The MALATANG Survey: The LGAS–LIR Correlation on Sub-kiloparsec Scale in Six Nearby Star-forming Galaxies as Traced by HCN J?=?4?→?3 and HCO+ J?=?4?→?3
文献类型：期刊论文
| 作者 | Tan,Qing-Hua2; Gao,Yu2; Zhang,Zhi-Yu3,4; Greve,Thomas R.5; Jiang,Xue-Jian2; Wilson,Christine D.6; Yang,Chen-Tao2,7,8; Bemis,Ashley6; Chung,Aeree9; Matsushita,Satoki1 |
| 刊名 | The Astrophysical Journal
 |
| 出版日期 | 2018-06-25 |
| 卷号 | 860期号:2 |
| 关键词 | galaxies: ISM galaxies: star formation infrared: galaxies ISM: molecules radio lines: galaxies |
| ISSN号 | 0004-637X |
| DOI | 10.3847/1538-4357/aac512 |
| 英文摘要 | Abstract We present and maps of six nearby star-forming galaxies, NGC 253, NGC 1068, IC 342, M82, M83, and NGC 6946, obtained with the James Clerk Maxwell Telescope as part of the MALATANG survey. All galaxies were mapped in the central 2′?×?2′?region at 14″ (FWHM) resolution (corresponding to linear scales of ～0.2–1.0 kpc). The LIR–L′dense relation, where the dense gas is traced by the and the emission, measured in our sample of spatially resolved galaxies is found to follow the linear correlation established globally in galaxies within the scatter. We find that the luminosity ratio, LIR/L′dense, shows systematic variations with LIR within individual spatially resolved galaxies, whereas the galaxy-integrated ratios vary little. A rising trend is also found between LIR/L′dense ratio and the warm-dust temperature gauged by the 70 μm/100 μm flux ratio. We find that the luminosity ratios of IR/HCN (4–3) and IR/HCO+ (4–3), which can be taken as a proxy for the star formation efficiency (SFE) in the dense molecular gas (SFEdense), appear to be nearly independent of the dense gas fraction (fdense) for our sample of galaxies. The SFE of the total molecular gas (SFEmol) is found to increase substantially with fdense when combining our data with those on local (ultra)luminous infrared galaxies and high-z quasars. The mean line ratio measured for the six targeted galaxies is 0.9?±?0.6. No significant correlation is found for the ratio with the star formation rate as traced by LIR, nor with the warm-dust temperature, for the different populations of galaxies. |
| 语种 | 英语 |
| WOS记录号 | IOP:0004-637X-860-2-AAC512 |
| 出版者 | The American Astronomical Society |
| 源URL | [http://ir.bao.ac.cn/handle/114a11/35538]  |
| 专题 | 中国科学院国家天文台 |
| 作者单位 | 1.Academia Sinica Institute of Astronomy and Astrophysics, P.O. Box 23-141, Taipei 10617, Taiwan 2.Purple Mountain Observatory & Key Laboratory for Radio Astronomy, Chinese Academy of Sciences, 8 Yuanhua Road, Nanjing 210034, People’s Republic of China; qhtan@pmo.ac.cn, yugao@pmo.ac.cn 3.Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ, UK 4.ESO, Karl-Schwarzschild-Str. 2, D-85748 Garching, Germany 5.Department of Physics and Astronomy, University College London, Gower Street, London WC1E6BT, UK 6.Department of Physics and Astronomy, McMaster University, Hamilton, ON L8S 4M1, Canada 7.Institut d’Astrophysique Spatiale, CNRS, Univ. Paris-Sud, Université Paris-Saclay, Bāt. 121, F-91405, Orsay Cedex, France 8.European Southern Observatory, Alonso de Córdova 3107, Casilla 19001, Vitacura, Santiago, Chile 9.Department of Astronomy, Yonsei University, 50 Yonsei-ro, Seodaemun-gu, Seoul 03722, Republic of Korea 10.School of Astronomy and Space Science, Nanjing University, Nanjing 210093, People’s Republic of China |
| 推荐引用方式 GB/T 7714 | Tan,Qing-Hua,Gao,Yu,Zhang,Zhi-Yu,et al. The MALATANG Survey: The LGAS–LIR Correlation on Sub-kiloparsec Scale in Six Nearby Star-forming Galaxies as Traced by HCN J?=?4?→?3 and HCO+ J?=?4?→?3[J]. The Astrophysical Journal,2018,860(2). |
| APA | Tan,Qing-Hua.,Gao,Yu.,Zhang,Zhi-Yu.,Greve,Thomas R..,Jiang,Xue-Jian.,...&Zhu,Ming.(2018).The MALATANG Survey: The LGAS–LIR Correlation on Sub-kiloparsec Scale in Six Nearby Star-forming Galaxies as Traced by HCN J?=?4?→?3 and HCO+ J?=?4?→?3.The Astrophysical Journal,860(2). |
| MLA | Tan,Qing-Hua,et al."The MALATANG Survey: The LGAS–LIR Correlation on Sub-kiloparsec Scale in Six Nearby Star-forming Galaxies as Traced by HCN J?=?4?→?3 and HCO+ J?=?4?→?3".The Astrophysical Journal 860.2(2018). |
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