Other
Scientific paper
Dec 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...21110209v&link_type=abstract
American Astronomical Society, AAS Meeting #211, #102.09; Bulletin of the American Astronomical Society, Vol. 39, p.918
Other
Scientific paper
We describe the results of recent Chandra ACIS observations of the Vela-like pulsar PSR J2021+3651 and its pulsar wind nebulae (PWN). This "Dragonfly Nebula” displays an axisymmetric morphology, with bright inner jets, a double-ridged equatorial inner nebula, and 30" long polar jet. The PWN is embedded in faint diffuse emission with a bow shock structure bracketing the pulsar at a radius of 1' and trailing off to the west over 2-3'. The pulsar spectrum is well fit by a thermal component (kT = 0.16 +/- 0.02 keV) combined with a power-law and a hydrogen column density of 6.7x1021 cm-2. The power-law spectrum of the extended emission demonstrates distinct synchrotron burn-off, with gamma ranging from 1.1 in the hard inner jet, to 1.45 in the equatorial PWN, and ultimately to 1.9 in the far reaches of the outer nebula. We spatially fit the "Dragonfly Nebula” with a model which assumes toroidal morphology and find that a highly inclined (86 +/- 1 deg) double torus is preferred. Currently the PWN surrounding the Vela pulsar is the only other system with observed double structure. One peculiarity of the system is the high pulsar dispersion measure, which suggests a large 12kpc distance. The scale of the PWN, the emitting area of the hot neutron star and the inferred spindown efficiency for PWN emission all suggest a more modest distance of 3-4 kpc. Given the likely connection with the gamma-ray source GeV J2020+3658, these geometry and distance constraints should be very helpful in interpreting new GeV and TeV observations.
Etten Adam Van
Ng Cheuk-Yiu
Romani Roger W.
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