100 μm and 160 μm emission as resolved star-formation rate estimators in M 33 (HERM33ES)
100 μm and 160 μm emission as resolved star-formation rate estimators in M 33 (HERM33ES)
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100 μm 和 160 μm 发射作为 M 33 (HERM33ES) 中已解析的恒星形成率估计器
DOI：
10.1051/0004-6361/201014649
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发表时间：
2010
影响因子：
6.5
通讯作者：
S. Verley
中科院分区：
文献类型：
--
作者：
M. Boquien;D. Calzetti;C. Kramer;E. Xilouris;Frank Bertoldi;J. Braine;C. Buchbender;F. Combes;F. Israel;Baerbel S. Koribalski;S. Lord;G. Quintana;M. Relaño;M. Röllig;Gordon J. Stacey;F. Tabatabaei;R. Tilanus;F. V. D. Tak;P. Werf;S. Verley
上下文。在过去的几年里，几项研究已经提供了仅仅一个红外波段的恒星形成率(SFR)或总红外光度的估计。然而，这些关系通常是针对整个星系得出的，众所周知，这些星系包含的大规模漫射辐射与最近的恒星形成事件并不一定相关。
目标。我们提供了从100μm和160μm的已分辨恒星形成区估算稳定比的新关系式。
方法：研究方法。我们选择了附近(840kpc)星系M33中的单个恒星形成区。我们结合Hα和24μm的辐射来估计稳定辐射比，以校准100μm和160μm的稳定辐射比估计值，如图所示。这些数据是在HERM33ES开放时间关键程序的框架内获得的。
结果。在Σ_(Sfr)接近2dex的动态范围内，我们发现100μm的辐射是对sfr的近线性估计，而在160μm处的辐射则略呈超线性。
结论。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Σ_(Sfr)时，恒星形成驱动尘埃温度，而在低Σ_(Sfr)时，辐射传输和尘埃加热过程中的不确定性和变化占主导地位。需要对星系和单个恒星形成区域进行详细的模拟，以解释两者之间的异同，并评估
星系中漫射辐射的比例。
Context. 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.
Aims. We provide new relations to estimate the SFR from resolved star-forming regions at 100 μm and 160 μm.
Methods. We select individual star-forming regions in the nearby (840 kpc) galaxy M33. We estimate the SFR combining the emission in Hα and at 24 μm to calibrate the emission at 100 μm and 160 μm as SFR estimators, as mapped with PACS/Herschel. The data are obtained in the framework of the HERM33ES open time key program.
Results. There is less emission in the HII regions at 160 μm than at 100 μm. Over a dynamic range of almost 2 dex in Σ_(SFR) we find that the 100 μm emission is a nearly linear estimator of the SFR, whereas that at 160 μm is slightly superlinear.
Conclusions. The behaviour of individual star-forming regions is surprisingly similar to that of entire galaxies. At high Σ_(SFR), star formation drives the dust temperature, whereas uncertainties and variations in radiation-transfer and dust-heated processes dominate at low Σ_(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.
M33 的 PACS 和 SPIRE 光度计图：Herschel M33 扩展勘测 (HERM33ES) 的第一个结果
影响因子：
6.5
作者：
Kramer
通讯作者：
Kramer