  Infrared spectroscopy between 0.8 and 2.5 microns has been obtained for both
components of three unbound asteroid pairs, using the NASA-IRTF with the SpeX
instrument. Pair primary (2110) Moore-Sitterly is classified as an S-type
following the Bus-DeMeo taxonomy; the classification for secondary (44612) 1999
RP27 is ambiguous: S/Sq/Q/K/L-type. Primary (10484) Hecht and secondary (44645)
1999 RC118 are classified as V-types. IR spectra for Moore-Sitterly and Hecht
are each linked with available visual photometry. The classifications for
primary (88604) 2001 QH293 and (60546) 2000 EE85 are ambiguous:
S/Sq/Q/K/L-type. Subtle spectral differences between them suggest the primary
may have more weathered material on its surface. Dynamical integrations have
constrained the ages of formation: 2110-44612 > 782 kyr; 10484-44645 = 348
(+823,-225) kyr; 88604-60546 = 925 (+842,-754) kyr. The spectral similarity of
seven complete pairs is ranked in comparison with nearby background asteroids.
Two pairs, 17198-229056 and 19289-278067, have significantly different spectra
between the components, compared to the similarity of spectra in the background
population. The other pairs are closer than typical, supporting an
interpretation of each pair's formation from a common parent body.
