PSR J1907+0602: A RADIO-FAINT GAMMA-RAY PULSAR POWERING A BRIGHT TeV PULSAR WIND NEBULA

被引：78

作者：

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

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

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

Baldini, L. ^{[5
]}

Ballet, J. ^{[6
]}

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

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

Baughman, B. M. ^{[11
]}

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

Bellazzini, R. ^{[5
]}

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

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

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

Bonamente, E. ^{[12
,13
]}

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

Bregeon, J. ^{[5
]}

Brez, A. ^{[5
]}

Brigida, M. ^{[14
,15
]}

Bruel, P. ^{[16
]}

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

Buson, S. ^{[10
]}

Caliandro, G. A. ^{[14
,15
]}

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

Camilo, F. ^{[18
]}

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

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

Cecchi, C. ^{[12
,13
]}

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

Chekhtman, A. ^{[1
,23
]}

Cheung, C. C. ^{[20
]}

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

Ciprini, S. ^{[12
,13
]}

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

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

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

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

Conrad, J. ^{[28
,29
]}

Cutini, S. ^{[30
]}

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

de Palma, F. ^{[14
,15
]}

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

Dingus, B. L. ^{[33
]}

Dormody, M. ^{[34
,35
]}

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

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

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

Dumora, D. ^{[36
,37
]}

Farnier, C. ^{[26
]}

Favuzzi, C. ^{[14
,15
]}

Fegan, S. J. ^{[16
]}

机构：

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

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

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

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

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

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

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

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

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

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

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

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

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

[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] NASA, Goddard Space Flight Ctr, 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, Coll Sci, Ctr Earth Observing & Space Res, Fairfax, VA 22030 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] Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden

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

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

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

[33] Los Alamos Natl Lab, Los Alamos, NM 87545 USA

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

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

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

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

[38] Arecibo Observ, Arecibo, PR 00612 USA

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

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

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

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

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

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

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

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

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

[48] RIKEN, Inst Phys & Chem Res, 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 / 711卷 / 01期

基金：

美国国家航空航天局;

关键词：

gamma rays: general; pulsars: general; pulsars: individual (PSR J1907+0602); supernovae: individual (SNR G40.5-0.5); X-RAY; GALACTIC PLANE; AREA TELESCOPE; REMNANT; EMISSION; CATALOG;

D O I：

10.1088/0004-637X/711/1/64

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present multiwavelength studies of the 106.6 ms gamma-ray pulsar PSR J1907+06 near the TeV source MGRO J1908+06. Timing observations with Fermi result in a precise position determination for the pulsar of R.A. = 19(h)07(m)54.(s)7(2), decl. = +06 degrees 02'16(2)'' placing the pulsar firmly within the TeV source extent, suggesting the TeV source is the pulsar wind nebula of PSR J1907+0602. Pulsed gamma-ray emission is clearly visible at energies from 100 MeV to above 10 GeV. The phase-averaged power-law index in the energy range E > 0.1 GeV is Gamma = 1.76 +/- 0.05 with an exponential cutoff energy E-c = 3.6 +/- 0.5 GeV. We present the energy-dependent gamma-ray pulsed light curve as well as limits on off-pulse emission associated with the TeV source. We also report the detection of very faint (flux density of similar or equal to 3.4 mu Jy) radio pulsations with the Arecibo telescope at 1.5 GHz having a dispersion measure DM = 82.1 +/- 1.1 cm(-3) pc. This indicates a distance of 3.2 +/- 0.6 kpc and a pseudo-luminosity of L-1400 similar or equal to 0.035 mJy kpc(2). A Chandra ACIS observation revealed an absorbed, possibly extended, compact (less than or similar to 4 '') X-ray source with significant nonthermal emission at R.A. = 19(h)07(m)54.(s)76, decl. = + 06 degrees 02'14.'' 6 with a flux of 2.3(-1.4)(+0.6) x 10(-14) erg cm(-2) s(-1). From archival ASCA observations, we place upper limits on any arcminute scale 2-10 keV X-ray emission of similar to 1 x 10(-13) erg cm(-2) s(-1). The implied distance to the pulsar is compatible with that of the supernova remnant G40.5-0.5, located on the far side of the TeV nebula from PSR J1907+0602, and the S74 molecular cloud on the nearer side which we discuss as potential birth sites.

引用

页码：64 / 74

页数：11

共 41 条

[41] Molecular gas distribution around the supernova remnant G40.5-0.5
Yang, J
Zhang, JL
Cai, ZY
Lu, DR
Tan, YH
[J]. CHINESE JOURNAL OF ASTRONOMY AND ASTROPHYSICS, 2006, 6 (02): : 210 - 216

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