期刊
ASTROPHYSICAL JOURNAL
卷 744, 期 2, 页码 -出版社
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/744/2/81
关键词
ISM: individual objects (HESS J1356-645, G309.8-2.6); pulsars: individual (PSR J1357-6429); X-rays: individual (CXOU J135605.9-642909, 1RXS J135605.5-642902)
资金
- Chandra award [GO0-11070X]
- NASA [NNX09AT11G, NNX09AC81G, NNX09AC84G]
- National Science Foundation [AST09-08733, AST09-08611]
- Ministry of Education and Science of the Russian Federation [11.G34.31.0001]
- Division Of Astronomical Sciences
- Direct For Mathematical & Physical Scien [0908611, 0908733] Funding Source: National Science Foundation
- NASA [NNX09AT11G, 120558, NNX09AC81G, 108107] Funding Source: Federal RePORTER
We observed the young pulsar J1357-6429 with the Chandra and XMM-Newton observatories. The pulsar spectrum fits well a combination of an absorbed power-law model (Gamma = 1.7 +/- 0.6) and a blackbody model (kT = 140(-40)(+60) eV, R similar to 2 km at the distance of 2.5 kpc). Strong pulsations with pulsed fraction of 42% +/- 5%, apparently associated with the thermal component, were detected in 0.3-1.1 keV. Surprisingly, the pulsed fraction at higher energies, 1.1-10 keV, appears to be smaller, 23% +/- 4%. The small emitting area of the thermal component either corresponds to a hotter fraction of the neutron star surface or indicates inapplicability of the simplistic blackbody description. The X-ray images also reveal a pulsar wind nebula (PWN) with complex, asymmetric morphology comprised of a brighter, compact PWN surrounded by the fainter, much more extended PWN whose spectral slopes are Gamma = 1.3 +/- 0.3 and Gamma = 1.7 +/- 0.2, respectively. The extended PWN with the observed flux of similar to 7.5 x 10(-13) erg s(-1) cm(-2) is a factor of 10 more luminous then the compact PWN. The pulsar and its PWN are located close to the center of the extended TeV source HESS J1356-645, which strongly suggests that the very high energy emission is powered by electrons injected by the pulsar long ago. The X-ray to TeV flux ratio, similar to 0.1, is similar to those of other relic PWNe. We found no other viable candidates to power the TeV source. A region of diffuse radio emission, offset from the pulsar toward the center of the TeV source, could be synchrotron emission from the same relic PWN rather than from the supernova remnant.
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