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<ri:Resource created="2021-05-10T13:05:00Z" status="active" updated="2025-05-19T09:50:00Z" version="1.2" xmlns:cs="http://www.ivoa.net/xml/ConeSearch/v1.0" xmlns:ri="http://www.ivoa.net/xml/RegistryInterface/v1.0" xmlns:vr="http://www.ivoa.net/xml/VOResource/v1.0" xmlns:vs="http://www.ivoa.net/xml/VODataService/v1.1" xmlns:xsi="http://www.w3.org/2001/XMLSchema-instance" xsi:schemaLocation="http://www.ivoa.net/xml/ConeSearch/v1.0 http://vo.ari.uni-heidelberg.de/docs/schemata/ConeSearch.xsd http://www.ivoa.net/xml/VOResource/v1.0 http://vo.ari.uni-heidelberg.de/docs/schemata/VOResource.xsd http://www.ivoa.net/xml/VODataService/v1.1 http://vo.ari.uni-heidelberg.de/docs/schemata/VODataService.xsd" xsi:type="vs:CatalogService"><title>Completed KMOS^3D^ survey NIR obs.</title><shortName>J/ApJ/886/124</shortName><identifier>ivo://CDS.VizieR/J/ApJ/886/124</identifier><altIdentifier>doi:10.26093/cds/vizier.18860124</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Wisnioski E.</name></creator><creator><name>Schreiber N.M.F.</name></creator><creator><name>Fossati M.</name></creator><creator><name>Mendel J.T.</name></creator><creator><name>Wilman D.,Genzel R.</name></creator><creator><name>Bender R.</name></creator><creator><name>Wuyts S.</name></creator><creator><name>Davies R.L.</name></creator><creator><name>Ubler H.</name></creator><creator><name>Bandara K.,Beifiori A.</name></creator><creator><name>Belli S.</name></creator><creator><name>Brammer G.</name></creator><creator><name>Chan J.</name></creator><creator><name>Davies R.I.</name></creator><creator><name>Fabricius M.,Galametz A.</name></creator><creator><name>Lang P.</name></creator><creator><name>Lutz D.</name></creator><creator><name>Nelson E.J.</name></creator><creator><name>Momcheva I.</name></creator><creator><name>Price S.,Rosario D.</name></creator><creator><name>Saglia R.</name></creator><creator><name>Seitz S.</name></creator><creator><name>Shimizu T.</name></creator><creator><name>Tacconi L.J.</name></creator><creator><name>Tadaki K.,van Dokkum P.G.</name></creator><creator><name>Wuyts E.</name></creator><date role="Updated">2021-07-05T13:00:25Z</date><date role="Created">2021-05-10T13:05:00Z</date><contact><name>CDS support team</name><address>CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France</address><email>cds-question@unistra.fr</email></contact></curation><content><subject>galaxies</subject><subject>spectroscopy</subject><subject>surveys</subject><subject>redshifted</subject><subject>absolute-magnitude</subject><subject>galaxy-kinematics</subject><subject>infrared-astronomy</subject><subject>visible-astronomy</subject><description>We present the completed KMOS^3D^ survey, an integral field spectroscopic survey of 739 log(M_*_/M_{sun}_)&gt;9 galaxies at 0.6&lt;z&lt;2.7 using the K-band Multi Object Spectrograph (KMOS) at the Very Large Telescope. The KMOS3D 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 H{alpha}, [NII], and [SII] 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 1M_{sun}_/yr, as well as to resolve 81% of detected galaxies with &gt;=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 nondetected samples exhibiting different spectral energy distribution shapes. Comparison of H{alpha} and UV+IR star formation rates reveal that dust attenuation corrections may be underestimated by 0.5dex at the highest masses (log(M_*_/M_{sun}_)&gt;10.5). We confirm our first year results of a high rotation-dominated fraction (monotonic velocity gradient and v_rot_/{sigma}_0_&gt;3.36^0.5^) of 77% for the full KMOS^3D^ 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_*_/M_{sun}_)&lt;10.5.</description><source format="bibcode">2019ApJ...886..124W</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/886/124</referenceURL><type>Catalog</type><contentLevel>Research</contentLevel><relationship><relationshipType>IsServedBy</relationshipType><relatedResource ivo-id="ivo://CDS.VizieR/TAP">TAP VizieR generic service</relatedResource></relationship><relationship><relationshipType>IsServedBy</relationshipType><relatedResource>Conesearch service</relatedResource></relationship><relationship><relationshipType>related-to</relationshipType><relatedResource ivo-id="ivo://CDS.VizieR/II/246">II/246 : 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/437/883">J/A+A/437/883 : K20 survey: spectroscopic catalogue (Mignoli+, 2005)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/455/107">J/A+A/455/107 : 3D spectroscopy with VLT/GIRAFFE (Flores+, 2006)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJS/179/124">J/ApJS/179/124 : Subaru/XMM-Newton deep survey (SXDS) III. 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