M105的晕和行星状星云群追踪到的其群环境：II。利用单个恒星的运动学揭示狮子座I星系NGC 3384和M105周围群内光的存在
The halo of M105 and its group environment as traced by planetary nebula populations: II. Using kinematics of single stars to unveil the presence of intragroup light around the Leo I galaxies NGC 3384 and M105
摘要：
M105是附近狮子座I星系群中的一个早期型星系，狮子座I星系群是包含所有星系类型的最近星系群，因此是探索低质量组内光（IGL）组装的绝佳环境。利用行星状星云摄谱仪对M105及其周围30'x30'的狮子座I群行星状星云进行了一次新的扩展运动学观测。我们使用PNe作为晕和IGL中漫射恒星光的运动学示踪剂，并采用高斯混合模型来分离伴星星系NGC 3384的贡献，并将PNe与M105周围的晕和IGL分量联系起来。我们给出了314个PNe的星表，其中93个与NGC 3384紧密相联，169个与M105紧密相联。M105的PNe还与它的晕和周围的指数包络有关。我们构造光滑的速度和速度色散场，并计算投影旋转，速度色散，和$λ_R$配置文件的每个组件。Halo PNe的速度色散和旋转分布呈下降趋势，而指数包络的速度色散和旋转在大半径处显著增加。我们确定了三个具有不同运动学的区域，这些区域与不同的恒星星族属性有关：（一）旋转核心（ii）从1到$1~R_\mathrm{eff}$的晕由中等金属丰度的恒星组成（iii）指数包络线超过了我们最远的数据点16颗$R_\mathrm{eff}$，主要由贫金属（[M/H]<-1）恒星组成。后者的高速色散和适度的旋转是一致的测量矮卫星星系的狮子座I组，表明指数包络线的痕迹过渡到IGL。
英文摘要：
M105 is an early-type galaxy in the nearby Leo I group, the closest galaxy group to contain all galaxy types and therefore an excellent environment to explore the low-mass end of intra-group light (IGL) assembly. We present a new extended kinematic survey of planetary nebulae (PNe) in M105 and the surrounding 30'x30' in the Leo I group with the Planetary Nebula Spectrograph. We use PNe as kinematic tracers of the diffuse stellar light in the halo and IGL and employ Gaussian mixture models to separate contributions from the companion galaxy NGC 3384 and associate PNe with halo and IGL components around M105. We present a catalogue of 314 PNe and firmly associate 93 with NGC 3384 and 169 with M105. The PNe in M105 are further associated with its halo and the surrounding exponential envelope. We construct smooth velocity and velocity dispersion fields and calculate projected rotation, velocity dispersion, and $λ_R$ profiles for each component. Halo PNe exhibit declining velocity dispersion and rotation profiles, while the velocity dispersion and rotation of the exponential envelope increase notably at large radii. We identify three regimes with distinct kinematics that are linked to distinct stellar population properties: (i) the rotating core (within $1~R_\mathrm{eff}$) formed in situ and dominated by metal-rich ([M/H]~0) stars likely formed in situ, (ii) the halo from 1 to $7.5~R_\mathrm{eff}$ consisting of intermediate-metallicity stars ([M/H]>-1), either formed in situ or brought in through major mergers, and (iii) the exponential envelope reaching beyond our farthest data point at 16 $R_\mathrm{eff}$, predominately composed of metal-poor ([M/H]<-1) stars. The high velocity dispersion and moderate rotation of the latter are consistent with that measured for dwarf satellite galaxies in the Leo I group, indicating that the exponential envelope traces the transition to the IGL.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
