2010/01/06 by Fermi LAT Collaboration, the Fermi Pulsar Timing Consortium, M. Ackermann +100
Physics and Astronomy · #Astronomy #Astrophysical Phenomena and Observations #Astrophysics #Astrophysics and Cosmic Phenomena #Fermi Gamma-ray Space Telescope #Flux (metallurgy) #Galaxy #Luminosity #Millisecond pulsar #Nebula #Physics #Pulsar #Pulsar wind nebula #Pulsars and Gravitational Waves Research #Stars #Supernova #Supernova remnant #Telescope #astro-ph.HE
paper · pdf · doi:10.1088/0004-637x/711/1/64
published as A. A. Abdo et al 2010 ApJ 711 64-74
arxiv created 2010/01/06 · openalex publication_date 2010/02/06 · arxiv updated 2015/05/14 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
We present multiwavelength studies of the 106.6 ms γ-ray pulsar PSR J1907+06 near the TeV source MGRO J1908+06. Timing observations with Fermi result in a precise position determination for the pulsar of R.A. = 19 h 07 m 54 7(2), decl. = +06°02'16(2)'' placing the pulsar firmly within the TeV source extent, suggesting the TeV source is the pulsar wind nebula of PSR J1907+0602. Pulsed γ-ray emission is clearly visible at energies from 100 MeV to above 10 GeV. The phase-averaged power-law index in the energy range E > 0.1 GeV is Γ = 1.76 ± 0.05 with an exponential cutoff energy E c = 3.6 ± 0.5 GeV. We present the energy-dependent γ-ray pulsed light curve as well as limits on off-pulse emission associated with the TeV source. We also report the detection of very faint (flux density of ≃ 3.4 μJy) radio pulsations with the Arecibo telescope at 1.5 GHz having a dispersion measure DM = 82.1 ± 1.1 cm −3 pc. This indicates a distance of 3.2 ± 0.6 kpc and a pseudo-luminosity of L 1400 ≃ 0.035 mJy kpc 2 . A Chandra ACIS observation revealed an absorbed, possibly extended, compact (≲4'') X-ray source with significant nonthermal emission at R.A. = 19 h 07 m 54 76, decl. = +06°02'14 6 with a flux of 2.3 +0.6 −1.4 × 10 −14 erg cm −2 s −1 . From archival ASCA observations, we place upper limits on any arcminute scale 2–10 keV X-ray emission of ∼1 × 10 −13 erg cm −2 s −1 . The implied distance to the pulsar is compatible with that of the supernova remnant G40.5 − 0.5, located on the far side of the TeV nebula from PSR J1907+0602, and the S74 molecular cloud on the nearer side which we discuss as potential birth sites.