The FMOS-COSMOS survey of star-forming galaxies at $z\sim1.6$. V:
  Properties of dark matter halos containing H$\alpha$ emitting galaxies
  We study the properties of dark matter halos that contain star-forming
galaxies at $1.43 \le z \le 1.74$ using the FMOS-COSMOS survey. The sample
consists of 516 objects with a detection of the H$\alpha$ emission line, that
represent the star-forming population at this epoch having a stellar mass range
of $10^{9.57}\le M_\ast/M_\odot \lesssim 10^{11.4}$ and a star formation rate
range of $15\lesssim \mathrm{SFR}/(M_\odot \mathrm{yr^{-1}}) \lesssim 600$. We
measure the projected two-point correlation function while carefully taking
into account observational biases, and find a significant clustering amplitude
at scales of $0.04$-$10~h^{-1}~\mathrm{cMpc}$, with a correlation length $r_0 =
5.21^{+0.70}_{-0.67}~h^{-1}~\mathrm{cMpc}$ and a bias $b=2.59^{+0.41}_{-0.34}$.
We interpret our clustering measurement using a halo occupation distribution
model. The sample galaxies appear to reside in halos with mass $M_\mathrm{h} =
4.6^{+1.1}_{-1.6}\times10^{12}~h^{-1}M_\odot$ on average that will likely
become present-day halos of mass $M_\mathrm{h} (z=0)
\sim2\times10^{13}~h^{-1}M_\odot$, equivalent to the typical halo mass scale of
galaxy groups. We then confirm the decline of the stellar-to-halo mass ratio at
$M_\mathrm{h}<10^{12}~M_\odot$, finding $M_\ast/M_\mathrm{h} \approx
5\times10^{-3}$ at $M_\mathrm{h}=10^{11.86}~M_\odot$, which is lower by a
factor of 2-4 than those measured at higher masses. Finally, we use our results
to illustrate the future capabilities of Subaru's Prime-Focus Spectrograph, a
next-generation instrument that will provide strong constraints on the
galaxy-formation scenario by obtaining precise measurements of galaxy
clustering at $z>1$.
