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XMM-Newton and Chandra observations of G272.2-3.2. Evidence of stellar ejecta in the central region

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Sánchez Ayaso, E. and Combi, J. A. and Bocchino, F. and Albacete Colombo, J. F. and López Santiago, J. and Marti, J. and Castro Rubio, Elisa de (2013) XMM-Newton and Chandra observations of G272.2-3.2. Evidence of stellar ejecta in the central region. Astronomy and astrophysics, 552 . ISSN 0004-6361

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Official URL: http://dx.doi.org/10.1051/0004-6361/201219709




Abstract

Aims. We aim to study the spatial distribution of the physical and chemical properties of the X-ray emitting plasma of the supernova remnant G272.2-3.2 in order to obtain important constraints on its ionization stage, the progenitor supernova explosion, and the age of the remnant. Methods. We report on combined XMM-Newton and Chandra images, median photon energy maps, silicon and sulfur equivalent width maps, and a spatially resolved spectral analysis for a set of regions of the remnant. Complementary radio and Ha observations, available in the literature, are also used to study the multi-wavelength connection of all detected emissions. Results. The X-ray morphology of the remnant displays an overall structure with an almost circular appearance and a centrally brightened hard region with a peculiar elongated hard structure oriented along the northwest-southeast direction of the central part. The X-ray spectral study of the regions shows distinct K alpha emission-line features of metal elements, confirming the thermal origin of the emission. The X-ray spectra are well represented by an absorbed variable abundance non-equilibrium ionization thermal plasma model, which produces elevated abundances of Si, S, and Fe in the circular central region, typical of ejecta material. The values of abundances found in the central region of the supernova remnant favor a Type Ia progenitor for this remnant. The outer region shows abundances below the solar value, to be expected if the emission arises from the shocked interstellar medium. The relatively low ionization timescales suggest non-equilibrium ionization. We identify the location of the contact discontinuity. Its distance to the outer shock is higher than expected for expansion in a uniform media, which suggests that the remnant spent most of its time in more dense medium.


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© ESO 2013. We are grateful to the referee for her/his valuable suggestions and comments, which helped us to improve the paper. The authors acknowledge support by DGI of the Spanish Ministerio de Educación y Ciencia under grants AYA2010-21782-C03-03, FEDER funds, Plan Andaluz de Investigación Desarrollo e Innovación (PAIDI) of Junta de Andalucía as research group FQM-322, and the excellence fund FQM-5418. J.A.C. and J.F.A.C. are researchers of CONICET. J.F.A.C. was supported by grant PIP 2011-0100285 (CONICET). J.A.C. by grant PICT 2008-0627, from ANPCyT and PIP 20100078 (CONICET). J.L.S. acknowledges support by the Spanish Ministerio de Innovación y Tecnología under grant AYA2008-06423-C03-03. F. B. acknowledges partial support of the ASI-INAF agreement n. I/009/10/0.

Uncontrolled Keywords:Supernova remnant g272.2-3.2; Shock-cloud interaction; Photon imaging camera; Abundances; Emission; Catalog; Rosat
Subjects:Sciences > Physics > Astrophysics
Sciences > Physics > Astronomy
ID Code:30664
Deposited On:05 Jun 2015 11:00
Last Modified:10 Dec 2018 15:05

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