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

被引：47

作者：

Abdo, A. A. ^{[1
]}

Ackermann, M. ^{[2
,3
]}

Ajello, M. ^{[2
,3
]}

Atwood, W. B. ^{[4
,5
]}

Baldini, L. ^{[6
]}

Ballet, J. ^{[7
]}

Barbiellini, G. ^{[8
,9
]}

Bastieri, D. ^{[10
,11
]}

Battelino, M. ^{[12
]}

Baughman, B. M. ^{[13
]}

Bechtol, K. ^{[2
,3
]}

Bellazzini, R. ^{[6
]}

Berenji, B. ^{[2
,3
]}

Bloom, E. D. ^{[2
,3
]}

Bogaert, G. ^{[14
]}

Borgland, A. W. ^{[2
,3
]}

Bregeon, J. ^{[6
]}

Brez, A. ^{[6
]}

Brigida, M. ^{[15
,16
]}

Bruel, P. ^{[14
]}

Burnett, T. H. ^{[17
]}

Caliandro, G. A. ^{[15
,16
]}

Cameron, R. A. ^{[2
,3
]}

Camilo, F. ^{[18
]}

Caraveo, P. A. ^{[19
]}

Casandjian, J. M. ^{[7
]}

Cecchi, C. ^{[20
,21
]}

Charles, E. ^{[2
,3
]}

Chekhtman, A. ^{[1
,22
]}

Chen, A. W. ^{[19
]}

Cheung, C. C. ^{[23
]}

Chiang, J. ^{[2
,3
]}

Ciprini, S. ^{[20
,21
]}

Cognard, I. ^{[24
,25
]}

Cohen-Tanugi, J. ^{[26
]}

Cominsky, L. R. ^{[27
]}

Conrad, J. ^{[12
,28
]}

Cutini, S. ^{[29
]}

Demorest, P. ^{[30
]}

Dermer, C. D. ^{[1
]}

de Angelis, A. ^{[31
,32
]}

de Luca, A. ^{[33
]}

de Palma, F. ^{[15
,16
]}

Digel, S. W. ^{[2
,3
]}

Dormody, M. ^{[4
,5
]}

do Couto E Silva, E. ^{[2
,3
]}

Drell, P. S. ^{[2
,3
]}

Dubois, R. ^{[2
,3
]}

Dumora, D. ^{[34
,35
]}

Espinoza, C. ^{[36
]}

机构：

[1] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA

[2] Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA

[3] Stanford Univ, Stanford Linear Accelerator Ctr, Stanford, CA 94305 USA

[4] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA

[5] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA

[6] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy

[7] Univ Paris Diderot, CNRS, CEA, IRFU,Lab AIM,Serv Astrophys,CEA Saclay, F-91191 Gif Sur Yvette, France

[8] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy

[9] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy

[10] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy

[11] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy

[12] Royal Inst Technol KTH, Dept Phys, SE-10691 Stockholm, Sweden

[13] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA

[14] Ecole Polytech, CNRS, Lab Leprince Ringuet, IN2P3, F-91128 Palaiseau, France

[15] Univ Politecn Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy

[16] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy

[17] Univ Washington, Dept Phys, Seattle, WA 98195 USA

[18] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA

[19] Ist Astrofis Spaziale & Fis Cosm, INAF, I-20133 Milan, Italy

[20] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy

[21] Univ Perugia, Dipartimento Fis, I-60123 Perugia, Italy

[22] George Mason Univ, Fairfax, VA 22030 USA

[23] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA

[24] CNRS, UMR 6115, LPCE, F-45071 Orleans 02, France

[25] INSU, CNRS, Observ Paris, Stn Radioastron Nancay, F-18330 Nancay, France

[26] Univ Montpellier 2, Lab Phys Theor & Astroparticules, CNRS, IN2P3, Montpellier, France

[27] Sonoma State Univ, Dept Phys & Astron, Rohnert Pk, CA 94928 USA

[28] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden

[29] Sci Data Ctr, Agenzia Spaziale Italiana ASI, I-00044 Frascati, Roma, Italy

[30] Natl Radio Astron Observ, Charlottesville, VA 22903 USA

[31] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy

[32] Grp Coll Udine, Sez Trieste, Ist Nazl Fis Nucl, I-33100 Udine, Italy

[33] IUSS, I-27100 Pavia, Italy

[34] CEN Bordeaux Gradignan, CNRS, IN2P3, UMR 5797, F-33175 Gradignan, France

[35] Univ Bordeaux, Ctr Etud Nucl Bordeaux Gradignan, UMR 5797, F-33175 Gradignan, France

[36] Univ Manchester, Jodrell Bank, Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England

[37] Arecibo Observ, Arecibo, PR 00612 USA

[38] Hiroshima Univ, Dept Phys Sci, Higashihiroshima 7398526, Japan

[39] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Higashihiroshima 7398526, Japan

[40] Univ Maryland, College Pk, MD 20742 USA

[41] CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia

[42] Tokyo Inst Technol, Dept Phys, Meguro, Tokyo 1528551, Japan

[43] RIKEN, Inst Phys & Chem Res, Cosm Radiat Lab, Wako, Saitama 3510198, Japan

[44] Univ Calif Santa Cruz, Lick Observ, UCO, Santa Cruz, CA 95064 USA

[45] UPS, CNRS, Ctr Etud Spatiale Rayonnements, F-31028 Toulouse, France

[46] W Virginia Univ, Dept Phys, Morgantown, WV 26506 USA

[47] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA

[48] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy

[49] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany

[50] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA

来源：

ASTROPHYSICAL JOURNAL | 2009年 / 700卷 / 02期

关键词：

gamma rays: observations; pulsars: general; pulsars: individual (PSR J2021+3651); EMISSION; PULSARS; MODEL; POLARIZATION; CLUSTERS; CATALOG; GEMINGA; CRAB;

D O I：

10.1088/0004-637X/700/2/1059

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

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) x 10(-8) cm(-2) s(-1). The photon spectrum is well described by an exponentially cut-off power law of the form dF/dE = kE(-Gamma)e((-E/Ec)), where the energy E is expressed in GeV. The photon index is Gamma = 1.5 +/- 0.1 +/- 0.1 and the exponential cut-off is E-c = 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.

引用

页码：1059 / 1066

页数：8

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