Hard X-ray emission from the SNR G337.2+0.1

Details Hard X-ray emission from the SNR G337.2+0.1 Hard X-ray emission from the SNR G337.2+0.1

Jun 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007ap%26ss.309..395c&link_type=abstract

Astrophysics and Space Science, Volume 309, Issue 1-4, pp. 395-399

Astronomy and Astrophysics

Astrophysics

1

X-Rays: Individual (Ax J1635.9&Minus, 4719), (Ism:) Supernova Remnants, Ism: Individual (G337.2+0.1), X-Rays: Ism, Radiation Mechanisms: Non-Thermal

Scientific paper

We report hard X-ray emission of the non-thermal supernova remnant G337.2+0.1. The source presents centrally filled and diffuse X-ray emission. A spectral study confirms that the column density of the central part of the object is about N H˜5.9(±1.5)×1022 cm-2 and its X-ray spectrum is well represented by a single power-law with a photon index Γ=0.96±0.56. Detailed spectral analysis indicates that the outer region is highly absorbed and quite softer than the inner region. Characteristics already observed in other well-known X-ray plerions. Based on the gathered information, we confirm the SNR nature of G337.2+0.1, and suggest that the central region of the source is a pulsar wind nebula (PWN), originated by an energetic though yet undetected pulsar.

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