AI 中文总结
本研究利用17.75年Fermi-LAT数据在恒星形成区S140探测到GeV γ射线源4FGL J2220.8+6319e，其辐射与S140 IRS1所在分子云重合，由该天体驱动的喷流可解释其辐射，排除恒星风作为能量来源。
AI 中文摘要
我们利用17.75年的Fermi-LAT数据，在S140 HII区探测到一个GeV γ射线源，在0.1-500 GeV能段的源探测显著性约为32.1σ。该辐射具有显著延展特性（1 GeV以上的AIC证据比为2×10^9），因此被命名为4FGL J2220.8+6319e。该γ射线辐射在空间上与包含大质量年轻恒星天体S140 IRS1的分子云重合。其光谱用对数抛物线谱拟合效果最佳（TS_cur(LP)=104.1），可通过强子模型和轻子模型重现。S140 IRS1驱动的喷流提供了可行的粒子加速位点，其注入时标和最大粒子能量与理论预期一致，而恒星风在能量上不被支持。
英文摘要
We report the detection of a GeV γ-ray source in the S140 HII region using 17.75 years of Fermi-LAT data, with a source-detection significance of ~32.1σ in the 0.1-500 GeV energy band. The emission is significantly extended (AIC evidence ratio above 1 GeV is 2x10^9) and is therefore designated as 4FGL J2220.8+6319e. The γ-ray emission coincides spatially with a molecular cloud that hosts the massive young stellar object S140 IRS1. Its spectrum is best fitted by a log-parabolic spectrum (TS_cur(LP) = 104.1) and can be reproduced by both hadronic and leptonic models. The jet driven by S140 IRS1 offers a viable particle acceleration site, yielding injection timescales and maximum particle energies consistent with theoretical expectations, whereas stellar winds are energetically disfavored.
CommentsAccepted for publication in ApJ
