[TCA Student Seminar]
Please find the schedule listed in the tabulation below. Each seminar starts at 12 p.m. and takes place in the NCTS Physics 4F Lecture Hall, Cosmology Hall, NTU.
For more detailed information regarding each seminar, please see it in the section below the tabulation a week before the seminar.
| Date | Speaker 1 | Affiliation | Supervisor | Speaker 2 | Affiliation | Supervisor |
| 2025/7/24 | Pon-Yin Wang | TKU | Hsi-An Pan | |||
| 2025/8/22 | Tsung-Han Chuang | NTNU | Yueh-Ning Lee | Jyun-Heng Lin | NTNU | Chin-Fei Lee |
| 2025/9/26 | Chiung-Yin Chang | NTHU | Hsiang-Yi Karen Yang | Huan-Ping Chao | NCKU | Kwan-Lok Li |
| 2025/10/31 | Yi-Yang Lee | NTHU | Hsiang-Yi Karen Yang | Prangsutip Cherdwongsung | NTHU | Ing-Guey Jiang |
| 2025/11/28 | Yu-Xuan Nancy Lin | NYCU | Shih-Ping Lai | Tz-En Gau | NTU | Chia-Yu Hu |
| 2025/12/26 | Szu-Ting Chen | NTHU | Shin-Ping Lai | Afif Ismail | NTNU | Hung-Yi Pu |
Time: 2025/07/24 (Thu.) 12 p.m.
Place: NCTS Physics 4F Lecture Hall, Cosmology Hall, NTU
Talk Title: Tracing Gas and Star formation in Galaxy Mergers with ALMA and MaNGA
Speaker: Pon-Yin Wang (Tamkang University)
Register for Lunch Box: https://forms.gle/41juY8MZyL2eWX2i7
Abstract:
Galaxy interactions play a crucial role in the evolution of galaxies in the local universe, often triggering enhanced star formation. Simulations consistently suggest that such interactions significantly reshape the distribution of molecular gas within galactic disks, thereby altering the spatial distribution of star formation. In this study, we aim to observationally investigate the distribution of gas and star formation across different merger stages and assess the extent to which these observations align with simulation predictions. Here we analyze a sample of 15 galaxies—including galaxy pairs and post-mergers—with stellar masses log(M*) ≥ 10 [M⊙] and redshifts in the range 0.02 < z < 0.1, using data from ALMA and SDSS-MaNGA. We also construct radial profiles of gas fraction, star formation rate(SFR), and star formation efficiency(SFE), extending from the galactic center to 1.5 effective radii(Re). Our results indicate that the gas fraction is the primary driver of elevated SFR in close pair systems. Nevertheless, all merger stages exhibit an inconsistent relationship between SFR and gas mass, suggesting the presence of a common regulatory mechanism governing star formation during galaxy interactions.
