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

 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.)

 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 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!

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

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

 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 Relative intensities for 50<n<400 are calculated using approximate formula: ≈1

3000 A

 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!