Context : Investigating the evolution of protoplanetary disks is crucial for our understanding of star and planet formation .
Several theoretical and observational studies have been performed in the last decades to advance this knowledge .
The launch of satellites operating at infrared wavelengths , such as the Spitzer Space Telescope and the Herschel Space Observatory , has provided important tools for the investigation of the properties of circumstellar disks .

Aims : FT Tauri is a young star in the Taurus star forming region that was included in a number of spectroscopic and photometric surveys .
We investigate the properties of the star , the circumstellar disk , and the accretion/ejection processes and propose a consistent gas and dust model also as a reference for future observational studies .

Methods : We performed a multi-wavelength data analysis to derive the basic stellar and disk properties , as well as mass accretion/outflow rate from TNG/DOLoRes , WHT/LIRIS , NOT/NOTCam , Keck/NIRSpec , and Herschel /PACS spectra .
From the literature , we compiled a complete Spectral Energy Distribution .
We then performed detailed disk modeling using the MCFOST and ProDiMo codes .
Multi-wavelength spectroscopic and photometric measurements were compared with the reddened predictions of the codes in order to constrain the disk properties .

Results : We determine the stellar mass ( \sim 0.3 M _ { \odot } ) , luminosity ( \sim 0.35 L _ { \odot } ) and age ( \sim 1.6 Myr ) , as well as the visual extinction of the system ( 1.8 mag ) .
We estimate the mass accretion rate ( \sim 3 \cdot 10 ^ { -8 } M _ { \odot } / yr ) to be within the range of accreting objects in Taurus .
The evolutionary state and the geometric properties of the disk are also constrained .
The radial extent ( 0.05 to 200 AU ) , flaring angle ( power-law with exponent = 1.15 ) , and mass ( 0.02 { M _ { \odot } } ) of the circumstellar disk are typical of a young primordial disk .
This object can serve as a benchmark for primordial disks with significant mass accretion rate , high gas content and typical size .

Conclusions :