Discovery of variable VHE γ-ray emission from the binary system 1FGL J1018.6–5856
Discovery of variable VHE γ-ray emission from the binary system 1FGL J1018.6–5856
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发表时间：
2015
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通讯作者：
H. C. A. Abramowski;F. Aharonian;F. Benkhali;A. Akhperjanian;E. Anguner;M. Backes;A. Balzer;Y. Becherini;J. Tjus;D. Berge;S. Bernhard;K. Bernlohr;E. Birsin;R. Blackwell;M. Bottcher;C. Boisson;J. Bolmont;P. Bordas;J. Bregeon;F. Brun;P. Brun;M. Bryan;T. Bulik;J. Carr;S. Casanova;N. Chakraborty;R. Chalme-Calvet;R. Chaves;A. Chen;M. Chr'etien;S. Colafrancesco;G. Cologna;J. Conrad;Camille Couturier;Y. Cui;I. Davids;B. Degrange;C. Deil;P. deWilt;A. Djannati-Atai;W. Domainko;A. Donath;L. Drury;G. Dubus;K. Dutson;J. Dyks;M. Dyrda;T. Edwards;K. Egberts;P. Eger;J. Ernenwein;P. Espigat;C. Farnier;S. Fegan;F. Feinstein;M. V. Fernandes;D. Fernandez;A. Fiasson;G. Fontaine;A. Forster;M. Fussling;S. Gabici;M. Gajdus;Y. Gallant;T. Garrigoux;G. Giavitto;B. Giebels;J. Glicenstein;D. Gottschall;A. Goyal;M. Grondin;M. Grudzi'nska;D. Hadasch;S. Haffner;J. Hahn;J. Hawkes;G. Heinzelmann;G. Henri;G. Hermann;O. Hervet;A. Hillert;J. Hinton;W. Hofmann;P. Hofverberg;C. Hoischen;M. Holler;D. Horns;A. Ivascenko;A. Jacholkowska;C. Jahn;M. Jamrozy;M. Janiak;F. Jankowsky;I. Jung-Richardt;M. Kastendieck;K. Katarzy'nski;U. Katz;D. Kerszberg;B. Kh'elifi;M. Kieffer;S. Klepser;D. Klochkov;W. Klu'zniak;D. Kolitzus;N. Komin;K. Kosack;S. Krakau;F. Krayzel;P. Kruger;H. Laffon;G. Lamanna;J. Lau;J. Lefaucheur;V. Lefranc;A. Lemière;M. Lemoine-Goumard;J. Lenain;T. Lohse;A. Lopatin;C.-C. Lu-C.;R. Lui;V. Marandon;A. Marcowith;C. Mariaud;R. Marx;G. Maurin;N. Maxted;M. Mayer;P. Meintjes;U. Menzler;M. Meyer;A. Mitchell;R. Moderski;M. Mohamed;K. Moraa;E. Moulin;T. Murach;M. Naurois;J. Niemiec;L. Oakes;H. Odaka;S. Ottl;S. Ohm;E. Wilhelmi;B. Opitz;M. Ostrowski;I. Oya;M. Panter;R. Parsons;M. Arribas;N. Pekeur;G. Pelletier;P. Petrucci;B. Peyaud;S. Pita;H. Poon;H. Prokoph;G. Puhlhofer;M. Punch;A. Quirrenbach;S. Raab;I. Reichardt;A. Reimer;O. Reimer;M. Renaud;R. Reyes;F. Rieger;C. Romoli;S. Rosier-Lees;G. Rowell;B. Rudak;C. Rulten;V. Sahakian;D. Šálek;D. Sanchez;A. Santangelo;M. Sasaki;R. Schlickeiser;F. Schussler;A. Schulz;U. Schwanke;S. Schwemmer;A. Seyffert;R. Simoni;H. Sol;F. Spanier;G. Spengler;F. Spies;L. Stawarz;R. Steenkamp;C. Stegmann;F. Stinzing;K. Stycz;I. Sushch;J. Tavernet;T. Tavernier;A. Taylor;R. Terrier;M. Tluczykont;C. Trichard;K. Valerius;J. V. D. Walt;C. Eldik;B. V. Soelen;G. Vasileiadis;J. Veh;C. Venter;A. Viana;P. Vincent;J. Vink;F. Voisin;H. Volk;T. Vuillaume;S. Wagner;P. Wagner;R. Wagner;M. Weidinger;Q. Weitzel;R. White;A. Wierzcholska;P. Willmann;A. Wornlein;D. Wouters;R. Yang;V. Zabalza;D. Zaborov;M. Zacharias;A. Zdziarski;A. Zech;F. Zefi;N. Żywucka
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作者：
H. C. A. Abramowski;F. Aharonian;F. Benkhali;A. Akhperjanian;E. Anguner;M. Backes;A. Balzer;Y. Becherini;J. Tjus;D. Berge;S. Bernhard;K. Bernlohr;E. Birsin;R. Blackwell;M. Bottcher;C. Boisson;J. Bolmont;P. Bordas;J. Bregeon;F. Brun;P. Brun;M. Bryan;T. Bulik;J. Carr;S. Casanova;N. Chakraborty;R. Chalme-Calvet;R. Chaves;A. Chen;M. Chr'etien;S. Colafrancesco;G. Cologna;J. Conrad;Camille Couturier;Y. Cui;I. Davids;B. Degrange;C. Deil;P. deWilt;A. Djannati-Atai;W. Domainko;A. Donath;L. Drury;G. Dubus;K. Dutson;J. Dyks;M. Dyrda;T. Edwards;K. Egberts;P. Eger;J. Ernenwein;P. Espigat;C. Farnier;S. Fegan;F. Feinstein;M. V. Fernandes;D. Fernandez;A. Fiasson;G. Fontaine;A. Forster;M. Fussling;S. Gabici;M. Gajdus;Y. Gallant;T. Garrigoux;G. Giavitto;B. Giebels;J. Glicenstein;D. Gottschall;A. Goyal;M. Grondin;M. Grudzi'nska;D. Hadasch;S. Haffner;J. Hahn;J. Hawkes;G. Heinzelmann;G. Henri;G. Hermann;O. Hervet;A. Hillert;J. Hinton;W. Hofmann;P. Hofverberg;C. Hoischen;M. Holler;D. Horns;A. Ivascenko;A. Jacholkowska;C. Jahn;M. Jamrozy;M. Janiak;F. Jankowsky;I. Jung-Richardt;M. Kastendieck;K. Katarzy'nski;U. Katz;D. Kerszberg;B. Kh'elifi;M. Kieffer;S. Klepser;D. Klochkov;W. Klu'zniak;D. Kolitzus;N. Komin;K. Kosack;S. Krakau;F. Krayzel;P. Kruger;H. Laffon;G. Lamanna;J. Lau;J. Lefaucheur;V. Lefranc;A. Lemière;M. Lemoine-Goumard;J. Lenain;T. Lohse;A. Lopatin;C.-C. Lu-C.;R. Lui;V. Marandon;A. Marcowith;C. Mariaud;R. Marx;G. Maurin;N. Maxted;M. Mayer;P. Meintjes;U. Menzler;M. Meyer;A. Mitchell;R. Moderski;M. Mohamed;K. Moraa;E. Moulin;T. Murach;M. Naurois;J. Niemiec;L. Oakes;H. Odaka;S. Ottl;S. Ohm;E. Wilhelmi;B. Opitz;M. Ostrowski;I. Oya;M. Panter;R. Parsons;M. Arribas;N. Pekeur;G. Pelletier;P. Petrucci;B. Peyaud;S. Pita;H. Poon;H. Prokoph;G. Puhlhofer;M. Punch;A. Quirrenbach;S. Raab;I. Reichardt;A. Reimer;O. Reimer;M. Renaud;R. Reyes;F. Rieger;C. Romoli;S. Rosier-Lees;G. Rowell;B. Rudak;C. Rulten;V. Sahakian;D. Šálek;D. Sanchez;A. Santangelo;M. Sasaki;R. Schlickeiser;F. Schussler;A. Schulz;U. Schwanke;S. Schwemmer;A. Seyffert;R. Simoni;H. Sol;F. Spanier;G. Spengler;F. Spies;L. Stawarz;R. Steenkamp;C. Stegmann;F. Stinzing;K. Stycz;I. Sushch;J. Tavernet;T. Tavernier;A. Taylor;R. Terrier;M. Tluczykont;C. Trichard;K. Valerius;J. V. D. Walt;C. Eldik;B. V. Soelen;G. Vasileiadis;J. Veh;C. Venter;A. Viana;P. Vincent;J. Vink;F. Voisin;H. Volk;T. Vuillaume;S. Wagner;P. Wagner;R. Wagner;M. Weidinger;Q. Weitzel;R. White;A. Wierzcholska;P. Willmann;A. Wornlein;D. Wouters;R. Yang;V. Zabalza;D. Zaborov;M. Zacharias;A. Zdziarski;A. Zech;F. Zefi;N. Żywucka
用HESS望远镜阵列对与费米γ射线双星1FGL J1018.6-5856重合的甚高能（VHE）源HESS J1018-589 A进行重新观测，发现源探测显著性大于9σ，并探测到发射γ射线通量的变化（χ2/ν为238.3/155）。这种变化证实了HESS J1018-589 A与费米LAT探测到的高能γ射线双星的关联，也证实了点状源是一个新的VHE双星系统。HESS J1018-589 A的光谱与光子指数为2.20 ± 0.14stat ± 0.2sys的幂律函数拟合最好。探测到的辐射能量高达120 TeV。在1 TeV的能量下，平均微分通量水平为（2.9 ± 0.4）× 10−13 TeV−1 cm−2 s−1，相当于蟹状星云在相同能量下通量的101%。在逐夜光变曲线中清楚地检测到可变性。当折叠在16.58天的轨道周期上时，重组的光变曲线峰值与观测到的X射线和高能相位图同相。HESS相图与恒定通量的拟合提供了在Nσ > 3σ水平上的周期性的证据。VHE相位图的形状和测量的光谱表明，一个低倾角，低偏心率的系统，具有适度的影响，从VHE γ射线吸收由于对生产（τ）。1在300 GeV）。
Re-observations with the HESS telescope array of the very high-energy (VHE) source HESS J1018–589 A that is coincident with the FermiLAT γ-ray binary 1FGL J1018.6–5856 have resulted in a source detection significance of more than 9σ and the detection of variability (χ2/ν of 238.3/155) in the emitted γ-ray flux. This variability confirms the association of HESS J1018–589 A with the high-energy γ-ray binary detected by Fermi-LAT and also confirms the point-like source as a new VHE binary system. The spectrum of HESS J1018–589 A is best fit with a power-law function with photon index Γ = 2.20 ± 0.14stat ± 0.2sys. Emission is detected up to ∼20 TeV. The mean differential flux level is (2.9 ± 0.4) × 10−13 TeV−1 cm−2 s−1 at 1 TeV, equivalent to ∼1% of the flux from the Crab Nebula at the same energy. Variability is clearly detected in the night-by-night light curve. When folded on the orbital period of 16.58 days, the rebinned light curve peaks in phase with the observed X-ray and high-energy phaseograms. The fit of the HESS phaseogram to a constant flux provides evidence of periodicity at the level of Nσ > 3σ. The shape of the VHE phaseogram and measured spectrum suggest a low-inclination, low-eccentricity system with a modest impact from VHE γ-ray absorption due to pair production (τ . 1 at 300 GeV).