Figure: a) Spectrum of the off-nuclear, stellar component. The absence of
broad Balmer lines, together with the strong redshifted CaII
doublet feature verifies that the host galaxy has been successfully
isolated from the nuclear flux. b) Pure Seyfert spectrum obtained by
subtracting the stellar spectrum from the total nuclear spectrum until the
CaII feature vanishes. Note that the stellar absorption feature of
Mg B around 5200Å (rest frame) is also successfully removed.
For the blue data we extracted the spectrum of the host galaxy (which appears on the long slit frames as a clearly defined `fuzz' surrounding the bright nuclear emission.) The spectra extracted from the individual long-slit frames were again co-added to form a single spectrum. Figure 2a shows this co-added spectrum. The absence of any broad Balmer lines from this spectrum is verification that we have successfully isolated the stellar component. Note that there is narrow [OII] and [OIII] line emission present in this spectrum. We attribute this to the narrow line region (NLR) possessing significant spatial extent (and therefore contaminating the spectrum of the host galaxy.)
The stellar spectrum reveals several absorption features. The weak
H 
absorption indicates the presence of a young stellar population.
An older stellar population give rise to the Mg B, FeI, G-band and
CaII absorption features.