Relevant bibliographies by topics / AGN galaxies

Contents

  1. Journal articles
  2. Dissertations / Theses
  3. Books
  4. Book chapters
  5. Conference papers
  6. Reports

Academic literature on the topic 'AGN galaxies'

Author: Grafiati
Published: 4 June 2021
Last updated: 2 February 2022

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Journal articles on the topic "AGN galaxies"

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Veilleux, Sylvain. "AGN host galaxies." New Astronomy Reviews 52, no. 6 (August 2008): 289–306. http://dx.doi.org/10.1016/j.newar.2008.06.011.

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Turatto, Massimo, Enrico Cappellaro, and Artashes R. Petrosian. "Supernova Types, Star Formation and AGN." Symposium - International Astronomical Union 194 (1999): 364–72. http://dx.doi.org/10.1017/s0074180900162308.

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New values of the frequencies of SNe are presented and discussed in relation to their use as SF indicators. The rate of core-collapse SNe is correlated to the colors and the FIR excesses of the parent galaxies in the sense that galaxies with blue colors and strong infrared excess have higher occurrence of type II and Ib/c SNe than other galaxies. This is in agreement with the expectation that they contain a higher fraction of massive stars. Instead no correlation is present for SNIa. The SN frequency does not correlate with the galaxy activity probably because searches are unable to discover SNe in the nuclear regions of galaxies.A number of SNe with spectra similar to those of AGN exist. Their characteristic features are explained with explosion of SNe in dense environments, reminding of cSNR's invoked in the starburst model for AGNs. Some recent, peculiar SNe seem linked to GRB's opening the possibility that at least some GRB's arise from this kind of stellar explosion.
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Shabala, Stanislav, Sugata Kaviraj, and Joseph Silk. "Effects of large-scale AGN feedback in local galaxies." Proceedings of the International Astronomical Union 8, S292 (August 2012): 375. http://dx.doi.org/10.1017/s1743921313001762.

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AbstractThe effects of active galactic nucleus (AGN) feedback on group and cluster galaxies are investigated. We examine the colors of non-AGN hosts (i.e. satellite galaxies) by comparing galaxies overrun by radio AGN with similar galaxies located outside the radio AGN contours. We find that powerful Fanaroff-Riley type II (edge-brightened) radio AGN truncate star formation in the galaxies overrun by AGN-driven bow shocks. On the other hand, the ubiquitous Fanaroff-Riley type I (core-dominated) AGN do not affect neighboring galaxies. This result shows that, despite their rarity, feedback from powerful radio AGN is an important factor in the evolution of group/cluster galaxies.
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Barthel, Peter. "Star-forming AGN host galaxies." New Astronomy Reviews 45, no. 9-10 (October 2001): 591–99. http://dx.doi.org/10.1016/s1387-6473(01)00139-7.

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Greene, Jenny E., Aaron J. Barth, and Luis C. Ho. "The smallest AGN host galaxies." New Astronomy Reviews 50, no. 9-10 (November 2006): 739–42. http://dx.doi.org/10.1016/j.newar.2006.06.080.

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Dashyan, Gohar, Joseph Silk, Gary A. Mamon, Yohan Dubois, and Tilman Hartwig. "AGN feedback in dwarf galaxies?" Monthly Notices of the Royal Astronomical Society 473, no. 4 (October 23, 2017): 5698–703. http://dx.doi.org/10.1093/mnras/stx2716.

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Kaviraj, Sugata, Stanislav S. Shabala, Adam T. Deller, and Enno Middelberg. "Radio AGN in spiral galaxies." Monthly Notices of the Royal Astronomical Society 454, no. 2 (October 6, 2015): 1595–604. http://dx.doi.org/10.1093/mnras/stv1957.

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Väisänen, Petri. "AGN, host galaxies, and starbursts." Proceedings of the International Astronomical Union 15, S356 (October 2019): 169. http://dx.doi.org/10.1017/s1743921320002811.

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AbstractAGN by definition live in galaxies. Despite a long history of studies, there is still much ongoing research into the interplay of the nucleus and the host galaxy, how do they affect each other, how is their evolution intertwined. This review will briefly go over the historical developments behind the current understanding of AGN host galaxies, their types and characteristics. It will discuss the starburst and AGN connection in particular, and how these phenomena may be connected or influence each other by means of e.g. gas flows. Finally, some examples of AGN/starburst evolution studies from SALT and other large telescopes will be presented.
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Erastova, L. K. "Byurakan Surveys: Density of Bright AGN." International Astronomical Union Colloquium 184 (2002): 92–93. http://dx.doi.org/10.1017/s0252921100030529.

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It is clear now that morphological criteria don’t divide galaxies from QSOs. Many galaxies are stellar-like objects and, conversely, quasars have host galaxies of various luminosities. For instance, two objects - SBS 1120+586A and SBS 1123+598 - absolutely do not differ from stars on the charts of the POSS and were classified as BSO-type. But they turned out to be galaxies with moderate luminosities (Markarian et al. 1988). Erastova (2000) produced a list of stellar-like galaxies from the SBS. Out of 339 KUV objects, 107 (31.6%) are emission-line galaxies of various luminosities (Darling & Wegner 1996). A considerable number of active galaxies appear among CSO - Case stellar objects. Conversely, objects having extended images on low-dispersion spectral plates turned out to be QSOs. SBS 1520+530 is a gravitationally lensed QSO with z=1.855 and on our low-dispersion plates appears as a galaxy (Chavushyan et al., 1997).
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de Vries, Nathan, I. A. G. Snellen, R. T. Schilizzi, M. D. Lehnert, and M. N. Bremer. "Massive galaxies with very young AGN." Proceedings of the International Astronomical Union 3, S245 (July 2007): 261–62. http://dx.doi.org/10.1017/s1743921308017870.

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AbstractGigahertz Peaked Spectrum (GPS) radio galaxies are generally thought to be the young counterparts of classical extended radio sources and live in massive ellipticals. GPS sources are vital for studying the early evolution of radio-loud AGN, the trigger of their nuclear activity, and the importance of feedback in galaxy evolution. We study the Parkes half-Jansky sample of GPS radio galaxies of which now all host galaxies have been identified and 80% has their redshifts determined (0.122 < z < 1.539). Analysis of the absolute magnitudes of the GPS host galaxies show that at z > 1 they are on average a magnitude fainter than classical 3C radio galaxies. This suggests that the AGN in young radio galaxies have not yet much influenced the overall properties of the host galaxy. However their restframe UV luminosities indicate that there is a low level of excess as compared to passive evolution models.
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Dissertations / Theses on the topic "AGN galaxies"

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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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Hill, Michael David. "The evolution of galaxies and AGN." Thesis, Durham University, 2010. http://etheses.dur.ac.uk/508/.

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This thesis presents a study of some current questions regarding the evolution of galaxies and AGN. We first argue that the bright submillimetre number counts may be dominated by obscured AGN rather than ultraluminous starbursts. Through statistical analyses of the ECDFS and WHDF, we show that N_H > 10^22 cm^−2 AGN are typically bright at 870um, with less absorbed AGN being much weaker sub-mm emitters. Overall, X-ray-detected AGN contribute 1.5+/-0.1 Jy deg^−2 to the sub-mm background, ~3% of the total, in agreement with the prediction of an AGN model which also fits the bright sub-mm counts. When Compton-thick, X-ray-undetected sources are included, this non-unified model predicts a total AGN contribution to the sub-mm background of 25-40%. The measured dependences of sub-mm flux on X-ray flux, luminosity and column density all agree well with model predictions. We therefore suggest that sub-mm galaxies may contain the absorbed AGN population which has long been sought to explain the X-ray background. Moving to shorter wavelengths, we find that AGN may continue to dominate the source counts down to ~200um. Below this, dusty star-forming galaxies are shown to fit the observed number counts and colours reasonably well. Below ~5um starlight takes over from dust as the main source of flux. These conclusions are supported by the good fit to the observations of phenomenological models assuming pure luminosity evolution. Finally, using a new survey of z~3 Lyman-break galaxies (LBGs), we find evidence for the supernova-driven feedback which is thought to be an essential ingredient of galaxy evolution. By cross-correlating LBG positions with Lya absorption in quasar sightlines, we find (a) that the intergalactic medium shows excess neutral hydrogen within 4 h^−1 Mpc of LBG positions, consistent with their lying in overdense regions, but also (b) that a Lya transmission spike may exist extending out to ~1.5 h^−1 Mpc around LBGs, indicating that galactic winds from LBGs may have ionised the IGM within this radius.
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Bieri, Rebekka. "The Role of AGN Feedback in Galaxy Formation." Thesis, Paris 6, 2016. http://www.theses.fr/2016PA066292/document.

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L’objectif de ma thèse porte sur les interactions entre les noyaux actifs de galaxies et le milieu interstellaire des galaxies. En particulier, je mets l’accent sur les deux mécanismes possibles responsables de la production des vents par les trous noirs : les jets et les vents produits par le rayonnement de ces trous noirs. Les simulations hydrodynamiques de haute résolution des galaxies comprenant la rétroac- tion d’un jet ont montré que l’activité des noyaux actifs peut conduire à une pression exces- sive sur les régions denses de formation stellaire dans les galaxies, et donc à augmenter la formation d’étoiles, conduisant à un effet positif de rétroaction. Je montre que ces noyaux actifs induits par pression régulée et formation d’étoiles peuvent aussi être une explica- tion possible des taux de formation stellaire élevés observés dans l’Univers à haut décalage spectral. De plus, j’ai également étudié en détails comment le rayonnement émis à partir d’un disque d’accrétion autour du trou noir agit efficacement avec le milieu interstellaire et entraîne un fort vent galactique, en simulant la propagation des photons à partir des équations hydrodynamiques du rayonnement. Les simulations montrent que la grande luminosité d’un quasar est en effet capable de conduire des vents à grande échelle et à grande vitesse. Le rayonnement infrarouge est nécessaire pour transérer efficacement le gaz par multi-diffusion sur la poussière dans les nuages denses. Le nombre typique de multi-diffusion diminue rapidement quand le nuage central de gaz central se dilate et se rompt, ce qui permet au rayonnement de s’échapper à travers les canaux à faible densité
Supermassive black holes (SMBHs) are known to reside in the centres of most large galaxies. The masses of these SMBHs are known to correlate with large-scale properties of the host galaxy suggesting that the growth of the BHs and large-scale structures are tightly linked. A natural explanation for the observed correlation is to invoke a self-regulated mechanism involving feedback from Active Galactic Nuclei (AGN). The focus of this thesis is on the interactions between AGN outflows and the ISM and how the feedback impacts the host galaxy. In particular, it focuses on the two possible mechanism of outflows, namely, outflows related to AGN jets and outflows produced by AGN radiation. High resolution, galaxy scale hydrodynamical simulations of jet-driven feedback have shown that AGN activity can over-pressurise dense star-formation regions of galaxies and thus enhance star formation, leading to a positive feedback effect. I propose, that such AGN-induced pressure-regulated star formation may also be a possible explanation of the high star formation rates recently found in the high-redshift Universe. In order to study in more detail the effects of over-pressurisation of the galaxy, I have performed a large set of isolated disc simulations with varying gas-richness in the galaxy. I found that even moderate levels of over-pressurisation of the galaxy boosts the global star formation rate by an order of magnitude. Additionally, stable discs turn unstable which leads to significant fragmentation of the gas content of the galaxy, similar to what is observed in high-redshift galaxies. The observed increase in the star formation rate of the galaxy is in line with theoretical predictions. I have also studied in detail how radiation emitted from a thin accretion disc surrounding the BH effectively couples to the surrounding ISM and drives a large scale wind. Quasar activity is typically triggered by extreme episodes of gas accretion onto the SMBH, in particular in high-redshift galaxies. The photons emitted by a quasar eventually couple to the gas and drive large scale winds. In most hydrodynamical simulations, quasar feedback is approximated as a local thermal energy deposit within a few resolution elements, where the efficiency of the coupling between radiation of the gas is represented by a single parameter tuned to match global observations. In reality, this parameter conceals various physical processes that are not yet fully un- derstood as they rely on a number of assumptions about, for instance, the absorption of photons, mean free paths, optical depths, and shielding. To study the coupling between the photons and the gas I simulated the photon propagation using radiation-hydrodynamical equations (RHD), which describe the emission, absorption and propagation of photons with the gas and dust. Such an approach is critical for a better understanding of the coupling between the radiation and gas and how hydrodynamical sub-grid models can be improved in light of these results
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Satyapal, Shobita, Nathan J. Secrest, Claudio Ricci, Sara L. Ellison, Barry Rothberg, Laura Blecha, Anca Constantin, Mario Gliozzi, Paul McNulty, and Jason Ferguson. "Buried AGNs in Advanced Mergers: Mid-infrared Color Selection as a Dual AGN Candidate Finder." IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/626062.

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A direct consequence of hierarchical galaxy formation is the existence of dual supermassive black holes, which may be preferentially triggered as active galactic nuclei (AGNs) during galaxy mergers. Despite decades of searching, however, dual AGNs are extremely rare, and most have been discovered serendipitously. Using the all-sky WISE survey, we identified a population of over 100 morphologically identified interacting galaxies or mergers that display red mid-infrared colors often associated in extragalactic sources with powerful AGNs. The vast majority of these advanced mergers are optically classified as star-forming galaxies, which suggests that they may represent an obscured population of AGNs that cannot be found through optical studies. In this work, we present Chandra/ACIS observations and near-infrared spectra with the Large Binocular Telescope of six advanced mergers with projected pair separations less than similar to 10 kpc. The combined X-ray, near-infrared, and mid-infrared properties of these mergers provide confirmation that four out of the six mergers host at least one AGN, with four of the mergers possibly hosting dual AGNs with projected separations less than similar to 10 kpc, despite showing no firm evidence for AGNs based on optical spectroscopic studies. Our results demonstrate that (1) optical studies miss a significant fraction of single and dual AGNs in advanced mergers, and (2) mid-infrared pre-selection is extremely effective in identifying dual AGN candidates in late-stage mergers. Our multi-wavelength observations suggest that the buried AGNs in these mergers are highly absorbed, with intrinsic column densities in excess of similar to N-H > 10(24) cm(-2), consistent with hydrodynamic simulations.
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Secrest, Nathan J., Henrique R. Schmitt, Laura Blecha, Barry Rothberg, and Jacqueline Fischer. "Was 49b: An Overmassive AGN in a Merging Dwarf Galaxy?" IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/623232.

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We present a combined morphological and X-ray analysis of Was. 49, an isolated, dual-AGN system notable for the presence of a dominant AGN, Was 49b, in the disk of the primary galaxy, Was 49a, at a projected radial distance of 8. kpc from the nucleus. Using X-ray data from Chandra, the Nuclear Spectroscopic Telescope Array, and Swift, we find that this AGN has a bolometric luminosity of L-bol similar to 10(45) erg s(-1), with a black hole mass of M-BH = 1.3(-0.9)(+10)M(circle dot) . Despite the large mass, our analysis of optical data from the Discovery Channel Telescope shows that the supermassive black hole (SMBH) is hosted by a stellar counterpart with a mass of only 5.6(-2.6)(+4.9)M(circle dot), which makes the SMBH potentially larger than expected from SMBH-galaxy scaling relations, and the stellar counterpart exhibits a morphology that is consistent with dwarf elliptical galaxies. Our analysis of the system in the r and K bands indicates that Was. 49 is a minor merger, with the mass ratio of Was 49b to Was 49a between similar to 1:7 and similar to 1:15. This is in contrast with findings that the most luminous merger-triggered AGNs are found in major mergers and that minor mergers predominantly enhance AGN activity in the primary galaxy.
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Batiste, Merida, Misty C. Bentz, Sandra I. Raimundo, Marianne Vestergaard, and Christopher A. Onken. "Recalibration of the MBH–σ⋆ Relation for AGN." IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/623860.

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We present a recalibration of the M-BH-sigma(star) relation, based on a sample of 16 reverberation-mapped galaxies with newly determined bulge stellar velocity dispersions (sigma(star)) from integral-field spectroscopy (IFS), and a sample of 32 quiescent galaxies with publicly available IFS. For both samples, sigma(star) is determined via two different methods that are popular in the literature, and we provide fits for each sample based on both sets of sigma(star). We find the fit to the active galactic nucleus sample is shallower than the fit to the quiescent galaxy sample, and that the slopes for each sample are in agreement with previous investigations. However, the intercepts to the quiescent galaxy relations are notably higher than those found in previous studies, due to the systematically lower sigma(star) measurements that we obtain from IFS. We find that this may be driven, in part, by poorly constrained measurements of bulge effective radius (r(e)) for the quiescent galaxy sample, which may bias the sigma(star) measurements low. We use these quiescent galaxy parameterizations, as well as one from the literature, to recalculate the virial scaling factor f. We assess the potential biases in each measurement, and suggest f = 4.82 +/- 1.67 as the best currently available estimate. However, we caution that the details of how sigma(star) is measured can significantly affect f, and there is still much room for improvement.
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Kirkpatrick, Allison, Stacey Alberts, Alexandra Pope, Guillermo Barro, Matteo Bonato, Dale D. Kocevski, Pablo Pérez-González, et al. "The AGN–Star Formation Connection: Future Prospects with JWST." IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/626176.

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The bulk of the stellar growth over cosmic time is dominated by IR-luminous galaxies at cosmic noon (z = 1-2), many of which harbor a hidden active galactic nucleus (AGN). We use state-of-the-art infrared color diagnostics, combining Spitzer and Herschel observations, to separate dust-obscured AGNs from dusty star-forming galaxies (SFGs) in the CANDELS and COSMOS surveys. We calculate 24 mu m counts of SFGs, AGN/star-forming "Composites," and AGNs. AGNs and Composites dominate the counts above 0.8 mJy at 24 mu m, and Composites form at least 25% of an IR sample even to faint detection limits. We develop methods to use the Mid-Infrared Instrument (MIRI) on JWST to identify dust-obscured AGNs and Composite galaxies from z similar to 1-2. With the sensitivity and spacing of MIRI filters, we will detect >4 times as many AGN hosts as with Spitzer/IRAC criteria. Any star formation rates based on the 7.7 mu m PAH feature (likely to be applied to MIRI photometry) must be corrected for the contribution of the AGN, or the star formation rate will be overestimated by similar to 35% for cases where the AGN provides half the IR luminosity and similar to 50% when the AGN accounts for 90% of the luminosity. Finally, we demonstrate that our MIRI color technique can select AGNs with an Eddington ratio of lambda(Edd) similar to 0.01 and will identify AGN hosts with a higher specific star formation rate than X-ray techniques alone. JWST/MIRI will enable critical steps forward in identifying and understanding dust-obscured AGNs and the link to their host galaxies.
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Bourne, Martin Albert. "Destroying galaxies (or not) with AGN feedback." Thesis, University of Leicester, 2015. http://hdl.handle.net/2381/36273.

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Supermassive black holes (SMBHs) are believed to reside at the centres of most galaxies. Observations suggest that the host galaxies are strongly affected by feedback produced by accreting SMBHs. Feedback in the form of ultra-fast outflows (UFOs), which are expected to interact with the interstellar medium (ISM), have been used to explain scaling relations between SMBHs and their host galaxies. Such relations suggest that the feedback and ISM must couple very weakly, however, it is not clear how this is achieved. In this thesis I provide observational tests to constrain UFO shock physics. I show that if UFO shocks cool via inverse Compton (IC) scattering, they should be observable in X-rays, but are not actually seen. The likely explanation for this is that the outflow is in a two-temperature, non-radiative regime. This implies that AGN outflows do not loose their kinetic energy to radiation and that an alternative energy loss mechanism is needed to explain the weak coupling required. I use high-resolution simulations to investigate an UFO impacting upon a turbulent ISM. Complex processes occur in the turbulent medium, such as the detachment of mass and energy flows, which are missed in a homogeneous medium. While the shocked UFO can escape through low density regions, high density clumps are resistant to feedback and can continue to have negative radial velocities. Energy losses in the multiphase ISM may provide an alternative to the IC radiative loss mechanism. Given the importance placed upon simulations in aiding our understanding of AGN feedback, I present a resolution study using a commonly employed sub-grid feedback prescription. I find that changes in resolution impact upon feedback efficiency, although not necessarily in a systematic way. I therefore suggest caution when analysing simulation results in order to ensure that numerical artefacts are not interpreted as physical phenomena.
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Hyde, Ashley. "Far infrared galaxies : star formation and AGN." Thesis, Imperial College London, 2014. http://hdl.handle.net/10044/1/25502.

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This thesis examines the AGN - star formation relation in galaxies out to z=4, probing the interplay between these two phenomena at various redshifts, for different galaxy morphologies, and at different luminosities. We have created a catalogue of 12,000 local infrared galaxies with optical morphological classifications, BPT analysis, and physical parameters derived from SED fits. We explore the variation in specific SFR and AGN fraction with morphology, compare star formation rate estimators, and provide a morphological breakdown of the IR luminosity distribution. Focusing on the Spirals and Barred Spirals from the M-IIFSCz, we find their distributions of specific star formation rates are statistically consistent. Conversely, Barred Spirals have a significantly higher AGN fraction than non-barred Spirals at both high and low stellar masses, but if we control for g-r colour, the AGN fraction is independent of bar presence. We discuss the implications of this result. We perform spectroscopic follow-up of 46 galaxies identified in the IIFSCz as ULIRGs and HLIRGs through photometric redshifts. By deriving spectroscopic redshifts, we show that their photometric redshifts are overestimated by an average factor of zphot/zspec=1.7. We quantify the implications for the Luminosity Function and show that applying a general correction for photometric redshift over- estimation reduces the number density of HLIRGs by 75%. At 1
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Laporte, Nicolas, Kimihiko Nakajima, Richard S. Ellis, Adi Zitrin, Daniel P. Stark, Ramesh Mainali, and G. W. Roberts-Borsani. "A Spectroscopic Search for AGN Activity in the Reionization Era." IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/626417.

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The ubiquity of Lyman alpha (Ly alpha) emission in a sample of four bright [O III]- strong star-forming galaxies with redshifts above seven has led to the suggestion that such luminous sources represent a distinct population compared with their fainter, more numerous counterparts. The presence of Lya emission within the reionization era could indicate that these sources created early ionized bubbles due to their unusually strong radiation, possibly because of the presence of active galactic nuclei. To test this hypothesis, we secured long integration spectra with XSHOOTER on the VLT for three z similar or equal to 7 sources selected to have similar luminosities and prominent excess fluxes in the IRAC 3.6 or 4.5 mu m band, usually attributed to strong [O III] emission. We secured additional spectroscopy for one of these galaxies at z = 7.15 using MOSFIRE at the Keck telescope. For the most well-studied source in our sample with the strongest IRAC excess, we detect significant nebular emission from He II and N V indicative of a non-thermal source. For the other two sources at z = 6.81 and z = 6.85, for which no previous optical/near-infrared spectroscopy was available, Ly alpha is seen in one and C III] emission in the other. Although based on a modest sample, our results further support the hypothesis that the phenomenon of intense [O III] emission is associated preferentially with sources lying in early ionized bubbles. However, even though one of our sources at z = 7.15 suggests the presence of non-thermal radiation, such ionized bubbles may not uniquely arise in this manner. We discuss the unique advantages of extending such challenging diagnostic studies with JWST.
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Books on the topic "AGN galaxies"

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AGN feedback in galaxy formation: Proceedings of the workshop held in Vulcano, Italy, May 18--22, 2008. New York: Cambridge University Press, 2011.

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Sandage, Allan. The age of the galactic disk. Baltimore, MD: Space Telescope Science Institute, 1990.

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Kerschbaum, F. Why galaxies care about AGB stars II: Shining examples and common inhabitants : proceedings of a conference held at University Campus, Vienna, Austria, 16-20 August 2010. Edited by Astronomical Society of the Pacific. San Francisco: Astronomical Society of the Pacific, 2011.

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Multiwavelength AGN Surveys and Studies (IAU S304). Cambridge University Press, 2014.

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(Editor), Stephen S. Holt, Susan G. Neff (Editor), and C. Megan Urry (Editor), eds. Testing the AGN Paradigm (AIP Conference Proceedings). American Institute of Physics, 1998.

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S, Holt Stephen, Neff Susan G, and Urry Claudia Megan, eds. Testing the AGN paradigm: College Park, MD 1991. New York: American Institute of Physics, 1992.

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United States. National Aeronautics and Space Administration., ed. International AGN watch: Continuous monitoring of NGC 4151. [Washington, DC: National Aeronautics and Space Administration, 1995.

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United States. National Aeronautics and Space Administration., ed. Simultaneous X-ray and far-ultraviolet spectra of AGN with ASCA and HUT: Final technical report submitted to NASA for grant NAG5-2935. [Washington, DC: National Aeronautics and Space Administration, 1997.

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United States. National Aeronautics and Space Administration., ed. Simultaneous X-ray and far-ultraviolet spectra of AGN with ASCA and HUT: Final technical report submitted to NASA for grant NAG5-2935. [Washington, DC: National Aeronautics and Space Administration, 1997.

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United States. National Aeronautics and Space Administration., ed. Simultaneous X-ray and far-ultraviolet spectra of AGN with ASCA and HUT: Final technical report submitted to NASA for grant NAG5-2935. [Washington, DC: National Aeronautics and Space Administration, 1997.

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Book chapters on the topic "AGN galaxies"

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García-Burillo, Santiago, Françoise Combes, J. Graciá-Carpio, and A. Usero. "AGN Feeding and AGN Feedback." In Mapping the Galaxy and Nearby Galaxies, 150–55. New York, NY: Springer New York, 2008. http://dx.doi.org/10.1007/978-0-387-72768-4_22.

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González-Delgado, Rosa Maria, and Enrique Pérez. "Star Formation and AGN." In The Nearest Active Galaxies, 127–34. Dordrecht: Springer Netherlands, 1993. http://dx.doi.org/10.1007/978-94-011-1930-6_19.

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Goerdt, A., K. J. Fricke, and W. Kollatschny. "Circumnuclear Populations in Nearby AGN." In The Nearest Active Galaxies, 5–12. Dordrecht: Springer Netherlands, 1993. http://dx.doi.org/10.1007/978-94-011-1930-6_2.

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Veilleux, Sylvain. "The Starburst-AGN Connection." In Starburst Galaxies: Near and Far, 88–94. Berlin, Heidelberg: Springer Berlin Heidelberg, 2001. http://dx.doi.org/10.1007/978-3-642-56538-0_11.

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Terlevich, Roberto. "AGN as Starbursts: modelling the multifrequency spectrum." In Windows on Galaxies, 87–96. Dordrecht: Springer Netherlands, 1990. http://dx.doi.org/10.1007/978-94-009-0543-6_12.

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Frank, J. "Fuelling AGN by Non-Axisymmetric Instabilities." In Dynamics and Interactions of Galaxies, 483–84. Berlin, Heidelberg: Springer Berlin Heidelberg, 1990. http://dx.doi.org/10.1007/978-3-642-75273-5_123.

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Kollatschny, Wolfram, and Alexander Goerdt. "AGN Host Galaxies at Intermediate Redshift." In The Early Universe with the VLT, 400–401. Berlin, Heidelberg: Springer Berlin Heidelberg, 1997. http://dx.doi.org/10.1007/978-3-540-49709-7_57.

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Fried, Josef W., and Jochen Heidt. "Host Galaxies of Radio-Loud AGN." In ESO Astrophysics Symposia, 215–16. Berlin, Heidelberg: Springer Berlin Heidelberg, 1997. http://dx.doi.org/10.1007/978-3-540-69648-3_39.

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Stasinska, Grazyna. "Statistical Studies of AGN and QSOs." In Observational Evidence of Activity in Galaxies, 143–46. Dordrecht: Springer Netherlands, 1987. http://dx.doi.org/10.1007/978-94-009-3851-9_22.

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Chatterjee, Tapan K. "Nuclear Activity in Interacting Galaxies." In Multi-Wavelength Continuum Emission of AGN, 499. Dordrecht: Springer Netherlands, 1994. http://dx.doi.org/10.1007/978-94-010-9537-2_197.

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Conference papers on the topic "AGN galaxies"

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Villforth, Carolin, and Fred Hamann. "Host galaxies of binary AGN." In Nuclei of Seyfert galaxies and QSOs - Central engine & conditions of star formation. Trieste, Italy: Sissa Medialab, 2013. http://dx.doi.org/10.22323/1.169.0077.

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Gerssen, Joris, David Wilman, Lise Christensen, Victor P. Debattista, and C. C. Popescu. "Mapping Star Forming & AGN Galaxies." In HUNTING FOR THE DARK: THE HIDDEN SIDE OF GALAXY FORMATION. AIP, 2010. http://dx.doi.org/10.1063/1.3458498.

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HECKMAN, T. M., and G. KAUFFMANN. "THE HOST GALAXIES OF 23,000 AGN." In Proceedings of the Guillermo Haro Conference 2003. WORLD SCIENTIFIC, 2004. http://dx.doi.org/10.1142/9789812702432_0089.

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Ptak, A. "Low-luminosity AGN and normal galaxies." In X-RAY ASTRONOMY: Stellar Endpoints,AGN, and the Diffuse X-ray Background. AIP, 2001. http://dx.doi.org/10.1063/1.1434645.

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Ozernoy, Leonid. "Probing the monster in luminous starburst galaxies." In Testing the AGN paradigm diagnostics. AIP, 1992. http://dx.doi.org/10.1063/1.42241.

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Penfold, Jack, and Perry E. Radau. "H β and [OIII] velocities in Seyfert galaxies." In Testing the AGN paradigm diagnostics. AIP, 1992. http://dx.doi.org/10.1063/1.42244.

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Andreasian, N. K. "Rotation curves of two galaxies with megamaser radiation." In Testing the AGN paradigm diagnostics. AIP, 1992. http://dx.doi.org/10.1063/1.42251.

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Nieto, J. L., G. Monnet, R. Bacon, E. Emsellem, and E. Pecontal. "Supermassive black holes in the centers of galaxies?" In Testing the AGN paradigm diagnostics. AIP, 1992. http://dx.doi.org/10.1063/1.42253.

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Maisack, M., T. Yaqoob, R. Staubert, and E. Kendziorra. "Constraints on pairs and reflection in active galaxies." In Testing the AGN paradigm diagnostics. AIP, 1992. http://dx.doi.org/10.1063/1.42282.

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De Young, David S., Sebastian Heinz, and Eric Wilcots. "Radio AGN Feedback." In THE MONSTER’S FIERY BREATH: FEEDBACK IN GALAXIES, GROUPS, AND CLUSTERS. AIP, 2009. http://dx.doi.org/10.1063/1.3293049.

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Reports on the topic "AGN galaxies"

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Blanton, Elizabeth L., T. E. Clarke, Craig L. Sarazin, Scott W. Randall, and Brian R. McNamara. AGN Feedback in Clusters of Galaxies. Fort Belvoir, VA: Defense Technical Information Center, January 2010. http://dx.doi.org/10.21236/ada520956.

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Parker, Ashley Marie. An Improved Technique for Increasing the Accuracy of Photometrically Determined Redshifts for ___Blended___ Galaxies. Office of Scientific and Technical Information (OSTI), August 2012. http://dx.doi.org/10.2172/1049741.

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Spacek, Alexander Edward. Comparing Observations to Simulations: An Attempt to Constrain Active Galactic Nucleus Feedback Energy Around Galaxies Using the Sunyaev-Zel'dovich Effect. Office of Scientific and Technical Information (OSTI), January 2018. http://dx.doi.org/10.2172/1418780.

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