在SHARDS巡天中自$z=0.6$以来S0星系反截断恒星轮廓的演化：I -样品和方法
Evolution of the anti-truncated stellar profiles of S0 galaxies since $z=0.6$ in the SHARDS survey: I - Sample and Methods
摘要：
关于S 0-E/S 0星系结构起源的争论可能是由于难以比较不同深度的表面亮度剖面、光度校正和PSF效应（几乎总是被忽略）。我们的目标是量化在0.2<z<0.6的S 0星系样本中III型（反截断）盘的性质。在本文中，我们提出了样本选择和详细描述的方法来鲁棒地跟踪结构的边缘和校正PSF效应。我们选取了GOODS-N场中150个0.2<z<0.6的静止星系样本进行分类。我们对44个S 0-E/S 0星系进行了定量结构分析。我们校正了它们的表面亮度曲线的PSF失真，并分析了当不应用PSF校正时结构和光度参数的偏差。此外，我们还开发了Elbow，这是一种自动统计方法，用于确定可能的断裂是否显著-或不显著-及其类型，并将其公开提供。我们在0.2<z<0.6的范围内发现了14个反截短的S 0-E/S 0星系（约占最终样本的30%）。这个分数与当地宇宙中报道的相似。在我们的样本中，在PSF未校正的配置文件中观察到的III型断裂中约有25%是伪影，并且它们的配置文件在PSF校正后变成I型。PSF效应也软化了II型轮廓。我们发现我们样本的I型S 0和E/S 0星系的轮廓与III型星系的内部轮廓相一致，而与外部轮廓相反。我们已经获得了第一个强大的和可靠的样本的14个反截断的S 0-E/S 0星系超出本地宇宙，在范围0.2<z<0.6。即使在HST/ACS图像的窄PSF的情况下，PSF效应也会显着影响星系盘表面亮度轮廓的形状，因此未来的研究应该努力纠正它们。
英文摘要：
The controversy about the origin of the structure of S0--E/S0 galaxies may be due to the difficulty of comparing surface brightness profiles with different depths, photometric corrections and PSF effects (almost always ignored). We aim to quantify the properties of Type-III (anti-truncated) discs in a sample of S0 galaxies at 0.2<z<0.6. In this paper, we present the sample selection and describe in detail the methods to robustly trace the structure in their outskirts and correct for PSF effects. We have selected and classified a sample of 150 quiescent galaxies at 0.2<z<0.6 in the GOODS-N field. We perform a quantitative structural analysis of 44 S0-E/S0 galaxies. We corrected their surface brightness profiles for PSF distortions and analysed the biases in the structural and photometric parameters when the PSF correction is not applied. Additionally, we have developed Elbow, an automatic statistical method to determine whether a possible break is significant - or not - and its type and made it publicly available. We found 14 anti-truncated S0-E/S0 galaxies in the range 0.2<z<0.6 (~30% of the final sample). This fraction is similar to the those reported in the local Universe. In our sample, ~25% of the Type-III breaks observed in PSF-uncorrected profiles are artifacts, and their profiles turn into a Type I after PSF correction. PSF effects also soften Type-II profiles. We found that the profiles of Type-I S0 and E/S0 galaxies of our sample are compatible with the inner profiles of the Type-III, in contrast with the outer profiles. We have obtained the first robust and reliable sample of 14 anti-truncated S0--E/S0 galaxies beyond the local Universe, in the range 0.2<z<0.6. PSF effects significantly affect the shape of the surface brightness profiles in galaxy discs even in the case of the narrow PSF of HST/ACS images, so future studies on the subject should make an effort to correct them.
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