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PSR J1907+0602: A Radio-Faint Gamma-Ray Pulsar Powering a Bright TeV Pulsar Wind Nebula

A. Abdo, A. / Ackermann, M. / Ajello, M. / Baldini, L. / Ballet, J. / Barbiellini, G. / Bastieri, D. / M. Baughman, B. / Bechtol, K. / Bellazzini, R. / Berenji, B. / D. Blandford, R. / D. Bloom, E. / Bonamente, E. / W. Borgland, A. / Bregeon, J. / Brez, A. / Brigida, M. / Bruel, P. / H. Burnett, T. / Buson, S. / A. Caliandro, G. / A. Cameron, R. / Camilo, F. / A. Caraveo, P. / M. Casandjian, J. / Cecchi, C. / Çelik, Ö. / Chekhtman, A. / C. Cheung, C. / Chiang, J. / Ciprini, S. / Claus, R. / Cognard, I. / Cohen-Tanugi, J. / R. Cominsky, L. / Conrad, J. / Cutini, S. / De Angelis, A. / De Palma, F. / W. Digel, S. / L. Dingus, B. / Dormody, M. / Do Couto E Silva, E. / S. Drell, P. / Dubois, R. / Dumora, D. / Farnier, C. / Favuzzi, C. / J. Fegan, S. / B. Focke, W. / Fortin, P. / Frailis, M. / C. C. Freire, P. / Fukazawa, Y. / Funk, S. / Fusco, P. / Gargano, F. / Gasparrini, D. / Gehrels, N. / Germani, S. / Giavitto, G. / Giebels, B. / Giglietto, N. / Giordano, F. / Glanzman, T. / Godfrey, G. / A. Grenier, I. / Grondin, M.-H. / E. Grove, J. / Guillemot, L. / Guiriec, S. / Hanabata, Y. / K. Harding, A. / Hays, E. / E. Hughes, R. / S. Jackson, M. / Jóhannesson, G. / S. Johnson, A. / J. Johnson, T. / N. Johnson, W. / Johnston, S. / Kamae, T. / Katagiri, H. / Kataoka, J. / Kawai, N. / Kerr, M. / Knödlseder, J. / L. Kocian, M. / Kuss, M. / Lande, J. / Latronico, L. / Lemoine-Goumard, M. / Longo, F. / Loparco, F. / Lott, B. / N. Lovellette, M. / Lubrano, P. / Makeev, A. / Marelli, M. / N. Mazziotta, M. / E. Mcenery, J. / Meurer, C. / F. Michelson, P. / Mitthumsiri, W. / Mizuno, T. / A. Moiseev, A. / Monte, C. / E. Monzani, M. / Morselli, A. / V. Moskalenko, I. / Murgia, S. / L. Nolan, P. / P. Norris, J. / Nuss, E. / Ohsugi, T. / Omodei, N. / Orlando, E. / F. Ormes, J. / Paneque, D. / Parent, D. / Pelassa, V. / Pepe, M. / Pesce-Rollins, M. / Piron, F. / Porter, T.A. / Rainò, S. / Rando, R. / S. Ray, P. / Razzano, M. / Reimer, A. / Reimer, O. / Reposeur, T. / Ritz, S. / S. E. Roberts, M. / S. Rochester, L. / Y. Rodriguez, A. / W. Ro'Mani, R. / Roth, M. / Ryde, F. / F.-W. Sadrozinski, H. / Sanchez, D. / Sander, A. / M. Saz Parkinson, P. / D. Scargle, J. / Sgrò, C. / J. Siskind, E. / A. Smith, D. / D. Smith, P. / Spandre, G. / Spinelli, P. / S. Strickman, M. / J. Suson, D. / Tajima, H. / Takahashi, H. / Tanaka, T. / B. Thayer, J. / G. Thayer, J. / Theureau, G. / J. Thompson, D. / Tibaldo, L. / Tibolla, O. / F. Torres, D. / Tosti, G. / Tramacere, A. / Uchiyama, Y. / L. Usher, T. / Van Etten, A. / Vasileiou, V. / Venter, C. / Vilchez, N. / Vitale, V. / P. Waite, A. / Wang, P. / Watters, K. / L. Winer, B. / T. Wolff, M. / S. Wood, K. / Ylinen, T. / Ziegler, M. - 2010
We present multiwavelength studies of the 106.6 ms gamma-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. = 19h07m547(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 gamma-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 = 1.76 \pm 0.05 with an exponential cutoff energy E_{c} = 3.6 \pm 0.5 GeV. We present the energy-dependent gamma-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 microJy) radio pulsations with the Arecibo telescope at 1.5 GHz having a dispersion measure DM = 82.1 \pm 1.1 cm^{-3}pc. This indicates a distance of 3.2 \pm 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 arcsec) X-ray source with significant non-thermal emission at R.A. = 19h07m54.76, decl. = +06:02:14.6 with a flux of 2.3^{+0.6}_{-1.4} X 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 X 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.

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