The KMOS3D Survey: Demographics and Properties of Galactic Outflows at z = 0.6–2.7
The KMOS3D Survey: Demographics and Properties of Galactic Outflows at z = 0.6–2.7
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DOI：
10.3847/1538-4357/ab0ca2
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发表时间：
2018-07
期刊：
影响因子：
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通讯作者：
N. F. Schreiber;H. Übler;R. Davies;R. Genzel;R. Genzel;E. Wisnioski;E. Wisnioski;S. Belli;
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文献类型：
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作者：
N. F. Schreiber;H. Übler;R. Davies;R. Genzel;R. Genzel;E. Wisnioski;E. Wisnioski;S. Belli;
本文主要基于Hα、[N ii]和[S ii]线发射的积分场谱，对599个正常星系在红移0.6 < z < 2.7时的电离气体外流进行了普查。该样本相当均匀地覆盖了质量为9.0 < log（M*/M *）< 11.7的恒星形成星系的主要序列，并探讨了静止星系和星暴异常星系的区域。大约有三分之一显示出指示外流的高速分量，大致相等地分为由星星形成（SF）和活动星系核（AGN）驱动的风。SF驱动风的发生率主要与SF属性相关。这些外流的典型速度为450 km s−1，局部电子密度为ne 380 cm−3，在所有星系质量下的适度质量加载因子为10.1 -0.2，能量与年轻恒星群体的动量驱动相容。SF驱动的风可能会从log（M*/M）<$0.3星系逃逸，但在较热和较冷的外流阶段，似乎需要大量的质量、动量和能量来解释低质量区域的低星系形成效率。更快的活动星系核驱动的外流（1000-2000 km s−1）通常在log（M*/M <$）<$10.7以上被探测到，在log（M*/M <$）<$11.2的星系中高达75%。活动星系核驱动风的发生率、强度和速度与恒星质量和中心浓度密切相关。它们流出的电离气体看起来密度更大（ne = 1000 cm−3），可能是被压缩和激波激发的。这些风具有与SF驱动的风相当的质量负载因子，但携带的动量（能量）是SF驱动的风的2.10（2.50）倍。结果证实了我们以前的研究结果的高占空比，能量驱动的外流动力的活动星系核以上的Schechter质量，这可能有助于SF淬火。
We present a census of ionized gas outflows in 599 normal galaxies at redshift 0.6 < z < 2.7, mostly based on integral field spectroscopy of Hα, [N ii], and [S ii] line emission. The sample fairly homogeneously covers the main sequence of star-forming galaxies with masses 9.0 < log(M*/M⊙) < 11.7, and probes into the regimes of quiescent galaxies and starburst outliers. About one-third exhibits the high-velocity component indicative of outflows, roughly equally split into winds driven by star formation (SF) and active galactic nuclei (AGNs). The incidence of SF-driven winds correlates mainly with SF properties. These outflows have typical velocities of ∼450 km s−1, local electron densities of ne ∼ 380 cm−3, modest mass loading factors of ∼0.1–0.2 at all galaxy masses, and energetics compatible with momentum driving by young stellar populations. The SF-driven winds may escape from log(M*/M⊙) ≲ 10.3 galaxies, but substantial mass, momentum, and energy in hotter and colder outflow phases seem required to account for low galaxy formation efficiencies in the low-mass regime. Faster AGN-driven outflows (∼1000–2000 km s−1) are commonly detected above log(M*/M⊙) ∼ 10.7, in up to ∼75% of log(M*/M⊙) ≳ 11.2 galaxies. The incidence, strength, and velocity of AGN-driven winds strongly correlates with stellar mass and central concentration. Their outflowing ionized gas appears denser (ne ∼ 1000 cm−3), and possibly compressed and shock-excited. These winds have comparable mass loading factors as the SF-driven winds but carry ∼10 (∼50) times more momentum (energy). The results confirm our previous findings of high-duty-cycle, energy-driven outflows powered by AGN above the Schechter mass, which may contribute to SF quenching.