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Stellar parameter determination is a challenging task when dealing withgalactic giant stars. The combination of different investigation techniques hasproven to be a promising approach. We analyse archive spectra obtained with theShort-Wavelength-Spectrometer (SWS) onboard of ISO, and new interferometricobservations from the Very Large Telescope MID-infrared Interferometricinstrument (VLTI/MIDI) of a very well studied carbon-rich giant: TX Psc. Theaim of this work is to determine stellar parameters using spectroscopy andinterferometry. The observations are used to constrain the model atmosphere,and eventually the stellar evolutionary model in the region where the tracksmap the beginning of the carbon star sequence. Two different approaches areused to determine stellar parameters: (i) the 'classic' interferometricapproach where the effective temperature is fixed by using the angular diameterin the N-band (from interferometry) and the apparent bolometric magnitude; (ii)parameters are obtained by fitting a grid of state-of-the-art hydrostaticmodels to spectroscopic and interferometric observations. We find a goodagreement between the parameters of the two methods. The effective temperatureand luminosity clearly place TX Psc in the carbon-rich AGB star domain in theH-R-diagram. Current evolutionary tracks suggest that TX Psc became a C-starjust recently, which means that the star is still in a 'quiet' phase comparedto the subsequent strong-wind regime. This is in agreement with the C/O ratiobeing only slightly larger than 1.

Catching the fish - Constraining stellar parameters for TX Psc using spectro-interferometric observations