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 (0.3–10 keV) of $\sim {10}^{30.5}\text{erg}/\text{s}$, 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 ∼ 5 keV, and column density ${\mathrm{N}}_{\mathrm{H}}=2.6\times {10}^{22}{\text{cm}}^{-2}$ (${\mathrm{A}}_{\mathrm{V}}\sim 10$). 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.

我们使用钱德拉（Chandra）X射线观察，向大规模恒星形成区域G5.89-0.39的恒星群体展示了我们的调查结果，以及其与TeV伽玛射线源HESSJ1800-240B的潜在联系。G5.89-0.39包含两个单独的HII区域G5.89-0.39A和G5.89-0.39B（超紧凑型HII区域）。我们使用源检测算法wavdetect在我们的观测中识别了159个单独的X射线点源。35个X射线源与HII复合物G5.89-0.39相关。35个X射线源的平均未吸收光度（0.3–10 keV）为$〜{10}^{30.5}\text{尔格}/\text{s}$，典型代表B7–B5型星。在我们的观察中，可能会发现G5.89-0.39B的潜在电离源，称为Feldt星，其未吸收的X射线光度暗示B7–B5星。这些能量源的叠加能谱与kT〜5 keV的单热等离子体APEC模型和柱密度非常吻合${\mathrm{ñ}}_{\mathrm{H}}=2.6\times {10}^{22}{\text{厘米}}^{-2}$ （${\mathrm{一种}}_{\mathrm{V}}〜10$）。朝向G5.89-0.39A和B的剩余（减去源）X射线发射分别比其各自堆叠的源发光度大30％和25％。假设该残留发射来自未解析的恒星源，那么G5.89-0.39A和B中B型等效恒星的总含量将为75颗恒星，这与先前对G5.89中热恒星总恒星质量的估计一致-0.39。我们还研究了G5.89-0.39中35个X射线源的变异性。这些来源中有十个被标记为可变。需要进一步研究以确定变异性的确切原因，但是变异性可能指向主序前恒星。这样的恒星种群可以提供足够的动能，以解决源HESSJ1800-240B中GeV到TeV伽马射线发射的一部分。然而，