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.  Saz; 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.

doi:10.1088/0004-637X/705/1/1

Radio Detection of LAT PSRs J1741-2054 and J2032+4127: No Longer Just Gamma-Ray Pulsars

Journal Article · Wed Oct 07 00:00:00 EDT 2009 · The Astrophysical Journal

DOI:https://doi.org/10.1088/0004-637X/705/1/1· OSTI ID:1357430

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. Saz; Ziegler, M.; Dormody, M.; Thompson, D. J.; Smith, D. A.; Harding, A. K.; Abdo, A. A. more »

We present that 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 $$\dot{E} = 9.4\times 10^{33}$$ 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 gamma-ray pulsars. Faint, diffuse X-ray emission in a Chandra image is possibly its pulsar wind nebula. Finally, 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.

View Accepted Manuscript (DOE)

Research Organization:: SLAC National Accelerator Laboratory (SLAC), Menlo Park, CA (United States)

Sponsoring Organization:: USDOE

Contributing Organization:: Fermi-LAT Collaboration

Grant/Contract Number:: AC02-76SF00515

OSTI ID:: 1357430

Alternate ID(s):: OSTI ID: 21378417

Journal Information:: The Astrophysical Journal, Journal Name: The Astrophysical Journal Journal Issue: 1 Vol. 705; ISSN 0004-637X

Publisher:: Institute of Physics (IOP)Copyright Statement

Country of Publication:: United States

Language:: English

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