HESS observations of the 2021 periastron passage of PSR B1259-63/LS 2883

被引:1
作者
Aharonian, F. [1 ,2 ,3 ]
Ait Benkhali, F. [4 ]
Aschersleben, J. [5 ]
Ashkar, H. [6 ]
Backes, M. [7 ,8 ]
Barbosa Martins, V. [9 ]
Batzofin, R. [10 ]
Becherini, Y. [11 ,12 ]
Berge, D. [9 ,13 ]
Bernloehr, K. [2 ]
Boettcher, M. [8 ]
Boisson, C. [14 ]
Bolmont, J. [15 ]
de Bony de Lavergne, M. [16 ]
Borowska, J. [13 ]
Bouyahiaoui, M. [2 ]
Brose, R. [1 ]
Brown, A. [17 ]
Brun, F. [16 ]
Bruno, B. [18 ]
Bulik, T. [19 ]
Burger-Scheidlin, C. [1 ]
Caroff, S. [20 ]
Casanova, S. [21 ]
Celic, J. [18 ]
Cerruti, M. [11 ]
Chand, T. [8 ]
Chandra, S. [8 ]
Chen, A. [22 ]
Chibueze, J. [8 ]
Chibueze, O. [8 ]
Cotter, G. [17 ]
Damascene Mbarubucyeye, J. [9 ]
Devin, J. [23 ]
Djuvsland, J. [2 ]
Dmytriiev, A. [8 ]
Egberts, K. [10 ]
Einecke, S. [24 ]
Ernenwein, J. -p. [25 ]
Fontaine, G. [6 ]
Funk, S. [18 ]
Gabici, S. [11 ]
Gallant, Y. A. [23 ]
Glawion, D. [18 ]
Glicenstein, J. F. [16 ]
Goswami, P. [11 ]
Grolleron, G. [15 ]
Haerer, L. [2 ]
Hess, B. [26 ]
Hofmann, W. [2 ]
机构
[1] Dublin Inst Adv Studies, 31 Fitzwilliam Pl, Dublin 2, Ireland
[2] Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany
[3] Yerevan State Univ, 1 Alek Manukyan St, Yerevan 0025, Armenia
[4] Heidelberg Univ, Landessternwarte, Konigstuhl, D-69117 Heidelberg, Germany
[5] Univ Groningen, Kapteyn Astron Inst, Landleven 12, NL-9747 AD Groningen, Netherlands
[6] Ecole Polytech, Inst Polytech Paris, Lab Leprince Ringuet, CNRS, F-91128 Palaiseau, France
[7] Univ Namibia, Dept Phys, Private Bag 13301, Windhoek 10005, Namibia
[8] North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa
[9] Deutsch Elektronen Synchrotron DESY, Platanenallee 6, D-15738 Zeuthen, Germany
[10] Univ Potsdam, Inst Phys & Astron, Karl Liebknecht Str 24-25, D-14476 Potsdam, Germany
[11] Univ Paris, CNRS, Astroparticule & Cosmol, F-75013 Paris, France
[12] Linnaeus Univ, Dept Phys & Elect Engn, S-35195 Vaxjo, Sweden
[13] Univ Berlin, Inst Phys Humboldt, Newtonstr 15, D-12489 Berlin, Germany
[14] Univ Paris Cite, Univ PSL, Lab Univers & Theories, Observ Paris,CNRS, 5 Pl Jules Janssen, F-92190 Meudon, France
[15] Sorbonne Univ, LPNHE, Lab Phys Nucl & Hautes Energies, CNRS,IN2P3, 4 Pl Jussieu, F-75005 Paris, France
[16] Univ Paris Saclay, IRFU, CEA, F-91191 Gif Sur Yvette, France
[17] Univ Oxford, Dept Phys, Denys Wilkinson Bldg,Keble Rd, Oxford OX1 3RH, England
[18] Friedrich Alexander Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, Nikolaus Fiebiger Str 2, D-91058 Erlangen, Germany
[19] Univ Warsaw, Astron Observ, Al Ujazdowskie 4, PL-00478 Warsaw, Poland
[20] Univ Savoie Mont Blanc, CNRS, Lab Annecy Phys Particules IN2P3, F-74000 Annecy, France
[21] Inst Fizyki Jadrowej PAN, Ul Radzikowskiego 152, PL-31342 Krakow, Poland
[22] Univ Witwatersrand, Sch Phys, 1 Jan Smuts Ave, ZA-2050 Braamfontein, South Africa
[23] Univ Montpellier, IN2P3, CNRS, Lab Univers & Particules Montpellier,CC 72, Pl Eugene Bataillon, F-34095 Montpellier 5, France
[24] Univ Adelaide, Sch Phys Sci, Adelaide, SA 5005, Australia
[25] Aix Marseille Univ, CNRS, IN2P3, CPPM, Marseille, France
[26] Univ Tubingen, Inst Astron & Astrophys, Sand 1, D-72076 Tubingen, Germany
[27] Univ Innsbruck, Inst Experimentalphys, Technikerstr 25, A-6020 Innsbruck, Austria
[28] Uniwersytet Jagiellonski, Obserwatorium Astron, Ul Orla 171, PL-31501 Krakow, Poland
[29] Nicolaus Copernicus Univ, Inst Astron, Fac Phys Astron & Informat, Grudziadzka 5, PL-87100 Torun, Poland
[30] Rikkyo Univ, Dept Phys, 3-34-1 Nishi Ikebukuro,Toshima Ku, Tokyo 1718501, Japan
[31] Polish Acad Sci, Nicolaus Copernicus Astron Ctr, Ul Bartycka 18, PL-00176 Warsaw, Poland
[32] Univ Bordeaux, CNRS, LP2I Bordeaux, UMR 5797, F-33170 Gradignan, France
[33] Univ Free State, Dept Phys, POB 339, ZA-9300 Bloemfontein, South Africa
[34] Univ Amsterdam, Anton Pannekoek Inst Astron, GRAPPA, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands
[35] Univ Tokyo, Univ Tokyo Inst Adv Study UTIAS, Kavli Inst Phys & Math Universe WPI, 5-1-5 Kashiwa-No-Ha, Kashiwa, Chiba 2778583, Japan
[36] Konan Univ, Dept Phys, 8-9-1 Okamoto,Higashinada, Kobe, Hyogo 6588501, Japan
[37] Univ Hamburg, Inst Experimentalphys, Luruper Chaussee 149, D-22761 Hamburg, Germany
基金
新加坡国家研究基金会; 奥地利科学基金会; 爱尔兰科学基金会; 日本学术振兴会; 英国科学技术设施理事会; 澳大利亚研究理事会;
关键词
radiation mechanisms: non-thermal; binaries: general; pulsars: individual: PSR B1259-63/LS 2883; GAMMA-RAY BINARIES; HIGH-ENERGY EMISSION; X-RAY; MULTIWAVELENGTH OBSERVATIONS; NONRELATIVISTIC WINDS; RADIO OBSERVATIONS; SYSTEM; PULSAR; DISCOVERY; RADIATION;
D O I
10.1051/0004-6361/202449612
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
PSR B1259-63/LS 2883 is a gamma-ray binary system that hosts a pulsar in an eccentric orbit, with a 3.4 yr period, around an O9.5Ve star (LS 2883). At orbital phases close to periastron passages, the system radiates bright and variable non-thermal emission, for which the temporal and spectral properties of this emission are, for now, poorly understood. In this regard, very high-energy (VHE) emission is especially useful to study and constrain radiation processes and particle acceleration in the system. We report on an extensive VHE observation campaign conducted with the High Energy Stereoscopic System, comprised of approximately 100 h of data taken over five months, from t(p) - 24 days to t(p) + 127 days around the system's 2021 periastron passage (where t(p) is the time of periastron). We also present the timing and spectral analyses of the source. The VHE light curve in 2021 is consistent overall with the stacked light curve of all previous observations. Within the light curve, we report a VHE maximum at times coincident with the third X-ray peak first detected in the 2021 X-ray light curve. In the light curve - although sparsely sampled in this time period - we see no VHE enhancement during the second disc crossing. In addition, we see no correspondence to the 2021 GeV flare in the VHE light curve. The VHE spectrum obtained from the analysis of the 2021 dataset is best described by a power law of spectral index Gamma = 2.65 +/- 0.04(stat) +/- 0.04(sys), a value consistent with the spectral index obtained from the analysis of data collected with H.E.S.S. during the previous observations of the source. We report spectral variability with a difference of Delta Gamma = 0.56 +/- 0.18(stat) +/- 0.10(sys) at 95% confidence intervals, between sub-periods of the 2021 dataset. We also detail our investigation into X-ray/TeV and GeV/TeV flux correlations in the 2021 periastron passage. We find a linear correlation between contemporaneous flux values of X-ray and TeV datasets, detected mainly after t(p) + 25 days, suggesting a change in the available energy for non-thermal radiation processes. We detect no significant correlation between GeV and TeV flux points, within the uncertainties of the measurements, from similar to t(p) - 23 days to similar to t(p) + 126 days. This suggests that the GeV and TeV emission originate from different electron populations.
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页数:14
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