Institutional Repository of Radio Astronomy Research Laboratory
| Methanol masers in NGC 253 with ALCHEMI | |
Humire, P. K.1; Henkel, C.1,2,3 ; Hernandez-Gomez, A.1; Martin, S.4,5; Mangum, J.6; Harada, N.7,8,9; Muller, S.10; Sakamoto, K.8; Tanaka, K.11; Yoshimura, Y.12; Nakanishi, K.7,9; Muhle, S.13; Herrero-Illana, R.4,14; Meier, D. S.15,16; Caux, E.17; Aladro, R.1; Mauersberger, R.1; Viti, S.18,19; Colzi, L.20; Rivilla, V. M.20; Gorski, M.10; Menten, K. M.1; Huang, K. Y.18; Aalto, S.10; van der Werf, P. P.18; Emig, K. L.6
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| 2022-07-01 | |
| Source Publication | Astronomy & Astrophysics
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| ISSN | 0004-6361 |
| Volume | 663Pages:A33 |
| Contribution Rank | 3 |
| Abstract | Context. Methanol masers of Class I (collisionally pumped) and Class II (radiatively pumped) have been studied in great detail in our Galaxy in a variety of astrophysical environments such as shocks and star-forming regions and are they are helpful to analyze the properties of the dense interstellar medium. However, the study of methanol masers in external galaxies is still in its infancy. Aims. Our main goal is to search for methanol masers in the central molecular zone (CMZ; inner 500 pc) of the nearby starburst galaxy NGC 253. Methods. Covering a frequency range between 84 and 373 GHz (lambda = 3.6-0.8 mm) at high angular (1.('')6 similar to similar to 27 pc) and spectral (similar to 8-9 km s(-1)) resolution with ALCHEMI (ALMA Comprehensive High-resolution Extragalactic Molecular Inventory), we have probed different regions across the CMZ of NGC 253. In order to look for methanol maser candidates, we employed the rotation diagram method and a set of radiative transfer models. Results. We detect for the first time masers above 84 GHz in NGC 253, covering an ample portion of the J(-1)->(J - 1)(0) - E line series (at 84, 132, 229, and 278 GHz) and the J(0)->(J - 1)(1) - A series (at 95, 146, and 198 GHz). This confirms the presence of the Class I maser line at 84 GHz, which was already reported, but now being detected in more than one location. For the J(-1)->(J- 1)(0) - E line series, we observe a lack of Class I maser candidates in the central star-forming disk. Conclusions. The physical conditions for maser excitation in the J(-1)->(J - 1)(0) - E line series can be weak shocks and cloud-cloud collisions as suggested by shock tracers (SiO and HNCO) in bi-symmetric shock regions located in the outskirts of the CMZ. On the other hand, the presence of photodissociation regions due to a high star-formation rate would be needed to explain the lack of Class I masers in the very central regions. |
| Keyword | galaxies: spiral galaxies: starburst masers submillimeter: galaxies radio lines: galaxies resolved ammonia thermometry star-formation nuclear starburst shock tracers mega-masers ch3oh maser line survey galaxies emission ngc-253 Astronomy & Astrophysics |
| Subtype | Article |
| DOI | 10.1051/0004-6361/202243384 |
| URL | 查看原文 |
| Indexed By | SCI |
| Language | 英语 |
| WOS ID | WOS:000822072900003 |
| Citation statistics | |
| Document Type | 期刊论文 |
| Identifier | http://ir.xao.ac.cn/handle/45760611-7/5134 |
| Collection | 射电天文研究室_恒星形成与演化研究团组 |
| Affiliation | 1.Max-Planck-Institut für Radioastronomie, Auf-dem-Hügel 69, 53121 Bonn, Germany;; 2.Astron. Dept., Faculty of Science, King Abdulaziz University, PO Box 80203, Jeddah 21589, Saudi Arabia; 3.Xinjiang Astronomical Observatory, Chinese Academy of Sciences, 830011 Urumqi, PR China; 4.European Southern Observatory, Alonso de Córdova, 3107, Vitacura, Santiago 763-0355, Chile; 5.Joint ALMA Observatory, Alonso de Córdova, 3107, Vitacura, Santiago 763-0355, Chile; 6.National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA 22903-2475, USA; 7.National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan; 8.Institute of Astronomy and Astrophysics, Academia Sinica, 11F of AS/NTU Astronomy-Mathematics Building, No.1, Sec. 4, Roosevelt Rd, Taipei 10617, Taiwan; 9.Department of Astronomy, School of Science, The Graduate University for Advanced Studies (SOKENDAI), 2-21-1 Osawa, Mitaka, Tokyo 181-1855, Japan; 10.Department of Space, Earth and Environment, Chalmers University of Technology, Onsala Space Observatory, 43992 Onsala, Sweden; 11.Department of Physics, Faculty of Science and Technology, Keio University, 3-14-1 Hiyoshi, Yokohama, Kanagawa 223-8522, Japan; 12.Institute of Astronomy, Graduate School of Science, The University of Tokyo, 2-21-1 Osawa, Mitaka, Tokyo 181-0015, Japan; 13.Argelander-Institut für Astronomie, Universität Bonn, Auf dem Hügel 71, 53121 Bonn, Germany; 14.Institute of Space Sciences (ICE, CSIC), Campus UAB, Carrer de Magrans, 08193 Barcelona, Spain; 15.New Mexico Institute of Mining and Technology, 801 Leroy Place, Socorro, NM 87801, USA; 16.National Radio Astronomy Observatory, PO Box O, 1003 Lopezville Road, Socorro, NM 87801, USA; 17.IRAP, Université de Toulouse, CNRS, UPS, CNES, Toulouse, France; 18.Leiden Observatory, Leiden University, PO Box 9513, 2300 RA Leiden, The Netherlands; 19.Department of Physics and Astronomy, University College London, Gower Street, London WC1E6BT, UK; 20.Centro de Astrobiología (CSIC-INTA), Ctra. de Torrejón a Ajalvir km 4, 28850 Torrejón de Ardoz, Madrid, Spain |
| Recommended Citation GB/T 7714 | Humire, P. K.,Henkel, C.,Hernandez-Gomez, A.,et al. Methanol masers in NGC 253 with ALCHEMI[J]. Astronomy & Astrophysics,2022,663:A33. |
| APA | Humire, P. K..,Henkel, C..,Hernandez-Gomez, A..,Martin, S..,Mangum, J..,...&Emig, K. L..(2022).Methanol masers in NGC 253 with ALCHEMI.Astronomy & Astrophysics,663,A33. |
| MLA | Humire, P. K.,et al."Methanol masers in NGC 253 with ALCHEMI".Astronomy & Astrophysics 663(2022):A33. |
| Files in This Item: | ||||||
| File Name/Size | DocType | Version | Access | License | ||
| Humire-2022-Methanol（13444KB） | 期刊论文 | 出版稿 | 开放获取 | CC BY-NC-SA | View Application Full Text | |
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