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
Tan,Qing-Hua1; Gao,Yu1; Zhang,Zhi-Yu2,3; Greve,Thomas R.4; Jiang,Xue-Jian1; Wilson,Christine D.5; Yang,Chen-Tao1,6,7; Bemis,Ashley5; Chung,Aeree8; Matsushita,Satoki9; Shi,Yong10; Ao,Yi-Ping1,11; Brinks,Elias12; Currie,Malcolm J.13; Davis,Timothy A.14; Grijs,Richard de15,16,17; Ho,Luis C.15; Imanishi,Masatoshi11; Kohno,Kotaro18,19; Lee,Bumhyun8; Parsons,Harriet20; Rawlings,Mark G.20; Rigopoulou,Dimitra21; Rosolowsky,Erik22; Bulger,Joanna23,24; Chen,Hao10; Chapman,Scott C.25; Eden,David26; Gear,Walter K.14; Gu,Qiu-Sheng10; He,Jin-Hua27,28,29; Jiao,Qian1; Liu,Dai-Zhong1,30; Liu,Li-Jie1,21; Li,Xiao-Hu31; Micha?owski,Micha? J.32; Nguyen-Luong,Quang33,34,35; Qiu,Jian-Jie10; Smith,Matthew W. L.14; Violino,Giulio12; Wang,Jian-Fa1; Wang,Jun-Feng36; Wang,Jun-Zhi37; Yeh,Sherry23,38; Zhao,Ying-He39; Zhu,Ming31
Source PublicationThe Astrophysical Journal
AbstractAbstract 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.
Keywordgalaxies: ISM galaxies: star formation infrared: galaxies ISM: molecules radio lines: galaxies
WOS IDIOP:0004-637X-860-2-aac512
PublisherThe American Astronomical Society
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Document Type期刊论文
Affiliation1.Purple Mountain Observatory & Key Laboratory for Radio Astronomy, Chinese Academy of Sciences, 8 Yuanhua Road, Nanjing 210034, People’s Republic of China;,
2.Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ, UK
3.ESO, Karl-Schwarzschild-Str. 2, D-85748 Garching, Germany
4.Department of Physics and Astronomy, University College London, Gower Street, London WC1E6BT, UK
5.Department of Physics and Astronomy, McMaster University, Hamilton, ON L8S 4M1, Canada
6.Institut d’Astrophysique Spatiale, CNRS, Univ. Paris-Sud, Université Paris-Saclay, Bāt. 121, F-91405, Orsay Cedex, France
7.European Southern Observatory, Alonso de Córdova 3107, Casilla 19001, Vitacura, Santiago, Chile
8.Department of Astronomy, Yonsei University, 50 Yonsei-ro, Seodaemun-gu, Seoul 03722, Republic of Korea
9.Academia Sinica Institute of Astronomy and Astrophysics, P.O. Box 23-141, Taipei 10617, Taiwan
10.School of Astronomy and Space Science, Nanjing University, Nanjing 210093, People’s Republic of China
11.National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
12.Centre for Astrophysics Research, University of Hertfordshire, College Lane, Hatfield AL10 9AB, UK
13.RAL Space, Rutherford Appleton Laboratory, Harwell Campus, Didcot, Oxfordshire, OX11 0QX, UK
14.School of Physics and Astronomy, Cardiff University, Queen's Buildings, The Parade, Cardiff CF24 3AA, UK
15.Kavli Institute for Astronomy & Astrophysics and Department of Astronomy, Peking University, Yi He Yuan Lu 5, Hai Dian District, Beijing 100871, People’s Republic of China
16.Department of Physics and Astronomy, Macquarie University, Balaclava Road, North Ryde, NSW 2109, Australia
17.International Space Science Institute–Beijing, 1 Nanertiao, Zhongguancun, Hai Dian District, Beijing 100190, People’s Republic of China
18.Institute of Astronomy, Graduate School of Science, The University of Tokyo, Osawa, Mitaka, Tokyo 181-0015, Japan
19.Research Center for the Early Universe, Graduate School of Science, The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan
20.East Asian Observatory, 660 N. A’ohōkū Place, University Park, Hilo, HI 96720-2700, USA
21.Department of Physics, University of Oxford, Oxford, OX1 3RH, UK
22.University of Alberta, 116 St. and 85 Ave., Edmonton, AB T6G 2R3, Canada
23.Subaru Telescope, NAOJ, 650 N. A’ohōkū Place, Hilo, HI 96720, USA
24.Institute for Astronomy Maui, University of Hawaii, 34 Ohia Ku St., Pukalani, HI, 96768, USA
25.Department of Physics and Atmospheric Science, Dalhousie University, Halifax, NS B3H 4R2, Canada
26.Astrophysics Research Institute, Liverpool John Moores University, IC2, Liverpool Science Park, 146 Brownlow Hill, Liverpool, L3 5RF, UK
27.Key Laboratory for the Structure and Evolution of Celestial Objects, Yunnan Observatories, Chinese Academy of Sciences, 396 Yangfangwang, Guandu District, Kunming, 650216, People’s Republic of China
28.Chinese Academy of Sciences South America Center for Astronomy, China-Chile Joint Center for Astronomy, Camino El Observatorio #1515, Las Condes, Santiago, Chile
29.Departamento de Astronomía, Universidad de Chile, Casilla 36-D, Santiago, Chile
30.Max Planck Institute for Astronomy, K?nigstuhl 17, D-69117 Heidelberg, Germany
31.National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, People’s Republic of China
32.Astronomical Observatory Institute, Faculty of Physics, Adam Mickiewicz University, ul. S?oneczna 36, 60-286 Poznań, Poland
33.NAOJ Chile Observatory, National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
34.Korea Astronomy and Space Science Institute, 776 Daedeok daero, Yuseoung, Daejeon 34055, Republic of Korea
35.CITA, University of Toronto, 60 St. George Street, Toronto, ON M5S 3H8, Canada
36.Department of Astronomy, Xiamen University, 422 Siming South Road, Xiamen 361005, People’s Republic of China
37.Shanghai Astronomical Observatory, Chinese Academy of Sciences, 80 Nandan Road, Shanghai 200030, People’s Republic of China
38.W. M. Keck Observatory, 65-1120 Mamalahoa Hwy., Kamuela, HI 96743, USA
39.Yunnan Observatories, Chinese Academy of Sciences, Kunming 650011, People’s Republic of China
Recommended Citation
GB/T 7714
Tan,Qing-Hua,Gao,Yu,Zhang,Zhi-Yu,等. 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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