## 3. Principal component analysisPCA is a mathematical tool, which can reduce a multi-dimensional data set into a small number of linearly independent variables. A general description of the PCA method can be found in Kendall & Stuart (1976) or Jolliffe (1986). The special case of PCA applied to AGN spectra is described by Mittaz et al. (1990) or by Francis et al. (1992) for object-to-object variations. ## 3.1. Description of the methodThe analysis we applied to the spectra of each object was done as
follows. We constructed a matrix
containing the fluxes of the The aim of the PCA is to form a new base , in
which only a few number of the The matrix , which is the expression of
in the new base , contains
the fluxes of the In our analysis, we concentrate on only two components: the
principal component and the rest component, which is constructed by
subtracting the principal from the total component and is therefore
the sum of the minor components. In Fig. 1, we
show the decomposition into these two components of (a) the mean and
(b) the variance spectrum taken around the C IV
1549 line of NGC 3783. The lightcurve of the
total component is obtained by a vectorial addition of the lightcurves
in the
## 3.2. Properties of the componentsThe power of the PCA lies in the diagonalization of the covariance matrix of . A diagonal covariance matrix ensures that all structures constituting a single PCA component vary simultaneously, while the different components have variations that are completely uncorrelated at zero lag. We applied the PCA on the widest possible spectral range to include a significant fraction of the continuum in the analysis. This ensures that the principal component reflects the main continuum variations, since the continuum is known to vary with larger amplitudes than the emission-lines. Fig. 1b illustrates that in NGC 3783 nearly all continuum variations are described by the principal component alone. Under this assumption, we can physically interpret the line profiles in the two components. The line profile in the principal component shows which line-part varies simultaneously with the continuum, whereas the line profile in the rest component shows line-parts that do not vary in tune with the continuum. To test this interpretation and to further investigate the relationship between the continuum and our two components, we applied the PCA method to only the well sampled observations of the 1989 monitoring campaign on NGC 5548 (Clavel et al. 1991). In Fig. 2a, we compare the principal and the rest component lightcurves with the original continuum lightcurve at 1350 Å from Clavel et al. (1991) in units of .
We analysed the correlation of the two components with the UV continuum using the interpolated cross-correlation function (ICCF) of Gaskell & Sparke (1986) as described by White & Peterson (1994). The results show that the principal component variations are indeed strongly correlated with those of the continuum flux at zero lag, while the rest component variations are completely uncorrelated at zero lag with those of the continuum. However, the cross-correlation between the rest component and the UV continuum suggests that the variable line-parts in the rest component follow the continuum with a delay of the order of 25 days. This lag is twice as large as the lag between the continuum and the integrated Ly and C IV lines (8-16 days) (Clavel et al. 1991), which means that the PCA divides the line into two parts: a line-part that responds to the continuum with a very small delay (≲ 5 days) and a line-part that responds with a much longer delay ( 25 days). The C IV line profile of these two parts is shown in Fig. 2c. The full width at half maximum (FWHM) of the line-part in the rest component is much narrower (1 850 ) than in the principal component (7 300 ). However, the full width at 1/4 maximum of the line-part in the rest component (6 650 ) shows that high velocities are also present. This analysis suggests that the line-part in the principal component is emitted in the inner broad-line region (BLR), since it responds with large amplitudes and nearly zero lag to the continuum, whereas the line-part in the rest component is both constituted of a less varying contribution from outer parts of the BLR that respond with a greater delay to the continuum and of a non-varying contribution from the narrow-line region (NLR). The lag of 25 days found for the rest component in NGC 5548 is comparable to the lag of the C III ] 1909 line (26-32 days) (Clavel et al. 1991) and to the Balmer-line lags ( 20 days for H ) (e.g. Peterson et al. 1991). It is therefore possible that the C IV line-part in the rest component is emitted at about the same distance from the ionizing continuum than the C III ] or the H line. In other objects, the temporal sampling of the observations does not allow us to determine a clear lag between the two components and the continuum. However, this will be possible with the other monitoring campaign data, that will soon be available in the IUEFA. © European Southern Observatory (ESO) 1998 Online publication: December 16, 1997 |