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Abell S1063、MACS J0416 .1-2403和MACS J1149 .5+2223中早型星系的柯门迪关系作为波长的函数

The Kormendy relation of early-type galaxies as a function of wavelength in Abell S1063, MACS J0416.1-2403, and MACS J1149.5+2223

L. Tortorelli, A. Mercurio, G. Granata, P. Rosati, C. Grillo, M. Nonino, A. Acebron, G. Angora, P. Bergamini, G. B. Caminha, U. Meštrić, E. Vanzella

备注：
Accepted for publication in A&A as letter to the editor, 6 pages, 1 figure, 1 table
发表信息：
A&A 671, L9 (2023)
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摘要：

的波长依赖性的Kormendy关系（KR）的特点是在低红移，但在中间的红移研究不足。KR提供了早期星系（ETG）人口演化的信息。因此，通过研究它，我们可以揭示这些物体的组装过程和它们的尺寸演化。由于不同红移的研究通常是在不同的静止系波段进行的，因此研究KR是否依赖于波长是很重要的。了解这种依赖关系是正确解释我们从这些研究中得出的结论的基础。我们分析了三个哈勃前沿场星系团Abell S1063（z = 0.348），MACSJ0416.1-2403（z = 0.396）和MACS J1149.5+2223（z = 0.542）的KR随波长的变化。这是第一次在中等红移的波长范围内对ETG的KR进行了一致的探索。我们利用非常深的HST测光，从观察到的B-波段的H-波段，和MUSE积分场光谱。我们通过一个新开发的Python包称为morphofit，我们在以前的工作中进行的结构参数估计，提高。通过在星系团ETG上的使用，我们发现在所有三个星系团中，KR斜率随着从光学到近红外（NIR）波段的波长而平滑增加，由于ETG的被动老化，在红移较低的情况下，拦截变得较弱。恒星星族。斜率的趋势是一致的，在较低的红移与以前的研究结果。斜率随波长的增加意味着相对于光学状态，在NIR中较小的ETG比较大的ETG更集中。由于不同的波段探测星系中不同的恒星星族，斜率的增加也意味着较小的ETG相对于较大的ETG具有更强的内部梯度。

英文摘要：

The wavelength dependence of the Kormendy relation (KR) is well characterised at low redshift but poorly studied at intermediate redshifts. The KR provides information on the evolution of the population of early-type galaxies (ETGs). Therefore, by studying it, we may shed light on the assembly processes of these objects and their size evolution. As studies at different redshifts are generally conducted in different rest-frame wavebands, it is important to investigate whether the KR is dependent on wavelength. Knowledge of such a dependence is fundamental to correctly interpreting the conclusions we might draw from these studies. We analyse the KRs of the three Hubble Frontier Fields clusters, Abell S1063 (z = 0.348), MACSJ0416.1-2403 (z = 0.396), and MACS J1149.5+2223 (z = 0.542), as a function of wavelength. This is the first time the KR of ETGs has been explored consistently over such a large range of wavelengths at intermediate redshifts. We exploit very deep HST photometry, ranging from the observed B-band to the H-band, and MUSE integral field spectroscopy. We improve the structural parameter estimation we performed in a previous work by means of a newly developed Python package called morphofit. With its use on cluster ETGs, we find that the KR slopes increase smoothly with wavelength from the optical to the near-infrared (NIR) bands in all three clusters, with the intercepts becoming fainter at lower redshifts due to the passive ageing of the ETG stellar populations. The slope trend is consistent with previous findings at lower redshifts. The slope increase with wavelength implies that smaller ETGs are more centrally concentrated than larger ETGs in the NIR with respect to the optical regime. As different bands probe different stellar populations in galaxies, the slope increase also implies that smaller ETGs have stronger internal gradients with respect to larger ETGs.

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