标题： ATLASGAL云团中HII区域的恒星形成历史、恒星形成效率和电离源 显示英文标题

标题： The star formation histories, star formation efficiencies and ionizing sources of ATLASGAL clumps with HII regions

摘要： 1226 ATLASGAL云团与HII区域匹配了CORNISH-北/南调查中的射电源，其中392个有对应的射电源。我们根据Lyman连续谱通量确定了恒星光度。当HII云团的光度小于$\approx$10$^{3.7}$L$_{\odot}$，对应云团质量为$\approx$10$^{2.55}$M$_{\odot}$时，通过Lyman连续谱通量得到的恒星光度会高估实际的恒星光度，因为吸积到原恒星上的物质对射电辐射有显著贡献。在减去吸积光度后，我们得到了合理的恒星光度估计值。使用0.5 Myr等时线，我们根据恒星光度计算了恒星质量，并发现它们大致遵循嵌入星团的$m_{\rm max}-M_{\rm ecl}$关系，与电离源代表HII云团嵌入星团中最 massive 的恒星一致。我们还研究了可能的耀斑活动对观测到的恒星光度的贡献，发现可以忽略不计。我们进一步研究了SFE随云团质量的变化。 根据每个HII云团中最重恒星的推导质量，使用理论上的$m_{\rm max}-M_{\rm ecl}$关系，我们计算了相应嵌入星团的质量，然后计算了云团的SFE。 SFE随着云团质量的增加而减少，中位值为$\approx$0.3。 我们还根据我们在之前工作中开发的模型，独立推导了每个HII云团的SFE。 从观测和模型中推导出的HII云团的SFE有很好的一致性。 关于ATLASGAL云团的恒星形成历史，低质量云团可能比高质量云团更早达到恒星形成的峰值，这与低质量云团较短的自由下落时间一致。 显示英文摘要

摘要： 1226 ATLASGAL clumps with HII regions were matched with radio sources in the CORNISH-North/South surveys, and 392 of them have corresponding radio sources. We determined the stellar luminosity according to the Lyman continuum flux. When the bolometric luminosity of HII-clumps is less than $\approx$ 10$^{3.7}$ L$_{\odot}$, corresponding to a clump mass $\approx$ 10$^{2.55}$ M$_{\odot}$, the stellar luminosities derived from the Lyman continuum flux overestimate the actual stellar luminosities, because the accretion onto the protostars contributes significantly to the radio emission. After subtracting the accretion luminosity, we obtained reasonable estimates of the stellar luminosity. Using the 0.5 Myr isochrone, we calculated the stellar masses according to the stellar luminosities, and found that they roughly follow the $m_{\rm max}-M_{\rm ecl}$ relation of embedded clusters, consistent with the ionizing sources representing the most massive stars in the embedded clusters of HII-clumps. We also studied the contribution of the possible flaring activity to the observed stellar luminosity and found that they can be neglected. We further studied the change of SFE with the clump mass. According to the derived mass of the most massive star in each HII-clump, using the theoretical $m_{\rm max}-M_{\rm ecl}$ relation, we calculated the mass of the corresponding embedded cluster and then the SFE of the clump. The SFE decreases with increasing clump mass, with a median value of $\approx$0.3. We also independently derived the SFE for each HII-clump based on the model developed in our previous work. The SFEs of HII-clumps derived from the observation and the model are in good agreement. Concerning the star formation histories of the ATLASGAL clumps, low-mass clumps may reach the peak of star formation earlier than high-mass clumps, consistent with the shorter free-fall time of low-mass clumps.