Discovery of X-Ray Emission from a Radio Supernova Remnant G352.7-0.1

Details Discovery of X-Ray Emission from a Radio Supernova Remnant G352.7-0.1 Discovery of X-Ray Emission from a Radio Supernova Remnant G352.7-0.1

Apr 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998pasj...50..249k&link_type=abstract

Publications of the Astronomical Society of Japan, v.50, p.249-255.

Astronomy and Astrophysics

Astronomy

10

Abundances, Ism: Individual (G3527-01), Supernova Remnants, X-Rays: Sources, X-Rays: Spectra

Scientific paper

We report on the first detection of X-rays from the radio supernova remnant (SNR) G352.7-0.1 with the ASCA Galactic Plane Survey Project. An X-ray image with a shell-like morphology similar to that of the radio band and a spectrum with prominent K-shell lines from highly ionized Si, S, and Ar are presented. These features provide convincing evidence that the X-rays are due to a shock-heated optically thin hot plasma. The spectra are represented by a non-equilibrium ionization (NEI) model with an electron temperature of kT ~ 2.0 keV, an ionization parameter of tau ~ 10(11.0) cm(-3) s, and an absorption of N_H ~ 2.9 times 10(22) cm(-2) . We report on evidence of overabundances of Si and S of ~ 3.7 and ~ 3.4, relative to the solar values, respectively. The large absorption indicates that G352.7-0.1 is near to the galactic center region and, after removing the absorption, the X-ray flux in the 1--10 keV band is estimated to be F_X(1--10 keV) ~ 1.2times 10(-11) erg cm(-2) s(-1) . Assuming the SNR to be in the Sedov phase and near to the galactic center (8.5 kpc), G352.7-0.1 is estimated to have a SN explosion energy and age of E_SN ~ 2 times 10(50) erg and t_age ~ 2200 yr, respectively; hence, it is a middle-aged SNR.

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