The KMOS3D Survey: Data Release and Final Survey Paper

The KMOS3D Survey: Data Release and Final Survey PaperWisnioski, E.Förster Schreiber, N. M.Fossati, M.Mendel, J. T.Wilman, D.Genzel, R.Bender, R.Wuyts, S.Davies, R. L.Übler, H.Bandara, K.Beifiori, A.Belli, S.Brammer, G.Chan, J.Davies, R. I.Fabricius, M.Galametz, A.Lang, P.Lutz, D.Nelson, Erica J.Momcheva, I.Price, S.Rosario, D.Saglia, R.Seitz, S.Shimizu, T.Tacconi, L. J.Tadaki, K.van Dokkum, P. G.Wuyts, E.DOI: info:10.3847/1538-4357/ab4db8v. 886124
Wisnioski, E., Förster Schreiber, N. M., Fossati, M., Mendel, J. T., Wilman, D., Genzel, R., Bender, R., Wuyts, S., Davies, R. L., Übler, H., Bandara, K., Beifiori, A., Belli, S., Brammer, G., Chan, J., Davies, R. I., Fabricius, M., Galametz, A., Lang, P., Lutz, D., Nelson, Erica J., Momcheva, I., Price, S., Rosario, D., Saglia, R. et al. 2019. "The KMOS3D Survey: Data Release and Final Survey Paper." The Astrophysical Journal 886:124. https://doi.org/10.3847/1538-4357/ab4db8
ID: 154542
Type: article
Authors: Wisnioski, E.; Förster Schreiber, N. M.; Fossati, M.; Mendel, J. T.; Wilman, D.; Genzel, R.; Bender, R.; Wuyts, S.; Davies, R. L.; Übler, H.; Bandara, K.; Beifiori, A.; Belli, S.; Brammer, G.; Chan, J.; Davies, R. I.; Fabricius, M.; Galametz, A.; Lang, P.; Lutz, D.; Nelson, Erica J.; Momcheva, I.; Price, S.; Rosario, D.; Saglia, R.; Seitz, S.; Shimizu, T.; Tacconi, L. J.; Tadaki, K.; van Dokkum, P. G.; Wuyts, E.
Abstract: We present the completed KMOS3D survey, an integral field spectroscopic survey of 739 {log}({M}\star /{M}ȯ )> 9 galaxies at 0.6 )> 9 galaxies at 0.6 )> 9 galaxies at 0.6 3D survey 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 Hα, [N II], and [S II] emission lines. We detect Hα 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 yr−1, as well as to resolve 81% of detected galaxies with ≥3 resolution elements along the kinematic major axis. The detection fraction of Hα is a strong function of both color and offset from the main sequence, with the detected and nondetected samples exhibiting different spectral energy distribution shapes. Comparison of Hα and UV+IR star formation rates reveal that dust attenuation corrections may be underestimated by 0.5 dex at the highest masses ({log}({M}\star /{M}ȯ )> 10.5). We confirm our first year results of a high rotation-dominated fraction (monotonic velocity gradient and v rot/{σ }0> \sqrt{3.36}) of 77% for the full KMOS3D 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}ȯ ))http://www.mpe.mpg.de/ir/KMOS3D). Based on observations obtained at the Very Large Telescope (VLT) of the European Southern Observatory (ESO), Paranal, Chile (ESO program IDS 092A-0091, 093.A-0079, 093.A-0079, 094.A-0217, 095.A-0047, 096.A-0025, 097.A-0028, 098.A-0045, 099.A-0013, 0100.A-0039, and 0101.A-0022).