  We present spectroscopic observations of 26 galaxies of type E and S0, based
on their blue morphologies, located in voids by the study of Grogin & Geller
(1999). Measurements of redshift, velocity dispersion, and four Lick line
indices, Mgb, Fe5270, Fe5335, and Hbeta with their errors are given for all of
these galaxies, along with Hbeta, [OIII], Halpha, and [NII] emission line
strengths for a subset of these objects. These sources are brighter than M star
for low density regions and tend to be bluer than their counterpart early-type
objects in high density regions. Using the models of Thomas et al. (2003) gives
metal abundances and ages with a median alpha enhancement, [alpha/Fe] = +0.13,
and median metals abundance, [Z/H] = +0.22, values comparable to those found
for E and S0 galaxies in clusters, but with a wider spread in [Z/H] towards low
values. If the emission line subsample is interpreted as younger, the
proportion of young objects is higher than for early-types in higher density
regions. There is a significant incidence of sources in the sample with
emission lines in their spectra (46% with Hbeta and [OIII] and 69% with Halpha
or [NII]) as well as shells and rings in their morphologies (19%). The
diagnostic log[NII/Halpha], log[OIII/Hbeta] diagram places 10 of 12 emission
line galaxies in or near the star forming and liner region and two among the
Seyferts. The Halpha fluxes indicate star formation rates of 0.2 to 1.0 Msun
per yr. The percentage of these early-type void galaxies undergoing star
formation appears to be higher compared to their cluster counterparts and the
range of ages wider.
