  We present a tentative constraint on cosmological parameters $\Omega_m$ and
$\sigma_8$ from a joint analysis of galaxy clustering and galaxy-galaxy lensing
from DESI Legacy Imaging Surveys Data Release 9 (DR9), covering approximately
10000 square degrees and spanning the redshift range of 0.1 to 0.9. To study
the dependence of cosmological parameters on lens redshift, we divide lens
galaxies into seven approximately volume-limited samples, each with an equal
width in photometric redshift. To retrieve the intrinsic projected correlation
function $w_{\rm p}(r_{\rm p})$ from the lens samples, we employ a novel method
to account for redshift uncertainties. Additionally, we measured the
galaxy-galaxy lensing signal $\Delta\Sigma(r_{\rm p})$ for each lens sample,
using source galaxies selected from the shear catalog by applying our
\texttt{Fourier\_Quad} pipeline to DR9 images. We model these observables
within the flat $\Lambda$CDM framework, employing the minimal bias model. To
ensure the reliability of the minimal bias model, we apply conservative scale
cuts: $r_{\rm p} > 8$ and $12 ~h^{-1}{\rm Mpc}$, for $w_{\rm p}(r_{\rm p})$ and
$\Delta\Sigma(r_{\rm p})$, respectively. Our findings suggest a mild tendency
that $S_8 \equiv \sigma_8 \sqrt{\Omega_m/0.3} $ increases with lens redshift,
although this trend is only marginally significant. When we combine low
redshift samples, the value of $S_8$ is determined to be $0.84 \pm 0.02$,
consistent with the Planck results but significantly higher than the 3$\times$
2pt analysis by 2-5$\sigma$. Despite the fact that further refinements in
measurements and modeling could improve the accuracy of our results, the
consistency with standard values demonstrates the potential of our method for
more precise and accurate cosmology in the future.
