The abundance of massive compact galaxies at 1.0<z<3.0 in 3D-HST/CANDELS

作     者：Shi-Ying Lu Yi-Zhou Gu Guan-Wen Fang Qi-Rong Yuan 

作者机构：Department of Physics and Institute of Theoretical Physics Nanjing Normal University Nanjing 210023 China Institute for Astronomy and History of Science and Technology Dali UniversityDali 671003 China 

出 版 物：《Research in Astronomy and Astrophysics》 (天文和天体物理学研究（英文版）)

年 卷 期：2019年第19卷第10期

页      面：109-120页

核心收录：

学科分类：0709[理学-地质学] 07[理学] 0708[理学-地球物理学] 0825[工学-航空宇航科学与技术] 0704[理学-天文学] 

基　　金：the 3D-HST Treasury Program (GO 12177 and 12328) with the NASA/ESA HSTsupported by the National Natural Science Foundation of China (Nos. 11673004, 11873032 and 11433005) by the Research Fund for the Doctoral Program of Higher Education of China (No. 20133207110006) he support from Yunnan young and middleaged academic and technical leaders reserve talent program (No. 201905C160039) 

主　　题：galaxies high-redshift-galaxies massive-compact-galaxies evolution-galaxies 

摘      要：Based on a large sample of massive(M* 1010 M⊙) compact galaxies at 1.0 z 3.0 in five 3 D-HST/CANDELS fields, we quantify the fractional abundance and comoving number density of massive compact galaxies as a function of redshift. The samples of compact quiescent galaxies(cQGs) and compact star-forming galaxies(cSFGs) are constructed by various selection criteria of compact galaxies in the literature, and the effect of compactness definition on abundance estimate has proven to be remarkable,particularly for the cQGs and cSFGs at high redshifts. Regardless of the compactness criteria adopted,their overall redshift evolutions of fractional abundance and number density are found to be rather *** samples of the cQGs exhibit a sustained increase in number density from z ~ 3 to 2 and a plateau at 1 z 2. For massive cSFGs, a plateau in the number density at 2 z 3 can be found, as well as a continuous drop from z ~ 2 to 1. The evolutionary trends of the cQG and cSFG abundances support the scenario that the cSFGs at z≥ 2 may have been rapidly quenched into quiescent phase via violent dissipational processes, such as major merger and disk instabilities. The rarity of the cSFGs at lower redshifts(z 1) can be interpreted by the decrease of gas reservoirs in dark matter halos and the consequent low efficiency of gas-rich dissipation.