Welcome to Sukyoung K. Yi's group (GEM) homepage!
이석영 교수의 은하진화 연구 그룹 홈페이지에 오신것을 환영합니다.
Science Goal 연구 목표
We aim to understand the formation and evolution of galaxies. 우리 그룹의 연구 목표는 은하의 형성과 진화과정을 이해하는 것입니다.
News 소식
- The 2020 GEM 2nd workshop will be held on 19 - 21 August, 2020 in Yonsei University, Seoul, Korea (Cancelled)
- The 2020 GEM workshop will be held on 14 - 17 January, 2020 in Gyeongju, Korea
- Minjung Park's paper has been introduced by AAS Nova (23 September 2019).
- Dr. Sandro Tacchella will visit GEM (8-11 July, 2019)
- The 2019 GEM - CASCADE workshop will be held on 1 - 4 July, 2019 in Jeju, Korea
- The 2018 GEM workshop will be held on 2 - 4 July, 2018 in Kangnung, Korea
- Dr. Scott Croom, Dr. Julia Bryant and Dr. Warrick Couch will visit GEM (10-13 Apr 2017)
- Dr. Barbara Cantinella and Dr. Luca Cortese at ICRAR are visiting GEM (1-15 Apr 2017)
- SAMI workshop will be held at KASI. (12 Apr 2017)
- Environment workshop wiil be held. (3 Apr 2017)
Recent Paper 최근 논문
YZiCS: Unveiling the Quenching History of Cluster Galaxies Using Phase-space Analysis
Rhee, Jinsu; Smith, Rory; Choi, Hoseung; Contini, Emanuele; Jung, S. Lyla; Han, San; Yi, Sukyoung K.
Summary
This study tries to constrain the quenching timescales of galaxies in local cluster environments by combining a cosmological simulation data (YZiCS) with an SDSS cluster catalog through the phase-space analysis. The star formation history for the sample galaxies are constrained by using abundance matching between the time since infall distribution and the star formation rate distribution of the galaxies The following are our main results on the constrained quenching timescales. (i) Part of the quenching takes place outside clusters by consuming cold gas with the e-folding timescale of 3 Gyr with a strong inverse mass dependence. (ii) The pace of quenching is maintained roughly for 2 Gyr ("delay time") during the first crossing time into the cluster. (iii) Quenching becomes more dramatic (e-folding timescale of roughly 1 Gyr) after delay time, probably because ram pressure stripping is strongest near the cluster center. Counterintuitively, more massive galaxies show shorter quenching timescales mainly because they enter their clusters with lower gas fractions due to ex-situ quenching in the first place.