2013
DOI: 10.1051/0004-6361/201220555
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On the self-regulation of intense star-formation in galaxies atz= 1−3

Abstract: We have analyzed the properties of the Hα and [Nii]λ6583 rest-frame optical emission lines of a sample of 53 intensely star forming galaxies at z = 1.3 to 2.7 observed with SINFONI on the ESO-VLT. Similar to previous authors, we find large velocity dispersions in the lines, σ = few 10−250 km s −1 . Our data agree well with simulations where we applied beam-smearing and assumed a scaling relation of the form: velocity dispersion is proportional to the square root of the star-formation intensity (star-formation … Show more

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Cited by 81 publications
(117 citation statements)
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References 119 publications
(242 reference statements)
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“…The star formation rate per unit area is probably also low in the outer disks (as is observed both in local and distant galaxies, e.g. Kennicutt & Evans 2012;Lehnert et al 2013). Thus both the enrichment and the mixing timescales will be much longer since the star formation occurs at a much lower intensity.…”
Section: Scenario Within the Context Of Distant Galaxiesmentioning
confidence: 95%
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“…The star formation rate per unit area is probably also low in the outer disks (as is observed both in local and distant galaxies, e.g. Kennicutt & Evans 2012;Lehnert et al 2013). Thus both the enrichment and the mixing timescales will be much longer since the star formation occurs at a much lower intensity.…”
Section: Scenario Within the Context Of Distant Galaxiesmentioning
confidence: 95%
“…Such a value for the star formation intensity, which is likely a lower limit, would imply that Milky Way would have a star formation intensity similar to that of nearby starbursts and distant intensely star-forming galaxies at z ∼ 2−3 (e.g. Lehnert & Heckman 1996;Dib et al 2006;Lehnert et al 2009Lehnert et al , 2013 Above these values, there is a sharp increase in the velocity dispersion of the ISM with Σ SFR . We thus suggest that the relations found between stellar vertical velocity (or z max ) and age reflects similar relations in the ISM: stars formed in a thick ISM, whose high dispersions were sustained for several Gyr by intense star formation (but notice not necessarily high star formation rates overall).…”
Section: Inside-out Formation Of the Diskmentioning
confidence: 99%
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“…The effects of feedback from massive stars and active galactic nuclei allow this direct coupling of star formation with the gas supply to be broken (e.g. Peirani et al 2012;Lehnert et al 2013). This decoupling is important as not only do we need the relative growth of galaxies not to track the gas supply too closely, as observed in the evolution of the sSFR, but also because baryonic mass fraction in galaxies is small and does not follow the halo mass function (Baldry et al 2008;Papastergis et al 2012) suggesting that either a fraction of the baryons are not accreted or they are efficiently removed from the galaxy.…”
Section: Introductionmentioning
confidence: 99%