  Mass loss plays a crucial role in the lives of massive stars, especially as
the star leaves the main sequence and evolves to the red supergiant (RSG)
phase. However, the physical processes that trigger mass-loss events in RSGs
are not well understood. Recently, we showed that adding a static wind to a
MARCS atmospheric model can accurately reproduce observed extensions in the
atmospheres of RSGs. In this work, we compute synthetic observables that match
new interferometric data of the RSGs AH Sco, KW Sgr, V602 Car, CK Car, and V460
Car obtained with VLTI/MATISSE and GRAVITY. We computed model spectra and
visibilities and found the best-fit model, mass-loss rate, and best-fit angular
Rosseland diameter for the observations. We matched our model to the data,
covering a wavelength range of $1.8-5.0\,\mu$m, which corresponds to the $K$,
$L,$ and $M$ bands. Our models reproduce the spectro-interferometric data over
this wide wavelength range, including extended atmospheric layers of CO,
H$_2$O, and SiO. We obtain Rosseland angular diameters between
$3.0<\theta_{\mathrm{Ross}}<5.5$ mas and mass-loss rates of $-6.5<\log
\dot{M}/M_{\odot}\mathrm{yr}^{-1}<-4$. The partial pressure of SiO relative to
the gas pressure and the SiO 4.0$\,\mu$m line intensity increase between 2 and
3 stellar radii. The relative intensity depends on the luminosity used for our
models, since the more luminous models have a higher mass-loss rate. This work
further demonstrates that our MARCS+wind model can reproduce the observed
physical extension of RSG atmospheres for several spectral diagnostics spanning
a broad wavelength range. We reproduce both spectra and visibilities of newly
obtained data as well as provide temperature and density stratifications that
are consistent with the observations. With the MATISSE data, we newly include
the extension of SiO layers as a precursor of silicate dust.
