AI 中文总结
该研究通过LHAASO和Fermi-LAT数据分析，发现超高能伽马射线源1LHAASO J1852+0050u与恒星形成区高度相关，其GeV-100TeV发射最可能由恒星形成区中的质子加速和强子相互作用主导。
AI 中文摘要
恒星形成区（SFRs），包括HII区，最近作为能够产生PeV宇宙射线的粒子加速潜在场所（即潜在的银河系PeVatrons）而受到显著关注。然而，已知作为候选PeVatrons的恒星形成区仍然非常稀少。在此，我们报告了超高能伽马射线源1LHAASO J1852+0050u与重合的恒星形成区之间极可能的物理关联。利用约4年的LHAASO数据，对延展源1LHAASO J1852+0050u（本研究中称为J1852）进行了重新分析，其显著性约为13σ，39%包含半径为0.35°。该延展源在投影上覆盖了数十个HII区和一个高能脉冲星PSR J1853+0056。我们重新分析了约16年的Fermi-LAT数据，发现一个与LHAASO源J1852重合的GeV源（命名为SrcAG）。CO谱线观测显示一个分子团块，它与伽马射线源重合，并与距离约3.3 kpc的超致密HII区G34.26+0.15相关。对谱能量分布的拟合表明，PSR J1853+0056无论对于J1852还是SrcAG都无法提供观测到的伽马射线通量。尽管隐藏脉冲星对伽马射线发射的贡献无法排除，但最可能的情况是，GeV-100TeV伽马射线发射主要由恒星形成区通过恒星形成区内加速的质子与分子云之间的p-p强子相互作用所驱动：GeV发射归因于由原恒星活动加速的质子，而TeV发射则归因于由恒星形成区内大质量恒星加速的质子。
英文摘要
Star-forming regions (SFRs), including HII regions, have recently attracted significant attention as potential sites of particle acceleration capable of producing PeV cosmic rays, i.e. as potential Galactic PeVatrons. Yet, SFRs known as candidate PeVatrons are still very rare. Here we report a highly likely physical association between the UHE gamma-ray source 1LHAASO J1852+0050u and coincident star-forming regions. Using $\sim$4 years of LHAASO data, the extended source 1LHAASO J1852+0050u (called J1852 in this study) was reanalyzed with a significance of $\sim$13$σ$ and 39%-containment radius of 0.35$°$. This extended source projectively covers dozens of HII regions and an energetic pulsar PSR J1853+0056. We reanalyzed $\sim$16 years of Fermi-LAT data and found a GeV source (named SrcAG) coincident with the LHAASO source J1852. The CO-line observation shows a molecular clump which coincides with the gamma-ray sources and is related with the ultra-compact HII region G34.26+0.15 at the distance of $\sim$3.3 kpc. Fitting to the spectral energy distribution indicates that PSR J1853+0056 cannot afford the observed gamma-ray flux either for J1852 or SrcAG. Although the contribution from hidden pulsars to the gamma-ray emission could not be excluded, it is most likely that the GeV-100TeV gamma-ray emission is dominantly powered by SFR through p-p hadronic interaction between the protons accelerated in the SFR and MCs: the GeV emission is ascribed to the protons accelerated by protostars' activities, while the TeV emission ascribed to the protons accelerated by massive stars in the SFR.
CommentsAccepted for publication in MNRAS. 14 pages. 7 figures & 5 tables included
