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Asteroid systems such as binaries and pairs are indicative of physicalproperties and dynamical histories of the Small Solar System Bodies. Althoughnumerous observational and theoretical studies have been carried out, theformation mechanism of asteroid pairs is still unclear, especially fornear-Earth asteroid (NEA) pairs. We conducted a series of optical photometricand polarimetric observations of a small NEA 2010 XC$_{15}$ in 2022 December toinvestigate its surface properties. The rotation period of 2010 XC$_{15}$ ispossibly a few to several dozen hours and color indices of 2010 XC$_{15}$ arederived as $g-r=0.435\pm0.008$, $r-i=0.158\pm0.017$, and $r-z=0.186\pm0.009$ inthe Pan-STARRS system. The linear polarization degrees of 2010 XC$_{15}$ are afew percent at the phase angle range of 58$^{\circ}$ to 114$^{\circ}$. We foundthat 2010 XC$_{15}$ is a rare E-type NEA on the basis of its photometric andpolarimetric properties. Taking the similarity of not only physical propertiesbut also dynamical integrals and the rarity of E-type NEAs into account, wesuppose that 2010 XC$_{15}$ and 1998 WT$_{24}$ are of common origin (i.e.,asteroid pair). These two NEAs are the sixth NEA pair and first E-type NEA pairever confirmed, possibly formed by rotational fission. We conjecture that theparent body of 2010 XC$_{15}$ and 1998 WT$_{24}$ was transported from themain-belt through the $\nu_6$ resonance or Hungaria region.

Photometry and Polarimetry of 2010 XC$_{15}$: Observational Confirmation of E-type Near-Earth Asteroid Pair