%0 Generic %1 wuyts2016evolution %A Wuyts, Eva %A Wisnioski, Emily %A Fossati, Matteo %A Schreiber, Natascha M. Förster %A Genzel, Reinhard %A Davies, Ric %A Mendel, J. Trevor %A Naab, Thorsten %A Röttgers, Bernhard %A Wilman, David J. %A Wuyts, Stijn %A Bandara, Kaushala %A Beifiori, Alessandra %A Belli, Sirio %A Bender, Ralf %A Brammer, Gabriel B. %A Burkert, Andreas %A Chan, Jeffrey %A Galametz, Audrey %A Kulkarni, Sandesh K. %A Lang, Philipp %A Lutz, Dieter %A Momcheva, Ivelina G. %A Nelson, Erica J. %A Rosario, David %A Saglia, Roberto P. %A Seitz, Stella %A Tacconi, Linda J. %A Tadaki, Ken-ichi %A Übler, Hannah %A van Dokkum, Pieter %D 2016 %K evolution gradient metallicity %T The evolution of metallicity and metallicity gradients from z=2.7-0.6 with KMOS3D %U http://arxiv.org/abs/1603.01139 %X We present measurements of the NII/Ha ratio as a probe of gas-phase oxygen abundance for a sample of 419 star-forming galaxies at z=0.6-2.7 from the KMOS3D near-IR multi-IFU survey. The mass-metallicity relation (MZR) is determined consistently with the same sample selection, metallicity tracer, and methodology over the wide redshift range probed by the survey. We find good agreement with long-slit surveys in the literature, except for the low-mass slope of the relation at z~2.3, where this sample is less biased than previous samples based on optical spectroscopic redshifts. In this regime we measure a steeper slope than some literature results. Excluding the AGN contribution from the MZR reduces sensitivity at the high mass end, but produces otherwise consistent results. There is no significant dependence of the NII/Ha ratio on SFR or environment at fixed redshift and stellar mass. The IFU data allow spatially resolved measurements of NII/Ha, from which we can infer abundance gradients for 180 galaxies, thus tripling the current sample in the literature. The observed gradients are on average flat, with only 15 gradients statistically offset from zero at >3sigma. We have modelled the effect of beam-smearing, assuming a smooth intrinsic radial gradient and known seeing, inclination and effective radius for each galaxy. Our seeing-limited observations can recover up to 70% of the intrinsic gradient for the largest, face-on disks, but only 30% for the smaller, more inclined galaxies. We do not find significant trends between observed or corrected gradients and any stellar population, dynamical or structural galaxy parameters, mostly in agreement with existing studies with much smaller sample sizes. In cosmological simulations, strong feedback is generally required to produce flat gradients at high redshift.

@misc{wuyts2016evolution, abstract = {We present measurements of the [NII]/Ha ratio as a probe of gas-phase oxygen abundance for a sample of 419 star-forming galaxies at z=0.6-2.7 from the KMOS3D near-IR multi-IFU survey. The mass-metallicity relation (MZR) is determined consistently with the same sample selection, metallicity tracer, and methodology over the wide redshift range probed by the survey. We find good agreement with long-slit surveys in the literature, except for the low-mass slope of the relation at z~2.3, where this sample is less biased than previous samples based on optical spectroscopic redshifts. In this regime we measure a steeper slope than some literature results. Excluding the AGN contribution from the MZR reduces sensitivity at the high mass end, but produces otherwise consistent results. There is no significant dependence of the [NII]/Ha ratio on SFR or environment at fixed redshift and stellar mass. The IFU data allow spatially resolved measurements of [NII]/Ha, from which we can infer abundance gradients for 180 galaxies, thus tripling the current sample in the literature. The observed gradients are on average flat, with only 15 gradients statistically offset from zero at >3sigma. We have modelled the effect of beam-smearing, assuming a smooth intrinsic radial gradient and known seeing, inclination and effective radius for each galaxy. Our seeing-limited observations can recover up to 70% of the intrinsic gradient for the largest, face-on disks, but only 30% for the smaller, more inclined galaxies. We do not find significant trends between observed or corrected gradients and any stellar population, dynamical or structural galaxy parameters, mostly in agreement with existing studies with much smaller sample sizes. In cosmological simulations, strong feedback is generally required to produce flat gradients at high redshift.}, added-at = {2016-03-05T17:04:05.000+0100}, author = {Wuyts, Eva and Wisnioski, Emily and Fossati, Matteo and Schreiber, Natascha M. Förster and Genzel, Reinhard and Davies, Ric and Mendel, J. Trevor and Naab, Thorsten and Röttgers, Bernhard and Wilman, David J. and Wuyts, Stijn and Bandara, Kaushala and Beifiori, Alessandra and Belli, Sirio and Bender, Ralf and Brammer, Gabriel B. and Burkert, Andreas and Chan, Jeffrey and Galametz, Audrey and Kulkarni, Sandesh K. and Lang, Philipp and Lutz, Dieter and Momcheva, Ivelina G. and Nelson, Erica J. and Rosario, David and Saglia, Roberto P. and Seitz, Stella and Tacconi, Linda J. and Tadaki, Ken-ichi and Übler, Hannah and van Dokkum, Pieter}, biburl = {https://www.bibsonomy.org/bibtex/2f49957c0b3da5ba1571953b5f014f597/miki}, description = {[1603.01139] The evolution of metallicity and metallicity gradients from z=2.7-0.6 with KMOS3D}, interhash = {098f5c126792ccefe0f74bae38763828}, intrahash = {f49957c0b3da5ba1571953b5f014f597}, keywords = {evolution gradient metallicity}, note = {cite arxiv:1603.01139Comment: submitted to ApJ}, timestamp = {2016-03-05T17:04:05.000+0100}, title = {The evolution of metallicity and metallicity gradients from z=2.7-0.6 with KMOS3D}, url = {http://arxiv.org/abs/1603.01139}, year = 2016 }