  In this paper, we study the slowly rotating neutron stars in $f(R, T)$
gravity based on Hartle-Thorne formalism. We first consider the simplest
matter-geometry coupled modified gravity, namely $f(R, T)=R+2\chi T$. We
compute the mass, radius, moment of inertia, change in radius, and binding
energy due to rotation, eccentricity, quadrupole moment, and the tidal love
number. The quantities, which are of the second order in angular velocity, like
change in radius and binding energy due to rotation, eccentricity, and
quadrupole moment, deviate more from their corresponding general relativistic
counterparts in lighter neutron stars than heavier ones. Whereas the moment of
inertia, which is of the first order in angular velocity, in $f(R, T)=R+2\chi
T$ modified gravity, barely diverges from the general relativistic one. The
Equation of state-independent I-Love-Q relation retains in this $f(R, T) $
modified gravity, and it coincides with the general relativistic ones within
less than one percent even for the maximum allowed coupling parameters. We also
study the slowly rotating neutron star in $f(R, T)=R+\alpha R^{2}+2\chi T$ up
to first order their angular velocity. We calculate the mass, radius, and
moment of inertia of neutron stars in this modified gravity. The results show
that the impact of the matter-geometric coupling parameter is greater on
lighter neutron stars in both of these modified gravity models.
