The Isophotal Structure of Star-forming Galaxies at 0.5 < z < 1.8 in CANDELS: Implications for the Evolution of Galaxy Structure - Archive ouverte HAL Access content directly
Journal Articles The Astrophysical Journal Year : 2018

The Isophotal Structure of Star-forming Galaxies at 0.5 < z < 1.8 in CANDELS: Implications for the Evolution of Galaxy Structure

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Dongfei Jiang
  • Function : Author
F. S. Liu
  • Function : Author
Xianzhong Zheng
  • Function : Author
Hassen M. Yesuf
  • Function : Author
David C. Koo
  • Function : Author
S. M. Faber
  • Function : Author
Yicheng Guo
  • Function : Author
Anton M. Koekemoer
  • Function : Author
Weichen Wang
  • Function : Author
Jerome J. Fang
  • Function : Author
Guillermo Barro
  • Function : Author
Meng Jia
  • Function : Author
Wei Tong
  • Function : Author
Lu Liu
  • Function : Author
Xianmin Meng
  • Function : Author
Dale Kocevski
  • Function : Author
Elizabeth J. Mcgrath
  • Function : Author

Abstract

We have measured the radial profiles of isophotal ellipticity (ɛ) and disky/boxy parameter A 4 out to radii of about three times the semimajor axes for ∼4600 star-forming galaxies (SFGs) between redshift 0.5 and 1.8 in the CANDELS/GOODS-S and UDS fields. Based on the average size-mass relation in each redshift bin, we divide our galaxies at a given mass into Small SFGs (SSFGs; smaller than the average) and Large SFGs (LSFGs; larger than the average). We show that, at low masses ({M}* < {10}10{M}), the SSFGs generally have nearly flat ɛ and A 4 profiles in both edge-on and face-on views, especially at z> 1. Moreover, the median A 4 values at all radii are almost zero. In contrast, the highly inclined low-mass LSFGs in the same mass-redshift bins generally have monotonically increasing ɛ profiles with radius and disky feature dominated in the intermediate regions. These findings imply that at these redshifts, the low-mass SSFGs are not disk-like, whereas the low-mass LSFGs likely harbour disk-like components flattened by significant rotations. At high masses ({M}* > {10}10{M}), both highly inclined SSFGs and LSFGs generally exhibit distinct trends in both ɛ and A 4 profiles, which increase at lower radii, reach maxima, then decrease at larger radii. Such the feature is more prevalent for more massive ({M}* > {10}10.5{M}) galaxies or at lower redshifts (z< 1.4). This feature can be simply explained if galaxies possess all three components: central bulges, disks in the intermediate regions, and halo-like stellar components in the outskirts.

Dates and versions

insu-03666279 , version 1 (12-05-2022)

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Dongfei Jiang, F. S. Liu, Xianzhong Zheng, Hassen M. Yesuf, David C. Koo, et al.. The Isophotal Structure of Star-forming Galaxies at 0.5 < z < 1.8 in CANDELS: Implications for the Evolution of Galaxy Structure. The Astrophysical Journal, 2018, 854, ⟨10.3847/1538-4357/aaa5ad⟩. ⟨insu-03666279⟩
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