  The signature of wind patterns caused by the interplay of rotation and energy
redistribution in hot Jupiters is detectable at high spectral resolution, yet
no direct comparison has been attempted between predictions from general
circulation models (GCMs) and observed high-resolution spectra. We present the
first of such comparisons on near-infrared transmission spectra of the hot
Jupiter HD 189733b. Exploring twelve rotation rates and two chemical regimes,
we have created model spectra from 3-D GCMs and cross-correlated them with the
observed spectra. Comparing our models against those of HD 189733b, we obtain
three key results: (1) we confirm CO and H$_2$O in the planet's atmosphere at a
detection significance of 8.2$\sigma$; (2) we recover the signature of
$\sim$km/s day-to-night winds at $\sim$mbar pressures; and (3) we constrain the
rotation period of the planet to between 1.2 and 4.69 days (synchronous
rotation (2.2 days) remains consistent with existing observations). Our results
do not suffer from the shortcomings of 1-D models as cross correlation
templates - mainly that these models tend to over-constrain the slower rotation
rates and show evidence for anomalous blue shifts. Our 3-D models instead match
the observed line-of-sight velocity of this planet by self-consistently
including the effects of high-altitude day-to-night winds. Overall, we find a
high degree of consistency between HD 189733b observations and our GCM-based
spectra, implying that the physics and chemistry are adequately described in
current 3-D forward models for the purpose of interpreting observations at high
spectral resolution.
