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Relevant bibliographies by topics / Nuclei-quasars

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Academic literature on the topic 'Nuclei-quasars'

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Published: 14 March 2023

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Journal articles on the topic "Nuclei-quasars"

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Kellermann, KI. "Compact Radio Sources, Quasars and Active Galactic Nuclei." Australian Journal of Physics 47, no. 5 (1994): 599. http://dx.doi.org/10.1071/ph940599.

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This paper reviews John G. Bolton's contributions to our understanding of compact radio sources associated with quasars and active galactic nuclei (AGNs), and his work leading to the discovery of quasars. Particular attention is given to the interpretation of the observed properties of quasars and AGNs within the framework of unified models which interpret the wide variety of observed properties as being the result of orientation rather than of any intrinsic differences.

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Kembhavi, Ajit K., Jayant V. Narlikar, and Kimberly A. Weaver. "Quasars and Active Galactic Nuclei: An Introduction." Physics Today 53, no. 5 (May 2000): 60–61. http://dx.doi.org/10.1063/1.883085.

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Pismis, P., E. Moreno, and A. Garcia-Barreto. "Collimated Bipolar Outflow and the Formation of Nuclear Spirals; Possible Role of Magnetic Fields." Symposium - International Astronomical Union 140 (1990): 447–48. http://dx.doi.org/10.1017/s0074180900190813.

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The existence of non–steady phenomena, namely activity in the form of radial motions (outflow) of matter from the nuclei of galaxies is well established at present. Active Galactic Nuclei (AGN) constitute a topic of great interest and are intensively studied by all existing observational techniques. Conventionally objects classified as AGN span a range from quasars, radio galaxies to Seyferts 1 and 2. It appears, however, that there exist galaxies which exhibit somewhat milder activity which does not qualify their inclusion in the AGN group. The designation of MAGN (M for mildly) was suggested in the past (Pismis, 1986) to cover the less energetic nuclei. It may be reasonable to consider that active nuclei form a sequence, the difference along it being due to the energetics of the nuclei, from the most active quasars and radio galaxies down to the mildest ones like M31 or our Galaxy. The phenomenon underlying the activity may thus be universal, subject to the intrinsic energetics of the nuclei (Pismis, 1987).

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Cavaliere, A., E. Giallongo, and F. Vagnetti. "From local active galactic nuclei to early quasars." Astrophysical Journal 296 (September 1985): 402. http://dx.doi.org/10.1086/163459.

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Antonucci, Robert. "Unified Models for Active Galactic Nuclei and Quasars." Annual Review of Astronomy and Astrophysics 31, no. 1 (September 1993): 473–521. http://dx.doi.org/10.1146/annurev.aa.31.090193.002353.

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Ellingson, E., H. K. C. Yee, and R. F. Green. "Quasars and active galactic nuclei in rich environments. I - Fields surrounding optically faint quasars." Astrophysical Journal Supplement Series 76 (June 1991): 455. http://dx.doi.org/10.1086/191574.

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Hough, D. H., and A. C. S. Readhead. "Relativistic Beaming and the Nuclei of Double-lobed Radio Quasars." Symposium - International Astronomical Union 129 (1988): 99–100. http://dx.doi.org/10.1017/s0074180900134114.

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We have defined a complete sample of double-lobed 3CR quasars with minimal orientation bias. Properties of these objects on the >kpc scale are consistent with the simple beaming model for their nuclei. VLBI maps of six nuclei reveal “core-jet” structures. Both nuclei mapped at multiple epochs are modestly superluminal (3C245, 3.1c; 3C263, 1.3c; H0=100 km/s/Mpc, q0=0.5). The distribution of apparent velocities in this sample will provide a stringent test of beaming.

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Banks, Michael. "NASA launches X-ray mission." Physics World 35, no. 1 (January 1, 2022): 13ii. http://dx.doi.org/10.1088/2058-7058/35/01/17.

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Falcke, H. "11.2. The nature of compact radio cores in galaxies." Symposium - International Astronomical Union 184 (1998): 459–60. http://dx.doi.org/10.1017/s0074180900085569.

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Compact radio cores, which are often assumed to mark the presence of a super-massive black hole, are not only found in the nuclei of powerful quasars but also in nearby galaxies. While in quasars they are typically associated with relativistic jets, the nature of those cores in low-luminosity AGN is less clear. Here, I will briefly mention some of the recent theories (ADAFs or jets) and observations of the latter class of objects.

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Akujor, Chidi E., R. W. Porcas, A. R. Patnaik, and A. Ardeberg. "Optically Quiet Quasars – Radio and Optical Investigations." Symposium - International Astronomical Union 159 (1994): 419. http://dx.doi.org/10.1017/s0074180900176041.

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The activity in the nuclei of bright galaxies could arise from a number of sources: they may contain compact variable radio sources, they may be strong IR/optical/X–ray continuum sources, or they may have strong emission lines. Usually but not always these properties go together as in radio loud quasars. However, there appears to exist a class of objects which resemble quasars in radio structure and brightness – have strong flat spectrum cores but appear fainter than would be suggested by their radio brightness – unidentified on sky surveys (Zensus & Porcas, 1985, in J. Dyson, ed, AGN). These are called ‘optically quiet quasars’ (OQQs).

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Dissertations / Theses on the topic "Nuclei-quasars"

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Haehnelt, Martin. "Quasars and the formation of galactic nuclei." Thesis, University of Cambridge, 1994. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.319491.

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Fernandes, Gomes da Costa Tiago André. "The interaction between quasars and their cosmic environment." Thesis, University of Cambridge, 2015. https://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.709197.

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Schindler, Jan-Torge, Xiaohui Fan, Ian D. McGreer, Qian Yang, Jin Wu, Linhua Jiang, and Richard Green. "The Extremely Luminous Quasar Survey in the SDSS Footprint. I. Infrared-based Candidate Selection." IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/627103.

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Studies of the most luminous quasars at high redshift directly probe the evolution of the most massive black holes in the early universe and their connection to massive galaxy formation. However, extremely luminous quasars at high redshift are very rare objects. Only wide-area surveys have a chance to constrain their population. The Sloan Digital Sky Survey (SDSS) has so far provided the most widely adopted measurements of the quasar luminosity function at z > 3. However, a careful re-examination of the SDSS quasar sample revealed that the SDSS quasar selection is in fact missing a significant fraction of z greater than or similar to 3 quasars at the brightest end. We identified the purely optical-color selection of SDSS, where quasars at these redshifts are strongly contaminated by late-type dwarfs, and the spectroscopic incompleteness of the SDSS footprint as the main reasons. Therefore, we designed the Extremely Luminous Quasar Survey (ELQS), based on a novel near-infrared JKW2 color cut using Wide-field Infrared Survey Explorer mission (WISE) AllWISE and 2MASS all-sky photometry, to yield high completeness for very bright (m(i) < 18.0) quasars in the redshift range of 3.0 <= z <= 5.0. It effectively uses random forest machinelearning algorithms on SDSS and WISE photometry for quasar-star classification and photometric redshift estimation. The ELQS will spectroscopically follow-up similar to 230 new quasar candidates in an area of similar to 12,000 deg(2) in the SDSS footprint to obtain a well-defined and complete quasar sample for an accurate measurement of the brightend quasar luminosity function (QLF) at 3.0 <= z <= 5.0. In this paper, we present the quasar selection algorithm and the quasar candidate catalog.

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Grier, C. J., J. R. Trump, Yue Shen, Keith Horne, Karen Kinemuchi, Ian D. McGreer, D. A. Starkey, et al. "The Sloan Digital Sky Survey Reverberation Mapping Project: Hα and Hβ Reverberation Measurements from First-year Spectroscopy and Photometry." IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/627102.

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We present reverberation mapping results from the first year of combined spectroscopic and photometric observations of the Sloan Digital Sky Survey Reverberation Mapping Project. We successfully recover reverberation time delays between the g+i band emission and the broad H beta emission line for a total of 44 quasars, and for the broad Ha emission line in 18 quasars. Time delays are computed using the JAVELIN and CREAM software and the traditional interpolated cross-correlation function (ICCF): using well-defined criteria, we report measurements of 32 H beta and 13 Ha lags with JAVELIN, 42 H beta and 17 Ha lags with CREAM, and 16 H beta and eight Ha lags with the ICCF. Lag values are generally consistent among the three methods, though we typically measure smaller uncertainties with JAVELIN and CREAM than with the ICCF, given the more physically motivated light curve interpolation and more robust statistical modeling of the former two methods. The median redshift of our H beta-detected sample of quasars is 0.53, significantly higher than that of the previous reverberation mapping sample. We find that in most objects, the time delay of the Ha emission is consistent with or slightly longer than that of H beta. We measure black hole masses using our measured time delays and line widths for these quasars. These black hole mass measurements are mostly consistent with expectations based on the local M-BH-sigma* relationship, and are also consistent with single-epoch black hole mass measurements. This work increases the current sample size of reverberation-mapped active galaxies by about two-thirds and represents the first large sample of reverberation mapping observations beyond the local universe (z < 0.3).

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Coatman, Liam. "A near-infrared view of luminous quasars : black hole masses, outflows and hot dust." Thesis, University of Cambridge, 2017. https://www.repository.cam.ac.uk/handle/1810/269406.

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Supermassive black holes (BHs) and their host-galaxies are thought to evolve in tandem, with the energy output from the rapidly-accreting BH regulating star formation and the growth of the BH itself. The goal of better understanding this process has led to much work focussing on the properties of quasars at high redshifts, $z\gtrsim 2$, when cosmic star formation and BH accretion both peaked. At these redshifts, however, ground-based statistical studies of the quasar population generally have no access to the rest-frame optical spectral region, which is needed to measure H$\beta$-based BH masses and narrow line region outflow properties. The cornerstone of this thesis has been a new near-infrared spectroscopic catalogue providing rest-frame optical data on 434 luminous quasars at redshifts $1.5 \lesssim z \lesssim 4$. At high redshift, $z \gtrsim 2$, quasar BH masses are derived using the velocity-width of the CIV broad emission-line, based on the assumption that the observed velocity-widths arise from virial-induced motions. However, CIV exhibits significant asymmetric structure which suggests that the associated gas is not tracing virial motions. By combining near-infrared spectroscopic data (covering the hydrogen Balmer lines) with optical spectroscopy from SDSS (covering CIV), we have quantified the bias in CIV BH masses as a function of the CIV blueshift. CIV BH masses are shown to be over-estimated by almost an order of magnitude at the most extreme blueshifts. Using the monotonically increasing relationship between the CIV blueshift and the mass ratio BH(CIV)/BH(H$\alpha$) we derive an empirical correction to all CIV BH-masses. The correction depends only on the CIV line properties and therefore enables the derivation of un-biased virial BH mass estimates for the majority of high-luminosity, high-redshift, spectroscopically confirmed quasars. Quasars driving powerful outflows over galactic scales is a central tenet of galaxy evolution models involving 'quasar feedback' and significant resources have been devoted to searching for observational evidence of this phenomenon. We have used [OIII] emission to probe ionised gas extended over kilo-parsec scales in luminous $z\gtrsim2$ quasars. Broad [OIII] velocity-widths and asymmetric structure indicate that strong outflows are prevalent in this population. We estimate the kinetic power of the outflows to be up to a few percent of the quasar bolometric luminosity, which is similar to the efficiencies required in recent quasar-feedback models. [OIII] emission is very weak in quasars with large CIV blueshifts, suggesting that quasar-driven winds are capable of sweeping away gas extended over kilo-parsec scales in the host galaxies. Using data from a number of recent wide-field photometric surveys, we have built a parametric SED model that is able to reproduce the median optical to infrared colours of tens of thousands of AGN at redshifts $1 < z < 3$. In individual objects, we find significant variation in the near-infrared SED, which is dominated by emission from hot dust. We find that the hot dust abundance is strongly correlated with the strength of outflows in the quasar broad line region, suggesting that the hot dust may be in a wind emerging from the outer edges of the accretion disc.

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Constantin, Anca. "Linking the Power Sources of Emission-Line Galaxy Nuclei from the Highest to the Lowest Redshifts." Ohio University / OhioLINK, 2004. http://www.ohiolink.edu/etd/view.cgi?ohiou1097611827.

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Down, Emily. "The orientation of accretion disks and jets in quasars." Thesis, University of Oxford, 2008. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.572597.

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All massive nearby galaxies, including our own, host supermassive black holes. Active galactic nuclei (AGN) are seen when such black holes accrete, and when they produce powerful jets of synchrotron-emitting plasma, they are termed radio-loud AGN. The close correlation between black hole mass and galaxy bulge mass in elliptical galaxies indicates that AGN feedback may be the key to the regulation of galaxy formation. It is thus necessary to fully understand the structure of AGN, the way that they are fuelled, and their duty cycle, in order to study the feedback processes and get a clear picture of galaxy formation. In this thesis, independent methods are developed to constrain the accretion disk and radio jet angles to the line of sight. H IX emission from a sub-sample of high-redshift quasars is measured from near-infrared spectroscopy and modelled as sums of different components, including the characteristic double-peaked profile which results from a thin, rotating accretion disk. Comparing the models using Bayesian evidence, almost all quasars were found to have infrared spectra consistent with the presence of a disk. The jet inclination angles of the same set of quasars were constrained by fitting a model, including the effect of Doppler boosting and the receding torus model for dust obscuration, to the radio \ spectral energy distribution. The fitted disk and jet angles correlate strongly, and are consistent with a model in which the radio jets are launched orthogonally to the plane of the accretion disk, as expected if the jet is powered by energy drawn from the spin of the black hole. Both disk and jet angles correlate with the observed linear source size, which is a projection effect; when deprojected using the fitted angles, the distribution of source sizes agrees with a scenario in which the sources expand into the surrounding medium at a constant rate up to ~ 1 Mpc and then shut off, probably as the nuclei become quiescent. The accretion disk angle was found to correlate weakly with the low-frequency radio luminosity, which provides direct, albeit tenuous, evidence for the receding torus model.

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Bouffet, Romuald. "Evolution de la structure VLBI des sources de l'ICRF : lien entre astrométrie et astrophysique." Thesis, Bordeaux, 2015. http://www.theses.fr/2015BORD0083/document.

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Les Noyaux Actifs de Galaxies (AGN) se situent au centre de galaxies extrêmement lointainesdont la luminosité provient de l’interaction d’un trou noir central supermassif et d’undisque d’accrétion. Il en résulte l’éjection à des vitesses relativistes de jets de matière collimatés.L’interférométrie à très longue base (VLBI) permet, grâce aux très grandes résolutionsatteintes, d’observer finement la structure de ces jets et de déterminer très précisément laposition astrométrique des objets. En raison de leur distance, les AGN ne présentent pas demouvements propres, ce qui les rend idéaux pour la construction de systèmes de référenceultra-précis et très stables.Des instabilités en position de quelques centaines de microsecondes d’arc, généralementimputées aux variations de la structure des jets, sont toutefois souvent observées sur des échellesde temps de quelques mois à quelques années. Le travail présenté ici étudie le lien entre les deuxphénomènes de façon statistique. Sur la base d’observations VLBI régulières conduites entre1994 et 2003, nous comparons l’évolution de la position astrométrique et de la structure des jetspour un échantillon de 68 AGN sur une période de 10 ans. Les résultats de l’étude indiquent quela corrélation entre les deux phénomènes existe mais n’est pas aussi forte qu’attendue. Le travailest complété par une simulation des effets causés sur la trajectoire des jets par la précessiondu disque d’accrétion ainsi que par la présence d’un système binaire de trous noirs. Appliquéeau cas de la source 1308+326, l’étude montre que l’amplitude de ces effets est compatible avecles oscillations de la trajectoire observées en VLBI
Active Galactic Nuclei (AGN) are located in the center of extremely distant and bright galaxies. Their luminosity comes from the interaction between a super-massive central blackhole and an accretion disk, producing a relativistic collimated jet of matter. Thanks to the extremely high resolution achieved by Very Long Base line Interferometry (VLBI), the jet structure may be studied in detail, while the astrometric position of the AGN is determined with ahigh accuracy. Because of their location at cosmological distances, no proper motions are detected for those objects, making them ideal fiducial points for building highly-precise celestial reference frames.Instabilities up to a few hundreds of micro arc seconds are yet often observed in astrometricpositions on time scales from months to years. This is generally thought to be caused by theevolution of source structure. The study presented here investigates the correlation between the two phenomena on a statistical basis. Based on regular VLBI observations conducted between1994 and 2003, astrometric position variations and source structure evolution are compared fora sample of 68 AGN over a period of 10 years. The results indicate that a correlation between the two phenomena does exist but it is not as strong as expected. Additionally, a simulation of the effects caused by the precession of the accretion disc and the potential presence of abinary black hole in the center of the AGN is presented. Applied to the source 1308+326, the simulation shows that the magnitude of the effects is consistent with the oscillations of the jet trajectory observed on VLBI scale

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Blank, Marvin, and Wolfgang J. Duschl. "Viscous time lags between starburst and AGN activity." OXFORD UNIV PRESS, 2016. http://hdl.handle.net/10150/621734.

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There is strong observational evidence indicating a time lag of order of some 100 Myr between the onset of starburst and AGN activity in galaxies. Dynamical time lags have been invoked to explain this. We extend this approach by introducing a viscous time lag the gas additionally needs to flow through the AGN's accretion disc before it reaches the central black hole. Our calculations reproduce the observed time lags and are in accordance with the observed correlation between black hole mass and stellar velocity dispersion.

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Draper, Aden R. "Understanding the connection between active galactic nuclei and host star formation through multi-wavelength population synthesis modeling." Diss., Georgia Institute of Technology, 2012. http://hdl.handle.net/1853/45748.

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Supermassive black holes, black holes with masses <106 Msun, are found at the centers of all massive galaxies. These massive black holes grew from smaller seed black holes through accretion events. Accreting black holes are very bright in the radio through very hard X-ray spectral regimes. Due to the location of these accreting black holes at the centers of galaxies, they are referred to as active galactic nuclei (AGN). It is understood that AGN are an important phase of galaxy evolution; however, the role of AGN in massive galaxy formation is very poorly constrained. Here, the unique tool of multi-wavelength population synthesis modeling is used to study the average properties of AGN and their host galaxies with a focus on host galaxy star formation and the role of black hole growth in galaxy evolution. Knowledge of the AGN population from deep X-ray surveys is combined with theoretical AGN spectral energy distributions to predict various observables of the AGN population in wavelength regions from the far infrared to very hard X-rays. Comparison of the model predictions to observations constrains the model input parameters and allows for the determination of average properties of the AGN population. Particular attention is paid to a special class of AGN known as Compton thick AGN. These AGN are deeply embedded in gas and dust such that the column density obscuring the line of sight to the central engine of the AGN exceeds 1/σT ~ 10²⁴ cm⁻², where σT is the Thomson cross-section of the electron---a column density comparable to that of the human chest. Theoretical and simulational evidence suggest that these Compton thick AGN may be recently triggered, rapidly accreting AGN, making them of special interest to researchers. I found that Compton thick AGN are likely to contribute ~20% of the peak of the cosmic X-ray background (XRB) at ~30 keV and demonstrated that a significant portion of Compton thick AGN may be accreting very rapidly. Moreover, Compton thick AGN do not appear to follow the orientation based unified model of AGN. According to the unified model, AGN exhibit a range of obscuration levels due to a dusty 'torus' which, depending on the orientation of the torus to the observer's line of sight, may obscure the central engine of the AGN. Upon further investigation into the stellar populations of AGN host galaxies, it appears that the unified model holds in general at z < 1, but not at z > 1. I found that this is likely due to the dominant triggering mechanism of AGN switching from major mergers at z > 1.5 to secular processes by z ~ 1.

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Books on the topic "Nuclei-quasars"

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1938-, Narlikar Jayant Vishnu, ed. Quasars and active galactic nuclei: An introduction. Cambridge: Cambridge University Press, 1999.

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Space Telescope Science Institute (U. Polarization of Active Galactic Nuclei and Quasars. S.l: s.n, 1986.

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Kvazary i aktivnostʹ i͡ader galaktik. Moskva: "Nauka," Glav. red. fiziko-matematicheskoĭ lit-ry, 1985.

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Active galactic nuclei: From the central black hole to the galactic environment. Princeton, N.J: Princeton University Press, 1999.

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Bahcall, John N. PKS 2349-014: A luminous quasar with thin wisps, a large off-center nebulosity, and a close companion galaxy. [Washington, DC: National Aeronautics and Space Administration, 1995.

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Sofia, Kirhakos, Schneider Donald P, and United States. National Aeronautics and Space Administration., eds. PKS 2349-014: A luminous quasar with thin wisps, a large off-center nebulosity, and a close companion galaxy. [Washington, DC: National Aeronautics and Space Administration, 1995.

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Sofia, Kirhakos, Schneider Donald P, and United States. National Aeronautics and Space Administration., eds. PKS 2349-014: A luminous quasar with thin wisps, a large off-center nebulosity, and a close companion galaxy. [Washington, DC: National Aeronautics and Space Administration, 1995.

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Sofia, Kirhakos, Schneider Donald P, and United States. National Aeronautics and Space Administration., eds. PKS 2349-014: A luminous quasar with thin wisps, a large off-center nebulosity, and a close companion galaxy. [Washington, DC: National Aeronautics and Space Administration, 1995.

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Narlikar, Jayant V., and Ajit K. Kembhavi. Quasars and Active Galactic Nuclei: An Introduction. Cambridge University Press, 2012.

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Narlikar, Jayant V., and Ajit K. Kembhavi. Quasars and Active Galactic Nuclei: An Introduction. University of Cambridge ESOL Examinations, 1999.

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Book chapters on the topic "Nuclei-quasars"

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Combes, Françoise, Patrick Boissé, Alain Mazure, and Alain Blanchard. "Quasars and Other Active Nuclei." In Galaxies and Cosmology, 259–88. Berlin, Heidelberg: Springer Berlin Heidelberg, 2002. http://dx.doi.org/10.1007/978-3-662-04849-8_10.

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Wilkes, Belinda J. "Quasars and Active Galactic Nuclei." In Allen’s Astrophysical Quantities, 585–611. New York, NY: Springer New York, 2002. http://dx.doi.org/10.1007/978-1-4612-1186-0_24.

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Combes, Françoise, Patrick Boissé, Alain Mazure, and Alain Blanchard. "Quasars and Other Active Nuclei." In Galaxies and Cosmology, 239–67. Berlin, Heidelberg: Springer Berlin Heidelberg, 1995. http://dx.doi.org/10.1007/978-3-662-03190-2_10.

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Pérez-Fournon, I., and P. Biermann. "A Shock Model for Quasars and Active Galactic Nuclei." In Quasars, 405–6. Dordrecht: Springer Netherlands, 1986. http://dx.doi.org/10.1007/978-94-009-4716-0_92.

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Ananthakrishnan, S., and V. K. Kulkarni. "High Resolution VLBI Observations of the Nuclei of Bright Galaxies and Quasars at 327 MHz." In Quasars, 169–70. Dordrecht: Springer Netherlands, 1986. http://dx.doi.org/10.1007/978-94-009-4716-0_42.

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Wills, Beverley J., D. Wills, N. J. Evans, A. Natta, K. L. Thompson, M. Breger, M. L. Sitko, D. F. Lester, D. R. Garnett, and S. R. Sawyer. "Polarization of Iras Quasars and the Inner Structure of Active Galactic Nuclei." In Active Galactic Nuclei, 325–26. Dordrecht: Springer Netherlands, 1989. http://dx.doi.org/10.1007/978-94-009-0963-2_99.

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Hough, D. H., and A. C. S. Readhead. "Relativistic Beaming and the Nuclei of Double-lobed Radio Quasars." In The Impact of VLBI on Astrophysics and Geophysics, 99–100. Dordrecht: Springer Netherlands, 1988. http://dx.doi.org/10.1007/978-94-009-2949-4_35.

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Marshall, Herman L. "The Luminosity Function of Quasars and Low Luminosity Active Galactic Nuclei." In Structure and Evolution of Active Galactic Nuclei, 627–32. Dordrecht: Springer Netherlands, 1986. http://dx.doi.org/10.1007/978-94-009-4562-3_63.

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Peng, Qiuhe, Zongyun Li, and Deya Wang. "The Magnetic Monopoles Content of Galactic Nuclei, Quasars, Stars and Planets." In Structure and Evolution of Active Galactic Nuclei, 659–61. Dordrecht: Springer Netherlands, 1986. http://dx.doi.org/10.1007/978-94-009-4562-3_70.

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Ruzmaikin, A. A., A. M. Shukurov, and D. D. Sokoloff. "Problems of Magnetic Field Generation in Galactic Nuclei, Quasars and Radiogalaxies." In Astrophysics and Space Science Library, 269–83. Dordrecht: Springer Netherlands, 1988. http://dx.doi.org/10.1007/978-94-009-2835-0_9.

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Conference papers on the topic "Nuclei-quasars"

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Collin, Suzy. "Quasars and Galactic Nuclei, a Half-Century Agitated Story." In ALBERT EINSTEIN CENTURY INTERNATIONAL CONFERENCE. AIP, 2006. http://dx.doi.org/10.1063/1.2399629.

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WILKES, B. J. "SPECTRAL ENERGY DISTRIBUTIONS (SEDS) OF QUASARS AND ACTIVE GALACTIC NUCLEI (AGN)." In Proceedings of the Guillermo Haro Conference 2003. WORLD SCIENTIFIC, 2004. http://dx.doi.org/10.1142/9789812702432_0065.

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Chuprikov, Andrey, and I. Guirin. "Imaging of quasars and active galactic nuclei. Fine-scale structure evolution." In 8th European VLBI Network Symposium. Trieste, Italy: Sissa Medialab, 2007. http://dx.doi.org/10.22323/1.036.0015.

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Blaes, Omer. "Optical/ultraviolet continuum emission theory in radio quiet quasars and active galactic nuclei." In Accretion processes in astrophysical systems: Some like it hot! - eigth astrophysics conference. AIP, 1998. http://dx.doi.org/10.1063/1.55891.

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Sameshima, Hiroaki, Yuzuru Yoshii, and Kimiaki Kawara. "Chemical Evolution of the Universe at 0.7 < z < 1.6 Derived from Abundance Diagnostics of Quasars." In Proceedings of the 14th International Symposium on Nuclei in the Cosmos (NIC2016). Journal of the Physical Society of Japan, 2017. http://dx.doi.org/10.7566/jpscp.14.010203.

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