  The spatial distribution of the tropospheric methane on Titan was measured
using near-infrared spectroscopy. Ground-based observations at 1.5$\mu{\rm m}$
(H-band) were performed during the same night using instruments with adaptive
optics at both the W. M. Keck Observatory and at the Paranal Observatory on 17
July 2014 UT. The integral field observations with SINFONI on the VLT covered
the entire H-band at moderate resolving power,
$R=\lambda/\Delta\lambda\approx1,500$, while the Keck observations were
performed with NIRSPAO near 1.55254$\mu{\rm m}$ at higher resolution,
$R\approx25,000$. The moderate resolution observations are used for flux
calibration and for the determination of model parameters that can be
degenerate in the interpretation of high resolution spectra. Line-by-line
calculations of CH$_4$ and CH$_3$D correlated $k$ distributions from the HITRAN
2012 database were used, which incorporate revised line assignments near
1.5$\mu{\rm m}$. We fit the surface albedo and aerosol distributions in the VLT
SINFONI observations that cover the entire H-band window and used these
quantities to constrain the models of the high-resolution Keck NIRSPAO spectra
when retrieving the methane abundances. Cassini VIMS images of the polar
regions, acquired on 20 July 2014 UT, are used to validate the assumption that
the opacity of tropospheric aerosol is relatively uniform below 10 km. We
retrieved methane abundances at latitudes between 42$^{\circ}$ S and
80$^{\circ}$ N. The tropospheric methane in the Southern mid-latitudes was
enhanced by a factor of $\sim$10--40% over the nominal profile that was
measured using the GCMS on Huygens. The Northern hemisphere had $\sim$90% of
the nominal methane abundance up to polar latitudes (80$^{\circ}$N). These
measurements suggest that a source of saturated polar air is equilibrating with
dryer conditions at lower latitudes.
