[ FeII ]作为示踪超新星速率
[FeII] as a tracer supernova rate
摘要：
超新星在将处理过的物质反馈到星系的ISMof中起着不可或缺的作用，并负责宇宙的大部分化学富集。超新星的速率也可以揭示恒星的形成历史。超新星速率通常通过非热射电连续谱光度来测量，但本文在11个近距离星暴星系样本中建立了[FeII]1.26光度与超新星速率之间的定量关系。SINFONI数据立方体用于执行这种相关性的像素像素分析。使用Br等效宽度和光度作为Starburst 99的唯一观测输入，在每个像素处导出超新星速率，并创建超新星速率图。然后，这是比较形态和定量的[Fe Ⅱ]1.26光度图。我们发现超新星速率和[FeII]1.26之间在像素-像素的基础上有很强的线性和形态相关性：对数SNrate yr-1 pc-2 =（1.01 \pm 0.2）\ast log[FeII]1.26 ergs-1 pc-2 - 41.17 \pm 0.9 Starburst 99推导的超新星速率也与射电推导的超新星速率非常一致，这进一步证明了[Fe II]作为超新星速率示踪剂的强度。在这个星系样本中发现了强相关性，我们现在定性地使用[FeII]1.26来推导超新星速率，无论是像素像素还是积分星系。
英文摘要：
Supernovae play an integral role in the feedback of processed material into the ISMof galaxies and are responsible for most of the chemical enrichment of the universe. The rate of supernovae can also reveal the star formation histories. Supernova rate is usually measured through the non-thermal radio continuum luminosity, but in this paper we establish a quantitative relationship between the [FeII]1.26 luminosity and supernova rate in a sample of 11 near-by starburst galaxies. SINFONI data cubes are used to perform a pixel pixel analysis of this correlation. Using Br equivalent width and luminosity as the only observational inputs into Starburst 99, the supernova rate is derived at each pixel and a map of supernova rate is created. This is then compared morphologically and quantitatively to [FeII]1.26 luminosity map. We find a strong linear and morphological correlation between supernova rate and [FeII]1.26 on a pixel-pixel basis: log SNrate yr-1 pc-2 = (1.01 \pm 0.2) \ast log[FeII]1.26 ergs-1 pc-2 - 41.17 \pm 0.9 The Starburst 99 derived supernova rates are also in good agreement with the radio derived supernova rates, which further demonstrates the strength of [FeII] as a tracer of supernova rate. With the strong correlation found in this sample of galaxies, we now qualitatively use [FeII]1.26 to derive supernova rate on either a pixel-pixel or integrated galactic basis.
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