M33（HERM33ES）中100 μ m和160 μ m辐射作为分辨恒星形成率估算值
100 mum and 160 mum emission as resolved star-formation rate estimators in M33 (HERM33ES)
摘要：
在过去的几年里，一些研究已经提供了恒星形成率（SFR）的估计，或者仅仅从一个红外波段的总红外光度。然而，这些关系一般是整个星系，这是已知的，包含一个大规模的漫发射，不一定与最近的恒星形成插曲。我们提供了新的关系，估计SFR解决恒星形成区域在100妈妈和160妈妈。我们在附近（840 kpc）星系M33中选择单个恒星形成区。我们估计的SFR结合发射在Halpha和在24妈妈校准发射在100妈妈和160妈妈作为SFR估计，映射PACS/赫歇尔。这些数据是在HERM 33 ES开放时间关键项目的框架内获得的。在160 μ m处的HII区域中的发射比在100 μ m处的发射少。在一个动态范围内几乎2德克斯在西格玛（SFR），我们发现，100妈妈的排放是一个近线性估计的SFR，而在160妈妈是稍微超线性。单个恒星形成区域的行为与整个星系的行为惊人地相似。在高西格玛（SFR），恒星形成驱动尘埃温度，而辐射传输和尘埃加热过程的不确定性和变化在低西格玛（SFR）占主导地位。需要对星系和单个恒星形成区进行详细建模，以解释两者之间的相似性和差异，并评估星系中弥漫发射的比例。
英文摘要：
Over the past few years several studies have provided estimates of the SFR (star-formation rate) or the total infrared luminosity from just one infrared band. However these relations are generally derived for entire galaxies, which are known to contain a large scale diffuse emission that is not necessarily related to the latest star-formation episode. We provide new relations to estimate the SFR from resolved star-forming regions at 100 mum and 160 mum. We select individual star-forming regions in the nearby (840 kpc) galaxy M33. We estimate the SFR combining the emission in Halpha and at 24 mum to calibrate the emission at 100 mum and 160 mum as SFR estimators, as mapped with PACS/Herschel. The data are obtained in the framework of the HERM33ES open time key project. There is less emission in the HII regions at 160 mum than at 100 mum. Over a dynamic range of almost 2 dex in Sigma(SFR) we find that the 100 mum emission is a nearly linear estimator of the SFR, whereas that at 160 mum is slightly superlinear. The behaviour of individual star-forming regions is surprisingly similar to that of entire galaxies. At high Sigma(SFR), star formation drives the dust temperature, whereas uncertainties and variations in radiation-transfer and dust-heated processes dominate at low Sigma(SFR). Detailed modelling of both galaxies and individual star forming regions will be needed to interpret similarities and differences between the two and assess the fraction of diffuse emission in galaxies.
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