论文标题
清除：使用H $α$排放线图的星系中空间解决星形的演变
CLEAR: The Evolution of Spatially Resolved Star Formation in Galaxies between $0.5\lesssim z \lesssim1.7$ using H$α$ Emission Line Maps
论文作者
论文摘要
使用恒星形成星系的空间解析的H-α发射线图，我们研究了红移范围内星系组件中梯度的演变（$ 0.5 <z <z <1.7 $）。我们的$ z \ sim0.5 $测量来自深哈勃太空望远镜WFC3 G102 G102 G102 GRISM光谱作为Reionization（Clear）实验时烛台Lyman-Alpha发射的一部分获得的一部分。 For star-forming galaxies with Log$(M_{*}/\mathrm{M}_{\odot})\geqslant8.96$, the mean H-alpha effective radius is $1.2\pm0.1$ times larger than that of the stellar continuum, implying inside-out growth via star formation.该测量值在$1σ$之内与分别从3D-HST和KMOS-3D调查中测量的$ z \ sim1 $和$ z \ sim1.7 $相同，这意味着没有红移的演变。但是，我们观察到在1千帕克（$σ_\ mathrm {1kpc} $）内的恒星质量表面密度中的红移演化。 $ z \ sim0.5 $的星形星系，恒星质量为log $（m _ {*}/\ mathrm {m} _ {\ odot}）= 9.5 $具有$σ__\ mathrm {1kpc} $的比率为$σ__\ mathrm {1kpc} $ pm pm pm pm pm pm pm youm pm youm pm youm pm youm pm youm pm youm pm youm pm youm pm youm pm youm pm youm pm youm pm youm to y is pm youm to is pm youm to y is 2 is 2 $ z \ sim1 $星系。 $σ_{1 \ Mathrm {kpc，h}α} $/$σ_{1 \ Mathrm {kpc，cont}} $降低了更高的恒星质量。 $σ_{1 \ mathrm {kpc，h}α} $/$/$/$σ_{1 \ MATHRM {kpc，cont}} $ vers恒星质量的大部分红移进化，源于log（$σ_{1 \ mathrm {kpc，kpc，kpc，h} $） log（$σ_{1 \ Mathrm {kpc，cont}} $）从$ z \ sim 1 $至0.5（以固定的log $ $ $（m _ {*}/\ mathrm {m} _ {\ odot} _ {\ odot}）的固定恒星质量（m _ {*}/\ mathrm {\ odot}）= 9.5 $）。通过将我们的结果与TNG50宇宙学磁动力学模拟进行比较，我们排除了尘埃作为这种进化的驱动力。我们的结果与内外增长后的内外淬火一致，前者从$ z \ sim1 $到$ z \ s \ sim0.5 $驱动了$σ_{1 \ mathrm {kpc，h}α} $的显着下降。
Using spatially resolved H-alpha emission line maps of star-forming galaxies, we study the evolution of gradients in galaxy assembly over a wide range in redshift ($0.5<z<1.7$). Our $z\sim0.5$ measurements come from deep Hubble Space Telescope WFC3 G102 grism spectroscopy obtained as part of the CANDELS Lyman-alpha Emission at Reionization (CLEAR) Experiment. For star-forming galaxies with Log$(M_{*}/\mathrm{M}_{\odot})\geqslant8.96$, the mean H-alpha effective radius is $1.2\pm0.1$ times larger than that of the stellar continuum, implying inside-out growth via star formation. This measurement agrees within $1σ$ with those measured at $z\sim1$ and $z\sim1.7$ from the 3D-HST and KMOS-3D surveys respectively, implying no redshift evolution. However, we observe redshift evolution in the stellar mass surface density within 1 kiloparsec ($Σ_\mathrm{1kpc}$). Star-forming galaxies at $z\sim0.5$ with a stellar mass of Log$(M_{*}/\mathrm{M}_{\odot})=9.5$ have a ratio of $Σ_\mathrm{1kpc}$ in H-alpha relative to their stellar continuum that is lower by $(19\pm2)\%$ compared to $z\sim1$ galaxies. $Σ_{1\mathrm{kpc, H}α}$/$Σ_{1\mathrm{kpc,Cont}}$ decreases towards higher stellar masses. The majority of the redshift evolution in $Σ_{1\mathrm{kpc,H}α}$/$Σ_{1\mathrm{kpc,Cont}}$ versus stellar mass stems from the fact that Log($Σ_{1\mathrm{kpc, H}α}$) declines twice as much as Log($Σ_{1\mathrm{kpc, Cont}}$) from $z\sim 1$ to 0.5 (at a fixed stellar mass of Log$(M_{*}/\mathrm{M}_{\odot})=9.5$). By comparing our results to the TNG50 cosmological magneto-hydrodynamical simulation, we rule out dust as the driver of this evolution. Our results are consistent with inside-out quenching following in the wake of inside-out growth, the former of which drives the significant drop in $Σ_{1\mathrm{kpc, H}α}$ from $z\sim1$ to $z\sim0.5$.
