Bright [CII] 158$\mu$m emission in a quasar host galaxy at $z=6.54$
  The [CII] 158$\mu$m fine-structure line is known to trace regions of active
star formation and is the main coolant of the cold, neutral atomic medium. In
this \textit{Letter}, we report a strong detection of the [CII] line in the
host galaxy of the brightest quasar known at $z>6.5$, the Pan-STARRS1 selected
quasar PSO J036.5078+03.0498 (hereafter P036+03), using the IRAM NOEMA
millimeter interferometer. Its [CII] and total far-infrared luminosities are
$(5.8 \pm 0.7) \times 10^9 \,L_\odot$ and $(7.6\pm1.5) \times
10^{12}\,L_\odot$, respectively. This results in a $L_{[CII]} /L_{TIR}$ ratio
of $\sim 0.8\times 10^{-3}$, which is at the high end for those found for
active galaxies, though it is lower than the average found in typical main
sequence galaxies at $z\sim 0$. We also report a tentative additional line
which we identify as a blended emission from the $3_{22} - 3_{13}$ and $5_{23}
- 4_{32}$ H$_2$O transitions. If confirmed, this would be the most distant
detection of water emission to date. P036+03 rivals the current prototypical
luminous J1148+5251 quasar at $z=6.42$, in both rest-frame UV and [CII]
luminosities. Given its brightness and because it is visible from both
hemispheres (unlike J1148+5251), P036+03 has the potential of becoming an
important laboratory for the study of star formation and of the interstellar
medium only $\sim 800\,$Myr after the Big Bang.
