论文标题
最大星系中的光学发射线：形态，运动学和电离特性
Optical emission lines in the most massive galaxies: morphology, kinematics and ionisation properties
论文作者
论文摘要
为了更好地描述银河系恒星质量范围的上端，缪斯群众所周知的星系（M3G）调查针对的是最大的星系（M $> 10^{12} $ M $ _ {\ odot} $），在$ z \ sim0.046 $的$ z \ sim \ sim \ sim \ sim \ sim \ sim \ sim \ sim0.046 $中。该样品由25个早期类型星系组成：14个BCG，其中3个位于Shapley Super Cluster（SSC）的最密集区域，SSC中有11个大型卫星。在这项工作中，我们旨在得出气体的空间分布和运动学，并与Muse Data讨论其离子化机制和起源。我们使用广泛的单个恒星种群模型的库拟合光谱的连续体，并对发射线进行建模，最多使用三个高斯功能。在M3G样品中，在5个BCG中检测到电离气体，其中1个位于SSC的最密集区域，SSC中有6个大型卫星。在这些物体中，[OI]和[ni]在3个BCG和一个卫星中被检测到。气体几乎集中在几乎所有物体中，除了2个BCG显示出细丝和2个巨大的卫星，并具有延长的发射。 3 BCG的发射线曲线呈现红色/蓝光的组件。通过分析Balmer线比的平均$ E（B-V）$ 0.2-0.3来揭示灰尘的存在。发射线诊断图显示了主要的衬里线比，而恒星形成几乎没有污染。在80％的快速旋转器和35％的缓慢旋转器中检测到气体。恒星和气态旋转的方向相对于60％的卫星和25％的BCG对齐。未对准的存在表明气体的外部起源为3 BCG和2个卫星。另一方面，其中一些系统的特征是三轴和倾斜的恒星旋转，即使在未对准的情况下，也可以支持气体的内部起源。
To better characterize the upper end of the galaxy stellar mass range, the MUSE Most Massive Galaxies (M3G) Survey targeted the most massive galaxies (M$>10^{12}$ M$_{\odot}$) found in the densest known clusters of galaxies at $z\sim0.046$. The sample is composed by 25 early-type galaxies: 14 BCGs, of which 3 are in the densest region of the Shapley Super Cluster (SSC), and 11 massive satellites in the SSC. In this work we aim at deriving the spatial distribution and kinematics of the gas, and discussing its ionisation mechanism and origin in the optical wavelength range with MUSE data. We fit the continuum of the spectra using an extensive library of single stellar population models and model the emission lines employing up to three Gaussian functions. In the M3G sample, ionized-gas was detected in 5 BCGs, of which one is in the densest region of the SSC, and 6 massive satellites in the SSC. Among these objects, [OI] and [NI] were detected in 3 BCGs and one satellite. The gas is centrally concentrated in almost all objects, except for 2 BCGs that show filaments and 2 massive satellites with extended emission. The emission line profiles of 3 BCGs present red/blueshifted components. The presence of dust was revealed by analysing Balmer line ratios obtaining a mean $E(B-V)$ of 0.2-0.3. The emission-line diagnostic diagrams show predominately LINER line ratios with little contamination from star formation. The gas was detected in 80% of fast rotators and 35% of slow rotators. The orientations of stellar and gaseous rotations are aligned with respect to each other for 60% of satellites and 25% of BCGs. The presence of misalignments points to an external origin of the gas for 3 BCGs and 2 satellites. On the other hand, some of these systems are characterized by triaxial and prolate-like stellar rotation that could support an internal origin of the gas even in case of misalignments.
