有關於星系形成組裝歷史的影響,可以透過恆星暈的性質與星系觀測量(如
總星系質量、顏色或氣體比例)之間的趨勢來加以約束。然而,過去大部分針
對星系外恆星暈的研究,主要集中於辨認和分類個別低表面亮度的特徵。由於
模擬解析度的限制,目前模擬中對這些恆星暈子結構的再現還無法得到很好的
約束。此外,近年來有幾個調查開始探討恆星暈的總體比例,但對於恆星暈性
質的統計理解仍然缺乏。我們在模擬中看到了恆星暈比例與其宿主星系之間的
某些趨勢。我們預期在觀測上也會看到類似的結果。簡而言之,我們更感興趣
的是理解整個恆星暈的總體統計性質,而非個別的低表面亮度結構。這篇論文
的目標之一是開發統一的、自動化的恆星暈總體性質測量方法,這些方法容易
應用於大型數據集,並且可以與模型進行比較。我們利用暗能量光譜儀傳統成
像巡天的影像分析了具有恆星暈的星系,並重現了蜻蜓巡天的結果。我們發現
了恆星暈比例與其宿主星系之間的統計趨勢。到目前為止,只有模擬中存在對
恆星暈的深入統計研究。這一發現應該能夠增強我們探索星系組裝歷史及限制
宇宙學模型的信心。

The influence of assembly history on galaxy formation could be constrained by trends in stellar halo properties with galactic observables (such as the total galaxy mass, color or gas fraction). However, most previous work on images of extragalactic stellar halos has focused on identifying and classifying individual low surface brightness (LSB) features. Due to limitations in simulation resolution, the reproduction of these stellar halo substructures in simulations is currently not well constrained. In addition, several surveys in recent years have started to investigate the overall fraction of the stellar halo, but there is still a lack of statistical understanding regarding stellar halo properties. We have seen some tendency between the fraction of the stellar halo and its host galaxy in simulations. We expect to see similar results in theory from observation. In short, we are more interested in understanding the overall statistical properties of the entire stellar halo, rather than the individual LSB structures. One of the goal in this thesis is to develop uniform, automated measurements of bulk stellar halo properties that are easy to apply to large datasets and can be compared with models. We have analyzed galaxies with their stellar halo and reproduced the result from the Dragonfly Survey using images from the Dark Energy Spectroscopic Instrument Legacy Imaging Survey (DESI-LS). We find statistical trends in the correlation between stellar halo fractions and their host galaxies. So far, statistically significant studies of stellar halos exist only in simulations. This finding should give us more confidence to explore the assembly history of galaxies and constrain the cosmological models.

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