A. A. Abdo et al. 2009 ApJ 700 1059 doi:10.1088/0004-637X/700/2/1059
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
Show affiliationsWe 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
, 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.
gamma rays: observations; pulsars: general; pulsars: individual (PSR J2021+3651)
Issue 2 (2009 August 1)
Received 2009 January 16, accepted for publication 2009 May 27
Published 2009 July 8
A. A. Abdo et al. 2009 ApJ 700 1059
Bülent Kiziltan and Stephen E. Thorsett 2009 ApJ 693 L109
W M Tang and V S Chan 2005 Plasma Phys. Control. Fusion 47 R1
A V Dzhamay and E M Vorob'ev 1994 J. Phys. A: Math. Gen. 27 5541
B M Penetrante et al 1997 Plasma Sources Sci. Technol. 6 251
D Sameoto and C Menon 2009 J. Micromech. Microeng. 19 115026
D Sameoto and C Menon 2009 J. Micromech. Microeng. 19 115002
Mona Rahbar et al 2010 J. Micromech. Microeng. 20 015026
Gorazd Cvetič and Héctor E Martínez 2009 J. Phys. G: Nucl. Part. Phys. 36 125006
M L McClure and C C Dyer 2006 Class. Quantum Grav. 23 1971