A THREE-YEAR MULTI-WAVELENGTH STUDY OF THE VERY-HIGH-ENERGY γ-RAY BLAZAR 1ES 0229+200

被引:65
作者
Aliu, E. [1 ]
Archambault, S. [2 ]
Arlen, T. [3 ]
Aune, T. [3 ]
Behera, B. [4 ]
Beilicke, M. [5 ]
Benbow, W. [6 ]
Berger, K. [7 ,8 ]
Bird, R. [9 ]
Bouvier, A. [10 ,11 ]
Buckley, J. H. [5 ]
Bugaev, V. [5 ]
Byrum, K. [12 ]
Cerruti, M. [6 ]
Chen, X. [4 ,13 ]
Ciupik, L. [14 ]
Connolly, M. P. [15 ]
Cui, W. [16 ]
Duke, C. [17 ]
Dumm, J. [18 ]
Errando, M. [1 ]
Falcone, A. [19 ]
Federici, S. [4 ,13 ]
Feng, Q. [16 ]
Finley, J. P. [16 ]
Fleischhack, H. [4 ]
Fortin, P. [6 ]
Fortson, L. [18 ]
Furniss, A. [10 ,11 ]
Galante, N. [6 ]
Gillanders, G. H. [15 ]
Griffin, S. [2 ]
Griffiths, S. T. [20 ]
Grube, J. [14 ]
Gyuk, G. [14 ]
Hanna, D. [2 ]
Holder, J. [7 ,8 ]
Hughes, G. [4 ]
Humensky, T. B. [21 ]
Johnson, C. A. [10 ,11 ]
Kaaret, P. [20 ]
Kertzman, M. [22 ]
Khassen, Y. [9 ]
Kieda, D. [23 ]
Krawczynski, H. [5 ]
Krennrich, F. [24 ]
Lang, M. J. [15 ]
Madhavan, A. S. [24 ]
Maier, G. [4 ]
Majumdar, P. [3 ,25 ]
机构
[1] Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA
[2] McGill Univ, Dept Phys, Montreal, PQ, Canada
[3] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA
[4] DESY, D-15738 Zeuthen, Germany
[5] Washington Univ, Dept Phys, St Louis, MO 63130 USA
[6] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA
[7] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA
[8] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA
[9] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland
[10] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA
[11] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA
[12] Argonne Natl Lab, Argonne, IL 60439 USA
[13] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany
[14] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA
[15] Natl Univ Ireland Galway, Sch Phys, Galway, Ireland
[16] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA
[17] Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA
[18] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA
[19] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA
[20] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA
[21] Columbia Univ, Dept Phys, New York, NY 10027 USA
[22] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA
[23] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA
[24] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA
[25] Saha Inst Nucl Phys, Kolkata 700064, India
[26] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA
[27] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA
[28] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA
[29] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA
[30] Anderson Univ, Dept Phys, Anderson, IN 46012 USA
[31] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland
[32] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA
[33] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 94307 USA
[34] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland
基金
美国国家科学基金会; 加拿大自然科学与工程研究理事会; 美国国家航空航天局; 爱尔兰科学基金会;
关键词
BL Lacertae objects: general; BL Lacertae objects: individual (1ES 0229+200; VER J0232+202); diffuse radiation; galaxies: active; gamma rays: general; magnetic fields; EXTRAGALACTIC BACKGROUND LIGHT; ACTIVE GALACTIC NUCLEI; BL LACERTAE OBJECTS; X-RAY; TEV BLAZARS; MAGNETIC-FIELDS; OPTICAL DEPTH; RADIATION; EMISSION; SPECTRA;
D O I
10.1088/0004-637X/782/1/13
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
The high-frequency-peaked BL Lacertae object 1ES 0229+200 is a relatively distant (z = 0.1396), hard-spectrum (Gamma similar to 2.5), very-high-energy (VHE; E > 100 GeV) emitting gamma-ray blazar. VHE measurements of this active galactic nucleus have been used to place constraints on the intensity of the extragalactic background light and the intergalactic magnetic field (IGMF). A multi-wavelength study of this object centered around VHE observations by Very Energetic Radiation Imaging Telescope Array System (VERITAS) is presented. This study obtained, over a period of three years, an 11.7 standard deviation detection and an average integral flux F(E > 300 GeV) = (23.3 +/- 2.8(stat) +/- 5.8(sys)) x 10(-9) photons m(-2) s(-1), or 1.7% of the Crab Nebula's flux (assuming the Crab Nebula spectrum measured by H. E. S. S). Supporting observations from Swift and RXTE are analyzed. The Swift observations are combined with previously published Fermi observations and the VHE measurements to produce an overall spectral energy distributionwhich is then modeled assuming one-zone synchrotron-self-Compton emission. The chi(2) probability of the TeV flux being constant is 1.6%. This, when considered in combination with measured variability in the X-ray band, and the demonstrated variability of many TeV blazars, suggests that the use of blazars such as 1ES 0229+200 for IGMF studies may not be straightforward and challenges models that attribute hard TeV spectra to secondary gamma-ray production along the line of sight.
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