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Weak gravitational lensing induces flux dependent fluctuations in theobserved galaxy number density distribution. This cosmic magnification(magnification bias) effect in principle enables lensing reconstructionalternative to cosmic shear and CMB lensing. However, the intrinsic galaxyclustering, which otherwise overwhelms the signal, has hindered itsapplication. Through a scaling relation found by principal component analysisof the galaxy clustering in multi-band photometry space, we design a minimumvariance linear estimator to suppress the intrinsic galaxy clustering and toreconstruct the lensing convergence map. In combination of the CosmoDC2 galaxymock and the CosmicGrowth simulation, we test this proposal for a LSST-likegalaxy survey with $ugrizY$ photometry bands. The scaling relation holdsexcellently at multipole $\ell<10^3$, and remains reasonably well to $\ell\sim3000$. The linear estimator efficiently suppresses the galaxy intrinsicclustering, by a factor of $\sim 10^2$. For galaxies in the photo-z range$0.8<z_\kappa<1.2$, the reconstructed convergence map is cosmic variancelimited per $\ell$ mode at $\ell<10^2$, and shot noise limited at $\ell>= 200$.Its cross-correlation with cosmic shear of galaxies can achieve $S/N >= 200$.When the source redshift of cosmic shear galaxies $z_\gamma<z_\kappa$, thesystematic error is negligible at all investigated scales ($\ell<3000$). When$z_\gamma\geq z_\kappa$, the systematic error caused by the residual intrinsicgalaxy clustering becomes non-negligible. We discuss possible mitigation of theresidual intrinsic galaxy clustering required for accurate measurement at$\ell>10^3$. This work further demonstrates the potential of lensingmeasurement through cosmic magnification to enhance the weak lensing cosmology.

A method of weak lensing reconstruction through cosmic magnification with multi-band photometry information