Overview of the LSST-PL collaboration status.
Microlensing is the only tool to discover and study a population of hidden dark compact objects, including neutron stars, black holes and even the primordial black holes which could form part of the dark matter. We will show how LSST will contribute to this topic, with long-term whole sky observations and depth. We will discuss the lessons learned from Gaia and OGLE surveys which can be...
I shall describe some promising features of our Local Universe that can help reveal some feature of a particle DM candidate. Simulations of galaxy and DM structure formation of warm, cold and self-interacting DM candidates indicate that features of the Galactic and M31 halo like: tidal streams gaps, satellite galaxies orbit parameter distribution and their internal properties can differ...
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
source...
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...
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...
Cataloging the Solar System is one of the main science themes that drive the LSST project. LSST is expected to discover ten times more objects from every minor body population than currently known, and provide hundreds of flux and color data for individual bodies. This will be a total game changer. On the one hand, transformative research will be done by the LSST community, but on the other...
Galaxies form from primordial density perturbations that stop expanding and pass through a turnaround epoch, at which curvature is strongly positive: about five times as strong as density, when both are expressed as domain-averaged $\Omega$s. Moreover, a tight relation is expected between curvature and the domain-averaged expansion rate prior to turnaround. The high number density of LSST...
I envisage to use LSST data for general large-scale structure studies, in particular within the LSST Dark Energy Science Collaboration (DESC). Particular applications may include: photometric redshift derivation, application of resulting catalogs for such studies as tomographic angular clustering, galaxy-galaxy lensing, cross-correlations with CMB lensing etc. Other possible topics of interest...
I would like to use the SED technique for selection of galaxies which do not follow the energy balance like super dusty galaxies or possible lensing objects.
I am planning to apply different machine learning methods to broad range of tasks, such as object classification based on both flux measurements and raw images, novelty detection and correction of the distorted images.
Broad spectroscopic lines, large redshift range and variety of properties make quasar detection in photometric surveys a particularly difficult task, and estimation of their photometric redshifts is even more challenging. I will present a quasar detection method based on photometric ugri data in Kilo-Degree Survey (KIDS) - an imaging deep and wide field survey covering 447 sq. deg. on the sky...
In a talk I would like to present methods developed or currently under development for TOROS project that have potential to be useful for LSST. Most important methods developed be me for TOROS is background rejection using Convolutional Neural Networks (with 99.5 % accuracy). The other methods currently under development involves galaxy subtraction using GANs, scheduling using reinforcement...
