RADIO DETECTION OF LAT PSRs J1741-2054 AND J2032+4127: NO LONGER JUST GAMMA-RAY PULSARS
- 7 October 2009
- journal article
- research article
- Published by American Astronomical Society in The Astrophysical Journal
- Vol. 705 (1), 1-13
- https://doi.org/10.1088/0004-637x/705/1/1
Abstract
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 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. 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.Keywords
This publication has 61 references indexed in Scilit:
- A Population of Gamma-Ray Millisecond Pulsars Seen with the Fermi Large Area TelescopeScience, 2009
- Detection of 16 Gamma-Ray Pulsars Through Blind Frequency Searches Using the Fermi LATScience, 2009
- MILAGRO OBSERVATIONS OF MULTI-TeV EMISSION FROM GALACTIC SOURCES IN THE FERMI BRIGHT SOURCE LISTThe Astrophysical Journal, 2009
- PULSED GAMMA-RAYS FROM PSR J2021+3651 WITH THEFERMILARGE AREA TELESCOPEThe Astrophysical Journal, 2009
- DISCOVERY OF PULSATIONS FROM THE PULSAR J0205+6449 IN SNR 3C 58 WITH THE FERMI GAMMA-RAY SPACE TELESCOPEThe Astrophysical Journal, 2009
- FERMI/LARGE AREA TELESCOPE BRIGHT GAMMA-RAY SOURCE LISTThe Astrophysical Journal Supplement Series, 2009
- FERMILARGE AREA TELESCOPE OBSERVATIONS OF THE VELA PULSARThe Astrophysical Journal, 2009
- Discovery of TeV Gamma-Ray Emission from the Cygnus Region of the GalaxyThe Astrophysical Journal, 2007
- The unidentified TeV source (TeV J2032+4130) and surrounding field: Final HEGRA IACT-System resultsAstronomy & Astrophysics, 2005
- An unidentified TeV source in the vicinity of Cygnus OB2Astronomy & Astrophysics, 2002