We present a kinematic study of ionized extraplanar gas in two low-inclination late-type galaxies (NGC 3982 and NGC 4152) using integral field spectroscopy data from the DiskMass H α sample. We first isolate the extraplanar gas emission by masking the H α flux from the regularly rotating disc. The extraplanar gas emission is then modelled in the 3D position–velocity domain using a parametric model described by three structural and four kinematic parameters. Best-fitting values for the model are determined via a Bayesian MCMC approach. The reliability and accuracy of our modelling method are carefully determined via tests using mock data. We detect ionized extraplanar gas in both galaxies, with scale heights $0.83^{+0.27}_{-0.40}\, \mathrm{kpc}$ (NGC 3982) and $1.87^{+0.43}_{-0.56}\, \mathrm{kpc}$ (NGC 4152) and flux fraction between the extraplanar gas and the regularly rotating gas within the disc of 27 and 15 per cent, respectively, consistent with previous determinations in other systems. We find lagging rotation of the ionized extraplanar gas in both galaxies, with vertical rotational gradients $-22.24^{+6.60}_{-13.13} \, \mathrm{km\, s^{-1}\, kpc^{-1}}$ and $-11.18^{+3.49}_{-4.06}\, \mathrm{km\, s^{-1}\, kpc^{-1}}$, respectively, and weak evidence for vertical and radial inflow in both galaxies. The above results are similar to the kinematics of the neutral extraplanar gas found in several galaxies, though this is the first time that 3D kinematic modelling of ionized extraplanar gas has been carried out. Our results are broadly consistent with a galactic fountain origin combined with gas accretion. However, a dynamical model is required to better understand the formation of ionized extraplanar gas.

中文翻译：

---

螺旋星系 NGC 3982 和 NGC 4152 中电离面外气体的运动学分析

我们使用来自 DiskMass H α 样本的积分场光谱数据，对两个低倾角晚型星系（NGC 3982 和 NGC 4152）中的电离面外气体进行了运动学研究。我们首先通过掩盖来自有规律旋转的圆盘的 H α 通量来隔离平面外气体排放。然后使用由三个结构参数和四个运动学参数描述的参数模型在 3D 位置-速度域中对平面外气体排放进行建模。模型的最佳拟合值通过贝叶斯 MCMC 方法确定。我们的建模方法的可靠性和准确性是通过使用模拟数据的测试仔细确定的。我们检测到两个星系中的电离面外气体，尺度高度为 $0.83^{+0.27}_{-0.40}\, \mathrm{kpc}$ (NGC 3982) 和 $1.87^{+0.43}_{-0.56}\, \mathrm{kpc}$ (NGC 4152) 和平面外气体和圆盘内有规律旋转的气体之间的通量分数分别为 27% 和 15%，这与之前在其他系统中的测定结果一致。我们发现两个星系中电离面外气体的滞后旋转，垂直旋转梯度 $-22.24^{+6.60}_{-13.13} \, \mathrm{km\, s^{-1}\, kpc^{- 1}}$ 和 $-11.18^{+3.49}_{-4.06}\, \mathrm{km\, s^{-1}\, kpc^{-1}}$, 垂直的弱证据和两个星系的径向流入。上述结果类似于在几个星系中发现的中性面外气体的运动学，尽管这是第一次对电离面外气体进行 3D 运动学建模。我们的结果与银河喷泉起源与气体吸积相结合大致一致。然而，