1. Kovačević, J., Popovic, L. Č., Kollatschny, W., Saikia, P.

2.  In order to understand physical and kinematical properties of AGN emission regions we investigate the correlations between different spectral properties.  In previuos work we found: - kinematical linkage between optical Fe II lines and Intermediate Line Region (ILR), which indicates the ILR origin of optical Fe II. - different correlations between EWs of lines (and line components) vs. L cont. - different correlations between spectral properties in “pure AGN” sample, and composit objects (AGN + starburst) sample, which indicates different physical processes in emission regions. - etc... (Kovačević et al. 2010, Popović et al. 2011)  Present work: extension of research to UV part of spectra!  GOAL: to compare UV and optical spectral properties (specially UV Fe II lines with optical Fe II, in order to find location of their emission region, etc.)

3.  1 step: determination of the UV pseudocontinuum in the sample!  Not easy because: 1. complex shape of UV pseudocontinuum: Power low + Balmer conti nuum (Grandi 1982) Tsuzuki et al. 2006 2. Our sample contains spectra within spectral range: 2900 A – 5500 A (SDSS) (only two continuum windows : ~4200 A and ~5100A! Complex shape of UV pseudocontinuum cannot be fitted well!

4. Sameshima et al. 2010 Tsuzuki et al. 2006, Sameshima et al. 2010

5. Convolving Balmer continuum equation with Gaussian (FWHM Gaussian = FWHM broad Hβ) Jin et al. 2012

6.  We try to make model which: - we could use for fitting spectra within 2900 A – 5500 A range (with two continuum windows). It could be done by reducing number of free parameters: calculating the intensity of Balmer continuum! - we try to make good fit near Balmer edge (3646 A)! Our model consists of: Power law + Balmer continuum (λ<3646A) + high order Balmer lines (n=3-400), (λ>3646A) They are fitted by one Gaussian with the same width and shift as Hγ. The relative intensites for Balmer lines with n<50 are taken from the paper: Storey and Hummer 1995. Relative intensities for 50<n<400 are calculated using approximate formula: ≈1

8. 3000 A

9.  The intensity of Balmer continuum near Balmer edge (~3646A) may be well estimated using fitting result for intensity of prominant Balmer lines (for example Hγ).  Model with high order Balmer lines n=3-400, for λ>3646A, improve the fit near Balmer edge.  Majority of analysed spectra have pseudocontinuum window at ~3000 A.  Calculated intensity of Balmer continuum, as well as one more continuum window (~3000A) should enable determination of UV pseudocontinuum in 2900 A – 5500 A range.  Future work: construction UV Fe II template, analysis of relationships between UV/optical spectral parameters... Thank you for your attention!