PROBING THE NATURE OF THE UNIDENTIFIED TeV GAMMA-RAY SOURCE HESS J0632+057 WITH SWIFT

被引:29
作者
Falcone, A. D. [1 ]
Grube, J. [2 ]
Hinton, J. [3 ]
Holder, J. [4 ,5 ]
Maier, G. [6 ]
Mukherjee, R. [7 ]
Skilton, J. [3 ]
Stroh, M. [1 ]
机构
[1] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA
[2] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland
[3] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England
[4] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA
[5] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA
[6] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada
[7] Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA
基金
美国国家科学基金会;
关键词
gamma rays: observations; X-rays: binaries; X-rays: individual(HESS J0632+057); DISCOVERY; RADIATION; VERITAS;
D O I
10.1088/2041-8205/708/1/L52
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
New generation TeV gamma-ray telescopes have discovered many new sources, including several enigmatic unidentified TeV objects. HESS J0632+057 is a particularly interesting unidentified TeV source since: it is a point source, it has a possible hard-spectrum X-ray counterpart and a positionally consistent Be star, it has evidence of long-term very high energy gamma-ray flux variability, and it is postulated to be a newly detected TeV/X-ray binary. We have obtained Swift X-ray telescope observations of this source from MJD 54857 to 54965, in an attempt to ascertain its nature and to investigate the hypothesis that it is a previously unknown X-ray/TeV binary. Variability and spectral properties similar to those of the other three known X-ray/TeV binaries have been observed, with measured flux increases by factors of similar to 3. X-ray variability is present on multiple timescales including days to months; however, no clear signature of periodicity is present on the timescales probed by these data. If binary modulation is present and dominating the measured variability, then the period of the orbit is likely to be >= 54 days (half of this campaign), or it has a shorter period with a variable degree of flux modulation on successive high states. If the two high states measured to date are due to binary modulation, then the favored period is approximately 35-40 days. More observations are required to determine if this object is truly a binary system and to determine the extent that the measured variability is due to inter-orbit flaring effects or periodic binary modulation.
引用
收藏
页码:L52 / L56
页数:5
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