Hostname: page-component-586b7cd67f-r5fsc Total loading time: 0 Render date: 2024-11-28T17:48:12.498Z Has data issue: false hasContentIssue false
  • English
  • Français

Searching for X-ray counterparts of Fermi Gamma-ray pulsars in Suzaku observations

Published online by Cambridge University Press:  05 September 2012

Yu Aoki ,
Takahiro Enomoto ,
Yoichi Yatsu ,
Nobuyuki Kawai ,
Takeshi Nakamori ,
Jun Kataoka  and
P. Saz Parkinson
Yu Aoki
Affiliation:
Dept. of Physics, Tokyo Institute of Technology, B2-12-1 Oookayama Meguro Tokyo, 152-8551, Japan email: [email protected]
Takahiro Enomoto
Affiliation:
Dept. of Physics, Tokyo Institute of Technology, B2-12-1 Oookayama Meguro Tokyo, 152-8551, Japan email: [email protected]
Yoichi Yatsu
Affiliation:
Dept. of Physics, Tokyo Institute of Technology, B2-12-1 Oookayama Meguro Tokyo, 152-8551, Japan email: [email protected]
Nobuyuki Kawai
Affiliation:
Dept. of Physics, Tokyo Institute of Technology, B2-12-1 Oookayama Meguro Tokyo, 152-8551, Japan email: [email protected]
Takeshi Nakamori
Affiliation:
Research Institute for Science and Engineering, Waseda University, Japan
Jun Kataoka
Affiliation:
Research Institute for Science and Engineering, Waseda University, Japan
P. Saz Parkinson
Affiliation:
Santa Cruz Institute for Particle Physics, Dept. of Physics and Dept. of Astronomy and Astrophysics, University of California at Santa Cruz, Santa Cruz, CA 95064, 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 report the Suzaku follow-up observations of the Gamma-ray pulsars, 1FGL J0614,13328, J1044.55737, J1741.82101, and J1813.31246, which were discovered by the Fermi Gamma-ray observatory. Analysing Suzaku/XIS data, we detected X-ray counterparts of these pulsars in the Fermi error circle and interpreted their spectra with absorbed power-law functions. These results indicate that the origin of these X-ray sources is non-thermal emission from the pulsars or from Pulsar Wind Nebulae (PWNe) surrounding them. Moreover we found that J1741.82101 exhibits a peculiar profile: spin-down luminosity vs flux ratio between X- and gamma-rays is unusually large compared to usual radio pulsars.

Keywords

PulsarPulsar wind nebulaeGamma-ray pulsars. Fermi.
Type
Poster Papers
Information
Proceedings of the International Astronomical Union , Volume 7 , Symposium S279: Death of Massive Stars: Supernovae and Gamma-Ray Bursts , April 2011 , pp. 317 - 318
Copyright
Copyright © International Astronomical Union 2012

References

Amari, S., Hoppe, P., Zinner, E., & Lewis, R. S. 1995, Meteoritics, 30, 490CrossRefGoogle Scholar
Anders, E. & Zinner, E. 1993, Meteoritics, 28, 490CrossRefGoogle Scholar
Bernatowicz, T. J., Messenger, S., Pravdivtseva, O., Swan, P., & Walker, R. M. 2003, Geochim. Cosmochim. Acta, 67, 4679CrossRefGoogle Scholar
Busso, M., Gallino, R., & Wasserburg, G. J. 1999, ARAA, 37, 239CrossRefGoogle Scholar
Croat, T. K., Stadermann, F. J., & Bernatowicz, T. J. 2005, ApJ, 631, 976CrossRefGoogle Scholar
Draine, B. T. 2003, ARAA, 41, 241CrossRefGoogle Scholar
Hoppe, P. & Zinner, E. 2000, J. Geophys. Res., A105, 10371CrossRefGoogle Scholar
Hoppe, P., Ott, U., & Lugmair, G. W. 2004, New Astron. Revs, 48, 171CrossRefGoogle Scholar
Kanai, Y., 2010, Ph.D. thesis, Tokyo Institute of TechnologyGoogle Scholar
Lodders, K. & Fegley, B. 1998, Meteorit. Planet. Sci., 33, 871CrossRefGoogle Scholar
Meyer, B. S., Clayton, D. D., & The, L.-S. 2000, ApJ (Letters), 540, L49CrossRefGoogle Scholar