模拟UV到附近恒星形成星系的射电SED：Grasil的新Parsec SSP
Modelling the UV to radio SEDs of nearby star-forming galaxies: new Parsec SSP for Grasil
摘要：
利用更新后的PARSEC大质量恒星演化轨迹数据库，计算了不同金属丰度和IMF质量上限条件下年轻简单恒星星族（SSP）的积分恒星光、电离光子收支和超新星爆发率.使用云，我们计算并包括在SSP光谱的星云发射的贡献。我们还重新审视了来自年轻恒星的热和非热射电辐射贡献。使用GRASIL，我们可以预测全色光谱和任何类型的恒星形成星系的主要复合线，包括尘埃吸收和再发射的影响。我们检查新的模型对选定的观测良好的附近星系的光谱能量分布（SED）。从最佳拟合模型，我们得到一组一致的恒星形成率（SFR）校准波长范围从紫外线（UV）到无线电。我们还提供了分析校准，考虑到金属和IMF的SSP的质量上限的依赖。我们表明，后者的限制可以很好地约束结合信息，从观察到的远红外，24 μm，33 GHz和Hα光度。另一个有趣的属性来自拟合是，虽然在正常的星系中，线的衰减显着高于附近的连续体，在个别恒星爆发区域，它们是相似的，支持这种效应是由于年龄选择性灭绝的概念。由于在这些条件下的巴耳末衰减方法可能是不准确的，我们提供的关系，估计从观测到的24 μm或33 GHz的通量的衰减。这些关系对于年轻高红移星系的分析是有用的。
英文摘要：
By means of the updated PARSEC database of evolutionary tracks of massive stars, we compute the integrated stellar light, the ionizing photon budget and the supernova rates of young simple stellar populations (SSPs), for different metallicities and IMF upper mass limits. Using CLOUDY we compute and include in the SSP spectra the neb- ular emission contribution. We also revisit the thermal and non-thermal radio emission contribution from young stars. Using GRASIL we can thus predict the panchromatic spectrum and the main recombination lines of any type of star-forming galaxy, including the effects of dust absorption and re-emission. We check the new models against the spectral energy distributions (SEDs) of selected well-observed nearby galaxies. From the best-fit models we obtain a consistent set of star formation rate (SFR) calibrations at wavelengths ranging from ultraviolet (UV) to radio. We also provide analytical calibrations that take into account the dependence on metallcity and IMF upper mass limit of the SSPs. We show that the latter limit can be well constrained by combining information from the observed far infrared, 24 μm, 33 GHz and Hα luminosities. Another interesting property derived from the fits is that, while in a normal galaxy the attenuation in the lines is significantly higher than that in the nearby continuum, in individual star bursting regions they are similar, supporting the notion that this effect is due to an age selective extinction. Since in these conditions the Balmer decrement method may not be accurate, we provide relations to estimate the attenuation from the observed 24 μm or 33 GHz fluxes. These relations can be useful for the analysis of young high redshift galaxies.
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