  We collected a sample of ten hitherto unidentified SPB stars with the aim of
describing their pulsational properties and identifying pulsational modes.
Photometric time series data from various surveys were collected and analyzed
using diverse frequency search algorithms. We calculated astrophysical
parameters and investigated the location of our sample stars in the \logTeff\
versus \logl\ diagram. Current pulsational models were calculated and used for
the identification of pulsational modes in our sample stars. An extensive grid
of stellar models along with their g-mode eigenfrequencies was calculated and
subsequently cross-matched with the observed pulsational frequencies. The
best-fit models were then used in an attempt to constrain stellar parameters
such as mass, age, metallicity, and convective overshoot. We present detected
frequencies, corresponding g-mode identifications, and the masses and ages of
the stellar models producing the best frequency cross-matches. We partially
succeeded in constraining stellar parameters, in particular concerning mass and
age. Where applicable, rotation periods have been derived from the spacing of
triplet component frequencies. No evolved SPB stars are present in our sample.
We identify two candidate high-metallicity objects (HD\,86424 and HD\,163285),
one young SPB star (HD\,36999), and two candidate young SPB stars (HD\,61712
and HD\,61076). We demonstrate the feasibility of using ground-based
observations to perform basic asteroseismological analyses of SPB stars. Our
results significantly enlarge the sample of known SPB stars with reliable
pulsational mode identifications, which provides important input parameters for
modeling attempts aiming to investigate the internal processes at work in upper
main-sequence stars.
