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We present the most precise estimate to date of the clustering of quasars onvery small scales, based on a sample of 47 binary quasars with magnitudes of$g<20.85$ and proper transverse separations of $\sim 25\,h^{-1}$\,kpc. Oursample of binary quasars, which is about 6 times larger than any previousspectroscopically confirmed sample on these scales, is targeted using a KernelDensity Estimation technique (KDE) applied to Sloan Digital Sky Survey (SDSS)imaging over most of the SDSS area. Our sample is "complete" in that all of theKDE target pairs with $17.0 \lesssim R \lesssim 36.2\,h^{-1}$\,kpc in our areaof interest have been spectroscopically confirmed from a combination ofprevious surveys and our own long-slit observational campaign. We catalogue 230candidate quasar pairs with angular separations of $<8\arcsec$, from which ourbinary quasars were identified. We determine the projected correlation functionof quasars ($\bar W_{\rm p}$) in four bins of proper transverse scale over therange $17.0 \lesssim R \lesssim 36.2\,h^{-1}$\,kpc. The implied small-scalequasar clustering amplitude from the projected correlation function, integratedacross our entire redshift range, is $A=24.1\pm3.6$ at $\sim 26.6~h^{-1}$\,kpc. Our sample is the first spectroscopically confirmed sample ofquasar pairs that is sufficiently large to study how quasar clustering evolveswith redshift at $\sim 25 ~h^{-1}$ kpc. We find that empirical descriptions ofhow quasar clustering evolves with redshift at $\sim 25 ~h^{-1}$ Mpc alsoadequately describe the evolution of quasar clustering at $\sim 25 ~h^{-1}$kpc.

Clustering on very small scales from a large sample of confirmed quasar pairs: Does quasar clustering track from Mpc to kpc scales?