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

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

doi:10.3847/2041-8213/aca7b9

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

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

Physics And Astronomy

Producción científica: Article › revisión exhaustiva

57 Citas (Scopus)

Resumen

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.

Idioma original	English
Número de artículo	L22
Publicación	Astrophysical Journal Letters
Volumen	944
N.º	2
DOI	https://doi.org/10.3847/2041-8213/aca7b9
Estado	Published - feb 1 2023

Nota bibliográfica

Publisher Copyright:
© 2023. The Author(s). Published by the American Astronomical Society.

Financiación

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. 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.

Financiadores	Número del financiador
Australian Victorian Government
Centre National d’Etudes Spatiales
Instituto Nacional del Cáncer
Canadian Institute for Theoretical Astrophysics
CNRS Programme National Physique Chimie du Milieu Interstellaire
Smithsonian Institution
Commissariat à l'Énergie Atomique et aux Énergies Alternatives
Harvard Transdisciplinary Research in Energetics and Cancer Center, Harvard University
Instituto Nacional de Pediatria
Canadian Space Agency
H2020 European Research Council
Alexander von Humboldt-Stiftung
Horizon 2020
Natural Sciences and Engineering Research Council of Canada	CH2137/1-1
Science and Technology Facilities Council	ST/N00485X/1
German Ministry for Economic Affairs and Climate Action	KR4598/2-1, 50OO2206
Horizon 2020 Framework Programme	694343, 726384, 714907, 855130
Agencia Nacional de Investigación y Desarrollo	FB210003
Australian Research Council	DE220100766, CE170100013
Fondo Nacional de Desarrollo Científico y Tecnológico	1211000, RGPIN-2022-03499, EXC-2094-390783311
Knut och Alice Wallenbergs Stiftelse	BI1546/3-1, 1653300
National Science Foundation Arctic Social Science Program	2205628, JWST-GO-02107.009-A
German Excellence Strategy in the Heidelberg Cluster of Excellence STRUCTURES	EXC 2181-390900948
Deutsche Forschungsgemeinschaft	138713538, ANR-21-CE31-0010
Centre of Excellence for Integrative Brain Function, Australian Research Council	MCIN/AEI/10.13039/501100011033, PID2019-106027GA-C44

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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10.3847/2041-8213/aca7b9

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Barnes, A. T., Watkins, E. J., Meidt, S. E., Kreckel, K., Sormani, M. C., Treß, R. G., Glover, S. C. O., Bigiel, F., Chandar, R., Emsellem, E., Lee, J. C., Leroy, A. K., Sandstrom, K. M., Schinnerer, E., Rosolowsky, E., Belfiore, F., Blanc, G. A., Boquien, M., Brok, J. D., ... Williams, T. G. (2023). PHANGS-JWST First Results: Multiwavelength View of Feedback-driven Bubbles (the Phantom Voids) across NGC 628. Astrophysical Journal Letters, 944(2), Artículo L22. https://doi.org/10.3847/2041-8213/aca7b9

@article{16cc3830aec843fba0ce3036875534a1,

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

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.",

author = "Barnes, \{Ashley T.\} and Watkins, \{Elizabeth J.\} and Meidt, \{Sharon E.\} and Kathryn Kreckel and Sormani, \{Mattia C.\} and Tre{\ss}, \{Robin G.\} and Glover, \{Simon C.O.\} and Frank Bigiel and Rupali Chandar and Eric Emsellem and Lee, \{Janice C.\} and Leroy, \{Adam K.\} and Sandstrom, \{Karin M.\} and Eva Schinnerer and Erik Rosolowsky and Francesco Belfiore and Blanc, \{Guillermo A.\} and M{\'e}d{\'e}ric Boquien and Brok, \{Jakob den\} and Yixian Cao and M{\'e}lanie Chevance and Dale, \{Daniel A.\} and Egorov, \{Oleg V.\} and Cosima Eibensteiner and Kathryn Grasha and Brent Groves and Hamid Hassani and Henshaw, \{Jonathan D.\} and Sarah Jeffreson and Jim{\'e}nez-Donaire, \{Mar{\'i}a J.\} and Keller, \{Benjamin W.\} and Klessen, \{Ralf S.\} and Koch, \{Eric W.\} and Kruijssen, \{J. M.Diederik\} and Larson, \{Kirsten L.\} and Jing Li and Daizhong Liu and Lopez, \{Laura A.\} and Murphy, \{Eric J.\} and Lukas Neumann and J{\'e}r{\^o}me Pety and Francesca Pinna and Miguel Querejeta and Florent Renaud and Toshiki Saito and Sarbadhicary, \{Sumit K.\} and Amy Sardone and Smith, \{Rowan J.\} and Stuber, \{Sophia K.\} and Jiayi Sun and Thilker, \{David A.\} and Antonio Usero and Whitmore, \{Bradley C.\} and Williams, \{Thomas G.\}",

note = "Publisher Copyright: {\textcopyright} 2023. The Author(s). Published by the American Astronomical Society.",

year = "2023",

month = feb,

day = "1",

doi = "10.3847/2041-8213/aca7b9",

language = "English",

volume = "944",

number = "2",

}

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 & Williams, TG 2023, 'PHANGS-JWST First Results: Multiwavelength View of Feedback-driven Bubbles (the Phantom Voids) across NGC 628', Astrophysical Journal Letters, vol. 944, n.º 2, L22. https://doi.org/10.3847/2041-8213/aca7b9

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.

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 - https://www.scopus.com/pages/publications/85148700930

UR - https://www.scopus.com/pages/publications/85148700930#tab=citedBy

U2 - 10.3847/2041-8213/aca7b9

DO - 10.3847/2041-8213/aca7b9

M3 - Article

AN - SCOPUS:85148700930

SN - 2041-8205

VL - 944

JO - Astrophysical Journal Letters

JF - Astrophysical Journal Letters

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M1 - L22

ER -

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

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