ATOMS: ALMA three-millimeter observations of massive star-forming regions -XIII. Ongoing triggered star formation within clump-fed scenario found in the massive ( 1500 M⊙) clump
| Autor: | Siju Zhang, Ke Wang, Tie Liu, Annie Zavagno, Mika Juvela, Hongli Liu, Anandmayee Tej, Amelia M Stutz, Shanghuo Li, Leonardo Bronfman, Qizhou Zhang, Paul F Goldsmith, Chang Won Lee, Enrique Vázquez-Semadeni, Ken’ichi Tatematsu, Wenyu Jiao, Fengwei Xu, Chao Wang, Jian-Wen Zhou |
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| Přispěvatelé: | Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS) |
| Jazyk: | angličtina |
| Rok vydání: | 2023 |
| Předmět: |
stars: formation
Astrophysics - Solar and Stellar Astrophysics Space and Planetary Science [SDU]Sciences of the Universe [physics] Astrophysics of Galaxies (astro-ph.GA) stars: kinematics and dynamics FOS: Physical sciences Astronomy and Astrophysics ISM: H II regions ISM: photodissociation region (PDR) ISM: clouds Astrophysics - Astrophysics of Galaxies Solar and Stellar Astrophysics (astro-ph.SR) |
| Zdroj: | Monthly Notices of the Royal Astronomical Society Monthly Notices of the Royal Astronomical Society, 2023, ⟨10.1093/mnras/stad011⟩ |
| ISSN: | 0035-8711 1365-2966 |
| DOI: | 10.1093/mnras/stad011⟩ |
| Popis: | Whether ionization feedback triggers the formation of massive stars is highly debated. Using ALMA 3 mm observations with a spatial resolution of $\sim 0.05$ pc and a mass sensitivity of 1.1 $\rm M_\odot$ beam$^{-1}$ at 20 K, we investigate the star formation and gas flow structures within the ionizing feedback-driven structure, a clump-scale massive ($\gtrsim 1500$ $\rm M_\odot$) bright-rimmed cloud (BRC) associated with IRAS 18290-0924. This BRC is bound only if external compression from ionized gas is considered. A small-scale ($\lesssim1$ pc) age sequence along the direction of ionizing radiation is revealed for the embedded cores and protostars, which suggests triggered star formation via radiation-driven implosion (RDI). Furthermore, filamentary gas structures converge towards the cores located in the BRC's center, indicating that these filaments are fueling mass towards cores. The local core-scale mass infall rate derived from H$^{13}$CO$^+$ $J=1-0$ blue profile is of the same order of magnitude as the filamentary mass inflow rate, approximately 1 $\rm M_\odot$ kyr$^{-1}$. A photodissociation region (PDR) covering the irradiated clump surface is detected in several molecules, such as CCH, HCO$^+$, and CS whereas the spatial distribution stratification of these molecules is indistinct. CCH spectra of the PDR possibly indicate a photoevaporation flow leaving the clump surface with a projected velocity of $\sim2$ km s$^{-1}$. Our new observations show that RDI accompanied by a clump-fed process is operating in this massive BRC. Whether this combined process works in other massive BRCs is worth exploring with dedicated surveys. 34 pages with 20 figures, Accepted by MNRAS on 2022 December 28 |
| Databáze: | OpenAIRE |
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