Localizing the VHE γ-ray source at the Galactic Centre

被引：63

作者：

Acero, F. ^{[1
]}

Aharonian, F. ^{[2
,3
]}

Akhperjanian, A. G. ^{[4
]}

Anton, G. ^{[5
]}

de Almeida, U. Barres ^{[6
]}

Bazer-Bachi, A. R. ^{[7
]}

Becherini, Y. ^{[8
]}

Behera, B. ^{[9
]}

Bernloehr, K. ^{[2
,10
]}

Bochow, A. ^{[2
]}

Boisson, C. ^{[11
]}

Bolmont, J. ^{[12
]}

Borrel, V. ^{[7
]}

Braun, I. ^{[2
]}

Brucker, J. ^{[5
]}

Brun, F. ^{[12
]}

Brun, P. ^{[13
]}

Buehler, R. ^{[2
]}

Bulik, T. ^{[14
]}

Buesching, I. ^{[15
]}

Boutelier, T. ^{[16
]}

Chadwick, P. M. ^{[6
]}

Charbonnier, A. ^{[12
]}

Chaves, R. C. G. ^{[2
]}

Cheesebrough, A. ^{[6
]}

Conrad, J. ^{[17
]}

Chounet, L. -M. ^{[18
]}

Clapson, A. C. ^{[2
]}

Coignet, G. ^{[19
]}

Dalton, M. ^{[10
]}

Daniel, M. K. ^{[6
]}

Davids, I. D. ^{[15
,20
]}

Degrange, B. ^{[18
]}

Deil, C. ^{[2
]}

Dickinson, H. J. ^{[6
]}

Djannati-Atai, A. ^{[8
]}

Domainko, W. ^{[2
]}

Drury, L. O'C. ^{[3
]}

Dubois, F. ^{[19
]}

Dubus, G. ^{[16
]}

Dyks, J. ^{[21
]}

Dyrda, M. ^{[22
]}

Egberts, K. ^{[2
]}

Eger, P.

Espigat, P. ^{[8
]}

Fallon, L. ^{[3
]}

Farnier, C. ^{[1
]}

Fegan, S. ^{[18
]}

Feinstein, F. ^{[1
]}

Fiasson, A. ^{[19
]}

机构：

[1] Univ Montpellier 2, Lab Phys Theor & Astroparticules, CNRS, IN2P3, F-34095 Montpellier 5, France

[2] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany

[3] Dublin Inst Adv Studies, Dublin 2, Ireland

[4] Yerevan Phys Inst, Yerevan 375036, Armenia

[5] Univ Erlangen Nurnberg, Inst Phys, D-91058 Erlangen, Germany

[6] Univ Durham, Dept Phys, Durham DH1 3LE, England

[7] CNRS UPS, Ctr Etud Spatiale Rayonnements, F-31029 Toulouse 4, France

[8] Univ Paris 07, CNRS, APC, F-75205 Paris 13, France

[9] Univ Heidelberg, D-69117 Heidelberg, Germany

[10] Humboldt Univ, Inst Phys, D-12489 Berlin, Germany

[11] Univ Paris Diderot, CNRS, LUTH, Observ Paris, F-92190 Meudon, France

[12] Univ Paris 07, LPNHE, Univ Paris 06, F-75252 Paris 5, France

[13] CE Saclay, IRFU DSM CEA, F-91191 Gif Sur Yvette, France

[14] Univ Warsaw, Astron Observ, PL-00478 Warsaw, Poland

[15] North West Univ, Unit Space Phys, ZA-2520 Potchefstroom, South Africa

[16] Univ Grenoble 1, Lab Astrophys Grenoble, INSU CNRS, F-38041 Grenoble 9, France

[17] Stockholm Univ, Dept Phys, Oskar Klein Ctr, SE-10691 Stockholm, Sweden

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

[19] Univ Savoie, Lab Annecy le Vieux Phys Particulas, CNRS, IN2P3, F-74941 Annecy Le Vieux, France

[20] Univ Namibia, Dept Phys, Windhoek, Namibia

[21] Nicolaus Copernicus Astron Ctr, PL-00716 Warsaw, Poland

[22] Inst Fizyki Jaadrowej PAN, PL-31342 Krakow, Poland

[23] Ruhr Univ Bochum, Inst Theoret Phys, Lehrstuhl Weltraum & Astrophys 4, D-44780 Bochum, Germany

[24] Univ Hamburg, Inst Expt Phys, D-22761 Hamburg, Germany

[25] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England

[26] Univ Tubingen, Inst Astron & Astrophys, D-72076 Tubingen, Germany

[27] Nicholas Copernicus Univ, Torun Ctr Astron, PL-87100 Torun, Poland

[28] Charles Univ Prague, Fac Math & Phys, Inst Nucl & Particle Phys, CR-18000 Prague 8, Czech Republic

[29] Univ Adelaide, Sch Chem & Phys, Adelaide, SA 5005, Australia

[30] Uniwersytet Jagiellonski, Obserwatorium Astron, PL-30244 Krakow, Poland

[31] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria

[32] Royal Inst Technol KTH, Oskar Klein Ctr, Dept Phys, SE-10691 Stockholm, Sweden

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2010年 / 402卷 / 03期

基金：

英国科学技术设施理事会; 新加坡国家研究基金会;

关键词：

ISM: individual: Sgr A East; ISM: individual: Sgr A*; ISM: individual: G 359; 95-0; 04; Galaxy: centre; gamma-rays: observations; MASSIVE BLACK-HOLE; SAGITTARIUS A-ASTERISK; SUPERNOVA REMNANT; CENTER REGION; HESS; DIRECTION; EMISSION; ACCELERATION; ASTRONOMY; SPECTRUM;

D O I：

10.1111/j.1365-2966.2009.16014.x

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The inner 10 pc of our Galaxy contains many counterpart candidates of the very high energy (VHE; > 100 GeV) gamma-ray point source HESS J1745-290. Within the point spread function of the H.E.S.S. measurement, at least three objects are capable of accelerating particles to VHE and beyond and of providing the observed gamma-ray flux. Previous attempts to address this source confusion were hampered by the fact that the projected distances between these objects were of the order of the error circle radius of the emission centroid (34 arcsec, dominated by the pointing uncertainty of the H.E.S.S. instrument). Here we present H.E.S.S. data of the Galactic Centre region, recorded with an improved control of the instrument pointing compared to H.E.S.S. standard pointing procedures. Stars observed during gamma-ray observations by optical guiding cameras mounted on each H.E.S.S. telescope are used for off-line pointing calibration, thereby decreasing the systematic pointing uncertainties from 20 to 6 arcsec per axis. The position of HESS J1745-290 is obtained by fitting a multi-Gaussian profile to the background-subtracted gamma-ray count map. A spatial comparison of the best-fitting position of HESS J1745-290 with the position and morphology of candidate counterparts is performed. The position is, within a total error circle radius of 13 arcsec, coincident with the position of the supermassive black hole Sgr A* and the recently discovered pulsar wind nebula candidate G359.95-0.04. It is significantly displaced from the centroid of the supernova remnant Sgr A East, excluding this object with high probability as the dominant source of the VHE gamma-ray emission.

引用

页码：1877 / 1882

页数：6

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