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PULSED GAMMA-RAYS FROM PSR J2021+3651 WITH THE FERMI LARGE AREA TELESCOPE

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A. A. Abdo1,54, M. Ackermann2, M. Ajello2, W. B. Atwood3, L. Baldini4, J. Ballet5, G. Barbiellini6,7, D. Bastieri8,9, M. Battelino10, B. M. Baughman11, K. Bechtol2, R. Bellazzini4, B. Berenji2, E. D. Bloom2, G. Bogaert12, A. W. Borgland2, J. Bregeon4, A. Brez4, M. Brigida13,14, P. Bruel12, T. H. Burnett15, G. A. Caliandro13,14, R. A. Cameron2, F. Camilo16, P. A. Caraveo17, J. M. Casandjian5, C. Cecchi18,19, E. Charles2, A. Chekhtman20,1, A. W. Chen17, C. C. Cheung21, J. Chiang2, S. Ciprini18,19, I. Cognard22, J. Cohen-Tanugi23, L. R. Cominsky24, J. Conrad10,25, S. Cutini26, P. Demorest27, C. D. Dermer1, A. de Angelis28, A. de Luca29, F. de Palma13,14, S. W. Digel2, M. Dormody3, E. do Couto e Silva2, P. S. Drell2, R. Dubois2, D. Dumora30,31, C. Espinoza32, C. Farnier23, C. Favuzzi13,14, W. B. Focke2, M. Frailis28, P. C. C. Freire33, Y. Fukazawa34, S. Funk2, P. Fusco13,14, F. Gargano14, D. Gasparrini26, N. Gehrels21,35, S. Germani18,19, B. Giebels12, N. Giglietto13,14, F. Giordano13,14, T. Glanzman2, G. Godfrey2, I. A. Grenier5, M.-H. Grondin30,31, J. E. Grove1, L. Guillemot30,31, S. Guiriec23, Y. Hanabata34, A. K. Harding21, M. Hayashida2, E. Hays21, R. E. Hughes11, G. Jóhannesson2, A. S. Johnson2, R. P. Johnson3, T. J. Johnson21,35, W. N. Johnson1, S. Johnston36, T. Kamae2, H. Katagiri34, J. Kataoka37, N. Kawai38,37, M. Kerr15, B. Kiziltan39, J. Knödlseder40, N. Komin5,23, M. Kramer32, F. Kuehn11, M. Kuss4, J. Lande2, L. Latronico4, S.-H. Lee2, M. Lemoine-Goumard30,31, F. Longo6,7, F. Loparco13,14, B. Lott30,31, M. N. Lovellette1, P. Lubrano18,19, A. G. Lyne32, A. Makeev20,1, R. N. Manchester36, M. Marelli17, M. N. Mazziotta14, W. McConville21, J. E. McEnery21, M. A. McLaughlin41, C. Meurer25, P. F. Michelson2, W. Mitthumsiri2, T. Mizuno34, A. A. Moiseev42, C. Monte13,14, M. E. Monzani2, A. Morselli43, I. V. Moskalenko2, S. Murgia2, P. L. Nolan2, A. Noutsos32, E. Nuss23, T. Ohsugi34, N. Omodei4, E. Orlando44, J. F. Ormes45, M. Ozaki46, D. Paneque2, J. H. Panetta2, D. Parent30,31, M. Pepe18,19, M. Pesce-Rollins4, F. Piron23, T. A. Porter3, S. Rainò13,14, R. Rando8,9, S. M. Ransom27, M. Razzano4, A. Reimer2, O. Reimer2, T. Reposeur30,31, S. Ritz21,35, L. S. Rochester2, A. Y. Rodriguez47, R. W. Romani2, F. Ryde10, H. F.-W. Sadrozinski3, D. Sanchez12, P. M. Saz Parkinson3, C. Sgrò4, A. Sierpowska-Bartosik47, E. J. Siskind48, D. A. Smith30,31, P. D. Smith11, G. Spandre4, P. Spinelli13,14, B. W. Stappers32, J.-L. Starck5, M. S. Strickman1, D. J. Suson49, H. Tajima2, H. Takahashi34, T. Takahashi46, T. Tanaka2, J. B. Thayer2, J. G. Thayer2, G. Theureau22, D. J. Thompson21, S. E. Thorsett3, L. Tibaldo8,9, D. F. Torres50,47, G. Tosti18,19, A. Tramacere51,2, Y. Uchiyama2, T. L. Usher2, A. Van Etten2, N. Vilchez40, V. Vitale43,52, A. P. Waite2, E. Wallace15, K. Watters2, P. Weltevrede36, K. S. Wood1, T. Ylinen53,10 and M. Ziegler3

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We report the detection of pulsed gamma-rays from the young, spin-powered radio pulsar PSR J2021+3651 using data acquired with the Large Area Telescope (LAT) on the Fermi Gamma-ray Space Telescope (formerly GLAST). The light curve consists of two narrow peaks of similar amplitude separated by 0.468 ± 0.002 in phase. The first peak lags the maximum of the 2 GHz radio pulse by 0.162 ± 0.004 ± 0.01 in phase. The integral gamma-ray photon flux above 100 MeV is (56 ± 3 ± 11) × 10–8 cm–2 s–1. The photon spectrum is well described by an exponentially cut-off power law of the form ${dF \over dE} = kE^{-\Gamma } e^{(-E/E_c)}$, where the energy E is expressed in GeV. The photon index is Γ = 1.5 ± 0.1 ± 0.1 and the exponential cut-off is Ec = 2.4 ± 0.3 ± 0.5 GeV. The first uncertainty is statistical and the second is systematic. The integral photon flux of the bridge is approximately 10% of the pulsed emission, and the upper limit on off-pulse gamma-ray emission from a putative pulsar wind nebula is < 10% of the pulsed emission at the 95% confidence level. Radio polarization measurements yield a rotation measure of RM = 524 ± 4 rad m–2 but a poorly constrained magnetic geometry. Re-analysis of Chandra X-ray Observatory data enhanced the significance of the weak X-ray pulsations, and the first peak is roughly phase aligned with the first gamma-ray peak. We discuss the emission region and beaming geometry based on the shape and spectrum of the gamma-ray light curve combined with radio and X-ray measurements, and the implications for the pulsar distance. Gamma-ray emission from the polar cap region seems unlikely for this pulsar.


Keywords

gamma rays: observations; pulsars: general; pulsars: individual (PSR J2021+3651)


Dates

Issue 2 (2009 August 1)

Received 2009 January 16, accepted for publication 2009 May 27

Published 2009 July 8



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