A Halo Occupation Interpretation Of Quasars At $z\sim1.5$ Using Very
  Small Scale Clustering Information
  We combine the most precise small scale ($< 100\, \rm h^{-1}kpc$) quasar
clustering constraintsto date with recent measurements at large scales ($> 1\,
\rm h^{-1}Mpc$) from the extended Baryon Oscillation Spectroscopic Survey
(eBOSS) to better constrain the satellite fraction of quasars at $z\sim 1.5$ in
the halo occupation formalism. We build our Halo Occupation Distribution (HOD)
framework based on commonly used analytic forms for the one and two-halo terms
with two free parameters: the minimum halo mass that hosts a central quasar and
the fraction of satellite quasars that are within one halo. Inspired by recent
studies that propose a steeper density profile for the dark matter haloes that
host quasars, we explore HOD models at kiloparsec scales and best-fit
parameters for models with $10\times$ higher concentration parameter. We find
that an HOD model with a satellite fraction of $f_{\rm sat} =
0.071_{-0.004}^{+0.009}$ and minimum mass of $\rm M_{m} = 2.31_{-0.38}^{+0.41}
\times 10^{12}\, \, \rm h^{-1} M_{\odot}$ for the host dark matter haloes best
describes quasar clustering (on all scales) at $z \sim 1.5$. Our results are
marginally inconsistent with earlier work that studied brighter quasars,
hinting at a luminosity-dependence to the one-halo term.
