理論モデルに基づき構築された銀河やAGN の模擬カタログは、観測のエラーを評価したり、 観測データから宇宙論や銀河形成・進化の情報を多く引き出したりするための重要なデータである。 模擬カタログを構築する代表的な手法として
などが挙げられる。
それぞれの手法を比較し、長所と短所をまとめなさい。
PFS やVera Rubin などによる新しいサーベイ観測のために、どのような模擬カタログが必要か考察しなさい。
課題(2)で考察した模擬カタログをUchuu シミュレーションのハローカタログを利用して 実際に構築してみなさい。
We will review the internal properties of galaxies at 1 < z < 2 using multi-band JWST images. Structures include the presence of disks, bulges, spiral arms and clumps. Analysis tools are being developed to optimally detect and quantify these structures within star-forming galaxies less hampered by dust and working at rest-frame optical wavelengths. Participants will run software tools to analyze JWST images and consider important science questions to address such as the growth of bulges and fueling of Active Galactic Nuclei.
銀河中心には超巨大ブラックホール が普遍的に存在し、超巨大ブラックホール形成・進化は銀河の形成進化史と密接に関係することが観測的に示唆されています【1】。 これは超巨大ブラックホールと銀河の共進化を示唆しますが、その起源は明らかになっていません。 活動銀河核（AGN）とは、銀河中心の超巨大ブラックホールへのガス降着の際に解放される重力エネルギーによって、膨大な輻射、AGN ジェットやアウトフローを伴う天体です。 そのため、超巨大ブラックホールと銀河の共進化の起源として、AGNフィードバック（周辺ガスへの運動量・エネルギー注入）がブラックホール成長や銀河の形成・進化に大きな影響を与えることで共進化を制御している可能性が指摘されています【２】。 そこで、AGN の寿命（AGN の活動期間）についての次の課題を考えることで、銀河と超巨大ブラックホールの共進化についての理解を深める新たな研究計画を提案してみてください。
With the advent of multi-wavelength and multi-messenger big data, along with the rapid advancement of machine learning, observational research in modern astronomy has diversified significantly. Broadly speaking, research approaches can be categorized into two types:
Participants are invited to discuss either 1., 2., or both in this group work, depending on their interests.
With the launch of the James Webb Space Telescope (JWST) in recent years, previously unknown populations of astronomical objects have been uncovered, drawing increasing attention to their physical nature. From the perspective of AGN (Active Galactic Nuclei) research, participants are encouraged to explore and discuss the following topics:
Current and upcoming telescopes and instruments are expected to acquire imaging and spectroscopic data for tens of millions to billions of objects. This marks a true transition into the big data era in astronomy. Concurrently, the emergence of machine learning has greatly diversified data analysis techniques.
We invite discussion on promising and innovative directions for AGN research using the following optical and infrared facilities and methods:
We especially welcome discussion on AGN research utilizing Subaru PFS, which began the SSP observations in March.
The gas in the universe is believed to have been ionized at around redshift 6. Recent observations of the cosmic microwave background, quasar absorption lines, and galaxies have gradually improved our understanding of cosmic reionization. However, the three major unresolved issues of cosmic reionization remain:
1. How did ionization proceed? (Reionization history)
2. What kinds of objects caused reionization? (Ionizing sources)
3. What was the structure of the ionized regions? (Ionization structure)
In our group work, let’s consider what kinds of reionization histories, ionizing sources, and ionization structures are possible, taking into account recent observational data from instruments like JWST and recent simulations. In addition to that, let’s theoretically propose an entirely new method for studying reionization—one that is distinct from existing approaches such as CMB, quasar Lya absorption lines, Lyman-alpha emitting galaxies, and 21 cm line observations.
The CGM has been studied through absorption lines imprinted on bright background sources or on the targets themselves, and through the direct detection of emission lines [1, 2, 3]. While it is widely recognized that the CGM is multiphase, simultaneously observing multiple phases in the same sample remains a significant challenge. As a result, many studies have focused on single-phase observations or have combined results from different samples/targets to infer the physical properties of the CGM and related inflow/outflow processes. These limitations are largely due to instrumental capabilities and observational techniques, which restrict the available tracers depending on the redshift and type of the target. With the advent of state-of-the-art and future instruments, the observational capabilities for studying the CGM (/IGM) are expected to significantly improve. In this group work, please address the following two points: 1. Summarize key previous studies on the CGM (/IGM), including their main findings, sample characteristics (including redshift information), instruments used, and observational techniques. 2. Propose a new observational strategy to study the CGM (/IGM) using current or upcoming instruments. If existing or planned instruments are insufficient, suggest the specifications or performance improvements that would be necessary.
