to that of PSR 1E1048.1-5937, the well-known candidate transition object between anomalous X-ray pulsars and SGRs. Alternatively, the two-component BB model implies X-ray emission from a small (R 1km) hot spot(s) (kT 1keV) in addition to emission from the neutron star's cooler surface (R 10km, kT 0.4keV). There is a considerable discrepancy in the estimated column toward 0526-66 between BB+PL and BB+BB model fits. Discriminating these spectral models would be crucial to test the long-debated physical association between N49 and 0526-66.

Original languageEnglish (US)
Article number117
JournalAstrophysical Journal
Volume748
Issue number2
DOIs
StatePublished - Apr 1 2012

Fingerprint

repeaters
Magellanic clouds
supernova remnants
ejecta
gamma rays
power law
explosions
explosion
x rays
shell
coolers
massive stars
pulsars
neutron stars
explosive
metal
photons
products
metals
energy

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Park, Sangwook ; Hughes, John P. ; Slane, Patrick O. ; Burrows, David N. ; Lee, Jae Joon ; Mori, Koji. / An X-ray study of supernova remnant N49 and soft gamma-ray repeater 0526-66 in the Large Magellanic Cloud. In: Astrophysical Journal. 2012 ; Vol. 748, No. 2.
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abstract = "We report on the results from our deep Chandra observation (120ks) of the supernova remnant (SNR) N49 and soft gamma-ray repeater (SGR) 0526-66 in the Large Magellanic Cloud. We firmly establish the detection of an ejecta {"}bullet{"} beyond the southwestern boundary of N49. The X-ray spectrum of the bullet is distinguished from that of the main SNR shell, showing significantly enhanced Si and S abundances. We also detect an ejecta feature in the eastern shell, which shows metal overabundances similar to those of the bullet. If N49 was produced by a core-collapse explosion of a massive star, the detected Si-rich ejecta may represent explosive O-burning or incomplete Si-burning products from deep interior of the SN. On the other hand, the observed Si/S abundance ratio in the ejecta may favor Type Ia origin for N49. We refine the Sedov age of N49, τSed 4800yr, with the explosion energy E 0 1.8 × 1051erg. Our blackbody (BB) + power law (PL) model for the quiescent X-ray emission from SGR 0526-66 indicates that the PL photon index (Γ 2.5) is identical to that of PSR 1E1048.1-5937, the well-known candidate transition object between anomalous X-ray pulsars and SGRs. Alternatively, the two-component BB model implies X-ray emission from a small (R 1km) hot spot(s) (kT 1keV) in addition to emission from the neutron star's cooler surface (R 10km, kT 0.4keV). There is a considerable discrepancy in the estimated column toward 0526-66 between BB+PL and BB+BB model fits. Discriminating these spectral models would be crucial to test the long-debated physical association between N49 and 0526-66.",
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An X-ray study of supernova remnant N49 and soft gamma-ray repeater 0526-66 in the Large Magellanic Cloud. / Park, Sangwook; Hughes, John P.; Slane, Patrick O.; Burrows, David N.; Lee, Jae Joon; Mori, Koji.

In: Astrophysical Journal, Vol. 748, No. 2, 117, 01.04.2012.

Research output: Contribution to journalArticle

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T1 - An X-ray study of supernova remnant N49 and soft gamma-ray repeater 0526-66 in the Large Magellanic Cloud

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AB - We report on the results from our deep Chandra observation (120ks) of the supernova remnant (SNR) N49 and soft gamma-ray repeater (SGR) 0526-66 in the Large Magellanic Cloud. We firmly establish the detection of an ejecta "bullet" beyond the southwestern boundary of N49. The X-ray spectrum of the bullet is distinguished from that of the main SNR shell, showing significantly enhanced Si and S abundances. We also detect an ejecta feature in the eastern shell, which shows metal overabundances similar to those of the bullet. If N49 was produced by a core-collapse explosion of a massive star, the detected Si-rich ejecta may represent explosive O-burning or incomplete Si-burning products from deep interior of the SN. On the other hand, the observed Si/S abundance ratio in the ejecta may favor Type Ia origin for N49. We refine the Sedov age of N49, τSed 4800yr, with the explosion energy E 0 1.8 × 1051erg. Our blackbody (BB) + power law (PL) model for the quiescent X-ray emission from SGR 0526-66 indicates that the PL photon index (Γ 2.5) is identical to that of PSR 1E1048.1-5937, the well-known candidate transition object between anomalous X-ray pulsars and SGRs. Alternatively, the two-component BB model implies X-ray emission from a small (R 1km) hot spot(s) (kT 1keV) in addition to emission from the neutron star's cooler surface (R 10km, kT 0.4keV). There is a considerable discrepancy in the estimated column toward 0526-66 between BB+PL and BB+BB model fits. Discriminating these spectral models would be crucial to test the long-debated physical association between N49 and 0526-66.

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