DETECTION OF EXTENDED VHE GAMMA RAY EMISSION FROM G106.3+2.7 WITH VERITAS

被引:67
作者
Acciari, V. A. [3 ]
Aliu, E. [1 ,2 ]
Arlen, T. [4 ]
Aune, T. [5 ,6 ]
Bautista, M. [7 ]
Beilicke, M. [8 ]
Benbow, W. [3 ]
Boltuch, D. [1 ,2 ]
Bradbury, S. M. [9 ]
Buckley, J. H. [8 ]
Bugaev, V. [8 ]
Butt, Y. [10 ]
Byrum, K. [11 ]
Cannon, A. [12 ]
Cesarini, A. [13 ]
Chow, Y. C. [4 ]
Ciupik, L. [14 ]
Cogan, P. [7 ]
Cui, W. [15 ]
Dickherber, R. [8 ]
Ergin, T. [10 ]
Fegan, S. J. [4 ]
Finley, J. P. [15 ]
Fortin, P. [16 ]
Fortson, L. [14 ]
Furniss, A. [5 ,6 ]
Gall, D. [15 ]
Gillanders, G. H. [13 ]
Gotthelf, E. V. [17 ]
Grube, J. [12 ]
Guenette, R. [7 ]
Gyuk, G. [14 ]
Hanna, D. [7 ]
Holder, J. [1 ,2 ]
Horan, D. [18 ]
Hui, C. M. [19 ]
Humensky, T. B. [20 ]
Kaaret, P. [21 ]
Karlsson, N. [14 ]
Kertzman, M. [22 ]
Kieda, D. [19 ]
Konopelko, A. [23 ]
Krawczynski, H. [8 ]
Krennrich, F. [24 ]
Lang, M. J. [13 ]
LeBohec, S. [19 ]
Maier, G. [7 ]
McCann, A. [7 ]
McCutcheon, M. [7 ]
Millis, J. [25 ]
机构
[1] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA
[2] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA
[3] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA
[4] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA
[5] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA
[6] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA
[7] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada
[8] Washington Univ, Dept Phys, St Louis, MO 63130 USA
[9] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England
[10] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA
[11] Argonne Natl Lab, Argonne, IL 60439 USA
[12] Natl Univ Ireland Univ Coll Dublin, Sch Phys, Dublin 4, Ireland
[13] Natl Univ Ireland, Sch Phys, Galway, Ireland
[14] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA
[15] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA
[16] Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA
[17] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA
[18] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France
[19] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA
[20] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA
[21] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA
[22] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA
[23] Pittsburg State Univ, Dept Phys, Pittsburg, KS 66762 USA
[24] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA
[25] Anderson Univ, Dept Phys, Anderson, IN 46012 USA
[26] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland
[27] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA
[28] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland
基金
爱尔兰科学基金会; 美国国家科学基金会; 加拿大自然科学与工程研究理事会; 英国科学技术设施理事会;
关键词
gamma rays: observations; ISM: individual (G106.3+2.7=VER J2227+608); pulsars: individual (J2229+6114); supernova remnants; PULSAR WIND NEBULAE; SOURCE 3EG J2227+6122; GALACTIC-PLANE SURVEY; SUPERNOVA REMNANT; MOLECULAR CLOUDS; SOURCE LIST; TELESCOPE; DISCOVERY; ASTRONOMY; FIELD;
D O I
10.1088/0004-637X/703/1/L6
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We report the detection of very-high-energy (VHE) gamma-ray emission from supernova remnant (SNR) G106.3+2.7. Observations performed in 2008 with the VERITAS atmospheric Cherenkov gamma-ray telescope resolve extended emission overlapping the elongated radio SNR. The 7.3 sigma (pre-trials) detection has a full angular extent of roughly 0 degrees.6 by 0 degrees.4. Most notably, the centroid of the VHE emission is centered near the peak of the coincident (CO)-C-12 (J = 1-0) emission, 0 degrees.4 away from the pulsar PSR J2229+6114, situated at the northern end of the SNR. Evidently the current-epoch particles from the pulsar wind nebula are not participating in the gamma-ray production. The VHE energy spectrum measured with VERITAS is well characterized by a power law dN/dE = N-0(E/3 TeV)(-Gamma) with a differential index of Gamma = 2.29 +/- 0.33(stat) +/- 0.30(sys) and a flux of N-0 = (1.15 +/- 0.27(stat) +/- 0.35(sys)) x 10(-13) cm(-2) s(-1) TeV-1. The integral flux above 1 TeV corresponds to similar to 5 percent of the steady Crab Nebula emission above the same energy. We describe the observations and analysis of the object and briefly discuss the implications of the detection in a multiwavelength context.
引用
收藏
页码:L6 / L9
页数:4
相关论文
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