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dc.contributor.authorSwinbank, A.M.
dc.contributor.authorSmail, Ian
dc.contributor.authorSobral, D.
dc.contributor.authorTheuns, T.
dc.contributor.authorBest, P.N.
dc.contributor.authorGeach, J. E.
dc.date.accessioned2013-06-17T12:30:43Z
dc.date.available2013-06-17T12:30:43Z
dc.date.issued2012-12-01
dc.identifier.citationSwinbank , A M , Smail , I , Sobral , D , Theuns , T , Best , P N & Geach , J E 2012 , ' The properties of the star-forming interstellar medium at z=0.8-2.2 from HiZELS II : star formation and clump scaling laws in gas-rich, turbulent disks ' , The Astrophysical Journal , vol. 760 , no. 2 , 130 . https://doi.org/10.1088/0004-637X/760/2/130
dc.identifier.issn0004-637X
dc.identifier.otherPURE: 1905653
dc.identifier.otherPURE UUID: f32ac35a-d942-4b86-b939-d27085a2fb88
dc.identifier.otherWOS: 000311217000034
dc.identifier.otherScopus: 84870261822
dc.identifier.urihttp://hdl.handle.net/2299/10783
dc.description.abstractWe present adaptive optics assisted integral field spectroscopy of nine Ha-selected galaxies at z = 0.84-2.23 drawn from the HiZELS narrowband survey. Our observations map the kinematics of these star-forming galaxies on similar to kpc scales. We demonstrate that within the interstellar medium of these galaxies, the velocity dispersion of the star-forming gas (sigma) follows a scaling relation sigma alpha Sigma(1/n)(SFR) constant (where Sigma(SFR) is the star formation surface density and the constant includes the stellar surface density). Assuming the disks are marginally stable (Toomre Q = 1), this follows from the Kennicutt-Schmidt relation (Sigma(SFR) = A Sigma(n)(gas)), and we derive best-fit parameters of n = 1.34 +/- 0.15 and A = 3.4(-1.6)(+2.5) x 10(-4) M-circle dot yr(-1) kpc(-2), consistent with the local relation, and implying cold molecular gas masses of M-gas = 10(9-10) M-circle dot and molecular gas fractions of M-gas/(M-gas + M-star) = 0.3 +/- 0.1, with a range of 10%-75%. We also identify 11 similar to kpc-scale star-forming regions (clumps) within our sample and show that their sizes are comparable to the wavelength of the fastest growing mode. The luminosities and velocity dispersions of these clumps follow the same scaling relations as local H II regions, although their star formation densities are a factor similar to 15 +/- 5 x higher than typically found locally. We discuss how the clump properties are related to the disk, and show that their high masses and luminosities are a consequence of the high disk surface density.en
dc.format.extent10
dc.language.isoeng
dc.relation.ispartofThe Astrophysical Journal
dc.rightsOpen
dc.subjectgalaxies: starburst
dc.subjectSINS SURVEY
dc.subjectINTEGRAL FIELD SPECTROSCOPY
dc.subjectNEARBY GALAXIES
dc.subjectHIGH-REDSHIFT SURVEY
dc.subjectgalaxies: evolution
dc.subjectgalaxies: high-redshift
dc.subjectH-ALPHA EMITTERS
dc.subjectHII-REGIONS
dc.subjectII REGIONS
dc.subjectSIMILAR-TO 2
dc.subjectGIANT MOLECULAR CLOUDS
dc.subjectULTRA DEEP FIELD
dc.titleThe properties of the star-forming interstellar medium at z=0.8-2.2 from HiZELS II : star formation and clump scaling laws in gas-rich, turbulent disksen
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.contributor.institutionScience & Technology Research Institute
dc.contributor.institutionCentre for Astrophysics Research
dc.description.statusPeer reviewed
dc.relation.schoolSchool of Physics, Astronomy and Mathematics
dc.description.versiontypeSubmitted Version
dcterms.dateAccepted2012-12-01
rioxxterms.versionSMUR
rioxxterms.versionofrecordhttps://doi.org/10.1088/0004-637X/760/2/130
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue
herts.rights.accesstypeOpen


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