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Chandra Observation of PSR B1823-13 and Its Pulsar Wind Nebula
An observation of the Vela-like pulsar B1823-13 and its synchrotronnebula with the Chandra X-Ray Observatory allowed us to resolve thepulsar and the fine structure of the nebula. The pulsar's spectrum fitsa power-law model with a photon index ΓPSR~2.4 for theplausible hydrogen column density nH=1×1022cm-2, corresponding to the luminosityLPSR~8×1031 ergs s-1 in the 0.5-8keV band, at a distance of 4 kpc. The pulsar radiation likely includesmagnetospheric and thermal components, but they cannot be reliablyseparated, because of the small number of counts detected and stronginterstellar absorption. The pulsar is surrounded by a compact,~25''×10'', pulsar wind nebula (PWN)elongated in the east-west direction, which includes a brighter innercomponent ~7''×3'', elongated in thenortheast-southwest direction. The slope of the compact PWN spectrum isΓcomp~1.3, and the 0.5-8 keV luminosity isLcomp~3×1032 ergs s-1. Thecompact PWN is surrounded by asymmetric diffuse emission (extended PWN)seen up to at least 2.4' south of the pulsar, with a softer spectrum(Γext~1.9 for nH=1×1022cm-2), and the 0.5-8 keV luminosityLext~1033-1034 ergs s-1. Wealso measured the pulsar's proper motion using archival VLA data,μα=23.0+/-2.5 mas yr-1 andμδ=-3.9+/-3.1 mas yr-1 (in LSR), whichcorresponds to the transverse velocity v⊥~440 kms-1. The direction of the proper motion is approximatelyparallel to the elongation of the compact PWN, but it is nearlyperpendicular to that of the extended PWN and to the direction towardthe center of the bright VHE γ-ray source HESS J1825-137, which isbelieved to be powered by PSR B1823-13.
| Interstellar polarization from observations of A and F stars in high and intermediate galactic latitudes, and from stars in the Mathewson and Ford polarization catalogue
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1986A&AS...64..487K&db_key=AST
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