  We investigated the stellar mass function and the binary fraction of 114
nearby open clusters (OCs) using the high-precision photometric data from Gaia
Data Release 3 (Gaia DR3). We estimated the mass of member stars by using a
ridge line (RL) that is better in line with the observed color-magnitude
diagram (CMD), thus obtaining more accurate stellar mass and binary mass ratio
($q$) at the low-mass region. By analyzing the present-day mass function (PDMF)
of star clusters, we found that 108 OCs follow a two-stage power-law
distribution, whereas 6 OCs present a single power-law PDMF. Subsequently, we
fitted the high(low)-mass index of PDMF ($dN/dm \propto m^{-\alpha}$), denoted
as $\alpha_{\rm h}$($\alpha_{\rm l}$), and segmentation point $m_{\rm c}$. For
our cluster sample, the median values of $\alpha_{\rm h}$ and $\alpha_{\rm l}$
are 2.65 and 0.95, respectively, which are approximately consistent with the
initial mass function (IMF) results provided by Kroupa (2001). We utilized the
cumulative radial number distribution of stars with different masses to
quantify the degree of mass segregation. We found a significant positive
correlation between the state of dynamical evolution and mass segregation in
OCs. We also estimated the fraction of binary stars with $q \geq 0.5$, ranging
from 6% to 34% with a median of 17%. Finally, we provided a catalog of 114
nearby cluster properties, including the total mass, the binary fraction, the
PDMF, and the dynamical state.
