Calibration of star formation rate tracers for short- and long-lived star formation episodes
Calibration of star formation rate tracers for short- and long-lived star formation episodes
复制标题
短期和长期恒星形成事件的恒星形成率示踪剂的校准
DOI：
10.1051/0004-6361/200913384
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发表时间：
2009
影响因子：
6.5
通讯作者：
J. Mas
中科院分区：
文献类型：
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作者：
H. Otí;J. Mas
上下文为了得到宇宙中星星形成的历史，需要一套不同波长的校准星星形成速率示踪剂。校准必须始终考虑到灭绝的影响，星星形成制度（短或长寿命）和演化状态，以避免在不同的红移范围的偏差。目标。我们使用进化合成模型优化激烈的情节星星形成计算一致的校准最常见的星星形成率示踪剂在不同的能量范围内，从X射线到射电光度。方法.我们已经计算了不同的估计考虑到近瞬时和连续的星星形成制度和星际消光（在高能量衰减，热再辐射在远红外）的影响的预测演变。我们还考虑了金属丰度对不同估计量校准的影响。结果本文给出了一套完整的星星形成速率示踪剂的一致性标定方法，并根据演化状态、星星形成机制、星际消光和初始质量函数对最常见的恒星形成区条件进行了计算。我们讨论了不同的示踪剂在不同的星星形成的情况下的有效性，并比较我们的预测与以前的校准的一般使用。结论.为了测量星星形成事件的强度，我们应该区分近瞬时和连续的星星形成机制。虽然星星形成强度（M�）应用于前者，但更常见的星星-
Context. To derive the history of star formation in the Universe a set of calibrated star formation rate tracers at different wavelengths is required. The calibration has to consistently take into account the effects of extinction, star formation regime (short or long-lived) and the evolutionary state to avoid biases at different redshift ranges. Aims. We use evolutionary synthesis models optimized for intense episodes of star formation to compute a consistent calibration of the most usual star formation rate tracers at different energy ranges, from X-ray to radio luminosities. Methods. We have computed the predicted evolution of the different estimators taking into account nearly-instantaneous and continuous star formation regimes and the effect of interstellar extinction (attenuation at high energies, thermal reradiation in the far infrared). We have also considered the effect of metallicity on the calibration of the different estimators. Results. A consistent calibration of a complete set of star formation rate tracers is presented, computed for the most usual star-forming regions conditions in terms of evolutionary state, star formation regime, interstellar extinction and initial mass function. We discuss the validity of the different tracers in different star formation scenarios and compare our predictions with previous calibrations of general use. Conclusions. In order to measure the intensity of star formation episodes we should distinguish between nearly-instantaneous and continuous star formation regimes. While the star formation strength (M� ) should be used for the former, the more common star –
马克斯·普朗克研究所/密歇根大学（美国）
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