Chandra observations of the HII complex G5.89-0.39 and TeV gamma-ray source HESSJ1800-240B
Chandra observations of the HII complex G5.89-0.39 and TeV gamma-ray source HESSJ1800-240B
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钱德拉对 HII 复合体 G5.89-0.39 和 TeV 伽马射线源 HESSJ1800-240B 的观测
DOI：
10.1016/j.jheap.2016.05.001
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发表时间：
2016
影响因子：
3.8
通讯作者：
S.
中科院分区：
文献类型：
--
作者：
Hampton;E. J.;Rowell;G.;Hofmann;W.;Horn;D.;Uchiyama;Y.;Wagner;S.
我们提出了我们的调查结果，使用钱德拉X射线观测，到大质量星星形成区G5的恒星人口。89-0.39，以及它与符合TeV伽马射线源HESSJ 1800 - 240 B的潜在连接。G5。89-0.39包含两个单独的HII区G5。89-0.39 A和G5。89-0.39 B（超致密HII区）。我们确定了159个单独的X射线点源，在我们的观察使用源检测算法wavdetect。35个X射线源与HII复合体G5有关。89-0.39.这35个X射线源的平均未吸收光度（0.3-10 keV）为30.5 erg/s，是典型的B7-B5型恒星。G5的潜在电离源。89-0.39 B被称为费尔特星星，在我们的观测中可能被确定为具有未吸收的X射线光度，暗示着B7-B5星星。这些源的叠加能谱与单热等离子体APEC模型很好地拟合，kT = 5 keV，柱密度NH = 2.6× 10 22 cm− 2（A V = 10）。朝向G5的残余（源扣除）X射线发射。89-0.39 A和B分别比它们各自的叠置源光度大约30%和25%。假设这些残余辐射是来自未分辨的恒星源，则G5中的总B型等效恒星含量。89-0.39 A和B将是75颗恒星，与早期对G5中热恒星总质量的估计一致。89-0.39.我们还研究了G5中35个X射线源的可变性。89-0.39.其中10个来源被标记为可变。需要进一步的研究来确定这种变化的确切原因，但是这种变化可能指向前主序星。这样的恒星族群可以提供足够的动能，来解释HESSJ 1800 - 240 B的部分GeV至TeV伽马射线辐射。然而，未来需要角分角分辨率的伽马射线成像来解开G5驱动的潜在伽马射线分量。89-0.39从那些由W28 SNR供电。
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. 89-0.39 A and G5. 89-0.39 B (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 (0.3–10 keV) of∼ 10 30.5 erg/s, typical of B7–B5 type stars. The potential ionising source of G5. 89-0.39 B 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∼ 5 keV, and column density N H= 2.6× 10 22 cm− 2 (A V∼ 10). The residual (source-subtracted) X-ray emission towards G5. 89-0.39 A 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. 89-0.39 A 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.
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发表时间：
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