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arXiv 1507.08669astro-ph.GA
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RESOLVE测量光度学和光度气体分馏技术的体积限制校准

RESOLVE Survey Photometry and Volume-limited Calibration of the Photometric Gas Fractions Technique

Kathleen D. Eckert, Sheila J. Kannappan, David V. Stark, Amanda J. Moffett, Mark A. Norris, Elaine M. Snyder, Erik A. Hoversten

备注：
(29 pages, 15 figures, accepted for publication in ApJ; a data table is available at http://resolve.astro.unc.edu/data/resolve_phot_dr1.txt and a code for predicting individual galaxy G/S probability distributions (pred_loggs_dist.pro) is available at https://github.com/keckert7/codes
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摘要：

我们为RESOLVE巡天提供了定制处理的紫外、光学和近红外测光，这是对附近宇宙两个子体积（RESOLVE-A和-B）内恒星、气体和动力学质量的体积有限普查，完成了重子质量~10^9.1-9.3 Msun。与标准流水线测光（例如，SDSS），我们的光度法使用最佳的背景减除，避免抑制颜色梯度，并包括系统误差。通过这些改进，我们测量到更亮的星等，更大的半径，更蓝的颜色，以及红色序列周围散射的实际增加。结合恒星质量从我们的测光与RESOLVE-A HI质量普查，我们创建的光度气体分数（PGF）技术，预测气体与恒星的质量比（G/S）从星系的颜色和可选的附加参数的体积有限的校准。我们分析了G/S颜色残差与潜在的第三个参数，发现轴比是最好的独立和物理意义的第三个参数。我们定义了一个“修改后的颜色”，从平面适合G/S作为一个功能的颜色和轴比。在完整的星系群中，G/S偏差的上限线性和平面拟合。因此，我们对整个PGF概率密度场进行了建模，从而能够对单个星系的上限进行迭代统计建模，并预测完整的G/S概率分布，其中红色具有双组分结构。我们使用的RESOLVE-B 21厘米普查测试几个PGF校准，发现最系统的下或高估气体质量，但全概率密度法表现良好。

英文摘要：

We present custom-processed UV, optical, and near-IR photometry for the RESOLVE survey, a volume-limited census of stellar, gas, and dynamical mass within two subvolumes of the nearby universe (RESOLVE-A and -B), complete down to baryonic mass ~10^9.1-9.3 Msun. In contrast to standard pipeline photometry (e.g., SDSS), our photometry uses optimal background subtraction, avoids suppressing color gradients, and includes systematic errors. With these improvements, we measure brighter magnitudes, larger radii, bluer colors, and a real increase in scatter around the red sequence. Combining stellar masses from our photometry with the RESOLVE-A HI mass census, we create volume-limited calibrations of the photometric gas fractions (PGF) technique, which predicts gas-to-stellar mass ratios (G/S) from galaxy colors and optional additional parameters. We analyze G/S-color residuals vs. potential third parameters, finding that axial ratio is the best independent and physically meaningful third parameter. We define a "modified color" from planar fits to G/S as a function of both color and axial ratio. In the complete galaxy population, upper limits on G/S bias linear and planar fits. We therefore model the entire PGF probability density field, enabling iterative statistical modeling of upper limits and prediction of full G/S probability distributions for individual galaxies, with two-component structure for red colors. We use the RESOLVE-B 21cm census to test several PGF calibrations, finding that most systematically under- or overestimate gas masses, but the full probability density method performs well.

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