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    Please use this identifier to cite or link to this item: https://tkuir.lib.tku.edu.tw/dspace/handle/987654321/124063

    Title: PHANGS-JWST First Results: Stellar-feedback-driven Excitation and Dissociation of Molecular Gas in the Starburst Ring of NGC 1365?
    Authors: Liu, Daizhong;Schinnerer, Eva;Cao, Yixian;Leroy, Adam;Usero, Antonio;Rosolowsky, Erik;Kruijssen, J. M. Diederik;Chevance, Mélanie;Glover, Simon C. O.;Sormani, Mattia C.;Bolatto, Alberto D.;Sun, Jiayi;Stuber, Sophia K.;Teng, Yu-Hsuan;Bigiel, Frank;Bešlić, Ivana;Grasha, Kathryn;Henshaw, Jonathan D.;Barnes, Ashley T.;Brok, Jakob S. den;Saito, Toshiki;Dale, Daniel A.;Watkins, Elizabeth J.;Pan, Hsi-An;Klessen, Ralf S.;Emsellem, Eric;Anand, Gagandeep S.;Deger, Sinan;Egorov, Oleg V.;Faesi, Christopher M.;Hassani, Hamid;Larson, Kirsten L.;Lee, Janice C.;Lopez, Laura A.;Pety, Jérôme;Sandstrom, Karin;Thilker, David A.;Whitmore, Bradley C.;Williams, Thomas G.
    Keywords: Interstellar medium;Molecular gas;Young massive clusters;Stellar feedback;Starburst galaxies;Interstellar line emission;Barred spiral galaxies;CO line emission;AGN host galaxies;Dust continuum emission
    Date: 2023-02-16
    Issue Date: 2023-05-12 12:06:03 (UTC+8)
    Publisher: American Astronomical Society
    Abstract: We compare embedded young massive star clusters (YMCs) to (sub-)millimeter line observations tracing the excitation and dissociation of molecular gas in the starburst ring of NGC 1365. This galaxy hosts one of the strongest nuclear starbursts and richest populations of YMCs within 20 Mpc. Here we combine near-/mid-IR PHANGS–JWST imaging with new Atacama Large Millimeter/submillimeter Array multi-J CO (1–0, 2–1 and 4–3) and [C i] (1–0) mapping, which we use to trace CO excitation via R42 = ICO(4−3)/ICO(2−1) and R21 = ICO(2−1)/ICO(1−0) and dissociation via RCICO = I[CI](1−0)/ICO(2−1) at 330 pc resolution. We find that the gas flowing into the starburst ring from northeast to southwest appears strongly affected by stellar feedback, showing decreased excitation (lower R42) and increased signatures of dissociation (higher RCICO) in the downstream regions. There, radiative-transfer modeling suggests that the molecular gas density decreases and temperature and [CI/CO] abundance ratio increase. We compare R42 and RCICO with local conditions across the regions and find that both correlate with near-IR 2 μm emission tracing the YMCs and with both polycyclic aromatic hydrocarbon (11.3 μm) and dust continuum (21 μm) emission. In general, RCICO exhibits ∼0.1 dex tighter correlations than R42, suggesting C i to be a more sensitive tracer of changing physical conditions in the NGC 1365 starburst than CO (4–3). Our results are consistent with a scenario where gas flows into the two arm regions along the bar, becomes condensed/shocked, forms YMCs, and then these YMCs heat and dissociate the gas.
    Relation: The Astrophysical Journal Letters 944(2)
    DOI: 10.3847/2041-8213/aca973
    Appears in Collections:[物理學系暨研究所] 期刊論文

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