PHANGS–JWST First Results: Mapping the 3.3 μm Polycyclic Aromatic Hydrocarbon Vibrational Band in Nearby Galaxies with NIRCam Medium Bands
We present maps of the 3.3 μ m 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 μ m PAH feature in the F335M filter (F3...
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IOP Publishing
2023-01-01
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| Series: | The Astrophysical Journal Letters |
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| Online Access: | https://doi.org/10.3847/2041-8213/acb0cf |
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| author | Karin M. Sandstrom Jérémy Chastenet Jessica Sutter Adam K. Leroy Oleg V. Egorov Thomas G. Williams Alberto D. Bolatto Médéric Boquien Yixian Cao Daniel A. Dale Janice C. Lee Erik Rosolowsky Eva Schinnerer Ashley. T. Barnes Francesco Belfiore F. Bigiel Mélanie Chevance Kathryn Grasha Brent Groves Hamid Hassani Annie Hughes Ralf S. Klessen J. M. Diederik Kruijssen Kirsten L. Larson Daizhong Liu Laura A. Lopez Sharon E. Meidt Eric J. Murphy Mattia C. Sormani David A. Thilker Elizabeth J. Watkins |
| author_facet | Karin M. Sandstrom Jérémy Chastenet Jessica Sutter Adam K. Leroy Oleg V. Egorov Thomas G. Williams Alberto D. Bolatto Médéric Boquien Yixian Cao Daniel A. Dale Janice C. Lee Erik Rosolowsky Eva Schinnerer Ashley. T. Barnes Francesco Belfiore F. Bigiel Mélanie Chevance Kathryn Grasha Brent Groves Hamid Hassani Annie Hughes Ralf S. Klessen J. M. Diederik Kruijssen Kirsten L. Larson Daizhong Liu Laura A. Lopez Sharon E. Meidt Eric J. Murphy Mattia C. Sormani David A. Thilker Elizabeth J. Watkins |
| author_sort | Karin M. Sandstrom |
| collection | DOAJ |
| description | We present maps of the 3.3 μ m 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 μ m PAH feature in the F335M filter (F335M _PAH ) 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 μ m. 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 F335M _PAH emission, we find that between 5% and 65% of the F335M intensity comes from the 3.3 μ m 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 μ m emission is well correlated with the 11.3 μ m PAH feature traced with the MIRI F1130W filter, as is expected, since both features arise from C–H vibrational modes. The average F335M _PAH /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. |
| first_indexed | 2024-03-12T03:37:05Z |
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| institution | Directory Open Access Journal |
| issn | 2041-8205 |
| language | English |
| last_indexed | 2024-03-12T03:37:05Z |
| publishDate | 2023-01-01 |
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| spelling | doaj.art-d15197a188b8491fb8c3b9df32c6ca712023-09-03T13:08:53ZengIOP PublishingThe Astrophysical Journal Letters2041-82052023-01-019442L710.3847/2041-8213/acb0cfPHANGS–JWST First Results: Mapping the 3.3 μm Polycyclic Aromatic Hydrocarbon Vibrational Band in Nearby Galaxies with NIRCam Medium BandsKarin M. Sandstrom0https://orcid.org/0000-0002-4378-8534Jérémy Chastenet1https://orcid.org/0000-0002-5235-5589Jessica Sutter2https://orcid.org/0000-0002-9183-8102Adam K. Leroy3https://orcid.org/0000-0002-2545-1700Oleg V. Egorov4https://orcid.org/0000-0002-4755-118XThomas G. Williams5https://orcid.org/0000-0002-0012-2142Alberto D. Bolatto6https://orcid.org/0000-0002-5480-5686Médéric Boquien7https://orcid.org/0000-0003-0946-6176Yixian Cao8https://orcid.org/0000-0001-5301-1326Daniel A. Dale9https://orcid.org/0000-0002-5782-9093Janice C. Lee10https://orcid.org/0000-0002-2278-9407Erik Rosolowsky11https://orcid.org/0000-0002-5204-2259Eva Schinnerer12https://orcid.org/0000-0002-3933-7677Ashley. T. Barnes13https://orcid.org/0000-0003-0410-4504Francesco Belfiore14https://orcid.org/0000-0002-2545-5752F. Bigiel15https://orcid.org/0000-0003-0166-9745Mélanie Chevance16https://orcid.org/0000-0002-5635-5180Kathryn Grasha17https://orcid.org/0000-0002-3247-5321Brent Groves18https://orcid.org/0000-0002-9768-0246Hamid Hassani19https://orcid.org/0000-0002-8806-6308Annie Hughes20https://orcid.org/0000-0002-9181-1161Ralf S. Klessen21https://orcid.org/0000-0002-0560-3172J. M. Diederik Kruijssen22https://orcid.org/0000-0002-8804-0212Kirsten L. Larson23https://orcid.org/0000-0003-3917-6460Daizhong Liu24https://orcid.org/0000-0001-9773-7479Laura A. Lopez25https://orcid.org/0000-0002-1790-3148Sharon E. Meidt26https://orcid.org/0000-0002-6118-4048Eric J. Murphy27https://orcid.org/0000-0001-7089-7325Mattia C. Sormani28https://orcid.org/0000-0001-6113-6241David A. Thilker29https://orcid.org/0000-0002-8528-7340Elizabeth J. Watkins30https://orcid.org/0000-0002-7365-5791Center for Astrophysics & Space Sciences, Department of Physics, University of California , San Diego, 9500 Gilman Drive, San Diego, CA 92093, USA kmsandstrom@ucsd.eduSterrenkundig Observatorium, Ghent University , Krijgslaan 281-S9, B-9000 Gent, BelgiumCenter for Astrophysics & Space Sciences, University of California , San Diego, 9500 Gilman Drive, San Diego, CA 92093, USADepartment of Astronomy, The Ohio State University , 140 West 18th Avenue, Columbus, OH 43210, USAAstronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg , Mönchhofstraße 12-14, D-69120 Heidelberg, GermanySub-department of Astrophysics, Department of Physics, University of Oxford , Keble Road, Oxford OX1 3RH, UK; Max-Planck-Institut für Astronomie , Königstuhl 17, D-69117 Heidelberg, GermanyDepartment of Astronomy and Joint Space-Science Institute, University of Maryland , College Park, MD 20742, USACentro de Astronomía (CITEVA), Universidad de Antofagasta , Avenida Angamos 601, Antofagasta, ChileMax-Planck-Institut für Extraterrestrische Physik (MPE) , Giessenbachstraße 1, D-85748 Garching, GermanyDepartment of Physics and Astronomy, University of Wyoming , Laramie, WY 82071, USAGemini Observatory/NSF’s NOIRLab , 950 N. Cherry Avenue, Tucson, AZ, USA; Steward Observatory, University of Arizona , 933 N. Cherry Ave, Tucson, AZ 85721, USADepartment of Physics, University of Alberta , Edmonton, Alberta, T6G 2E1, CanadaMax-Planck-Institut für Astronomie , Königstuhl 17, D-69117 Heidelberg, GermanyArgelander-Institut für Astronomie, Universität Bonn , Auf dem Hügel 71, D-53121 Bonn, GermanyINAF—Arcetri Astrophysical Observatory , Largo E. Fermi 5, I-50125, Florence, ItalyArgelander-Institut für Astronomie, Universität Bonn , Auf dem Hügel 71, D-53121 Bonn, GermanyUniversität Heidelberg , Zentrum für Astronomie, Institut für Theoretische Astrophysik, Albert-Ueberle-Straße 2, D-69120 Heidelberg, Germany; Cosmic Origins Of Life (COOL) Research DAOResearch School of Astronomy and Astrophysics, Australian National University , Canberra, ACT 2611, Australia; ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D) , AustraliaInternational Centre for Radio Astronomy Research, University of Western Australia , 7 Fairway, Crawley, 6009 WA, AustraliaDepartment of Physics, University of Alberta , Edmonton, Alberta, T6G 2E1, CanadaIRAP, Université de Toulouse , CNRS, CNES, UPS, (Toulouse), FranceUniversität Heidelberg , Zentrum für Astronomie, Institut für Theoretische Astrophysik, Albert-Ueberle-Straße 2, D-69120 Heidelberg, Germany; Universität Heidelberg , Interdisziplinäres Zentrum für Wissenschaftliches Rechnen, Im Neuenheimer Feld 205, D-69120 Heidelberg, GermanyCosmic Origins Of Life (COOL) Research DAOAURA for the European Space Agency (ESA), Space Telescope Science Institute , 3700 San Martin Drive, Baltimore, MD 21218, USAMax-Planck-Institut für Extraterrestrische Physik (MPE) , Giessenbachstraße 1, D-85748 Garching, GermanyDepartment of Astronomy, The Ohio State University , 140 West 18th Avenue, Columbus, OH 43210, USA; Center for Cosmology and Astroparticle Physics , 191 West Woodruff Avenue, Columbus, OH 43210, USA; Flatiron Institute , Center for Computational Astrophysics, NY 10010, USASterrenkundig Observatorium, Ghent University , Krijgslaan 281-S9, B-9000 Gent, BelgiumNational Radio Astronomy Observatory , 520 Edgemont Road, Charlottesville, VA 22903, USAUniversität Heidelberg , Zentrum für Astronomie, Institut für Theoretische Astrophysik, Albert-Ueberle-Straße 2, D-69120 Heidelberg, GermanyDepartment of Physics and Astronomy, The Johns Hopkins University , Baltimore, MD 21218, USAAstronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg , Mönchhofstraße 12-14, D-69120 Heidelberg, GermanyWe present maps of the 3.3 μ m 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 μ m PAH feature in the F335M filter (F335M _PAH ) 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 μ m. 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 F335M _PAH emission, we find that between 5% and 65% of the F335M intensity comes from the 3.3 μ m 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 μ m emission is well correlated with the 11.3 μ m PAH feature traced with the MIRI F1130W filter, as is expected, since both features arise from C–H vibrational modes. The average F335M _PAH /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.https://doi.org/10.3847/2041-8213/acb0cfPolycyclic aromatic hydrocarbonsInterstellar dustMedium band photometryJames Webb Space Telescope |
| spellingShingle | Karin M. Sandstrom Jérémy Chastenet Jessica Sutter Adam K. Leroy Oleg V. Egorov Thomas G. Williams Alberto D. Bolatto Médéric Boquien Yixian Cao Daniel A. Dale Janice C. Lee Erik Rosolowsky Eva Schinnerer Ashley. T. Barnes Francesco Belfiore F. Bigiel Mélanie Chevance Kathryn Grasha Brent Groves Hamid Hassani Annie Hughes Ralf S. Klessen J. M. Diederik Kruijssen Kirsten L. Larson Daizhong Liu Laura A. Lopez Sharon E. Meidt Eric J. Murphy Mattia C. Sormani David A. Thilker Elizabeth J. Watkins PHANGS–JWST First Results: Mapping the 3.3 μm Polycyclic Aromatic Hydrocarbon Vibrational Band in Nearby Galaxies with NIRCam Medium Bands The Astrophysical Journal Letters Polycyclic aromatic hydrocarbons Interstellar dust Medium band photometry James Webb Space Telescope |
| title | PHANGS–JWST First Results: Mapping the 3.3 μm Polycyclic Aromatic Hydrocarbon Vibrational Band in Nearby Galaxies with NIRCam Medium Bands |
| title_full | PHANGS–JWST First Results: Mapping the 3.3 μm Polycyclic Aromatic Hydrocarbon Vibrational Band in Nearby Galaxies with NIRCam Medium Bands |
| title_fullStr | PHANGS–JWST First Results: Mapping the 3.3 μm Polycyclic Aromatic Hydrocarbon Vibrational Band in Nearby Galaxies with NIRCam Medium Bands |
| title_full_unstemmed | PHANGS–JWST First Results: Mapping the 3.3 μm Polycyclic Aromatic Hydrocarbon Vibrational Band in Nearby Galaxies with NIRCam Medium Bands |
| title_short | PHANGS–JWST First Results: Mapping the 3.3 μm Polycyclic Aromatic Hydrocarbon Vibrational Band in Nearby Galaxies with NIRCam Medium Bands |
| title_sort | phangs jwst first results mapping the 3 3 μm polycyclic aromatic hydrocarbon vibrational band in nearby galaxies with nircam medium bands |
| topic | Polycyclic aromatic hydrocarbons Interstellar dust Medium band photometry James Webb Space Telescope |
| url | https://doi.org/10.3847/2041-8213/acb0cf |
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