HESS observations and VLT spectroscopy of PG 1553+113

被引：35

作者：

Aharonian, F. ^{[1
,14
]}

Akhperjanian, A. G. ^{[2
]}

de Almeida, U. Barres ^{[8
]}

Bazer-Bachi, A. R. ^{[3
]}

Behera, B. ^{[15
]}

Beilicke, M. ^{[4
]}

Benbow, W. ^{[1
]}

Bernloehr, K. ^{[1
,5
]}

Boisson, C. ^{[6
]}

Bolz, O. ^{[1
]}

Borrel, V. ^{[3
]}

Braun, I. ^{[1
]}

Brion, E. ^{[7
]}

Brown, A. M. ^{[8
]}

Buehler, R. ^{[1
]}

Bulik, T. ^{[25
]}

Buesching, I. ^{[9
]}

Boutelier, T. ^{[18
]}

Carrigan, S. ^{[1
]}

Chadwick, P. M. ^{[8
]}

Chounet, L. -M. ^{[10
]}

Clapson, A. C. ^{[1
]}

Coignet, G. ^{[11
]}

Cornils, R. ^{[4
]}

Costamante, L. ^{[1
]}

Dalton, M. ^{[5
]}

Degrange, B. ^{[10
]}

Dickinson, H. J. ^{[8
]}

Djannati-Atai, A. ^{[12
,13
]}

Domainko, W. ^{[1
]}

Drury, L. O'C. ^{[14
]}

Dubois, F. ^{[11
]}

Dubus, G. ^{[18
]}

Dyks, J. ^{[25
]}

Egberts, K. ^{[1
]}

Emmanoulopoulos, D. ^{[15
]}

Espigat, P. ^{[12
,13
]}

Farnier, C. ^{[16
]}

Feinstein, F. ^{[16
]}

Fiasson, A. ^{[16
]}

Foerster, A. ^{[1
]}

Fontaine, G. ^{[10
]}

Funk, Seb. ^{[5
]}

Fuessling, M. ^{[5
]}

Gallant, Y. A. ^{[16
]}

Giebels, B. ^{[10
]}

Glicenstein, J. F. ^{[7
]}

Glueck, B. ^{[17
]}

Goret, P. ^{[7
]}

Hadjichristidis, C. ^{[8
]}

机构：

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

[2] Yerevan Phys Inst, Yerevan 375036, Armenia

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

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

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

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

[7] CE Saclay, DAPNIA DSM CEA, F-91191 Gif Sur Yvette, France

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

[9] N W Univ, Unit Space Phys, ZA-2520 Potchefstroom, South Africa

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

[11] CNRS, IN2P3, Lab Annecy Le Vieux Phys Particules, F-74941 Annecy Le Vieux, France

[12] APC, UMR 7164, F-75231 Paris 5, France

[13] Univ Paris 07, CNRS, Observ Paris, CEA, F-75221 Paris 05, France

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

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

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

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

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

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

[20] Univ Paris 07, Univ Paris 06, CNRS, IN2P3,LPNHE, F-75252 Paris 5, France

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

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

[23] Univ Namibia, Windhoek, Namibia

[24] Uniwersytet Jagiellonski, Obserwatorium Astron, Krakow, Poland

[25] Nicolaus Copernicus Astron Ctr, Warsaw, Poland

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

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

来源：

ASTRONOMY & ASTROPHYSICS | 2008年 / 477卷 / 02期

基金：

英国科学技术设施理事会;

关键词：

galaxies : active; galaxies : BL Lacertae objects : individual : PG 1553+113; gamma rays : observations;

D O I：

10.1051/0004-6361:20078603

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Aims. The properties of the very high energy (VHE; E > 100 GeV) gamma-ray emission from the high-frequency peaked BL Lac PG 1553+113 are investigated. An attempt is made to measure the currently unknown redshift of this object. Methods. VHE Observations of PG 1553+113 were made with the High Energy Stereoscopic System (HESS) in 2005 and 2006. H + K (1.45 - 2.45 mu m) spectroscopy of PG 1553+113 was performed in March 2006 with SINFONI, an integral field spectrometer of the ESO Very Large Telescope (VLT) in Chile. Results. A VHE signal, similar to 10 standard deviations, is detected by HESS during the 2 years of observations (24.8 h live time). The integral flux above 300 GeV is (4.6 +/- 0.6(stat)+/- 0.9(syst)) x 10(-12) cm(-2) s(-1), corresponding to similar to 3.4% of the flux from the Crab Nebula above the same threshold. The time-averaged energy spectrum is measured from 225 GeV to similar to 1.3 TeV, and is characterized by a very soft power law (photon index of F=4.5 +/- 0.3(stat)+/- 0.1(syst)). No evidence for any flux or spectral variations is found on any sampled time scale within the VHE data. The redshift of PG 1553+113 could not be determined. Indeed, even though the measured SINFONI spectrum is the most sensitive ever reported for this object at near infrared wavelengths, and the sensitivity is comparable to the best spectroscopy at other wavelengths, no absorption or emission lines were found in the H+K spectrum presented here.

引用

页码：481 / 489

页数：9

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