A possible association of the new VHE γ-ray source HESS J1825-137 with the pulsar wind nebula G18.0-0.7

被引:15
作者
Aharonian, FA [1 ]
Akhperjanian, AG
Bazer-Bachi, AR
Beilicke, M
Benbow, W
Berge, D
Bernlöhr, K
Boisson, C
Bolz, O
Borrel, V
Braun, I
Breitling, F
Brown, AM
Chadwick, PM
Chounet, LM
Cornils, R
Costamante, L
Degrange, B
Dickinson, HJ
Djannati-Atai, A
Drury, LO
Dubus, G
Emmanoulopoulos, D
Espigat, P
Feinstein, F
Fontaine, G
Fuchs, Y
Funk, S
Gallant, YA
Giebels, B
Gillessen, S
Glicenstein, JF
Goret, P
Hadjichristidis, C
Hauser, M
Heinzelmann, G
Henri, G
Hermann, G
Hinton, JA
Hofmann, W
Holleran, M
Horns, D
Jacholkowska, A
de Jager, OC
Khélifi, B
Komin, N
Konopelko, A
Latham, IJ
Le Gallou, R
Lemière, A
机构
[1] Max Planck Inst Kernphys, D-69117 Heidelberg, Germany
[2] Yerevan Phys Inst, Yerevan 375036, Armenia
[3] UPS, CNRS, Ctr Etud Spatiale Rayonnements, Toulouse, France
[4] Univ Hamburg, Inst Expt Phys, Hamburg, Germany
[5] Humboldt Univ, Inst Phys, Berlin, Germany
[6] Observ Paris, Meudon Sect, CNRS,UMR 8102, LUTH, Paris, France
[7] Univ Durham, Dept Phys, Durham DH1 3LE, England
[8] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France
[9] Observ Paris, APC, CNRS, UMR 7164, Paris 05, France
[10] Dublin Inst Adv Studies, Dublin 4, Ireland
[11] Landessternwarte Konigstuhl, Heidelberg, Germany
[12] Univ Montpellier 2, Lab Phys Theor & Astroparticules, F-34095 Montpellier, France
[13] Univ Grenoble 1, CNRS, INSU, Lab Astrophys Grenoble, F-38041 Grenoble, France
[14] Ctr Etud Saclay, DAPNIA, DSM, CEA, F-91191 Gif Sur Yvette, France
[15] NW Univ, Unit Space Phys, Potchefstroom, South Africa
[16] Univ Paris 06, CNRS, IN2P3, Lab Phys Nucl & Hautes Energies, F-75252 Paris, France
[17] Univ Paris 07, CNRS, IN2P3, Lab Phys Nucl & Hautes Energies, F-75221 Paris, France
[18] Ruhr Univ Bochum, Inst Theoret Phys, Lehrstuhl 4, Bochum, Germany
[19] Charles Univ Prague, Inst Nucl & Particle Phys, Prague, Czech Republic
[20] Univ Namibia, Windhoek, Namibia
来源
ASTRONOMY & ASTROPHYSICS | 2005年 / 442卷 / 03期
关键词
ISM : plerions; ISM : individual objects : PSR B1823-13; HESS J1825-137; G; 18.0-0.7; gamma-rays : observations;
D O I
10.1051/0004-6361:200500180
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We report on a possible association of the recently discovered very high-energy gamma-ray source HESSJ1825-137 wit the pulsar wind nebula (commonly referred to as G 18.0-0.7) of the 2.1 x 10(4) year old Vela-like pulsar PSRB1823-13.HESSJ1825-137 was detected with a significance of 8.1 sigma in the Galactic Plane survey conducted wit the HESS instrument in 2004. The centroid position of HESSJ1825-137 is offset by 11' south of the pulsar position. XMM-Newton observations have revealed X-ray synchrotron emission of an asymmetric pulsar wind nebula extending to the south of the pulsar. We argue that the observed morphology and TeV spectral index suggest that HESSJ1825-137 and G18.0-0.7 may be associated: the lifetime of TeV emitting electrons is expected to be longer compared to the XMM-Newton X-ray emitting electrons, resulting in electrons from earlier epochs (when the spin-down power was larger) contributing to the present TeV flux. These electrons are expected to be synchrotron cooled, which explains the observed photon index of similar to 2.4, and the longer lifetime of TeV emitting electrons naturally explains why the TeV nebula is larger that the X-ray size. Finally, supernova remnant expansion into an inhomogeneous medium is expected to create reverse shocks interacting at different times wit the pulsar wind nebula, resulting in the offset X-ray and TeV gamma-ray morphology.
引用
收藏
页码:L25 / L29
页数:5
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