论文标题
从3FHL J1907.0+0713探测伽马射线的星形形成起源
Probing the star formation origin of gamma rays from 3FHL J1907.0+0713
论文作者
论文摘要
嵌入巨型分子云（GMC）的恒星形成（SF）区域是银河伽玛射线的潜在贡献者。检测到伽马射线源3FHL J1907.0+0713在0.2 $ - $ 300 GEV能量范围内的重要性约为13 $σ$，在从Fermi-Lat数据集中删除了PSR J1906+0722的伽马射线脉动期+0722大约10年的伽马射线脉动范围。 3FHL J1907.0+0713的能源光谱最适合于频谱指数为2.26 $ \ pm $ 0.05的电力法。 Nanten2获取的CO（$ j $ = 1 $ - $ 0）显示，3FHL J1907.0+0713与GMC重叠，GMC的峰值速度约为38 km S $^{ - 1} $。 3FHL J1907.0+0713的最合适位置距离银河系超新星残留物（SNR）3C 397距离约0.13度，并且与与弓箭盘中的星星相关。我们表明，3FHL J1907.0+0713，3C 397以及与PULSAR的任何位置巧合之间没有物理连接。 3FHL J1907.0+0713的频谱非常适合HADRONIC和LEPTONIC GAMMA-RAY发射模型，并且计算出2.6 kpc的总亮度为1.1 $ \ times $ 10 $^{34} $^{34} $ ERG S $^{ - 1 $^{ - 1} $。我们还讨论了来自3FHL J1907.0+0713的伽马射线的可能起源，其中SNR，大量的原恒星流出，失控的恒星中的恒星风，碰撞的风二元组和年轻的恒星集群被认为是候选源。
Star-forming (SF) regions embedded inside giant molecular clouds (GMCs) are potential contributors to Galactic gamma rays. The gamma-ray source 3FHL J1907.0+0713 is detected with a significance of roughly 13$σ$ in the 0.2 $-$ 300 GeV energy range after the removal of gamma-ray pulsation periods of PSR J1906+0722 from the Fermi-LAT data set of about 10 years. The energy spectrum of 3FHL J1907.0+0713 is best-fitted to a power law model with a spectral index of 2.26 $\pm$ 0.05. The CO($J$ = 1$-$0) data taken by NANTEN2 revealed that 3FHL J1907.0+0713 is overlapping with a GMC having a peak velocity of about 38 km s$^{-1}$. The best-fitting location of 3FHL J1907.0+0713 is measured to be approximately 0.13 degrees away from the Galactic supernova remnant (SNR) 3C 397 and it overlaps with a star that is associated with a bow-shock nebula. We show that there is no physical connection between 3FHL J1907.0+0713, 3C 397, as well as any positional coincidence with the pulsar. The spectrum of 3FHL J1907.0+0713 is fitting to both hadronic and leptonic gamma-ray emission models and the total luminosity at a distance of 2.6 kpc is calculated to be 1.1 $\times$ 10$^{34}$ erg s$^{-1}$. We also discuss possible SF origins of gamma rays from 3FHL J1907.0+0713, where SNRs, massive protostar outflows, stellar winds from runaway stars, colliding wind binaries, and young stellar clusters are considered as candidate sources.
