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Thanks to their large angular dimension and brightness, red giants andsupergiants are privileged targets for optical long-baseline interferometers.Sixteen red giants and supergiants have been observed with the VLTI/AMBERfacility over a two-years period, at medium spectral resolution (R=1500) in theK band. The limb-darkened angular diameters are derived from fits of stellaratmospheric models on the visibility and the triple product data. The angulardiameters do not show any significant temporal variation, except for onetarget: TX Psc, which shows a variation of 4% using visibility data. For theeight targets previously measured by Long-Baseline Interferometry (LBI) in thesame spectral range, the difference between our diameters and the literaturevalues is less than 5%, except for TX Psc, which shows a difference of 11%. Forthe 8 other targets, the present angular diameters are the first measured fromLBI. Angular diameters are then used to determine several fundamental stellarparameters, and to locate these targets in the Hertzsprung-Russell Diagram(HRD). Except for the enigmatic Tc-poor low-mass carbon star W Ori, thelocation of Tc-rich stars in the HRD matches remarkably well thethermally-pulsating AGB, as it is predicted by the stellar-evolution models.For pulsating stars with periods available, we compute the pulsation constantand locate the stars along the various sequences in the Period -- Luminositydiagram. We confirm the increase in mass along the pulsation sequences, aspredicted by the theory, except for W Ori which, despite being less massive,appears to have a longer period than T Cet along the first-overtone sequence.

Fundamental parameters of 16 late-type stars derived from their angular diameter measured with VLTI/AMBER