| Autor: |
Dongfei Jiang, F. S. Liu, Xianzhong Zheng, Hassen M. Yesuf, David C. Koo, S. M. Faber, Yicheng Guo, Anton M. Koekemoer, Weichen Wang, Jerome J. Fang, Guillermo Barro, Meng Jia, Wei Tong, Lu Liu, Xianmin Meng, Dale Kocevski, Elizabeth J. McGrath, Nimish P. Hathi |
| Předmět: |
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| Zdroj: |
Astrophysical Journal; 2/10/2018, Vol. 854 Issue 1, p1-1, 1p |
| Abstrakt: |
We have measured the radial profiles of isophotal ellipticity (ε) and disky/boxy parameter A4 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 (), the SSFGs generally have nearly flat ε and A4 profiles in both edge-on and face-on views, especially at . Moreover, the median A4 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 ε 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 (), both highly inclined SSFGs and LSFGs generally exhibit distinct trends in both ε and A4 profiles, which increase at lower radii, reach maxima, then decrease at larger radii. Such the feature is more prevalent for more massive () galaxies or at lower redshifts (). 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. [ABSTRACT FROM AUTHOR] |
| Databáze: |
Complementary Index |
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