论文标题
Z〜2的大型星系的结构演化
Structural evolution in massive galaxies at z~2
论文作者
论文摘要
我们在恒星质量选择的85个巨大的样本（$ M_ \ Mathrm {star}> 10^{11}} 〜M_ \ odot $）中，我们提出0.2 arcsec-solutional atacama大毫米/亚毫米/亚毫米阵列观测值，以870 $ $ m $ m的速度观测和商品-S。我们测量了62个巨大的SFG的剩余框架远红外（FIR）发射的有效半径。它们分布在FIR大小的宽范围内，从$ r_ \ mathrm {e，fir} = $ 0.4 kpc至$ r_ \ m r_ \ mathrm {e，fir} = $ 6 kpc。 FIR排放的有效半径比光学排放的有效半径较小2.3 $^{+1.9} _ { - 1.0} $，而比半大radius小的1.9 $^{+1.9} _ { - 1.0} $小。即使考虑到潜在的扩展组件，FIR尺寸也会变化约10％。通过将FIR的空间分布和光学发射的空间分布相结合，我们研究星系如何在1 kpc（$ M_ \ Mathrm {1KPC} $的半径内改变光学发射的有效半径和恒星质量。如果当前的恒星形成活性及其空间分布，则紧凑的星状爆炸将大部分巨大的SFG置于Z〜2的静态星系（QGS）的质量尺寸关系上。我们还发现，在300 MYR中，约38％的大型SFG可以达到$ M_ \ MathRM {1KPC} = 10^{10.5} 〜M_ \ odot $的中央质量，该= 10^{10.5} 〜M_ \ odot $，它围绕大型SFGS和QGS之间的边界。这些结果表明，外部转换方案，其中形成了更扩展磁盘的中心，可能是通过耗散盘中流入的。 ALMA 870 $μ$ M和JWST 3-4 $μ$ m的同步观察结果将明确验证这种情况。
We present 0.2arcsec-resolution Atacama Large Millimeter/submillimeter Array observations at 870 $μ$m in a stellar mass-selected sample of 85 massive ($M_\mathrm{star}>10^{11}~M_\odot$) star-forming galaxies (SFGs) at z=1.9-2.6 in the 3D-HST/CANDELS fields of UDS and GOODS-S. We measure the effective radius of the rest-frame far-infrared (FIR) emission for 62 massive SFGs. They are distributed over wide ranges of FIR size from $R_\mathrm{e,FIR}=$0.4 kpc to $R_\mathrm{e,FIR}=$6 kpc. The effective radius of the FIR emission is smaller by a factor of 2.3$^{+1.9}_{-1.0}$ than the effective radius of the optical emission and by a factor of 1.9$^{+1.9}_{-1.0}$ smaller than the half-mass radius. Even with taking into account potential extended components, the FIR size would change by ~10%. By combining the spatial distributions of the FIR and optical emission, we investigate how galaxies change the effective radius of the optical emission and the stellar mass within a radius of 1 kpc, $M_\mathrm{1kpc}$. The compact starburst puts most of massive SFGs on the mass--size relation for quiescent galaxies (QGs) at z~2 within 300 Myr if the current star formation activity and its spatial distribution are maintained. We also find that within 300 Myr, ~38% of massive SFGs can reach the central mass of $M_\mathrm{1kpc}=10^{10.5}~M_\odot$, which is around the boundary between massive SFGs and QGs. These results suggest an outside-in transformation scenario in which a dense core is formed at the center of a more extended disk, likely via dissipative in-disk inflows. Synchronized observations at ALMA 870 $μ$m and JWST 3-4 $μ$m will explicitly verify this scenario.
