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Barnes, AT, Watkins, EJ, Meidt, SE, Kreckel, K, Sormani, MC, Treß, RG, Glover, SCO, Bigiel, F, Chandar, R, Emsellem, E, Lee, JC, Leroy, AK, Sandstrom, KM, Schinnerer, E, Rosolowsky, E, Belfiore, F, Blanc, GA, Boquien, M, Brok, JD, Cao, Y , Chevance, M, Dale, DA, Egorov, OV, Eibensteiner, C, Grasha, K, Groves, B, Hassani, H, Henshaw, JD, Jeffreson, S, Jiménez-Donaire, MJ, Keller, BW, Klessen, RS, Koch, EW, Kruijssen, JMD, Larson, KL, Li, J, Liu, D, Lopez, LA, Murphy, EJ, Neumann, L, Pety, J, Pinna, F, Querejeta, M, Renaud, F, Saito, T, Sarbadhicary, SK, Sardone, A, Smith, RJ, Stuber, SK, Sun, J, Thilker, DA, Usero, A, Whitmore, BC and Williams, TG (2023) PHANGS-JWST First Results: Multiwavelength View of Feedback-driven Bubbles (the Phantom Voids) across NGC 628. Astrophysical Journal Letters, 944 (2). L22-L22. ISSN 2041-8205
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PHANGS-JWST First Results Multiwavelength View of Feedback-driven Bubbles (the Phantom Voids) across NGC 628.pdf - Published Version Available under License Creative Commons Attribution. Download (7MB) | Preview |
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 Hα 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 (∼105 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, H2 (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.
| Item Type: | Article |
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| Uncontrolled Keywords: | 0201 Astronomical and Space Sciences; Astronomy & Astrophysics |
| Subjects: | Q Science > QB Astronomy Q Science > QC Physics |
| Divisions: | Astrophysics Research Institute |
| Publisher: | American Astronomical Society |
| SWORD Depositor: | A Symplectic |
| Date Deposited: | 15 Jun 2023 12:11 |
| Last Modified: | 15 Jun 2023 12:15 |
| DOI or ID number: | 10.3847/2041-8213/aca7b9 |
| URI: | https://researchonline.ljmu.ac.uk/id/eprint/19846 |
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