The First Ka-band (26.1–35 GHz) Blind Line Survey toward Orion KL
We conducted a Ka -band (26.1–35 GHz) line survey toward Orion KL using the TianMa 65 m Radio Telescope (TMRT). It is the first blind line survey in the Ka band and achieves a sensitivity at the mK level (1–3 mK at a spectral resolution of ∼1 km s ^−1 ). In total, 592 Gaussian features are extracted...
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| Format: | Article |
| Language: | English |
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IOP Publishing
2024-01-01
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| Series: | The Astrophysical Journal Supplement Series |
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| Online Access: | https://doi.org/10.3847/1538-4365/ad1601 |
| _version_ | 1797316557951467520 |
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| author | Xunchuan Liu Tie Liu Zhiqiang Shen Sheng-Li Qin Qiuyi Luo Yan Gong Yu Cheng Christian Henkel Qilao Gu Fengyao Zhu Tianwei Zhang Rongbing Zhao Yajun Wu Bin Li Juan Li Zhang Zhao Jinqing Wang Weiye Zhong Qinghui Liu Bo Xia Li Fu Zhen Yan Chao Zhang Lingling Wang Qian Ye Aiyuan Yang Fengwei Xu Chao Zhang Somnath Dutta Shanghuo Li Meizhu Liu Dongting Yang Chuanshou Li Li Chen |
| author_facet | Xunchuan Liu Tie Liu Zhiqiang Shen Sheng-Li Qin Qiuyi Luo Yan Gong Yu Cheng Christian Henkel Qilao Gu Fengyao Zhu Tianwei Zhang Rongbing Zhao Yajun Wu Bin Li Juan Li Zhang Zhao Jinqing Wang Weiye Zhong Qinghui Liu Bo Xia Li Fu Zhen Yan Chao Zhang Lingling Wang Qian Ye Aiyuan Yang Fengwei Xu Chao Zhang Somnath Dutta Shanghuo Li Meizhu Liu Dongting Yang Chuanshou Li Li Chen |
| author_sort | Xunchuan Liu |
| collection | DOAJ |
| description | We conducted a Ka -band (26.1–35 GHz) line survey toward Orion KL using the TianMa 65 m Radio Telescope (TMRT). It is the first blind line survey in the Ka band and achieves a sensitivity at the mK level (1–3 mK at a spectral resolution of ∼1 km s ^−1 ). In total, 592 Gaussian features are extracted. Among them, 257 radio recombination lines (RRLs) are identified. The maximum Δ n of RRLs of H, He, and C are 20, 15, and 5, respectively. Through stacking, we have detected the β lines of ion RRLs (RRLs of C ^+ with the possible contribution of other ions like O ^+ ) for the first time, and a tentative signal of the γ lines of ion RRLs can also be seen on the stacked spectrum. Besides this, 318 other line features were assigned to 37 molecular species, and 10 of these species were not detected in the Q -band survey of TMRT. The vibrationally excited states of nine species were also detected. The emission of most species can be modeled under LTE. A number of transitions of E-CH3OH ( J _2 − J _1 ) display maser effects, which are confirmed by our modeling, and besides the bumping peak at J ∼ 6, there is another peak at J ∼ 13. Methylcyanoacetylene (CH _3 C _3 N) is detected in Orion KL for the first time. This work emphasizes that the Ka band, which was long ignored for spectral line surveys, is very useful for surveying RRLs and molecular lines simultaneously. |
| first_indexed | 2024-03-08T03:21:05Z |
| format | Article |
| id | doaj.art-f2369859f3864586916b88cd76a8fe98 |
| institution | Directory Open Access Journal |
| issn | 0067-0049 |
| language | English |
| last_indexed | 2024-03-08T03:21:05Z |
| publishDate | 2024-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal Supplement Series |
| spelling | doaj.art-f2369859f3864586916b88cd76a8fe982024-02-12T10:14:47ZengIOP PublishingThe Astrophysical Journal Supplement Series0067-00492024-01-012711310.3847/1538-4365/ad1601The First Ka-band (26.1–35 GHz) Blind Line Survey toward Orion KLXunchuan Liu0https://orcid.org/0000-0001-8315-4248Tie Liu1https://orcid.org/0000-0002-5286-2564Zhiqiang Shen2https://orcid.org/0000-0003-3540-8746Sheng-Li Qin3https://orcid.org/0000-0003-2302-0613Qiuyi Luo4https://orcid.org/0000-0003-4506-3171Yan Gong5Yu Cheng6https://orcid.org/0000-0002-8691-4588Christian Henkel7https://orcid.org/0000-0002-7495-4005Qilao Gu8Fengyao Zhu9Tianwei Zhang10https://orcid.org/0000-0002-1466-3484Rongbing Zhao11Yajun Wu12Bin Li13Juan Li14https://orcid.org/0000-0003-3520-6191Zhang Zhao15Jinqing Wang16Weiye Zhong17Qinghui Liu18Bo Xia19Li Fu20Zhen Yan21https://orcid.org/0000-0002-9322-9319Chao Zhang22https://orcid.org/0000-0002-5682-2906Lingling Wang23Qian Ye24Aiyuan Yang25https://orcid.org/0000-0003-4546-2623Fengwei Xu26https://orcid.org/0000-0001-5950-1932Chao Zhang27https://orcid.org/0000-0002-5682-2906Somnath Dutta28https://orcid.org/0000-0002-2338-4583Shanghuo Li29https://orcid.org/0000-0003-1275-5251Meizhu Liu30Dongting Yang31Chuanshou Li32Li Chen33Shanghai Astronomical Observatory, Chinese Academy of Sciences , Shanghai 200030, People’s Republic of China ; liuxunchuan@shao.ac.cn, liutie@shao.ac.cn, zshen@shao.ac.cnShanghai Astronomical Observatory, Chinese Academy of Sciences , Shanghai 200030, People’s Republic of China ; liuxunchuan@shao.ac.cn, liutie@shao.ac.cn, zshen@shao.ac.cnShanghai Astronomical Observatory, Chinese Academy of Sciences , Shanghai 200030, People’s Republic of China ; liuxunchuan@shao.ac.cn, liutie@shao.ac.cn, zshen@shao.ac.cnSchool of Physics and Astronomy, Yunnan University , Kunming, 650091, People’s Republic of ChinaShanghai Astronomical Observatory, Chinese Academy of Sciences , Shanghai 200030, People’s Republic of China ; liuxunchuan@shao.ac.cn, liutie@shao.ac.cn, zshen@shao.ac.cnMax-Planck-Institut für Radioastronomie , Auf dem Hügel 69, D-53125 Bonn, GermanyNational Astronomical Observatory of Japan , 2-21-1 Osawa, Mitaka, Tokyo, 181-8588, JapanMax-Planck-Institut für Radioastronomie , Auf dem Hügel 69, D-53125 Bonn, GermanyShanghai Astronomical Observatory, Chinese Academy of Sciences , Shanghai 200030, People’s Republic of China ; liuxunchuan@shao.ac.cn, liutie@shao.ac.cn, zshen@shao.ac.cnCenter for Intelligent Computing Platforms , Zhejiang Laboratory, Hangzhou, 311100, People’s Republic of ChinaI. Physikalisches Institut, Universität zu Köln , Zülpicher Straße 77, D-50937 Köln, GermanyShanghai Astronomical Observatory, Chinese Academy of Sciences , Shanghai 200030, People’s Republic of China ; liuxunchuan@shao.ac.cn, liutie@shao.ac.cn, zshen@shao.ac.cnShanghai Astronomical Observatory, Chinese Academy of Sciences , Shanghai 200030, People’s Republic of China ; liuxunchuan@shao.ac.cn, liutie@shao.ac.cn, zshen@shao.ac.cnShanghai Astronomical Observatory, Chinese Academy of Sciences , Shanghai 200030, People’s Republic of China ; liuxunchuan@shao.ac.cn, liutie@shao.ac.cn, zshen@shao.ac.cnShanghai Astronomical Observatory, Chinese Academy of Sciences , Shanghai 200030, People’s Republic of China ; liuxunchuan@shao.ac.cn, liutie@shao.ac.cn, zshen@shao.ac.cnShanghai Astronomical Observatory, Chinese Academy of Sciences , Shanghai 200030, People’s Republic of China ; liuxunchuan@shao.ac.cn, liutie@shao.ac.cn, zshen@shao.ac.cnShanghai Astronomical Observatory, Chinese Academy of Sciences , Shanghai 200030, People’s Republic of China ; liuxunchuan@shao.ac.cn, liutie@shao.ac.cn, zshen@shao.ac.cnShanghai Astronomical Observatory, Chinese Academy of Sciences , Shanghai 200030, People’s Republic of China ; liuxunchuan@shao.ac.cn, liutie@shao.ac.cn, zshen@shao.ac.cnShanghai Astronomical Observatory, Chinese Academy of Sciences , Shanghai 200030, People’s Republic of China ; liuxunchuan@shao.ac.cn, liutie@shao.ac.cn, zshen@shao.ac.cnShanghai Astronomical Observatory, Chinese Academy of Sciences , Shanghai 200030, People’s Republic of China ; liuxunchuan@shao.ac.cn, liutie@shao.ac.cn, zshen@shao.ac.cnShanghai Astronomical Observatory, Chinese Academy of Sciences , Shanghai 200030, People’s Republic of China ; liuxunchuan@shao.ac.cn, liutie@shao.ac.cn, zshen@shao.ac.cnShanghai Astronomical Observatory, Chinese Academy of Sciences , Shanghai 200030, People’s Republic of China ; liuxunchuan@shao.ac.cn, liutie@shao.ac.cn, zshen@shao.ac.cnShanghai Astronomical Observatory, Chinese Academy of Sciences , Shanghai 200030, People’s Republic of China ; liuxunchuan@shao.ac.cn, liutie@shao.ac.cn, zshen@shao.ac.cnShanghai Astronomical Observatory, Chinese Academy of Sciences , Shanghai 200030, People’s Republic of China ; liuxunchuan@shao.ac.cn, liutie@shao.ac.cn, zshen@shao.ac.cnShanghai Astronomical Observatory, Chinese Academy of Sciences , Shanghai 200030, People’s Republic of China ; liuxunchuan@shao.ac.cn, liutie@shao.ac.cn, zshen@shao.ac.cnNational Astronomical Observatories, Chinese Academy of Sciences , Beijing 100101, People’s Republic of China; Key Laboratory of Radio Astronomy and Technology, Chinese Academy of Sciences , A20 Datun Road, Chaoyang District, Beijing, 100101, People’s Republic of ChinaKavli Institute for Astronomy and Astrophysics, Peking University , 5 Yiheyuan Road, Haidian District, Beijing 100871, People’s Republic of ChinaInstitute of Astronomy and Astrophysics, School of Mathematics and Physics, Anqing Normal University , Anqing, People’s Republic of ChinaInstitute of Astronomy and Astrophysics , Academia Sinica, Roosevelt Road, Taipei 10617, Taiwan (R.O.C)Max Planck Institute for Astronomy , Königstuhl 17, D-69117 Heidelberg, GermanySchool of Physics and Astronomy, Yunnan University , Kunming, 650091, People’s Republic of ChinaSchool of Physics and Astronomy, Yunnan University , Kunming, 650091, People’s Republic of ChinaSchool of Physics and Astronomy, Yunnan University , Kunming, 650091, People’s Republic of ChinaSchool of Physics and Astronomy, Yunnan University , Kunming, 650091, People’s Republic of ChinaWe conducted a Ka -band (26.1–35 GHz) line survey toward Orion KL using the TianMa 65 m Radio Telescope (TMRT). It is the first blind line survey in the Ka band and achieves a sensitivity at the mK level (1–3 mK at a spectral resolution of ∼1 km s ^−1 ). In total, 592 Gaussian features are extracted. Among them, 257 radio recombination lines (RRLs) are identified. The maximum Δ n of RRLs of H, He, and C are 20, 15, and 5, respectively. Through stacking, we have detected the β lines of ion RRLs (RRLs of C ^+ with the possible contribution of other ions like O ^+ ) for the first time, and a tentative signal of the γ lines of ion RRLs can also be seen on the stacked spectrum. Besides this, 318 other line features were assigned to 37 molecular species, and 10 of these species were not detected in the Q -band survey of TMRT. The vibrationally excited states of nine species were also detected. The emission of most species can be modeled under LTE. A number of transitions of E-CH3OH ( J _2 − J _1 ) display maser effects, which are confirmed by our modeling, and besides the bumping peak at J ∼ 6, there is another peak at J ∼ 13. Methylcyanoacetylene (CH _3 C _3 N) is detected in Orion KL for the first time. This work emphasizes that the Ka band, which was long ignored for spectral line surveys, is very useful for surveying RRLs and molecular lines simultaneously.https://doi.org/10.3847/1538-4365/ad1601Single-dish antennasMillimeter astronomyRadio spectroscopyStar formationYoung stellar objectsOB stars |
| spellingShingle | Xunchuan Liu Tie Liu Zhiqiang Shen Sheng-Li Qin Qiuyi Luo Yan Gong Yu Cheng Christian Henkel Qilao Gu Fengyao Zhu Tianwei Zhang Rongbing Zhao Yajun Wu Bin Li Juan Li Zhang Zhao Jinqing Wang Weiye Zhong Qinghui Liu Bo Xia Li Fu Zhen Yan Chao Zhang Lingling Wang Qian Ye Aiyuan Yang Fengwei Xu Chao Zhang Somnath Dutta Shanghuo Li Meizhu Liu Dongting Yang Chuanshou Li Li Chen The First Ka-band (26.1–35 GHz) Blind Line Survey toward Orion KL The Astrophysical Journal Supplement Series Single-dish antennas Millimeter astronomy Radio spectroscopy Star formation Young stellar objects OB stars |
| title | The First Ka-band (26.1–35 GHz) Blind Line Survey toward Orion KL |
| title_full | The First Ka-band (26.1–35 GHz) Blind Line Survey toward Orion KL |
| title_fullStr | The First Ka-band (26.1–35 GHz) Blind Line Survey toward Orion KL |
| title_full_unstemmed | The First Ka-band (26.1–35 GHz) Blind Line Survey toward Orion KL |
| title_short | The First Ka-band (26.1–35 GHz) Blind Line Survey toward Orion KL |
| title_sort | first ka band 26 1 35 ghz blind line survey toward orion kl |
| topic | Single-dish antennas Millimeter astronomy Radio spectroscopy Star formation Young stellar objects OB stars |
| url | https://doi.org/10.3847/1538-4365/ad1601 |
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