早型星系中恒星质量的估算：程序、不确定性和模型依赖性
Stellar mass estimates in early-type galaxies: procedures, uncertainties and models dependence
摘要：
本文的目的是量化的依赖关系的光度和恒星质量的早期型星系的不同模型和模型参数，可用于分析观测数据的估计。本文件分为两部分。第一个分析M/L比率和不同波段的k修正对模型参数（IMF，金属丰度，恒星形成历史，年龄）的依赖性，假设一些最流行的分光光度代码通常用于研究星系的演化状态[.]。我们工作的第二部分是致力于量化的可靠性和系统学影响的质量和光度估计的最佳拟合技术应用于早期类型的星系在$1<z<2$的光度学SED的装置。为此，我们采用最佳拟合技术的基础上建立了广泛的早期型星系模型的一些模拟目录。然后，我们比较的光度和恒星质量估计从SED拟合与真实的已知输入值。的质量估计的善良被认为是依赖于质量估计通过推导它，但无论如何不能检索质量比在一个因素2-3，这取决于可用的光度数据的质量和/或星系的距离，因为更遥远的星系是平均较暗，从而受到较大的光度误差。最后，我们提出了一个新的经验质量估计的基础上的K波段视星等和观测（V-K）的颜色。我们表明，这种新的估计早期型星系的恒星质量含量的可靠性和稳定性，甚至高于那些最好的经典估计，不可忽视的优势，它不需要任何多波长的数据拟合。
英文摘要：
The aim of the present paper is to quantify the dependence of the estimates of luminosities and stellar mass of early-type galaxies on the different models and model parameters which can be used to analyze the observational data. The paper is organized in two parts. The first one analyzes the dependence of the M/L ratios and of the k-corrections in different bands on model parameters (IMF, metallicity, star formation history, age), assuming some among the most popular spectrophotometric codes usually adopted to study the evolutionary status of galaxies [...]. The second part of our work is dedicated to quantify the reliability and systematics affecting the mass and luminosity estimates obtained by means of the best fitting technique applied to the photometric SEDs of early-type galaxies at $1<z<2$. To this end, we apply the best fitting technique to some mock catalogs built on the basis of a wide set of models of early-type galaxies. We then compare the luminosity and the stellar mass estimated from the SED fitting with the true known input values. The goodness of the mass estimate is found to be dependent on the mass estimator adopted to derive it, but masses cannot anyhow be retrieved better than within a factor 2-3, depending on the quality of the available photometric data and/or on the distance of the galaxies since more distant galaxies are fainter on average and thus affected by larger photometric errors. Finally, we present a new empirical mass estimator based on the K band apparent magnitude and on the observed (V-K) colour. We show that the reliability of the stellar mass content derived with this new estimator for early-type galaxies and its stability are even higher than those achievable with the best classic estimators, with the not negligible advantage that it does not need any multi-wavelength data fitting.
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