星系标度关系的内禀散射
The Intrinsic Scatter of Galaxy Scaling Relations
摘要：
我们提出了一个简编盘星系标度关系和详细的表征其内在的散射。观测到的标度关系通常以其斜率、截距和散射为特征;然而，这些参数是观测误差和天体物理过程的混合物。我们介绍了一种新的贝叶斯框架计算的内在分散的比例关系，占非线性误差传播和协变的不确定性。贝叶斯固有散射比一阶经典方法获得的结果准确约25%，后者系统地低估了真实的固有散射。基于速度（V23.5）、大小（R23.5）、光度（L23.5）、颜色（g-z）、中心恒星表面密度（Sigma 1）、恒星质量（M*）、动力学质量（Mdyn）、恒星角动量（j*）和动力学角动量（jdyn）的结构星系标度关系被检验以证明贝叶斯形式主义的力量和重要性。我们的分析是基于一个不同的选择超过1000晚型星系的光度计和旋转曲线观测河外巡天汇编深光学光度计和扩展的旋转曲线。我们通过内在正交散点确定每个参数的最紧密关系，发现M*-V23.5，R23.5-j* 和L23.5-jdyn特别紧密。R23.5-L23.5、V23.5-（g-z）和R23.5-jdyn关系的分散性主要是内在的，使它们成为星系形成和演化研究的理想对象。我们的代码来计算贝叶斯固有的任何尺度关系的散布。我们量化的相关性质的许多不确定性的星系标度关系和审查的不确定性的磁盘倾斜校正和它们的影响散射估计。
英文摘要：
We present a compendium of disk galaxy scaling relations and a detailed characterization of their intrinsic scatter. Observed scaling relations are typically characterized by their slope, intercept, and scatter; however, these parameters are a mixture of observational errors and astrophysical processes. We introduce a novel Bayesian framework for computing the intrinsic scatter of scaling relations that accounts for nonlinear error propagation and covariant uncertainties. Bayesian intrinsic scatters are ~25percent more accurate than those obtained with a first-order classical method, which systematically underestimates the true intrinsic scatter. Structural galaxy scaling relations based on velocity (V23.5), size (R23.5), luminosity (L23.5), colour (g-z), central stellar surface density (Sigma1), stellar mass (M*), dynamical mass (Mdyn), stellar angular momentum (j*), and dynamical angular momentum (jdyn), are examined to demonstrate the power and importance of the Bayesian formalism. Our analysis is based on a diverse selection of over 1000 late-type galaxies from the Photometry and Rotation Curve Observations from Extragalactic Surveys compilation with deep optical photometry and extended rotation curves. We determine the tightest relation for each parameter by intrinsic orthogonal scatter, finding M*-V23.5, R23.5-j*, and L23.5-jdyn to be especially tight. The scatter of the R23.5-L23.5, V23.5-(g-z), and R23.5-jdyn relations is mostly intrinsic, making them ideal for galaxy formation and evolutionary studies. Our code to compute the Bayesian intrinsic scatter of any scaling relation is also presented. We quantify the correlated nature of many uncertainties in galaxy scaling relations and scrutinize the uncertain nature of disk inclination corrections and their effect on scatter estimates.
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