Red Geysers are quiescent galaxies with galactic scale ionised outflows, likely due to low-luminosity Active Galactic Nuclei (AGN). We used Gemini GMOS-IFU observations of the inner $\sim 1.0-3.0$ kpc of nine Red Geysers selected from the MaNGA survey to study the gas ionisation and kinematics. The emission-line ratios suggest the presence of Seyfert/LINER (Low Ionisation Nuclear Emission Region) nuclei in all sources. Two galaxies show H$α$ equivalent width (H$α$ EW) larger than 3 Å(indicative of AGN ionisation) within an aperture 2.5 arcsec of diameter ($1.3-3.7$ kpc at the distance of galaxies) for MaNGA data, while with the higher resolution GMOS data, four galaxies present H$α$ EW$>3$ Åwithin an aperture equal to the angular resolution ($0.3-0.9$ kpc). For two objects with GMOS-IFU data, the H$α$ EW is lower than 3 Åbut larger than 1.5 Å, most probably due to a faint AGN. The spatially resolved electron density maps show values between $100-3000$ cm$^{-3}$ and are consistent with those determined in other studies. The large (MaNGA) and the nuclear scale (GMOS-IFU) gas velocity fields are misaligned, with a kinematic position angle difference between 12$^{\circ}$ and 60$^{\circ}$. The [NII]$λ$6583 emission-line profiles are asymmetrical, with blue wings on the redshifted side of the velocity field and red wings on the blueshifted side. Our results support previous indications that the gas in Red Geysers is ionised by an AGN, at least in their central region, with the presence of outflows, likely originating in a precessing accretion disc.
The Next Generation Virgo Cluster Survey. XII. Stellar Populations and Kinematics of Compact, Low-Mass Early-Type Galaxies from Gemini GMOS-IFU Spectroscopy
On the properties of the interstellar medium in extremely metal-poor blue compact dwarf galaxies: GMOS-IFU spectroscopy and SDSS photometry of the double-knot galaxy HS 2236+1344
The First Integral Field Unit Spectroscopic View of Shocked Cluster Galaxies
星系团通过与其他星系团的合并而成长，产生Mpc宽的冲击波，以1000-2500 km/s的速度穿过星系团内的介质。为了研究并合激波对星系团性质的影响，我们首次观测了位于低红移（z~0.2）、大质量（~2 $\times10^{15}$ M $_\odot$）、后核通道并合星系团CIZA J2242.8+5301（绰号"香肠“）激波锋面尾流中的5 H $α$发射星系的空间分辨光谱.我们的Gemini/GMOS-N积分场单元（IFU）观测，旨在捕捉H $α$和[NII]发射，揭示了星云气体分布，运动学和金属在星系超过16 kpc尺度。虽然星系显示出旋转支持的证据，但通量和速度图具有复杂的特征，如与星系团合并轴对齐的尾巴和气体流出。由于梯度与由内而外的星系盘生长不相容，金属丰度图与整个星系盘内外的持续恒星形成（SF）是一致的。结合以前的结果，这些试点观测提供了进一步的证据，集群合并和SF触发集群星系之间可能存在联系，这是一个潜在的基本发现，揭示了星系与环境的相互作用。
