  Studying the behavior along the galaxy main sequence is key in furthering our
understanding of the possible connection between AGN activity and star
formation. We select a sample of 1215 AGN from the catalog of SDSS galaxy
properties from the Portsmouth group by detection of the high-ionization [Ne V]
3426 \r{A} emission line. Our sample extends from 10$^{40}$ to 10$^{42.5}$
erg/s in [Ne V] luminosity in a redshift range z = 0.17 to 0.57. We compare the
specific star formation rates (sSFRs, SFR scaled by galaxy mass) obtained from
the corrected [O II] and H{\alpha} luminosities, and the SED-determined values
from Portsmouth. We find that the emission-line-based sSFR values are
unreliable for the [Ne V] sample due to the AGN contribution, and proceed with
the SED sSFRs for our study of the main sequence. We find evidence for a
decrease in sSFR along the main sequence in the [Ne V] sample which is
consistent with results from the hard X-ray BAT AGN sample, which extends to
lower redshifts than our [Ne V] sample. Although we do not find evidence that
the concurrent AGN activity is suppressing star formation, our results are
consistent with a lower gas fraction in the host galaxies of the AGN as
compared to that of the star forming galaxies. If the evacuation of gas, and
therefore suppression of star formation is due to AGN activity, it must have
occurred in a previous epoch.
