luminosity peaks at 90 pc and drops rapidly thereafter, indicating that most
of the kinetic energy is deposited within about 100 pc from the SMBH. Both
values exceed the mass outflow rate and kinetic luminosity determined for the
UV/X-ray absorber outflows in NGC 4151, indicating the importance of NLR
outflows in providing feedback on scales where circumnuclear star formation
and bulge growth occur., archivePrefix = arXiv, arxivId = 1411.4507, author =
Crenshaw, D. Michael and Fischer, Travis C. and Kraemer, Steven B. and
Schmitt, Henrique R., doi = 10.1088/0004-637X/799/1/83, eprint = 1411.4507,
file = :home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Crenshaw et al. - 2015 - Feedback from mass outflows in
nearby active galactic nuclei. II. Outflows in the narrow-line region of NGC
415.pdf:pdf, issn = 15384357, journal = Astrophys. J., keywords = Galaxies:
Seyfert,Galaxies: active,Galaxies: individual (NGC 4151),Galaxies: kinematics
and dynamics, number = 1, pages = 1–6, title = Feedback from mass outflows in
nearby active galactic nuclei. II. Outflows in the narrow-line region of NGC
4151, volume = 799, year = 2015 @articleDuran2016, abstract = Relativistic
jets in active galactic nuclei (AGN) convert as much as half of their energy
into radiation. To explore the poorly understood processes that are
responsible for this conversion, we carry out fully 3D magnetohydrodynamic
(MHD) simulations of relativistic magnetized jets. Unlike the standard
approach of injecting the jets at large radii, our simulated jets self-
consistently form at the source and propagate and accelerate outward for
several orders of magnitude in distance before they interact with the ambient
medium. We find that this interaction can trigger strong energy dissipation of
two kinds inside the jets, depending on the properties of the ambient medium.
Those jets that form in a new outburst and drill a fresh hole through the
ambient medium fall victim to a 3D magnetic kink instability and dissipate
their energy primarily through magnetic reconnection in the current sheets
formed by the instability. On the other hand, those jets that form during
repeated cycles of AGN activity and escape through a pre-existing hole in the
ambient medium maintain their stability and dissipate their energy primarily
at MHD recollimation shocks. In both cases the dissipation region can be
associated with a change in the density profile of the ambient gas. The Bondi
radius in AGN jets serves as such a location., archivePrefix = arXiv, arxivId
= 1612.06929, author = Duran, Rodolfo Barniol and Tchekhovskoy, Alexander and
Giannios, Dimitrios, doi = 10.1093/mnras/stx1165, eprint = 1612.06929, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Duran, Tchekhovskoy, Giannios - 2016 - Three-dimensional
Simulations of AGN Jets Magnetic Kink Instability versus Conical
Shocks.pdf:pdf, keywords = active,galaxies,instabilities,jets,magnetic
fields,mhd, number = June, title = Three-dimensional Simulations of AGN Jets:
Magnetic Kink Instability versus Conical Shocks, url =
http://arxiv.org/abs/1612.06929%0Ahttp://dx.doi.org/10.1093/mnras/stx1165,
volume = 000, year = 2016 @articleCombes2017b, abstract = In the last decade,
observations have accumulated on gas outflows in galaxies, and in particular
massive molecular ones. The mass outflow rate is estimated between 1 and 5
times the star formation rate. For the highest maximal velocities, they are
driven by AGN; these outflows are therefore a clear way to moderate or
suppress star formation. Some of the most convincing examples at low redshift
come from the radio mode, when the radio jets are inclined toward the galaxy
plane, or expand in the hot intra-cluster medium, in cool core clusters.
However, AGN feedback can also be positive in many occasions, and the net
effect is difficult to evaluate. The quenching efficiency is discussed in view
of recent observations., author = Combes, Francoise, doi =
10.3389/fspas.2017.00010, file =
:home/william/Documents/Papers/fspas-04-00010.pdf:pdf, issn = 2296987X,
journal = Front. Astron. Sp. Sci., keywords = active galaxy nuclei,black
holes,galaxies,molecules,outflows, number = September, pages = 1–5, title =
AGN Feedback and Its Quenching Efficiency, volume = 4, year = 2017
@articleZhang2019, abstract = We calculate the spectrum of escaping cosmic
rays (CRs) accelerated in the shocks produced by expanding galactic
superbubbles powered by supernovae producing a continuous energy outflow in
star-forming galaxies. We solve the generalized Kompaneets equations adapted
to expansion in various external density profiles including exponential and
power-law shapes, and take into account that escaping CRs are dominated by
those around their maximum energies. We find that the escaping CR spectrum
largely depends on the specific density profiles and power source properties,
and the results are compared to and constrained by the observed CR spectrum.
As a particular case we apply the results to the Milky Way’s Fermi Bubbles,
and find that the Fermi Bubbles’ CRs in our model could explain the observed
CR flux and spectrum around the second knee at $10^{17}$ eV. At the same time,
our model can also explain the microwave haze observed by ${WMAP}$ and
${Planck}$, as well as the $$ 10 GeV gamma-rays observed by ${Fermi}$-LAT.,
archivePrefix = arXiv, arxivId = 1904.02333, author = Zhang, Zhaowei and
Murase, Kohta and Mészáros, Peter, eprint = 1904.02333, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Zhang, Murase, Mészáros - 2019 - Cosmic Rays Escaping from
Galactic Starburst-Driven Superbubbles and Application to the Fermi
Bubbles.pdf:pdf, keywords = acceleration of particles,astroparticle
physics,bubbles,cosmic rays,fermi bubbles,individual objects,ism,kinematics
and dynamics, number = Kompaneets 1960, pages = 1–16, title = Cosmic Rays
Escaping from Galactic Starburst-Driven Superbubbles and Application to the
Fermi Bubbles, url = http://arxiv.org/abs/1904.02333, year = 2019 @article316,
author = ربه, ابن عبد, file =
:home/william/Documents/Papers/1999ASPC..187..115B.pdf:pdf, pages = 400, title
= No Title العقد الفريد, year = 316 @articleKing2011, abstract = We discuss
massive outflows in galaxy bulges, particularly the ones driven by accretion
episodes where the central supermassive black hole reaches the Eddington
limit. We show that the quasar radiation field Compton-cools the wind shock
until this reaches distances ~1kpc from the black hole, but becomes too dilute
to do this at larger radii. Radiative processes cannot cool the shocked gas
within the flow time at any radius. Outflows are therefore momentum driven at
small radii (as required to explain theM-$\sigma$ relation). At large radii,
they are energy driven, contrary to recent claims. We solve analytically the
motion of an energy-driven shell after the central source has turned off. This
shows that the thermal energy in the shocked wind can drive further expansion
for a time ~10 times longer than the active time of the central source.
Outflows observed at large radii with no active central source probably result
from an earlier short (few Myr) active phase of this source. 2011 The Authors
Monthly Notices of the Royal Astronomical Society 2011 RAS., author = King, A
R and Zubovas, K and Power, C, doi = 10.1111/j.1745-3933.2011.01067.x, file =
:home/william/Documents/Papers/415-1-L6.pdf:pdf, issn = 17453933, journal =
Mon. Not. R. Astron. Soc. Lett., keywords = Accretion,Black hole
physics,Galaxies: evolution,Quasars: general,accretion discs, number = 1,
pages = 6–10, title = Large-scale outflows in galaxies, volume = 415, year =
2011 @articlePadovani2017, abstract = AGN are quite unique astronomical
sources emitting over more than 20 orders of magnitude in frequency, with
different electromagnetic bands providing windows on different sub-structures
and their physics. They come in a large number of flavors only partially
related to intrinsic differences. I highlight here the types of sources
selected in different bands, the relevant selection effects and biases, and
the underlying physical processes. I then look at the “big picture” by
describing the most important parameters one needs to describe the variety of
AGN classes and by discussing AGN at all frequencies in terms of their sky
surface density. I conclude with a look at the most pressing open issues and
the main new facilities, which will flood us with new data to tackle them.,
author = Padovani, Paolo, doi = 10.3389/fspas.2017.00035, file =
:home/william/Documents/Papers/fspas-04-00035.pdf:pdf, issn = 2296987X,
journal = Front. Astron. Sp. Sci., keywords = X-ray emission,active galactic
nuclei,infrared emission,quasars,radio emission,supermassive black
holes,$\gamma$-ray emission, number = November, pages = 1–7, title = Active
Galactic Nuclei at All Wavelengths and from All Angles, volume = 4, year =
2017 @articleScoville2000, abstract = We present near-infrared images obtained
with the Hubble Space Telescope NICMOS camera for a sample of nine luminous
[LIGs: LIR(8-1000 $\mu$m)=1011 Lsolar] and 15 ultraluminous (ULIGS: LIR=1012
Lsolar) infrared galaxies. The sample includes representative systems
classified as warm (f25$\mu$m/f60$\mu$m0.2) and cold (f25$\mu$m/f60$\mu$m=0.2)
based on the mid-infrared colors and systems with nuclear emission lines
classified as H II (i.e., starburst), QSO, Seyfert, and LINER. The
morphologies of the sample galaxies are diverse and provide further support
for the idea that they are created by the collision or interactions of spiral
galaxies. Although no new nuclei are seen in the NICMOS images, the NICMOS
images do reveal new spiral structures, bridges, and circumnuclear star
clusters. The colors and the luminosities of the observed clusters are
consistent with them being young (107-108 yr), formed as a result of galactic
interactions, and having masses much greater than those of Galactic globular
clusters. In NGC 6090 and VV 114, they are preferentially situated along the
area of overlap of the two galactic disks. With the exception of IR
17208-0018, all of the ULIGs have at least one compact (2.2 $\mu$m FWHM=200
pc) nucleus. Analysis of the near-infrared colors (i.e., m1.1-1.6 vs.
m1.6-2.2) derived from 1.1” diameter apertures suggests that the warm galaxies
have near-infrared colors consistent with QSO+hot dust emission and the cold
galaxies, as a group, have near-infrared colors consistent with reddened
starlight. In addition, the cold ULIG UGC 5101 (and possibly three others)
have near-infrared colors suggesting additional active galactic nucleus-like
near-infrared components in their nuclei. In a 2 kpc diameter aperture
measurement, the global colors of all of the cold galaxies except UGC 5101 are
consistent with starlight with a few magnitudes of visual extinction. The
general dichotomy of the near-infrared properties of the warm and the cold
galaxies are further supported by the light distributions: seven of the eight
warm galaxies have unresolved nuclear emission that contributes significantly
(i.e., =30%-40%) to the total near-infrared luminosity. The smooth, more
extended light observed in all of the galaxies is most likely composed of
giant and supergiant stars, but evidence at longer wavelengths suggests that
these stars contribute little to the high 8-1000 $\mu$m luminosity of these
galaxies. Finally, light profiles of nine of the 24 systems were fitted well
by an r1/4 law (and not so well by an exponential disk profile). Whether these
star systems eventually become massive central bulges or giant elliptical
galaxies will depend on how efficiently the present ISM is converted into
stars., author = Scoville, N. Z. and Evans, A. S. and Thompson, R. and Rieke,
M. and Hines, D. C. and Low, F. J. and Dinshaw, N. and Surace, J. A. and
Armus, L., doi = 10.1086/301248, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Coville - 2000 - Nicmos imaging of infrared-luminous
galaxies n. z. s coville.pdf:pdf, issn = 00046256, journal = Astron. J.,
keywords = active è galaxies,galaxies,interactions è galaxies,ism è
galaxies,starburst, number = 3, pages = 991–1061, title = NICMOS Imaging of
Infrared-Luminous Galaxies, volume = 119, year = 2000 @articleVoit2020,
abstract = Star formation in the universe’s most massive galaxies proceeds
furiously early in time but then nearly ceases. Plenty of hot gas remains
available but does not cool and condense into star-forming clouds. Active
galactic nuclei (AGN) release enough energy to inhibit cooling of the hot gas,
but energetic arguments alone do not explain why quenching of star formation
is most effective in high-mass galaxies. In fact, optical observations show
that quenching is more closely related to a galaxy’s central stellar velocity
dispersion ($_v$) than to any other characteristic. Here, we show that high
$_v$ is critical to quenching because a deep central potential well maximizes
the efficacy of AGN feedback. In order to remain quenched, a galaxy must
continually sweep out the gas ejected from its aging stars. Supernova heating
can accomplish this task as long as the AGN sufficiently reduces the gas
pressure of the surrounding circumgalactic medium (CGM). We find that CGM
pressure acts as the control knob on a valve that regulates AGN feedback and
suggest that feedback power self-adjusts so that it suffices to lift the CGM
out of the galaxy’s potential well. Supernova heating then drives a galactic
outflow that remains homogeneous if $_v 240 \, {km \, s^{-1}}$. AGN feedback
can effectively quench galaxies with a comparable velocity dispersion, but
feedback in galaxies with a much lower velocity dispersion tends to result in
convective circulation and accumulation of multiphase gas within the galaxy.,
archivePrefix = arXiv, arxivId = 2006.09381, author = Voit, G. M. and Bryan,
G. L. and Prasad, D. and Frisbie, R. and Li, Y. and Donahue, M. and O’Shea, B.
W. and Sun, M. and Werner, N., eprint = 2006.09381, file =
:home/william/Documents/Papers/2006.09381.pdf:pdf, keywords =
galaxies,halos,intergalactic medium,ism, title = A Black-Hole Feedback Valve
in Massive Galaxies, url = http://arxiv.org/abs/2006.09381, year = 2020
@articleZubovas2017, author = Zubovas, Kastytis, doi =
10.1038/s41550-017-0093, file =
:home/william/Documents/Papers/zubovas2017.pdf:pdf, issn = 23973366, journal =
Nat. Astron., number = April, pages = 1–2, publisher = Macmillan Publishers
Limited, title = Galaxy evolution: Let there be stars, url =
http://dx.doi.org/10.1038/s41550-017-0093, volume = 1, year = 2017
@articleTadhunter2014a, abstract = Massive outflows driven by active galactic
nuclei are widely recognized to have a key role in the evolution of galaxies,
by heating the ambient gas, expelling it from the nuclear regions, and thereby
affecting the star-formation histories of the galaxy bulges. It has been
proposed that the powerful jets of relativistic particles (such as electrons)
launched by some active nuclei can both accelerate and heat the molecular gas,
which often dominates the mass budgets of the outflows. Clear evidence for
this mechanism, in the form of detailed associations between the molecular gas
kinematics and features in the radio-emitting jets, has however been lacking.
Here we report that the warm molecular hydrogen gas in the western radio lobe
of the Seyfert galaxy IC 5063 is moving at high velocities-up to about 600
kilometres per second-relative to the galaxy disk. This suggests that the
molecules have been accelerated by fast shocks driven into the interstellar
medium by the expanding radio jets. These results demonstrate the general
feasibility of accelerating molecular outflows in fast shocks driven by active
nuclei., archivePrefix = arXiv, arxivId = 1407.1332, author = Tadhunter, C.
and Morganti, R. and Rose, M. and Oonk, J. B.R. and Oosterloo, T., doi =
10.1038/nature13520, eprint = 1407.1332, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Tadhunter et al. - 2014 - Jet acceleration of the fast
molecular outflows in the Seyfert galaxy IC 5063.pdf:pdf, isbn = 0028-0836,
issn = 14764687, journal = Nature, number = 7510, pages = 440–443, pmid =
25043049, publisher = Nature Publishing Group, title = Jet acceleration of the
fast molecular outflows in the Seyfert galaxy IC 5063, url =
http://dx.doi.org/10.1038/nature13520, volume = 511, year = 2014
@articleLamastra2019, abstract = Several observations are revealing the
widespread occurrence of mildly relativistic wide-angle AGN winds strongly
interacting with the gas of their host galaxy. Such winds are potential
cosmic-ray accelerators, as supported by gamma-ray observations of the nearby
Seyfert galaxy NGC 1068 with the Fermi gamma-ray space telescope. The non-
thermal emission produced by relativistic particles accelerated by the AGN-
driven wind observed in the circum-nuclear molecular disk of such galaxy is
invoked to produce the gamma-ray spectrum. The AGN wind model predicts a hard
spectrum that extend in the very high energy band which differs significantly
from those corresponding to other models discussed in the literature, like
starburst or AGN jet. We present dedicated simulations of observations through
the Cherenkov Telescope Array (CTA), the next-generation ground based gamma-
ray observatory, of the very high energy spectrum of the Seyfert galaxy NGC
1068 assuming the AGN wind and the AGN jet models. We demonstrate that,
considering 50 hours of observations, CTA can be effectively used to constrain
the two different emission models, providing important insight into the
physics governing the acceleration of particles in non-relativistic AGN-driven
outflows. This analysis strongly motivates observations of Seyfert and
starburst galaxies with CTA in order to test source population models of the
extragalactic gamma-ray and neutrino backgrounds., archivePrefix = arXiv,
arxivId = 1904.06918, author = Lamastra, Alessandra and Tavecchio, Fabrizio
and Romano, Patrizia and Landoni, Marco and Vercellone, Stefano, doi =
10.1016/j.astropartphys.2019.04.003, eprint = 1904.06918, file =
:home/william/Documents/Papers/1-s2.0-S0927650519300362-main.pdf:pdf, issn =
09276505, journal = Astropart. Phys., keywords = Galaxies,Gamma
rays,Individual,NGC 1068,Seyfert, pages = 16–23, publisher = Elsevier B.V.,
title = Unveiling the origin of the gamma-ray emission in NGC 1068 with the
Cherenkov Telescope Array, url =
https://doi.org/10.1016/j.astropartphys.2019.04.003, volume = 112, year = 2019
@articleAsahina2017a, abstract = 2017. The American Astronomical Society. All
rights reserved. By performing three-dimensional magnetohydrodynamics
simulations of subrelativistic jets and disk winds propagating into the
magnetized inhomogeneous interstellar medium (ISM), we investigate the
magnetic effects on the active galactic nucleus feedback. Our simulations
reveal that the magnetic tension force promotes the acceleration of the dense
gas clouds, since the magnetic field lines, which are initially straight, bend
around the gas clouds. In the jet models, the velocity dispersion of the
clouds increases with an increase in the initial magnetic fields. The
increment of the kinetic energy of the clouds is proportional to the initial
magnetic fields, implying that the magnetic tension force increases the energy
conversion efficiency from the jet to the gas clouds. Through simulations of
the mildly collimated disk wind and the funnel-shaped disk wind, we confirm
that such an enhancement of the energy conversion efficiency via the magnetic
fields appears even if the energy is injected via the disk winds. The
enhancement of the acceleration of the dense part of the magnetized ISM via
the magnetic tension force will occur wherever the magnetized inhomogeneous
matter is blown away., author = Asahina, Yuta and Nomura, Mariko and Ohsuga,
Ken, doi = 10.3847/1538-4357/aa6c5f, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Asahina, Nomura, Ohsuga - 2017 - Enhancement of Feedback
Efficiency by Active Galactic Nucleus Outflows via the Magnetic Tension Force
i.pdf:pdf, issn = 1538-4357, journal = Astrophys. J., keywords = ISM:
clouds,ISM: jets and outflows,magnetohydrodyn,clouds,ism,jets and out
fl,magnetohydrodynamics,mhd,ows,shock waves, number = 1, pages = 25, publisher
= IOP Publishing, title = Enhancement of Feedback Efficiency by Active
Galactic Nucleus Outflows via the Magnetic Tension Force in the Inhomogeneous
Interstellar Medium, url = http://dx.doi.org/10.3847/1538-4357/aa6c5f, volume
= 840, year = 2017 @articleBanda-Barragan2018, abstract = We present a set of
numerical experiments designed to systematically investigate how turbulence
and magnetic fields influence the morphology, energetics, and dynamics of
filaments produced in wind-cloud interactions. We cover 3D,
magnetohydrodynamic systems of supersonic winds impacting clouds with
turbulent density, velocity, and magnetic fields. We find that lognormal
density distributions aid shock propagation through clouds, increasing their
velocity dispersion and producing filaments with expanded cross-sections and
highly magnetized knots and subfilaments. In self-consistently turbulent
scenarios, the ratio of filament to initial cloud magnetic energy densities is
~1. The effect of Gaussian velocity fields is bound to the turbulence Mach
number: Supersonic velocities trigger a rapid cloud expansion; subsonic
velocities only have a minor impact. The role of turbulent magnetic fields
depends on their tension and is similar to the effect of radiative losses: the
stronger the magnetic field or the softer the gas equation of state, the
greater the magnetic shielding at wind-filament interfaces and the suppression
of Kelvin-Helmholtz instabilities. Overall, we show that including turbulence
and magnetic fields is crucial to understanding cold gas entrainment in
multiphase winds. While cloud porosity and supersonic turbulence enhance the
acceleration of clouds, magnetic shielding protects them from ablation and
causes Rayleigh-Taylor-driven subfilamentation. Wind-swept clouds in turbulent
models reach distances ~15-20 times their core radius and acquire bulk speeds
~0.3-0.4 of the wind speed in one cloud-crushing time, which are three times
larger than in non-turbulent models. In all simulations, the ratio of
turbulent magnetic to kinetic energy densities asymptotes at ~0.1-0.4, and
convergence of all relevant dynamical properties requires at least 64 cells
per cloud radius., archivePrefix = arXiv, arxivId = 1706.06607, author =
Banda-Barragán, W. E. and Federrath, C. and Crocker, R. M. and Bicknell, G.
V., doi = 10.1093/mnras/stx2541, eprint = 1706.06607, file =
:home/william/Documents/Papers/stx2541.pdf:pdf, issn = 13652966, journal =
Mon. Not. R. Astron. Soc., keywords = Galaxies: starburst,ISM: clouds,ISM:
magnetic fields,MHD,Methods: numerical,Turbulence, number = 3, pages =
3454–3489, title = Filament formation in wind-cloud interactions- II. Clouds
with turbulent density, velocity, and magnetic fields, volume = 473, year =
2018 @articleMelioli2006, abstract = Recent observational studies of the age
distribution of star clusters in nearby merging galaxies and starburst (SB)
galaxies indicate a premature death of the young clusters. The fate of an
evolving star cluster crucially depends of its gas content. This behaves like
a glue that helps to keep the star system gravitationally bound. In SB systems
where the rate of supemovae (SNe) explosions is elevated one should expect an
efficient heating of the gas and its complete removal which could then favor
the rapid dissociation of the evolving star clusters. Based on a
contemporaneous study of the dynamical evolution of the interstellar gas in SB
environments (Melioli & de Gouveia Dal Pino 2004, A&A, 424, 817) where it has
been considered also the presence of dense clouds that may inhibit the heating
efficiency of the interstellar gas by the SNe, we have here computed the
timescales for gas removal from young clusters embedded in these systems and
found that they are consistent with the very short timescales for cluster
dissolution which are inferred from the observational studies above. Our
results indicate that typical SB proto-clusters should start to disperse after
less than 5 Myr. For a given total gas mass content, this result is nearly
insensitive to the initial star formation efficiency. ESO 2006., archivePrefix
= arXiv, arxivId = astro-ph/0511663, author = Melioli, C. and De Gouveia Dal
Pino, E. M., doi = 10.1051/0004-6361:200500218, eprint = 0511663, file =
:home/william/Documents/Papers/0511663.pdf:pdf, issn = 14320746, journal =
Astron. Astrophys., keywords = Stellar cluster: ISM, SNc,Stellar clusters:
general, number = 3, primaryClass = astro-ph, title = ISM gas removal from
starburst galaxies and the premature death of star clusters, volume = 445,
year = 2006 @ARTICLEMorganti2013, author = Morganti, R. and Frieswijk, W. and
Oonk, R. J. B. and Oosterloo, T. and Tadhunter, C., title = ”Tracing the
extreme interplay between radio jets and the ISM in IC 5063”, journal = ,
keywords = galaxies: active, galaxies: individual: IC 5063, ISM: jets and
outflows, radio lines: galaxies, Astrophysics - Cosmology and Nongalactic
Astrophysics, year = 2013, month = apr, volume = 552, eid = L4, pages = L4,
doi = 10.1051/0004-6361/201220734, archivePrefix = arXiv, eprint = 1302.2236,
primaryClass = astro-ph.CO, adsurl =
https://ui.adsabs.harvard.edu/abs/2013A&A…552L…4M, adsnote = Provided by the
SAO/NASA Astrophysics Data System

@articleHarrison2017, abstract = Supermassive black holes are found at the
centres of massive galaxies. During the growth of these black holes they light
up to become visible as active galactic nuclei (AGNs) and release
extraordinary amounts of energy across the electromagnetic spectrum. This
energy is widely believed to regulate the rate of star formation in the black
holes’ host galaxies via so-called AGN feedback. However, the details of how
and when this occurs remain uncertain from both an observational and
theoretical perspective. I review some of the theoretical motivation and
observational results and discuss possible observational signatures of the
impact of supermassive black hole growth on star formation., archivePrefix =
arXiv, arxivId = 1703.06889, author = Harrison, C. M., doi =
10.1038/s41550-017-0165, eprint = 1703.06889, file =
:home/william/Documents/Papers/harrison2017.pdf:pdf, issn = 23973366, journal
= Nat. Astron., number = July, pages = 1–8, publisher = Macmillan Publishers
Limited, title = Impact of supermassive black hole growth on star formation,
url = http://dx.doi.org/10.1038/s41550-017-0165, volume = 1, year = 2017
@articleOSullivan2007, abstract = Preliminary VLBA polarisation results on 6
“blazars” from 6.5-cm to 7-mm are presented here. Observing at several
different wavelengths, separated by short and long intervals, enabled reliable
information about the magnetic (B) field structure to be obtained and for the
effect of Faraday Rotation to be determined and corrected. For all sources the
magnitude of the core Rotation Measure (RM) derived from the shorter
wavelength data was greater than that derived from the longer wavelength data,
consistent with a higher electron density and/or B-field strength closer to
the central engine. A transverse RM gradient was detected in the jet of
0954+658, providing evidence for the presence of a helical B-field surrounding
the jet. The RM in the core region of 2200+420 (BL Lac) displays sign changes
in different wavelength intervals (on different spatial scales); we suggest an
explanation for this in terms of modest bends in a helical B-field surrounding
the jet., archivePrefix = arXiv, arxivId = 0710.0128, author = O’Sullivan,
Shane P. and Gabuzda, Denise C, eprint = 0710.0128, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/O’Sullivan, Gabuzda - 2007 - Investigation of the Faraday
Rotation Measure and Magnetic Field Structures of Several AGN Jets on Sub-
Pars.pdf:pdf, journal = Astron. Soc. Pacific Conf. Ser., number = July 2006,
pages = 5, title = Investigation of the Faraday Rotation Measure and Magnetic
Field Structures of Several AGN Jets on Sub-Parsec to Parsec Scales, url =
http://arxiv.org/abs/0710.0128, volume = 386, year = 2007 @articleDobler2012,
abstract = The microwave ”haze” was first discovered with the initial release
of the full sky data from the Wilkinson Microwave Anisotropy Probe. It is
diffuse emission towards the center of our Galaxy with spectral behavior that
makes it difficult to categorize as any of the previously known emission
mechanisms at those wavelengths. With now seven years of WMAP data publicly
available, we have learned much about the nature of the haze, and with the
release of data from the Fermi Gamma-Ray Space Telescope and the discovery of
the gamma-ray haze/bubbles, we have had a spectacular confirmation of its
existence at other wavelengths. As the WMAP mission winds down and the Planck
mission prepares to release data, I take a last look at what WMAP has to tell
us about the origin of this unique Galactic feature. Much like the gamma-rays,
the microwave haze/bubbles is elongated in latitude with respect to longitude
by a factor of roughly two, and at high latitudes, the microwave emission cuts
off sharply above ~35 degrees (compared to ~50 degrees in the gammas). The
hard spectrum of electrons required to generate the microwave synchrotron is
consistent with that required to generate the gamma-ray emission via inverse
Compton scattering, though it is likely that these signals result from
distinct regions of the spectrum (~10 GeV for the microwaves, ~1 TeV for the
gammas). While there is no evidence for significant haze polarization in the
7-year WMAP data, I demonstrate explicitly that it is unlikely such a signal
would be detectable above the noise., author = Dobler, Gregory, doi =
10.1088/0004-637X/750/1/17, file = :home/william/.local/share/data/Mendeley
Ltd./Mendeley Desktop/Downloaded/Dobler - 2012 - A last look at the microwave
hazebubbles with WMAP.pdf:pdf, issn = 15384357, journal = Astrophys. J.,
keywords = Galaxy: center,ISM: bubbles,ISM: structure,radio continuum: ISM,
number = 1, title = A last look at the microwave haze/bubbles with WMAP,
volume = 750, year = 2012

@articleRiffel2021a, abstract = The near-infrared spectra of active galactic
nuclei (AGN) present emission lines of different atomic and molecular species.
The mechanisms involved in the origin of these emission lines in AGN are still
not fully understood. We use J- and K-band integral field spectra of six
luminous ($43.1L_{bol}/({erg\, s^{-1}})44.4$) Seyfert galaxies (NGC 788, Mrk
607, NGC 3227, NGC 3516, NGC 5506, and NGC 5899) in the local Universe (0.0039
z 0.0136) to investigate the gas excitation within the inner 100–300 pc radius
of the galaxies at spatial resolutions of a few tens of parsecs. In all
galaxies, the H2 emission originates from thermal processes with excitation
temperatures in the range 2400–5200 K. In the high-line ratio (HLR) region of
the H2/Br$\gamma$ versus [Fe ii]/Pa$\beta$ diagnostic diagram, which includes
29 per cent of the spaxels, shocks are the main excitation mechanism, as
indicated by the correlation between the line widths and line ratios. In the
AGN region of the diagram (64 per cent of the spaxels) the H2 emission is due
to the AGN radiation. The [Fe ii] emission is produced by a combination of
photoionization by the AGN radiation and shocks in five galaxies and is
dominated by photoionization in NGC 788. The [S ix]1.2523 $\mu$m coronal
emission line is present in all galaxies, and its flux distributions are
extended from 80 to 185 pc from the galaxy nuclei, except for NGC 5899, in
which this line is detected only in the integrated spectrum., archivePrefix =
arXiv, arxivId = 2103.08736, author = Riffel, Rogemar A and Bianchin, Marina
and Riffel, Rogério and Storchi-Bergmann, Thaisa and Schönell, Astor J and
Dahmer-Hahn, Luis Gabriel and Dametto, Natacha Z and Diniz, Marlon R, doi =
10.1093/mnras/stab788, eprint = 2103.08736, file =
:home/william/Documents/Papers/2111.09130.pdf:pdf, issn = 0035-8711, journal =
Mon. Not. R. Astron. Soc., keywords =
active,galaxies,kinematics,nuclei,seyfert, number = 4, pages = 5161–5178,
title = Gemini NIFS survey of feeding and feedback in nearby active galaxies –
IV. Excitation, volume = 503, year = 2021 @article2005A&A…439..521M, author =
Morganti, R and Oosterloo, T.~A. and Tadhunter, C.~N. and van Moorsel, G and
Emonts, B, doi = 10.1051/0004-6361:20053175, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Morganti et al. - 2005 - The location of the broad H i
absorption in 3C 305 clear evidence for a jet-accelerated neutral
outflow.pdf:pdf, journal = aap, keywords = galaxies: ISM,galaxies:
active,galaxies: individual: 3C 305, pages = 521–526, title = The location of
the broad H i absorption in 3C 305: clear evidence for a jet-accelerated
neutral outflow, volume = 439, year = 2005 @articleSchawinski2006, abstract =
Detailed high-resolution observations of the innermost regions of nearby
galaxies have revealed the presence of supermassive black holes. These black
holes may interact with their host galaxies by means of ’feedback’ in the form
of energy and material jets; this feedback affects the evolution of the host
and gives rise to observed relations between the black hole and the host. Here
we report observations of the ultraviolet emissions of massive early-type
galaxies. We derive an empirical relation for a critical black-hole mass (as a
function of velocity dispersion) above which the outflows from these black
holes suppress star formation in their hosts by heating and expelling all
available cold gas. Supermassive black holes are negligible in mass compared
to their hosts but nevertheless seem to play a critical role in the star
formation history of galaxies. 2006 Nature Publishing Group., author =
Schawinski, Kevin and Khochfar, Sadegh and Kaviraj, Sugata and Yi, Sukyoung K.
and Boselli, Alessandro and Barlow, Tom and Conrow, Tim and Forster, Karl and
Friedman, Peter G. and Martin, D. Chris and Morrissey, Patrick and Neff, Susan
and Schiminovich, David and Seibert, Mark and Small, Todd and Wyder, Ted K.
and Bianchi, Luciana and Donas, Jose and Heckman, Tim and Lee, Young Wook and
Madore, Barry and Milliard, Bruno and Rich, R. Michael and Szalay, Alex, doi =
10.1038/nature04934, file =
:home/william/Documents/Papers/schawinski2006.pdf:pdf, issn = 14764687,
journal = Nature, number = 7105, pages = 888–891, title = Suppression of star
formation in early-type galaxies by feedback from supermassive black holes,
volume = 442, year = 2006 @articleEso, author = Ésò, Î È Ôgß Î Ëørî and Ìqò, Ø
Ð Ùiï Î and Êaí, È É Ñ Êzêaè Õ and Ì, Ò Ú Ê Ì Ò Ø Ò Í Êùaü Í Î Ëqùaí Ò Ü Ô and
Êaögêaé, Ø and Íiâ, Î and Ö, Ë S Î È Ï Ð È Ïq Ë S Ò Ø Úfëð Ø Î Ë Ð Í and Ùaí,
Ð È Ésësî È Ì Í Ü Ùêaè É and Ì, Ò Ü Ô, file =
:home/william/Documents/Papers/1999pcim.conf…77E.pdf:pdf, title = ÙA f e ¥ z ¢
 s  @articleBlandford2001, abstract = Recent developments in the
spectropolarimetric study of compact objects, specifically black holes
(stellar and massive) and neutron stars are reviewed. The lectures are
organized around five topics: disks, jets, outflows, neutron stars and black
holes. They emphasize physical mechanisms and are intended to bridge the gap
between the fundamentals of polarimetry and the phenomenology of observed
cosmic sources of polarized radiation, as covered by the other lecturers.
There has been considerable recent progress in spectropolarimetry from radio
through optical frequencies and this is producing some unique diagnostics of
the physical conditions around compact objects. It is argued that there is a
great need to develop a correspondingly sensitive polarimetric capability at
ultraviolet through gamma-ray energies., archivePrefix = arXiv, arxivId =
astro-ph/0107228, author = Blandford, Roger and Agol, Eric and Broderick,
Avery and Heyl, Jeremy and Koopmans, Leon and Lee, Hee-Won, eprint = 0107228,
file = :home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Blandford et al. - 2001 - Compact Objects and Accretion
Disks.pdf:pdf, primaryClass = astro-ph, title = Compact Objects and Accretion
Disks, url = http://arxiv.org/abs/astro-ph/0107228, year = 2001
@articleField1965, author = Field, George B and Field, George B, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Field, Field - 1965 - THERMAL INSTABILITY George B. Field
Princeton University Observatory Received June 4, 1964 revised March 30,
1965.pdf:pdf, journal = Astrophys. J., pages = 531–567, title = THERMAL
INSTABILITY George B. Field Princeton University Observatory Received June 4,
1964; revised March 30, 1965, year = 1965 @articleTeng2009, abstract = We
report the results from our analysis of Suzaku X-ray Imaging Spectrometer
(XIS) (0.5-10 keV) and Hard X-ray Detector (HXD)/PIN (15-40 keV) observations
of five well-known local ultraluminous infrared galaxies: IRAS F05189-2524,
IRAS F08572 + 3915, Mrk 273, PKS 1345 + 12, and Arp 220. The XIS observations
of F05189-2524 and Mrk 273 reveal strong iron lines consistent with Fe
K$\alpha$ and changes in spectral shapes with respect to previous Chandra and
XMM-Newton observations. Mrk 273 is also detected by the HXD/PIN at ∼
1.8$\sigma$. For F05189-2524, modeling of the data from the different epochs
suggests that the change in spectral shape is likely due to the central source
switching off, leaving behind a residual reflection spectrum, or an increase
in the absorbing column. An increase in the covering fraction of the absorber
can describe the spectral variations seen in Mrk 273, although a reduction in
the intrinsic active galactic nucleus (AGN) luminosity cannot be formally
ruled out. The Suzaku spectra of Mrk 273 are well fitted by a ∼ 94% covering
fraction model with a column density of ∼ 1024 cm-2. The absorption-corrected
log[L 2-10keV/L IR] ratio is consistent with those found in PG Quasars. The
0.5-10 keV spectrum of PKS 1345 + 12 and Arp 220 seem unchanged from previous
observations and their hard X-ray emission is not convincingly detected by the
HXD/PIN. The large column density derived from CO observations and the large
equivalent width of an ionized Fe line in Arp 220 can be reconciled by an
ionized reflection model. F08572 + 3915 is undetected in both the XIS and
HXD/PIN, but the analysis of unpublished Chandra data provides a new
measurement at low energies. 2009. The American Astronomical Society. All
rights reserved., archivePrefix = arXiv, arxivId = 0809.2090, author = Teng,
Stacy H. and Veilleux, Sylvain and Anabuki, Naohisa and Dermer, Charles D. and
Gallo, Luigi C. and Nakagawa, Takao and Reynolds, Christopher S. and Sanders,
D. B. and Terashima, Yuichi and Wilson, Andrew S., doi =
10.1088/0004-637X/691/1/261, eprint = 0809.2090, file =
:home/william/Documents/Papers/Teng_2009_ApJ_691_261.pdf:pdf, issn = 15384357,
journal = Astrophys. J., keywords = X-rays: galaxies,galaxies:
active,galaxies: individual (IRAS F05189,galaxies: starburst, number = 1,
pages = 261–276, title = Suzaku observations of local ultraluminous infrared
galaxies, volume = 691, year = 2009 @articleTesileanu2008a, abstract =
Context. Time-dependent cooling processes are of paramount importance in the
evolution of astrophysical gaseous nebulae and, in particular, when radiative
shocks are present. Given the recent improvements in resolution of the
observational data, simulating these processes in a more realistic manner in
magnetohydrodynamic (MHD) codes will provide a unique tool for model
discrimination.Aims. The present work introduces a necessary set of tools that
can be used to model radiative astrophysical flows in the optically-thin
plasma limit. We aim to provide reliable and accurate predictions of emission
line ratios and radiative cooling losses in astrophysical simulations of
shocked flows. Moreover, we discuss numerical implementation aspects to ease
future improvements and implementation in other MHD numerical codes.Methods.
The most important source of radiative cooling for our plasma conditions comes
from the collisionally-excited line radiation. We evolve a chemical network,
including 29 ion species, to compute the ionization balance in non-equilibrium
conditions. The numerical methods are implemented in the PLUTO code for
astrophysical fluid dynamics and particular attention has been devoted to
resolve accuracy and efficiency issues arising from cooling timescales
considerably shorter than the dynamical ones.Results. After a series of
validations and tests, typical astrophysical setups are simulated in 1D and
2D, employing both the present cooling model and a simplified one. The
influence of the cooling model on structure morphologies can become important,
especially for emission line diagnostic purposes.Conclusions. The tests make
us confident that the use of the presented detailed radiative cooling
treatment will allow more accurate predictions in terms of emission line
intensities and shock dynamics in various astrophysical setups. 2008 ESO.,
archivePrefix = arXiv, arxivId = 0807.3657, author = Teşileanu, O. and
Mignone, A. and Massaglia, S., doi = 10.1051/0004-6361:200809461, eprint =
0807.3657, file = :home/william/Documents/Papers/0807.3657.pdf:pdf, issn =
00046361, journal = Astron. Astrophys., keywords = ISM: Herbig-Haro
objects,ISM: jets and outflows,Line: formation,Magnetohydrodynamics
(MHD),Methods: numerical,Radiation mechanisms: thermal, number = 1, pages =
429–440, title = Simulating radiative astrophysical flows with the PLUTO code:
A non-equilibrium, multi-species cooling function, volume = 488, year = 2008
@articleAckermann2014, abstract = The Fermi bubbles are two large structures
in the gamma-ray sky extending to 55° above and below the Galactic center. We
analyze 50 months of Fermi Large Area Telescope data between 100 MeV and 500
GeV above 10° in Galactic latitude to derive the spectrum and morphology of
the Fermi bubbles. We thoroughly explore the systematic uncertainties that
arise when modeling the Galactic diffuse emission through two separate
approaches. The gamma-ray spectrum is well described by either a log parabola
or a power law with an exponential cutoff. We exclude a simple power law with
more than 7$\sigma$ significance. The power law with an exponential cutoff has
an index of 1.9 ± 0.2 and a cutoff energy of 110 ± 50 GeV. We find that the
gamma-ray luminosity of the bubbles is erg s-1. We confirm a significant
enhancement of gamma-ray emission in the southeastern part of the bubbles, but
we do not find significant evidence for a jet. No significant variation of the
spectrum across the bubbles is detected. The width of the boundary of the
bubbles is estimated to be deg. Both inverse Compton (IC) models and hadronic
models including IC emission from secondary leptons fit the gamma-ray data
well. In the IC scenario, synchrotron emission from the same population of
electrons can also explain the WMAP and Planck microwave haze with a magnetic
field between 5 and 20 $\mu$G., author = Ackermann, M. and Albert, A. and
Atwood, W. B. and Baldini, L. and Ballet, J. and Barbiellini, G. and Bastieri,
D. and Bellazzini, R. and Bissaldi, E. and Blandford, R. D. and Bloom, E. D.
and Bottacini, E. and Brandt, T. J. and Bregeon, J. and Bruel, P. and Buehler,
R. and Buson, S. and Caliandro, G. A. and Cameron, R. A. and Caragiulo, M. and
Caraveo, P. A. and Cavazzuti, E. and Cecchi, C. and Charles, E. and Chekhtman,
A. and Chiang, J. and Chiaro, G. and Ciprini, S. and Claus, R. and Cohen-
Tanugi, J. and Conrad, J. and Cutini, S. and D’Ammando, F. and De Angelis, A.
and De Palma, F. and Dermer, C. D. and Digel, S. W. and Di Venere, L. and Do
Couto E Silva, E. and Drell, P. S. and Favuzzi, C. and Ferrara, E. C. and
Focke, W. B. and Franckowiak, A. and Fukazawa, Y. and Funk, S. and Fusco, P.
and Gargano, F. and Gasparrini, D. and Germani, S. and Giglietto, N. and
Giordano, F. and Giroletti, M. and Godfrey, G. and Gomez-Vargas, G. A. and
Grenier, I. A. and Guiriec, S. and Hadasch, D. and Harding, A. K. and Hays, E.
and Hewitt, J. W. and Hou, X. and Jogler, T. and Jóhannesson, G. and Johnson,
A. S. and Johnson, W. N. and Kamae, T. and Kataoka, J. and Knödlseder, J. and
Kocevski, D. and Kuss, M. and Larsson, S. and Latronico, L. and Longo, F. and
Loparco, F. and Lovellette, M. N. and Lubrano, P. and Malyshev, D. and
Manfreda, A. and Massaro, F. and Mayer, M. and Mazziotta, M. N. and McEnery,
J. E. and Michelson, P. F. and Mitthumsiri, W. and Mizuno, T. and Monzani, M.
E. and Morselli, A. and Moskalenko, I. V. and Murgia, S. and Nemmen, R. and
Nuss, E. and Ohsugi, T. and Omodei, N. and Orienti, M. and Orlando, E. and
Ormes, J. F. and Paneque, D. and Panetta, J. H., doi =
10.1088/0004-637X/793/1/64, file = :home/william/.local/share/data/Mendeley
Ltd./Mendeley Desktop/Downloaded/Ackermann et al. - 2014 - The spectrum and
morphology of the Fermi bubbles.pdf:pdf, issn = 15384357, journal = Astrophys.
J., keywords = Galaxy: general,Galaxy: halo,astroparticle physics,cosmic
rays,gamma rays: diffuse background,methods: data analysis, number = 1, title
= The spectrum and morphology of the Fermi bubbles, volume = 793, year = 2014
@articleCombes2009, author = Combes, F., doi = 10.1051/0004-6361/200912152,
file = :home/william/Documents/Papers/[Combes]-Commentary on Tully and Fisher
1977 paper.pdf:pdf, issn = 00046361, journal = Astron. Astrophys., number = 1,
pages = 119–120, title = From distances to galaxy evolution and the dark
matter problem, volume = 500, year = 2009 @articleSymeonidis2021, abstract =
We investigate the balance of power between stars and AGN across cosmic
history, based on the comparison between the infrared (IR) galaxy luminosity
function (LF) and the IR AGN LF. The former corresponds to emission from dust
heated by stars and AGN, whereas the latter includes emission from AGN-heated
dust only. We find that at all redshifts (at least up to z ∼ 2.5), the high-
luminosity tails of the two LFs converge, indicating that the most IR-luminous
galaxies are AGN-powered. Our results shed light to the decades-old conundrum
regarding the flatter high-luminosity slope seen in the IR galaxy LF compared
to that in the UV and optical. We attribute this difference to the increasing
fraction of AGN-dominated galaxies with increasing total IR luminosity (LIR).
We partition the LIR−z parameter space into a star formation-dominated and an
AGN-dominated region, finding that the most luminous galaxies at all epochs
lie in the AGN-dominated region. This sets a potential ‘limit’ to attainable
star formation rates, casting doubt on the abundance of ‘extreme starbursts’:
if AGN did not exist, LIR 1013 L⊙ galaxies would be significantly rarer than
they currently are in our observable Universe. We also find that AGN affect
the average dust temperatures (Tdust) of galaxies and hence the shape of the
well-known LIR−Tdust relation. We propose that the reason why local ULIRGs are
hotter than their high-redshift counterparts is because of a higher fraction
of AGN-dominated galaxies amongst the former group., archivePrefix = arXiv,
arxivId = 2102.11936, author = Symeonidis, M and Page, M J, doi =
10.1093/mnras/stab598, eprint = 2102.11936, file =
:home/william/Documents/Papers/2102.11936.pdf:pdf, issn = 0035-8711, journal =
Mon. Not. R. Astron. Soc., number = 3, pages = 3992–4007, title = AGN and star
formation across cosmic time, volume = 503, year = 2021 @articleTadhunter2008,
abstract = In the light of recent speculation that AGN have a major impact on
the evolution of their host galaxies, I review the observational evidence for
energetic outflows around AGN, concentrating in particular on the spatially
resolved outflows around radioloud AGN. There is now substantial evidence that
the large-scale radio jets have a major impact on the evolution of the hot and
warm ISM in the surround galaxy haloes and clusters on a ˜5 - 500 kpc scale.
However, although clear evidence for warm and cool outflows has also been
found on the smaller (5 kpc) scale of the NLR, these outflows are in general
much less energetic than those driven by the radio jets on a larger scale.
Indeed, the warm outflows detected in the NLR using both optical emission
lines and narrow UV absorption line are generally less massive and energetic
than those driven by extreme starbursts in ULIRGs. Apart from the radio jets,
the only AGN-induced outflows that come close to matching the requirements of
the galaxy evolution feedback models are those detected using the blueshifted
X-ray absorption edge features., author = Tadhunter, Clive, file =
:home/william/Documents/Papers/2008MmSAI..79.1205T.pdf:pdf, journal = Mem
SAIt, keywords = active,evolution,galaxies, pages = 1205–1212, title = The
importance of sub-relativistic outflows in AGN host galaxies, url =
http://sait.oat.ts.astro.it/MmSAI/79/PDF/1205.pdf, volume = 79, year = 2008
@articleIwasawa2017, abstract = We present an X-ray study of the ultra-
luminous infrared galaxy IRAS F00183-7111 (z = 0:327), using data obtained
from NuSTAR, Chandra X-ray Observatory, Suzaku and XMM-Newton. The Chandra
imaging shows that a point-like X-ray source is located at the nucleus of the
galaxy at energies above 2 keV. However, the point source resolves into
diffuse emission at lower energies, extending to the east, where the
extranuclear [Oiii]$\lambda$5007 emission, presumably induced by a galactic-
scale outflow, is present. The nuclear source is detected by NuSTAR up to the
rest-frame 30 keV. The strong, high-ionization Fe K line, first seen by XMM-
Newton, and subsequently by Suzaku and Chandra, is not detected in the NuSTAR
data. The line flux appears to have been declining continuously between 2003
and 2016, while the continuum emission remained stable to within 30%. Further
observations are needed to confirm this. The X-ray continuum below 10 keV is
characterised by a hard spectrum caused by cold absorption of NH ~1 × 1023
cm-2, compatible to that of the silicate absorption at 9.7 $\mu$m, and a broad
absorption feature around 8 keV which we attribute to a high-ionization Fe K
absorption edge. The latter is best described by a blueshifted, high-
ionization (log ϵ ~ 3) absorber with a column density of NH ~ 1 × 1024 cm-2,
similar to the X-ray high-velocity outflows observed in a number of active
nuclei. No extra hard component, which would arise from a strongly absorbed
(i.e. Compton-thick) source, is seen in the NuSTAR data. While a pure
reflection scenario (with a totally hidden central source) is viable, direct
emission from the central source of L2-10 keV ≈ 2 × 1044 erg s-1, behind
layers of cold and hot absorbing gas may be an alternative explanation. In
this case, the relative X-ray quietness (Lx/Lbol,AGN ≤ 6 × 10-3), the high-
ionization Fe line, strong outflows inferred from various observations, and
other similarities to the well-studied ULIRG/QSO Mrk 231 point that the
central source in this ULIRG might be accreting close to the Eddington limit.,
archivePrefix = arXiv, arxivId = 1709.01708, author = Iwasawa, K. and Spoon,
H. W.W. and Comastri, A. and Gilli, R. and Lanzuisi, G. and Piconcelli, E. and
Vignali, C. and Brusa, M. and Puccetti, S., doi = 10.1051/0004-6361/201730950,
eprint = 1709.01708, file = :home/william/Documents/Papers/1709.01708.pdf:pdf,
issn = 14320746, journal = Astron. Astrophys., keywords = Galaxies:
active,Galaxies: individual: IRAS F00183, 7111,X-rays: galaxies, pages = 1–9,
title = The active nucleus of the ULIRG IRAS F00183-7111 viewed by NuSTAR,
volume = 606, year = 2017 @articleKing2015a, abstract = Observational
arguments suggest that the growth phases of the supermassive black holes in
active galactic nuclei have a characteristic time-scale ˜105 yr. We show that
this is the time-scale expected in the chaotic accretion picture of black hole
feeding, because of the effect of self-gravity in limiting the mass of any
accretion-disc feeding event., author = King, Andrew and Nixon, Chris, doi =
10.1093/mnrasl/slv098, file = :home/william/.local/share/data/Mendeley
Ltd./Mendeley Desktop/Downloaded/King, Nixon - 2015 - AGN flickering and
chaotic accretion.pdf:pdf, issn = 17453933, journal = Mon. Not. R. Astron.
Soc. Lett., keywords = Accretion, accretion discs,Black hole physics,Galaxies:
active,Galaxies: seyfert,Quasars: supermassive black holes,X-rays: galaxies,
number = 1, pages = L46–L47, title = AGN flickering and chaotic accretion,
volume = 453, year = 2015 @articleRevalski2021, abstract = Outflows of ionized
gas driven by active galactic nuclei (AGN) may significantly impact the
evolution of their host galaxies. However, determining the energetics of these
outflows is difficult with spatially unresolved observations that are subject
to strong global selection effects. We present part of an ongoing study using
Hubble Space Telescope (HST) and Apache Point Observatory (APO) spectroscopy
and imaging to derive spatially-resolved mass outflow rates and energetics for
narrow line region (NLR) outflows in nearby AGN that are based on multi-
component photoionization models to account for spatial variations in the gas
ionization, density, abundances, and dust content. This expanded analysis adds
Mrk 3, Mrk 78, and NGC 1068, doubling the sample in Revalski (2019). We find
that the outflows contain total ionized gas masses of $M 10^{5.5} - 10^{7.5}$
$M_{}$ and reach peak velocities of $v 800 - 2000$ km s$^{-1}$. The outflows
reach maximum mass outflow rates of $M_{out} 3 - 12$ $M_{}$ yr$^{-1}$ and
encompass total kinetic energies of $E 10^{54} - 10^{56}$ erg. The outflows
extend to radial distances of $r 0.1 - 3$ kpc from the nucleus, with the gas
masses, outflow energetics, and radial extents positively correlated with AGN
luminosity. The outflow rates are consistent with in-situ ionization and
acceleration where gas is radiatively driven at multiple radii. These radial
variations indicate that spatially-resolved observations are essential for
localizing AGN feedback and determining the most accurate outflow parameters.,
archivePrefix = arXiv, arxivId = 2101.06270, author = Revalski, Mitchell and
Meena, Beena and Martinez, Francisco and Polack, Garrett E. and Crenshaw, D.
Michael and Kraemer, Steven B. and Collins, Nicholas R. and Fischer, Travis C.
and Schmitt, Henrique R. and Schmidt, Judy and Maksym, W. Peter and Rafelski,
Marc, eprint = 2101.06270, file =
:home/william/Documents/Papers/2101.06270.pdf:pdf, keywords = active,and
dynamics,galaxies,individual,ism,jets and outflows,kinematics,mrk 3,mrk 78,ngc
1068,seyfert, number = 5140, title = Quantifying Feedback from Narrow Line
Region Outflows in Nearby Active Galaxies – III. Results for the Seyfert 2
Galaxies Markarian 3, Markarian 78, and NGC 1068, url =
http://arxiv.org/abs/2101.06270, year = 2021 @articleLopez-Rodriguez2013a,
archivePrefix = arXiv, arxivId = 1302.6858, author = Lopez-Rodriguez, E. and
Packham, C. and Young, S. and Elitzur, M. and Levenson, N. A. and Mason, R. E.
and Almeida, C. Ramos and Alonso-Herrero, A. and Jones, T. J. and Perlman, E.,
doi = 10.5047/eps.2013.05.021, eprint = 1302.6858, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Lopez-Rodriguez et al. - 2013 - New insights into the study
of magnetic field in the clumpy torus of AGN using near-infrared
polarimetry.pdf:pdf, issn = 1343-8832, journal = Earth, Planets Sp., keywords
= agn,infrared,polarimetry,torus, number = 10, pages = 1117–1122, title = New
insights into the study of magnetic field in the clumpy torus of AGN using
near-infrared polarimetry, url =
http://link.springer.com/10.5047/eps.2013.05.021, volume = 65, year = 2013
@articleZubovas2018, abstract = Massive large-scale AGN outflows are an
important element of galaxy evolution, being a way through which the AGN can
affect most of the host galaxy. However, outflows evolve on timescales much
longer than typical AGN episode durations, therefore most AGN outflows are not
observed simultaneously with the AGN episode that inflated them. It is
therefore remarkable that rather tight correlations between outflow prop-
erties and AGN luminosity exist. In this paper, I show that such correlations
can be preserved during the fading phase of the AGN episode, provided that the
AGN lumi- nosity evolves as a power law with exponent $_{d} 1$ at late times.
I also show that subsequent AGN episodes that illuminate an ongoing outflow
are unlikely to produce outflow momentum or energy rates rising above the
observed correlations. However, there may be many difficult-to-detect outflows
with momentum and energy rates lower than expected from the current AGN
luminosity. Detailed observations of AGN out- flow properties might help
constrain the activity histories of typical and/or individual AGN.,
archivePrefix = arXiv, arxivId = 1710.01053, author = Zubovas, Kastytis, doi =
10.1093/mnras/stx2569, eprint = 1710.01053, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Zubovas - 2018 - Massive outflow properties suggest AGN
fade slowly.pdf:pdf, issn = 13652966, journal = Mon. Not. R. Astron. Soc.,
keywords = Accretion,Accretion discs,Galaxies: active,Galaxies:
evolution,Quasars: general, number = 3, pages = 3525–3535, title = Massive
outflow properties suggest AGN fade slowly, volume = 473, year = 2018
@articleVeilleux2005, abstract = Galactic winds are the primary mechanism by
which energy and metals are recycled in galaxies and are deposited into the
intergalactic medium. New observations are revealing the ubiquity of this
process, particularly at high redshift. We describe the physics behind these
winds, discuss the observational evidence for them in nearby star-forming and
active galaxies and in the high-redshift universe, and consider the
implications of energetic winds for the formation and evolution of galaxies
and the intergalactic medium. To inspire future research, we conclude with a
set of observational and theoretical challenges. Copyright 2005 by Annual
Reviews. All rights reserved., archivePrefix = arXiv, arxivId = astro-
ph/0504435, author = Veilleux, Sylvain and Cecil, Gerald and Bland-Hawthorn,
Joss, doi = 10.1146/annurev.astro.43.072103.150610, eprint = 0504435, file =
:home/william/Documents/Papers/annurev.astro.43.072103.150610.pdf:pdf, issn =
00664146, journal = Annu. Rev. Astron. Astrophys., keywords =
Evolution,Halos,Intergalactic medium,Kinematics and dynamics,Nuclei, pages =
769–826, primaryClass = astro-ph, title = Galactic winds, volume = 43, year =
2005 @articleZhang2022, abstract = CSS J102913+404220 is a peculiar narrow
line Seyfert 1 galaxy with an energetic nuclear optical outburst. We present a
detailed analysis of its multi-wavelength photometric and spectroscopic
observations covering a period of decade since outburst. We detect mid-
infrared (MIR) flares delayed by about two months relative to the optical
outburst, with an extremely high peak luminosity of log(L_4.6um)44 erg/s. The
MIR peak luminosity is at least an order of magnitude higher than any known
supernovae explosions, suggesting the optical outburst might be due to a
stellar tidal disruption event (TDE). We find late-time X-ray brightening by a
factor of 30 with respect to what is observed about 100 days after the optical
outburst peak, followed by a flux fading by a factor of ~4 within two weeks,
making it one of Active Galactic Nuclei (AGNs) with extreme variability.
Despite the dramatic X-ray variability, there are no coincident strong flux
variations in optical, UV and MIR bands. This unusual variability behavior has
been seen in other highly accreting AGNs and could be attributed to absorption
variability. In this scenario, the decrease in the covering factor of absorber
with accretion rate could cause the X-ray brightening, possibly induced by the
TDE. Most strikingly, while the UV/optical continuum remains little changes
with time, an evident enhancement in the flux of H_alpha broad emission line
is observed, about a decade after the nuclear optical outburst, which is an
anomalous behavior never seen in any other AGNs. Such an H_alpha anomaly could
be explained by the replenishment of gas clouds and excitation within Broad
Line Region (BLR) that originates, perhaps from the interaction of outflowing
stellar debris with BLR. The results highlight the importance of late-time
evolution of TDE that could affect the accreting properties of AGN, as
suggested by recent simulations., archivePrefix = arXiv, arxivId = 2201.11048,
author = Zhang, W. J. and Shu, X. W. and Sheng, Z. F. and Sun, L. M. and Dou,
L. M. and Jiang, N. and Wang, J. G. and Hu, X. Y. and Wang, Y. B. and Wang, T.
G., eprint = 2201.11048, file =
:home/william/Documents/Papers/2201.11048.pdf:pdf, keywords =
404220,accretion,accretion disks,active,css
j102913,galaxies,individual,x-rays, pages = 1–16, title = Discovery of late-
time X-ray flare and anomalous emission line enhancement after the nuclear
optical outburst in a narrow-line Seyfert 1 Galaxy, url =
http://arxiv.org/abs/2201.11048, year = 2022 @articleBlumenthal.G.1970,
abstract = Expressions are derived for the total energy loss and photon-
production spectrum by the processes of Compton scatter- ing, bremsstrahlung,
and synchrotron radiation from highly relativistic electrons. For Compton
scattering, the general case, the Thomson limit, and the extreme Klein
—Nishina limit are considered. Bremsstrahlung is treated for the cases where
the electron is scattered by a pure Coulomb field and by an atom. For the
latter case the effects of shielding are discussed extensively. The
synchrotron spectrum is derived for an electron moving in a circular orbit
perpendicular to the magnetic field and also for the general case where the
electron’s motion is helical. The total photon-production spec- trum is
derived for each process when there is a power-law distribution of electron
energies. The problems of the eBects of the three processes on the electron
distribution itself are considered. It is shown that if the electron loses a
small frac- tion of its energy in a single occurrence of a process, the
electron distribution function satisfies a continuity equation which is a
differential equation in energy space. For the more general case where the
electron can Jose energy in discrete amounts (as in bremsstrahlung and extreme
Klein —Nishina Compton losses), the electron distribution function satis6es an
integro-differential equation. Some approximate solutions to this equation are
derived for certain special cases., author = Blumenthal. G., Gould. J, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Blumenthal. G. - 1970 - Reviews of Modern Physics.pdf:pdf,
journal = Rev. Mod. Phys., number = 2, pages = 237–270, title = Reviews of
Modern Physics, volume = 42, year = 1970 @articleKrumholz2019a, abstract =
Star-forming gas clouds are strongly magnetized, and their ionization
fractions are high enough to place them close to the regime of ideal
magnetohydrodyamics on all but the smallest size scales. In this review we
discuss the effects of magnetic fields on the star formation rate (SFR) in
these clouds, and on the mass spectrum of the fragments that are the outcome
of the star formation process, the stellar initial mass function (IMF).
Current numerical results suggest that magnetic fields by themselves are minor
players in setting either the SFR or the IMF, changing star formation rates
and median stellar masses only by factors of ~2−3 compared to non-magnetized
flows. However, the indirect effects of magnetic fields, via their interaction
with star formation feedback in the form of jets, photoionization, radiative
heating, and supernovae, could have significantly larger effects. We explore
evidence for this possibility in current simulations, and suggest avenues for
future exploration, both in simulations and observations., archivePrefix =
arXiv, arxivId = 1902.02557, author = Krumholz, Mark R. and Federrath,
Christoph, doi = 10.3389/fspas.2019.00007, eprint = 1902.02557, file =
:home/william/Documents/Papers/fspas-06-00007.pdf:pdf, issn = 2296987X,
journal = Front. Astron. Sp. Sci., keywords = ISM: clouds,ISM: kinematics and
dynamics,ISM: magnetic fields,galaxies: star formation,magnetohydrodynamics
(MHD),stars: formation,turbulence, number = February, pages = 1–28, title =
The Role of Magnetic Fields in Setting the Star Formation Rate and the Initial
Mass Function, volume = 6, year = 2019 @articleRupke2018, abstract = Galaxy-
scale outflows of gas, or galactic winds (GWs), driven by energy from star
formation are a pivotal mechanism for regulation of star formation in the
current model of galaxy evolution. Observations of this phenomenon have
proliferated through the wide application of old techniques on large samples
of galaxies, the development of new methods, and advances in telescopes and
instrumentation. I review the diverse portfolio of direct observations of
stellar GWs since 2010. Maturing measurements of the ionized and neutral gas
properties of nearby winds have been joined by exciting new probes of
molecular gas and dust. Low-$z$ techniques have been newly applied in large
numbers at high $z$. The explosion of optical and near-infrared 3D imaging
spectroscopy has revealed the complex, multiphase structure of nearby GWs.
These observations point to stellar GWs being a common feature of rapidly
star-forming galaxies throughout at least the second half of cosmic history,
and suggest that scaling relationships between outflow and galaxy properties
persist over this period. The simple model of a modest-velocity, biconical
flow of multiphase gas and dust perpendicular to galaxy disks continues to be
a robust descriptor of these flows., archivePrefix = arXiv, arxivId =
1812.05184, author = Rupke, David S. N., doi = 10.3390/galaxies6040138, eprint
= 1812.05184, file = :home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Rupke - 2018 - A Review of Recent Observations of Galactic
Winds Driven by Star Formation.pdf:pdf, keywords = feedback,galactic
winds,outflows,star formation, title = A Review of Recent Observations of
Galactic Winds Driven by Star Formation, url =
http://arxiv.org/abs/1812.05184%0Ahttp://dx.doi.org/10.3390/galaxies6040138,
year = 2018 @articleDesch1998, abstract = Key processes are examined in the
heating and cooling of molecular gas with emphasis on environments for water
masers at the nuclei of galaxies. The exchange of infrared radiation between
the gas and dust grains is evaluated in determining the cooling of the gas and
in determining the thermal coupling between the gas and the dust grains.
Calculations are performed for the transport of continuum radiation through an
optically thick slab to assess the temperatures of the dust grains. The highly
refined observational description of the subparsec circumnuclear disk in the
galaxy NGC 4258 serves as a focus. The viscous dissipation that is inherent in
an accretion disk is reconsidered as a source of heat to create the masing
environment. Based on our cooling rates, the input of energy that is required
to create the bulk of the observed masing gas is evaluated and is found to be
comparable in magnitude (per unit surface area) to that generated by the
viscous dissipation. To be effective in actually creating the masing
environment, the distribution for the viscous dissipation of heat with
distance from the midplane of the disk must be quite different from the
distribution of the mass. Tentative evidence that this is plausible is
discussed. One consequence is the likely presence of a component of the disk
at the midplane that is colder and much more massive than the masing gas. The
recent interpretation that the inner disk of NGC 4258 may be advective is
especially useful for this description, since the viscous dissipation at the
location of the masers tends to be enhanced. A significant temperature
difference between the gas and the grains, which is necessary for masing, is
found to result regardless of whether the heating in these environments is
provided by viscous dissipation or by X-rays., author = Desch, S. J. and
Wallin, B. K. and Watson, W. D., doi = 10.1086/305391, file =
:home/william/Documents/Papers/Radiative_Cooling_and_Viscous_Dissipation_in_Molec.pdf:pdf,
issn = 0004-637X, journal = Astrophys. J., number = 2, pages = 775–785, title
= Radiative Cooling and Viscous Dissipation in Molecular Accretion Disks at
the Nuclei of Galaxies, volume = 496, year = 1998 @articleNielsen1998,
abstract = This paper presents a general formulation of least-squares
estimation using Lagrange multipliers. It is general in the sense that it
takes into account the covariance matrix of all measured quantities and allows
any known constraint to be imposed on the quantities being estimated. The
technique may be used to estimate parameters of a calibration curve for a
transducer taking into account the uncertainty and correlation coefficients of
the measured stimuli and responses. It may also be used to adjust measured
fundamental constants to a coherent set obeying the appropriate physical
laws., author = Nielsen, L., doi = 10.1088/0026-1394/35/2/6, file =
:home/william/Documents/Papers/Least-
squares_estimation_using_Lagrange_multiplier.pdf:pdf, issn = 00261394, journal
= Metrologia, number = 2, pages = 115–118, title = Least-squares estimation
using Lagrange multipliers, volume = 35, year = 1998 @articleFabian2001,
abstract = Although soft X-ray absorption features in AGNs were discovered
almost ten years ago, the nature and location of the gas creating them has
remained controversial. Guided by the results of recent high-resolution X-ray
spectroscopy, we argue that these features are created in a multitemperature
wind whose source of matter is photoionized evaporation from the inner edge of
the obscuring torus often found surrounding an AGN. Photoionized evaporation
in the presence of a copious mass source locks the ratio of ionizing intensity
to pressure to a critical value. However, a broad range of temperatures can
coexist in equilibrium for this value of the ratio of ionizing intensity to
pressure. Consequently, the flow is expected to be strongly inhomogeneous in
temperature. The inferred distance of this material from the source of
ionizing radiation depends on how much matter exists at the highest obtainable
temperature. This distance can be measured by monitoring how ionic column
densities respond to changes in the ionizing continuum on timescales of days
to years., archivePrefix = arXiv, arxivId = astro-ph/9502006, author = Fabian,
A. C. and Reynolds, C. S., doi = 10.1086/323442, eprint = 9502006, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Fabian, Reynolds - 2001 - Warm Absorbers in Active Galactic
Nuclei.pdf:pdf, issn = 0004-637X, journal = Astrophys. J., keywords =
Galaxies: Seyfert,Galaxies: active,Galaxies: nuclei,Quasars: absorption
lines,Ultraviolet: galaxies,X-rays: galaxies, number = 2, pages = 684–690,
primaryClass = astro-ph, title = Warm Absorbers in Active Galactic Nuclei, url
=
http://www.scopus.com/inward/record.url?eid=2-s2.0-0035841719&partnerID=tZOtx3y1,
volume = 561, year = 2001 @articleHansen2018, abstract = Radiative cooling
plays a crucial role in the dynamics of many astrophysical flows, and is
particularly important in the dense shocked gas within Herbig-Haro (HH)
objects and stellar jets. Simulating cooling processes accurately is necessary
to compare numerical simulations with existing and planned observations of HH
objects, such as those from the Hubble Space Telescope and the James Webb
Space Telescope. In this paper, we discuss a new, non-equilibrium cooling
scheme we have implemented into the three-dimensional magnetohydrodynamic
(MHD) code ASTROBEAR. The new cooling function includes ionization,
recombination, and excitation of all the important atomic species that cool
below 10 000 K. We tested the routine by comparing its predictions with those
from the well-tested onedimensional Cox-Raymond shock code (Raymond 1979). The
results show that ASTROBEAR accurately tracks the ionization fraction,
temperature, and other MHD variables for all lowvelocity (≲90 km s-1)
magnetized radiative shock waves. The new routine allows us to predict
synthetic emission maps in all the bright forbidden and permitted lines
observed in stellar jets, including H$\alpha$, [NII], [OI], and [S II]. We
present an example as to how these synthetic maps facilitate a direct
comparison with narrowband images of HH objects., archivePrefix = arXiv,
arxivId = 1809.02207, author = Hansen, E. C. and Hartigan, P. and Frank, A.
and Wright, A. and Raymond, J. C., doi = 10.1093/mnras/sty2471, eprint =
1809.02207, file = :home/william/Documents/Papers/1809.02207.pdf:pdf, issn =
13652966, journal = Mon. Not. R. Astron. Soc., keywords = (ISM:) Herbig-Haro
objects,(magnetohydrodynamics) MHD,ISM: jets and outflows,Line:
formation,Methods: numerical,Radiation mechanisms: thermal, number = 3, pages
= 3098–3107, title = Simulating radiative magnetohydrodynamical flows with
ASTROBEAR: Implementation and applications of non-equilibrium cooling, volume
= 481, year = 2018 @articleLunardini2015, abstract = The Fermi Bubbles have
been imaged in sub-TeV gamma rays at Fermi-LAT, and, if their origin is
hadronic, they might have been seen with low statistics in $0.1- 1$ PeV
neutrinos at IceCube. We discuss the detectability of these objects at the new
High Altitude Water Cherenkov (HAWC) gamma ray detector. HAWC will view the
North Bubble for $2-3$ hours a day, and will map its spectrum at 0.1-100 TeV.
For the hard primary proton spectrum required to explain five events at
IceCube, a high significance detection at HAWC will be achieved in less than
30 days. The combination of results at HAWC and IceCube will substantiate the
hadronic model, or constrain its spectral parameters., author = Lunardini,
Cecilia and Razzaque, Soebur and Yang, Lili, doi = 10.1103/PhysRevD.92.021301,
file = :home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Lunardini, Razzaque, Yang - 2015 - Multimessenger study of
the Fermi bubbles Very high energy gamma rays and neutrinos.pdf:pdf, issn =
15502368, journal = Phys. Rev. D - Part. Fields, Gravit. Cosmol., number = 2,
pages = 1–5, title = Multimessenger study of the Fermi bubbles: Very high
energy gamma rays and neutrinos, volume = 92, year = 2015 @articleRose2018a,
abstract = Although now routinely incorporated into hydrodynamic simulations
of galaxy evolution, the true importance of the feedback effect of the
outflows driven by active galactic nuclei (AGNs) remains uncertain from an
observational perspective. This is due to a lack of accurate information on
the densities, radial scales and level of dust extinction of the outflow
regions. Here we use the unique capabilities of VLT/Xshooter to investigate
the warm outflows in a representative sample of nine local (0.06 z 0.15)
Ultraluminous Infrared Galaxies (ULIRGs) with AGNs and, for the first time,
accurately quantify the key outflow properties. We find that the outflows are
compact (0.06 R[O III] 1.2 kpc), significantly reddened (median
E(B-V)~0.5magnitudes), and have relatively high electron densities (3.4 log10
ne (cm-3) 4.8). It is notable that the latter densities - obtained using
trans-auroral [S II] and [O II] emission-line ratios - exceed those typically
assumed for the warm, emission-line outflows in active galaxies, but are
similar to those estimated for broad and narrow absorption line outflow
systems detected in some type 1 AGN. Even if we make the most optimistic
assumptions about the true (deprojected) outflow velocities, we find
relatively modest mass outflow rates (0.07 M? 14 M⊙ yr-1) and kinetic powers
measured as a fraction of the AGN bolometric luminosities (4 × 10-4 E/LBOL 0.8
per cent). Therefore, although warm, AGN-driven outflows have the potential to
strongly affect the star formation histories in the inner bulge regions (r ~ 1
kpc) of nearby ULIRGs, we lack evidence that they have a significant impact on
the evolution of these rapidly evolving systems on larger scales.,
archivePrefix = arXiv, arxivId = 1710.06600, author = Rose, Marvin and
Tadhunter, Clive and Almeida, Cristina Ramos and Zaurín, Javier Rodríguez and
Santoro, Francesco and Spence, Robert, doi = 10.1093/MNRAS/STX2590, eprint =
1710.06600, file = :home/william/Documents/Papers/stx2590.pdf:pdf, issn =
13652966, journal = Mon. Not. R. Astron. Soc., keywords = Galaxies:
active,Galaxies: interactions,Quasars: emission lines,Quasars: general, number
= 1, pages = 128–156, title = Quantifying the AGN-driven outflows in ULIRGs
(QUADROS) - I: VLT/Xshooter observations of nine nearby objects, volume = 474,
year = 2018 @articleMartinez-Tibaduiza2020, abstract = In this work we
demonstrate new BCH-like relations involving the generators of the su(1,1),
su(2) and so(2,1) Lie algebras. We use our results to obtain in a
straightforward way the composition of an arbitrary number of elements of the
corresponding Lie groups. In order to make a self-consistent check of our
results, as a first application we recover the non-trivial composition law of
two arbitrary squeezing operators. As a second application, we show how our
results can be used to compute the time evolution operator of physical systems
described by time-dependent hamiltonians given by linear combinations of the
generators of the aforementioned Lie algebras., archivePrefix = arXiv, arxivId
= 2005.09500, author = Martínez-Tibaduiza, D. and Aragão, A. H. and Farina, C.
and Zarro, C. A.D., doi = 10.1016/j.physleta.2020.126937, eprint = 2005.09500,
file = :home/william/Documents/Papers/New BCH-like relations of the su(1, 1),
su(2) and so(2, 1) Lie algebras sublined.pdf:pdf, issn = 03759601, journal =
Phys. Lett. Sect. A Gen. At. Solid State Phys., keywords = Baker-Campbell-
Hausdorff relations,Lie Algebras,Squeezed States,Time-dependent hamiltonians,
number = 36, pages = 126937, publisher = Elsevier B.V., title = New BCH-like
relations of the su(1,1), su(2) and so(2,1) Lie algebras, url =
https://doi.org/10.1016/j.physleta.2020.126937, volume = 384, year = 2020
@article2011ApJ…737…26N, archivePrefix = arXiv, arxivId = 1007.3505, author =
Novak, G.~S. and Ostriker, J.~P. and Ciotti, L, doi =
10.1088/0004-637X/737/1/26, eprint = 1007.3505, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Novak, Ostriker, Ciotti - 2011 - Feedback from central
black holes in elliptical galaxies Two-dimensional models compared to one-
dimensi.pdf:pdf, journal = Apj, keywords = cD,galaxies: active,galaxies:
elliptical and lenticular,galaxies: nuclei,quasars: general, pages = 26, title
= Feedback from Central Black Holes in Elliptical Galaxies: Two-dimensional
Models Compared to One-dimensional Models, volume = 737, year = 2011
@articleZubovas2019, abstract = Warm absorbers are found in many AGN and
consist of clouds moving at moderate radial velocities, showing complex
ionization structures and having moderate to large column densities. Using 1D
numerical calculations, we confirm earlier suggestions that the energy
released by an AGN pushes the surrounding gas outward in a bubble until this
reaches transparency. Typical AGN episode durations of $510^4$ yr supply
enough energy for this, except in very gas-rich and/or very compact galaxies,
such as those in the early Universe. In those galaxies, the AGN might remain
hidden for many periods of activity, hiding the black hole growth. The typical
radii of $0.1-1$ kpc, velocities of $100-1000$ km s$^{-1}$ and resulting
optical depths are consistent with observations of warm absorbers. The
resulting structure is a natural outcome of outflows driven by AGN buried in
an optically thick gas envelope, and has a total mass comparable to the final
$M -$ mass the central supermassive black hole will eventually reach.These
results suggest that AGN can feed very efficiently by agitating this
surrounding dense material. This may not be easy to observe, as this gas is
Compton thick along many sightlines. The infall may produce episodic star
formation in the centre, building up nuclear star clusters simultaneously with
the growth of the central black hole., archivePrefix = arXiv, arxivId =
1901.02224, author = Zubovas, Kastytis and King, Andrew, eprint = 1901.02224,
file = :home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Zubovas, King - 2019 - Warm absorbers supermassive black
hole feeding, and Compton-thick AGN.pdf:pdf, keywords = accretion,accretion
discs,evolution,general,ism,quasars, number = January, pages = 1–9, title =
Warm absorbers: supermassive black hole feeding, and Compton-thick AGN, url =
http://arxiv.org/abs/1901.02224, volume = 9, year = 2019 @articleMhd, author =
Mhd, Week Astrophysical and Magneto-, Week Radiation and Stone, Jim, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley Desktop/Downloaded/Mhd,
Magneto-, Stone - Unknown - Numerical Methods Numerical Methods for
Astrophysical Two lectures on Numerical Methods.pdf:pdf, pages = 1–17, title =
Numerical Methods Numerical Methods for Astrophysical Two lectures on
Numerical Methods, volume = M @articleBolatto2013, abstract = CO line emission
represents the most accessible and widely used tracer of the molecular ISM.
This renders the translation of observed CO intensity into total H2 gas mass
critical to understanding star formation and the ISM in our Galaxy and beyond.
We review the theoretical underpinning, techniques, and results of efforts to
estimate this CO-to-H2 ”conversion factor,” XCO, in different environments. In
the Milky Way disk, we recommend a conversion factor of cm-2 (K km s-1)-1 with
±30% uncertainty. Studies of other ”normal galaxies” return similar values in
Milky Way-like disks, but with greater scatter and systematic uncertainty.
Departures from this Galactic conversion factor are both observed and
expected. Dust-based determinations, theoretical arguments, and scaling
relations all suggest that XCO increases with decreasing metallicity, turning
up sharply below metallicity ∼1/3-1/2 solar in a manner consistent with model
predictions that identify shielding as a key parameter. Based on spectral line
modeling and dust observations, XCO appears to drop in the central, bright
regions of some but not all galaxies, often coincident with regions of bright
CO emission and high stellar surface density. This lower XCO is also present
in the overwhelmingly molecular ISM of starburst galaxies, where several lines
of evidence point to a lower CO-to-H2 conversion factor. At high redshift,
direct evidence regarding the conversion factor remains scarce; we review what
is known based on dynamical modeling and other arguments. Copyright 2013 by
Annual Reviews. All rights reserved., archivePrefix = arXiv, arxivId =
1301.3498, author = Bolatto, Alberto D. and Wolfire, Mark and Leroy, Adam K.,
doi = 10.1146/annurev-astro-082812-140944, eprint = 1301.3498, file =
:home/william/Documents/Papers/bolatto2013.pdf:pdf, issn = 00664146, journal =
Annu. Rev. Astron. Astrophys., keywords = Galaxies: ISM,ISM: general,ISM:
molecules,Radio lines: ISM, number = June, pages = 207–268, title = The CO-
to-H2 conversion factor, volume = 51, year = 2013 @articleBicknell2018,
abstract = We propose that Gigahertz Peak Spectrum (GPS) and Compact Steep
Spectrum (CSS) radio sources are the signposts of relativistic jet feedback in
evolving galaxies. Our simulations of relativistic jets interacting with a
warm, inhomogeneous medium, utilizing cloud densities and velocity dispersions
in the range derived from optical observations, show that free-free absorption
can account for the ~ GHz peak frequencies and low-frequency power laws
inferred from the radio observations. These new computational models replace a
power-law model for the free-free optical depth a more fundamental model
involving disrupted log-normal distributions of warm gas. One feature of our
new models is that at early stages, the low-frequency spectrum is steep but
progressively flattens as a result of a broader distribution of optical
depths, suggesting that the steep low-frequency spectra discovered by
Callingham et al. may possibly be attributed to young sources. We also
investigate the inverse correlation between peak frequency and size and find
that the initial location on this correlation is determined by the average
density of the warm ISM. The simulated sources track this correlation
initially but eventually fall below it, indicating the need for a more
extended ISM than presently modelled. GPS and CSS sources can potentially
provide new insights into the phenomenon of AGN feedback since their peak
frequencies and spectra are indicative of the density, turbulent structure,
and distribution of gas in the host galaxy., archivePrefix = arXiv, arxivId =
1801.06518, author = Bicknell, Geoffrey V. and Mukherjee, Dipanjan and Wagner,
Alexander Y. and Sutherland, Ralph S. and Nesvadba, Nicole P.H., doi =
10.1093/mnras/sty070, eprint = 1801.06518, file =
:home/william/Documents/Papers/sty070.pdf:pdf, issn = 13652966, journal = Mon.
Not. R. Astron. Soc., keywords = Galaxies: evolution,ISM: jets and
outflows,Radio continuum: galaxies, number = 3, pages = 3493–3501, title =
Relativistic jet feedback - II. Relationship to gigahertz peak spectrum and
compact steep spectrum radio galaxies, volume = 475, year = 2018
@articleSobacchi2018, abstract = In the paradigm of magnetic launching of
astrophysical jets, instabilities in the magnetohydrodynamic (MHD) flow are a
good candidate to convert the Poynting flux into the kinetic energy of the
plasma. If the magnetized plasma fills the almost entire space, the jet is
unstable to helical perturbations of its body. However, the growth rate of
these modes is suppressed when the poloidal component of the magnetic field
has a vanishing gradient, which may be the actual case for a realistic
configuration. Here we show that, if the magnetized plasma is confined into a
limited region by the pressure of some external medium, the velocity shear at
the contact surface excites unstable modes which can affect a significant
fraction of the jet’s body. We find that when the Lorentz factor of the jet is
$\Gamma$ ~ 10 ($\Gamma$ ~ 100), these perturbations typically develop after
propagating along the jet for tens (hundreds) of jet’s radii. Surface modes
may therefore play an important role in converting the energy of the jet from
the Poynting flux to the kinetic energy of the plasma, particularly in active
galactic nuclei. The scaling of the dispersion relation with (i) the angular
velocity of the field lines and (ii) the sound speed in the confining gas is
discussed., archivePrefix = arXiv, arxivId = 1709.01103, author = Sobacchi, E.
and Lyubarsky, Y E, doi = 10.1093/mnras/stx2592, eprint = 1709.01103, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Lyubarsky - 2018 - External Confinement and Surface Modes
in Magnetised Force-Free Jets arXiv 1709 . 01103v2 astro-ph . HE 3 Oct
2017.pdf:pdf, issn = 13652966, journal = Mon. Not. R. Astron. Soc., keywords =
Galaxies: jets,Instabilities,MHD, number = 2, pages = 2813–2821, title =
External confinement and surface modes in magnetized force-free jets, volume =
473, year = 2018 @articleInoue2020, abstract = We report our high-resolution
(0.03 arcsec to 0.07 arcsec) ALMA imaging of the quadruply lensed radio-loud
quasar MG$\backslash$,J0414+0534 at redshift $z=2.639$ in the continuum and
the broad CO(11-10) line at $340\,$GHz. With the help of strong lensing
magnification and ALMA’s high-resolution, we succeeded in resolving the
jet/dust and CO gas in the quasar host galaxy both extending up to $1\,$kpc,
with a resolution of $50\,$pc for the first time. Both the continuum emission
and the CO(11-10) line have a similar bimodal structure aligned with the
quasar jets ($200\,$pc) observed by Very Long Baseline Interferometry (VLBI)
at $5\,$GHz and $8.4\,$GHz. The CO gas in the vicinity of both the eastern and
western jet components at the location of $80\,$pc from the quasar core are
moving at high velocities up to $600\,$${km}\,{s}^{-1}$ relative to the core.
The observed features show clear evidence of strong interaction between the
jets and interstellar medium (ISM). High temperature and high density
environments in the ISM of the quasar host galaxy, as suggested from CO line
ratios, also support this result. The small scale of the jets, the jet-ISM
interaction, and the continuum spectral energy distribution of this source
indicate that we are watching the infancy stage of quasar radio activity.,
archivePrefix = arXiv, arxivId = 2003.01650, author = Inoue, Kaiki Taro and
Matsushita, Satoki and Nakanishi, Kouichiro and Minezaki, Takeo, doi =
10.3847/2041-8213/ab7b7e, eprint = 2003.01650, file =
:home/william/Documents/Papers/[Inoue et al.]-ALMA 50-parsec-resolution
Imaging of Jet–ISM Interaction.pdf:pdf, issn = 2041-8213, journal = Astrophys.
J., keywords = Radio loud quasars,Radio jets,Molecular clouds,Str, number = 2,
pages = L18, publisher = IOP Publishing, title = ALMA 50-parsec-resolution
Imaging of Jet–ISM Interaction in the Lensed Quasar MG J0414+0534, url =
http://dx.doi.org/10.3847/2041-8213/ab7b7e, volume = 892, year = 2020
@articleRuffa2021, abstract = This is the fourth paper of a series
investigating the AGN fuelling/feedback processes in a sample of eleven nearby
low-excitation radio galaxies (LERGs). In this paper we present follow-up
Atacama Large Millimeter/submillimeter Array (ALMA) observations of one
source, NGC 3100, targeting the 12CO(1-0), 12CO(3-2), HCO+(4-3), SiO(3-2) and
HNCO(6-5) molecular transitions. 12CO(1-0) and 12CO(3-2) lines are nicely
detected and complement our previous 12CO(2-1) data. By comparing the relative
strength of these three CO transitions, we find extreme gas excitation
conditions (i.e. Tex ≳ 50 K) in regions that are spatially correlated with the
radio lobes, supporting the case for a jet-ISM interaction. An accurate study
of the CO kinematics demonstrates that, although the bulk of the gas is
regularly rotating, two distinct non-rotational kinematic components can be
identified in the inner gas regions: one can be associated to inflow/outflow
streaming motions induced by a two-armed spiral perturbation; the second one
is consistent with a jet-induced outflow with vmax ≈ 200 km s−1 and ${M}0.12$
M⊙ yr−1. These values indicate that the jet-CO coupling ongoing in NGC 3100 is
only mildly affecting the gas kinematics, as opposed to what expected from
existing simulations and other observational studies of (sub-)kpc scale jet-
cold gas interactions. HCO+(4-3) emission is tentatively detected in a small
area adjacent to the base of the northern radio lobe, possibly tracing a
region of jet-induced gas compression. The SiO(3-2) and HNCO(6-5) shock
tracers are undetected: this - along with the tentative HCO+(4-3) detection -
may be consistent with a deficiency of very dense (i.e. ncrit 106 cm−3) cold
gas in the central regions of NGC 3100., archivePrefix = arXiv, arxivId =
2112.00755, author = Ruffa, Ilaria and Prandoni, Isabella and Davis, Timothy A
and Laing, Robert A and Paladino, Rosita and Casasola, Viviana and Parma,
Paola and Bureau, Martin, doi = 10.1093/mnras/stab3541, eprint = 2112.00755,
file = :home/william/Documents/Papers/2112.00755.pdf:pdf, issn = 0035-8711,
journal = Mon. Not. R. Astron. Soc., keywords = active,cd,elliptical and
lenticular,evolution,galaxies,ism,nuclei, number = December, pages = 1–20,
title = The AGN fuelling/feedback cycle in nearby radio galaxies - IV.
Molecular gas conditions and jet-ISM interaction in NGC 3100, volume = 20,
year = 2021 @articleMiralles-Caballero2011, abstract = We present a
comprehensive characterization of the general properties (luminosity functions
(LFs), mass, size, ages, etc.) of optically selected compact stellar objects
(knots) in a representative sample of 32 low-z luminous and ultraluminous
infrared galaxies ((U)LIRGs). It is important to understand the formation and
evolution of these properties in such systems, which represent the most
extreme cases of starbursts in the low-z universe. We have made use of high
angular resolution Advanced Camera for Surveys images from the Hubble Space
Telescope in F435W (B) and F814W (I) bands. The galaxies in the sample
represent different interaction phases (first contact, pre-merger, merger, and
post-merger) and cover a wide luminosity range (11.46 ≤ log (L IR/L) ≤ 12.54).
With a median size of 32pc, most of the nearly 3000 knots detected consist of
complexes of star clusters. Some of the knots (15%) are so blue that their
colors indicate a young (i.e., 30Myr) and almost extinction-free population.
There is a clear correlation of the mass of these blue knots with their
radius, where MR 1.91 0.14, similar to that found in complexes of clusters in
M51 and in giant molecular clouds. This suggests that the star formation
within the knots is proportional to the gas density at any given radius. This
relation does not depend significantly on either the infrared luminosity of
the system or the interaction phase. The star formation of all the knots is
characterized by LFs of the knots with slopes close to 2. Nevertheless, we see
a marginally significant indication that the LF evolves with the interaction
process, becoming steeper from early to advanced merger phases. Due to size-
of-sample effects we are probably sampling knots in ULIRGs that intrinsically
more luminous (by a factor of about four) than in less luminous systems. They
also have sizes and are likely to have masses characteristic of clumps in
galaxies at z ≳ 1. Knots in post-mergers are on average (1.3-2 times) larger,
more luminous (2 mag) in the I band, and 0.5mag redder than those in systems
in earlier phases. Two scenarios are briefly discussed: (1) the likely
presence of relatively high extinction in the most advanced mergers and (2)
the dissolution of the less massive clusters and/or their coalescence into
more massive, evolved superclusters. 2011. The American Astronomical Society.
All rights reserved., archivePrefix = arXiv, arxivId = 1107.1777, author =
Miralles-Caballero, Daniel and Colina, Luis and Arribas, Santiago and Duc,
Pierre Alain, doi = 10.1088/0004-6256/142/3/79, eprint = 1107.1777, file =
:home/william/Documents/Papers/Miralles-Caballero.pdf:pdf, issn = 00046256,
journal = Astron. J., keywords = galaxies: evolution,galaxies:
interactions,galaxies: photometry,galaxies: star clusters: general,galaxies:
starburst, number = 3, title = Characterization of optically selected star-
forming knots in (U)LIRGs, volume = 142, year = 2011 @articleHeber2003,
abstract = We discovered that HD 188112, a bright (V =
$\backslash$magpt{10}{2}), nearby (80 pc) B-type star, is a unique subluminous
B (sdB) star. SdB stars are usually identified with models of core helium
burning Extreme Horizontal-Branch (EHB) stars of half a solar mass. A spectral
analysis of the hydrogen and helium lines resulted in T_eff = 21 500 +/- 500
K, log g = 5.66 +/- 0.05 placing the star below the EHB. HD 188112 was found
to be radial velocity (RV) variable and the RV curve has been measured to be
perfectly sinusoidal with a period of 0.606585 days and a semi-amplitude of
188.3 km s-1 indicating that it is a close binary system. From the atmospheric
parameters and the Hipparcos parallax we conclude that the sdB star is of low
mass (0.24 Msun). The mass of the sdB is too low to sustain core helium
burning and it is now evolving into a helium core white dwarf. A lower limit
to the mass of its unseen companion of 0.73 Msun is derived from the mass
function. Because the companion does not contribute to the spectral energy
distribution from the UV to the infrared it cannot be a main sequence star but
must be a white dwarf (WD), a neutron star (NS) or a black hole. The system
would qualify as pre-supernova Ia candidate (sdB+WD) if its total mass is
above the Chandrasekhar limit (1.4 Msun), or as post-supernova (sdB+NS) if the
companion mass is above that limit, requiring the inclination angle to be
lower than 51deg or 48deg, respectively. Based on observations collected at
the German-Spanish Astronomical Center (DSAZ), Calar Alto, operated by the
Max-Planck-Institut für Astronomie, Heidelberg jointly with the Spanish
National Commission for Astronomy. Based on observations collected at the
European Southern Observatory (ESO proposal No. 65.H-0341(A) and
69.D-0016(A))., archivePrefix = arXiv, arxivId = astro-ph/0304271, author =
Heber, U and Edelmann, H and Lisker, T and Napiwotzki, R, doi =
10.1051/0004-6361, eprint = 0304271, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Heber et al. - 2003 - Letter to the Editor
Astronomy.pdf:pdf, isbn = 0009-8981 (Print), issn = 00098981, journal =
Astron. Astrophys. Lett., keywords = binaries,early-type,fundamental
parameters,hd 188112,individual,spectroscopic,stars, pages = 477–480, pmid =
11432396, primaryClass = astro-ph, title = Letter to the Editor Astronomy,
volume = 480, year = 2003 @articleCattaneo2009, abstract = Virtually all
massive galaxies, including our own, host central black holes ranging in mass
from millions to billions of solar masses. The growth of these black holes
releases vast amounts of energy that powers quasars and other weaker active
galactic nuclei. A tiny fraction of this energy, if absorbed by the host
galaxy, could halt star formation by heating and ejecting ambient gas. A
central question in galaxy evolution is the degree to which this process has
caused the decline of star formation in large elliptical galaxies, which
typically have little cold gas and few young stars, unlike spiral galaxies.
2009 Macmillan Publishers Limited. All rights reserved., author = Cattaneo, A.
and Faber, S. M. and Binney, J. and Dekel, A. and Kormendy, J. and Mushotzky,
R. and Babul, A. and Best, P. N. and Brüggen, M. and Fabian, A. C. and Frenk,
C. S. and Khalatyan, A. and Netzer, H. and Mahdavi, A. and Silk, J. and
Steinmetz, M. and Wisotzki, L., doi = 10.1038/nature08135, file =
:home/william/Documents/Papers/cattaneo2009.pdf:pdf, issn = 00280836, journal
= Nature, number = 7252, pages = 213–219, title = The role of black holes in
galaxy formation and evolution, volume = 460, year = 2009
@articleKraemer2017a, abstract = XMM-Newton and Suzaku spectra of AGN have
revealed highly ionized gas, in the form of absorption lines from H-like and
He-like Fe. Some of these absorbers, ”Ultra Fast Outflows (UFOs)”, have radial
velocities of up to 0.25c. We have undertaken a detailed photo-ionization
study of high-ionization Fe absorbers, both UFOs and non-UFOs, in a sample of
AGN observed by XMM-Newton. We find that the heating and cooling processes in
UFOs are Compton-dominated, unlike the non-UFOs. Both types are characterized
by Force Multipliers on the order of unity, which suggests that they cannot be
radiatively accelerated in sub-Eddington AGN, unless they were much less
ionized at their point of origin. However, such highly ionized gas can be
accelerated via a Magneto-Hydrodynamic (MHD) wind. We explore this possibility
by applying a cold MHD flow model to the UFO in the well-studied Seyfert
galaxy, NGC 4151. We find that the UFO can be accelerated along magnetic
streamlines anchored in the accretion disk. In the process, we have been able
to constrain the magnetic field strength and the magnetic pressure in the UFO
and have determined that the system is not in magnetic/gravitational
equipartition.Open questions include the variability of the UFOs and the
apparent lack of non-UFOs in UFO sources., archivePrefix = arXiv, arxivId =
1711.07965, author = Kraemer, S. B. and Tombesi, F. and Bottorff, M. C., doi =
10.3847/1538-4357/aa9ce0, eprint = 1711.07965, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Kraemer, Tombesi, Bottorff - 2017 - Physical Conditions in
Ultra Fast Outflows in AGN.pdf:pdf, issn = 1538-4357, keywords =
accretion,accretion disks,active,galaxies,x-rays, title = Physical Conditions
in Ultra Fast Outflows in AGN, url =
http://arxiv.org/abs/1711.07965%0Ahttp://dx.doi.org/10.3847/1538-4357/aa9ce0,
volume = 35, year = 2017 @articleSusanne2010, abstract = Supernova explosions
are very violent events which transfer a significant amount of en-ergy to the
interstellar medium (ISM) and are responsible for a large variety of physical
processes. We will not discuss the actual explosion mechanisms here which are
thought to be due to carbon deflagration of white dwarfs (type I) or the core
collapse of massive stars (type II) but we will follow the dynamical evolution
of the supernova remnant (SNR), i.e. the expanding cloud of hot gas in the
ISM. This evolution can be divided into different phases according to the
dominant physical processes, and simplified models can be made at least for
the first stages, to get an idea of typical time scales, expansion velocities
and sizes. Free Expansion Phase The shock wave created by the explosion moves
outwards into the (more or less homo-geneous) interstellar gas at highly
supersonic speed. During the first phase of the SNR evolution the surrounding
ISM has no influence on the expansion of the shock wave, i.e. the pressure of
the interstellar gas is negligible. Assuming that most of the supernova energy
E SN (on the order of 10 44, author = Susanne, H, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Susanne - 2010 - Dynamical Evolution of Supernova Remnants
Lecture Notes.pdf:pdf, pages = 1–4, title = Dynamical Evolution of Supernova
Remnants Lecture Notes, year = 2010 @articleSalome2016, abstract = NGC 5128
(Centaurus A) is one of the best example to study AGN-feedback in the local
Universe. At 13.5 kpc from the galaxy, optical filaments with recent star
formation are lying along the radio-jet direction. We used the Atacama
Pathfinder EXperiment (APEX) to map the CO(2-1) emission all along the
filaments structure. Molecular gas mass of (8.2 ± 0.5) × 107 M$\alpha$ was
found over the 4.2 kpc-structure which represents about 3% of the total gas
mass of the NGC 5128 cold gas content. Two dusty mostly molecular structures
are identified, following the optical filaments. The region corresponds to the
crossing of the radio jet with the northern H i shell, coming from a past
galaxy merger. One filament is located at the border of the H i shell, while
the other is entirely molecular, and devoid of H i gas. The molecular mass is
comparable to the H i mass in the shell, suggesting a scenario where the
atomic gas was shocked and transformed in molecular clouds by the radio jet.
Comparison with combined far-IR Herschel and UV GALEX estimation of star
formation rates in the same regions leads to depletion times of more than 10
Gyr. The filaments are thus less efficient than discs in converting molecular
gas into stars. Kinetic energy injection triggered by shocks all along the jet
and gas interface is a possible process that appears to be consistent with
MUSE line ratio diagnostics derived in a smaller region of the northern
filaments. Whether the AGN is the sole origin of this energy input and what is
the dominant (mechanical vs. radiative) mode for this process is however still
to be investigated., author = Salomé, Q. and Salomé, P. and Combes, F. and
Hamer, S., doi = 10.1051/0004-6361/201628970, file =
:home/william/Documents/Papers/[Salome et al.]-Star formation efficiency along
the radio jet in Centaurus A.pdf:pdf, issn = 14320746, journal = Astron.
Astrophys., keywords = Galaxies: evolution,Galaxies: individual: Centaurus
A,Galaxies: interactions,Galaxies: star formation,Methods: data analysis,Radio
lines: galaxies, pages = 1–13, title = Atomic-to-molecular gas phase
transition triggered by the radio jet in Centaurus A, volume = 595, year =
2016 @articleTombesi2012a, abstract = Using the results of a previous X-ray
photo-ionization modelling of blue-shifted Fe K absorption lines on a sample
of 42 local radio-quiet AGNs observed with XMM-Newton, in this letter we
estimate the location and energetics of the associated ultra-fast outflows
(UFOs). Due to significant uncertainties, we are essentially able to place
only lower/upper limits. On average, their location is in the interval
~0.0003-0.03pc (~10^2-10^4 r_s) from the central black hole, consistent with
what is expected for accretion disk winds/outflows. The mass outflow rates are
constrained between ~0.01-1 M_{$\backslash$odot} yr^{-1}, corresponding to
5-10% of the accretion rates. The average lower-upper limits on the mechanical
power are log$\backslash$dot{E}_K~42.6-44.6 erg s^{-1}. However, the minimum
possible value of the ratio between the mechanical power and bolometric
luminosity is constrained to be comparable or higher than the minimum required
by simulations of feedback induced by winds/outflows. Therefore, this work
demonstrates that UFOs are indeed capable to provide a significant
contribution to the AGN cosmological feedback, in agreement with theoretical
expectations and the recent observation of interactions between AGN outflows
and the interstellar medium in several Seyferts galaxies., author = Tombesi,
F. and Cappi, M. and Reeves, J. N. and Braito, V., doi =
10.1111/j.1745-3933.2012.01221.x, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Tombesi et al. - 2012 - Evidence for ultrafast outflows in
radio-quiet AGNs – III . Location and energetics.pdf:pdf, isbn = 0306090201,
issn = 17453933, journal = Mon. Not. R. Astron. Soc. Lett., keywords =
Accretion,Accretion discs,Black hole physics,Galaxies: active,X-rays:
galaxies, number = 1, title = Evidence for ultrafast outflows in radio-quiet
AGNs - III. Location and energetics, volume = 422, year = 2012
@articleIshibashi2015, abstract = Galaxy-scale outflows, which are thought to
provide the link connecting the central black hole to its host galaxy, are now
starting to be observed. However, the physical origin of the mechanism driving
the observed outflows, whether due to energy-driving or radiation-driving, is
still debated; and in some cases, it is not clear whether the central source
is an active galactic nucleus (AGN) or a nuclear starburst. Here we study the
role of radiation pressure on dust in driving galactic-scale AGN outflows, and
analyse the dynamics of the outflowing shell as a function of the underlying
physical parameters. We show that high-velocity outflows ($$1000 km/s) with
large momentum flux ($10 L/c$) can be obtained, by taking into account the
effects of radiation trapping. In particular, the high observed values of the
momentum boosts can be reproduced, provided that the shell is initially
optically thick to the reprocessed infrared radiation. Alternatively, the
inferred measurements of the momentum flux may be significantly biased by AGN
variability. In this context, the observations of powerful outflows on
kiloparsec scales, with no or weak signs of ongoing nuclear activity at the
present time, could be re-interpreted as relics of past AGN episodes.,
archivePrefix = arXiv, arxivId = 1504.07393, author = Ishibashi, W. and
Fabian, A. C., doi = 10.1093/mnras/stv944, eprint = 1504.07393, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Ishibashi, Fabian - 2015 - AGN feedback Galactic-scale
outflows driven by radiation pressure on dust.pdf:pdf, isbn =
bibcode:2015arXiv150407393I, issn = 13652966, journal = Mon. Not. R. Astron.
Soc., keywords = Black hole physics,Galaxies: active,Galaxies:
evolution,Radiation: dynamics, number = 1, pages = 93–102, title = AGN
feedback: Galactic-scale outflows driven by radiation pressure on dust, volume
= 451, year = 2015

@ARTICLEMorganti2015, author = Morganti, Raffaella and Oosterloo, Tom and
Oonk, J. B. Raymond and Frieswijk, Wilfred and Tadhunter, Clive, title = ”The
fast molecular outflow in the Seyfert galaxy IC 5063 as seen by ALMA”, journal
= , keywords = galaxies: active, galaxies: individual: IC 5063, ISM: jets and
outflows, radio lines: galaxies, Astrophysics - Astrophysics of Galaxies, year
= 2015, month = aug, volume = 580, eid = A1, pages = A1, doi =
10.1051/0004-6361/201525860, archivePrefix = arXiv, eprint = 1505.07190,
primaryClass = astro-ph.GA, adsurl =
https://ui.adsabs.harvard.edu/abs/2015A&A…580A…1M, adsnote = Provided by the
SAO/NASA Astrophysics Data System

@articleGan2014a, abstract = Based on two-dimensional high-resolution
hydrodynamic numerical simulation, we study the mechanical and radiative
feedback effects from the central active galactic nucleus (AGN) on the
cosmological evolution of an isolated elliptical galaxy. The inner boundary of
the simulation domain is carefully chosen so that the fiducial Bondi radius is
resolved and the accretion rate of the black hole is determined self-
consistently. It is well known that when the accretion rates are high and low,
the central AGNs will be in cold and hot accretion modes, which correspond to
the radiative and kinetic feedback modes, respectively. The emitted spectrum
from the hot accretion flows is harder than that from the cold accretion
flows, which could result in a higher Compton temperature accompanied by a
more efficient radiative heating, according to previous theoretical works.
Such a difference of the Compton temperature between the two feedback modes,
the focus of this study, has been neglected in previous works. Significant
differences in the kinetic feedback mode are found as a result of the stronger
Compton heating. More importantly, if we constrain models to correctly predict
black hole growth and AGN duty cycle after cosmological evolution, we find
that the favored model parameters are constrained: mechanical feedback
efficiency diminishes with decreasing luminosity (the maximum efficiency being
~= 10-3.5), and X-ray Compton temperature increases with decreasing
luminosity, although models with fixed mechanical efficiency and Compton
temperature can be found that are satisfactory as well. We conclude that
radiative feedback in the kinetic mode is much more important than previously
thought., archivePrefix = arXiv, arxivId = 1403.0670, author = Gan, Zhaoming
and Yuan, Feng and Ostriker, Jeremiah P and Ciotti, Luca and Novak, Gregory S,
doi = 10.1088/0004-637X/789/2/150, eprint = 1403.0670, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley Desktop/Downloaded/Gan
et al. - 2014 - Active galactic nucleus feedback in an isolated elliptical
galaxy The effect of strong radiative feedback in the kin.pdf:pdf, issn =
15384357, journal = Astrophys. J., keywords = accretion,accretion disks,black
hole physics,cD,galaxies: active,galaxies: elliptical and lenticular,galaxies:
evolution,galaxies: nuclei, number = 2, pages = 14, title = Active galactic
nucleus feedback in an isolated elliptical galaxy: The effect of strong
radiative feedback in the kinetic mode, volume = 789, year = 2014
@articleBlandford2019a, abstract = The nuclei of most normal galaxies contain
supermassive black holes, which can accrete gas through a disk and become
active. These active galactic nuclei (AGNs) can form jets that are observed on
scales from astronomical units to megaparsecs and from meter wavelengths to
TeV energies. High-resolution radio imaging and multiwavelength/messenger
campaigns are elucidating the conditions under which this happens. Evidence is
presented that: □ Relativistic AGN jets are formed when the black hole spins
and the the accretion disk is strongly magnetized, perhaps on account of gas
accreting at high latitude beyond the black hole sphere of influence. □ AGN
jets are collimated close to the black hole by magnetic stress associated with
a disk wind. □ Higher-power jets can emerge from their galactic nuclei in a
relativistic, supersonic, and proton-dominated state, and they terminate in
strong, hot spot shocks; lower-power jets are degraded to buoyant plumes and
bubbles. □ Jets may accelerate protons to EeV energies, which contribute to
the cosmic ray spectrum and may initiate pair cascades that can efficiently
radiate synchrotron $\gamma$-rays. □ Jets were far more common when the
Universe was a few billion years old and black holes and massive galaxies were
growing rapidly. □ Jets can have a major influence on their environments,
stimulating and limiting the growth of galaxies. The observational prospects
for securing our understanding of AGN jets are bright., archivePrefix = arXiv,
arxivId = 1812.06025, author = Blandford, Roger and Meier, David and Readhead,
Anthony, doi = 10.1146/annurev-astro-081817-051948, eprint = 1812.06025, file
= :home/william/Documents/Papers/1812.06025.pdf:pdf, issn = 00664146, journal
= Annu. Rev. Astron. Astrophys., keywords = active galactic nuclei,black
holes,blazars,extragalactic radio sources,jets,$\gamma$-ray sources, pages =
467–509, title = Relativistic Jets from Active Galactic Nuclei, volume = 57,
year = 2019 @articleLehnert2009, abstract = We analyze the physical conditions
in the interstellar gas of 11 actively star-forming galaxies at z2, based on
integral-field spectroscopy from the ESO-VLT and Hubble Space Telescope/Near
Infrared Camera and Multi-Object Spectrometer imaging. We concentrate on the
high H$\alpha$ surface brightnesses, large line widths, line ratios, and the
clumpy nature of these galaxies. We show that photoionization calculations and
emission line diagnostics imply gas pressures and densities that are similar
to the most intense nearby star-forming regions at z = 0 but over much larger
scales (10-20 kpc). A relationship between surface brightness and velocity
dispersion can be explained through simple energy injection arguments and a
scaling set by nearby galaxies with no free parameters. The high velocity
dispersions are a natural consequence of intense star formation thus regions
of high velocity dispersion are not evidence for mass concentrations such as
bulges or rings. External mechanisms such as cosmological gas accretion
generally do not have enough energy to sustain the high velocity dispersions.
In some cases, the high pressures and low gas metallicites may make it
difficult to robustly distinguish between active galactic nucleus ionization
cones and star formation, as we show for BzK-15504 at z = 2.38. We construct a
picture where the early stages of galaxy evolution are driven by self-gravity
which powers strong turbulence until the velocity dispersion is high. Then
massive, dense, gas-rich clumps collapse, triggering star formation with high
efficiencies and intensities as observed. At this stage, the intense star
formation is likely self-regulated by the mechanical energy output of massive
stars. 2009. The American Astronomical Society. All rights reserved., author =
Lehnert, M. D. and Nesvadba, N. P.H. and Tiran, L. Le and Matteo, P. Di and
Van Driel, W. and Douglas, L. S. and Chemin, L. and Bournaud, F., doi =
10.1088/0004-637X/699/2/1660, file =
:home/william/Documents/Papers/Lehnert_2009_ApJ_699_1660.pdf:pdf, issn =
15384357, journal = Astrophys. J., keywords = Cosmology:
observations,Galaxies: evolution,Galaxies: kinematics and dynamics,Infrared:
galaxies, number = 2, pages = 1660–1678, title = Physical conditions in the
interstellar medium of intensely star-forming galaxies at redshift ∼ 2, volume
= 699, year = 2009 @articleDraine2003, abstract = This review surveys the
observed properties of interstellar dust grains: the wavelength-dependent
extinction of starlight, including absorption features, from UV to IR; optical
luminescence; IR emission; microwave emission; optical, UV, and X-ray
scattering by dust; and polarization of starlight and of infrared emission.
The relationship between presolar grains in meteorites and the interstellar
grain population is discussed. Candidate grain materials and abundance
constraints are considered. A dust model consisting of amorphous silicate
grains, graphite grains, and PAHs is compared with observed emission and
scattering. Some issues concerning evolution of interstellar dust are
discussed., archivePrefix = arXiv, arxivId = astro-ph/0304489, author =
Draine, B.T., doi = 10.1146/annurev.astro.41.011802.094840, eprint = 0304489,
file = :home/william/Documents/Papers/0304489.pdf:pdf, issn = 0066-4146,
journal = Annu. Rev. Astron. Astrophys., keywords = infrared
astronomy,interstellar grains,interstellar medium,light scattering, number =
1, pages = 241–289, primaryClass = astro-ph, title = Interstellar Dust Grains,
volume = 41, year = 2003 @articleCrocker2011, abstract = Recently evidence has
emerged for enormous features in the gamma-ray sky observed by the Fermi-LAT
instrument: bilateral ‘bubbles’ of emission centered on the core of the Galaxy
and extending to around 10 kpc above and below the Galactic plane. These
structures are coincident with a non-thermal microwave ‘haze’ found in WMAP
data and an extended region of X-ray emission detected by ROSAT. The bubbles’
gamma-ray emission is characterised by a hard and relatively uniform spectrum,
relatively uniform intensity, and an overall luminosity ~4 x 10^37 erg/s,
around one order of magnitude larger than their microwave luminosity while
more than order of magnitude less than their X-ray luminosity. Here we show
that the bubbles are naturally explained as due to a population of relic
cosmic ray protons and heavier ions injected by processes associated with
extremely long timescale (~8 Gyr) and high areal density star-formation in the
Galactic center., author = Crocker, Roland M. and Aharonian, Felix, doi =
10.1103/PhysRevLett.106.101102, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Crocker, Aharonian - 2011 - Fermi bubbles Giant,
multibillion-year-old reservoirs of galactic center cosmic rays.pdf:pdf, issn
= 10797114, journal = Phys. Rev. Lett., number = 10, pages = 1–4, title =
Fermi bubbles: Giant, multibillion-year-old reservoirs of galactic center
cosmic rays, volume = 106, year = 2011 @articleMorganti2017c, abstract =
Analytical and numerical galaxy-formation models indicate that active galactic
nuclei (AGNs) likely play a prominent role in the formation and evolution of
galaxies. However, quantifying this effect requires knowledge of how the
nuclear activity proceeds throughout the life of a galaxy, whether it
alternates with periods of quiescence and, if so, on what timescales these
cycles occur. This topic has attracted growing interest, but making progress
remains a challenging task. For optical and radio AGNs, a variety of
techniques are used to perform a kind of ’archaeology’ that traces the
signatures of past nuclear activity. Here we summarize recent findings
regarding the lifecycle of an AGN from optical and radio observations. The
limited picture we have so far suggests that these cycles can range from long
periods of 107-108 yr to shorter periods of 104-105 yr, even reaching extreme
events on timescales of just a few years. Together with simulations,
observational results regarding the multiple cycles of AGN activity help to
create a complete picture of the AGN lifecycle., archivePrefix = arXiv,
arxivId = 1709.01667, author = Morganti, Raffaella, doi =
10.1038/s41550-017-0223-0, eprint = 1709.01667, file =
:home/william/Documents/Papers/[Morganti, Raffaela]arqueology of AGNs.pdf:pdf,
issn = 23973366, journal = Nat. Astron., number = 9, pages = 596–605, title =
Archaeology of active galaxies across the electromagnetic spectrum, volume =
1, year = 2017 @articleDeBoer2014, abstract = The diffuse gamma-ray sky
revealed ’Bubbles’ of emission above and below the Galactic Plane symmetric
around the centre of the Milky Way with a height of 10 kpc in both directions.
At present there is no convincing explanation for the origin. To understand
the role of the Galactic Centre (GC) one has to study the Bubble spectrum
inside the disc, a region which has been excluded from previous analysis
because of the large foreground. From a novel template fit, which allows a
simultaneous determination of the signal and foreground in any direction, we
find that bubble-like emission is not only found in the halo, but in the
Galactic Plane as well with a width in latitude coinciding with the molecular
clouds. The longitude distribution has a width corresponding to the Galactic
Bar with an additional contribution from the Scutum-Centaurus arm. The energy
spectrum of the Bubbles coincides with the predicted contribution from CRs
trapped in sources (SCRs). Also the energetics fits well. Hence, we conclude
that the bubble-like emission has a hadronic origin, which arises from SCRs
and the Bubbles in the halo arise from hadronic interactions in advected gas.
Evidence for advection is provided by the ROSAT X-rays from hot gas in the
Bubble region., author = De Boer, Wim and Weber, Markus, doi =
10.1088/2041-8205/794/1/L17, file = :home/william/.local/share/data/Mendeley
Ltd./Mendeley Desktop/Downloaded/De Boer, Weber - 2014 - Fermi bubbles and
bubble-like emission from the galactic plane.pdf:pdf, issn = 20418213, journal
= Astrophys. J. Lett., keywords = Galaxy: structure,acceleration of
particles,gamma rays: ISM,gamma rays: diffuse background,methods:
numerical,shock waves, number = 1, pages = 1–6, title = Fermi bubbles and
bubble-like emission from the galactic plane, volume = 794, year = 2014
@articleDeAvillez2004a, abstract = The role of matter circulation between the
disk and halo in establishing the volume filling factors of the different ISM
phases in the Galactic disk (—z— ≤ 250 pc) is investigated, using a modified
version of the three-dimensional supernova-driven ISM model of Avillez (2000).
We carried out adaptive mesh refinement simulations of the ISM with five
supernova rates (in units of the Galactic value), $\sigma$/$\sigma$Gal = 1, 2,
4, 8 and 16 (corresponding to starburst conditions) using three finer level
resolutions of 2.5, 1.25 and 0.625 pc, allowing us to understand how
resolution would affect the volumes of gas phases in pressure equilibrium. We
find that the volume filling factors of the different ISM phases depend
sensitively on the existence of a duty cycle between the disk and halo acting
as a pressure release valve for the hot (T 105.5 K) phase in the disk. The
amount of cold gas (defined as the gas with T 103 K) picked up in the
simulations varies from a value of 19% for $\sigma$/$\sigma$Gal = 1 to ∼5% for
$\sigma$/$\sigma$Gal = 4 and ≤1% for higher SN rates. Background heating
prevents the cold gas from immediate collapse and thus ensures the stability
of the cold gas phase. The mean occupation fraction of the hot phase varies
from about 17% for the Galactic SN rate to ∼28%, for $\sigma$/$\sigma$Gal = 4,
and to 44% for $\sigma$/$\sigma$Gal = 16. Overall the filling factor of the
hot gas does not increase much as we move towards higher SN rates, following a
power law of fv,hot∝ ($\sigma$/$\sigma$Gal)0.363, Such a modest dependence on
the SN rate is a consequence of the evacuation of the hot phase into the halo
through the duty cycle. This leads to volume filling factors of the hot phase
considerably smaller than those predicted in the three-phase model of McKee &
Ostriker (1977) even in the absence of magnetic fields., archivePrefix =
arXiv, arxivId = astro-ph/0407034, author = De Avillez, M. A. and
Breitschwerdt, D., doi = 10.1051/0004-6361:200400025, eprint = 0407034, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley Desktop/Downloaded/De
Avillez, Breitschwerdt - 2004 - Volume filling factors of the ISM phases in
star forming galaxies I. The role of the disk-halo intera.pdf:pdf, issn =
00046361, journal = Astron. Astrophys., keywords = Galaxies: Ism,Galaxies:
Kinematics and dynamics,ISM: Structure, number = 3, pages = 899–911,
primaryClass = astro-ph, title = Volume filling factors of the ISM phases in
star forming galaxies I. The role of the disk-halo interaction, volume = 425,
year = 2004 @articleSilantev2009, abstract = We consider the integral light
polarization from optically thick accretion disks. Basic mechanism is the
multiple light scattering on free electrons (Milne’s problem) in magnetized
atmosphere. The Faraday rotation of the polarization plane changes both the
value of integral polarization degree $p$ and the position angle $$. Besides,
the characteristic spectra of these values appear. We are testing the known
relation between magnetic field of black hole at the horizon $B_{BH}$ and its
mass $M_{BH}$, and the usual power-law distribution inside the accretion disk.
The formulae for $p()$ and $()$ depend on a number of parameters describing
the particular dependence of magnetic field in accretion disk (the index of
power-law distribution, the spin of the black hole, etc.). Comparison of our
theoretical values of $p$ and $$ with observed polarization can help us to
choice more realistic values of parameters if the accretion disk mechanism
gives the main contribution to the observed integral polarization. The main
content is connected with estimation of validity of the relation between
$B_{BH}$ and $M_{BH}$. We found for the AGN NGC 4258 that such procedure does
not confirm the mentioned correlation between magnetic field and mass of black
hole., archivePrefix = arXiv, arxivId = 0908.2725, author = Silant’ev, N. A.
and Piotrovich, M Yu and Gnedin, Yu N and Natsvlishvili, T M, eprint =
0908.2725, file = :home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Silant et al. - 2018 - THE BLACK HOLE MASS AND MAGNETIC
FIELD CORRELATION IN AGN TESTING BY OPTICAL POLARIMETRY.pdf:pdf, keywords =
accretion disks m edd,are the ordinary and,eddington accretion
rates,polarization - magnetic fields,respec-, title = The Black Hole Mass and
Magnetic Field Correlation in AGN: Testing by Optical Polarimetry, url =
http://arxiv.org/abs/0908.2725, year = 2009 @articleMorganti2017b, abstract =
The energy released by Active Galactic Nuclei (AGN) in the form of radiation,
winds, or radio plasma jets, is known to impact on the surrounding
interstellar medium. The result of these processes, known as AGN (negative)
feedback, is suggested to prevent gas, in and around galaxies, from cooling,
and to remove, or at least redistribute, gas by driving massive and fast
outflows, hence playing a key role in galaxy evolution. Given its importance,
a large effort is devoted by the astronomical community to trace the effects
of AGN on the surrounding gaseous medium and to quantify their impact for
different types of AGN. This review briefly summarizes some of the recent
observational results obtained in different wavebands, tracing different
phases of the gas. I also summarize the new insights they have brought, and
the constraints they provide to numerical simulations of galaxy formation and
evolution. The recent addition of deep observations of cold gas and, in
particular, of cold molecular gas, has brought some interesting surprises and
has expanded our understanding of AGN and AGN feedback., archivePrefix =
arXiv, arxivId = 1712.05301, author = Morganti, Raffaella, doi =
10.3389/fspas.2017.00042, eprint = 1712.05301, file =
:home/william/Documents/Papers/fspas-04-00042.pdf:pdf, issn = 2296987X,
journal = Front. Astron. Sp. Sci., keywords = active galactic