论文标题
LIRGS中分子流出的激发和加速度：扩展的ESO 320-G030在200-PC尺度上流出
Excitation and acceleration of molecular outflows in LIRGs: The extended ESO 320-G030 outflow on 200-pc scales
论文作者
论文摘要
我们使用高空间分辨率（70 pc; 0.3“）co多转变（1-0、2-1、4-3和6-5）ALMA数据研究当地LIRG ESO320-G030中冷分子流出的物理条件和运动学，d = 48 mpc，logir/lir/lsun = 11.320.320.320.320.320.320.320.320.320.320.320.320。320。320。30.320。320。320。320。320。紧凑型和模糊的核星爆（SFR〜15 msun/yr; av〜40 mag）类似于流出中的ulirgs的核爆炸，而相对于其他核心的核心气体，相对于其他CO（4-3）而言，1-0/2-1的比率相对于其他CO（4-3）。非LTE辐射转移模型表明，流出分子云的特性与核和磁盘云的特性不同：流出中的动力学温度较低（〜9 K），而云的云层具有较低的柱子，假设较大的内部速度梯度，则是60^+250^+250_-45 km-45 km-45 km-45 km-45 km-45 km-45 km-45 km-45 km/s/s/s/s/s/s/s/s/s/s/s/s/s/s/s/s/s/s/s/s/s/s/s/s/s/s/s/s/s/s/s/s/s/s/s/s/s/s/s/s/s/s的com/s/s。不受自我的束缚流出量在190-560 PC之间显示0.8 km/s/pc的速度梯度，然后最大速度（〜750 km/s），最多1.7 kpc。 阶段。
We used high-spatial resolution (70 pc; 0.3") CO multi-transition (1-0, 2-1, 4-3, and 6-5) ALMA data to study the physical conditions and kinematics of the cold molecular outflow in the local LIRG ESO320-G030 (d=48 Mpc, log LIR/Lsun=11.3). ESO320-G030 is a double-barred isolated spiral, but its compact and obscured nuclear starburst (SFR~15 Msun/yr; Av~40 mag) resembles those of more luminous ULIRGs. In the outflow, the 1-0/2-1 ratio is enhanced with respect to the rest of the galaxy and the CO(4-3) transition is undetected. This indicates that the outflowing molecular gas is less excited than the gas in the nuclear starburst (launching site) and the galaxy disk. Non-LTE radiative transfer modeling reveals that the properties of the outflow molecular clouds differ from those of the nuclear and disk clouds: The kinetic temperature is lower (~9 K) in the outflow, and the outflowing clouds have lower column densities. Assuming a 10^-4 CO abundance, the large internal velocity gradients, 60^+250_-45 km/s/pc, imply that the outflowing molecular clouds are not bound by self-gravity. All this suggests that the life-cycle (formation, collapse, dissipation) of the disk clouds might differ from that of the outflowing clouds which might not be able to form stars. The low Tkin of the molecular outflow remains constant up to 1.7 kpc. This indicates that the heating by the hotter ionized outflow phase is not efficient and may favor the survival of the outflow molecular phase. The velocity structure of the outflow shows a 0.8 km/s/pc velocity gradient between 190-560 pc and then a constant maximum velocity (~750 km/s) up to 1.7 kpc. This is compatible with a pure gravitational evolution of the outflow under certain mass outflow rate and launching velocity variations. Alternatively, ram pressure acceleration and cloud evaporation could explain the observed kinematics and size of the molecular phase.
