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(abridged) We present ALMA observations of hydrogen fluoride, HF J=1-0, H20(220-211), and the 1.2 THz rest-frame continuum emission from the z=4.7 systemBR1202-0725. BR1202-0725 is a galaxy group consisting of a QSO, asub-millimeter galaxy (SMG), and two Ly-alpha emitters. We detected HF inemission in the QSO and possibly in absorption in the SMG, while water isdetected in emission in both the QSO and SMG. The QSO is the most luminous HFemitter yet found and has the same ratio of HF emission line to infraredluminosity as a sample of local AGN and the Orion Bar. This consistency coversabout 10 orders-of-magnitude in infrared luminosity, L_IR. Based on theconclusions of a study of HF emission in the Orion Bar and modeling, the HFemission in the QSO is either excited by collisions with electrons and H2 inmolecular plasmas irradiated by the AGN and intense star formation orpredominately by collisions with H2, with a modest contribution from electrons,in a relatively high temperature (~120 K), dense (~10^5 cm^-3) medium. AlthoughHF should be an excellent tracer of molecular outflows, we do not find strongevidence for outflows in HF in either the QSO or the SMG. From a putativeabsorption feature in HF in the SMG, we estimate an upper limit on the outflowrate, dM/dt_outflow <~45 M_sun/yr. The ratio of the outflow rate to the starformation rate is <5% for the SMG. The broadness of the H2O line in the SMG,FWHM~1020 km/s, may suggest that either the gas on large scales (>4 kpc) issignificantly more disturbed and turbulent due either to interactions and massexchange with the other members of the group or to the dissipation of theenergy of the intense star formation or both. The lack of significant molecularoutflows in either source may imply that much of the energy from the intensestar formation and AGN activity in this pair is being dissipated in their ISM.

Etching glass in the early Universe: Luminous HF and water emission in a QSO-SMG pair at z=4.7