Details

Autor(en) / Beteiligte

• Sun 孙, Jiayi 嘉懿
• He 何, Hao 浩
• Batschkun, Kyle
• Levy, Rebecca C.
• Emig, Kimberly
• Rodríguez, M. Jimena
• Hassani, Hamid
• Leroy, Adam K.
• Schinnerer, Eva
• Ostriker, Eve C.
• Wilson, Christine D.
• Bolatto, Alberto D.
• Mills, Elisabeth A. C.
• Rosolowsky, Erik
• Lee, Janice C.
• Dale, Daniel A.
• Larson, Kirsten L.
• Thilker, David A.
• Ubeda, Leonardo
• Whitmore, Bradley C.
• Williams, Thomas G.
• Barnes, Ashley T.
• Bigiel, Frank
• Chevance, Mélanie
• Glover, Simon C. O.
• Grasha, Kathryn
• Groves, Brent
• Henshaw, Jonathan D.
• Indebetouw, Rémy
• Jiménez-Donaire, María J.
• Klessen, Ralf S.
• Koch, Eric W.
• Liu, Daizhong
• Mathur, Smita
• Meidt, Sharon
• Menon, Shyam H.
• Neumann, Justus
• Pinna, Francesca
• Querejeta, Miguel
• Sormani, Mattia C.
• Tress, Robin G.

Titel

Hidden Gems on a Ring: Infant Massive Clusters and Their Formation Timeline Unveiled by ALMA, HST, and JWST in NGC 3351

Ist Teil von

• The Astrophysical journal, 2024-06, Vol.967 (2), p.133

Ort / Verlag

Philadelphia: IOP Publishing

Erscheinungsjahr

2024

Link zum Volltext

Quelle

EZB Electronic Journals Library

Beschreibungen/Notizen

• Abstract We use 0.1″ observations from the Atacama Large Millimeter Array (ALMA), Hubble Space Telescope (HST), and JWST to study young massive clusters (YMCs) in their embedded “infant” phase across the central starburst ring in NGC 3351. Our new ALMA data reveal 18 bright and compact (sub-)millimeter continuum sources, of which 8 have counterparts in JWST images and only 6 have counterparts in HST images. Based on the ALMA continuum and molecular line data, as well as ancillary measurements for the HST and JWST counterparts, we identify 14 sources as infant star clusters with high stellar and/or gas masses (∼10 5 M ⊙ ), small radii (≲ 5 pc), large escape velocities (6–10 km s −1 ), and short freefall times (0.5–1 Myr). Their multiwavelength properties motivate us to divide them into four categories, likely corresponding to four evolutionary stages from starless clumps to exposed H ii region–cluster complexes. Leveraging age estimates for HST-identified clusters in the same region, we infer an evolutionary timeline, ranging from ∼1–2 Myr before cluster formation as starless clumps, to ∼4–6 Myr after as exposed H ii region–cluster complexes. Finally, we show that the YMCs make up a substantial fraction of recent star formation across the ring, exhibit a nonuniform azimuthal distribution without a very coherent evolutionary trend along the ring, and are capable of driving large-scale gas outflows.