解析了星系的恒星质量图。I：全球质量估计的方法和影响
Resolved stellar mass maps of galaxies. I: method and implications for global mass estimates
摘要：
本文介绍了一种基于光学和近红外成像的空间分辨星系质量表面密度图的新技术。我们使用光学/近红外颜色来推断每个像素处的有效恒星质光比（M/L），然后将其乘以表面亮度以获得局部恒星表面质量密度。我们通过边缘化Charlot & Bruzual（2007）的50，000个恒星星族合成（SPS）模型的Monte Carlo库，构建了查找表，以将M/L表示为颜色的函数，其中包括TP-AGB恒星演化阶段的修订处方，具有广泛的尘埃排除。为了在星系中的任何位置提取可靠的通量和颜色信息，我们对图像进行中值自适应平滑，以保持尽可能高的空间分辨率。作为最实用和稳健的，因此是最可靠的方法，我们将H波段中的M/L表示为（g-i）和（i-H）的函数。以这种方式计算的恒星质量图在任何给定像素处的典型准确度为30%或更低，这是从模型中的散射确定的。我们比较了我们的基准方法得到的地图与使用其他组合的带通和旧的BC 03 TP-AGB处方。最后，我们比较总恒星质量的估计，通过整合解决的质量图与未解决的测光。在具有明显尘埃带的星系中，由于尘埃区在光通量中的代表性严重不足，因此未解决的估计可能会错过高达40%的恒星总质量。
英文摘要：
(Abridged) We introduce a novel technique to construct spatially resolved maps of stellar mass surface density in galaxies based on optical and near IR imaging. We use optical/NIR colour(s) to infer effective stellar mass-to-light ratios (M/L) at each pixel, which are then multiplied by the surface brightness to obtain the local stellar surface mass density. We build look-up tables to express M/L as a function of colour(s) by marginalizing over a Monte Carlo library of 50,000 stellar population synthesis (SPS) models by Charlot & Bruzual (2007), which include a revised prescription for the TP-AGB stellar evolutionary phase, with a wide range of dust exinctions. In order to extract reliable flux and colour information at any position in the galaxy, we perform a median adaptive smoothing of the images that preserves the highest possible spatial resolution. As the most practical and robust, and hence fiducial method, we express the M/L in the H band as a function of (g-i) and (i-H). Stellar mass maps computed in this way have a typical accuracy of 30 per cent or less at any given pixel, determined from the scatter in the models. We compare maps obtained with our fiducial method with those derived using other combinations of bandpasses and the old BC03 TP-AGB prescription. Finally, we compare total stellar mass estimates obtained by integrating resolved mass maps with those obtained with unresolved photometry. In galaxies with evident dust lanes, unresolved estimates may miss up to 40 per cent of the total stellar mass because dusty regions are strongly under-represented in the luminous fluxes.
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