短寿命和长寿命恒星形成事件的恒星形成率示踪剂的校准
Calibration of star formation rate tracers for short- and long-lived star formation episodes
摘要：
为了获得宇宙中恒星形成的历史，需要一套不同波长的校准恒星形成率示踪剂。校准必须始终考虑到灭绝，恒星形成制度（短或长寿命）和演化状态的影响，以避免在不同的红移范围内的偏差。我们使用进化的合成模型优化激烈的恒星形成的情节，以计算一致的校准最常见的恒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。近瞬时和连续的恒星形成制度，和星际灭绝的影响，以及金属丰度的校准的不同估计的效果。一致的校准一套完整的恒星形成率示踪剂，计算最常见的恒星形成区域的条件：演化状态，恒星形成制度，星际消光和初始质量函数。我们讨论了在不同的恒星形成的情况下，不同的示踪剂的有效性，并比较我们的预测与以前的校准一般使用。近瞬时和连续的恒星形成制度必须加以区分。虽然恒星形成强度（\msun）应该用于前者，但更常见的恒星形成率（\msun yr $^{-1}$）仅适用于在长时间内以恒定速率形成恒星的事件。此外，即使对于后者，也应该考虑到进化状态，因为大多数SFR示踪剂只有在1亿年的进化之后才稳定下来。
英文摘要：
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 evolutionary state to avoid biases at different redshift ranges. We use evolutionary synthesis models optimized for intense episodes of star formation in order to compute a consistent calibration of the most usual star formation rate tracers at different energy ranges, from X-ray to radio luminosities. Nearly-instantaneous and continuous star formation regimes, and the effect of interstellar extinction are considered, as well as the effect of metallicity on the calibration of the different estimators. A consistent calibration of a complete set of star formation rate tracers is presented, computed for the most usual star-forming regions conditions: 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. Nearly-instantaneous and continuous star formation regimes must be distinguished. While the Star Formation Strength (\msun) should be used for the former, the more common Star Formation Rate (\msun yr$^{-1}$) is only valid for episodes forming stars at a constant rate during extended periods for time. Moreover, even for the latter, the evolutionary state should be taken into account, since most SFR tracers stabilize only after 100 Myr of evolution.
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