DISCOVERY OF PULSATIONS FROM THE PULSAR J0205+6449 IN SNR 3C 58 WITH THE FERMI GAMMA-RAY SPACE TELESCOPE

被引：29

作者：

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

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

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

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

Axelsson, M. ^{[6
,7
]}

Baldini, L. ^{[8
]}

Ballet, J. ^{[9
]}

Barbiellini, G. ^{[10
,11
]}

Bastieri, D. ^{[12
,13
]}

Baughman, B. M. ^{[14
]}

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

Bellazzini, R. ^{[8
]}

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

Blandford, R. D. ^{[2
,3
]}

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

Bonamente, E. ^{[15
,16
]}

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

Bouvier, A. ^{[2
,3
]}

Bregeon, J. ^{[8
]}

Brez, A. ^{[8
]}

Brigida, M. ^{[17
,18
,19
]}

Bruel, P. ^{[20
]}

Burnett, T. H. ^{[21
]}

Caliandro, G. A. ^{[17
,18
,19
]}

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

Camilo, F. ^{[22
]}

Caraveo, P. A. ^{[23
]}

Casandjian, J. M. ^{[9
]}

Cecchi, C. ^{[15
,16
]}

Celik, Oe ^{[24
]}

Chekhtman, A. ^{[1
,25
]}

Cheung, C. C. ^{[24
]}

Chiang, J. ^{[2
]}

Ciprini, S. ^{[15
,16
]}

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

Cognard, I. ^{[26
,27
]}

Cohen-Tanugi, J. ^{[28
]}

Conrad, J. ^{[6
,29
,30
]}

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

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

de Palma, F. ^{[17
,18
,19
]}

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. ^{[33
,34
]}

Edmonds, Y. ^{[2
,3
]}

Espinoza, C. ^{[35
]}

Farnier, C. ^{[28
]}

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, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA

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

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

[6] Oskar Klein Ctr Cosmo Particle Phys, SE-10691 Stockholm, Sweden

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

[26] CNRS, LPCE, UMR 6115, Lab Phys & Chem Environm, F-45071 Orleans 02, France

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

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

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

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

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

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

[33] CEN Bordeaux Gradignan, CNRS, IN2P3, F-33175 Gradignan, France

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

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

[36] Arecibo Observ, Arecibo, PR 00612 USA

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

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

[39] Univ Alabama, Huntsville, AL 35899 USA

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

[41] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada

[42] Waseda Univ, Shinjuku Ku, Tokyo 1698050, Japan

[43] RIKEN, Cosm Radiat Lab, Wako, Saitama 3510198, Japan

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

[45] UPS, CNRS, Ctr Etud Spatiale Rayonnements, F-31028 Toulouse 4, France

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

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

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

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

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

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2009年 / 699卷 / 02期

基金：

瑞典研究理事会;

关键词：

pulsars: general; stars: neutron; SUPERNOVA REMNANT 3C-58; LARGE-AREA TELESCOPE; X-RAY; NOVA REMNANTS; EMISSION; GALAXY; MODEL;

D O I：

10.1088/0004-637X/699/2/L102

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We report the discovery of gamma-ray pulsations (>= 0.1 GeV) from the young radio and X-ray pulsar PSR J0205 + 6449 located in the Galactic supernova remnant 3C 58. Data in the gamma-ray band were acquired by the Large Area Telescope aboard the Fermi Gamma-ray Space Telescope (formerly GLAST), while the radio rotational ephemeris used to fold gamma-rays was obtained using both the Green Bank Telescope and the Lovell telescope at Jodrell Bank. The light curve consists of two peaks separated by 0.49 +/- 0.01 +/- 0.01 cycles which are aligned with the X-ray peaks. The first gamma-ray peak trails the radio pulse by 0.08 +/- 0.01 +/- 0.01, while its amplitude decreases with increasing energy as for the other gamma-ray pulsars. Spectral analysis of the pulsed gamma-ray emission suggests a simple power law of index -2.1 +/- 0.1 +/- 0.2 with an exponential cutoff at 3.0(-0.7)(+1.1) +/- 0.4 GeV. The first uncertainty is statistical and the second is systematic. The integral gamma-ray photon flux above 0.1 GeV is (13.7 +/- 1.4 +/- 3.0) x 10(-8) cm(-2) s(-1), which implies for a distance of 3.2 kpc and assuming a broad fan-like beam a luminosity of 8.3 x 10(34) erg s(-1) and an efficiency eta of 0.3%. Finally, we report a 95% upper limit on the flux of 1.7 x 10(-8) cm(-2) s(-1) for off-pulse emission from the object.

引用

页码：L102 / L107

页数：6

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