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We present results of time-series analysis of the first year of the Fairall 9 intensive disc-reverberation campaign. We used Swift and the Las Cumbres Observatory global telescope network to continuously monitor Fairall 9 from X-rays to near-infrared at a daily to subdaily cadence. The cross-correlation function between bands provides evidence for a lag spectrum consistent with the τ ∝ λ4/3 scaling expected for an optically thick, geometrically thin blackbody accretion disc. Decomposing the flux into constant and variable components, the variable component’s spectral energy distribution is slightly steeper than the standard accretion disc prediction. We find evidence at the Balmer edge in both the lag and flux spectra for an additional bound-free continuum contribution that may arise from reprocessing in the broad-line region. The inferred driving light curve suggests two distinct components, a rapidly variable (100 d) component with an opposite lag to the reverberation signal.

We perform non-hydrodynamical 2.5D simulations to study the dynamics of material above accretion disk based on the disk radiation pressure acting on dust. We assume a super-accreting underlying disk with the accretion rate of 10 times the Eddington rate with central black hole mass ranging from $10^7$ up to $10^9 M_{\odot}$. Such high accretion rates are characteristic for extreme sources. We show that for high accretors radiatively dust-driving mechanism based on FRADO model always leads to a massive outflow from the disk surface, and the failed wind develops only at larger radii. The outflow rate strongly depends on the black hole mass, and in optically-thick energy-driven solution can exceed the accretion rate for masses larger than $10^ 8 M_{\odot}$ but momentum-driven outflow does not exceed the accretion rate even for super-Eddington accretion, therefore not violating the adopted stationarity of the disk. However, even in this case the outflow from the disk implies a strong mechanical feedback., Comment: 13 pages, 3 figures, Accepted for publication in the journal of Dynamics (MDPI)

The extragalactic gamma-ray sky is dominated by blazars, active galactic nuclei (AGN) with a relativistic jet that is closely aligned with the line of sight. Galaxies develop an active nucleus if the central supermassive black hole (BH) accretes large amounts of ambient matter and magnetic flux. The inflowing mass accumulates around the plane perpendicular to the accretion flow's angular momentum. The flow is heated through viscous friction and part of the released energy is radiated as blackbody or non-thermal radiation, with luminosities that can dominate the accumulated stellar luminosity of the host galaxy. A fraction of the accretion flow luminosity is reprocessed in a surrounding field of ionised gas clouds. These clouds, revolving around the central BH, emit Doppler-broadened atomic emission lines. The region where these broad-line-emitting clouds are located is called broad-line region (BLR). About one in ten AGN forms an outflow of radiation and relativistic particles, called a relativistic jet. According to the Blandford-Znajek mechanism, this is facilitated through electromagnetic processes in the magnetosphere of a spinning BH. The latter induces a magnetospheric poloidal current circuit, generating a decelerating torque on the BH and inducing a toroidal magnetic field. Consequently, rotational energy of the BH is converted to Poynting flux streaming away mainly along the rotational axis and starting the jet. One possibility for particle acceleration near the jet base is realised by magnetospheric vacuum gaps, regions temporarily devoid of plasma, such that an intermittent electric field arises parallel to the magnetic field lines, enabling particle acceleration and contributing to the mass loading of the jets. Magnetised structures, containing bunches of relativistic electrons, propagate away from the galactic nucleus along the jets. Assuming that these electrons emit synchrotron radiation and that they inverse-Compton (IC) up-scatter abundant target photons, which can either be the synchrotron photons themselves or photons from external emitters, the emitted spectrum can be theoretically determined. Additionally taking into account that these emission regions move relativistically themselves and that the emission is Doppler-boosted and beamed in forward direction, the typical two-hump spectral energy distribution (SED) of blazars is recovered. There are however findings that challenge this well-established model. Short-time variability, reaching down to minute scales at very high energy gamma rays, is today known to be a widespread phenomenon of blazars, calling for very compact emission regions. In most models of such optically thick emission regions, the gamma-ray flux is usually pair-absorbed exponentially, without considering the cascade evolving from the pair-produced electrons. From the observed flux, it is often concluded that emission emanates from larger distances where the region is optically thin, especially from outside of the BLR. Only in few blazars gamma-ray attenuation associated with pair absorption in the BLR was clearly reported. With the advent of sophisticated high-energy or very high energy gamma-ray detectors, like the Fermi Large Area Telescope or the Major Atmospheric Gamma-ray Imaging Cherenkov telescopes, besides the extraordinarily fast variability spectral features have been found that cannot be explained by conventional models reproducing the two-hump SED. Two such narrow spectral features are discussed in this work. For the nearby blazar Markarian 501, hints to a sharp peak around 3 TeV have been reported from a multi-wavelength campaign carried out in July 2014, while for 3C 279 a spectral dip was found in 2018 data, that can hardly be described with conventional fitting functions. In this work it is examined whether these spectral peculiarities of blazar jet emission can be explained, if the full radiation reprocessing through an IC pair cascade is accounted for. Such a cascade is the multiple concatenation of IC scattering events and pair production events. In the cascades generally considered in this work, relativistic electrons and high-energy photons are injected into a fixed soft target photon field. A mathematical description for linear IC pair cascades with escape terms is delivered on the basis of preliminary works. The steady-state kinetic equations for the electrons and for the photons are determined, whereby it is paid attention to an explicit formulation and to motivating the correct integration borders of all integrals from kinematic constraints. In determining the potentially observable gamma-ray flux, both the attenuated injected flux and the flux evolving as an effect of IC up-scattering, pair absorption and escape are incorporated, giving the emerging spectra very distinct imprints. Much effort is dedicated to the numerical solution of the electrons' kinetic equation via iterative schemes. It is explained why pointwise iteration from higher to lower Lorentz factors is more efficient than iterating the whole set of sampling points. The algorithm is parallelised at two positions. First, several workers can perform pointwise iterations simultaneously. Second, the most demanding integral is cut into a number of part integrals which can be determined by multiple workers. Through these measures, the Python code can be readily applied to simulate steady-state IC pair cascades with escape. In the case of Markarian 501 the developed framework is as follows. The AGN hosts an advection-dominated accretion flow with a normalised accretion rate of several \(10^{-4}\) and an electron temperature near \(10^{10}\) K. On the one hand, the accretion flow illuminates the few ambient gas clouds with approximate radius \(10^{11}\) m, which reprocess a fraction 0.01 of the luminosity into hydrogen and helium emission lines. On the other hand, the gamma rays from the accretion flow create electrons and positrons in a sporadically active vacuum gap in the BH magnetosphere. In the active gap, a power of roughly 0.001 of the Blandford-Znajek power is extracted from the rotating BH through a gap potential drop of several \(10^{18}\) V, generating ultra-relativistic electrons, which subsequently are multiplied by a factor of about \(10^6\) through interaction with the accretion flow photons. This electron beam propagates away from the central engine and encounters the photon field of one passing ionised cloud. The resulting IC pair cascade is simulated and the evolving gamma-ray spectrum is determined. Just above the absorption troughs due to the hydrogen lines, the spectrum exhibits a narrow bump around 3 TeV. When the cascaded emission is added to the emission generated at larger distances, the observed multi-wavelength SED including the sharp peak at 3 TeV is reproduced, underlining that radiation processes beyond conventional models are motivated by distinct spectral features. The dip in the spectrum of 3C 279 is addressed by a similar cascade model. Three types of injection are considered, varying in the ratio of the photon density to the electron density and varying in the spectral shape. The IC pair cascade is assumed to happen either in the dense BLR photon field with a luminosity of several \(10^{37}\) W and a radial size of few \(10^{14}\) m or in the diluted photon field outside of the BLR. The latter scenario is however rejected as the spectral slope around several 100 MeV and the dip at few 10 GeV cannot be reconciled within this model. The radiation cascaded in the BLR can explain the observational data, irrespective of the assumed injected rate. It is therefore concluded that for this period of gamma-ray emission, the radiation production happens at the edge of the BLR of 3C 279. Both investigations show that IC pair cascades can account for fine structure seen in blazar SEDs. It is insufficient to restrict the radiation transport to pure exponential absorption of an injection term. Pair production and IC up-scattering by all generations of photons and electrons in the optically thick regime critically shape the emerging spectra. As the advent of future improved detectors will provide more high-precision spectra, further observations of narrow spectral features can be expected. It seems therefore recommendable to incorporate cascading into conventional radiation production models or to extend the model developed in this work by synchrotron radiation., Beobachtet man das Firmament im Licht der Gammastrahlung, stellen Blasare die Mehrzahl extragalaktischer Objekte dar. Blasare sind aktive Galaxienkerne mit einem relativistischen Jet, der entlang der Sichtlinie ausgerichtet ist. Galaxien haben einen aktiven Kern, wenn das zentrale supermassereiche Schwarze Loch große Mengen an Umgebungsmaterie und magnetischem Fluss akkretiert. Die nach Innen strömende Masse sammelt sich nahe der Ebene an, die senkrecht zum Drehimpuls des Akkretionsflusses steht. Das akkretierte Material wird durch viskose Reibung aufgeheizt und ein Teil der freigesetzten Energie wird als Schwarzkörper- oder nicht-thermische Strahlung abgestrahlt, deren Leuchtkraft die gesamte stellare Leuchtkraft der Wirtsgalaxie übertreffen kann. Ein Teil der Leuchtkraft des Akkretionsflusses wird in einem umgebenden Feld von ionisierten Gaswolken reprozessiert. Diese Wolken, die um das zentrale Schwarze Loch kreisen, emittieren Doppler-verbreiterte Emissionslinien. Den Teil des aktiven Galaxienkerns, in dem sich diese Wolken befinden, bezeichnet man als BLR (englisch: broad-line region). Ihr Abstand zum zentralen Schwarzen Loch beträgt typischerweise etwa 0,1 pc. Etwa einer von zehn aktiven Galaxienkernen bildet einen Ausfluss von Strahlung und relativistischen Teilchen aus, einen sogenannten relativistischen Jet. Dies wird gemäß dem Blandford-Znajek-Mechanismus durch elektromagnetische Prozesse in den Magnetosphären rotierender Schwarzer Löcher bewerkstelligt. Letztere induzieren einen poloidalen magnetosphärischen Stromkreis, der ein abbremsendes Drehmoment auf das Schwarze Loch ausübt und ein toroidales Magnetfeld erzeugt. Folglich wird die Rotationsenergie des Schwarzen Lochs in Poynting-Fluss umgewandelt, der hauptsächlich entlang der Rotationsachse abfließt und den Jet entstehen lässt. Durch Prozesse, die noch nicht eindeutig identifiziert wurden, werden geladene Teilchen in der Nähe der Jetbasis beschleunigt. Eine Möglichkeit dafür ist Teilchenbeschleunigung in magnetosphärischen Vakuum-Lücken. Dies sind Regionen, die vorübergehend nahezu frei von Plasma sind, sodass zeitweise ein elektrisches Feld parallel zu den Magnetfeldlinien entsteht, das die Teilchenbeschleunigung ermöglicht und zur Aufladung der Jets mit massebehafteten Teilchen beiträgt. Magnetisierte Strukturen, die relativistische Elektronen enthalten, bewegen sich entlang der Jets vom Galaxienkern weg. Unter der Annahme, dass diese Elektronen Synchrotronstrahlung aussenden und dass sie vorhandenen weichen Photonen, die entweder die Synchrotronphotonen selbst oder Photonen von externen Emittern sein können, durch inverse Compton-Streuung höhere Energien verleihen, kann das emittierte Spektrum berechnet werden. Berücksichtigt man zusätzlich, dass sich diese Emissionsgebiete selbst relativistisch bewegen und dass die Emission Doppler-verstärkt ist und bevorzugt in Vorwärtsrichtung abgestrahlt wird, erhält man die typische zweihöckrige spektrale Energieverteilung von Blasaren. Es gibt jedoch Erkenntnisse, die dieses bewährte Modell in Frage stellen. Kurzzeit-Variabilität, die bei sehr hochenergetischer Gammastrahlung bis zu Minuten-Skalen hinunterreicht, ist ein weit verbreitetes Phänomen bei Blasaren und setzt sehr kompakte Emissionsregionen voraus. In den meisten Modellen für solche optisch dicken Emissionsregionen wird der Gammastrahlenfluss durch Paarbildung lediglich exponentiell absorbiert, ohne die Kaskade zu berücksichtigen, die sich durch die erzeugten Elektronen entwickelt. Aus den Beobachtungen wird oft gefolgert, dass die Emission aus optisch dünnen Regionen bei größeren Entfernungen stammt, insbesondere von außerhalb der BLR. Nur bei wenigen Blasaren wurde eine Abschwächung der Gammastrahlung durch Absorption in der BLR eindeutig nachgewiesen. Durch moderne Gammastrahlen-Detektoren, wie das Fermi Large Area Telescope oder den Major Atmospheric Gamma-ray Imaging Cherenkov Teleskopen, wurden neben der Kurzzeit-Variabilität auch spektrale Merkmale gefunden, die nicht durch konventionelle Modelle, die die zweihöckrigen spektralen Energieverteilungen wiedergeben können, erklärt werden können. Zwei solcher besonderen spektralen Merkmale werden in dieser Arbeit diskutiert. Für den Blasar Markarian 501 wurden bei einer im Juli 2014 durchgeführten Multiwellenlängenkampagne Hinweise auf einen schmalen Buckel bei 3 TeV gefunden, während für 3C 279 in Daten von 2018 eine Mulde im Spektrum gefunden wurde, die mit oft verwendeten Fit-Funktionen nur schlecht beschrieben werden kann. In dieser Arbeit wird untersucht, ob diese spektralen Besonderheiten der Blasar-Jet-Emission erklärt werden können, wenn die vollständige Reprozessierung der Strahlung durch eine inverse Compton-Paar-Kaskade berücksichtigt wird. Eine solche Kaskade ist die mehrfache Aneinanderreihung von inverser Compton-Streuung und Paarproduktion. Bei den in dieser Arbeit allgemein betrachteten Kaskaden werden relativistische Elektronen und hochenergetische Photonen in eine Region mit niederenergetischen Photonen konstanter Dichte injiziert. Auf der Grundlage von Vorarbeiten wird eine mathematische Beschreibung für lineare inverse Compton-Paar-Kaskaden mit Entweichtermen ausgearbeitet. Es werden die zeit-unabhängigen kinetischen Gleichungen für Elektronen und Photonen hergeleitet, wobei auf eine vollständige Formulierung und auf die Begründung der korrekten Integrationsgrenzen aller Integrale durch die kinematischen Vorgaben geachtet wird. Bei der Bestimmung des potentiell beobachtbaren Gammastrahlenflusses werden sowohl der teilweise absorbierte, injizierte Fluss als auch der Fluss, der sich als Effekt der inversen Compton-Streuung, der Paar-Absorption und des Entweichens ergibt, einbezogen, was den entstehenden Spektren charakteristische Formen aufprägt. Die kinetische Gleichung der Elektronen wird durch iterative Vorgehensweisen numerisch gelöst. Es wird erklärt, warum eine punktweise Iteration von höheren zu niedrigeren Lorentz-Faktoren effizienter ist als die Iteration des gesamten Satzes von Stützstellen. Der Algorithmus wird an zwei Stellen parallelisiert. Erstens können mehrere Prozessor-Kerne gleichzeitig punktweise Iterationen durchführen. Zweitens wird das rechenintensivste Integral in mehrere Teilintegrale zerlegt, die von mehreren Kernen berechnet werden können. Durch diese Maßnahmen kann der Python-Code zur Simulation von zeitunabhängigen inversen Compton-Paar-Kaskaden eingesetzt werden. Im Fall von Markarian 501 wird folgendes Modell bemüht. Der aktive Galaxienkern hat einen advektionsdominierten Akkretionsfluss mit einer normalisierten Akkretionsrate von mehreren \(10^{-4}\) und einer Elektronentemperatur um \(10^{10}\) K. Einerseits bestrahlt der Akkretionsfluss die wenigen umgebenden Gaswolken mit ungefährem Radius von \(10^{11}\) m, die einen Faktor 0,01 der Leuchtkraft in Form von Wasserstoff- und Helium-Emissionslinien wieder abstrahlen. Andererseits erzeugen die vom Akkretionsfluss stammenden Gammaphotonen in einer zeitweise aktiven Vakuum-Lücke in der Magnetosphäre des Schwarzen Lochs Elektronen und Positronen. In der geöffneten Lücke wird dem rotierenden Schwarzen Loch durch einen Potentialunterschied von mehreren \(10^{18}\) V eine Leistung von etwa 0,001 der Blandford-Znajek-Leistung entzogen, wodurch ultra-relativistische Elektronen erzeugt werden, die anschließend durch Wechselwirkung mit den Photonen des Akkretionsflusses um einen Faktor von etwa \(10^6\) multipliziert werden. Dieser Elektronenstrahl verlässt die Magnetosphäre und trifft auf das Photonenfeld einer vorbeiziehenden ionisierten Wolke. Die daraus resultierende inverse Compton-Paar-Kaskade wird simuliert und das sich ergebende Gammastrahlenspektrum wird berechnet. Unmittelbar oberhalb der durch die Wasserstofflinien verursachten Absorptionströge erscheint bei rund 3 TeV ein schmaler Höcker. Wenn die Strahlung der Kaskade der aus größerer Entfernung stammenden Strahlung überlagert wird, wird die gesamte spektrale Energieverteilung einschließlich des scharfen Buckels bei 3 TeV reproduziert. Das bedeutet, dass schmale spektrale Merkmale für die Relevanz von Strahlungsprozessen sprechen, die über konventionelle Modelle hinausgehen. Der Trog im Spektrum von 3C 279 wird mit einem ähnlichen Kaskadenmodell untersucht. Es werden drei Fälle der Injektion betrachtet, die sich im Verhältnis der Photonen-Anzahl zur Elektronen-Anzahl und im spektralen Verlauf unterscheiden. Es wird angenommen, dass die Kaskade entweder im dichten Photonenfeld der BLR mit einer Leuchtkraft von mehreren \(10^{37}\) W und einer radialen Ausdehnung von einigen \(10^{14}\) m oder im ausgedünnten Photonenfeld außerhalb der BLR stattfindet. Das letztgenannte Szenario muss jedoch verworfen werden, da die spektrale Steigung bei einigen 100 MeV und der Absorptionstrog bei einigen 10 GeV innerhalb dieses Modells nicht miteinander in Einklang gebracht werden können. Die innerhalb der BLR kaskadierte Strahlung kann die Beobachtungsdaten unabhängig von der angenommenen Injektionsrate erklären. Daraus folgt, dass die Gammastrahlung während dieses Emissionsereignisses am Rande der BLR von 3C 279 produziert wird. Beide Untersuchungen zeigen, dass inverse Compton-Paar-Kaskaden Feinstrukturen in der spektralen Energieverteilung von Blasaren erklären können. Es reicht nicht aus, den Strahlungstransport auf reine exponentielle Absorption eines Injektionsterms zu beschränken. Paarbildung und inverse Compton-Streuung im optisch dicken Bereich und über alle Generationen von Photonen und Elektronen hinweg prägen die entstehenden Spektren entscheidend. Da künftige, verbesserte Detektoren detailliertere Spektren liefern werden, darf man weitere Berichte über schmale spektrale Merkmale erwarten. Es erscheint daher empfehlenswert, die Kaskadierung in konventionelle Modelle der Strahlungsproduktion mit einzubeziehen oder das in dieser Arbeit entwickelte Modell um Synchrotronstrahlung zu erweitern.

Variable active galactic nuclei showing periodic light curves have been proposed as massive black hole binary (MBHB) candidates. In such scenarios the periodicity can be due to relativistic Doppler-boosting of the emitted light. This hypothesis can be tested through the timing of scattered polarized light. Following the results of polarization studies in type I nuclei and of dynamical studies of MBHBs with circumbinary discs, we assume a coplanar equatorial scattering ring, whose elements contribute differently to the total polarized flux, due to different scattering angles, levels of Doppler boost, and line-of-sight time delays. We find that in the presence of a MBHB, both the degree of polarization and the polarization angle have periodic modulations. The minimum of the polarization degree approximately coincides with the peak of the light curve, regardless of the scattering ring size. The polarization angle oscillates around the semi-minor axis of the projected MBHB orbital ellipse, with a frequency equal either to the binary's orbital frequency (for large scattering screen radii), or twice this value (for smaller scattering structures). These distinctive features can be used to probe the nature of periodic MBHB candidates and to compile catalogs of the most promising sub-pc MBHBs. The identification of such polarization features in gravitational-wave detected MBHBs would enormously increase the amount of physical information about the sources, allowing the measurement of the individual masses of the binary components, and the orientation of the line of nodes on the sky, even for monochromatic gravitational wave signals., 11 pages, 6 figures, submitted to MNRAS

Active galactic nuclei (AGNs) are among the most luminous sources observed in the Universe - their overall luminosity can be over 12-15 orders of magnitude more luminous than our Sun’s. They harbour supermassive black holes at their centres that are estimated to have masses up to 10 billion solar masses and possess immense gravitational potential. When matter falls towards a black hole due to this potential, it gets heated up and shines. This is the only way to observe AGNs and their immediate environment. Quasars can be observed from cosmological distances and they can be excellent, not yet appreciated, indicators of the universe’s expansion rate. The analysis of several, mutually related issues regarding quasars is presented in this dissertation which will later facilitate the use of quasars in cosmology and tie them with the evolution of galaxies across cosmic time. Matter in-falling under the action of the gravity of the central supermassive black hole loses angular momentum while being accreted onto the black hole. This manifests in the form of an accretion disk around the black hole which in turn makes these systems non-spherically symmetric. The accreted matter gets heated up and radiates. The photon energy of the dissipated radiation spans from the near-infrared to the ultraviolet/X-rays and the radiation then illuminates the material surrounding the accretion disk. This phenomenon leads to the formation and emission of strong and broad emission lines. The size of this region, named broad-line region (BLR) extends from a few tens to a few thousand gravitational radii. These broad emission lines allow measuring the mass of the central supermassive black hole and underlie the use of quasars for cosmological applications, in addition to their vital role in estimating the driving parameters of the central engine and statistical studies that help address the diversity in AGN. Some of these emission lines are produced from the disk outflows which are highly ionized and are known as High-Ionization Lines (HILs, ionization potential, IP > 50 eV). On the other hand, emission lines from other ionic species are low ionized (IP < 20 eV) and are produced in a less ionized medium. These are called the Low-Ionization Lines (LILs). In this thesis, I concentrate on these Low-Ionization emission lines which are more reliable for black hole mass measurements. The emission line shapes, their intensity ratios and broadband spectral indices lead to the classifications of quasars. Principal Component Analysis (PCA) - a dimensionality reduction technique, that allowed to extract meaningful information from large datasets containing diverse quasar populations. A clear pattern originates from the analysis of the optical plane, i.e. the anti-correlation between the strength of the Fe II λ4570 (also known as RFeII) and the full width at half maximum (FWHM) of Hβ, and is known as the Quasar Main Sequence. The main sequence of quasars is an analogous scheme to the Hertzsprung-Rusell diagram. The stellar main sequence in the Hertzsprung-Rusell diagram is easy to understand since stars are characterized solely by their mass. Unlike stars, quasars are more complex. Their appearance is defined by the mass of the black hole, the accretion rate, spin and their inclination angle to the observer. The first issue is an attempt to have a deeper understanding of why such complex objects form an almost one-parameter family in the optical plane. Therefore, I introduce a physically motivated model which can explain these emission lines’ statistics. This model takes into account the underlying geometry of the active nucleus, including black hole mass, radiation from the accretion disk surrounding the black hole, the presence of hot corona, and the BLR gas cloud at the right distance from the centre. This ionized BLR gas cloud absorbs the radiation and re-emits in the form of the emission lines that are then observed in a spectrum. The radiative transfer in these media is solved to obtain the emission line ratios and line kinematic widths reflecting the motion of the line emitting clouds. The results from these model predictions are compared with available measurements of the emission line properties in ∼1 million quasars from the publicly available quasar catalogues. The model successfully reproduces the Main Sequence trend. In particular, iron emission calculations in the optical range require taking into account the iron atom model containing 371 levels with 68,535 transitions. The program shows that the model reproduces the behaviour of the quasar well if one also considers the complex relationship between the chemical composition and the density of the BLR clouds with the accretion rate. The higher the accretion rate, the more elements such as iron must be produced. This issue is addressed for the first time (Panda et al., 2018) by systematic theoretical modelling of the spectra of active galaxies. The results published in the first work required further clarification. Subsequently, I also include an additional spectral component - a warm corona (an inner warm comptonizing region to produce the soft X-ray excess) in the model (Panda et al., 2019a), and then incorporate the role of the viewing angle at which we observe the AGN (Panda et al., 2019c; Panda et al., 2020a). Treating the aspect of viewing angle and the distribution of the BLR clouds appropriately, I confirm the dependence of the Main Sequence on the Eddington ratio and the related observational trends - as a function of the shape of the ionizing continuum, cloud density, and composition, verified from prior observations. This allows me to affirm that quasars with different properties populate different parts of the Quasar Main Sequence. The results show that quasars that have very strong iron emission, accrete close to the Eddington limit and are seen under relatively small angles. These sources can serve as “standardizable” luminosity candles to probe the expansion of the Universe. The Fe II emission is observed from the ultraviolet to the near-infrared and acts as one of the main coolants of the BLR. However, the complex electronic structure of Fe II owing to varied excitation mechanisms makes it difficult to model the atom. In the concluding chapter of the thesis, the physical properties and location of the low ionization lines using the NIR Ca II triplet emission as a reliable proxy to the Fe II are explored. In the first part of the series (Panda et al., 2020b), the observational correlation between the strengths of the two species is updated and various photoionization models are tested taking into account (a) the ionization parameter, (b) the cloud density, (c) the metallicity, and (d) the column density, and, recover a linear, almost one-to-one relationship between the strengths of the two species. In the second part (Panda, 2021), synthetic equivalent widths (EWs) are derived accounting for reasonable covering fractions for these low-ionization species and a significant overlap in the emitting regions of the two species is recovered. This work also highlights the role of metallicity and cloud sizes in the study of accreting quasars and in addition the effect of the inclusion of microturbulence allows to limit the metal content in the BLR for the adequate Fe II emission. The collection of works in this thesis has shown that (i) the broad-line regions of active galaxies have an almost universal local density, (ii) there exists a coupling between the Eddington ratio and the metal content in these ionized media which validates the co-evolution of the host galaxy and the AGN, and (iii) the quasars can be used as reliable cosmological probes to investigate the expansion of our Universe., Supported by the Polish Funding Agency National Science Centre, grants 2015/17/B/ST9/03436/(OPUS 9) and 2017/26/A/ST9/00756 (MAESTRO 9)

It is well known that reverberation mapping of active galactic nuclei (AGN) reveals a relationship between AGN luminosity and the size of the broad-line region, and that use of this relationship, combined with the Doppler width of the broad emission line, enables an estimate of the mass of the black hole at the center of the active nucleus based on a single spectrum. An unresolved key issue is the choice of parameter used to characterize the line width, either FWHM or line dispersion (the square root of the second moment of the line profile). We argue here that use of FWHM introduces a bias, stretching the mass scale such that high masses are overestimated and low masses are underestimated. Here we investigate estimation of black hole masses in AGNs based on individual or "single epoch" observations, with a particular emphasis in comparing mass estimates based on line dispersion and FWHM. We confirm the recent findings that, in addition to luminosity and line width, a third parameter is required to obtain accurate masses and that parameter seems to be Eddington ratio. We present simplified empirical formulae for estimating black hole masses from the Hbeta 4861 A and C IV 1549 A emission lines. While the AGN continuum luminosity at 5100 A is usually used to predict the Hbeta reverberation lag, we show that the luminosity of the Hbeta broad component can be used instead without any loss of precision, thus eliminating the difficulty of accurately accounting for the host-galaxy contribution to the observed luminosity., Comment: 41 pages, 13 figures, accepted for publication in ApJ

Gravitational microlensing is a powerful tool for probing the inner structure of strongly lensed quasars and for constraining parameters of the stellar mass function of lens galaxies. This is achieved by analysing microlensing light curves between the multiple images of strongly lensed quasars and accounting for the effects of three main variable components: (1) the continuum flux of the source, (2) microlensing by stars in the lens galaxy, and (3) reverberation of the continuum by the broad line region (BLR). The latter, ignored by state-of-the-art microlensing techniques, can introduce high-frequency variations which we show carry information on the BLR size. We present a new method that includes all these components simultaneously and fits the power spectrum of the data in the Fourier space rather than the observed light curve itself. In this new framework, we analyse COSMOGRAIL light curves of the two-image system QJ 0158-4325 known to display high-frequency variations. Using exclusively the low-frequency part of the power spectrum, our constraint on the accretion disk radius agrees with the thin-disk model estimate and the results of previous work where the microlensing light curves were fit in real space. However, if we also take into account the high-frequency variations, the data favour significantly smaller disk sizes than previous microlensing measurements. In this case, our results are only in agreement with the thin-disk model prediction only if we assume very low mean masses for the microlens population, i.e. ⟨M⟩ = 0.01 M⊙. At the same time, including the differentially microlensed continuum reverberation by the BLR successfully explains the high frequencies without requiring such low-mass microlenses. This allows us to measure, for the first time, the size of the BLR using single-band photometric monitoring; we obtain RBLR = 1.6−0.8+1.5 × 1017 cm, in good agreement with estimates using the BLR size–luminosity relation.

Narrow-line Seyfert 1 galaxies (NLSy1s) are a well established class of &gamma, ray sources, showing the presence of a jet like the more common flat-spectrum radio quasars. The evidence of &gamma, ray emission poses the issue of the location of the &gamma, ray emitting zone and of the contribution of the &gamma, &gamma, absorption within the broad-line region (BLR), since such objects have been detected by Fermi-LAT in the MeV-GeV energy range but not by imaging atmospheric Cherenkov telescopes beyond 100 GeV. We discuss how the spectral properties of three NLSy1s (SBS 0846+513, PMN J0948+0022, and PKS 1502+036) derived from the Fermi Large Area Telescope Fourth Source Catalog (4FGL) compared with theoretical models based on the observed properties of the BLR. In particular, we focus on the question on how simple power-law spectral models and log-parabolic ones could be disentangled in &gamma, ray narrow-line Seyfert 1 galaxies by means of current Fermi-LAT or future imaging atmospheric Cherenkov telescopes data. We found that the only possibility for a log-parabolic model to mimic a power-law model in the energy band above E &sim, 100 GeV is to have a very small value of the curvature parameter &beta, &sim, 0.05 .

We use spectroscopic observations of the gravitationally lensed systems SDSS0924+0219(BC), Q1355-2257(AB), and SDSS1029+2623(BC) to analyze microlensing and dust extinction in the observed components. We detect chromatic microlensing effects in the continuum and microlensing in the broad emission line profiles of the systems SDSS0924+0219(BC), and Q1355-2257(AB). Using magnification maps to simulate microlensing and modeling the emitting region as a Gaussian intensity profile with size $r_s \propto \lambda ^p$, we obtain the probability density functions for a logarithmic size prior at $\lambda_{rest-frame}=3533$ {\AA}. In the case of SDSS0924+0219, we obtain: $r_s = 4^{+3}_{-2}$ $\sqrt{M/M_{\odot}}$ light-days (at $1 \sigma$), which is larger than the range of other estimates, and $p = 0.8 \pm 0.2$ (at $1 \sigma$), which is smaller than predicted by the thin disk theory, but still in agreement with previous results. In the case of Q1355-2257 we obtain (at $1 \sigma$): $r_s = 3.6^{+3.0}_{-1.6}$ $\sqrt{M/M_{\odot}}$ light-days, which is also larger than the theoretical prediction, and $p = 2.0 \pm 0.7$ that is in agreement with the theory within errors. SDSS1029+2326 spectra show evidence of extinction, probably produced by a galaxy in the vicinity of image C. Fitting an extinction curve to the data we estimate $\Delta E \sim 0.2$ in agreement with previous results. We found no evidence of microlensing for this system., Comment: 9 pages, 12 figures

The Sloan Digital Sky Survey Reverberation Mapping (SDSS-RM) program monitors 849 active galactic nuclei (AGN) both spectroscopically and photometrically. The photometric observations used in this work span over four years and provide an excellent baseline for variability studies of these objects. We present the photometric light curves from 2014 to 2017 obtained by the Steward Observatory's Bok telescope and the CFHT telescope with MegaCam. We provide details on the data acquisition and processing of the data from each telescope, the difference imaging photometry used to produce the light curves, and the calculation of a variability index to quantify each AGN's variability. We find that the Welch-Stetson J-index provides a useful characterization of AGN variability and can be used to select AGNs for further study., Comment: Accepted for publication in ApJS, 28 pages, 8 figures, 4 tables

3C 82 at a redshift of 2.87 is the most distant 3C (Third Cambridge Catalogue) quasar. Thus, it is a strong candidate to have the most luminous radio lobes in the Universe. 3C 82 belongs to the class of compact steep spectrum radio sources. We use single dish and interferometric radio observations in order to model the plasma state of these powerful radio lobes. It is estimated that the long-term time-averaged jet power required to fill these lobes with leptonic plasma is $\overline{Q} \approx 2.66 \pm 1.33 \times 10^{47} \rm{ergs/sec}$, among the largest time averaged jet powers from a quasar. Positing protonic lobes is not tenable since they would require two orders of magnitude more mass transport to the lobes than was accreted to the central black hole during their formation. The first high signal to noise optical spectroscopic observation obtained of this object indicates that there is a powerful high ionization broad line wind with a kinetic power $\sim 10^{45} \rm{ergs/sec}$ and a velocity $\sim 0.01$c. We also estimate from the broad lines in 2018 and the UV continuum in three epochs spread out over three decades that the accretion flow bolometric luminosity is $L_{\rm{bol}} \approx 3.2-5.8 \times 10^{46} \rm{ergs/sec}$. The ratio of $\overline{Q}/L_{\rm{bol}}\approx 6.91 \pm 3.41$, is perhaps the largest of any known quasar. Extremely powerful jets tend to strongly suppress powerful winds of ionized baryonic matter. Consequently, 3C 82 provides a unique laboratory for studying the dynamical limits of the central engine of outflow initiation in quasars., Comment: To appear in ApJ

We present reverberation-mapping lags and black-hole mass measurements using the CIV 1549 broad emission line from a sample of 349 quasars monitored as a part of the Sloan Digital Sky Survey Reverberation Mapping Project. Our data span four years of spectroscopic and photometric monitoring for a total baseline of 1300 days. We report significant time delays between the continuum and the CIV 1549 emission line in 52 quasars, with an estimated false-positive detection rate of 10%. Our analysis of marginal lag measurements indicates that there are on the order of 100 additional lags that should be recoverable by adding more years of data from the program. We use our measurements to calculate black-hole masses and fit an updated CIV radius-luminosity relationship. Our results significantly increase the sample of quasars with CIV RM results, with the quasars spanning two orders of magnitude in luminosity toward the high-luminosity end of the CIV radius-luminosity relation. In addition, these quasars are located at among the highest redshifts (z~1.4-2.8) of quasars with black hole masses measured with reverberation mapping. This work constitutes the first large sample of CIV reverberation-mapping measurements in more than a dozen quasars, demonstrating the utility of multi-object reverberation mapping campaigns., Comment: 42 pages (incl. 21 pages of tables): 12 figures, 5 tables. Submitted to AAS journals. Figures 8 and 12 are sets that will be provided in the online published version of the article, and the tables will also be provided fully online

To understand the nature of transient obscuring outflows in active galactic nuclei, we observed the Seyfert 1 galaxy NGC 3783 on two occasions in December 2016 triggered by Swift monitoring indicating strong soft X-ray absorption in November. We obtained ultraviolet spectra using COS on HST and optical spectra using FEROS on the MPG/ESO 2.2-m telescope that were simultaneous with X-ray spectra from XMM-Newton and NuSTAR. We find new components of broad, blue-shifted absorption associated with Ly$\alpha$, \ion{N}{v}, \ion{Si}{iv}, and \ion{C}{iv} in our COS spectra. The absorption extends from velocities near zero in the rest-frame of the host galaxy to $-6200$ $\rm km~s^{-1}$. These features appear for the first time in NGC 3783 at the same time as the heavy soft X-ray absorption seen in the XMM-Newton X-ray spectra. The X-ray absorption has a column density of $\sim 10^{23}~\rm cm^{-2}$, and it partially covers the X-ray continuum source. The X-ray absorption becomes more transparent in the second observation, as does the UV absorption. Combining the X-ray column densities with the UV spectral observations yields an ionization parameter for the obscuring gas of log $\xi =1.84^{+0.4}_{-0.2}$ $\rm erg~cm~s^{-1}$. Despite the high intensity of the UV continuum in NGC 3783, F(1470 \AA)=$8 \times 10^{-14}~\rm erg~cm^{-2}~s^{-1}~\AA^{-1}$, the well known narrow UV absorption lines are deeper than in earlier observations in unobscured states, and low ionization species such as \ion{C}{iii} appear, indicating that the narrow-line gas is more distant from the nucleus and is being shadowed by the gas producing the obscuration. Despite the high continuum flux levels in our observations of NGC 3783, moderate velocities in the UV broad line profiles have substantially diminished. We suggest that a collapse of the broad line region has led to the outburst and triggered the obscuring event., Comment: 24 pages, 29 figures, uses aa.cls. Accepted for publication in A&A, 10/29/2018

We present an analysis of 43 years (1972 to 2015) of spectroscopic observations of the Seyfert 1 galaxy NGC 5548. This includes 12 years of new unpublished observations (2003 to 2015). We compiled about 1600 H$\beta$ spectra and analyzed the long-term spectral variations of the 5100 \AA\ continuum and the H$\beta$ line. Our analysis is based on standard procedures including the Lomb-Scargle method, which is known to be rather limited to such heterogeneous data sets, and new method developed specifically for this project that is more robust and reveals a $\sim$5700 day periodicity in the continuum light curve, the H$\beta$ light curve and the radial velocity curve of the red wing of the H$\beta$ line. The data are consistent with orbital motion inside the broad emission line region of the source. We discuss several possible mechanisms that can explain this periodicity, including orbiting dusty and dust-free clouds, a binary black hole system, tidal disruption events, and the effect of an orbiting star periodically passing through an accretion disc., Comment: Accepted in ApJS, 64 pages, 10 figures and 4 tables

We present a systematic search for changing-look quasars based on repeat photometry from SDSS and Pan-STARRS1, along with repeat spectra from SDSS and SDSS-III BOSS. Objects with large, |\Delta g|>1 mag photometric variations in their light curves are selected as candidates to look for changes in broad emission line (BEL) features. Out of a sample of 1011 objects that satisfy our selection criteria and have more than one epoch of spectroscopy, we find 10 examples of quasars that have variable and/or "changing-look" BEL features. Four of our objects have emerging BELs; five have disappearing BELs, and one object shows tentative evidence for having both emerging and disappearing BELs. With redshifts in the range 0.20 < z < 0.63, this sample includes the highest-redshift changing-look quasars discovered to date. We highlight the quasar J102152.34+464515.6 at z = 0.204. Here, not only have the Balmer emission lines strongly diminished in prominence, including H$\beta$ all but disappearing, but the blue continuum $f_{\nu} \propto \nu^{1/3}$ typical of an AGN is also significantly diminished in the second epoch of spectroscopy. Using our selection criteria, we estimate that >15% of strongly variable luminous quasars display changing-look BEL features on rest-frame timescales of 8 to 10 years. Plausible timescales for variable dust extinction are factors of 2-10 too long to explain the dimming and brightening in these sources, and simple dust reddening models cannot reproduce the BEL changes. On the other hand, an advancement such as disk reprocessing is needed if the observed variations are due to accretion rate changes., Comment: 15 pages, 8 Figures, 3 Tables, replaced with version accepted to MNRAS