TeV Emission of Galactic Plane Sources with HAWC and HESS

被引：18

作者：

Abdalla, H. ^{[1
]}

Aharonian, F. ^{[2
,3
,4
]}

Benkhali, F. Ait ^{[3
]}

Anguner, E. O. ^{[5
]}

Arcaro, C. ^{[6
]}

Armand, C. ^{[7
]}

Armstrong, T. ^{[8
]}

Ashkar, H. ^{[9
]}

Backes, M. ^{[1
,6
]}

Baghmanyan, V ^{[10
,52
]}

Martins, V. Barbosa ^{[11
]}

Barnacka, A. ^{[12
]}

Barnard, M. ^{[6
]}

Becherini, Y. ^{[13
]}

Berge, D. ^{[11
]}

Bernlohr, K. ^{[3
]}

Bi, B. ^{[14
]}

Bottcher, M. ^{[6
]}

Boisson, C. ^{[15
]}

Bolmont, J. ^{[16
]}

Lavergne, M. de Bonyde ^{[7
]}

Breuhaus, M. ^{[3
]}

Brose, R. ^{[2
]}

Brun, F. ^{[9
,70
,71
]}

Brun, P. ^{[9
]}

Bryan, M. ^{[17
]}

Buechele, M. ^{[18
]}

Bulik, T. ^{[19
]}

Bylund, T. ^{[13
]}

Caroff, S. ^{[7
]}

Carosi, A. ^{[7
]}

Chand, T. ^{[6
]}

Chandra, S. ^{[6
]}

Chen, A. ^{[20
]}

Cotter, G. ^{[8
]}

Mbarubucyeye, J. Damascene ^{[11
]}

Davids, I. D. ^{[1
]}

Davies, J. ^{[8
]}

Deil, C. ^{[3
]}

Devin, J. ^{[21
]}

Dirson, L. ^{[22
]}

Djannati-Atai, A. ^{[21
]}

Dmytriiev, A. ^{[15
]}

Donath, A. ^{[3
]}

Doroshenko, V ^{[14
]}

Dreyer, L. ^{[6
]}

Duffy, C. ^{[23
]}

Dyks, J. ^{[24
]}

Egberts, K. ^{[25
]}

Eichhorn, F. ^{[18
]}

机构：

[1] Univ Namibia, Dept Phys, Private Bag 13301, Windhoek 10005, Namibia

[2] Dublin Inst Adv Studies, 31 Fitzwilliam Pl, Dublin 2, Ireland

[3] Max Planck Inst Nucl Phys, D-69117 Heidelberg, Germany

[4] RAU, High Energy Astrophys Lab, 123 Hovsep Emin St, Yerevan 0051, Armenia

[5] Aix Marseille Univ, CPPM, CNRS IN2P3, Marseille, France

[6] North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa

[7] Univ Savoie Mt Blanc, LAPP, CNRS, Lab Annecy Phys Particules,Univ Grenoble Alpes, F-74000 Annecy, France

[8] Univ Oxford, Dept Phys, Denys Wilkinson Bldg,Keble Rd, Oxford OX1 3RH, England

[9] Univ Paris Saclay, IRFU, CEA, F-91191 Gif Sur Yvette, France

[10] Inst Fizyki Jadrowej PAN, Ul Radzikowskiego 152, PL-31342 Krakow, Poland

[11] DESY, D-15738 Zeuthen, Germany

[12] Uniwersytet Jagiellonski, Obserwatorium Astron, Ul Orla 171, PL-30244 Krakow, Poland

[13] Linnaeus Univ, Dept Phys & Elect Engn, S-35195 Vaxjo, Sweden

[14] Univ Tubingen, Inst Astron & Astrophys, Sand 1, D-72076 Tubingen, Germany

[15] Univ Paris, Lab Univers & Theories, Observ Paris, CNRS,Univ PSL, F-92190 Meudon, France

[16] Sorbonne Univ, Univ Paris Diderot, Sorbonne Paris Cite, CNRS IN2P3,Lab Phys Nucl & Hautes Energies,LPNHE, 4 Pl Jussieu, F-75252 Paris, France

[17] Univ Amsterdam, Anton Pannekoek Inst Astron, GRAPPA, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands

[18] Friedrich Alexander Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, Erwin Rommel Str 1, D-91058 Erlangen, Germany

[19] Univ Warsaw, Astron Observ, Al Ujazdowskie 4, PL-00478 Warsaw, Poland

[20] Univ Witwatersrand, Sch Phys, 1 Jan Smuts Ave, ZA-2050 Johannesburg 2050, South Africa

[21] Univ Paris, CNRS, Astroparticule & Cosmol, F-75013 Paris, France

[22] Univ Hamburg, Inst Expt Phys, Luruper Chaussee 149, D-22761 Hamburg, Germany

[23] Univ Leicester, Dept Phys & Astron, Univ Rd, Leicester LE1 7RH, Leics, England

[24] Polish Acad Sci, Nicolaus Copernicus Astron Ctr, Ul Bartycka 18, PL-00716 Warsaw, Poland

[25] Univ Potsdam, Inst Phys & Astron, Karl Liebknecht Str 24-25, D-14476 Potsdam, Germany

[26] Univ Adelaide, Sch Phys Sci, Adelaide, SA 5005, Australia

[27] Ecole Polytech, Lab Leprince Ringuet, CNRS, Inst Polytech Paris, F-91128 Palaiseau, France

[28] Univ Montpellier, Lab Univers & Particules Montpellier, CNRS IN2P3, CC 72,Pl Eugene Bataillon, F-34095 Montpellier 5, France

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

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

[31] Heidelberg Univ, Landessternwarte, D-69117 Heidelberg, Germany

[32] Nicolaus Copernicus Univ, Fac Phys Astron & Informat, Inst Astron, Grudziadzka 5, PL-87100 Torun, Poland

[33] Rikkyo Univ, Dept Phys, Toshima Ku, 3-34-1 Nishi Ikebukuro, Tokyo 1718501, Japan

[34] Humboldt Univ, Inst Phys, Newtonstr 15, D-12489 Berlin, Germany

[35] Univ Free State, Dept Phys, POB 339, ZA-9300 Bloemfontein, South Africa

[36] Univ Tokyo, Dept Phys, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan

[37] Yerevan Phys Inst, 2 Alikhanian Bros St, Yerevan 375036, Armenia

[38] Univ Tokyo, Univ Tokyo Inst Adv Study UTIAS, Kavli Inst Phys & Math Universe WPI, 5-1-5 Kashiwa No Ha, Kashiwa, Chiba 2778583, Japan

[39] Los Alamos Natl Lab, Phys Div, Los Alamos, NM USA

[40] Univ Nacl Autonoma Mexico, Inst Fis, Ciudad De Mexico, Mexico

[41] Univ Autonoma Chiapas, Tuxtla Gutierrez, Chiapas, Mexico

[42] Univ Michoacana, Morelia, Michoacan, Mexico

[43] Univ Nacl Autonoma Mexico, Inst Geofis, Ciudad De Mexico, Mexico

[44] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA

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

[46] Univ Nacl Autonoma Mexico, Inst Astron, Ciudad De Mexico, Mexico

[47] Inst Nacl Astrofis Opt & Electr, Puebla, Mexico

[48] Polish Acad Sci, Inst Nucl Phys, IFJ PAN, PL-31342 Krakow, Poland

[49] Benemarita Univ Autanoma Puebla, Fac Ciencias Fis Matemat, Puebla, Mexico

[50] Univ Guadalajara, Ctr Univ Ciencias Exactase Ingn, Dept Fis, Guadalajara, Jalisco, Mexico

来源：

ASTROPHYSICAL JOURNAL | 2021年 / 917卷 / 01期

基金：

美国国家科学基金会; 日本学术振兴会; 奥地利科学基金会; 英国科学技术设施理事会; 澳大利亚研究理事会; 新加坡国家研究基金会;

关键词：

GAMMA-RAY SOURCES; CRAB-NEBULA; MILKY-WAY; PULSAR; CATALOG;

D O I：

10.3847/1538-4357/abf64b

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The High Altitude Water Cherenkov (HAWC) observatory and the High Energy Stereoscopic System (H.E.S.S.) are two leading instruments in the ground-based very-high-energy gamma-ray domain. HAWC employs the water Cherenkov detection (WCD) technique, while H.E.S.S. is an array of Imaging Atmospheric Cherenkov Telescopes (IACTs). The two facilities therefore differ in multiple aspects, including their observation strategy, the size of their field of view, and their angular resolution, leading to different analysis approaches. Until now, it has been unclear if the results of observations by both types of instruments are consistent: several of the recently discovered HAWC sources have been followed up by IACTs, resulting in a confirmed detection only in a minority of cases. With this paper, we go further and try to resolve the tensions between previous results by performing a new analysis of the H.E.S.S. Galactic plane survey data, applying an analysis technique comparable between H.E.S.S. and HAWC. Events above 1 TeV are selected for both data sets, the point-spread function of H.E.S.S. is broadened to approach that of HAWC, and a similar background estimation method is used. This is the first detailed comparison of the Galactic plane observed by both instruments. H.E.S.S. can confirm the gamma-ray emission of four HAWC sources among seven previously undetected by IACTs, while the three others have measured fluxes below the sensitivity of the H.E.S.S. data set. Remaining differences in the overall gamma-ray flux can be explained by the systematic uncertainties. Therefore, we confirm a consistent view of the gamma-ray sky between WCD and IACT techniques.

引用

页数：16

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