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Ajello, M; Barbiellini, G; Bastieri, D; Baughman, B. M; Bellazzini, R; Bloom, E. D; Borgland, A. W; Bregeon, J; Brigida, M; Bruel, P; Buson, S; Caliandro, G. A; Camilo, F; Cecchi, C; Cheung, C. C; Chiang, J; Ciprini, S; Cognard, I; Cominsky, L. R; Cutini, S; de Palma, F; Digel, S. W; Dingus, B. L; Dormody, M; do Couto e Silva, E; Drell, P. S; Dubois, R; Farnier, C; Favuzzi, C; Fegan, S. J; Fortin, P; Fusco, P; Gargano, F; Gasparrini, D; Gehrels, N; Giglietto, N; Giordano, F; Grondin, M.-H; Grove, J. E; Hanabata, Y; Harding, A. K; Hughes, R. E; Jóhannesson, G; Johnson, W. N; Johnston, S; Kawai, N; Kerr, M; Knödlseder, J; Kocian, M. L; Kuss, M; Latronico, L; Lemoine-Goumard, M; Lovellette, M. N; Lubrano, P; Makeev, A; Michelson, P. F; Mizuno, T; Moiseev, A. A; Morselli, A; Moskalenko, I. V; Murgia, S; Nolan, P. L; Norris, J. P; Nuss, E; Parent, D; Pelassa, V; Pesce-Rollins, M; Porter, T. A; Rainò, S; Ray, P. S; Razzano, M; Reimer, A; Reposeur, T; Roberts, M. S. E; Rodriguez, A. Y; Ro‘mani, R. W; Ryde, F; Sadrozinski, H. F.-W; Sander, A; Sgrò, C; Smith, D. A; Smith, P. D; Suson, D. J; Tajima, H; Takahashi, H; Thayer, J. B; Thayer, J. G; Thompson, D. J; Torres, D. F; Tosti, G; Tramacere, A; Uchiyama, Y; Usher, T. L; Vilchez, N; Wang, P; Watters, K; Winer, B. L; Wood, K. S; Ylinen, T; Ziegler, M
The Astrophysical journal, 03/2010, Letnik: 711, Številka: 1Journal Article
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.
