TY - JOUR
T1 - PHANGS-JWST First Results
T2 - Multiwavelength View of Feedback-driven Bubbles (the Phantom Voids) across NGC 628
AU - Barnes, Ashley T.
AU - Watkins, Elizabeth J.
AU - Meidt, Sharon E.
AU - Kreckel, Kathryn
AU - Sormani, Mattia C.
AU - Treß, Robin G.
AU - Glover, Simon C.O.
AU - Bigiel, Frank
AU - Chandar, Rupali
AU - Emsellem, Eric
AU - Lee, Janice C.
AU - Leroy, Adam K.
AU - Sandstrom, Karin M.
AU - Schinnerer, Eva
AU - Rosolowsky, Erik
AU - Belfiore, Francesco
AU - Blanc, Guillermo A.
AU - Boquien, Médéric
AU - Brok, Jakob den
AU - Cao, Yixian
AU - Chevance, Mélanie
AU - Dale, Daniel A.
AU - Egorov, Oleg V.
AU - Eibensteiner, Cosima
AU - Grasha, Kathryn
AU - Groves, Brent
AU - Hassani, Hamid
AU - Henshaw, Jonathan D.
AU - Jeffreson, Sarah
AU - Jiménez-Donaire, María J.
AU - Keller, Benjamin W.
AU - Klessen, Ralf S.
AU - Koch, Eric W.
AU - Kruijssen, J. M.Diederik
AU - Larson, Kirsten L.
AU - Li, Jing
AU - Liu, Daizhong
AU - Lopez, Laura A.
AU - Murphy, Eric J.
AU - Neumann, Lukas
AU - Pety, Jérôme
AU - Pinna, Francesca
AU - Querejeta, Miguel
AU - Renaud, Florent
AU - Saito, Toshiki
AU - Sarbadhicary, Sumit K.
AU - Sardone, Amy
AU - Smith, Rowan J.
AU - Stuber, Sophia K.
AU - Sun, Jiayi
AU - Thilker, David A.
AU - Usero, Antonio
AU - Whitmore, Bradley C.
AU - Williams, Thomas G.
N1 - Funding Information:
A.T.B. and F.B. would like to acknowledge funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program (grant agreement No. 726384/Empire). E.J.W. acknowledges the funding provided by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation)—Project-ID 138713538—SFB 881 (“The Milky Way System”, subproject P1). J.P.e. acknowledges support by the DAO i SM grant No. ANR-21-CE31-0010 and by the Programme National “Physique et Chimie du Milieu Interstellaire” (PCMI) of CNRS/INSU with INC/INP, cofunded by CEA and CNES. E.W.K. acknowledges support from the Smithsonian Institution as a Submillimeter Array (SMA) Fellow and the Natural Sciences and Engineering Research Council of Canada. J.M.D.K. gratefully acknowledges funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program via the ERC Starting Grant MUSTANG (grant No. 714907). COOL Research DAO is a Decentralized Autonomous Organization supporting research in astrophysics aimed at uncovering our cosmic origins. M.C. gratefully acknowledges funding from the DFG through an Emmy Noether Research Group (grant No. CH2137/1-1). R.S.K. acknowledges funding from the European Research Council via the ERC Synergy Grant “ECOGAL” (project ID 855130), from the Deutsche Forschungsgemeinschaft (DFG) via the Collaborative Research Center “The Milky Way System” (SFB 881—funding ID 138713538—subprojects A1, B1, B2, and B8) and from the Heidelberg Cluster of Excellence (EXC 2181-390900948) “STRUCTURES”, funded by the German Excellence Strategy. R.S.K. also thanks the German Ministry for Economic Affairs and Climate Action for funding in the project “MAINN” (funding ID 50OO2206). T.G.W. acknowledges funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program (grant No. 694343). K.K. and O.E. gratefully acknowledge funding from the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) in the form of an Emmy Noether Research Group (grant No. KR4598/2-1; PI: Kreckel). G.A.B. acknowledges the support from ANID Basal project FB210003. S.J. is supported by Harvard University through the ITC. M.B. acknowledges support from FONDECYT regular grant 1211000 and by the ANID BASAL project FB210003. E.R. acknowledges the support of the Natural Sciences and Engineering Research Council of Canada (NSERC), funding reference number RGPIN-2022-03499. This research was supported by the Excellence Cluster ORIGINS which is funded by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) under Germany's Excellence Strategy—EXC-2094-390783311. Some of the simulations in this paper have been carried out on the computing facilities of the Computational Center for Particle and Astrophysics (C2PAP). E.E. would like to thank Alexey Krukau and Margarita Petkova for their support through C2PAP. K.G. is supported by the Australian Research Council through the Discovery Early Career Researcher Award (DECRA) Fellowship DE220100766 funded by the Australian Government. K.G. is supported by the Australian Research Council Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), through project number CE170100013. M.Q. acknowledges support from the Spanish grant No. PID2019-106027GA-C44, funded by MCIN/AEI/10.13039/501100011033. F.R. acknowledges support from the Knut and Alice Wallenberg Foundation. C.E. acknowledges funding from the Deutsche Forschungsgemeinschaft (DFG) Sachbeihilfe, grant No. BI1546/3-1 A.K.L. gratefully acknowledges support by grant Nos. 1653300 and 2205628 from the National Science Foundation, by award JWST-GO-02107.009-A, and by a Humboldt Research Award from the Alexander von Humboldt Foundation. J.S. acknowledges support by the Natural Sciences and Engineering Research Council of Canada (NSERC) through a Canadian Institute for Theoretical Astrophysics (CITA) National Fellowship.
Funding Information:
This work also makes use of observations collected at the European Southern Observatory under ESO programmes 094.C-0623 (PI: Kreckel), 095.C-0473, 098.C-0484 (PI: Blanc), 1100.B-0651 (PHANGS–MUSE; PI: Schinnerer), as well as 094.B-0321 (MAGNUM; PI: Marconi), 099.B-0242, 0100.B-0116, 098.B-0551 (MAD; PI: Carollo) and 097.B-0640 (TIMER; PI: Gadotti). This publication uses the data from the AstroSat mission and the UVIT instrument of the Indian Space Research Organisation (ISRO), archived at the Indian Space Science Data center (ISSDC). This work is supported by a grant 19ASTROSA2 from the Canadian Space Agency.
Publisher Copyright:
© 2023. The Author(s). Published by the American Astronomical Society.
PY - 2023/2/1
Y1 - 2023/2/1
N2 - 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.
AB - 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.
UR - http://www.scopus.com/inward/record.url?scp=85148700930&partnerID=8YFLogxK
U2 - 10.3847/2041-8213/aca7b9
DO - 10.3847/2041-8213/aca7b9
M3 - Article
AN - SCOPUS:85148700930
SN - 2041-8205
VL - 944
JO - The Astrophysical Journal Letters
JF - The Astrophysical Journal Letters
IS - 2
M1 - L22
ER -