We have discovered both intermediate-order gravity mode and low-order pressure mode pulsation in the same star , HD 209295 .
It is therefore both a \gamma Doradus and a \delta Scuti star , which makes it the first pulsating star to be a member of two classes .

The analysis of our 128 h of multi-site spectroscopic observations carried out over two seasons reveals that the star is a single-lined spectroscopic binary with an orbital period of 3.10575 \pm 0.00010 d and an eccentricity of 0.352 \pm 0.011 .
Only weak pulsational signals are found in both the radial velocity and line-profile variations , but we have succeeded in showing that the two highest-amplitude \gamma Doradus pulsation modes are consistent with \ell = 1 and |m| = 1 .

These two modes dominated our 280 h of BVI _ { c } multi-site photometry , also obtained over two seasons .
We detected altogether ten frequencies in the light variations , one in the \delta Scuti regime and nine in the \gamma Doradus domain .
Five of the \gamma Doradus frequencies are exact integer multiples of the orbital frequency .
This observation leads us to suspect they are tidally excited .
Attempts to identify modes from the multicolour photometry failed .

We performed model calculations and a stability analysis of the pulsations .
The frequency range in which \delta Scuti modes are excited agree well with observations .
However , our models do not show excitation of \gamma Doradus pulsations , although the damping is smaller in the observed range .
We also investigated tidal excitation of \gamma Doradus modes .
Some of the observed harmonics of the orbital period were found to be unstable .
The observed orbital harmonics which are stable in the models can be understood as linear combinations of the unstable modes .

We could not detect the secondary component of the system in infrared photometry , suggesting that it may not be a main-sequence star .
Archival data of this star shows that it has a strong ultraviolet excess , the origin of which is not known .
The orbit of the primary is consistent with a secondary mass of M > 1.04 M _ { \sun } , which is indicative of a neutron star , although a white dwarf companion is not ruled out .