GAMMA-RAY AND RADIO PROPERTIES OF SIX PULSARS DETECTED BY THE FERMI LARGE AREA TELESCOPE

被引：50

作者：

Weltevrede, P. ^{[1
,2
]}

Abdo, A. A. ^{[3
,4
]}

Ackermann, M. ^{[5
,6
]}

Ajello, M. ^{[5
,6
]}

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

Baldini, L. ^{[9
]}

Ballet, J. ^{[10
]}

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

Bastieri, D. ^{[13
,14
]}

Baughman, B. M. ^{[15
]}

Bechtol, K. ^{[5
,6
]}

Bellazzini, R. ^{[9
]}

Berenji, B. ^{[5
,6
]}

Bloom, E. D. ^{[5
,6
]}

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

Borgland, A. W. ^{[5
,6
]}

Bregeon, J. ^{[9
]}

Brez, A. ^{[9
]}

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

Bruel, P. ^{[20
]}

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

Buson, S. ^{[14
]}

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

Cameron, R. A. ^{[5
,6
]}

Camilo, F. ^{[22
]}

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

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

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

Celik, Oe. ^{[24
,25
]}

Charles, E. ^{[5
,6
]}

Chekhtman, A. ^{[3
,26
]}

Cheung, C. C. ^{[3
,4
]}

Chiang, J. ^{[5
,6
]}

Ciprini, S. ^{[16
,17
]}

Claus, R. ^{[5
,6
]}

Cognard, I. ^{[27
,28
]}

Cohen-Tanugi, J. ^{[29
]}

Cominsky, L. R. ^{[30
]}

Conrad, J. ^{[8
,31
]}

Cutini, S. ^{[3
]}

Dermer, C. D. ^{[3
]}

Desvignes, G. ^{[27
,28
]}

de Angelis, A. ^{[33
,34
]}

de Luca, A. ^{[23
,35
]}

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

Digel, S. W. ^{[5
,6
]}

Dormody, M. ^{[36
,37
]}

do Couto e Silva, E. ^{[5
,6
]}

Drell, P. S. ^{[5
,6
]}

Dubois, R. ^{[5
,6
]}

机构：

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

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

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

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

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

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

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

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

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

[10] Univ Paris Diderot, CNRS, CEA Saclay, Lab AIM,CEA,IRFU,Serv Astrophys, 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] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy

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

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

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

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

[18] Univ Politecn Bari, Dipartimento Fis M Merlin, 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, CRESST, Greenbelt, MD 20771 USA

[25] Univ Maryland, Baltimore, MD 21250 USA

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

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

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

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

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

[31] Stockholm Univ, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden

[32] Agenzia Spaziale Italiana ASI Sci Data Ctr, I-00044 Rome, Italy

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

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

[35] IUSS, I-27100 Pavia, Italy

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

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

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

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

[40] Arecibo Observ, Arecibo, PR 00612 USA

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

[42] Max Planck Inst Radioastron, D-53121 Bonn, Germany

[43] Univ Alabama, Huntsville, AL 35899 USA

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

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

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

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

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

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

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

来源：

ASTROPHYSICAL JOURNAL | 2010年 / 708卷 / 02期

基金：

美国国家航空航天局; 瑞典研究理事会; 英国科学技术设施理事会; 美国国家科学基金会;

关键词：

pulsars: individual (PSRs J0631+1036; J0659+1414; J0742-2822; J1420-6048; J1509-5850; J1718-3825); MIDDLE-AGED PULSARS; PSR B0656+14; SOUTHERN PULSARS; EMPIRICAL-THEORY; NEUTRON-STARS; WIND NEBULAE; EMISSION REGION; SPACE-TELESCOPE; TIMING PACKAGE; YOUNG PULSARS;

D O I：

10.1088/0004-637X/708/2/1426

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 for PSRs J0631+1036, J0659+1414, J0742-2822, J1420-6048, J1509-5850, and J1718-3825 using the Large Area Telescope on board the Fermi Gamma-ray Space Telescope (formerly known as GLAST). Although these six pulsars are diverse in terms of their spin parameters, they share an important feature: their gamma-ray light curves are (at least given the current count statistics) single peaked. For two pulsars, there are hints for a double-peaked structure in the light curves. The shapes of the observed light curves of this group of pulsars are discussed in the light of models for which the emission originates from high up in the magnetosphere. The observed phases of the gamma-ray light curves are, in general, consistent with those predicted by high-altitude models, although we speculate that the gamma-ray emission of PSR J0659+1414, possibly featuring the softest spectrum of all Fermi pulsars coupled with a very low efficiency, arises from relatively low down in the magnetosphere. High-quality radio polarization data are available showing that all but one have a high degree of linear polarization. This allows us to place some constraints on the viewing geometry and aids the comparison of the gamma-ray light curves with high-energy beam models.

引用

页码：1426 / 1441

页数：16

共 86 条

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