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Barnes, AT 
ORCID: 0000-0003-0410-4504, Watkins, EJ ORCID: 0000-0002-7365-5791, Meidt, SE ORCID: 0000-0002-6118-4048, Kreckel, K ORCID: 0000-0001-6551-3091, Sormani, MC ORCID: 0000-0001-6113-6241, Treß, RG ORCID: 0000-0002-9483-7164, Glover, SCO ORCID: 0000-0001-6708-1317, Bigiel, F ORCID: 0000-0003-0166-9745, Chandar, R ORCID: 0000-0003-0085-4623, Emsellem, E ORCID: 0000-0002-6155-7166, Lee, JC ORCID: 0000-0002-2278-9407, Leroy, AK ORCID: 0000-0002-2545-1700, Sandstrom, KM ORCID: 0000-0002-4378-8534, Schinnerer, E ORCID: 0000-0002-3933-7677, Rosolowsky, E ORCID: 0000-0002-5204-2259, Belfiore, F ORCID: 0000-0002-2545-5752, Blanc, GA ORCID: 0000-0003-4218-3944, Boquien, M ORCID: 0000-0003-0946-6176, Brok, JD ORCID: 0000-0002-8760-6157, Cao, Y ORCID: 0000-0001-5301-1326 et al
(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 |
|---|---|
| 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 |
| Date of acceptance: | 29 November 2022 |
| Date of first compliant Open Access: | 15 June 2023 |
| Date Deposited: | 15 Jun 2023 12:11 |
| Last Modified: | 03 Jul 2025 12:34 |
| DOI or ID number: | 10.3847/2041-8213/aca7b9 |
| URI: | https://researchonline.ljmu.ac.uk/id/eprint/19846 |
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