We use cookies to ensure that we give you the best experience on our website. By continuing to browse this repository, you give consent for essential cookies to be used. You can read more about our Privacy and Cookie Policy.

Durham Research Online
You are in:

KROSS : mapping the Hα emission across the star formation sequence at z ≈ 1.

Magdis, G.E. and Bureau, M. and Stott, J.P. and Tiley, A. and Swinbank, A.M. and Bower, R. and Bunker, A.J. and Jarvis, M. and Johnson, H. and Sharples, R. (2016) 'KROSS : mapping the Hα emission across the star formation sequence at z ≈ 1.', Monthly notices of the Royal Astronomical Society., 456 (4). pp. 4533-4541.


We present first results from the KMOS (K-band Multi-Object Spectrograph) Redshift One Spectroscopic Survey, an ongoing large kinematical survey of a thousand, z ∼ 1 star-forming galaxies, with VLT KMOS. Out of the targeted galaxies (∼500 so far), we detect and spatially resolve Hα emission in ∼90 and 77 per cent of the sample, respectively. Based on the integrated Hα flux measurements and the spatially resolved maps, we derive a median star formation rate (SFR) of ∼7.0 M⊙ yr−1 and a median physical size of 〈r′1/2r1/2′〉 = 5.1 kpc. We combine the inferred SFRs and effective radii measurements to derive the star formation surface densities (ΣSFR) and present a ‘resolved’ version of the star formation main sequence (MS) that appears to hold at subgalactic scales, with similar slope and scatter as the one inferred from galaxy-integrated properties. Our data also yield a trend between ΣSFR and Δ(sSFR) (distance from the MS) suggesting that galaxies with higher sSFR are characterized by denser star formation activity. Similarly, we find evidence for an anticorrelation between the gas phase metallicity (Z) and the Δ(sSFR), suggesting a 0.2 dex variation in the metal content of galaxies within the MS and significantly lower metallicities for galaxies above it. The origin of the observed trends between ΣSFR–Δ(sSFR) and Z–Δ(sSFR) could be driven by an interplay between variations of the gas fraction or the star formation efficiency of the galaxies along and off the MS. To address this, follow-up observations of our sample that will allow gas mass estimates are necessary.

Item Type:Article
Keywords:Galaxy: evolution.
Full text:(VoR) Version of Record
Download PDF
Full text:(NA) Not Applicable
Download PDF (arXiv version)
Publisher Web site:
Publisher statement:This article has been accepted for publication in Monthly notices of the Royal Astronomical Society ©: 2016 The Author Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
Date accepted:12 December 2015
Date deposited:09 February 2016
Date of first online publication:22 January 2016
Date first made open access:09 February 2016

Save or Share this output

Look up in GoogleScholar