恒星形成对星系沿大小质量关系生长的调节作用，在0.7 < z < 2.7的KMOS $^{3D}$星系中H $α$追踪
The regulation of galaxy growth along the size-mass relation by star-formation, as traced by H$α$ in KMOS$^{3D}$ galaxies at 0.7 < z < 2.7
摘要：
本文给出了KMOS 3D巡天中281个恒星形成星系的H $α$发射跟踪恒星形成测量的0.7 < z < 2.7的半光尺寸。尺寸通过拟合2D指数盘模型得出，自举误差平均为20%。H $α$的平均尺寸是恒星连续体的1.19（1.26）倍，由于径向尘埃梯度，通过恒星形成的恒星尺寸增长的上限只有43%的内在散射。在固定的连续谱尺寸下，H $α$尺寸与恒星质量、恒星形成速率、红移或形态没有剩余趋势。唯一显著的残留趋势是在固定的连续遮蔽下，H $α$被灰尘过度遮蔽。在固定恒星质量的连续谱尺寸的散射很可能是由晕旋转参数的散射驱动的。H $α$尺寸与连续体尺寸之比的稳定性表明，在很宽的物理条件和宇宙时间范围内，晕旋和角动量向盘的转移具有高度的稳定性。这可能需要通过反馈过程进行地方监管。我们的研究结果的含义，因为我们证明使用一个玩具模型，是我们的上限恒星形成驱动的增长是足够的恒星形成星系大约沿着观察到的大小质量关系，一致的星系的大小增长在恒定的累积共同移动数密度。为了解释观测到的恒星形成盘星系的大小-质量关系的演化，可能需要其他过程，例如致密星系的优先淬火或星系合并。
英文摘要：
We present half-light sizes measured from H$α$ emission tracing star-formation in 281 star-forming galaxies from the KMOS3D survey at 0.7 < z < 2.7. Sizes are derived by fitting 2D exponential disk models, with bootstrap errors averaging 20%. H$α$ sizes are a median (mean) of 1.19 (1.26) times larger than those of the stellar continuum, which due to radial dust gradients places an upper limit on the growth in stellar size via star formation, with just 43% intrinsic scatter. At fixed continuum size the H$α$ size shows no residual trend with stellar mass, star formation rate, redshift or morphology. The only significant residual trend is with the excess obscuration of H$α$ by dust, at fixed continuum obscuration. The scatter in continuum size at fixed stellar mass is likely driven by the scatter in halo spin parameters. The stability of the ratio of H$α$ size to continuum size demonstrates a high degree of stability in halo spin and in the transfer of angular momentum to the disk over a wide range of physical conditions and cosmic time. This may require local regulation by feedback processes. The implication of our results, as we demonstrate using a toy model, is that our upper limit on star-formation driven growth is sufficient only to evolve star-forming galaxies approximately along the observed size-mass relation, consistent with the size growth of galaxies at constant cumulative co-moving number density. To explain the observed evolution of the size-mass relation of star-forming disk galaxies other processes, such as the preferential quenching of compact galaxies or galaxy mergers, may be required.
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