Kinematic Lensing with the Roman Space Telescope
  Kinematic lensing (KL) is a new cosmological measurement technique that
combines traditional weak lensing (WL) shape measurements of disc galaxies with
their kinematic information. Using the Tully-Fisher relation KL breaks the
degeneracy between intrinsic and observed ellipticity and significantly reduces
the impact of multiple systematics that are present in traditional WL. We
explore the performance of KL given the instrument capabilities of the
$\textit{Roman Space Telescope}$, assuming overlap of the High Latitude Imaging
Survey (HLIS), the High Latitude Spectroscopy Survey (HLSS) over 2,000 deg$^2$.
Our KL suitable galaxy sample has a number density of
$n_{\mathrm{gal}}=4~\mathrm{arcmin}^{-1}$ with an estimated shape noise level
of $\sigma_{\epsilon}=0.035$. We quantify the cosmological constraining power
on $\Omega_{\mathrm{m}}$-$S_8$, $w_p$-$w_a$ by running simulated likelihood
analyses that account for redshift and shear calibration uncertainties,
intrinsic alignment and baryonic feedback. Compared to a traditional WL survey
we find that KL significantly improves the constraining power on
$\Omega_{\mathrm{m}}$-$S_8$ (FoM$_{\mathrm{KL}}$=1.70FoM$_{\mathrm{WL}}$) and
$w_p$-$w_a$ (FoM$_{\mathrm{KL}}$=3.65FoM$_{\mathrm{WL}}$). We also explore a
"narrow tomography KL survey" using 30 instead of the default 10 tomographic
bins, however we find no meaningful enhancement to the FoM even when assuming a
significant time-dependence in our fiducial dark energy input scenarios.
