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SUMMARY:Revealing the in-situ molecular gas structure around giant molecul
 ar clouds and star clusters
DTSTART:20260929T023000Z
DTEND:20260929T033000Z
DTSTAMP:20260925T012600Z
UID:indico-event-5337@indico-tdli.sjtu.edu.cn
DESCRIPTION:Speakers: Hao He(何浩) (University of Bonn)\n\nHost: Xiaoti
 an XuJoin Tencent Meeting：https://meeting.tencent.com/dm/0nOEIYhOaExIMee
 ting ID: 536879894 (no password）\nAbstract:Molecular gas structure encod
 es key information about the physical processes involved in giant molecula
 r cloud (GMC) formation and collapse\, as well as their response to stella
 r feedback. While a large number of studies have systematically characteri
 zed the physical properties of individual GMCs\, their spatial distributio
 n and surrounding gas structure have been less extensively studied. In thi
 s talk\, I will present a novel method for characterizing in-situ gas stru
 cture by stacking radial profiles. For GMCs\, we measure the CO(2–1) pro
 file around each GMC peak position and obtain stacked representative inten
 sity profiles for GMCs in different environments and with different physic
 al properties. Our stacked intensity profiles can generally be characteriz
 ed as a combination of two Gaussians plus a constant\, with the broad Gaus
 sian component reflecting the degree of surrounding gas concentration and 
 being more prominent around more massive and gravitationally bound GMCs. W
 e also stack CO(2–1) intensity profiles around PHANGS-HST star clusters 
 of different masses and ages. We find that star clusters spatially associa
 ted with H II regions show the highest CO(2–1) concentration\, with a cl
 uster formation efficiency from gas of ∼1%. Clusters older than 4 Myr sh
 ow a flat intensity profile\, indicating the role of stellar feedback in c
 learing gas on such a short timescale. We demonstrate that our method work
 s effectively on high-resolution observations of large samples\, providing
  a general and quantitative description of in-situ gas structure\, and can
  serve as a benchmark for simulations of star formation from molecular gas
  to star clusters.\nBiography:Dr. Hao He is a postdoc at University of Bon
 n working in the group of Prof. Frank Bigiel. He received Ph.D. at McMaste
 r University in 2023 before the current postdoc position. His research foc
 us on molecular gas and star formation in nearby galaxies at scales of gia
 nt molecular clouds (GMCs) and beyond (< 100 pc)\, utilizing high-resoluti
 on ALMA data and extensive multi-wavelength comparison. In his Ph.D.\, he 
 focuses on detailed characterization of starburst galaxy mergers (i.e. ult
 ra/ luminous infrared galaxies or U/LIRGs) with both observations and simu
 lations. He is now a member of PHANGS team and focuses on characterizing r
 adial profiles of CO distribution around star-forming products\, such as G
 MCs and star clusters. He is also extensively involved in HI studies using
  PHANGS-MeerKAT data\, specifically to quantify the velocity dispersion an
 d its environmental dependence\, and aim for constraining the driving mech
 anisms of HI turbulence and disk dynamics.\n\n\nhttps://indico-tdli.sjtu.e
 du.cn/event/5337/
URL:https://indico-tdli.sjtu.edu.cn/event/5337/
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