H 2356-309 的多波段观测
摘要
目的：研究高频峰 BL Lac 天体 H 2356-309 (z=0.165) 宽带辐射的性质。方法：2004年至2007年间，利用高能立体视野系统（HESS）对 H 2356-309 进行了甚高能（VHE；E > 100 GeV）观测。2005年6月12/13日和6月14/15日，利用 XMM-Newton 卫星进行了同步光学/紫外和 X 射线观测。2005年还同期进行了 NRT 射电观测。2007年也进行了 ATOM 光学监测观测。结果：经过四年的 HESS 观测（116.8 小时有效时间），HESS 探测到了强烈的 VHE 信号，总计约 13 sigma。240 GeV 以上的积分通量为 I(>240 GeV) = (3.06 +- 0.26 {stat} +- 0.61 {syst}) x 10^{-12} cm^{-2} s^{-1}，相当于观测到的蟹状星云通量的约 1.6%。从 200 GeV 到 2 TeV 测量了时间平均能谱，其特征为幂律谱（光子指数为 Gamma = 3.06 +- 0.15 {stat} +- 0.10 {syst}）。在数月和数年的时间尺度上看到了 H 2356-309 的 VHE 通量存在显著的小幅度变化，但在更短的时间尺度上没有发现。在这些数据中没有发现 VHE 谱斜率存在任何变化的证据。XMM-Newton X 射线测量显示其处于历史低 X 射线态，特征为两个夜晚均呈现硬的折断幂律谱。结论：该耀变体的宽带谱能量分布（SED）可以使用简单的单区同步自康普顿（SSC）模型很好地拟合。在 SSC 情景下，未来可能会预期出现更高的 VHE 通量，因为观测到的 X 射线通量处于历史低水平。
引用
@article{arxiv.1004.2089,
title = {Multi-wavelength Observations of H 2356-309},
author = {HESS Collaboration and A. Abramowski and F. Acero and F. Aharonian and A. G. Akhperjanian and G. Anton and U. Barres de Almeida and A. R. Bazer-Bachi and Y. Becherini and B. Behera and W. Benbow and K. Bernloehr and A. Bochow and C. Boisson and J. Bolmont and V. Borrel and J. Brucker and F. Brun and P. Brun and R. Buehler and T. Bulik and I. Buesching and T. Boutelier and P. M. Chadwick and A. Charbonnier and R. C. G. Chaves and A. Cheesebrough and J. Conrad and L. -M. Chounet and A. C. Clapson and G. Coignet and L. Costamante and M. Dalton and M. K. Daniel and I. D. Davids and B. Degrange and C. Deil and H. J. Dickinson and A. Djannati-Atai and W. Domainko and L. O'C. Drury and F. Dubois and G. Dubus and J. Dyks and M. Dyrda and K. Egberts and P. Eger and P. Espigat and L. Fallon and C. Farnier and S. Fegan and F. Feinstein and M. V. Fernandes and A. Fiasson and A. Foerster and G. Fontaine and M. Fuessling and S. Gabici and Y. A. Gallant and L. Gerard and D. Gerbig and B. Giebels and J. F. Glicenstein and B. Glueck and P. Goret and D. Goering and D. Hampf and M. Hauser and S. Heinz and G. Heinzelmann and G. Henri and G. Hermann and J. A. Hinton and A. Hoffmann and W. Hofmann and P. Hofverberg and M. Holleran and S. Hoppe and D. Horns and A. Jacholkowska and O. C. de Jager and C. Jahn and I. Jung and K. Katarzynski and U. Katz and S. Kaufmann and M. Kerschhaggl and D. Khangulyan and B. Khelifi and D. Keogh and D. Klochkov and W. Kluzniak and T. Kneiske and Nu. Komin and K. Kosack and R. Kossakowski and G. Lamanna and J. -P. Lenain and T. Lohse and C. -C. Lu and V. Marandon and A. Marcowith and J. Masbou and D. Maurin and T. J. L. McComb and M. C. Medina and J. Mehault and R. Moderski and E. Moulin and M. Naumann-Godo and M. de Naurois and D. Nedbal and D. Nekrassov and N. Nguyen and B. Nicholas and J. Niemiec and S. J. Nolan and S. Ohm and J-F. Olive and E. de Ona Wilhelmi and B. Opitz and K. J. Orford and M. Ostrowski and M. Panter and M. Paz Arribas and G. Pedaletti and G. Pelletier and P. -O. Petrucci and S. Pita and G. Puehlhofer and M. Punch and A. Quirrenbach and B. C. Raubenheimer and M. Raue and S. M. Rayner and O. Reimer and M. Renaud and R. de los Reyes and F. Rieger and J. Ripken and L. Rob and S. Rosier-Lees and G. Rowell and B. Rudak and C. B. Rulten and J. Ruppel and F. Ryde and V. Sahakian and A. Santangelo and R. Schlickeiser and F. M. Schoeck and A. Schoenwald and U. Schwanke and S. Schwarzburg and S. Schwemmer and A. Shalchi and I. Sushch and M. Sikora and J. L. Skilton and H. Sol and L. Stawarz and R. Steenkamp and C. Stegmann and F. Stinzing and A. Szostek and P. H. Tam and J. -P. Tavernet and R. Terrier and O. Tibolla and M. Tluczykont and K. Valerius and C. van Eldik and G. Vasileiadis and C. Venter and L. Venter and J. P. Vialle and A. Viana and P. Vincent and M. Vivier and H. J. Voelk and F. Volpe and S. Vorobiov and S. J. Wagner and M. Ward and A. A. Zdziarski and A. Zech and H. -S. Zechlin},
journal= {arXiv preprint arXiv:1004.2089},
year = {2015}
}
备注
11 pages; 13 figures; Accepted for publication in Astronomy & Astrophysics; Figure 8 (SED) updated from V1 to have erroneously plotted optical point (without host galaxy subtracted) removed.