Venemans, Bram P.Bram P.VenemansDECARLI, ROBERTOROBERTODECARLIWalter, FabianFabianWalterBañados, EduardoEduardoBañadosBertoldi, FrankFrankBertoldiFan, XiaohuiXiaohuiFanFarina, Emanuele PaoloEmanuele PaoloFarinaMazzucchelli, ChiaraChiaraMazzucchelliRiechers, DominikDominikRiechersRix, Hans-WalterHans-WalterRixWang, RanRanWangYang, YujinYujinYang2020-10-072020-10-0720180004-637Xhttp://hdl.handle.net/20.500.12386/27667We present Atacama Large Millimeter Array 1 mm observations of the rest-frame far-infrared (FIR) dust continuum in 27 quasars at redshifts 6.0 ≲ z < 6.7. We detect FIR emission at ≳3σ in all quasar host galaxies with flux densities at ∼1900 GHz in the rest-frame of 0.12 < S <SUB>rest,1900 GHz</SUB> < 5.9 mJy, with a median (mean) flux density of 0.88 mJy (1.59 mJy). The implied FIR luminosities range from {L}<SUB>FIR</SUB>} = (0.27-13) × 10<SUP>12</SUP> {L}<SUB>☉ </SUB>, with 74% of our quasar hosts having {L}<SUB>FIR</SUB>} > 10<SUP>12</SUP> {L}<SUB>☉ </SUB>. The estimated dust masses are {M}<SUB>dust</SUB>} = 10<SUP>7</SUP>-10<SUP>9</SUP> {M}<SUB>☉ </SUB>. If the dust is heated only by star formation, then the star formation rates in the quasar host galaxies are between 50 and 2700 {M}<SUB>☉ </SUB> {yr}}<SUP>-1</SUP>. In the framework of the host galaxy-black hole coevolution model a correlation between ongoing black hole growth and star formation in the quasar host galaxy would be expected. However, combined with results from the literature to create a luminosity-limited quasar sample, we do not find a strong correlation between quasar UV luminosity (a proxy for ongoing black hole growth) and FIR luminosity (star formation in the host galaxy). The absence of such a correlation in our data does not necessarily rule out the coevolution model, and could be due to a variety of effects (including different timescales for black hole accretion and FIR emission).STAMPAenArticle10.3847/1538-4357/aadf35000448352900009https://iopscience.iop.org/article/10.3847/1538-4357/aadf352018ApJ...866..159VFIS/05 - ASTRONOMIA E ASTROFISICA