  Large-scale structure (LSS) surveys will increasingly provide stringent
constraints on our cosmological models. Recently, the density-marked
correlation function (MCF) has been introduced, offering an easily computable
density-correlation statistic. Simulations have demonstrated that MCFs offer
additional, independent constraints on cosmological models beyond the standard
two-point correlation (2PCF). In this study, we apply MCFs for the first time
to SDSS CMASS data, aiming to investigate the statistical information regarding
clustering and anisotropy properties in the Universe and assess the performance
of various weighting schemes in MCFs. Upon analyzing the CMASS data, we observe
that, by combining different weights ($\alpha = [-0.2, 0, 0.2, 0.6]$), the MCFs
provide a tight and independent constraint on the cosmological parameter
$\Omega_m$, yielding $\Omega_m = 0.293 \pm0.006$ at the $1\sigma$ level, which
represents a significant reduction in the statistical error by a factor of 3.4
compared to that from 2PCF. Our constraint is consistent with recent findings
from the small-scale clustering of BOSS galaxies \cite{arXiv:2203.08999v2}
within the 1$\sigma$ level. However, we also find that our estimate is lower
than the Planck measurements by about 2.6$\sigma$, indicating the potential
presence of new physics beyond the standard cosmological model if all the
systematics are fully corrected. The method outlined in this study can be
extended to other surveys and datasets, allowing for the constraint of other
cosmological parameters. Additionally, it serves as a valuable tool for
forthcoming emulator analysis on the Chinese Space Station Telescope (CSST).
