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

Barnes, Ashley; Watkins, Elizabeth J.; Meidt, Sharon E.; Kreckel, Kathryn; Sormani, Mattia C.; Treß, Robin G.; Glover, Simon C. O.; Bigiel, Frank; Chandar, Rupali; Emsellem, Éric; Lee, Janice; Leroy, Adam K.; Sandström, Karin; Schinnerer, E.; Rosolowsky, Erik; Belfiore, Francesco; Blanc, Guillermo A.; Boquien, M.; Brok, Jakob S. den; Cao, Yixian; Chevance, Mélanie; Dale, Daniel A.; Egorov, Oleg V.; Eibensteiner, Cosima; Grasha, Kathryn; Groves, Brent; Hassani, Hamid; Henshaw, Jonathan D.; Jeffreson, Sarah; Jiménez-Donaire, María J.; Keller, Ben; Klessen, Ralf S.; Koch, Eric W.; Kruijssen, J. M. Diederik; Larson, Kirsten L.; Li, Jing; Liu, Daizhong; Lopez, Laura A.; Murphy, E. J.; Neumann, Lukáš; Pety, J.; Pinna, Francesca; Tosaki, Tomoka; Sarbadhicary, Sumit K.; Sardone, Amy; Smith, Rowan J.; Stuber, Sophia K.; Sun, Jiayi; Thilker, David A.; Usero, A.; Whitmore, Bradley C.; Williams, Thomas G.

doi:10.3847/2041-8213/aca7b9

Cited by 16 publications

(8 citation statements)

References 109 publications

(119 reference statements)

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“…In addition, the 3.3 μm feature can be mapped with NIRCam at 2-3 times finer angular resolution than the 7.7 μm or 11.3 μm bands, yielding 5-10 pc resolution in our targets. This allows measurements of the sizes of H II regions and bubbles (see Barnes et al 2023;Watkins et al 2023), the identification of filamentary structure (Meidt et al 2023;Thilker et al 2023), the identification of embedded clusters (Rodriguez et al 2023), and potentially tracing the gas column at higher resolution than is routinely possible with any millimeter or radio facilities (Leroy et al 2023;Sandstrom et al 2023).…”

Section: Discussionmentioning

confidence: 99%

PHANGS–JWST First Results: Mapping the 3.3 μm Polycyclic Aromatic Hydrocarbon Vibrational Band in Nearby Galaxies with NIRCam Medium Bands

Sandström¹,

Chastenet

Sutter

et al. 2023

ApJL

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We present maps of the 3.3 μm polycyclic aromatic hydrocarbon (PAH) emission feature in NGC 628, NGC 1365, and NGC 7496 as observed with the Near-Infrared Camera imager on JWST from the PHANGS–JWST Cycle 1 Treasury project. We create maps that isolate the 3.3 μm PAH feature in the F335M filter (F335MPAH) using combinations of the F300M and F360M filters for removal of starlight continuum. This continuum removal is complicated by contamination of the F360M by PAH emission and variations in the stellar spectral energy distribution slopes between 3.0 and 3.6 μm. We modify the empirical prescription from Lai et al. to remove the starlight continuum in our highly resolved galaxies, which have a range of starlight- and PAH-dominated lines of sight. Analyzing radially binned profiles of the F335MPAH emission, we find that between 5% and 65% of the F335M intensity comes from the 3.3 μm feature within the inner 0.5 r 25 of our targets. This percentage systematically varies from galaxy to galaxy and shows radial trends within the galaxies related to each galaxy’s distribution of stellar mass, interstellar medium, and star formation. The 3.3 μm emission is well correlated with the 11.3 μm PAH feature traced with the MIRI F1130W filter, as is expected, since both features arise from C–H vibrational modes. The average F335MPAH/F1130W ratio agrees with the predictions of recent models by Draine et al. for PAHs with size and charge distributions shifted toward larger grains with normal or higher ionization.

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Section: Discussionmentioning

confidence: 99%

PHANGS–JWST First Results: Mapping the 3.3 μm Polycyclic Aromatic Hydrocarbon Vibrational Band in Nearby Galaxies with NIRCam Medium Bands

Sandström¹,

Chastenet

Sutter

et al. 2023

ApJL

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“…In Watkins et al (2022), we only find 12 unbroken bubbles in NGC 628 in CO due to these constraints. HI emission offers an alternative, as can be seen in the THINGS HI map (Bagetakos et al 2011;Krause et al 2015), but at 200 pc resolution it resolves only the largest bubble features (Barnes et al 2023).…”

Section: A Panchromatic Picture Of Bubble Features In Ngc 628mentioning

confidence: 99%

“…Altogether, we find 31% of bubbles overlap with at least one smaller bubble, and bubble nesting occurs 3.2 times more often than expected from random chance, in total, when comparing the two. In future work, we will explore the exact nature of this relationship in more detail (i.e., whether the nested bubbles represent regions of new star formation, or have been simply relocated or uncovered by the expansion of the larger bubble; see Barnes et al 2023).…”

Section: Global Catalog Propertiesmentioning

confidence: 99%

“…Assuming that the deviation of the bubble axis ratio (q, which is the inverse of the aspect ratio) from unity originates entirely from the rotation curve, we can estimate the bubble expansion velocity, v exp , as a function of shear and galactocentric radius, and hence the time over which bubbles are visibly identifiable. For the exact details of the assumptions and method used in this estimate, see Barnes et al (2023), where it is presented in full.…”

Section: Expected Number Of Bubblesmentioning

confidence: 99%

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PHANGS–JWST First Results: A Statistical View on Bubble Evolution in NGC 628

Watkins¹,

Barnes

Henny

et al. 2023

ApJL

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The first JWST observations of nearby galaxies have unveiled a rich population of bubbles that trace the stellar-feedback mechanisms responsible for their creation. Studying these bubbles therefore allows us to chart the interaction between stellar feedback and the interstellar medium, and the larger galactic flows needed to regulate star formation processes globally. We present the first catalog of bubbles in NGC 628, visually identified using Mid-Infrared Instrument F770W Physics at High Angular resolution in Nearby GalaxieS (PHANGS)–JWST observations, and use them to statistically evaluate bubble characteristics. We classify 1694 structures as bubbles with radii between 6 and 552 pc. Of these, 31% contain at least one smaller bubble at their edge, indicating that previous generations of star formation have a local impact on where new stars form. On large scales, most bubbles lie near a spiral arm, and their radii increase downstream compared to upstream. Furthermore, bubbles are elongated in a similar direction to the spiral-arm ridgeline. These azimuthal trends demonstrate that star formation is intimately connected to the spiral-arm passage. Finally, the bubble size distribution follows a power law of index p = −2.2 ± 0.1, which is slightly shallower than the theoretical value by 1–3.5σ that did not include bubble mergers. The fraction of bubbles identified within the shells of larger bubbles suggests that bubble merging is a common process. Our analysis therefore allows us to quantify the number of star-forming regions that are influenced by an earlier generation, and the role feedback processes have in setting the global star formation rate. With the full PHANGS–JWST sample, we can do this for more galaxies.

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“…Figure 7 shows the filamentary organization of the gas in NGC 628, which prompted initial investigations of ISM structure using PAHs as ISM tracers (e.g., Sandstrom et al 2023b;Barnes et al 2023;Watkins et al 2023). Sandstrom et al (2023b) demonstrated a new JWST band combination that produces high-quality maps of the PAH feature at 3.3 μm with excellent stellar continuum subtraction.…”

Section: A High-resolution View Of the Neutral Ismmentioning

confidence: 99%

The PHANGS–JWST Treasury Survey: Star Formation, Feedback, and Dust Physics at High Angular Resolution in Nearby GalaxieS

Lee

Sandström

Leroy

et al. 2023

ApJL

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The PHANGS collaboration has been building a reference data set for the multiscale, multiphase study of star formation and the interstellar medium (ISM) in nearby galaxies. With the successful launch and commissioning of JWST, we can now obtain high-resolution infrared imaging to probe the youngest stellar populations and dust emission on the scales of star clusters and molecular clouds (∼5–50 pc). In Cycle 1, PHANGS is conducting an eight-band imaging survey from 2 to 21 μm of 19 nearby spiral galaxies. Optical integral field spectroscopy, CO(2–1) mapping, and UV-optical imaging for all 19 galaxies have been obtained through large programs with ALMA, VLT-MUSE, and Hubble. PHANGS–JWST enables a full inventory of star formation, accurate measurement of the mass and age of star clusters, identification of the youngest embedded stellar populations, and characterization of the physical state of small dust grains. When combined with Hubble catalogs of ∼10,000 star clusters, MUSE spectroscopic mapping of ∼20,000 H ii regions, and ∼12,000 ALMA-identified molecular clouds, it becomes possible to measure the timescales and efficiencies of the earliest phases of star formation and feedback, build an empirical model of the dependence of small dust grain properties on local ISM conditions, and test our understanding of how dust-reprocessed starlight traces star formation activity, all across a diversity of galactic environments. Here we describe the PHANGS–JWST Treasury survey, present the remarkable imaging obtained in the first few months of science operations, and provide context for the initial results presented in the first series of PHANGS–JWST publications.

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

Cited by 16 publications

References 109 publications

PHANGS–JWST First Results: Mapping the 3.3 μm Polycyclic Aromatic Hydrocarbon Vibrational Band in Nearby Galaxies with NIRCam Medium Bands

PHANGS–JWST First Results: Mapping the 3.3 μm Polycyclic Aromatic Hydrocarbon Vibrational Band in Nearby Galaxies with NIRCam Medium Bands

PHANGS–JWST First Results: A Statistical View on Bubble Evolution in NGC 628

The PHANGS–JWST Treasury Survey: Star Formation, Feedback, and Dust Physics at High Angular Resolution in Nearby GalaxieS

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