FERMI LARGE AREA TELESCOPE OBSERVATIONS OF THE VELA-X PULSAR WIND NEBULA

被引：58

作者：

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

Ackermann, M. ^{[1
,2
]}

Ajello, M. ^{[1
,2
]}

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

Baldini, L. ^{[5
]}

Ballet, J. ^{[6
]}

Barbiellini, G. ^{[7
,8
]}

Bastieri, D. ^{[9
,10
]}

Bechtol, K. ^{[1
,2
]}

Bellazzini, R. ^{[5
]}

Berenji, B. ^{[1
,2
]}

Blandford, R. D. ^{[1
,2
]}

Bloom, E. D. ^{[1
,2
]}

Bonamente, E. ^{[11
,12
]}

Borgland, A. W. ^{[1
,2
]}

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

Bregeon, J. ^{[5
]}

Brez, A. ^{[5
]}

Brigida, M. ^{[13
,14
]}

Bruel, P. ^{[15
]}

Burnett, T. H. ^{[16
]}

Buson, S. ^{[10
]}

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

Cameron, R. A. ^{[1
,2
]}

Caraveo, P. A. ^{[18
]}

Carrigan, S. ^{[10
]}

Casandjian, J. M. ^{[6
]}

Cecchi, C. ^{[11
,12
]}

Celik, Oe ^{[19
,20
,21
,22
]}

Chekhtman, A. ^{[3
,23
]}

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

Chiang, J. ^{[1
,2
]}

Ciprini, S. ^{[12
]}

Claus, R. ^{[1
,2
]}

Cohen-Tanugi, J. ^{[24
]}

Conrad, J. ^{[25
,26
,27
,28
]}

de Angelis, A. ^{[27
,28
]}

de Palma, F. ^{[13
,14
]}

Dormody, M. ^{[29
,30
]}

do Couto e Silva, E. ^{[1
,2
]}

Drell, P. S. ^{[1
,2
]}

Dubois, R. ^{[1
,2
]}

Dumora, D. ^{[31
,32
]}

Farnier, C. ^{[24
]}

Favuzzi, C. ^{[13
,14
]}

Fegan, S. J. ^{[15
]}

Focke, W. B. ^{[1
,2
]}

Fortin, P. ^{[15
]}

Frailis, M. ^{[27
,28
]}

Fukazawa, Y. ^{[33
]}

机构：

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

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

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

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

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

[8] Univ Trieste, Dipartmento Fis, I-34127 Trieste, Italy

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

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

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

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

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

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

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

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

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

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

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

[20] CRESST, Greenbelt, MD 20771 USA

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

[37] Univ Alabama, Ctr Space Plasma & Aeronom Res, Huntsville, AL 35899 USA

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

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

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

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

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

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

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

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

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

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

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

[49] JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan

[50] Sterrenkundig Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands

来源：

ASTROPHYSICAL JOURNAL | 2010年 / 713卷 / 01期

基金：

美国国家航空航天局;

关键词：

gamma rays: general; pulsars: general; pulsars:; individual; (Vela; PSR J0835-4510); SUPERNOVA REMNANT; SYNCHROTRON NEBULA; RAY-EMISSION; EVOLUTION; DISCOVERY; RADIATION; RADIO; HESS; LAT; GHZ;

D O I：

10.1088/0004-637X/713/1/146

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We report on gamma-ray observations in the off-pulse window of the Vela pulsar PSR B0833-45 using 11 months of survey data from the Fermi Large Area Telescope (LAT). This pulsar is located in the 8 degrees diameter Vela supernova remnant, which contains several regions of non-thermal emission detected in the radio, X-ray, and gamma-ray bands. The gamma-ray emission detected by the LAT lies within one of these regions, the 2 degrees x 3 degrees area south of the pulsar known as Vela-X. The LAT flux is significantly spatially extended with a best-fit radius of 0.degrees 88 +/- 0.degrees 12 for an assumed radially symmetric uniform disk. The 200 MeV to 20 GeV LAT spectrum of this source is well described by a power law with a spectral index of 2.41 +/- 0.09 +/- 0.15 and integral flux above 100 MeV of (4.73 +/- 0.63 +/- 1.32) x 10(-7) cm(-2) s(-1). The first errors represent the statistical error on the fit parameters, while the second ones are the systematic uncertainties. Detailed morphological and spectral analyses give strong constraints on the energetics and magnetic field of the pulsar wind nebula system and favor a scenario with two distinct electron populations.

引用

页码：146 / 153

页数：8

共 35 条

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