DECARLI, ROBERTOROBERTODECARLIWalter, FabianFabianWalterVenemans, Bram P.Bram P.VenemansBañados, EduardoEduardoBañadosBertoldi, FrankFrankBertoldiCarilli, ChrisChrisCarilliFan, XiaohuiXiaohuiFanFarina, Emanuele PaoloEmanuele PaoloFarinaMazzucchelli, ChiaraChiaraMazzucchelliRiechers, DominikDominikRiechersRix, Hans-WalterHans-WalterRixStrauss, Michael A.Michael A.StraussWang, RanRanWangYang, YujinYujinYang2020-10-072020-10-0720180004-637Xhttp://hdl.handle.net/20.500.12386/27675We present a survey of the [C II] 158 μm line and underlying far-infrared (FIR) dust continuum emission in a sample of 27 z≳ 6 quasars using the Atacama Large Millimeter Array (ALMA) at ∼ 1<SUP>\prime\prime</SUP> resolution. The [C II] line was significantly detected (at > 5-σ) in 23 sources (85%). We find typical line luminosities of {L}<SUB>[{{C</SUB>}{{II}}]}={10}<SUP>9-10</SUP> {L}<SUB>☉ </SUB>, and an average line width of ∼385 {km} {{{s}}}<SUP>-1</SUP>. The [C II]-to-far-infrared luminosity ratios ([C II]/FIR) in our sources span one order of magnitude, highlighting a variety of conditions in the star-forming medium. Four quasar host galaxies are clearly resolved in their [C II] emission on a few kpc scales. Basic estimates of the dynamical masses of the host galaxies give masses between 2 × 10<SUP>10</SUP> and 2 × 10<SUP>11</SUP> {M}<SUB>☉ </SUB>, i.e., more than an order of magnitude below what is expected from local scaling relations, given the available limits on the masses of the central black holes (> 3× {10}<SUP>8</SUP> {M}<SUB>☉ </SUB>, assuming Eddington-limited accretion). In stacked ALMA [C II] spectra of individual sources in our sample, we find no evidence of a deviation from a single Gaussian profile. The quasar luminosity does not strongly correlate with either the [C II] luminosity or equivalent width. This survey (with typical on-source integration times of 8 minutes) showcases the unparalleled sensitivity of ALMA at millimeter wavelengths, and offers a unique reference sample for the study of the first massive galaxies in the universe.STAMPAenArticle10.3847/1538-4357/aaa5aa2-s2.0-85042693377000425306100020https://iopscience.iop.org/article/10.3847/1538-4357/aaa5aa2018ApJ...854...97DFIS/05 - ASTRONOMIA E ASTROFISICA