The Detection of Higher-order Millimeter Hydrogen Recombination Lines in the Large Magellanic Cloud
We report the first extragalactic detection of the higher-order millimeter hydrogen recombination lines (Δ n > 2). The γ -, ϵ -, and η -transitions have been detected toward the millimeter continuum source N 105–1 A in the star-forming region N 105 in the Large Magellanic Cloud with the Atacama L...
| Main Authors: | , , , , , , , , , , , , |
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| Format: | Article |
| Language: | English |
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IOP Publishing
2023-01-01
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| Series: | The Astrophysical Journal |
| Subjects: | |
| Online Access: | https://doi.org/10.3847/1538-4357/acf5ed |
| _version_ | 1827629993681747968 |
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| author | Marta Sewiło Kazuki Tokuda Stan E. Kurtz Steven B. Charnley Thomas Möller Jennifer Wiseman C.-H. Rosie Chen Remy Indebetouw Álvaro Sánchez-Monge Kei E. I. Tanaka Peter Schilke Toshikazu Onishi Naoto Harada |
| author_facet | Marta Sewiło Kazuki Tokuda Stan E. Kurtz Steven B. Charnley Thomas Möller Jennifer Wiseman C.-H. Rosie Chen Remy Indebetouw Álvaro Sánchez-Monge Kei E. I. Tanaka Peter Schilke Toshikazu Onishi Naoto Harada |
| author_sort | Marta Sewiło |
| collection | DOAJ |
| description | We report the first extragalactic detection of the higher-order millimeter hydrogen recombination lines (Δ n > 2). The γ -, ϵ -, and η -transitions have been detected toward the millimeter continuum source N 105–1 A in the star-forming region N 105 in the Large Magellanic Cloud with the Atacama Large Millimeter/submillimeter Array. We use the H40 α line, the brightest of the detected recombination lines (H40 α , H36 β , H50 β , H41 γ , H57 γ , H49 ϵ , H53 η , and H54 η ), to determine the electron temperature and study ionized gas kinematics in the region, and the 3 mm free–free continuum emission to determine the physical parameters: the size, emission measure, and electron density. We compare the physical properties of N 105–1 A to a large sample of Galactic compact and ultracompact (UC) H ii regions and conclude that N 105–1 A is similar to the most luminous ( L > 10 ^5 L _⊙ ) UC H ii regions in the Galaxy. N 105–1 A is ionized by an O5.5 V star; it is deeply embedded in its natal molecular clump, and likely associated with a (proto)cluster. We incorporate high-resolution molecular line data including CS, SO, SO _2 , and CH _3 OH (∼0.12 pc), and HCO ^+ and CO (∼0.087 pc) to explore the molecular environment of N 105–1 A. Based on the CO data, we find evidence for a cloud–cloud collision that likely triggered star formation in the region. We find no clear outflow signatures, but the presence of filaments and streamers indicates ongoing accretion onto the clump hosting the UC H ii region. Sulfur chemistry in N 105–1 A is consistent with the accretion shock model predictions. |
| first_indexed | 2024-03-09T14:00:07Z |
| format | Article |
| id | doaj.art-958b00ad68954f0cb5fde3108e81792c |
| institution | Directory Open Access Journal |
| issn | 1538-4357 |
| language | English |
| last_indexed | 2024-03-09T14:00:07Z |
| publishDate | 2023-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj.art-958b00ad68954f0cb5fde3108e81792c2023-11-30T09:31:38ZengIOP PublishingThe Astrophysical Journal1538-43572023-01-0195912210.3847/1538-4357/acf5edThe Detection of Higher-order Millimeter Hydrogen Recombination Lines in the Large Magellanic CloudMarta Sewiło0https://orcid.org/0000-0003-2248-6032Kazuki Tokuda1https://orcid.org/0000-0002-2062-1600Stan E. Kurtz2https://orcid.org/0000-0003-4444-5602Steven B. Charnley3https://orcid.org/0000-0001-6752-5109Thomas Möller4https://orcid.org/0000-0002-9277-8025Jennifer Wiseman5https://orcid.org/0000-0002-1143-6710C.-H. Rosie Chen6https://orcid.org/0000-0002-3925-9365Remy Indebetouw7https://orcid.org/0000-0002-4663-6827Álvaro Sánchez-Monge8https://orcid.org/0000-0002-3078-9482Kei E. I. Tanaka9https://orcid.org/0000-0002-6907-0926Peter Schilke10https://orcid.org/0000-0003-2141-5689Toshikazu Onishi11https://orcid.org/0000-0001-7826-3837Naoto Harada12https://orcid.org/0000-0002-8217-7509Exoplanets and Stellar Astrophysics Laboratory, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA ; marta.m.sewilo@nasa.gov; Department of Astronomy, University of Maryland , College Park, MD 20742, USA; Center for Research and Exploration in Space Science and Technology, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USADepartment of Earth and Planetary Sciences, Faculty of Science, Kyushu University , Nishi-ku, Fukuoka 819-0395, Japan; National Astronomical Observatory of Japan, National Institutes of Natural Sciences , 2-21-1 Osawa, Mitaka, Tokyo 181-8588, JapanInstituto de Radioastronomía y Astrofísica, Universidad Nacional Autónoma de México , Apdo. Postal 3-72, 58090 Morelia, Michoacán, MexicoAstrochemistry Laboratory, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USAI. Physikalisches Institut der Universität zu Köln , Zülpicher Str. 77, D-50937, Köln, GermanyExoplanets and Stellar Astrophysics Laboratory, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA ; marta.m.sewilo@nasa.govMax-Planck-Institut für Radioastronomie , Auf dem Hügel 69, D-53121 Bonn, GermanyDepartment of Astronomy, University of Virginia , P.O. Box 400325, Charlottesville, VA 22904, USA; National Radio Astronomy Observatory, 520 Edgemont Rd., Charlottesville, VA 22903, USAInstitut de Ciències de l’Espai (ICE, CSIC) , Can Magrans s/n, E-08193, Bellaterra, Barcelona, Spain; Institut d’Estudis Espacials de Catalunya (IEEC) , Barcelona, SpainTokyo Institute of Technology , 2 Chome-12-1 Ookayama, Meguro City, Tokyo 152-8550, JapanI. Physikalisches Institut der Universität zu Köln , Zülpicher Str. 77, D-50937, Köln, GermanyDepartment of Physics, Graduate School of Science, Osaka Metropolitan University , 1-1 Gakuen-cho, Naka-ku, Sakai, Osaka 599-8531, JapanDepartment of Earth and Planetary Sciences, Faculty of Science, Kyushu University , Nishi-ku, Fukuoka 819-0395, JapanWe report the first extragalactic detection of the higher-order millimeter hydrogen recombination lines (Δ n > 2). The γ -, ϵ -, and η -transitions have been detected toward the millimeter continuum source N 105–1 A in the star-forming region N 105 in the Large Magellanic Cloud with the Atacama Large Millimeter/submillimeter Array. We use the H40 α line, the brightest of the detected recombination lines (H40 α , H36 β , H50 β , H41 γ , H57 γ , H49 ϵ , H53 η , and H54 η ), to determine the electron temperature and study ionized gas kinematics in the region, and the 3 mm free–free continuum emission to determine the physical parameters: the size, emission measure, and electron density. We compare the physical properties of N 105–1 A to a large sample of Galactic compact and ultracompact (UC) H ii regions and conclude that N 105–1 A is similar to the most luminous ( L > 10 ^5 L _⊙ ) UC H ii regions in the Galaxy. N 105–1 A is ionized by an O5.5 V star; it is deeply embedded in its natal molecular clump, and likely associated with a (proto)cluster. We incorporate high-resolution molecular line data including CS, SO, SO _2 , and CH _3 OH (∼0.12 pc), and HCO ^+ and CO (∼0.087 pc) to explore the molecular environment of N 105–1 A. Based on the CO data, we find evidence for a cloud–cloud collision that likely triggered star formation in the region. We find no clear outflow signatures, but the presence of filaments and streamers indicates ongoing accretion onto the clump hosting the UC H ii region. Sulfur chemistry in N 105–1 A is consistent with the accretion shock model predictions.https://doi.org/10.3847/1538-4357/acf5edStar formationMagellanic CloudsStar forming regionsAstrochemistryMolecular cloudsH II regions |
| spellingShingle | Marta Sewiło Kazuki Tokuda Stan E. Kurtz Steven B. Charnley Thomas Möller Jennifer Wiseman C.-H. Rosie Chen Remy Indebetouw Álvaro Sánchez-Monge Kei E. I. Tanaka Peter Schilke Toshikazu Onishi Naoto Harada The Detection of Higher-order Millimeter Hydrogen Recombination Lines in the Large Magellanic Cloud The Astrophysical Journal Star formation Magellanic Clouds Star forming regions Astrochemistry Molecular clouds H II regions |
| title | The Detection of Higher-order Millimeter Hydrogen Recombination Lines in the Large Magellanic Cloud |
| title_full | The Detection of Higher-order Millimeter Hydrogen Recombination Lines in the Large Magellanic Cloud |
| title_fullStr | The Detection of Higher-order Millimeter Hydrogen Recombination Lines in the Large Magellanic Cloud |
| title_full_unstemmed | The Detection of Higher-order Millimeter Hydrogen Recombination Lines in the Large Magellanic Cloud |
| title_short | The Detection of Higher-order Millimeter Hydrogen Recombination Lines in the Large Magellanic Cloud |
| title_sort | detection of higher order millimeter hydrogen recombination lines in the large magellanic cloud |
| topic | Star formation Magellanic Clouds Star forming regions Astrochemistry Molecular clouds H II regions |
| url | https://doi.org/10.3847/1538-4357/acf5ed |
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