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- [1] Chandra observations of the HII complex G5.89-0.39 and TeV source HESSJ1800-240BHIGH ENERGY GAMMA-RAY ASTRONOMY, 2012, 1505 : 269 - 272Hampton, E.Rowell, G.Horns, D.Uchiyama, Y.Funk, S.Wagner, S.
Chandra observations of the HII complex G5.89-0.39 and TeV gamma-ray source HESSJ1800-240B
被引：8
|作者：
Hampton, E. J.
[1
,6
]
Rowell, G.
[1
]
Hofmann, W.
[2
]
Horns, D.
[3
]
Uchiyama, Y.
[4
]
Wagner, S.
[5
]
机构：
[1] Univ Adelaide, Sch Chem Phys, Adelaide, SA 5005, Australia
[2] Max Planck Inst Kernhys, POB 103980, D-69029 Heidelberg, Germany
[3] Univ Hamburg, Inst Expt Phys, Luruper Chausse 149, D-22761 Hamburg, Germany
[4] Rikkyo Univ, Dept Phys, Toshima Ku, 3-34-1 Nishi Ikebukuro, Tokyo 1718501, Japan
[5] Heidelberg Univ, Landessternwarte, D-69117 Heidelberg, Germany
[6] Australian Natl Univ, Res Sch Astron & Astrophys, Mt Stromlo Observ, Cotter Rd, Weston, ACT 2611, Australia
关键词：
MASS STAR-FORMATION;
MM LINE SURVEY;
MOLECULAR CLOUDS;
X-RAYS;
PARTICLE-ACCELERATION;
COLLIDING WINDS;
STELLAR CONTENT;
EMISSION;
YOUNG;
GAS;
D O I：
10.1016/j.jheap.2016.05.001
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
We present the results of our investigation, using a Chandra X-ray observation, into the stellar population of the massive star formation region G5.89-0.39, and its potential connection to the coincident TeV gamma-ray source HESSJ1800-240B. G5.89-0.39 comprises two separate HII regions G5.89-0.39A and G5.89-0.39B (an ultra-compact HII region). We identified 159 individual X-ray point sources in our observation using the source detection algorithm wavdetect. 35 X-ray sources are associated with the HII complex G5.89-0.39. The 35 X-ray sources represent an average unabsorbed luminosity (0.3-10keV) of similar to 10(30.5) erg/s, typical of B7-B5 type stars. The potential ionising source of G5.89-0.39B known as Feldt's star is possibly identified in our observation with an unabsorbed X-ray luminosity suggestive of a B7-B5 star. The stacked energy spectra of these sources is well-fitted with a single thermal plasma APEC model with kT similar to 5keV, and column density N-H= 2.6 x10(22)cm(-2)(A(V) similar to 10). The residual (source-subtracted) X-ray emission towards G5.89-0.39A and B is about 30% and 25% larger than their respective stacked source luminosities. Assuming this residual emission is from unresolved stellar sources, the total B-type-equivalent stellar content in G5.89-0.39A and B would be 75 stars, consistent with an earlier estimate of the total stellar mass of hot stars in G5.89-0.39. We have also looked at the variability of the 35 X-ray sources in G5.89-0.39. Ten of these sources are flagged as being variable. Further studies are needed to determine the exact causes of the variability, however the variability could point towards pre-main sequence stars. Such a stellar population could provide sufficient kinetic energy to account for a part of the GeV to TeV gamma-ray emission in the source HESSJ1800-240B. However, future arc-minute angular resolution gamma-ray imaging will be needed to disentangle the potential gamma-ray components powered by G5.89-0.39 from those powered by the W28 SNR. (C) 2016 Elsevier B.V. All rights reserved.
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页码：1 / 19
页数：19
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