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JWST Observations of Starbursts: Polycyclic Aromatic Hydrocarbon Emission at the Base of the M 82 Galactic Wind

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arxiv 2401.16648 v4 pith:2R7QM2NO submitted 2024-01-30 astro-ph.GA

JWST Observations of Starbursts: Polycyclic Aromatic Hydrocarbon Emission at the Base of the M 82 Galactic Wind

Alberto D. Bolatto , Rebecca C. Levy , Elizabeth Tarantino , Martha L. Boyer , Deanne B. Fisher , Adam K. Leroy , Serena A. Cronin , Ralf S. Klessen
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J. D. Smith Dannielle A. Berg Torsten Boeker Leindert A. Boogaard Eve C. Ostriker Todd A. Thompson Juergen Ott Laura Lenkic Laura A. Lopez Daniel A. Dale Sylvain Veilleux Paul P. van der Werf Simon C. O. Glover Karin M. Sandstrom Evan D. Skillman John Chisholm Vicente Villanueva Thomas S.-Y. Lai Sebastian Lopez Elisabeth A. C. Mills Kimberly L. Emig Lee Armus Divakara Maya David S. Meier Ilse De Looze Rodrigo Herrera-Camus Fabian Walter Monica Relano Hannah B. Koziol Joshua Marvil Maria J. Jimenez-Donaire Paul Martini
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We present new observations of the central 1 kpc of the M 82 starburst obtained with the James Webb Space Telescope (JWST) near-infrared camera (NIRCam) instrument at a resolution ~0.05"-0.1" (~1-2 pc). The data comprises images in three mostly continuum filters (F140M, F250M, and F360M), and filters that contain [FeII] (F164N), H2 v=1-0 (F212N), and the 3.3 um PAH feature (F335M). We find prominent plumes of PAH emission extending outward from the central starburst region, together with a network of complex filamentary substructure and edge-brightened bubble-like features. The structure of the PAH emission closely resembles that of the ionized gas, as revealed in Paschen alpha and free-free radio emission. We discuss the origin of the structure, and suggest the PAHs are embedded in a combination of neutral, molecular, and photoionized gas.

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Cited by 1 Pith paper

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  1. Survival is not Enough: Dust Sputtering, Growth, and H$_2$ Formation in Galactic Winds

    astro-ph.GA 2026-07 conditional novelty 7.5

    Entrained clouds form high H2 fractions only with dust growth at densities ≳10–30 times the cloud-survival critical density; without growth, DGR dilution and sputtering keep them atomic.