Hostname: page-component-cd9895bd7-fscjk Total loading time: 0 Render date: 2024-12-25T16:56:12.067Z Has data issue: false hasContentIssue false
  • English
  • Français

X-ray imaging and spectroscopic study of the SNR Kes 73 hosting the magnetar 1E 1841–045

Published online by Cambridge University Press:  29 January 2014

H. S. Kumar ,
S. Safi-Harb ,
P. O. Slane  and
E. V. Gotthelf
H. S. Kumar
Affiliation:
Department of Physics & Astronomy, University of Manitoba, Winnipeg, Canada email: [email protected]
S. Safi-Harb
Affiliation:
Department of Physics & Astronomy, University of Manitoba, Winnipeg, Canada email: [email protected] Canada Research Chair
P. O. Slane
Affiliation:
Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
E. V. Gotthelf
Affiliation:
Columbia Astrophysics Laboratory, Columbia university, New York, NY 10027, USA
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We present the first detailed Chandra and XMM-Newton study of the young Galactic supernova remnant (SNR) Kes 73 associated with the anomalous X-ray pulsar (AXP) 1E 1841–045. Images of the remnant in the radio (20 cm), infrared (24 μm), and X-rays (0.5–7 keV) reveal a spherical morphology with a bright western limb. High-resolution Chandra images show bright diffuse emission across the remnant, with several small-scale clumpy and knotty structures filling the SNR interior. The overall Chandra and XMM-Newton spectrum of the SNR is best described by a two-component thermal model with the hard component characterized by a low ionization timescale, suggesting that the hot plasma has not yet reached ionization equilibrium. The soft component is characterized by enhanced metal abundances from Mg, Si, and S, suggesting the presence of metal-rich supernova ejecta. We discuss the explosion properties of the supernova and infer the mass of its progenitor star. Such studies shed light on our understanding of SNRs associated with highly magnetized neutron stars.

Keywords

ISM: individual (SNR Kes 73) – pulsars: individual (AXP 1E 1841−045) – supernova remnants – X-rays: ISM
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Symposium S296: Supernova Environmental Impacts , January 2013 , pp. 235 - 238
Copyright
Copyright © International Astronomical Union 2014 

References

Chevalier, R. G. 2005, ApJ, 619, 839CrossRefGoogle Scholar
Pinheiro Gonçalves, D., Noriega-Crespo, A., Paladini, R., Martin, P. G., & Carey, S. J. 2011, AJ, 142, 47CrossRefGoogle Scholar
Gotthelf, E. V. & Vasisht, G. 1997, ApJ, 486, L133CrossRefGoogle Scholar
Kriss, G. A., Becker, R. H., Helfand, D. J., & Canizares, C. J. 1985, Apj, 288, 703Google Scholar
Kumar, H. S., Safi-Harb, S., Slane, P. O., & Gotthelf, E. V. 2013, ApJ, submittedGoogle Scholar
Lopez, L. A., Ramirez-Ruiz, E., Huppenkothen, D., Badenes, C., & Pooley, D. A. 2011, ApJ, 732, 114CrossRefGoogle Scholar
Safi-Harb, S. & Kumar, H. S. 2012, Proceedings of IAUS 291, Cambridge University Press, Vol 291, 480 (arXiv:1211.5261)Google Scholar
Vasisht, G. & Gotthelf, E. V. 1997, ApJ, 486, L129Google Scholar
Vink, J. & Kuiper, L. 2006, MNRAS 370 1, L14Google Scholar
Woosley, S. E. & Weaver, T. A. 1995, ApJSS, 101, 181CrossRefGoogle Scholar