Publication: KMOS LENsing Survey (KLENS): Morpho-kinematic analysis of star-forming galaxies at z ~ 2
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We present results from the KMOS LENsing Survey (KLENS), which is exploiting gravitational lensing to study the kinematics of 24 star -forming galaxies at 1.4 < z < 3.5 with a median mass of log(M-*/M-circle dot) = 9.6 and a median star formation rate (SFR) of 7.5 M-circle dot yr(-1). We find that 25% of these low mass/low SFR galaxies are rotation -dominated, while the majority of our sample shows no velocity gradient. When combining our data with other surveys, we find that the fraction of rotation -dominated galaxies increases with the stellar mass, and decreases for galaxies with a positive offset from the main sequence (higher specific star formation rate). We also investigate the evolution of the intrinsic velocity dispersion, sigma(0), as a function of the redshift, z, and stellar mass, M-*, assuming galaxies in quasi-equilibrium (Toomre Q parameter equal to 1). From the z -sigma(0) relation, we find that the redshift evolution of the velocity dispersion is mostly expected for massive galaxies (log(M-*/M-circle dot) > 10). We derive a M* - sigma(0) relation, using the Tully Fisher relation, which highlights that a different evolution of the velocity dispersion is expected depending on the stellar mass, with lower velocity dispersions for lower masses, and an increase for higher masses, stronger at higher redshift. The observed velocity dispersions from this work and from comparison samples spanning 0 < z < 3.5 appear to follow this relation, except at higher redshift (z > 2), where we observe higher velocity dispersions for low masses (log(M-*/M-circle dot) similar to 9.6) and lower velocity dispersions for high masses (log(M-*/M-circle dot) similar to 10.9) than expected. This discrepancy could, for instance, suggest that galaxies at high redshift do not satisfy the stability criterion, or that the adopted parametrization of the specific star formation rate and molecular properties fail at high redshift.
© ESO 2018. This work has made use of the Rainbow Cosmological Surveys Database, which is operated by the Universidad Complutense de Madrid (UCM), partnered with the University of California Observatories at Santa Cruz (UCO/Lick, UCSC). We are very grateful to Tucker Jones and Nicha Leethochawalit for sharing their two-dimensional modeling codes. We also want to thank Mark Swinbank for advice on the data reduction and Nicolas Bouche for discussions on GalPaK<SUP>3D</SUP>. This work was supported by the Swiss National Science Foundation. MG is grateful to the Fonds de recherche du Quebec Nature et Technologies (FRQNT) for financial support. PGP-G acknowledges support from Spanish Government MINECO grants AYA2015-63650-P and AYA2015-70815-ERC.