BEGIN:VCALENDAR VERSION:2.0 PRODID:-//CERN//INDICO//EN BEGIN:VEVENT SUMMARY:Tracking the nature of DM in the Local Universe DTSTART;VALUE=DATE-TIME:20190314T104000Z DTEND;VALUE=DATE-TIME:20190314T110000Z DTSTAMP;VALUE=DATE-TIME:20260516T015822Z UID:indico-contribution-10-326@events.ncbj.gov.pl DESCRIPTION:Speakers: Wojciech Hellwing (CTF PAS)\nI shall describe some p romising features of our Local Universe that can help reveal some feature of a particle DM candidate. Simulations of galaxy and DM structure formati on of warm\, cold and self-interacting DM candidates indicate that feature s of the Galactic and M31 halo like: tidal streams gaps\, satellite galaxi es orbit parameter distribution and their internal properties can differ s ignificantly in different DM candidate scenarios. Observations that the LS ST will foster will allow us to use these features as potential DM tale-te ll.\n\nhttps://events.ncbj.gov.pl/event/10/contributions/326/ LOCATION: URL:https://events.ncbj.gov.pl/event/10/contributions/326/ END:VEVENT BEGIN:VEVENT SUMMARY:Photometric Reverberation Mapping using LSST DTSTART;VALUE=DATE-TIME:20190314T115000Z DTEND;VALUE=DATE-TIME:20190314T120000Z DTSTAMP;VALUE=DATE-TIME:20260516T015822Z UID:indico-contribution-10-319@events.ncbj.gov.pl DESCRIPTION:Speakers: Swayamtrupta Panda (Center for Theoretical Physics - PAS)\nAn overview of our proposed project - Using a set of prepared AGN templates for a range of AGN parameters that are based on SED broadband mo delling\, 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 th en be performed for representative objects using several cadences which ar e now under consideration. This method will improve the current standards of photometric reverberation method – using multi-channel and time-lag estimations from various methods.\n\nhttps://events.ncbj.gov.pl/event/10/c ontributions/319/ LOCATION: URL:https://events.ncbj.gov.pl/event/10/contributions/319/ END:VEVENT BEGIN:VEVENT SUMMARY:machine learning based quasar detection in photometric surveys DTSTART;VALUE=DATE-TIME:20190314T153000Z DTEND;VALUE=DATE-TIME:20190314T154000Z DTSTAMP;VALUE=DATE-TIME:20260516T015822Z UID:indico-contribution-10-325@events.ncbj.gov.pl DESCRIPTION:Speakers: Szymon Nakoneczny (National Centre for Nuclear Resea rch\, Astrophysics Division\, Warsaw\, Poland)\nBroad spectroscopic lines\ , large redshift range and variety of properties make quasar detection in photometric surveys a particularly difficult task\, and estimation of thei r photometric redshifts is even more challenging. I will present a quasar detection method based on photometric ugri data in Kilo-Degree Survey (KID S) - an imaging deep and wide field survey covering 447 sq. deg. on the sk y (Nakoneczny et al. 2019). The KiDS third data release contains 49 millio ns of sources among which\, however\, a vast majority does not have any sp ectroscopically confirmed identification. We successfully trained a Random Forest classifier based on the KIDS data and a set of known quasars ident ified by the SDSS spectroscopic survey. Our final catalog consists of 190\ ,000 quasar candidates and its training purity equals 91%. Additional vali dation of the catalog was made by the means of comparison with GAIA second data release\, other already existing quasar catalogs and WISE photometri c data. Our method can be easily applied to the future LSST data\, and dev eloped further to make use of the LSST time domain data.\n\nhttps://events .ncbj.gov.pl/event/10/contributions/325/ LOCATION: URL:https://events.ncbj.gov.pl/event/10/contributions/325/ END:VEVENT BEGIN:VEVENT SUMMARY:Machine learning application to the LSST data DTSTART;VALUE=DATE-TIME:20190314T152000Z DTEND;VALUE=DATE-TIME:20190314T153000Z DTSTAMP;VALUE=DATE-TIME:20260516T015822Z UID:indico-contribution-10-316@events.ncbj.gov.pl DESCRIPTION:Speakers: Artem Poliszczuk (NCBJ)\nI am planning to apply diff erent machine learning methods to broad range of tasks\, such as object cl assification based on both flux measurements and raw images\, novelty dete ction and correction of the distorted images.\n\nhttps://events.ncbj.gov.p l/event/10/contributions/316/ LOCATION: URL:https://events.ncbj.gov.pl/event/10/contributions/316/ END:VEVENT BEGIN:VEVENT SUMMARY:AI methods developed / under development for TOROS that might be u se for LSST DTSTART;VALUE=DATE-TIME:20190314T154000Z DTEND;VALUE=DATE-TIME:20190314T155500Z DTSTAMP;VALUE=DATE-TIME:20260516T015822Z UID:indico-contribution-10-322@events.ncbj.gov.pl DESCRIPTION:Speakers: Zadrożny Adam (NCBJ)\nIn a talk I would like to pre sent methods developed or currently under development for TOROS project th at have potential to be useful for LSST. Most important methods developed be me for TOROS is background rejection using Convolutional Neural Network s (with 99.5 % accuracy). The other methods currently under development in volves galaxy subtraction using GANs\, scheduling using reinforcement lear ning and image subtraction using neural networks.\n\nhttps://events.ncbj.g ov.pl/event/10/contributions/322/ LOCATION: URL:https://events.ncbj.gov.pl/event/10/contributions/322/ END:VEVENT BEGIN:VEVENT SUMMARY:General LSS studies with LSST DTSTART;VALUE=DATE-TIME:20190314T142000Z DTEND;VALUE=DATE-TIME:20190314T144000Z DTSTAMP;VALUE=DATE-TIME:20260516T015822Z UID:indico-contribution-10-321@events.ncbj.gov.pl DESCRIPTION:Speakers: Maciek Bilicki (CFT PAN & NCBJ)\nI envisage to use L SST 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 c atalogs for such studies as tomographic angular clustering\, galaxy-galaxy lensing\, cross-correlations with CMB lensing etc. Other possible topics of interest are related to peculiar motions (large-scale flows etc.) using appropriate photometry-based techniques (e.g. Nusser et al. 2011) and/or transverse motions.\n\nhttps://events.ncbj.gov.pl/event/10/contributions/3 21/ LOCATION: URL:https://events.ncbj.gov.pl/event/10/contributions/321/ END:VEVENT BEGIN:VEVENT SUMMARY:SED fitting as a tool for searching peculiar galaxies DTSTART;VALUE=DATE-TIME:20190314T144000Z DTEND;VALUE=DATE-TIME:20190314T145000Z DTSTAMP;VALUE=DATE-TIME:20260516T015822Z UID:indico-contribution-10-314@events.ncbj.gov.pl DESCRIPTION:Speakers: Katarzyna Malek (NCBJ)\nI 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.\n\nhttps://events. ncbj.gov.pl/event/10/contributions/314/ LOCATION: URL:https://events.ncbj.gov.pl/event/10/contributions/314/ END:VEVENT BEGIN:VEVENT SUMMARY:LSST supernovae Ia and the turnaround epoch DTSTART;VALUE=DATE-TIME:20190314T140000Z DTEND;VALUE=DATE-TIME:20190314T142000Z DTSTAMP;VALUE=DATE-TIME:20260516T015822Z UID:indico-contribution-10-323@events.ncbj.gov.pl DESCRIPTION:Speakers: Boudewijn Roukema (Toruń Centre for Astronomy\, Nic olaus Copernicus University)\nGalaxies form from primordial density pertur bations that stop expanding and pass through a turnaround epoch\, at which curvature is strongly positive: about five times as strong as density\, w hen both are expressed as domain-averaged $\\Omega$s. Moreover\, a tight r elation is expected between curvature and the domain-averaged expansion ra te prior to turnaround. The high number density of LSST supernovae of type Ia that are followed up by spectroscopic redshifts should offer many oppo rtunities for testing these two predictions of general relativity.\n\nhttp s://events.ncbj.gov.pl/event/10/contributions/323/ LOCATION: URL:https://events.ncbj.gov.pl/event/10/contributions/323/ END:VEVENT BEGIN:VEVENT SUMMARY:Different time-delay measurement methods in reverberating AGN DTSTART;VALUE=DATE-TIME:20190314T131500Z DTEND;VALUE=DATE-TIME:20190314T132500Z DTSTAMP;VALUE=DATE-TIME:20260516T015822Z UID:indico-contribution-10-318@events.ncbj.gov.pl DESCRIPTION:Speakers: Michal Zajacek ()\nWe will provide an overview of di fferent methods how to reliably measure the time delay between the variabl e AGN continuum and the emission-line light curves in the broad line regio n (BLR) of active galactic nuclei. In particular\, we will also discuss me thods how to assess the uncertainties of these methods and how these error s can propagate further to the current models of the BLR.\n\nhttps://event s.ncbj.gov.pl/event/10/contributions/318/ LOCATION: URL:https://events.ncbj.gov.pl/event/10/contributions/318/ END:VEVENT BEGIN:VEVENT SUMMARY:Cosmological Evolution of the Radio-loudness of Quasar Sources DTSTART;VALUE=DATE-TIME:20190314T132500Z DTEND;VALUE=DATE-TIME:20190314T134000Z DTSTAMP;VALUE=DATE-TIME:20260516T015822Z UID:indico-contribution-10-327@events.ncbj.gov.pl DESCRIPTION:Speakers: Lukasz Stawarz (Jagiellonian Univ.\, Krakow)\nI will present our (Singal et al. 2011\, 2013) approach to the cosmological evol ution of the radio-loudness parameter for quasar sources. In particular\, I will show how we determine the radio and optical luminosity evolutions f or a set of >5\,000 quasars combining the SDSS and FORST data\, based on t he method of Efron and Petrosian (1993)\, to access the intrinsic distribu tion of the radio-loudness parameter (defined as the ratio of the radio to optical luminosity)\, taking into account the truncations and correlation s inherent in the data. In this approach\, we found that the intrinsic dis tribution of the radio-loudness is quite different from the observed one\, is smooth with no evidence of a bimodality\, and that the fraction of the radio-loud quasars increases with inscribing redshift (contrary to severa l claims presented in the literature).\n\nhttps://events.ncbj.gov.pl/event /10/contributions/327/ LOCATION: URL:https://events.ncbj.gov.pl/event/10/contributions/327/ END:VEVENT BEGIN:VEVENT SUMMARY:Can reverberation-measured quasars be used for cosmology? DTSTART;VALUE=DATE-TIME:20190314T114000Z DTEND;VALUE=DATE-TIME:20190314T115000Z DTSTAMP;VALUE=DATE-TIME:20260516T015822Z UID:indico-contribution-10-317@events.ncbj.gov.pl DESCRIPTION:Speakers: Mary Loli Martínez-Aldama (CFT)\nQuasars have been proposed as a new class of standard candles such as\nSupernovae\, their la rge redshift range and high luminosities make them\nexcellent candidates. Reverberation mapping (RM) method offers to\nestimate the distance to the source from the time delay measurement of\nthe emission lines with respect to the continuum\, since the time delay\ndepends on the absolute luminosi ty of the source. This radius-luminosity\n(RL) relation showed a low scatt er and was proposed to use for the\ncosmological purposes. However\, in th e recent years the increase of the\nstudied sample\, and in particular the inclusion of highly accreting QSO\nhas increased the dispersion in the RL relation\, with many objects\nshowing time delays shorter than the expect ed. Using Hb RM\nmeasurements for 117 sources with a 0.2\n\nhttps://events .ncbj.gov.pl/event/10/contributions/317/ LOCATION: URL:https://events.ncbj.gov.pl/event/10/contributions/317/ END:VEVENT BEGIN:VEVENT SUMMARY:In search of CL AGN DTSTART;VALUE=DATE-TIME:20190314T113000Z DTEND;VALUE=DATE-TIME:20190314T114000Z DTSTAMP;VALUE=DATE-TIME:20260516T015822Z UID:indico-contribution-10-313@events.ncbj.gov.pl DESCRIPTION:Speakers: Marzena Sniegowska (CAMK PAN\, CFT PAN)\nAs was clai med in literature\, CL AGN do not form the homogeneous sample. They vary w idely in their timescale of phenomena or type of transient (from bright-s tate to dim-state or vice versa). The nature of state changes in CL AGN is still a mystery\, however\, different scenarios to explain these phenomen a are proposed. I will discuss if CL AGN are a unique phenomenon and how w e can identify them in the LSST sample.\n\nhttps://events.ncbj.gov.pl/even t/10/contributions/313/ LOCATION: URL:https://events.ncbj.gov.pl/event/10/contributions/313/ END:VEVENT BEGIN:VEVENT SUMMARY:Wavelength-dependent time delays in AGN accretion discs DTSTART;VALUE=DATE-TIME:20190314T112000Z DTEND;VALUE=DATE-TIME:20190314T113000Z DTSTAMP;VALUE=DATE-TIME:20260516T015822Z UID:indico-contribution-10-315@events.ncbj.gov.pl DESCRIPTION:Speakers: Aleksandra Olejak (CFT PAN)\nThe idea of measuring a nd using wavelength-dependent time delays between\nthe optical continuum a t different EM wavelengths in order to determine AGN\naccretion disk struc ture has been known for many years. For example Sergeev et\nal. (2005) mod elled the lag-luminosity relation with a disc reprocessing model\,\nwhere time delays were caused by different light travel times from the ionizing\ nsource and regions of continuum emission. Collier et al. (1999) gave an i dea how\nAGNs can be used in cosmology as standard candles by measuring th e flux and\nthe time delays between the optical/UV continuum in an accreti on disc. Right\nnow scientists\, for example Cackett et al. 2007 fit the w avelength-dependent\ntime delays of AGNs with a disc reprocessing models\, what allows to measure\nthe distances to the AGNs. However this method ne eds to be improved in order\nto determine more accurate estimation of cosm ological quantities such as the\nHubble constant. After that\, it could be conveniently applied to six-color AGN\nlightcuves from LSST.\n\nhttps://e vents.ncbj.gov.pl/event/10/contributions/315/ LOCATION: URL:https://events.ncbj.gov.pl/event/10/contributions/315/ END:VEVENT BEGIN:VEVENT SUMMARY:AGN variability with LSST DTSTART;VALUE=DATE-TIME:20190314T110000Z DTEND;VALUE=DATE-TIME:20190314T112000Z DTSTAMP;VALUE=DATE-TIME:20260516T015822Z UID:indico-contribution-10-312@events.ncbj.gov.pl DESCRIPTION:Speakers: Bozena Czerny (Center for Theoretical Physics)\nI wi ll discuss what science we can do using the six-color lightcurves from LSS T for active galactic nuclei. This includes the power density spectra\, st ructure functions\, and time delays. In particular\, time delay measuremen ts can be used to do cosmology with quasars.\n\nhttps://events.ncbj.gov.pl /event/10/contributions/312/ LOCATION: URL:https://events.ncbj.gov.pl/event/10/contributions/312/ END:VEVENT BEGIN:VEVENT SUMMARY:Milky Way black hole population from lensing with the LSST DTSTART;VALUE=DATE-TIME:20190314T102000Z DTEND;VALUE=DATE-TIME:20190314T104000Z DTSTAMP;VALUE=DATE-TIME:20260516T015822Z UID:indico-contribution-10-320@events.ncbj.gov.pl DESCRIPTION:Speakers: Lukasz Wyrzykowski (Warsaw University Astronomical O bservatory)\nMicrolensing is the only tool to discover and study a populat ion of hidden dark compact objects\, including neutron stars\, black holes and even the primordial black holes which could form part of the dark mat ter. 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 applied to LSST.\n\nhttps://events.ncb j.gov.pl/event/10/contributions/320/ LOCATION: URL:https://events.ncbj.gov.pl/event/10/contributions/320/ END:VEVENT BEGIN:VEVENT SUMMARY:Minor Body Science in the LSST Era DTSTART;VALUE=DATE-TIME:20190314T134000Z DTEND;VALUE=DATE-TIME:20190314T140000Z DTSTAMP;VALUE=DATE-TIME:20260516T015822Z UID:indico-contribution-10-324@events.ncbj.gov.pl DESCRIPTION:Speakers: Michał Drahus (OA UJ)\nCataloging the Solar System is one of the main science themes that drive the LSST project. LSST is exp ected to discover ten times more objects from every minor body population than currently known\, and provide hundreds of flux and color data for ind ividual bodies. This will be a total game changer. On the one hand\, trans formative research will be done by the LSST community\, but on the other h and\, small body science will quickly fade in the communities having no ac cess to these new discoveries and data. Our team wishes to join the LSST f amily and explore LSST data on every level. We will discuss examples of LS ST-enabled minor body science based on (i) realtime alerts\, (ii) daily or bit releases\, (iii) annual catalog releases\, and (iv) our own\, customiz ed deep stacks.\n\nhttps://events.ncbj.gov.pl/event/10/contributions/324/ LOCATION: URL:https://events.ncbj.gov.pl/event/10/contributions/324/ END:VEVENT BEGIN:VEVENT SUMMARY:Overview DTSTART;VALUE=DATE-TIME:20190314T100000Z DTEND;VALUE=DATE-TIME:20190314T102000Z DTSTAMP;VALUE=DATE-TIME:20260516T015822Z UID:indico-contribution-10-311@events.ncbj.gov.pl DESCRIPTION:Speakers: Agnieszka Pollo (National Centre for Nuclear Researc h AND Jagiellonian University)\nOverview of the LSST-PL collaboration stat us.\n\nhttps://events.ncbj.gov.pl/event/10/contributions/311/ LOCATION: URL:https://events.ncbj.gov.pl/event/10/contributions/311/ END:VEVENT END:VCALENDAR