The fundamental plane of EDisCS galaxies - The effect of size evolution
The fundamental plane of EDisCS galaxies - The effect of size evolution
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EDisCS 星系的基本平面 - 尺寸演化的影响
DOI：
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发表时间：
2010
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通讯作者：
D. Zaritsky
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文献类型：
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作者：
R. Saglia;P. Sánchez;P. Sánchez;Ralf Bender;L. Simard;V. Desai;A. Aragón;B. Milvang;C. Halliday;P. Jablonka;P. Jablonka;S. Noll;B. Poggianti;D. Clowe;G. Lucia;R. Pelló;G. Rudnick;T. Valentinuzzi;S. D. M. White;D. Zaritsky
我们使用ESO远距星系团巡天（EDisCS）数据集研究了光谱早型星系在星系团、星系群和红移达0.9的领域中的演化。我们测量了154个星系团和68个场星系的结构参数（圆化半光度半径Re、表面亮度Ie和速度色散σ）。平均而言，我们获得了10%的Re精度，0.1dex的logIe，和10%的σ。我们的样品中的20%的星系团和10%的场光谱早型星系的I带的大小在一个1弧秒半径的光圈，作为微弱的I1 = 22。我们研究的基本平面（FP）的零点的演变，并确认在文献中的结果，但现在也为低集群速度分散制度。从表面上看，团簇中的质光比变化为Δ log M/LB =（−0.54 ± 0.01）z =（−1.61 ± 0.01）log（1 + z），与它们的速度色散无关。场星系的演化更强（Δ log M/LB =（−0.76 ± 0.01）z =（−2.27 ± 0.03）log（1 + z））。如果对不完全性作修正，则得到一个稍微温和的演化。在FP的旋转与红移检测到低的统计意义。α和β FP系数随着红移而减小，或者等效地，FP残差与星系质量相关，并在低质量时逐渐变负。在z ≥ 0.7的星系团中，这种效应是可见的，而在较低的红移z ≥ 0.5的场星系中，这种效应是可见的。我们调查我们的星系样本的大小演变。与以前的结果一致，我们发现具有动力学质量或恒星质量的星系的半光度半径
We study the evolution of spectral early-type galaxies in clusters, groups, and the field up to redshift 0.9 using the ESO Distant Cluster Survey (EDisCS) dataset. We measure structural parameters (circularized half-luminosity radii Re, surface brightness Ie, and velocity dispersions σ )f or 154 cluster and 68 field galaxies. On average, we achieve precisions of 10% in Re ,0 .1 dex in logIe, and 10% in σ .W e sample≈20% of cluster and ≈10% of field spectral early-type galaxies to an I band magnitude in a 1 arcsec radius aperture as faint as I1 = 22. We study the evolution of the zero point of the fundamental plane (FP) and confirm results in the literature, but now also for the low cluster velocity dispersion regime. Taken at face value, the mass-to-light ratio varies as Δ log M/LB = (−0.54 ± 0.01)z = (−1.61 ± 0.01) log(1 + z) in clusters, independent of their velocity dispersion. The evolution is stronger (Δ log M/LB = (−0.76 ± 0.01)z = (−2.27 ± 0.03) log(1 + z)) for field galaxies. A somewhat milder evolution is derived if a correction for incompleteness is applied. A rotation in the FP with redshift is detected with low statistical significance. The α and β FP coefficients decrease with redshift, or, equivalently, the FP residuals correlate with galaxy mass and become progressively negative at low masses. The effect is visible at z ≥ 0.7 for cluster galaxies and at lower redshifts z ≥ 0.5 for field galaxies. We investigate the size evolution of our galaxy sample. In agreement with previous results, we find that the half-luminosity radius for a galaxy with a dynamical or stellar mass