Effect of Local Environment on Galaxy Quenching and Morphology at z < 1

我们利用Subaru Hyper Suprime-Cam（HSC）成像，覆盖100 deg^2，测量z < 1的约150万个星系的结构特性。我们使用模拟星系仔细校准了我们的测量结果，以解释各种系统偏差。我们使用模拟星系进行的测试表明，我们获得的i< 24.5等星系的尺寸精度为5%（或更高）。作为科学的证明，PI利用尺寸测量结果在恒星质量的广泛范围内稳健地确定了尺寸-质量关系，并表明该关系更好地表征为双幂函数：该关系在枢轴质量上方的斜率更陡。 我们的结果与星载观测的结果非常一致，特别是对于低质量星系，这强烈地表明我们的尺寸测量是稳健的，而不是由系统偏差驱动的，比以前的深空观测更大的大质量星系样本使我们能够推导出更严格的约束对大多数大质量星系的尺寸质量关系。本文的结果弥补了局域宇宙（z~0）和高红移工作之间的差距。 PI已将题为“Hyper Suprime-Cam Subaru Strategic Survey：A Mass-Dependent Slope of the Galaxy Size-Mass Relation at z<1”的出版物提交给《天体物理学杂志》。该手稿已被接受出版。我们还向HSC协作提供了我们的目录。

We utilised the Subaru Hyper Suprime-Cam (HSC) imaging, covering 100 deg^2, to measure structural properties of ~1.5 million galaxies at z < 1. We carefully calibrated our measurements using simulated galaxies to account for various systematic biases. Our test using the simulated galaxies showed that we obtain sizes for galaxies with i< 24.5 mag with 5% accuracy (or better).As a demonstration of science, PI has utilised the size measurements to robustly determine the size-mass relation over the broad range in stellar mass and show that the relations for are better characterised a double-power function: the relation is steeper slope above the pivot mass. Our result from the HSC are in excellent agreements with those from the spaced-based observations, particularly for low-mass galaxies, strongly suggesting that our size measurements are robust and not driven by a systematic bias.The larger sample of massive galaxies than the previous deep surveys enable us to derive the tighter constraint on the size-mass relation for most massive galaxies. The results presented here bridge the gap between the local Universe (z~0) and the high redshift works. PI has submitted the publication with the title “Hyper Suprime-Cam Subaru Strategic Survey: A Mass-Dependent Slope of the Galaxy Size-Mass Relation at z<1” to The Astrophysical Journal. The manuscript has been accepted for publication. We have also made our catalog available to HSC Collaboration.