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VALES - IV. Exploring the transition of star formation efficiencies between normal and starburst galaxies using APEX/SEPIA Band-5 and ALMA at low redshift
Cheng, C.1,2; Ibar, E.1; Hughes, T. M.1,2,3,4; Villanueva, V.1; Leiton, R.1; Orellana, G.1; Munoz Arancibia, A.1; Lu, N.2; Xu, C. K.2; Willmer, C. N. A.5; Huang, J.2; Cao, T.2; Yang, C.6,7,8; Xue, Y. Q.3,4; Torstensson, K.6
2018-03-01
Source PublicationMONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
ISSN0035-8711
Volume475Issue:1Pages:248-256
Corresponding AuthorCheng, C.(chengcheng@bao.ac.cn) ; Ibar, E.(eduardo.ibar@uv.cl) ; Hughes, T. M.(thomas.hughes@uv.cl)
AbstractIn this work, we present new the Swedish-ESO PI receiver for the Atacama Pathfinder Experiment APEX/SEPIA Band-5 observations targeting the CO (J = 2-1) emission line of 24 Herschel-detected galaxies at z = 0.1-0.2. Combining this sample with our recent new Valparafso ALMA Line Emission Survey (VALES), we investigate the star formation efficiencies [SFEs = star formation rate (SFR)/M-H2] of galaxies at low redshift. We find the SFE of our sample bridges the gap between normal star-forming galaxies and Ultra-Luminous Infrared Galaxies (ULIRGs), which are thought to be triggered by different star formation modes. Considering the SFE' as the SFR and the L'(CO) ratio, our data show a continuous and smooth increment as a function of infrared luminosity (or star formation rate) with a scatter about 0.5 dex, instead of a steep jump with a bimodal behaviour. This result is due to the use of a sample with a much larger range of sSFR/sSFR(ms) using LIRGs, with luminosities covering the range between normal and ULIRGs. We conclude that the main parameters controlling the scatter of the SFE in star-forming galaxies are the systematic uncertainty of the alpha(CO) conversion factor, the gas fraction, and physical size.
Keywordgalaxies: ISM galaxies: starburst galaxies: star formation submillimetre: galaxies
DOI10.1093/mnras/stx3183
WOS KeywordCO-H2 CONVERSION FACTOR ; MOLECULAR GAS ; INFRARED GALAXIES ; FORMING GALAXIES ; MODEL ; LINE
Indexed BySCI
Language英语
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS IDWOS:000427144200020
PublisherOXFORD UNIV PRESS
Citation statistics
Cited Times:1[WOS]   [WOS Record]     [Related Records in WOS]
Document Type期刊论文
Identifierhttp://libir.pmo.ac.cn/handle/332002/22461
Collection中国科学院紫金山天文台
Corresponding AuthorCheng, C.; Ibar, E.; Hughes, T. M.
Affiliation1.Univ Valparaiso, Inst Fis & Astron, Avda Gran Bretana 1111, Valparaiso, Chile
2.Chinese Acad Sci, South Amer Ctr Astron, China Chile Joint Ctr Astron, Natl Astron Observ, Beijing 100012, Peoples R China
3.Univ Sci & Technol China, Dept Astron, CAS Key Lab Res Galaxies & Cosmol, Hefei 230026, Anhui, Peoples R China
4.Univ Sci & Technol China, Sch Astron & Space Sci, Hefei 230026, Anhui, Peoples R China
5.Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA
6.European Southern Observ, Alonso Cordova 3107,Casilla 19001, Santiago 19, Chile
7.Chinese Acad Sci, Key Lab Radio Astron, Purple Mt Observ, Nanjing 210008, Jiangsu, Peoples R China
8.Univ Paris Saclay, Univ Paris Sud, CNRS, Inst Astrophys Spatiale, Bat 121, F-91405 Orsay, France
Recommended Citation
GB/T 7714
Cheng, C.,Ibar, E.,Hughes, T. M.,et al. VALES - IV. Exploring the transition of star formation efficiencies between normal and starburst galaxies using APEX/SEPIA Band-5 and ALMA at low redshift[J]. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,2018,475(1):248-256.
APA Cheng, C..,Ibar, E..,Hughes, T. M..,Villanueva, V..,Leiton, R..,...&Torstensson, K..(2018).VALES - IV. Exploring the transition of star formation efficiencies between normal and starburst galaxies using APEX/SEPIA Band-5 and ALMA at low redshift.MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,475(1),248-256.
MLA Cheng, C.,et al."VALES - IV. Exploring the transition of star formation efficiencies between normal and starburst galaxies using APEX/SEPIA Band-5 and ALMA at low redshift".MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 475.1(2018):248-256.
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