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We use ALMA observations of the host galaxy of the quasar ULAS-J1342+0928 atz=7.54 to study the dust continuum and far infrared lines emitted from itsinterstellar medium. The Rayleigh-Jeans tail of the dust continuum is wellsampled with eight different spectral setups, and from a modified black bodyfit we obtain an emissivity coefficient of beta=1.85+-0.3. Assuming a standarddust temperature of 47 K we derive a dust mass of Mdust=0.35x10^8 Msol and astar formation rate of 150+-30 Msol/yr. We have >4sigma detections of the[CII]_158, [OIII]_88 and [NII]_122 atomic fine structure lines and limits onthe [CI]_369, [OI]_146 and [NII]_205 emission. We also report multiple limitsof CO rotational lines with Jup >= 7, as well as a tentative 3.3sigma detectionof the stack of four CO lines (Jup=11, 10, 8, 7). We find line deficits thatare in agreement with local ultra luminous infrared galaxies. Comparison of the[NII]_122 and [CII]_158 lines indicates that the [CII]_158 emission arisespredominantly from the neutral medium, and we estimate that thephoto-disassociation regions in J1342+0928 have densities <~5x10^4cm^-3. Thedata suggest that ~16% of hydrogen is in ionized form and that the HII regionshave high electron densities of n_e>180 cm^-3. Our observations favor a lowgas-to-dust ratio of <100 and a metallicity of the interstellar mediumcomparable to the Solar value. All the measurements presented here suggest thatthe host galaxy of J1342+0928 is highly enriched in metal and dust, despitebeing observed just 680 Myr after the Big Bang.

An ALMA multi-line survey of the interstellar medium of the redshift 7.5 quasar host galaxy J1342+0928