PHANGS–JWST First Results: Multiwavelength View of Feedback-driven Bubbles (the Phantom Voids) across NGC 628

The Astrophysical Journal. Letters

article

Ashley. T. Barnes¹  Elizabeth J. Watkins³  Sharon E. Meidt⁴  Kathryn Kreckel³  Mattia C. Sormani⁵  Robin G. Treß⁶  Simon C. O. Glover⁵  Frank Bigiel¹  Rupali Chandar⁷  Eric Emsellem²  Janice C. Lee⁹  Adam K. Leroy^1,10  Karin M. Sandstrom^1,12  Eva Schinnerer^1,13  Erik Rosolowsky^1,14  Francesco Belfiore^1,15  Guillermo A. Blanc^1,16  Médéric Boquien^1,18  Jakob den Brok¹  Yixian Cao^1,19  Mélanie Chevance⁵  Daniel A. Dale^2,21  Oleg V. Egorov³  Cosima Eibensteiner¹  Kathryn Grasha^2,22  Brent Groves^2,24  Hamid Hassani^1,14  Jonathan D. Henshaw^1,13  Sarah Jeffreson^2,26  María J. Jiménez-Donaire^2,27  Benjamin W. Keller^2,28  Ralf S. Klessen⁵  Eric W. Koch^2,26  J. M. Diederik Kruijssen^2,20  Kirsten L. Larson^3,30  Jing Li³  Daizhong Liu^1,19  Laura A. Lopez^1,10  Eric J. Murphy^3,32  Lukas Neumann¹  Jérôme Pety^3,33  Francesca Pinna^1,13  Miguel Querejeta^2,27  Florent Renaud^3,35  Toshiki Saito^3,36  Sumit K. Sarbadhicary^1,10  Amy Sardone^1,10  Rowan J. Smith^3,37  Sophia K. Stuber^1,13  Jiayi Sun^3,38  David A. Thilker^4,40  Antonio Usero^2,27  Bradley C. Whitmore^4,41  Thomas G. Williams^1,13 

[1] Argelander-Institut für Astronomie, Universität Bonn;European Southern Observatory;Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg;Sterrenkundig Observatorium, Universiteit Gent;Universität Heidelberg, Zentrum für Astronomie, Institut für Theoretische Astrophysik;Institute of Physics, Laboratory for Galaxy Evolution and Spectral Modelling;Ritter Astrophysical Research Center, University of Toledo;Univ Lyon, Univ Lyon1, ENS de Lyon, CNRS, Centre de Recherche Astrophysique de Lyon UMR5574;Gemini Observatory/NSF's NO iRLab;Department of Astronomy, The Ohio State University;Center for Cosmology and Astroparticle Physics;Department of Physics, University of California;Max-Planck-Institut für Astronomie;Department of Physics, University of Alberta;INAFArcetri Astrophysical Observatory;The Observatories of the Carnegie Institution for Science;Departamento de Astronomía, Universidad de Chile;Centro de Astronomía ,(CITEVA), Universidad de Antofagasta;Max-Planck-Institut für Extraterrestrische Physik;Cosmic Origins Of Life ,(COOL) Research DAO, coolresearch.io;Department of Physics and Astronomy, University of Wyoming;Research School of Astronomy and Astrophysics, Australian National University;ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions;International Center for Radio Astronomy Research, University of Western Australia;Astrophysics Research Institute, Liverpool John Moores University;Center for Astrophysics;Observatorio Astronómico Nacional;Department of Physics and Materials Science, University of Memphis;Universität Heidelberg;AURA for the European Space Agency ,(ESA), Space Telescope Science Institute;Flatiron Institute, Center for Computational Astrophysics;National Radio Astronomy Observatory;IRAM;LERMA, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Universités;Department of Astronomy and Theoretical Physics;National Astronomical Observatory of Japan;Jodrell Bank Centre for Astrophysics, Department of Physics and Astronomy, University of Manchester;Department of Physics and Astronomy, McMaster University;Canadian Institute for Theoretical Astrophysics ,(CITA), University of Toronto;Department of Physics and Astronomy, The Johns Hopkins University;Space Telescope Science Institute;Sub-department of Astrophysics, Department of Physics, University of Oxford

DOI  :  10.3847/2041-8213/aca7b9

来源: IOP Publishing Limited

【 摘 要 】

We present a high-resolution view of bubbles within the Phantom Galaxy (NGC 628), a nearby (∼10 Mpc), star-forming (∼2M _⊙ 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 αobservations 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 HI , H₂ (CO), and Hiigas 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.

【 授权许可】

Unknown