The JCMT Nearby Galaxies Legacy Survey - VIII. CO data and the LCO(3-2)-LFIR correlation in the SINGS sample

被引：70

作者：

Wilson, C. D. ^{[1
]}

Warren, B. E. ^{[1
,2
]}

Israel, F. P. ^{[3
]}

Serjeant, S. ^{[4
]}

Attewell, D. ^{[1
]}

Bendo, G. J. ^{[5
]}

Butner, H. M. ^{[6
]}

Chanial, P. ^{[7
]}

Clements, D. L. ^{[8
]}

Golding, J. ^{[1
]}

Heesen, V. ^{[9
]}

Irwin, J. ^{[10
]}

Leech, J. ^{[11
]}

Matthews, H. E. ^{[12
]}

Muhle, S. ^{[13
]}

Mortier, A. M. J. ^{[14
]}

Petitpas, G. ^{[15
]}

Sanchez-Gallego, J. R. ^{[16
,17
]}

Sinukoff, E. ^{[1
]}

Shorten, K. ^{[1
]}

Tan, B. K. ^{[11
]}

Tilanus, R. P. J. ^{[18
,19
]}

Usero, A. ^{[20
]}

Vaccari, M. ^{[21
,22
]}

Wiegert, T. ^{[23
]}

Zhu, M. ^{[24
]}

Alexander, D. M. ^{[25
]}

Alexander, P. ^{[26
,27
]}

Azimlu, M. ^{[15
,28
]}

Barmby, P. ^{[28
]}

Brar, R. ^{[10
]}

Bridge, C. ^{[29
]}

Brinks, E. ^{[9
]}

Brooks, S. ^{[1
]}

Coppin, K. ^{[30
]}

Cote, S. ^{[31
]}

Cote, P. ^{[31
]}

Courteau, S. ^{[10
]}

Davies, J. ^{[32
]}

Eales, S. ^{[32
]}

Fich, M. ^{[33
]}

Hudson, M. ^{[33
]}

Hughes, D. H. ^{[34
]}

Ivison, R. J. ^{[35
,36
]}

Knapen, J. H. ^{[16
,17
]}

Page, M. ^{[8
]}

Parkin, T. J. ^{[1
]}

Rigopoulou, D. ^{[11
,37
]}

Rosolowsky, E. ^{[38
]}

Seaquist, E. R. ^{[39
]}

机构：

[1] McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada

[2] Univ Western Australia, Int Ctr Radio Astron Res, Crawley, WA 6009, Australia

[3] Leiden Univ, Sterrewacht Leiden, NL-2300 RA Leiden, Netherlands

[4] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England

[5] Univ Manchester, UK ALMA Reg Ctr Node, Jodrell Bank Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England

[6] James Madison Univ, Dept Phys & Astron, Harrisonburg, VA 22807 USA

[7] Univ Paris Diderot, Lab AIM Paris Saclay, CEA DSM Irfu, CNRS,CE Saclay, F-91191 Gif Sur Yvette, France

[8] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England

[9] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England

[10] Queens Univ, Dept Phys Engn Phys & Astron, Kingston, ON K7L 3N6, Canada

[11] Univ Oxford, Oxford OX1 3RH, England

[12] Natl Res Council Canada, Herzberg Inst Astrophys, DRAO, Penticton, BC V2A 69J, Canada

[13] Joint Inst VLBI Europe, NL-7990 AA Dwingeloo, Netherlands

[14] Univ Edinburgh, Scottish Univ Phys Alliance, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland

[15] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA

[16] Inst Astrofis Canarias, E-38205 Tenerife, Spain

[17] Univ La Laguna, Dept Astrofis, E-38200 San Cristobal la Laguna, Tenerife, Spain

[18] Joint Astron Ctr, Hilo, HI 96720 USA

[19] Netherlands Org Sci Res, NL-2509 AC The Hague, Netherlands

[20] Observ Madrid, OAN, E-28014 Madrid, Spain

[21] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy

[22] Univ Western Cape, Dept Phys, Astrophys Grp, ZA-7535 Bellville, Cape Town, South Africa

[23] Univ Manitoba, Dept Phys & Astron, Winnipeg, MB R3T 2N2, Canada

[24] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China

[25] Univ Durham, Dept Phys, Durham DH1 3LE, England

[26] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England

[27] Kavli Inst Cosmol Cambridge, Cambridge CB3 0HA, England

[28] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada

[29] CALTECH, Pasadena, CA 91125 USA

[30] McGill Univ, Dept Phys, Montreal, PQ H2A 2T8, Canada

[31] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada

[32] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales

[33] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada

[34] INAOE, Puebla 72000, Mexico

[35] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland

[36] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland

[37] Rutherford Appleton Lab, RALSpace, Didcot OX11 0NL, Oxon, England

[38] Univ British Columbia, Kelowna, BC V1V 1V7, Canada

[39] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada

[40] Royal Mil Coll Canada, Dept Phys, Kingston, ON K7K 7B4, Canada

[41] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England

[42] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands

[43] Joint ALMA Off, Santiago, Chile

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2012年 / 424卷 / 04期

基金：

加拿大自然科学与工程研究理事会; 英国科学技术设施理事会; 美国国家航空航天局;

关键词：

stars: formation; ISM: molecules; galaxies: ISM; galaxies: kinematics and dynamics; galaxies: spiral; LOW-METALLICITY ENVIRONMENTS; SPECTRAL ENERGY-DISTRIBUTION; CO-TO-H-2 CONVERSION FACTOR; LUMINOUS INFRARED GALAXIES; TELESCOPE KEY PROJECT; STAR-FORMATION RATE; WARM MOLECULAR GAS; VIRGO CLUSTER; INTERSTELLAR-MEDIUM; RADIAL-DISTRIBUTION;

D O I：

10.1111/j.1365-2966.2012.21453.x

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The James Clerk Maxwell Telescope Nearby Galaxies Legacy Survey (NGLS) comprises an H?i-selected sample of 155 galaxies spanning all morphological types with distances less than 25?Mpc. We describe the scientific goals of the survey, the sample selection and the observing strategy. We also present an atlas and analysis of the CO J=3 - 2 maps for the 47 galaxies in the NGLS which are also part of the Spitzer Infrared Nearby Galaxies Survey. We find a wide range of molecular gas mass fractions in the galaxies in this sample and explore the correlation of the far-infrared luminosity, which traces star formation, with the CO luminosity, which traces the molecular gas mass. By comparing the NGLS data with merging galaxies at low and high redshift, which have also been observed in the CO J=3 - 2 line, we show that the correlation of far-infrared and CO luminosity shows a significant trend with luminosity. This trend is consistent with a molecular gas depletion time which is more than an order of magnitude faster in the merger galaxies than in nearby normal galaxies. We also find a strong correlation of the LFIR/LCO(3-2) ratio with the atomic-to-molecular gas mass ratio. This correlation suggests that some of the far-infrared emission originates from dust associated with atomic gas and that its contribution is particularly important in galaxies where most of the gas is in the atomic phase.

引用

页码：3050 / 3080

页数：31

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