  We determine the physical parameters of the outer atmosphere of a sample of
eight evolved stars, including the red supergiant {\alpha} Scorpii, the red
giant branch stars {\alpha} Bootis and {\gamma} Crucis, the K giant {\lambda}
Velorum, the normal M giants BK Virginis and SW Virginis, and the Mira star W
Hydrae (in two different luminosity phases) by spatially resolving the stars in
the individual carbon monoxide (CO) first overtone lines. We used the
Astronomical Multi-BEam combineR (AMBER) instrument at the Very Large Telescope
Interferometer (VLTI), in high-resolution mode (${\lambda}/{\Delta}{\lambda}
{\approx} 12000$) between 2.28 and 2.31 ${\mu}m$ in the K band.The maximal
angular resolution is 10 mas, obtained using a triplet telescope configuration,
with baselines from 7 to 48 m. By using a numerical model of a molecular
atmosphere in a spherical shells (MOLsphere), called PAMPERO (an acronym for
the "Physical Approach of Molecular Photospheric Ejection at
high-angular-Resolution for evOlved stars"), we add multiple extended CO layers
above the photospheric MARCS model at an adequate spatial resolution. We use
the differential visibilities and the spectrum to estimate the size ($R$) of
the CO MOLsphere, its column density (${N_{CO}}$) and temperature (${T_{mol}}$)
distributions along the stellar radius. The combining of the ${\chi^2}$
minimization and a fine grid approach for uncertainty analysis leads to
reasonable ${N_{CO}}$ and ${T_{mol}}$ distributions along the stellar radius of
the MOLsphere.
