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Home List of Titles Radio detection of LAT PSRs J1741-2054 and J2032+4127: no longer just gamma-ray pulsars
Please use this identifier to cite or link to this item: http://hdl.handle.net/1959.3/69544
- Radio detection of LAT PSRs J1741-2054 and J2032+4127: no longer just gamma-ray pulsars
- Camilo, F.; Ray, P. S.; Ransom, S. M.; Burgay, M.; Johnson, T. J.; Kerr, M.; Gotthelf, E. V.; Halpern, J. P.; Reynolds, J.; Romani, R. W.; Demorest, P.; Johnston, S.; van Straten, W.; Parkinson, P. M. S.; Ziegler, M.; Dormody, M.; Thompson, D. J.; Smith, D. A.; Harding, A. K.; Abdo, A. A.; Crawford, F.; Freire, P. C. C.; Keith, M.; Kramer, M.; Roberts, M. S. E.; Weltevrede, P.; Wood, K. S.
- Sixteen pulsars have been discovered so far in blind searches of photons collected with the Large Area Telescope on the Fermi Gamma-ray Space Telescope. We here report the discovery of radio pulsations from two of them. PSR J1741–2054, with period P = 413 ms,was detected in archival Parkes telescope data and subsequently has been detected at the Green Bank Telescope (GBT). Its received flux varies greatly due to interstellar scintillation and it has a very small dispersion measure of DM = 4.7 pc cm−3, implying a distance of ≈ 0.4 kpc and possibly the smallest luminosity of any known radio pulsar. At this distance, for isotropic emission, its gamma-ray luminosity above 0.1 GeV corresponds to 28% of the spin-down luminosity of ˙E = 9.4×1033 erg s−1. The gamma-ray profile occupies 1/3 of pulse phase and has three closely spaced peaks with the first peak lagging the radio pulse by δ = 0.29 P. We have also identified a soft Swift source that is the likely X-ray counterpart. In many respects PSR J1741–2054 resembles the Geminga pulsar. The second source, PSR J2032+4127, was detected at the GBT. It has P = 143 ms, and its DM = 115 pc cm−3 suggests a distance of ≈ 3.6 kpc, but we consider it likely that it is located within the Cyg OB2 stellar association at half that distance. The radio emission is nearly 100% linearly polarized, and the main radio peak precedes by δ = 0.15 P the first of two narrow gamma-ray peaks that are separated by Δ = 0.50 P. The second peak has a harder spectrum than the first one, following a trend observed in young gammaray pulsars. Faint, diffuse X-ray emission in a Chandra image is possibly its pulsar wind nebula. The wind of PSR J2032+4127 is responsible for the formerly unidentified HEGRA source TeV J2032+4130. PSR J2032+4127 is coincident in projection with MT91 213, a Be star in Cyg OB2, although apparently not a binary companion of it.
- Publication type
- Journal article
- Research centre
- Swinburne University of Technology. Faculty of Information and Communication Technologies. Centre for Astrophysics and Supercomputing
- Astrophysical Journal, Vol. 705, no. 1 (Nov 2009), pp. 1-13
- Publication year
- FOR Code(s)
- 0201 Astronomical and Space Sciences
- CYG OB2; Gamma ray pulsars; J2032+4130; Neutron stars; Open clusters; PSR J1741-2054; PSR J2032+4127; Source TeV; Swift J174157.6-205411; TEV J2032+4130; TEV-J2032+4130; X-rays
- Institute of Physics Publishing
- Publisher URL
- Copyright © 2009 The American Astronomical Society. All rights reserved. The American Astronomical Society does not allow institutions to archive either the accepted manuscript or the published version of the article. However, you can find an earlier version of the full text here: http://arxiv.org/abs/0908.2626.
- Peer reviewed