The intrinsic Baldwin effect in broad Balmer lines of six long-term monitored AGNs

We investigate the intrinsic Baldwin effect (Beff) of the broad H$\alpha$ and H$\beta$ emission lines for six Type 1 active galactic nuclei (AGNs) with different broad line characteristics: two Seyfert 1 (NGC 4151 and NGC 5548), two AGNs with double-peaked broad line profiles (3C 390.3 and Arp 102B), one narrow line Seyfert 1 (Ark 564), and one high-luminosity quasar with highly red asymmetric broad line profiles (E1821+643). We found that a significant intrinsic Beff was present in all Type 1 AGNs in our sample. Moreover, we do not see strong difference in intrinsic Beff slopes in different types of AGNs which probably have different physical properties, such as inclination, broad line region geometry, or accretion rate. Additionally, we found that the intrinsic Beff was not connected with the global one, which, instead, could not be detected in the broad H$\alpha$ or H$\beta$ emission lines. In the case of NGC 4151, the detected variation of the Beff slope could be due to the change in the site of line formation in the BLR. Finally, the intrinsic Beff might be caused by the additional optical continuum component that is not part of the ionization continuum.Comment: 12 pages, 8 figures, Accepted for publication in A&

Broad emission lines variability: a window into the heart of AGN

The broad emission lines of active galactic nuclei (AGN) are known to vary both in flux and shape, and are often showing very complex line profiles. They can give us invaluable information about the kinematics and geometry of the broad line region (BLR) where these lines are originating from. The BLR is close to the supermassive black hole in AGN and may hold basic information about the formation and fueling of AGN. Here we summarize the results of the line and continuum variability of a sample of broad line AGN, obtained with the long-term optical monitoring campaign performed with telescopes of SAO (Russia), OAGH and OAN-SPM (Mexico), and Calar Alto (Spain). We monitored different type of broad line AGN (double-peaked, radio loud and radio quiet, NLSy1 and a supermassive binary black hole candidate) which show different variability characteristics that can be explained by different physical properties in BLR

Long-term monitoring of the broad-line region properties in a selected sample of AGN

We present the results of the long-term optical monitoring campaign of active galactic nuclei (AGN) coordinated by the Special Astrophysical Observatory of the Russian Academy of Science. This campaign has produced a remarkable set of optical spectra, since we have monitored for several decades different types of broad-line (type 1) AGN, from a Seyfert 1, double-peaked line, radio loud and radio quiet AGN, to a supermassive binary black hole candidate. Our analysis of the properties of the broad line region (BLR) of these objects is based on the variability of the broad emission lines. We hereby give a comparative review of the variability properties of the broad emission lines and the BLR of seven different type 1 AGNs, emphasizing some important results, such as the variability rate, the BLR geometry, and the presence of the intrinsic Baldwin effect. We are discussing the difference and similarity in the continuum and emission line variability, focusing on what is the impact of our results to the supermassive black hole mass determination from the BLR properties.Comment: Published in Frontiers in Astronomy and Space Scienc

Polarization in the broad lines of NLSy 1 galaxies

<p>One of the characteristics of NLSy1 optical spectra is the narrower broad lines (FWHM~2000 km/s) and presence of strong Fe II lines around Hbeta. Additionally, very often, Hbeta and Halpha broad lines show Lorentzian like profile, that can indicate some specific kinematics of the broad line region (BLR). Polarization in broad lines can indicate the BLR kinematics (see e.g. Smith et al. 2005, MNRAS, 359, 846; Afanasiev et al. 2014, MNRAS, 440, 519; Afanasiev & Popovic 2015, ApJ, 800L, 35). Here we explore a group of NLSy1 galaxies (Mkn 335, Mkn 1501, Mkn 10,NGC 4051, Akn 564, Zw1, and PG0844+349), in order to constrain a dominant kinematics in the BLR. We found that in all observed NLSy1 the Kepelrian motion in the BLR is dominant. Using the method given in Afanasiev & Popovic 2015, we measure the masses of the central black hole in this sample of NLSy1 galaxies.</p