학술논문
PHANGS–JWST First Results: Multiwavelength View of Feedback-driven Bubbles (the Phantom Voids) across NGC 628
Document Type
article
Author
Ashley. T. Barnes; Elizabeth J. Watkins; Sharon E. Meidt; Kathryn Kreckel; Mattia C. Sormani; Robin G. Treß; Simon C. O. Glover; Frank Bigiel; Rupali Chandar; Eric Emsellem; Janice C. Lee; Adam K. Leroy; Karin M. Sandstrom; Eva Schinnerer; Erik Rosolowsky; Francesco Belfiore; Guillermo A. Blanc; Médéric Boquien; Jakob den Brok; Yixian Cao; Mélanie Chevance; Daniel A. Dale; Oleg V. Egorov; Cosima Eibensteiner; Kathryn Grasha; Brent Groves; Hamid Hassani; Jonathan D. Henshaw; Sarah Jeffreson; María J. Jiménez-Donaire; Benjamin W. Keller; Ralf S. Klessen; Eric W. Koch; J. M. Diederik Kruijssen; Kirsten L. Larson; Jing Li; Daizhong Liu; Laura A. Lopez; Eric J. Murphy; Lukas Neumann; Jérôme Pety; Francesca Pinna; Miguel Querejeta; Florent Renaud; Toshiki Saito; Sumit K. Sarbadhicary; Amy Sardone; Rowan J. Smith; Sophia K. Stuber; Jiayi Sun; David A. Thilker; Antonio Usero; Bradley C. Whitmore; Thomas G. Williams
Source
The Astrophysical Journal Letters, Vol 944, Iss 2, p L22 (2023)
Subject
Language
English
ISSN
2041-8213
2041-8205
2041-8205
Abstract
We present a high-resolution view of bubbles within the Phantom Galaxy (NGC 628), a nearby (∼10 Mpc), star-forming (∼2 M _⊙ yr ^−1 ), face-on ( i ∼ 9°) grand-design spiral galaxy. With new data obtained as part of the Physics at High Angular resolution in Nearby GalaxieS (PHANGS)-JWST treasury program, we perform a detailed case study of two regions of interest, one of which contains the largest and most prominent bubble in the galaxy (the Phantom Void, over 1 kpc in diameter), and the other being a smaller region that may be the precursor to such a large bubble (the Precursor Phantom Void). When comparing to matched-resolution H α observations from the Hubble Space Telescope, we see that the ionized gas is brightest in the shells of both bubbles, and is coincident with the youngest (∼1 Myr) and most massive (∼10 ^5 M _⊙ ) stellar associations. We also find an older generation (∼20 Myr) of stellar associations is present within the bubble of the Phantom Void. From our kinematic analysis of the H I , H _2 (CO), and H ii gas across the Phantom Void, we infer a high expansion speed of around 15 to 50 km s ^−1 . The large size and high expansion speed of the Phantom Void suggest that the driving mechanism is sustained stellar feedback due to multiple mechanisms, where early feedback first cleared a bubble (as we observe now in the Precursor Phantom Void), and since then supernovae have been exploding within the cavity and have accelerated the shell. Finally, comparison to simulations shows a striking resemblance to our JWST observations, and suggests that such large-scale, stellar-feedback-driven bubbles should be common within other galaxies.