All Tables

Table 1: Log of observations. Column 1: Julian date-2 400 000, Col. 2: UT date, Col. 3: continuum fluxes at 5100 Å measured by Kollatschny et al. (2001), Col. 4: our measurements of the continuum flux (in unit of 10^-15 erg^-1 s^-1 cm^-2 Å^-1) after removal of the host galaxy contribution.
Table 2: Observed permitted Fe II multiplets in the narrow line system of the spectrum of Mark 110. Column 1: multiplet number, Col. 2: transition, Col. 3: upper level energy, Col. 4: number of observed lines/number of lines in the multiplet in the observed spectral range.
Table 3: Observed and computed line ratios, referred to the flux of the relevant H $\beta$ component ( $20.3\times 10^{-15}$ erg s^-1 cm^-2), of the forbidden lines detected in the NLR of Mrk110. R is the distance of the emitting cloud from the ionizing source in cm, n the density in cm^-3 and $N_{\rm H}$ the column density in cm^-2.
Table 4: Same as Table 3 for the permitted lines.
Table A.1: Lines observed in the stronger narrow line system. Column 1: line identification, Col. 2: rest wavelength, Col. 3: intensity relative to H $\beta$ (H $\beta$ flux = $20.3\times 10^{-15}$ erg s^-1 cm^-2).