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The parallax of pulsation, and its implementations such as theBaade-Wesselink method and the infrared surface bright- ness technique, is anelegant method to determine distances of pulsating stars in a quasi-geometricalway. However, these classical implementations in general only use a subset ofthe available observational data. Freedman & Madore (2010) suggested a morephysical approach in the implementation of the parallax of pulsation in orderto treat all available data. We present a global and model-basedparallax-of-pulsation method that enables including any type of observationaldata in a consistent model fit, the SpectroPhoto-Interferometric modeling ofPulsating Stars (SPIPS). We implemented a simple model consisting of apulsating sphere with a varying effective temperature and a combina- tion ofatmospheric model grids to globally fit radial velocities, spectroscopic data,and interferometric angular diameters. We also parametrized (and adjusted) thereddening and the contribution of the circumstellar envelopes in thenear-infrared photometric and interferometric measurements. We show thesuccessful application of the method to two stars: delta Cep and eta Aql. Theagreement of all data fitted by a single model confirms the validity of themethod. Derived parameters are compatible with publish values, but with ahigher level of confidence. The SPIPS algorithm combines all the availableobservables (radial velocimetry, interferometry, and photometry) to estimatethe physical parameters of the star (ratio distance/ p-factor, Teff, presenceof infrared excess, color excess, etc). The statistical precision is improved(compared to other methods) thanks to the large number of data taken intoaccount, the accuracy is improved by using consistent physical modeling and thereliability of the derived parameters is strengthened thanks to the redundancyin the data.

Cepheid distances from the SpectroPhoto-Interferometry of Pulsating Stars (SPIPS) - Application to the prototypes delta Cep and eta Aql