RADIO AND γ-RAY CONSTRAINTS ON THE EMISSION GEOMETRY AND BIRTHPLACE OF PSR J2043+2740

被引：9

作者：

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

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

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

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

Ballet, J. ^{[7
]}

Barbiellini, G. ^{[8
,9
]}

Baring, M. G. ^{[10
]}

Bastieri, D. ^{[11
,12
]}

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

Bellazzini, R. ^{[13
]}

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

Bonamente, E. ^{[14
,15
]}

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

Bregeon, J. ^{[13
]}

Brez, A. ^{[13
]}

Brigida, M. ^{[16
,17
]}

Bruel, P. ^{[18
]}

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

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

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

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

Camilo, F. ^{[20
]}

Caraveo, P. A. ^{[21
]}

Casandjian, J. M. ^{[7
]}

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

Celik, Oe ^{[22
,23
,24
,25
]}

Chaty, S. ^{[7
]}

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

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

Ciprini, S. ^{[15
]}

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

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

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

Colafrancesco, S. ^{[30
]}

Cutini, S. ^{[30
]}

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

de Palma, F. ^{[16
,17
]}

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

Dumora, D. ^{[31
]}

Ea, C. M. ^{[2
]}

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

Ferrara, E. C. ^{[22
]}

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

Frailis, M. ^{[32
,33
,34
]}

Freire, P. C. C. ^{[1
]}

Fukazawa, Y. ^{[35
]}

Funk, S. ^{[5
,6
]}

Fusco, P. ^{[16
,17
]}

Gargano, F. ^{[17
]}

Germani, S. ^{[14
,15
]}

机构：

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

[23] CRESST, Greenbelt, MD 20771 USA

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

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

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

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

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

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

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

[31] Univ Bordeaux 1, CNRS, Ctr Etud Nucl Bordeaux Gradignan, IN2P3, F-33175 Gradignan, France

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

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

[34] Osserv Astron Trieste, Ist Nazl Astrofis, I-34143 Trieste, Italy

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

[36] INAF Ist Radioastron, I-40129 Bologna, Italy

[37] Univ Alabama, CSPAR, Huntsville, AL 35899 USA

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

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

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

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

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

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

[44] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan

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

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

[47] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan

[48] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan

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

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

来源：

ASTROPHYSICAL JOURNAL | 2011年 / 728卷 / 02期

基金：

英国科学技术设施理事会;

关键词：

gamma rays: stars; pulsars: individual (PSR J2043+2740); LARGE-AREA TELESCOPE; FERMI-LAT OBSERVATIONS; CYGNUS LOOP; SUPERNOVA REMNANT; SPACE-TELESCOPE; VELOCITY VECTORS; PROPER-MOTION; LIGHT CURVES; VELA PULSAR; POLARIZATION;

D O I：

10.1088/0004-637X/728/2/77

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We report on the first year of Fermi gamma-ray observations of pulsed high-energy emission from the old PSR J2043 + 2740. The study of the gamma-ray efficiency of such old pulsars gives us an insight into the evolution of pulsars' ability to emit in gamma rays as they age. The gamma-ray light curve of this pulsar above 0.1 GeV is clearly defined by two sharp peaks, 0.353 +/- 0.035 periods apart. We have combined the gamma-ray profile characteristics of PSR J2043 + 2740 with the geometrical properties of the pulsar's radio emission, derived from radio-polarization data, and constrained the pulsar-beam geometry in the framework of a two-pole caustic (TPC) and an outer gap (OG) model. The ranges of magnetic inclination and viewing angle were determined to be {alpha, zeta} similar to {52 degrees-57 degrees, 61 degrees-68 degrees} for the TPC model, and {alpha, zeta} similar to {62 degrees-73 degrees, 74 degrees-81 degrees} and {alpha, zeta} similar to {72 degrees-83 degrees, 60 degrees-75 degrees} for the OG model. Based on this geometry, we assess possible birth locations for this pulsar and derive a likely proper motion, sufficiently high to be measurable with VLBI. At a characteristic age of 1.2 Myr, PSR J2043 + 2740 is the third oldest of all discovered, non-recycled, gamma-ray pulsars: it is twice as old as the next oldest, PSR J0357 + 32, and younger only than the recently discovered PSR J1836 + 5925 and PSR J2055 + 25, both of which are at least five and ten times less energetic, respectively.

引用

页数：12

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