SATELLITE EMISSION FEATURES IN 2 SEYFERT-GALAXIES - NEW EVIDENCE THAT RADIO-QUIET AGN POSSESS SUBRELATIVISTIC WINDS

HST/FOS spectra are presented for three bright Seyfert galaxies including one (PG 1351+64) which possesses blue-displaced absorption features in C IV, Si IV, N V, and Ly alpha (but not in Mg II) similar to those seen at high redshift in the broad-absorption-line (BAL) QSOs. Several features of the absorptions in PG 1351+64, including variability seen in archival IUE data, confirm their similarity to the BAL clouds rather than to the ''associated absorber'' phenomenon which they superficially resemble. In PG 1351+64 ''satellite'' emission lines (called herein E1 and E2) have been detected nearly symmetrically placed at +/-4000 km s(-1) around the Mg II emission line; this velocity is just larger than the most blue-displaced of the BALs, suggesting that these two phenomena are related. The satellite line luminosity, L(E1)approximate to(3x10(41) erg s(-1)) h(75)(-2), requires a cloud emission measure n(e)(2) V-c approximate to(1X10(64) cm(-3)) h(75)(-2) at T approximate to 30 000 K. We believe the Mg II lines are produced by 50-90 km s(-1) shocks driven into dense (similar to 10(6) cm(-3), pre-shock) clouds by the ram pressure of a 0.1. M(circle dot) yr(-1) wind leaving the nucleus at velocity 4000 km s(-1). The detection of satellite lines in Mg II, the detection of the blue-shifted cloud in H alpha and H beta and the nondetection of this cloud in C IV restricts the cloud shocks to velocities upsilon(c) less than or equal to 90 km s(-1) and requires a cloud/wind density contrast greater than or equal to 10(3). In this model, the emitting clouds are located at distances of R(eff)approximate to 10(18-19) cm from the nucleus and are entrained and shock-accelerated to similar to 4000 km s(-1). The possible detection of similar ''satellite'' emission features in the non-BAL Seyfert, Ton 951, suggests that the subrelativistic wind that accelerates BAL clouds is a physical feature of many radio-quiet AGN.