TY - JOUR
T1 - Studying the γ-ray pulsar J1932+1916 and its pulsar wind nebula with Chandra
AU - Medvedev, O. D.
AU - Karpova, A. V.
AU - Shibanov, Yu A.
AU - Zyuzin, D. A.
AU - Pavlov, G. G.
N1 - Funding Information:
GGP acknowledges support from the ACIS Instrument Team contract SV4-74018 issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-03060. The ACIS Guaranteed Time Observations included here were selected by the ACIS Instrument Principal Investigator, Gordon P. Garmire, of the Huntingdon Institute for X-ray Astronomy, LLC, which is under contract to the Smithsonian Astrophysical Observatory; Contract SV2-82024. For figure 3 we used the data from the VGPS survey conducted by the National Radio Astronomy Observatory (NRAO) instruments. NRAO is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. DAZ thanks Pirinem School of Theoretical Physics for hospitality.
Publisher Copyright:
© 2019 Published under licence by IOP Publishing Ltd.
PY - 2019/12/11
Y1 - 2019/12/11
N2 - We report on the results of Chandra X-ray observations of the γ-ray radio-quiet pulsar J1932+1916. We confirm the previous detection of the pulsar counterpart and its pulsar wind nebula in X-rays from low spatial resolution data obtained by Suzaku and Swift. The Chandra data with much better spatial resolution resolved the fine structure of the nebula in the pulsar vicinity, which can be interpreted as jets bent by the ram pressure. The size of this compact part is about 30″, and it is surrounded by a weak asymmetric diffusive emission extended up to ≈2.′8. The X-ray spectra of the pulsar, the compact and extended parts of the nebula can be described by the power-law models with photon indexes of 0.44-0.61+0.57, 2.34-0.79+0.95 and 2.14-0.31+0.32, respectively. The actual pulsar's X-ray flux is several times weaker than it was obtained with Suzaku and Swift where it was dominated by the unresolved nebula. We discuss possible associations of J1932+1916 with the nearby supernova remnant G54.4-0.3.
AB - We report on the results of Chandra X-ray observations of the γ-ray radio-quiet pulsar J1932+1916. We confirm the previous detection of the pulsar counterpart and its pulsar wind nebula in X-rays from low spatial resolution data obtained by Suzaku and Swift. The Chandra data with much better spatial resolution resolved the fine structure of the nebula in the pulsar vicinity, which can be interpreted as jets bent by the ram pressure. The size of this compact part is about 30″, and it is surrounded by a weak asymmetric diffusive emission extended up to ≈2.′8. The X-ray spectra of the pulsar, the compact and extended parts of the nebula can be described by the power-law models with photon indexes of 0.44-0.61+0.57, 2.34-0.79+0.95 and 2.14-0.31+0.32, respectively. The actual pulsar's X-ray flux is several times weaker than it was obtained with Suzaku and Swift where it was dominated by the unresolved nebula. We discuss possible associations of J1932+1916 with the nearby supernova remnant G54.4-0.3.
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U2 - 10.1088/1742-6596/1400/2/022018
DO - 10.1088/1742-6596/1400/2/022018
M3 - Conference article
AN - SCOPUS:85077605146
SN - 1742-6588
VL - 1400
JO - Journal of Physics: Conference Series
JF - Journal of Physics: Conference Series
IS - 2
M1 - 022018
T2 - International Conference PhysicA.SPb 2019
Y2 - 22 October 2019 through 24 October 2019
ER -