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The Great Laboratory M51: Probing the Physics of Star Formation and Radio Emission on the 100pc-Scale

伟大的实验室 M51：在 100 颗尺度上探索恒星形成和射电发射的物理现象

基本信息

批准号：
41960361
负责人：
Dr. Eva Schinnerer
金额：
--
依托单位：
Max-Planck-Institut für Astronomie (MPIA)
依托单位国家：
德国
项目类别：
Priority Programmes
财政年份：
2007
资助国家：
德国
起止时间：
2006-12-31 至 2010-12-31
项目状态：
已结题

来源：
https://gepris.dfg.de/gepris/projekt/41960361?language=en
关键词：
Great Laboratory M51 Probing Physics

项目摘要

The empirical radio-IR relation is widely used out to high-z to estimate star formation rates (SFRs), despite the fact that its origin is poorly understood. Processes within giant molecular clouds where stars form (at the 100 pc scale) must control it. The grand-design spiral M51 is ideal for a detailed study of the underlying physics of the radio-SFR relation, due to the range of physical conditions in the spiral disk, and the large body of high-resolution (1-2") data available from the X-ray to the radio. Our imaging radio data from the VLA and Effelsberg observatories at 20cm, 6cm and 4cm are ideally suited to study the nature of the radio emission (thermal/nonthermal decomposition, turn-over frequency) and to test whether the radio emission is indeed an unbiased tracer of star formation, over a wide range of physical environments. In addition, we have high resolution mid-IR imaging spectroscopic data from the Spitzer telescope which will be used for an in-depth study of a density wave in a spiral region. Both datasets combined will provide new and critical insight into the star formation process in the disks of galaxies. In short, continued funding for the post-doc G. Dumas is requested to (a) to study the radio-IR relation on GMC scale, (b) to compare the applicability of star formation tracer from the UV to the radio, and (c) to gain a physical picture of a spiral density wave.

经验射电-红外关系被广泛应用于高Z估计星星形成率（SFR），尽管事实上，它的起源是知之甚少。巨大的分子云中恒星形成的过程（100 pc尺度）必须控制它。由于螺旋盘中的物理条件范围，以及从X射线到射电的大量高分辨率（1-2”）数据，宏伟设计的螺旋M51是详细研究射电-SFR关系的基础物理的理想选择。我们从VLA和Effelsberg天文台在20厘米，6厘米和4厘米的成像无线电数据非常适合于研究无线电发射的性质（热/非热分解，翻转频率），并测试无线电发射是否确实是一个公正的示踪星星形成，在广泛的物理环境。此外，我们有高分辨率的中红外成像光谱数据从斯皮策望远镜，将用于深入研究的密度波在螺旋区域。这两个数据集的结合将为星系盘中星星的形成过程提供新的和关键的见解。简而言之，继续资助博士后G。大仲马被要求（a）研究GMC尺度上的射电-红外关系，（B）比较从紫外到射电的星星形成示踪剂的适用性，（c）获得螺旋密度波的物理图像。