PSR J1856+0245:: Arecibo discovery of a young, energetic pulsar coincident with the TeV γ-ray source HESS J1857+026

被引:30
作者
Hessels, J. W. T. [1 ]
Nice, D. J. [2 ]
Gaensler, B. M. [3 ]
Kaspi, V. M. [4 ]
Lorimer, D. R. [5 ]
Champion, D. J. [6 ]
Lyne, A. G. [7 ]
Kramer, M. [7 ]
Cordes, J. M. [8 ]
Freire, P. C. C. [9 ]
Camilo, F. [10 ]
Ransom, S. M. [11 ]
Deneva, J. S. [8 ]
Bhat, N. D. R. [12 ]
Cognard, I. [13 ]
Crawford, F. [14 ]
Jenet, F. A. [15 ]
Kasian, L. [16 ]
Lazarus, P. [4 ]
van Leeuwen, J. [17 ]
McLaughlin, M. A. [5 ]
Stairs, I. H. [16 ]
Stappers, B. W. [7 ]
Venkataraman, A. [9 ]
机构
[1] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands
[2] Bryn Mawr Coll, Dept Phys, Bryn Mawr, PA 19010 USA
[3] Univ Sydney, Sch Phys, Inst Astron, Sydney, NSW 2006, Australia
[4] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada
[5] W Virginia Univ, Dept Phys, Morgantown, WV 26506 USA
[6] ATNF CSIRO, Epping, NSW 1710, Australia
[7] Univ Manchester, Jordell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England
[8] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA
[9] Arecibo Observ, NAIC, Arecibo, PR 00612 USA
[10] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA
[11] Natl Radio Astron Observ, Charlottesville, VA 22903 USA
[12] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia
[13] CNRS, LPCE, F-45071 Orleans, France
[14] Franklin & Marshall Coll, Dept Phys & Astron, Lancaster, PA 17604 USA
[15] Univ Texas Brownsville, Ctr Gravitat Wave Astron, Brownsville, TX 78520 USA
[16] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada
[17] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA
基金
美国国家科学基金会;
关键词
gamma rays : observations; pulsars : general; pulsars : individual (PSR J1856+0245); stars : neutron; X-rays : individual (AX J185651+0245);
D O I
10.1086/590908
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We present the discovery of the Vela-like radio pulsar J1856+0245 in the Arecibo PALFA survey. PSR J1856+0245 has a spin period of 81 ms, a characteristic age of 21 kyr, and a spin-down luminosity (E) over dot = 4.6 x 10(36) ergs s(-1). It is positionally coincident with the TeV gamma-ray source HESS J1857+026, which has no other known counterparts. Young, energetic pulsars create wind nebulae, and more than a dozen pulsar wind nebulae have been associated with very high energy ( 100 GeV-100 TeV) gamma-ray sources discovered with the HESS telescope. The gamma-ray emission seen from HESS J1857+026 is potentially produced by a pulsar wind nebula powered by PSR J1856+0245; faint X-ray emission detected by ASCA at the pulsar's position supports this hypothesis. The inferred gamma-ray efficiency is epsilon(gamma) = L(gamma)/(E) over dot = 3.1 % (1-10 TeV, for a distance of 9 kpc), comparable to that observed in similar associations.
引用
收藏
页码:L41 / L44
页数:4
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