http://hdl.handle.net/123456789/11 http://hdl.handle.net/123456789/5766 ANALIZA PROMENLJIVOSTI AKTIVNIH GALAKTIČKIH JEZGARA KOMBINOVANOM PRIMENOM SAMOORGANIZUJUĆIH MAPA I NEURONSKIH PROCESA Čvorović - Hajdinjak, Iva This doctoral dissertation addresses the development and application of advanced methods for analyzing the temporal variability of active galactic nuclei (AGN) through the modeling of their optical light curves. The research integrates unsupervised and generative learning techniques, by combining Self- Organizing Maps (SOM) for data preprocessing and Conditional Neural Processes (CNP) for light curve prediction. For the first time in the study of AGN light curves, clustering via SOM has been implemented for preprocessing, alongside the application of CNP for modeling variability. This innovative approach facilitates a more effective modeling of light curves characterized by uneven sampling and missing observations. The QNPy software package was developed and optimized for large-scale parallel processing of extensive time series data. The proposed methodology was validated using light curves from the All-Sky Automated Survey for SuperNovae (ASAS-SN) and the SWIFT/BAT mission, covering a broad range of time scales and variability. The analysis prove that clustering light curves with SOM enhances the performance of neural process, particularly for objects exhibiting simpler variability patterns. The effects of SOM hyperparameters on clustering and prediction performance were carefully examined. The models were validated using loss function and mean squared error evaluations on real data. The proposed methodology shows strong potential for scalable processing of the large time-series data, anticipated in upcoming projects such as the Vera C. Rubin Observatory’s Legacy Survey of Space and Time, enabling automated classification, anomaly detection, and the extraction of scientifically significant objects from catalogs containing hundreds of millions of sources. http://hdl.handle.net/123456789/5748 VARIATION OF V AND R MAGNITUDES FOR SELECTED QUASARS AND THE LINK BETWEEN THE GAIA CRF AND ICRF SYSTEMS Jovanović, Miljana One of the main objectives of the Gaia mission of the European Space Agency is to construct a celestial reference frame at the wavelengths of the optical domain, Gaia CRF. This frame needs a link to the International Celestial Reference Frame – ICRF which is fixed with respect to distant objects (quasars). The objects serving for the purpose of linking are required to be visible in both domains (optical and radio). A set of 47 such objects has been proposed and included which in the radio domain have no detected extended emission. The mentioned objects are active galactic nuclei (AGN) the brightness of which varies over the whole electromagnetic spectrum. The brightness change may be due to activity in different AGN regions, but also to external factors. Such variations can lead to changes in the photocentre position and, consequently, to changes of the object coordinates. In order to establish which objects are suitable for linking these two frames we have examined the brightness variation in the optical domain. The objects have been observed from 2013 in the V and R bands. We have analysed the brightness, colour (V − R) and optical spectral index (α). It has been established that for the majority of objects the brightness is variable, or possibly variable. Almost 15% of all objects have significant changes in their brightness (more than 1 mag), only ∼10% are stable with minor brightness changes of ∼0.3 mag. The results concerning the change analysis of the colour and α are also presented. Based on these results 17 objects are chosen as suitable for linking ICRF to Gaia CRF. The results of the analysis, as well as the observed values, are essential for the examination of these objects because of their importance in astrometry, also in astrophysics. These data are relevant to a better understanding of formation and evolution of galaxies. http://hdl.handle.net/123456789/5606 HIDRODINAMIČKA I SINHROTRONSKA RADIO-EVOLUCIJA OSTATAKA SUPERNOVIH U NEHOMOGENOJ MEÐUZVEZDANOJ SREDINI Kostić, Petar The models of radio synchrotron emission of supernova remnants (SNRs) imply uniform density ahead of shock wave, so the evolution of luminosity is usu- ally studied in such an environment, most often through the surface-brightness-to- diameter dependence, the Σ–D relation. This field aims to better understand the SNR evolution, the emission models, but also the methods for determining their distance. It is not an easy task because of a very large scatter in the Σ–D Milky Way sample. The dissertation puts a different perspective at the Σ–D relation (usually treated as power-law function), assuming that non-uniform environment around the stars considerably affects its shape and slope, that may vary during the SNR expansion. It makes the ambient density structure an important factor whose impact must be investigated. The numerical code for hydrodynamic (HD) simulations and the emission model were developed. The 3D HD simulations were performed in different non-uniform environments, including low-density bubbles and a variety of clumpy models. Based on the simulation results, a semi-analytical 3D spherically-symmetric model of HD and Σ–D evolution of SNRs in clumpy medium was developed, which is used to generate large Σ–D samples. The results show that after entering the clumpy medium the SNR brightness enhances, but afterward the Σ–D slope steepens, shortening the brightness evolu- tion lifetime. Despite the evident increase in slope in clumpy medium, the Galactic sample average slope flattens at ≈ 13–50 pc. After analyzing the generated SNR samples in clumpy medium it is concluded that the significant flattening and scatter in Galactic sample originates in sporadic emission jumps of individual SNRs in a limited diameter interval. The additional analyses of selection effects are needed to investigate these issues. http://hdl.handle.net/123456789/5583 Numeričke simulacije sudara galaksija i nastanka morfoloških podstruktura Milošević, Stanislav In this dissertation, we presented galaxy mergers and the forming of stellar morphological substructures. We assume a large spiral galaxy and dwarf galaxy which is a satellite of the first one. We used N-body simulations to present different scenarios for the merger of two galaxies, and after that, we analyzed the properties of formed structures. The investigation of the formation of these structures and their properties is important for understanding the dynamics and evolution of galaxies. First, we did simulations where we investigated the influence of the properties of dwarf galaxies on the forming structures. We tested: 1. morphology of the dwarf galaxy where we used two models – dwarf with a disk and spheroidal dwarf galaxy; 2. inclination of the orbit in the case of a very radial merger, because in that case, we have the formation of the stellar shells and streams; 3. direction of rotation of the dwarf in the case of a dwarf with a disk. In each case, after the merger, we have stellar shells and streams formed. Morphology, inclination of the orbit, and direction of rotation have their influence on the properties of formed substructures, and on the timescale of disruption of the remnant of the dwarf. In the case of the merger of Andromeda galaxy (M31) and dwarf galaxy, the satellite of M31, we investigate the properties of the Giant Stellar Stream (GSS), as well as the Northeast shell (NE) and West shell (W). The orientation of the GSS, distances, and velocities of the GSS, NE, and W shells from our simulation are in agreement with the observed one. For the first time, we explained the observed metallicity distribution in these substructures. With a linearly decreasing gradient of the initial metallicity in the dwarf galaxy before the merger, using Monte Carlo (MC) simulations, we successfully explained the observed metallicity distribution in these substructures. These results are a contribution to the investigation of metallicity gradients in dwarf galaxies which is important for galaxy evolution in general.