I will discuss what science we can do using the six-color lightcurves from LSST for active galactic nuclei. This includes the power density spectra, structure functions, and time delays. In particular, time delay measurements can be used to do cosmology with quasars.
The idea of measuring and using wavelength-dependent time delays between
the optical continuum at different EM wavelengths in order to determine AGN
accretion disk structure has been known for many years. For example Sergeev et
al. (2005) modelled the lag-luminosity relation with a disc reprocessing model,
where time delays were caused by different light travel times from the ionizing
As was claimed in literature, CL AGN do not form the homogeneous sample. They vary widely in their timescale of phenomena or type of transient (from bright-state to dim-state or vice versa). The nature of state changes in CL AGN is still a mystery, however, different scenarios to explain these phenomena are proposed. I will discuss if CL AGN are a unique phenomenon and how we can identify...
Quasars have been proposed as a new class of standard candles such as
Supernovae, their large redshift range and high luminosities make them
excellent candidates. Reverberation mapping (RM) method offers to
estimate the distance to the source from the time delay measurement of
the emission lines with respect to the continuum, since the time delay
depends on the absolute luminosity of the...
An overview of our proposed project - Using a set of prepared AGN templates for a range of AGN parameters that are based on SED broadband modelling, we seek to calculate the contribution of the major lines (Hβ, Mg II, CIV) to the photometric channels, taking into account the Balmer continuum, FeII pseudo-continuum and other lines. The simulations will then be performed for representative...
We will provide an overview of different methods how to reliably measure the time delay between the variable AGN continuum and the emission-line light curves in the broad line region (BLR) of active galactic nuclei. In particular, we will also discuss methods how to assess the uncertainties of these methods and how these errors can propagate further to the current models of the BLR.
I will present our (Singal et al. 2011, 2013) approach to the cosmological evolution of the radio-loudness parameter for quasar sources. In particular, I will show how we determine the radio and optical luminosity evolutions for a set of >5,000 quasars combining the SDSS and FORST data, based on the method of Efron and Petrosian (1993), to access the intrinsic distribution of the...