The KMOS^3D Survey: data release and final survey paper

Abstract

We present the completed KMOS${}^{3D}$ survey $-$ an integral field spectroscopic survey of 739, $\log (M_{\star }/M_{\odot })>9$, galaxies at $0.6<z<2.7$ using the K-band Multi Object Spectrograph (KMOS) at the Very Large Telescope (VLT). KMOS${}^{3D}$ provides a population-wide census of kinematics, star formation, outflows, and nebular gas conditions both on and off the star-forming galaxy main sequence through the spatially resolved and integrated properties of H$\alpha$, [N II], and [S II] emission lines. We detect H$\alpha$ emission for 91% of galaxies on the main sequence of star-formation and 79% overall. The depth of the survey has allowed us to detect galaxies with star-formation rates below 1 M${}_{\odot }$/ yr${}^{-1}$, as well as to resolve 81% of detected galaxies with $\ge 3$ resolution elements along the kinematic major axis. The detection fraction of H$\alpha$ is a strong function of both color and offset from the main sequence, with the detected and non-detected samples exhibiting different SED shapes. Comparison of H$\alpha$ and UV+IR star formation rates (SFRs) reveal that dust attenuation corrections may be underestimated by 0.5 dex at the highest masses ($\log (M_{\star }/M_{\odot })>10.5$). We confirm our first year results of a high rotation dominated fraction (monotonic velocity gradient and $v_{\mathrm{rot}}$/${\sigma }_0>\sqrt{3.36}$) of 77% for the full KMOS${}^{3D}$ H$\alpha$sample. The rotation-dominated fraction is a function of both stellar mass and redshift with the strongest evolution measured over the redshift range of the survey for galaxies with $\log (M_{\star }/M_{\odot })<10.5$. With this paper we include a final data release of all 739 observed objects.

26 pages, 18 figures, 8 tables; re-submitted after minor revisions to ApJ; associated data release at: http://www.mpe.mpg.de/ir/KMOS3D

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• CLEAR: Survey Overview, Data Analysis and Products
• Systematically Asymmetric: A comparison of \hi\ profile asymmetries in real and simulated galaxies
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