论文标题
自$ z = 1 $以来，恒星大小的质量大小关系的演变
The evolution of the stellar mass-size relation of bulges and disks since $z = 1$
论文作者
论文摘要
我们探讨了不同形态类型的星系的恒星质量关系的演变，特别是凸起和磁盘成分。 We use a sample of $\sim35,000$ galaxies within a redshift range $0 < z < 1$, and stellar mass $\log_{10}(\mathrm{M}_*/\mathrm{M}_\odot) \geq 9.5$ volume-limited sample drawn from the combined DEVILS and HST-COSMOS region for which we presented a morphological classification在Paper-I中的双组分（BD），Pure-Disk（PD），椭圆形（E）和紧凑型（C）的子类中，以及在纸张中的结构分解为磁盘（d），散射凸起（DB）和紧凑型凸起（CB）。我们发现，与磁盘相比，椭圆形和凸起遵循更陡峭的$ m _* - r_e $关系，可能表明了不同的进化机制。椭圆机和磁盘结构始终遵循$ \ sim0.5 $和$ \ sim0.3 $的不变斜率。我们量化了磁盘遵循红移独立的$ m _* - r_e $斜率，无论存在或不存在凸起组件（即BD或PD），这表明所有磁盘都具有相似的来源和进化途径。由于$ z = 1 $ compact-bulges存在着陡峭的关系，而不遵循ES的关系，而散布式式荷尔巴斯则经历了适度的变平。总体而言，我们发现$ m _* - r_e $在最后一个$ \ sim8 $ gyr中的关系几乎没有变化，尽管尽管恒星形成，质量进化，形态过渡和合并正在持续下降，但进化仍沿着$ m _* - r_e $ trails移动星系。这似乎与内而外的生长和进化图是一致的，在恒星质量中，星系的大小在大小上生长。此外，至少在$ z <1 $中，次要合并可能是ES增长的原因。
We explore the evolution of the stellar mass-size relation of galaxies of different morphological types and specifically bulge and disk components. We use a sample of $\sim35,000$ galaxies within a redshift range $0 < z < 1$, and stellar mass $\log_{10}(\mathrm{M}_*/\mathrm{M}_\odot) \geq 9.5$ volume-limited sample drawn from the combined DEVILS and HST-COSMOS region for which we presented a morphological classification into sub-classes of double-component (BD), pure-disk (pD), elliptical (E), and compact (C) in Paper-I and a structural decomposition into disk (D), diffuse bulge (dB), and compact bulge (cB) in Paper-II. We find that compared to disks, ellipticals and bulges follow steeper $M_*-R_e$ relations, likely indicating distinct evolutionary mechanisms. Ellipticals and disk structures follow consistently unchanged slopes of $\sim0.5$ and $\sim0.3$, respectively, at all redshifts. We quantify that disks follow a redshift independent $M_*-R_e$ slope regardless of the presence or absence of a bulge component (i.e., BD or pD) suggesting a similar origin and evolutionary pathway for all disks. Since $z = 1$ compact-bulges present a steepening relation which do not follow that of Es whilst diffuse-bulges experience a modest flattening. Overall, we find a close-to-no variation in the $M_*-R_e$ relations over the last $\sim8$ Gyr suggesting that despite ongoing although declining star-formation, mass evolution, morphological transitions and mergers, evolution moves galaxies along their $M_*-R_e$ trails. This seems to be consistent with an inside-out growth and evolution picture in which galaxies grow in size as they do in stellar mass. Besides, minor mergers are likely to be responsible for the growth of Es, at least in $z < 1$.
