Deep absorption in SDSS J110511.15+530806.5

We study the origin of the anomalous deep absorption in a spectrum of the SDSS J110511.15+530806.5 distant quasar (z=1.929) obtained by the Sloan Digital Sky Survey in Data Release 7 of the optical catalog. We aim to estimate the velocity of absorbing material, and we show that this material considerably affects our measurements of the black hole (BH) mass in massive quasars with the use of common virial mass estimators. The spectral shape of the quasar was modeled assuming that the accretion disk emission is influenced by a hot corona, warm skin, and absorbing material located close to the nucleus. The whole analysis was undertaken with XSPEC models and tools. The overall spectral shape was represented with the AGNSED model, while the deep absorption is well described by two Gaussians. The observed spectrum and the fitting procedure allowed us to estimate the BH mass in the quasar as $3.52 \pm 0.01 \times 10^9 M_{\odot}$, the nonzero BH spin is $a_* = 0.32 \pm 0.04$, and the accretion rate is $\dot m=0.274 \pm 0.001$. The velocities of the detected absorbers lie in the range of 6330-108135 km/s. When we consider that absorption is caused by the CIV ion, one absorber is folding toward the nucleus with a velocity of 73887 km/s. We derived a BI index of about 20300 km/s and a mass outflow rate up to 38.5 % of the source accretion rate. The high absorption observed in SDSS J110511.15+530806.5 is evidence of fast winds that place the source in the group of objects on the border with UFO (ultra-fast outflows), strong broad absorption line (BAL), and fast failed radiatively accelerated dusty outflow (FRADO). This absorption affects the BH mass measurement by two orders of magnitude as compared to virial mass estimation.Comment: Accepted for publication in Astronomy & Astrophysics (A&A). 10 pages, 7 figure

The disk reverberation mapping of X-ray weak quasars: a case study of SDSS J153913.47+395423.4

The widely adopted ``lamppost'' thermal reprocessing model, in which the variable UV/optical emission is a result of the accretion disk reprocessing of the highly fluctuating X-ray emission, can be tested by measuring inter-band time lags in quasars spanning a range of X-ray power. This work reports the inter-band time lag in an apparently X-ray weak quasar, SDSS J153913.47+395423.4. A significant cross-correlation with a time delay of $\sim 33$ days (observed-frame) is detected in the Zwicky Transient Facility (ZTF) $g$ and $r$ light curves of SDSS J153913.47+395423.4. The observed X-ray power seems to be too weak to account for the observed inter-band cross-correlation with time delay. Hence the X-ray weak quasar SDSS J153913.47+395423.4 is either intrinsically X-ray normal (but observationally X-ray weak), or the X-ray emission is not the only mechanism to drive UV/optical variability. In the former case, the required X-ray power is at least 19 times stronger than observed, which requires either an exceptionally anisotropic corona or Compton-thick obscuration. Alternatively, the Corona-heated Accretion disk Reprocessing (CHAR) or the EUV torus models may account for the observed time lags.Comment: 10 pages, 4 figures, accepted for publication in the Astrophysical Journa

Parametry globalne kwazarów z anomalnym widmem elektromagnetycznym

Uniwersytet w Białymstoku. Wydział Fizyki.Praca dotyczy analizy galaktyk z aktywnymi jądrami (galaktyki aktywne, AGN). Najjaśniejszym typem galatyk aktywnych jest kwazar. W jej centrum znajduje się supermasywna czarna. Jednym z najmniej poznanych podtypów kwazarów są kwazary o słabych liniach emisyjnych (ang. WLQ). Podstawowym celem pracy doktorskiej jest ocena parametrów globalnych, takich jak: masa czarnej dziury, tempo akrecji, spin czarnej dziury oraz inklinacje kwazarów WLQ w oparciu o metodę dopasowania widma ciągłego. Metoda ta, w przeciwieństwie doinnych metod estymacji mas czarnych dziur, nie zależy od obserwowanej szerokości połówkowej mierzonej w połowie maksimum linii emisyjnej. Pomiar tej szerokości może być obciążony ze względu na słabość lub brak linii emisyjnych w tych kwazarach. Korzystając z rozkładu energii spektralnej kwazarów, dopasowałem geometrycznie cienki i optycznie gruby model dysku akrecyjnego opisany równaniami Novikova i Thorne'a. Otrzymałem model kontinuum dysku akrecyjnego dla 10 słabych kwazarów linii emisyjnych. Drugi projekt zawarty w tej pracy doktorskiej, dotyczył opisu nieprawidłowej, głębokiej absorpcji kwazara SDSS J110511.15+530806.5. Sprawdziłem poprawność postawionej tezy, że istnienie gorącej korony oraz ciepłego naskórka wokół dysku akrecyjnego wyjaśniają to zjawisko.The thesis concerns the analysis of the Active Galactic Nuclei. These are galaxies with an active core. The most luminous type of Active Galactic Nuclei is Quasar. It contains the supermassive black hole at the center. One of the least known subtype of Quasars are: Weak emission-Line Quasars. Their recognizable feature are weak emission-lines. The primary goal of PhD thesis is to evaluate the global parameters such as: the black hole mass, the accretion rate, spin of the black hole, and the inclination of weak emission-line quasars based on the continuum fit method. This method apart from the literature black hole masses estimation methods does not depend on the observed Full Width at Half Maximum of emission line, which could be biased due to the weakness or lack of the emission lines in these quasars. Using the Spectral Energy Distribution of quasars, I have fitted the geometrically thin and optically thick accretion disk model described by Novikov & Thorne equations. I have obtained the model of the continuum of the accretion disk for the 10 weak emission-line quasars. The second project concerned the description of abnormal, deep absorption of SDSS J110511.15+530806.5 quasar. I checked the correctness of the thesis posed that corona and warm skin concept above/around an accretion disk explain this phenomenon