论文标题
Sami Galaxy调查：低$ Z $星形星系和湍流驱动因素的气速分散
The SAMI Galaxy Survey: Gas velocity dispersions in low-$z$ star-forming galaxies and the drivers of turbulence
论文作者
论文摘要
我们推断出在一系列集成的星形形成率（sfr $ \ in [10^{ - 3}，10^2]，10^2] $ m $ _ \ odot $ yr $ yr $^{ - 1} $ 0.1 $ 0.1 $ 0.1 $ 0.1 $的固有电离气体运动学（Sfr $ \ in [10^{ - 3}，10^2]，10^{ - 3}，10^2] $ 0.1 $ 0.1 $ 0.1 $ 0.1 $ 0.1 $ 0.1 $ 0.1 $）使用一致的3D技术。总样本是来自Sami Galaxy调查和发电机调查的星系的组合。对于从Sami Galaxy调查中获取的典型低$ Z $星系，我们发现垂直速度分散（$σ_{V，Z} $）与恒星形成率，恒星质量，HI GAS质量和旋转速度的度量呈正相关。最大的相关性是恒星形成速率表面密度（$σ_\ text {sfr} $）。使用总样本，我们发现$σ_{V，z} $随着$ [$ 10^{ - 3} $，1] m $ _ \ odot $ yr $ yr $^{ - 1} $ in $ [$ 10^{ - 3} $，$ 17 \ pm3 $ s $ s $ s $ s $ pm^$ pm^$ jm^$ jm^$^$ km^$^$ jm^$ jm^$ jm^$^$ 24 s s s $ [$ 10^{ - 3} $，$ yr $^$^$ a陡峭的增加到$σ_{v，z} $ \ sim 80 $ km s $ s $^{ - 1} $ sfr $ \ gtrsim 1 $ m $ _ \ odot $ yr $ yr $^{ - 1} $。这与最新的理论模型一致，该模型表明，由星形形成反馈过程驱动的$σ_{V，z} $地板，在$σ_{V，z} $上的上升速度在较高的sfr上进行，由气体通过光盘的重力传输驱动。
We infer the intrinsic ionised gas kinematics for 383 star-forming galaxies across a range of integrated star-formation rates (SFR $\in [10^{-3}, 10^2]$ M$_\odot$ yr$^{-1}$) at $z \lesssim 0.1$ using a consistent 3D forward-modelling technique. The total sample is a combination of galaxies from the SAMI Galaxy Survey and DYNAMO survey. For typical low-$z$ galaxies taken from the SAMI Galaxy Survey, we find the vertical velocity dispersion ($σ_{v, z}$) to be positively correlated with measures of star-formation rate, stellar mass, HI gas mass, and rotational velocity. The greatest correlation is with star-formation rate surface density ($Σ_\text{SFR}$). Using the total sample, we find $σ_{v, z}$ increases slowly as a function of integrated star-formation rate in the range SFR $\in$ [$10^{-3}$, 1] M$_\odot$ yr$^{-1}$ from $17\pm3$ km s$^{-1}$ to $24\pm5$ km s$^{-1}$ followed by a steeper increase up to $σ_{v, z}$ $\sim 80$ km s$^{-1}$ for SFR $\gtrsim 1$ M$_\odot$ yr$^{-1}$. This is consistent with recent theoretical models that suggest a $σ_{v, z}$ floor driven by star-formation feedback processes with an upturn in $σ_{v, z}$ at higher SFR driven by gravitational transport of gas through the disc.
