后发座星系团中超越Sérsic +指数盘形态
Beyond Sérsic + exponential disc morphologies in the Coma Cluster
摘要：
通过对深空加拿大-法国-夏威夷望远镜$i$波段成像的分析，我们在很宽的光度范围（$-17$ \，$>$ \，$M_g$ \，$>$ \，$-22$）和星团中心半径范围（$0$ \，$<$ \，$r_{\rm{cluster}}$ \，$<$\，1. 3 $r_{200}$）上探索后发座星系团内部星系结构的多样性。我们通过GALFIT提出了2D多分量分解，包括多达三个光度分量的各种候选模型形态。特别关注的是早期型星系与外部光盘（即S 0），并从简单的（“未破碎”）指数盘的偏差。严格的过滤可确保每个模型组件在统计学上显著提高拟合优度。在我们的样本中的大多数后发座星系团成员（478 631）是可靠的对称结构模型拟合。其中，134个（$28\%$）是单一的Sérsic对象，143个（$30\%$）由2个组件结构很好地描述，而201个（$42\%$）需要更复杂的模型。多成分的Sérsic星系类似于被扩展的类高斯外部结构（$R_e > 10$ kpc）包围的紧凑的伪凸起（$n\sim$\，2，$R_e \sim$ \，4 kpc）。11%的星系（$N=52$）在其外部轮廓中具有断裂，表明“截断”或“反截断”盘。在破裂半径之外，截断星系在结构上与指数盘一致，不利于物理截断作为它们的形成机制。反截断星系的膨胀光度与星系光度密切相关，表明这些系统的膨胀增强起源。这两种类型的破碎盘被发现压倒性的（$>70\%$）在“棒”星系，尽管低测量的酒吧部分后发座（$20\pm2\%$）。因此，星系棒在破碎盘结构的形成中起着重要的作用。没有强烈的变化，星系结构的检测与投影集群中心半径。
英文摘要：
[abridged] We explore the diversity of internal galaxy structures in the Coma cluster across a wide range of luminosities ($-17$\,$>$\,$M_g$\,$>$\,$-22$) and cluster-centric radii ($0$\,$<$\,$r_{\rm{cluster}}$\,$<$\,1.3 $r_{200}$) through analysis of deep Canada-France-Hawaii Telescope $i$ band imaging. We present 2D multi-component decomposition via GALFIT, encompassing a wide range of candidate model morphologies with up to three photometric components. Particular focus is placed on early-type galaxies with outer discs (i.e. S0s), and deviations from simple (`unbroken') exponential discs. Rigorous filtering ensures that each model component provides a statistically significant improvement to the goodness-of-fit. The majority of Coma cluster members in our sample (478 of 631) are reliably fitted by symmetric structural models. Of these, 134 ($28\%$) are single Sérsic objects, 143 ($30\%$) are well-described by 2 component structures, while 201 ($42\%$) require more complex models. Multi-component Sérsic galaxies resemble compact psuedobulges ($n\sim$\,2, $R_e \sim$\, 4 kpc) surrounded by extended Gaussian-like outer structures ($R_e > 10$ kpc). 11\% of galaxies ($N=52$) feature a break in their outer profiles, indicating `truncated' or `anti-truncated' discs. Beyond the break radius, truncated galaxies are structurally consistent with exponential discs, disfavouring physical truncation as their formation mechanism. Bulge luminosity in anti-truncated galaxies correlates strongly with galaxy luminosity, indicating a bulge-enhancing origin for these systems. Both types of broken disc are found overwhelmingly ($>70\%$) in `barred' galaxies, despite a low measured bar fraction for Coma ($20\pm2\%$). Thus, galaxy bars play an important role in formation of broken disc structures. No strong variation in galaxy structure is detected with projected cluster-centric radius.
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