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arXiv · 1202.1588

Elemental Abundances in the Possible Type Ia Supernova Remnant G344.7-0.1

Hiroya Yamaguchi·Masaomi Tanaka·Keiichi Maeda·Patrick O. Slane·Adam Foster·Randall K. Smith·Satoru Katsuda·Rie Yoshii
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Abstract

Recent studies on the Galactic supernova remnant (SNR) G344.7-0.1 have commonly claimed its origin to be a core-collapse supernova (SN) explosion, based on its highly asymmetric morphology and/or proximity to a star forming region. In this paper, however, we present an X-ray spectroscopic study of this SNR using Suzaku, which is supportive of a Type Ia origin. Strong K-shell emission from lowly ionized Fe has clearly been detected, and its origin is determined, for the first time, to be the Fe-rich SN ejecta. The abundance pattern is highly consistent with that expected for a somewhat-evolved Type Ia SNR. It is suggested, therefore, that the X-ray point-like source CXOU J170357.8-414302 located at the SNR's geometrical center is not associated with the SNR but is likely to be a foreground object. Our result further indicates that G344.7-0.1 is the first possible Type Ia SNR categorized as a member of the so-called "mixed-morphology" class. In addition, we have detected emission from He-like Al at ~1.6 keV, the first clear detection of this element in the spectrum of an extended X-ray source. The possible enhancement of the Al/Mg abundance ratio from the solar value suggests that the ambient interstellar medium has a relatively high metallicity (not less than 10% of the solar value), if this SNR has indeed a Type Ia origin. We also report marginal detection of Cr and Mn, although the measured fluxes have large statistical and systematic uncertainties.

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Hiroya Yamaguchi, Masaomi Tanaka, Keiichi Maeda, Patrick O. Slane, Adam Foster, Randall K. Smith, Satoru Katsuda, Rie Yoshii. 2012-02-08. Elemental Abundances in the Possible Type Ia Supernova Remnant G344.7-0.1. https://doi.org/10.1088/0004-637x/749/2/137

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