Measuring Scaling Relations: Fitting Technique Matters

Bryanne McDonough, Olivia Curtis and Tereasa G. Brainerd
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Abstract

Scaling relationships, both integrated and spatially resolved, arise owing to the physical processes that govern galaxy evolution and are frequently measured in both observed and simulated data. However, the accuracy and comparability of these measurements are hindered by various differences between studies such as spatial resolution, sample selection criteria, and fitting technique. In this Letter, we compare variations of standard least-squares techniques to the ridge line method for identifying spatially resolved scaling relations (Σ*−ΣSFR, Σ*−Σgas, and Σgas−ΣSFR) for TNG100 galaxies. We find that using the ridge line technique to fit these scaling relations with a double linear function (in logarithmic space) results in significantly better fits than fitting with ordinary least squares. We further illustrate the utility of the ridge line technique with an investigation into the dependence of resolved star formation main-sequence (rSFMS) measurements on spatial resolution and smoothing scale. Specifically, we find that the slope of the rSFMS at low Σ* is independent (within 2σ) of spatial resolution and smoothing scale. Finally, we discuss the need for a consistent reanalysis of resolved scaling relations in the literature and physically motivate adoption of the ridge line technique over other fitting methods.
测量尺度关系:拟合技术问题
尺度关系,无论是集成的还是空间解决的,都是由于控制星系演化的物理过程而产生的,并且经常在观测和模拟数据中进行测量。然而,这些测量的准确性和可比性受到研究之间的各种差异的阻碍,如空间分辨率、样本选择标准和拟合技术。在这篇文章中,我们比较了标准最小二乘技术与岭线方法的变化,用于识别TNG100星系的空间分辨尺度关系(Σ*−ΣSFR, Σ*−Σgas和Σgas−ΣSFR)。我们发现使用脊线技术用双线性函数(在对数空间中)拟合这些比例关系的结果明显优于普通最小二乘拟合。我们进一步说明了山脊线技术的实用性,研究了分辨恒星形成主序(rSFMS)测量对空间分辨率和平滑尺度的依赖。具体来说,我们发现在Σ*低的位置,rSFMS的斜率与空间分辨率和平滑尺度无关(在2σ范围内)。最后,我们讨论了对文献中已解决的尺度关系进行一致再分析的必要性,并在物理上激励采用脊线技术而不是其他拟合方法。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
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