FERMI LARGE AREA TELESCOPE OBSERVATIONS OF THE CRAB PULSAR AND NEBULA

被引：217

作者：

Abdo, A. A. ^{[1
,2
]}

Ackermann, M. ^{[3
,4
]}

Ajello, M. ^{[3
,4
]}

Atwood, W. B. ^{[5
,6
]}

Axelsson, M. ^{[7
,8
]}

Baldini, L. ^{[9
]}

Ballet, J. ^{[10
]}

Barbiellini, G. ^{[11
,12
]}

Baring, M. G. ^{[13
]}

Bastieri, D. ^{[14
,15
]}

Bechtol, K. ^{[3
,4
]}

Bellazzini, R. ^{[9
]}

Berenji, B. ^{[3
,4
]}

Blandford, R. D. ^{[3
,4
]}

Bloom, E. D. ^{[3
,4
]}

Bonamente, E. ^{[16
,17
]}

Borgland, A. W. ^{[3
,4
]}

Bregeon, J. ^{[9
]}

Brez, A. ^{[9
]}

Brigida, M. ^{[18
,19
,20
]}

Bruel, P. ^{[21
]}

Burnett, T. H. ^{[22
]}

Caliandro, G. A. ^{[23
]}

Cameron, R. A. ^{[3
,4
]}

Camilo, F. ^{[24
]}

Caraveo, P. A. ^{[25
]}

Casandjian, J. M. ^{[10
]}

Cecchi, C. ^{[16
,17
]}

Celik, Oe. ^{[26
,27
,28
,29
]}

Chekhtman, A. ^{[1
,30
]}

Cheung, C. C. ^{[1
,2
]}

Chiang, J. ^{[3
,4
]}

Ciprini, S. ^{[17
]}

Claus, R. ^{[3
,4
]}

Cognard, I. ^{[31
,32
]}

Cohen-Tanugi, J. ^{[33
]}

Cominsky, L. R. ^{[34
]}

Conrad, J. ^{[8
,35
]}

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

de Angelis, A. ^{[36
,37
]}

de Luca, A. ^{[38
]}

de Palma, F. ^{[18
,19
,20
]}

Digel, S. W. ^{[3
,4
]}

Silva, E. do Couto e ^{[3
,4
]}

Drell, P. S. ^{[3
,4
]}

Dubois, R. ^{[3
,4
]}

Dumora, D. ^{[39
,40
]}

Espinoza, C. ^{[41
]}

Farnier, C. ^{[33
]}

Favuzzi, C. ^{[18
,19
,20
]}

机构：

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

[2] Natl Acad Sci, Natl Res Council Res Associate, Washington, DC 20001 USA

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

[4] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA

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

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

[7] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden

[8] Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden

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

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

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

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

[13] Rice Univ, Dept Phys & Astron, Houston, TX 77251 USA

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

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

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

[17] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy

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

[19] Politecn Bari, I-70126 Bari, Italy

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

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

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

[23] IEEC CSIC, Inst Ciencies Espai, Barcelona 08193, Spain

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

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

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

[27] CRESST, Greenbelt, MD 20771 USA

[28] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA

[29] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA

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

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

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

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

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

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

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

[37] Ist Nazl Fis Nucl, Sez Trieste, Grp Collegato Udine, I-33100 Udine, Italy

[38] IUSS, I-27100 Pavia, Italy

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

[40] Ctr Etud Nucl Bordeaux Gradignan, UMR 5797, IN2P3, CNRS, F-33175 Gradignan, France

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

[42] Arecibo Observ, Arecibo, PR 00612 USA

[43] ASI, Sci Data Ctr, I-00044 Frascati, Roma, Italy

[44] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan

[45] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA

[46] Univ Maryland, Dept Phys, College Pk, MD 20742 USA

[47] Univ Maryland, Dept Astron, College Pk, MD 20742 USA

[48] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA

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

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

来源：

ASTROPHYSICAL JOURNAL | 2010年 / 708卷 / 02期

基金：

美国国家航空航天局; 英国科学技术设施理事会; 瑞典研究理事会;

关键词：

gamma rays: observations; ISM: individual (Crab Nebula); pulsars: individual (Crab); supernova remnants; GAMMA-RAY PULSARS; HIGH-ENERGY; TIMING OBSERVATIONS; SPACE-TELESCOPE; LIGHT CURVES; EGRET DATA; X-RAYS; 50; TEV; EMISSION; RADIATION;

D O I：

10.1088/0004-637X/708/2/1254

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We report on gamma-ray observations of the Crab Pulsar and Nebula using 8 months of survey data with the Fermi Large Area Telescope (LAT). The high quality light curve obtained using the ephemeris provided by the Nancay and Jodrell Bank radio telescopes shows two main peaks stable in phase with energy. The first gamma-ray peak leads the radio main pulse by (281 +/- 12 +/- 21) mu s, giving new constraints on the production site of non-thermal emission in pulsar magnetospheres. The first uncertainty is due to gamma-ray statistics, and the second arises from the rotation parameters. The improved sensitivity and the unprecedented statistics afforded by the LAT enable precise measurement of the Crab Pulsar spectral parameters: cut-off energy at E(c) = (5.8 +/- 0.5 +/- 1.2) GeV, spectral index of Gamma = (1.97 +/- 0.02 +/- 0.06) and integral photon flux above 100 MeV of (2.09 +/- 0.03 +/- 0.18) x 10(-6) cm(-2) s(-1). The first errors represent the statistical error on the fit parameters, while the second ones are the systematic uncertainties. Pulsed gamma-ray photons are observed up to similar to 20 GeV which precludes emission near the stellar surface, below altitudes of around 4-5 stellar radii in phase intervals encompassing the two main peaks. A detailed phase-resolved spectral analysis is also performed: the hardest emission from the Crab Pulsar comes from the bridge region between the two gamma-ray peaks while the softest comes from the falling edge of the second peak. The spectrum of the nebula in the energy range 100 MeV-300 GeV is well described by the sum of two power laws of indices Gamma(sync) = (3.99 +/- 0.12 +/- 0.08) and Gamma(IC) = (1.64 +/- 0.05 +/- 0.07), corresponding to the falling edge of the synchrotron and the rising edge of the inverse Compton (IC) components, respectively. This latter, which links up naturally with the spectral data points of Cherenkov experiments, is well reproduced via IC scattering from standard magnetohydrodynamic nebula models, and does not require any additional radiation mechanism.

引用

页码：1254 / 1267

页数：14

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