Kelvin-Helmholtz (KH) instability (KHI) results in an unavoidable catastrophe
of the disc developed at the interface between the reversely rotating parts,
and demonstrate that a close binary of supermassive black holes provides tidal
torques as the unique external sources to prevent the disc from the KH
catastrophe. We are led to the inescapable conclusion that there must be a
binary black hole at the center of NGC 1068, to prevent it from the KH
catastrophe. The binary is composed of black holes with a separation of
$0.1\,$pc from GRAVITY/VLTI observations, a total mass of $1.310^{7}\:M_{}$
and a mass ratio of $0.3$ estimated from the angular momentum budge of the
global system. The KHI gives rise to forming a gap without cold gas at the
velocity interface which overlaps with the observed gap of hot and cold dust
regions. Releases of kinematic energies from the KHI of the disc are in
agreement with observed emissions in radio and $$-rays. Such a binary is
shrinking with a timescale much longer than the local Hubble time via
gravitational waves, however, the KHI leads to an efficient annihilation of
the orbital angular momentum and speed up merge of the binary, providing a new
paradigm of solving the long term issue of ”final parsec problem”. Future
observations of GRAVITY+/VLTI are expected to be able to spatially resolve the
CB-SMBHs suggested in this paper., archivePrefix = arXiv, arxivId =
2005.01220, author = Wang, J. -M. and Songsheng, Y. -Y. and Li, Y. -R. and Du,
P. and Zhe, Y., eprint = 2005.01220, file =
:home/william/Documents/Papers/[Wang et al.]-Dynamical evidence of the sub-
parsec counter-rotating disc for a.pdf:pdf, keywords = accretion,accretion
discs,active,binary,black holes,galaxies, number = May, title = Dynamical
evidence of the sub-parsec counter-rotating disc for a close binary of
supermassive black holes in the nucleus of NGC 1068, url =
http://arxiv.org/abs/2005.01220, year = 2020 @articleMukherjee2016, abstract =
We present the results of three dimensional relativistic hydrodynamic
simulations of interaction of AGN jets with a dense turbulent two-phase
interstellar medium, which would be typical of high redshift galaxies. We
describe the effect of the jet on the evolution of the density of the
turbulent ISM. The jet driven energy bubble affects the gas to distances up to
several kiloparsecs from the injection region. The shocks resulting from such
interactions create a multi-phase ISM and radial outflows. One of the striking
result of this work is that low power jets (P_jet 10^{43} erg/s) although less
efficient in accelerating clouds, are trapped in the ISM for a longer time and
hence affect the ISM over a larger volume. Jets of higher power drill through
with relative ease. Although the relativistic jets launch strong outflows,
there is little net mass ejection to very large distances, supporting a
galactic fountain scenario for local feedback., archivePrefix = arXiv, arxivId
= 1606.01143, author = Mukherjee, Dipanjan and Bicknell, Geoffrey V. and
Sutherland, Ralph and Wagner, Alex, doi = 10.1093/mnras/stw1368, eprint =
1606.01143, file = :home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Mukherjee et al. - 2016 - Relativistic jet feedback in
high-redshift galaxies - I. Dynamics.pdf:pdf, issn = 13652966, journal = Mon.
Not. R. Astron. Soc., keywords = Galaxies: ISM,Galaxies: evolution,Galaxies:
highredshift,Galaxies: jets,Hydrodynamics,Methods: numerical, number = 1,
pages = 967–983, title = Relativistic jet feedback in high-redshift galaxies -
I. Dynamics, volume = 461, year = 2016 @articleRiffel2011a, abstract = We have
mapped the stellar and gaseous kinematics, as well as the emission-line flux
distributions and ratios, from the inner ≈450pc radius of the Seyfert 2 galaxy
Mrk1157, using two-dimensional near-infrared J- and K l-band spectra obtained
with the Gemini Near-Infrared Integral-Field Spectrograph instrument at a
spatial resolution of ≈35pc and velocity resolution of ≈40kms -1. The stellar
velocity field shows a rotation pattern, with a discrete S-shaped zero
velocity curve - a signature of a nuclear bar. The presence of a bar is also
supported by the residual map between the observed rotation field and a model
of circular orbits in a Plummer potential. The stellar velocity dispersion
($\sigma$ *) map presents a partial ring of low-$\sigma$ * values (50-60kms
-1) at 250pc from the nucleus surrounded by higher $\sigma$ * values from the
galaxy bulge. We propose that this ring has origin in kinematically colder
regions with recent star formation. The stellar velocity dispersion of the
bulge (100kms -1) implies in a black hole mass of M BH= 8.3 +3.2- 2.2× 10 6M
⊙. Emission-line flux distributions are most extended along the position angle
PA = 27°/153°, reaching at least 450pc from the nucleus and following the
orientation observed in previous optical emission-line [Oiii] imaging and
radio jets. The molecular hydrogen gas has an excitation temperature T exc≈
2300K and its emission is dominated by thermal processes, mainly due to X-ray
heating by the active nucleus, with a possible small contribution from shocks
produced by the radio jet. The [Feii] excitation has a larger contribution
from shocks produced by the radio jet, as evidenced by the line-ratio maps and
velocity dispersion maps, which show spatial correlation with the radio
structures. The coronal lines are resolved, extending up to ≈150pc and are
also slightly more extended along PA = 27°/153°. The gaseous kinematics show
two components: one due to the gas located in the galaxy plane, in similar
rotation to that of the stars, and another in outflow, which is oriented close
to the plane of the sky, thus extending to high latitudes, as the galaxy plane
is inclined by ≈45° relative to the plane of the sky. The gas rotating in the
plane dominates the H 2 and Pa$\beta$ emission, while the gas in outflow is
observed predominantly in [Feii] emission. The [Feii] emission is originated
in gas being pushed by the radio jet, which destroys dust grains, releasing
Fe. From the outflow velocities and implied geometry, we estimate a mass-
outflow rate of for the ionized gas and a kinetic power for the outflow of.
The distinct flux distributions and kinematics of the H 2- and [Feii]-emitting
gas, with the former more restricted to the plane of the galaxy and the latter
tracing the outflows related to radio jets, are a common characteristic of six
Seyfert galaxies (ESO428-G14, NGC4051, 7582 and4151, Mrk1066, and now Mrk1157)
we have studied so far using similar two-dimensional observations and other
two (Circinus and NGC2110) using long-slit observations. We conclude that the
H 2 emission surrounding the nucleus in the galaxy plane is a tracer of the
gas feeding to the active nucleus, while the [Feii] emission is a tracer of
its feedback. 2011 The Authors Monthly Notices of the Royal Astronomical
Society 2011 RAS., archivePrefix = arXiv, arxivId = 1107.2564, author =
Riffel, Rogemar A. and Storchi-Bergmann, Thaisa, doi =
10.1111/j.1365-2966.2011.19441.x, eprint = 1107.2564, file =
:home/william/Documents/Papers/mnras0417-2752.pdf:pdf, issn = 00358711,
journal = Mon. Not. R. Astron. Soc., keywords = Galaxies: ISM,Galaxies:
Seyfert,Galaxies: individual: Mrk1157,Galaxies: individual: NGC591,Galaxies:
kinematics and dynamics,Infrared: galaxies, number = 4, pages = 2752–2769,
title = Feeding and feedback in the active nucleus of Mrk 1157 probed with the
Gemini Near-Infrared Integral-Field Spectrograph, volume = 417, year = 2011
@articleGabuzda, abstract = Long-lived, stable jets are observed in a wide
variety of systems, from protostars, through Galactic compact objects to
active galactic nuclei (AGN). Magnetic fields play a central role in
launching, accelerating, and collimating the jets through various media. The
termination of jets in molecular clouds or the interstellar medium deposits
enormous amounts of mechanical energy and momentum, and their interactions
with the external medium, as well, in many cases, as the radiation processes
by which they are observed, are intimately connected with the magnetic fields
they carry. This review focuses on the properties and structures of magnetic
fields in long-lived jets, from their launch from rotating magnetized young
stars, black holes, and their accretion discs, to termination and beyond. We
compare the results of theory, numerical simulations, and observations of
these diverse systems and address similarities and differences between
relativistic and non-relativistic jets in protostellar versus AGN systems. On
the observational side, we focus primarily on jets driven by AGN because of
the strong observational constraints on their magnetic field properties, and
we discuss the links between the physics of these jets on all scales. 2012
Springer Science+Business Media B.V., archivePrefix = arXiv, arxivId =
1205.2073, author = Pudritz, Ralph E. and Hardcastle, Martin J. and Gabuzda,
Denise C, doi = 10.1007/s11214-012-9895-z, eprint = 1205.2073, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Gabuzda, May - Unknown - Magnetic Fields in Astrophysical
Jets From Launch to Termination.pdf:pdf, issn = 00386308, journal = Space Sci.
Rev., keywords = Jets,Magnetic fields,Polarization,Radio continuum:
galaxies,X-rays: galaxies, number = 1-4, pages = 27–72, title = Magnetic
fields in astrophysical jets: From launch to termination, volume = 169, year =
2012 @article2010A&A…521A..57T, archivePrefix = arXiv, arxivId = astro-
ph.HE/1006.2858, author = Tombesi, F and Cappi, M and Reeves, J.~N. and
Palumbo, G.~G.~C. and Yaqoob, T and Braito, V and Dadina, M, doi =
10.1051/0004-6361/200913440, eprint = 1006.2858, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Tombesi et al. - 2010 - Evidence for ultra-fast outflows in
radio-quiet AGNs I . Detection and statistical incidence of Fe K-shell
absor.pdf:pdf, journal = aap, keywords = X-ray: galaxies,black hole
physics,galaxies: Seyfert,line: identification, pages = A57, primaryClass =
astro-ph.HE, title = Evidence for ultra-fast outflows in radio-quiet AGNs. I.
Detection and statistical incidence of Fe K-shell absorption lines, volume =
521, year = 2010

@ARTICLENetzer2015, author = Netzer, Hagai, title = ”Revisiting the Unified
Model of Active Galactic Nuclei”, journal = , keywords = Astrophysics -
Astrophysics of Galaxies, year = 2015, month = aug, volume = 53, pages =
365-408, doi = 10.1146/annurev-astro-082214-122302, archivePrefix = arXiv,
eprint = 1505.00811, primaryClass = astro-ph.GA, adsurl =
https://ui.adsabs.harvard.edu/abs/2015ARA&A..53..365N, adsnote = Provided by
the SAO/NASA Astrophysics Data System

@articleGnat2007, abstract = We present new computations of the equilibrium
and non-equilibrium cooling efficiencies and ionization states for low-density
radiatively cooling gas containing cosmic abundances of the elements H, He, C,
N, O, Ne, Mg, Si, S, and Fe. We present results for gas temperatures between
1e4 and 1e8 K, assuming dust-free and optically thin conditions, and no
external radiation. For non-equilibrium cooling we solve the coupled time-
dependent ionization and energy loss equations for a radiating gas cooling
from an initially hot, 5e6K equilibrium state, down to 1e4K. We present
results for heavy element compositions ranging from 1e-3 to 2 times the
elemental abundances in the Sun. We consider gas cooling at constant density
(isochoric) and at constant pressure (isobaric). We calculate the critical
column densities and temperatures at which radiatively cooling clouds make the
dynamical transition from isobaric to isochoric evolution. We construct ion
ratio diagnostics for the temperature and metallicity in radiatively cooling
gas. We provide numerical estimates for the maximal cloud column densities for
which the gas remains optically thin to the cooling radiation. We present our
computational results in convenient on-line figures and tables (see
http://wise-obs.tau.ac.il/~orlyg/cooling/)., archivePrefix = arXiv, arxivId =
astro-ph/0608181, author = Gnat, Orly and Sternberg, Amiel, doi =
10.1086/509786, eprint = 0608181, file =
:home/william/Documents/Papers/Gnat_2007_ApJS_168_213.pdf:pdf, issn =
0067-0049, journal = Astrophys. J. Suppl. Ser., number = 2, pages = 213–230,
primaryClass = astro-ph, title = Time‐dependent Ionization in Radiatively
Cooling Gas, volume = 168, year = 2007 @articleLeighly2016, abstract = Mrk 231
is a nearby quasar with an unusually red near-UV-to-optical continuum,
generally explained as heavy reddening by dust (e.g., Leighly et al. 2014).
Yan et al. 2015 proposed that Mrk~231 is a milli-parsec black-hole binary with
little intrinsic reddening. We show that if the observed FUV continuum is
intrinsic, as assumed by Yan et al. 2015, it fails by a factor of about 100 in
powering the observed strength of the near-infrared emission lines, and the
thermal near and mid-infrared continuum. In contrast, the line and continuum
strengths are typical for a reddened AGN spectral energy distribution. We find
that the HeI*/Pbeta ratio is sensitive to the spectral energy distribution for
a one-zone model. If this sensitivity is maintained in general broad-line
region models, then this ratio may prove a useful diagnostic for heavily
reddened quasars. Analysis of archival HST STIS and FOC data revealed evidence
that the far-UV continuum emission is resolved on size scales of ~40 parsecs.
The lack of broad absorption lines in the far-UV continuum might be explained
if it were not coincident with the central engine. One possibility is that it
is the central engine continuum reflected from the receding wind on the far
side of the quasar., archivePrefix = arXiv, arxivId = 1604.03456, author =
Leighly, Karen M. and Terndrup, Donald M. and Gallagher, Sarah C. and Lucy,
Adrian B., doi = 10.3847/0004-637x/829/1/4, eprint = 1604.03456, file =
:home/william/Documents/Papers/Leighly_2016_ApJ_829_4.pdf:pdf, issn =
0004-637X, journal = Astrophys. J., keywords = accretion,accretion
disks,accretion, accretion disks,emission lines,individual,mrk
231,quasars,quasars: emission lines,quasars: individual (Mrk 231),quasars:
supermassive black holes,supermassive black holes, number = 1, pages = 4,
publisher = IOP Publishing, title = the Binary Black Hole Model for Mrk 231
Bites the Dust, url = http://dx.doi.org/10.3847/0004-637X/829/1/4, volume =
829, year = 2016 @articleSturm2011, abstract = Mass outflows driven by stars
and active galactic nuclei (AGNs) are a key element in many current models of
galaxy evolution. They may produce the observed black-hole-galaxy mass
relation and regulate and quench both star formation in the host galaxy and
black hole accretion. However, observational evidence of such feedback
processes through outflows of the bulk of the star-forming molecular gas is
still scarce. Here we report the detection of massive molecular outflows,
traced by the hydroxyl molecule (OH), in far-infrared spectra of ULIRGs
obtained with Herschel-PACS as part of the SHINING key project. In some of
these objects the (terminal) outflow velocities exceed 1000kms-1, and their
outflow rates (up to 1200 M yr -1) are several times larger than their star
formation rates. We compare the outflow signatures in different types of
ULIRGs and in starburst galaxies to address the issue of the energy source
(AGN or starburst) of these outflows. We report preliminary evidence that
ULIRGs with a higher AGN luminosity (and higher AGN contribution to L IR) have
higher terminal velocities and shorter gas depletion timescales. The outflows
in the observed ULIRGs are able to expel the cold gas reservoirs from the
centers of these objects within 106-108 years. 2011. The American Astronomical
Society. All rights reserved., archivePrefix = arXiv, arxivId = 1105.1731,
author = Sturm, E. and Gonzlez-Alfonso, E. and Veilleux, S. and Fischer, J.
and Graci-Carpio, J. and Hailey-Dunsheath, S. and Contursi, A. and Poglitsch,
A. and Sternberg, A. and Davies, R. and Genzel, R. and Lutz, D. and Tacconi,
L. and Verma, A. and Maiolino, R. and De Jong, J. A., doi =
10.1088/2041-8205/733/1/L16, eprint = 1105.1731, file =
:home/william/Documents/Papers/1105.1731.pdf:pdf, issn = 20418205, journal =
Astrophys. J. Lett., keywords = Galaxies: active,ISM: jets and
outflows,galaxies: evolution,galaxies: starburst, number = 1 PART 2, pages =
1–14, title = Massive molecular outflows and negative feedback in ULIRGs
observed by herschel-pacs, volume = 733, year = 2011 @articleVanDenBosch2015,
abstract = We have conducted an optical long-slit spectroscopic survey of 1022
galaxies using the 10m Hobby-Eberly Telescope (HET) at McDonald Observatory.
The main goal of the HET Massive Galaxy Survey (HETMGS) is to find nearby
galaxies that are suitable for black hole mass measurements. In order to
measure accurately the black hole mass, one should kinematically resolve the
region where the black hole dominates the gravitational potential. For most
galaxies, this region is much less than an arcsecond. Thus, black hole masses
are best measured in nearby galaxies with telescopes that obtain high-spatial
resolution. The HETMGS focuses on those galaxies predicted to have the largest
sphere-of-influence, based on published stellar velocity dispersions or the
galaxy fundamental plane. To ensure coverage over galaxy types, the survey
targets those galaxies across a face-on projection of the fundamental plane.
We present the sample selection and resulting data products from the long-slit
observations, including central stellar kinematics and emission line ratios.
The full dataset, including spectra and resolved kinematics, is available
online. Additionally, we show that the current crop of black hole masses are
highly biased towards dense galaxies and that especially large disks and low
dispersion galaxies are under-represented. This survey provides the necessary
groundwork for future systematic black hole mass measurement campaigns.,
author = Van Den Bosch, Remco C.E. and Gebhardt, Karl and Gültekin, Kayhan and
Yildirim, Akin and Walsh, Jonelle L., doi = 10.1088/0067-0049/218/1/10, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley Desktop/Downloaded/van
den Bosch et al. - 2015 - Hunting for Supermassive Black Holes in Nearby
Galaxies With the Hobby-Eberly Telescope.pdf:pdf, issn = 00670049, journal =
Astrophys. Journal, Suppl. Ser., keywords = catalogs,galaxies: elliptical and
lenticular, cD,galaxies: spiral,galaxies: structure,quasars: supermassive
black holes,surveys, number = 1, title = Hunting for Supermassive Black Holes
in Nearby Galaxies With the Hobby-Eberly Telescope, volume = 218, year = 2015
@articleChung2009, abstract = We present 12CO J=1–0 observations of
ultraluminous infrared galaxies (ULIRGs) obtained using the Redshift Search
Receiver (RSR) on the 14-m telescope of the Five College Radio Astronomy
Observatory. The RSR is a novel, dual-beam, dual-polarization receiver
equipped with an ultra-wideband spectrometer backend that is being built as a
facility receiver for the Large Millimeter Telescope. Our sample consists of
29 ULIRGs in the redshift range of 0.04-0.11, including 10 objects with no
prior 12CO measurements. We have detected 27 systems (a detection rate of
93%), including 9 ULIRGs that are detected in CO for the first time. Our study
has increased the number of local ULIRGs with CO measurements by ~15%. The CO
line luminosity L’_CO, correlates well with far-infrared luminosity L_FIR,
following the general trend of other local ULIRGs. However, compared to
previous surveys we probe deeper into the low CO luminosity end of ULIRG
population as a single study by including a number of CO faint objects in the
sample. As a result, we find 1) a smoother transition between the ULIRG
population and local QSOs in L_FIR-L’_CO (”star formation efficiency”) space,
and 2) a broader range of L_FIR/L’_CO flux ratio (~60–1000 L_sun/[K
km/s/pc^2]) than previously reported. In our new survey, we also have found a
small number of ULIRGs with extreme L_FIR/L’_CO which had been known to be
rare. The mid-IR color and radio-excess of 56 local ULIRGs as a function of
FIR-to-CO flux ratio is examined and compared with those of spirals/starburst
galaxies and low-z QSOs. In this paper, using a large sample of local ULIRGs
we explore the origin of their current power source and potential evolution to
QSOs., archivePrefix = arXiv, arxivId = 0906.2797, author = Chung, Aeree and
Narayanan, Gopal and Yun, Min S. and Heyer, Mark and Erickson, Neal R., doi =
10.1088/0004-6256/138/3/858, eprint = 0906.2797, file =
:home/william/Documents/Papers/0906.2797.pdf:pdf, issn = 0004-6256, journal =
Astron. J., number = 3, pages = 858–872, title = the Redshift Search Receiver
Observations of 12 Co J = 1 → 0 in 29 Ultraluminous Infrared Galaxies , volume
= 138, year = 2009 @articleNielsen2016, abstract = The â €standard’ model of
cosmology is founded on the basis that the expansion rate of the universe is
accelerating at present-As was inferred originally from the Hubble diagram of
Type Ia supernovae. There exists now a much bigger database of supernovae so
we can perform rigorous statistical tests to check whether these â
€standardisable candles’ indeed indicate cosmic acceleration. Taking account
of the empirical procedure by which corrections are made to their absolute
magnitudes to allow for the varying shape of the light curve and extinction by
dust, we find, rather surprisingly, that the data are still quite consistent
with a constant rate of expansion., archivePrefix = arXiv, arxivId =
1506.01354, author = Nielsen, J T and Guffanti, A and Sarkar, S, doi =
10.1038/srep35596, eprint = 1506.01354, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Nielsen, Guffanti, Sarkar - 1990 - Marginal evidence for
cosmic acceleration from Type Ia supernovae.pdf:pdf, issn = 20452322, journal
= Sci. Rep., pages = 1–8, publisher = Nature Publishing Group, title =
Marginal evidence for cosmic acceleration from Type Ia supernovae, url =
http://dx.doi.org/10.1038/srep35596, volume = 6, year = 2016
@articleKaaret2017, author = Kaaret, Philip and Feng, Hua and Roberts, Timothy
P, file = :home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Kaaret, Feng, Roberts - 2017 - Ultraluminous X-Ray
Sources.pdf:pdf, keywords = accretion physics,black holes,galaxies,neutron
stars,x-ray binaries,x-rays, pages = 303–342, title = Ultraluminous X-Ray
Sources, year = 2017 @articleKraemer2015, abstract = We present a detailed,
photoionization modeling analysis of XMM-Newton/Reflection Grating
Spectrometer observations of the Seyfert 2 galaxy NGC 1068. The spectrum,
previously analyzed by Kinkhabwala et al., reveals a myriad of soft X-ray
emission lines, including those from H- and He-like carbon, nitrogen, oxygen,
and neon, and M- and L-shell iron. As noted in the earlier analysis, based on
the narrowness of the radiative recombination continua, the electron
temperatures in the emission-line gas are consistent with photoionization,
rather than collisional ionization. The strengths of the carbon and nitrogen
emission lines, relative to those of oxygen, suggest unusual elemental
abundances, which we attribute to the star formation history of the host
galaxy. Overall, the emission lines are blueshifted with respect to systemic,
with radial velocities ∼160 km s-1, similar to that of [O III] $\lambda$5007,
and thus consistent with the kinematics and orientation of the optical
emission-line gas and, hence, likely part of an active galactic nucleus driven
outflow. We were able to achieve an acceptable fit to most of the strong
emission lines with a two-component photoionization model, generated with
cloudy. The two components have ionization parameters and column densities of
logU = -0.05 and 1.22 and logNH = 20.85 and 21.2 and covering factors of 0.35
and 0.84, respectively. The total mass of the X-ray gas is roughly an order of
magnitude greater than the mass of ionized gas determined from optical and
near-IR spectroscopy, which indicates that it may be the dominant component of
the narrow-line region. Furthermore, we suggest that the medium that produces
the scattered/polarized optical emission in NGC 1068 possesses similar
physical characteristics to those of the more highly ionized of the X-ray
model components., archivePrefix = arXiv, arxivId = 1410.6799, author =
Kraemer, S. B. and Sharma, N. and Turner, T. J. and George, Ian M. and Michael
Crenshaw, D., doi = 10.1088/0004-637X/798/1/53, eprint = 1410.6799, file =
:home/william/Documents/Papers/1410.6799.pdf:pdf, issn = 15384357, journal =
Astrophys. J., keywords = Galaxies: Active,Galaxies: Individual (NGC
1068),Galaxies: Seyfert,X-rays: Galaxies, number = 1, pages = 1–32, title =
Physical conditions in the x-ray emission-line gas in NGC 1068, volume = 798,
year = 2015 @articleMorganti2018, abstract = This review summarises what we
have learnt in the last two decades based on H i 21 cm absorption observations
about the cold interstellar medium (ISM) in the central regions of active
galaxies and about the interplay between this gas and the active nucleus
(AGN). H i absorption is a powerful tracer on all scales, from the parsec-
scales close to the central black hole to structures of many tens of kpc
tracing interactions and mergers of galaxies. Given the strong radio continuum
emission often associated with the central activity, H i absorption
observations can be used to study the H i near an active nucleus out to much
higher redshifts than is possible using H i emission. In this way, H i
absorption has been used to characterise in detail the general ISM in active
galaxies, to trace the fuelling of radio-loud AGN, to study the feedback
occurring between the energy released by the active nucleus and the ISM, and
the impact of such interactions on the evolution of galaxies and of their AGN.
In the last two decades, significant progress has been made in all these
areas. It is now well established that many radio loud AGN are surrounded by
small, regularly rotating gas disks that contain a significant fraction of H
i. The structure of these disks has been traced down to parsec scales by very
long baseline interferometry observations. Some groups of objects, and in
particular young and recently restarted radio galaxies, appear to have a
particularly high detection rate of H i. This is interesting in connection
with the evolution of these AGN and their impact on the surrounding ISM. This
is further confirmed by an important discovery, made thanks to technical
upgrades of radio telescopes, namely the presence of fast, AGN-driven outflows
of cold gas which give a direct view of the impact of the energy released by
AGN on the evolution of galaxies (AGN feedback). In addition, evidence has
been collected that clouds of cold gas can play a role in fuelling the nuclear
activity. This review ends by briefly describing the upcoming large, blind H i
absorption surveys planned for the new radio telescopes which will soon become
operational. These surveys will allow to significantly expand existing work,
but will also allow to explore new topics, in particular, the evolution of the
cold ISM in AGN., archivePrefix = arXiv, arxivId = 1807.01475, author =
Morganti, Raffaella and Oosterloo, Tom, doi = 10.1007/s00159-018-0109-x,
eprint = 1807.01475, file = :home/william/Documents/Papers/Morganti-
Oosterloo2018_Article_TheInterstellarAndCIrcumnuclea.pdf:pdf, issn = 09354956,
journal = Astron. Astrophys. Rev., keywords = Galaxies: active,ISM: jets and
outflow,Radio lines: galaxies, number = 1, pages = 1–59, publisher = Springer
Berlin Heidelberg, title = The interstellar and circumnuclear medium of active
nuclei traced by HI 21 cm absorption, url =
https://doi.org/10.1007/s00159-018-0109-x, volume = 26, year = 2018
@articleJones2019, abstract = We report the discovery of a high-redshift,
massive molecular outflow in the starburst galaxy SPT 0346-52 (z =5.656) via
the detected absorption of high-excitation water transitions (H2O 42,3-41,4
and H2O 33,0-32,1) with the Atacama Large Millimeter/submillimeter Array
(ALMA). The host galaxy is one of the most powerful starburst galaxies at high
redshift (star formation rate; SFR ∼3600 M year-1), with an extremely compact
(∼320 pc) star formation region and a SFR surface density (SFR 5500 M year-1
kpc-2) five times higher than ”maximum”(i.e. Eddington-limited) starbursts,
implying a highly transient phase. The estimated outflow rate is ∼500 M
year-1, which is much lower than the SFR, implying that in this extreme
starburst the outflow capabilities saturate and the outflow is no longer
capable of regulating star formation, resulting in a runaway process in which
star formation will use up all available gas in less than 30 Myr. Finally,
while previous kinematic investigations of this source revealed possible
evidence for an ongoing major merger, the coincidence of the hyper-compact
starburst and high-excitation water absorption indicates that this is a single
starburst galaxy surrounded by a disc., archivePrefix = arXiv, arxivId =
1911.09967, author = Jones, G. C. and Maiolino, R. and Caselli, P. and
Carniani, S., doi = 10.1051/0004-6361/201936989, eprint = 1911.09967, file =
:home/william/Documents/Papers/aa36989-19.pdf:pdf, issn = 14320746, journal =
Astron. Astrophys., keywords = Galaxies: high-redshift,Galaxies:
starburst,ISM: jets and outflows, pages = 1–7, title = Detection of a high-
redshift molecular outflow in a primeval hyperstarburst galaxy, volume = 632,
year = 2019 @article2013MNRAS.430.3235M, archivePrefix = arXiv, arxivId =
1301.5005, author = Melioli, C and de Gouveia Dal Pino, E.~M. and Geraissate,
F.~G., doi = 10.1093/mnras/stt126, eprint = 1301.5005, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Melioli, de Gouveia Dal Pino, Geraissate - 2013 - Evolution
of M82-like starburst winds revisited 3D radiative cooling hydrodynamical
si.pdf:pdf, journal = MNRAS, keywords = ISM: abundances,ISM: bubbles,ISM: jets
and outflows,galaxies: ISM,galaxies: kinematics and dynamics,galaxies:
starburst, pages = 3235–3248, title = Evolution of M82-like starburst winds
revisited: 3D radiative cooling hydrodynamical simulations, volume = 430, year
= 2013 @articleChen2020a, abstract = Large-scale outflows are generally
considered as a possible evidence that active galactic nuclei (AGNs) can
severely affect their host galaxies. Recently an ultraluminous IR galaxy
(ULIRG) at $z=0.49$, AKARI J0916248+073034, was found to have a galaxy-scale
[OIII] $$5007 outflow with one of the highest energy-ejection rates at $z1.6$.
However, the central AGN activity estimated from its torus mid-IR (MIR)
radiation is weak relative to the luminous [OIII] emission. In this work we
report the first NuSTAR hard X-ray follow-up of this ULIRG to constrain its
current AGN luminosity. The intrinsic 2-10 keV luminosity shows a 90% upper-
limit of $3.010^{43}$ erg s$^{-1}$ assuming Compton-thick obscuration
($N_{H}=1.510^{24}$ cm$^{-2}$), which is only 3.6% of the luminosity expected
from the extinction corrected [OIII] luminosity. With the NuSTAR observation,
we succeed to identify that this ULIRG has a most extreme case of X-ray
deficit among local ULIRGs. A possible scenario to explain the drastic
declining in both of the corona (X-ray) and torus (MIR) is that the primary
radiation from the AGN accretion disk is currently in a fading status, as a
consequence of a powerful nuclear wind suggested by its powerful ionized
outflow in the galaxy scale., archivePrefix = arXiv, arxivId = 2011.06914,
author = Chen, Xiaoyang and Ichikawa, Kohei and Noda, Hirofumi and Kawamuro,
Taiki and Kawaguchi, Toshihiro and Toba, Yoshiki and Akiyama, Masayuki, doi =
10.3847/2041-8213/abca30, eprint = 2011.06914, file =
:home/william/Documents/Papers/2011.06914.pdf:pdf, issn = 2041-8205, journal =
Astrophys. J., keywords = active galaxies,ulirg,x-ray agn, number = 1, pages =
L2, title = NuSTAR Non-detection of a Faint Active Galactic Nucleus in an
Ultraluminous Infrared Galaxy with Kpc-scale Fast Wind, volume = 905, year =
2020 @articleCruz1999, author = Cruz, Santa, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley Desktop/Downloaded/Cruz
- 1999 - ( 1999. The American Astronomical Society. All rights reserved.
Printed in U.S.A.pdf:pdf, number = 1994, pages = 118–135, title = ( 1999. The
American Astronomical Society. All rights reserved. Printed in U.S.A., volume
= 20, year = 1999 @articleFukumura2017, abstract = We analyze a 900-ks stacked
Chandra/HETG spectrum of NGC 3783 in the context of magnetically-driven
accretion-disk wind models in an effort to provide tight constraints on the
global conditions of the underlying absorbers. Motivated by the earlier
measurements of its absorption measure distribution (AMD) indicating X-ray-
absorbing ionic columns that decrease slowly with decreasing ionization
parameter, we employ 2D magnetohydrodynamic (MHD) disk-wind models to describe
the global outflow. We compute its photoionization structure along with the
wind kinematic properties allowing us to further calculate in a self-
consistent fashion the shapes of the major X-ray absorption lines. With the
wind radial density profile determined by the AMD, the profiles of the
ensemble of the observed absorption features are determined by the two global
parameters of the MHD wind; i.e. disk inclination $\backslash$theta_obs and
wind density normalization n_o. Considering the most significant absorption
features in the (~1.8A-20A) range, we show that the MHD-wind is best described
by n(r)~6.9e11(r/ro)^-1.15 [cm^-3] and $\backslash$theta_obs=44deg. We argue
that winds launched by X-ray heating, radiation pressure or even MHD winds but
with steeper radial density profiles are strongly disfavored by data.
Considering the properties of Fe K band absorption features (i.e. Fe xxv and
Fe xxvi), while typically prominent in the AGN X-ray spectra, they appear to
be weak in NGC 3783. For the specific parameters of our model obtained by
fitting the AMD and the rest of absorption features, these features are found
to be weak in agreement with observation., archivePrefix = arXiv, arxivId =
1712.08181, author = Fukumura, Keigo and Kazanas, Demosthenes and Shrader,
Chris and Behar, Ehud and Tombesi, Francesco and Contopoulos, Ioannis, doi =
10.3847/1538-4357/aaa3f6, eprint = 1712.08181, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Fukumura et al. - 2017 - Magnetized Disk-Winds in NGC
3783.pdf:pdf, isbn = 0112210201, issn = 1538-4357, journal = Astrophys. J.,
keywords = accretion,accretion disks,accretion,accretion disks,galaxies:
individual
(NG,galaxies,individual,magnetohydrodynamics,methods,mhd,ngc3783,numerical,seyfert,
number = 1, pages = 40, publisher = IOP Publishing, title = Magnetized Disk-
Winds in NGC 3783, url = http://arxiv.org/abs/1712.08181, volume = 853, year =
2017 @articleTan2021, abstract = Infrared quasi-stellar objects (IR QSOs) are
a rare subpopulation selected from ultraluminous infrared galaxies (ULIRGs)
and have been regarded as promising candidates of ULIRG-to-optical QSO
transition objects. Here we present NOEMA observations of the CO(1-0) line and
3 mm continuum emission in an IR QSO IRAS F07599+6508 at $z=0.1486$, which has
many properties in common with Mrk 231. The CO emission is found to be
resolved with a major axis of $$6.1 kpc that is larger than the size of $$4.0
kpc derived for 3 mm continuum. We identify two faint CO features located at a
projected distance of $$11.4 and 19.1 kpc from the galaxy nucleus,
respectively, both of which are found to have counterparts in the optical and
radio bands and may have a merger origin. A systematic velocity gradient is
found in the CO main component, suggesting that the bulk of molecular gas is
likely rotationally supported. Based on the radio-to-millimeter spectral
energy distribution and IR data, we estimate that about 30$\%$ of the flux at
3 mm arises from free-free emission and infer a free-free-derived star
formation rate of 77 $M_\\{yr^{-1}}$, close to the IR estimate corrected for
the AGN contribution. We find a high-velocity CO emission feature at the
velocity range of about -1300 to -2000 km s$^{-1}$. Additional deep CO
observations are needed to confirm the presence of a possible very high-
velocity CO extension of the OH outflow in this IR QSO., archivePrefix =
arXiv, arxivId = 2104.01069, author = Tan, Qing-Hua and Gao, Yu and Daddi,
Emanuele and Xia, Xiao-Yang and Hao, Cai-Na and Omont, Alain and Kohno,
Kotaro, eprint = 2104.01069, file =
:home/william/Documents/Papers/2104.01069.pdf:pdf, keywords = ISM-
galaxies,active-galaxies,evolution-galaxies,galaxies,molecules,starburst-ISM,
number = 2012, title = Deep Observations of CO and Free-Free Emission in
Ultraluminous Infrared QSO IRAS F07599+6508, url =
http://arxiv.org/abs/2104.01069, year = 2021 @articleCosta2015, abstract =
Observations of the emission from spatially extended cold gas around bright
high-redshift QSOs reveal surprisingly large velocity widths exceeding 2000 km
s^(-1), out to projected distances as large as 30 kpc. The high velocity
widths have been interpreted as the signature of powerful AGN-driven outflows.
Naively, these findings appear in tension with hydrodynamic models in which
AGN-driven outflows are energy-driven and thus very hot with typical
temperatures T = 10^6-7 K. Using the moving-mesh code Arepo, we perform ’zoom-
in’ cosmological simulations of a z = 6 QSO and its environment, following
black hole growth and feedback via energy-driven outflows. In the simulations,
the QSO host galaxy is surrounded by a clumpy circum-galactic medium pre-
enriched with metals due to supernovae-driven galactic outflows. As a result,
part of the AGN-driven hot outflowing gas can cool radiatively, leading to
large amounts ( 10^9 M_sun) of cold gas comoving with the hot bipolar outflow.
This results in velocity widths of spatially extended cold gas similar to
those observed. We caution, however, that gas inflows, random motions in the
deep potential well of the QSO host galaxy and cooling of supernovae-driven
winds contribute significantly to the large velocity width of the cold gas in
the simulations, complicating the interpretation of observational data.,
author = Costa, Tiago and Sijacki, Debora and Haehnelt, Martin G., doi =
10.1093/mnrasl/slu193, file = :home/william/.local/share/data/Mendeley
Ltd./Mendeley Desktop/Downloaded/Costa, Sijacki, Haehnelt - 2015 - Fast cold
gas in hot AGN outflows.pdf:pdf, issn = 17453933, journal = Mon. Not. R.
Astron. Soc. Lett., keywords = Cosmology: theory,Methods: numerical,Quasars:
supermassive black holes, number = 1, pages = L30–L34, title = Fast cold gas
in hot AGN outflows, volume = 448, year = 2015 @articleCarretti2013, abstract
= The nucleus of the Milky Way is known to harbour regions of intense star
formation activity as well as a super-massive black hole. Recent Fermi space
telescope observations have revealed regions of $\backslash$gamma-ray emission
reaching far above and below the Galactic Centre, the so-called Fermi bubbles.
It is uncertain whether these were generated by nuclear star formation or by
quasar-like outbursts of the central black hole and no information on the
structures’ magnetic field has been reported. Here we report on the detection
of two giant, linearly-polarized radio Lobes, containing three ridge-like sub-
structures, emanating from the Galactic Centre. The Lobes each extend ~60 deg,
bear a close correspondence to the Fermi bubbles, are located in the Galactic
bulge, and are permeated by strong magnetic fields of up to 15 $\backslash$mu
G. Our data signal that the radio Lobes originate in a bi-conical, star-
formation (rather than black hole) driven outflow from the Galaxy’s central
200 pc that transports a massive magnetic energy of ~10^55 erg into the
Galactic halo. The ridges wind around this outflow and, we suggest, constitute
a ‘phonographic’ record of nuclear star formation activity over at least 10
Myr., author = Carretti, Ettore and Crocker, Roland M. and Staveley-Smith,
Lister and Haverkorn, Marijke and Purcell, Cormac and Gaensler, B. M. and
Bernardi, Gianni and Kesteven, Michael J. and Poppi, Sergio, doi =
10.1038/nature11734, file = :home/william/.local/share/data/Mendeley
Ltd./Mendeley Desktop/Downloaded/Carretti et al. - 2013 - Giant magnetized
outflows from the centre of the Milky Way.pdf:pdf, issn = 00280836, journal =
Nature, number = 7430, pages = 66–69, publisher = Nature Publishing Group,
title = Giant magnetized outflows from the centre of the Milky Way, url =
http://dx.doi.org/10.1038/nature11734, volume = 493, year = 2013

@ARTICLESchure2009, author = Schure, K. M. and Kosenko, D. and Kaastra, J. S.
and Keppens, R. and Vink, J., title = ”A new radiative cooling curve based on
an up-to-date plasma emission code”, journal = , keywords = hydrodynamics,
ISM: evolution, radiation mechanisms: thermal, Astrophysics - Galaxy
Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics,
year = 2009, month = dec, volume = 508, number = 2, pages = 751-757, doi =
10.1051/0004-6361/200912495, archivePrefix = arXiv, eprint = 0909.5204,
primaryClass = astro-ph.GA, adsurl =
https://ui.adsabs.harvard.edu/abs/2009A&A…508..751S, adsnote = Provided by the
SAO/NASA Astrophysics Data System

@articleKomossa2015a, abstract = Aims: Radio-loud narrow-line type 1 galaxies
provide us with a fresh look at the blazar phenomenon, the causes of radio
loudness, and the physics of jet formation. We present a multi-wavelength
study of the radio-loud narrow-line type 1 quasar RX J2314.9+2243, which
exhibits some remarkable multi-wavelength properties. It is among the few
radio-loud narrow-line type 1 galaxies, with a tentative $\gamma$-ray
detection, is luminous in the infrared, and shows an exceptionally broad and
blueshifted [OIII]$\lambda$5007 emission-line component. Methods: In order to
understand the nature of this source, we have obtained optical, UV, X-ray, and
radio observations of RX J2314.9+2243. Results: Its spectral energy
distribution (SED) shows a broad hump extending between the IR and far-UV, a
steep radio spectrum and flat X-ray spectrum. Its IR to far-UV SED is
consistent with a scenario, in which synchrotron emission from a jet dominates
the broadband emission, even though an absorption scenario cannot yet be fully
excluded. The high blueshift of its very broad [OIII] component, 1260 km s-1,
is consistent with a face-on view, with the jet (and outflow) pointing towards
us. RX J2314.9+2243 likely represents an extreme case of AGN induced feedback
in the local universe. The optical spectrum (FITS format) is only available at
the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (ftp://130.79.128.5)
or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/574/A121, author =
Komossa, S. and Xu, Dawei and Fuhrmann, L. and Grupe, D. and Yao, S. and Fan,
Z. and Myserlis, I. and Angelakis, E. and Karamanavis, V. and Yuan, W. and
Zensus, J. A., doi = 10.1051/0004-6361/201424814, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Komossa et al. - 2015 - What powers the radio-loud narrow-
line Seyfert 1 galaxy RX J2314.92243.pdf:pdf, issn = 0004-6361, journal =
Astron. Astrophys., keywords = 2243,9,active,evolution,galaxies,individual,rx
j2314,seyfert, pages = A121, title = What powers the radio-loud narrow-line
Seyfert 1 galaxy RX J2314.9+2243?, url =
http://www.aanda.org/10.1051/0004-6361/201424814, volume = 574, year = 2015
@articleXu2015, author = Xu, Ye, file =
:home/william/Documents/Papers/[Cunnigham(thesis)]-Molecular.Outflows.in.SF.regions.pdf:pdf,
number = August, title = Molecular spectra in massive star forming regions,
year = 2015 @articleYang2017, abstract = The Fermi bubbles, two giant gamma-
ray bubbles above and below the Galactic center (GC), are among the most
important findings of the Fermi Gamma-ray Space Telescope. Because of the
proximity, spatially resolved, multi-wavelength observations offer excellent
opportunities to learn about the physical origin of the bubbles. One of the
unique features of the observed bubbles is that their gamma-ray spectrum,
including a high-energy cutoff at ~110 GeV and the overall shape of the
spectrum, is nearly spatially uniform. The high-energy spectral cutoff is
suggestive of a leptonic origin as it could be a signature of synchrotron and
inverse-Compton (IC) cooling of cosmic-ray (CR) electrons; however, even for a
leptonic model, it is not obvious why the spectrum should be spatially
uniform. In this work, we investigate the formation of the Fermi bubble in the
leptonic jet scenario using a newly implemented CRSPEC module in FLASH that
allows us to track the evolution of CR spectrum on-the-fly during the
simulations. We show that the high-energy cutoff is caused by fast synchrotron
and IC cooling near the GC when the jets were first launched. After the jets
propagate away from the GC, the dynamical timescale of the jets become the
shortest among all relevant timescales, and therefore the spectrum is
essentially advected with only mild cooling losses. This could explain why the
bubble spectrum is nearly spatially uniform: the CRs from different parts of
the bubbles as seen today all share the same origin near the GC at early stage
of the bubble expansion. We find that the CR spatial and spectral distribution
predicted by the leptonic jet model can simultaneously match the
normalization, spectral shape, and high-energy cutoff of the observed gamma-
ray spectrum and their spatial uniformity, suggesting that past AGN jet
activity is a likely mechanism for the formation of the Fermi bubbles.,
archivePrefix = arXiv, arxivId = 1706.05025, author = Yang, H. -Y. K. and
Ruszkowski, M., doi = ARTN 2 10.3847/1538-4357/aa9434, eprint = 1706.05025,
file = :home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Yang, Ruszkowski - 2017 - The Spatially Uniform Spectrum of
the Fermi Bubbles the Leptonic AGN Jet Scenario.pdf:pdf, isbn = 0004-637x,
issn = 15384357, journal = Astrophys. J., keywords = cosmic rays,cosmic
rays,Galaxy: nucleus,gamma rays: galaxies,m,galaxies,galaxy,gamma
rays,magnetohydrodynamics,mhd,nucleus, number = 1, pages = 2, publisher = IOP
Publishing, title = The Spatially Uniform Spectrum of the Fermi Bubbles: the
Leptonic AGN Jet Scenario, url = http://arxiv.org/abs/1706.05025, volume =
850, year = 2017 @articleDiMatteo2005, abstract = In the early Universe, while
galaxies were still forming, black holes as massive as a billion solar masses
powered quasars. Supermassive black holes are found at the centres of most
galaxies today, where their masses are related to the velocity dispersions of
stars in their host galaxies and hence to the mass of the central bulge of the
galaxy. This suggests a link between the growth of the black holes and their
host galaxies, which has indeed been assumed for a number of years. But the
origin of the observed relation between black hole mass and stellar velocity
dispersion, and its connection with the evolution of galaxies, have remained
unclear. Here we report simulations that simultaneously follow star formation
and the growth of black holes during galaxy-galaxy collisions. We find that,
in addition to generating a burst of star formation, a merger leads to strong
inflows that feed gas to the supermassive black hole and thereby power the
quasar. The energy released by the quasar expels enough gas to quench both
star formation and further black hole growth. This determines the lifetime of
the quasar phase (approaching 100 million years) and explains the relationship
between the black hole mass and the stellar velocity dispersion.,
archivePrefix = arXiv, arxivId = astro-ph/0502199, author = Di Matteo, Tiziana
and Springel, Volker and Ilernquist, Lars, doi = 10.1038/nature03335, eprint =
0502199, file = :home/william/Documents/Papers/dimatteo2005.pdf:pdf, issn =
00280836, journal = Nature, number = 7026, pages = 604–607, primaryClass =
astro-ph, title = Energy input from quasars regulates the growth and activity
of black holes and their host galaxies, volume = 433, year = 2005
@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 = 0906.2797, author = García-
Marín, M. and Colina, Luis and Arribas, Santiago and Miralles-Caballero,
Daniel and Colina, Luis and Arribas, Santiago and Duc, Pierre Alain and Chung,
Aeree and Narayanan, Gopal and Yun, Min S. and Heyer, Mark and Erickson, Neal
R., doi = 10.1088/0004-6256/142/3/79, eprint = 0906.2797, file =
:home/william/Documents/Papers/aa12537-09.pdf:pdf;:home/william/Documents/Papers/Miralles-
Caballero.pdf:pdf;:home/william/Documents/Papers/0906.2797.pdf:pdf, issn =
00046361, journal = Astron. J., keywords = Galaxies: fundamental
parameters,Galaxies: interactions,Galaxies: structure,galaxies:
evolution,galaxies: interactions,galaxies: photometry,galaxies: star clusters:
general,galaxies: starburst, number = 3, pages = 858–872, title = Integral
field optical spectroscopy of a representative sample of ULIRGs, volume = 142,
year = 2009 @articleSaturni2018, abstract = Star-forming galaxies at high
redshift show anomalous values of infrared excess, which can be described only
by extremizing the existing relations between the shape of their ultraviolet
continuum emission and their infrared-to-ultraviolet luminosity ratio, or by
constructing $\backslash$textit{ad-hoc} models of star formation and dust
distribution. We present an alternative explanation, based on unveiled AGN
activity, to the existence of such galaxies. In fact, the presence of a weak
AGN configures as a natural scenario in order to explain the observed spectral
properties of such high-$z$ objects in terms of a continuum slope distribution
rather than altered infrared excesses, due to the different shape of the AGN
continuum emission with respect to quiescent galaxies. To this aim, we
directly compare the infrared-to-ultraviolet properties of high-redshift
galaxies to those of known categories of AGN (quasars and Seyferts). We also
infer the characteristics of their possible X-ray emission. We find a strong
similarity between the spectral shapes and luminosity ratios of AGN with the
corresponding properties of such galaxies. In addition, we derive expected
X-ray fluxes that are compatible with energetics from AGN activity. We
conclude that a moderate AGN contribution to the UV emission of such high-$z$
objects is a valid alternative to explain their spectral properties. Even the
presence of an active nucleus in each source would not violate the expected
quasar statistics. Furthermore, we suggest that the observed similarities
between anomalous star-forming galaxies and quasars may provide a benchmark
for future theoretical and observational studies on the galaxy population in
the early Universe., archivePrefix = arXiv, arxivId = 1806.07423, author =
Saturni, Francesco Gabriele and Mancini, Mattia and Pezzulli, Edwige and
Tombesi, Francesco, eprint = 1806.07423, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Saturni et al. - 2018 - Zombie or active An alternative
explanation to the properties of star-forming galaxies at high
redshift.pdf:pdf, keywords =
active,galaxies,general,infrared,ism,photometry,quasars,ultraviolet, pages =
1–13, title = ”Zombie” or active? An alternative explanation to the properties
of star-forming galaxies at high redshift, url =
http://arxiv.org/abs/1806.07423, volume = 131, year = 2018
@article2011ApJ…742…44T, archivePrefix = arXiv, arxivId = astro-
ph.HE/1109.2882, author = Tombesi, F and Cappi, M and Reeves, J.~N. and
Palumbo, G.~G.~C. and Braito, V and Dadina, M, doi =
10.1088/0004-637X/742/1/44, eprint = 1109.2882, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Tombesi et al. - 2011 - Evidence for Ultra-Fast Outflows in
radio-quiet active galactic nuclei. II. Detailed photoionization modeling
of.pdf:pdf, journal = Apj, keywords = X-rays: galaxies,black hole
physics,galaxies: Seyfert,galaxies: active,line: identification,plasmas, pages
= 44, primaryClass = astro-ph.HE, title = Evidence for Ultra-fast Outflows in
Radio-quiet Active Galactic Nuclei. II. Detailed Photoionization Modeling of
Fe K-shell Absorption Lines, volume = 742, year = 2011 @articleLonsdale2006,
abstract = At luminosities above ~ 10 11 L ⊙ , infrared galaxies become the
dominant population of extragalactic objects in the local Universe ( z 0.5),
being more numerous than optically selected starburst and Seyfert galaxies,
and QSOs at comparable bolometric luminosity. At the highest luminosities,
ultraluminous infrared galaxies (ULIGs: L ir 10 12 L ⊙ ), outnumber optically
selected QSOs by a factor of ~ 1.5–2. All of the nearest ULIGs ( z 0.1) appear
to be advanced mergers that are powered by both a circumnuclear starburst and
AGN, both of which are fueled by an enormous concentration of molecular gas (~
10 10 M ⊙ ) that has been funneled into the merger nucleus. ULIGs may
represent a primary stage in the formation of massive black holes and
elliptical galaxy cores. The intense circumnuclear starburst that accompanies
the ULIG phase may also represent a primary stage in the formation of globular
clusters, and the metal enrichment of the intergalactic medium by gas and dust
expelled from the nucleus due to the combined forces of supernova explosions
and powerful stellar winds. , archivePrefix = arXiv, arxivId = astro-
ph/0603031, author = Sanders, D.B. and Surace, J.A. and Ishida, C.M., doi =
10.1017/s0074180900112859, eprint = 0603031, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Lonsdale, Farrah, Smith - 2006 - Ultraluminous Infrared
Galaxies.pdf:pdf, issn = 0074-1809, journal = Symp. - Int. Astron. Union,
pages = 289–294, primaryClass = astro-ph, title = Ultraluminous Infrared
Galaxies, url = http://arxiv.org/abs/astro-
ph/0603031%0Ahttp://dx.doi.org/10.1007/3-540-30313-8_9, volume = 186, year =
1999 @articleFeltre2017, abstract = Spectroscopic studies of active galactic
nuclei (AGN) are powerful means of probing the physical properties of the
ionized gas within them. In particular, near future observational facilities,
such as the James Webb Space Telescope (JWST), will allow detailed statistical
studies of rest-frame ultraviolet and optical spectral features of the very
distant AGN with unprecedented accuracy. In this proceedings, we discuss the
various ways of exploiting new dedicated photoionization models of the narrow-
line emitting regions (NLR) of AGN for the interpretation of forthcoming
revolutionary datasets., author = Feltre, Anna and Charlot, Stephane and
Mignoli, Marco and Bongiorno, Angela and Calura, Francesco and Chevallard,
Jacopo and Curtis-Lake, Emma and Gilli, Roberto and Plat, Adele, doi =
10.3389/fspas.2017.00032, file =
:home/william/Documents/Papers/fspas-04-00032.pdf:pdf, issn = 2296987X,
journal = Front. Astron. Sp. Sci., keywords = active galaxies,emission
lines,spectral models,spectroscopy,ultraviolet, number = November, pages =
1–5, title = Ultraviolet/Optical Emission of the Ionized Gas in AGN:
Diagnostics of the Ionizing Source and Gas Properties, volume = 4, year = 2017
@articleMalyshev2017, abstract = The Fermi bubbles are one of the most
remarkable features in the gamma-ray sky revealed by the Fermi Large Area
Telescope (LAT). The nature of the gamma-ray emission and the origin of the
bubbles are still open questions. In this note, we will review some basic
features of leptonic and hadronic modes of gamma-ray production. At the
moment, gamma rays are our best method to study the bubbles, but in order to
resolve the origin of the bubbles multi-wavelength and multi-messenger
observations will be crucial., archivePrefix = arXiv, arxivId = 1704.02629,
author = Malyshev, Dmitry, doi = 10.1051/epjconf/201713603011, eprint =
1704.02629, file = :home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Malyshev - 2017 - Fermi Bubbles an Elephant in the Gamma-
ray Sky.pdf:pdf, pages = 4–7, title = Fermi Bubbles: an Elephant in the Gamma-
ray Sky, url =
http://arxiv.org/abs/1704.02629%0Ahttp://dx.doi.org/10.1051/epjconf/201713603011,
volume = 3011, year = 2017 @article1996ApJ…462..563N, author = Navarro, J.~F.
and Frenk, C.~S. and White, S.~D.~M., doi = 10.1086/177173, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Navarro, Frenk, White - 1996 - The Structure of Cold Dark
Matter Halos.pdf:pdf, journal = Apj, keywords = COSMOLOGY: DARK
MATTER,COSMOLOGY: THEORY,GALAXIES: HALOS,METHODS: NUMERICAL, pages = 563,
title = The Structure of Cold Dark Matter Halos, volume = 462, year = 1996
@articleShangguan2020, abstract = The molecular gas serves as a key probe of
the complex interplay between black hole accretion and star formation in the
host galaxies of active galactic nuclei (AGNs). We use CO(2–1) observations
from a new ALMA survey, in conjunction with literature measurements, to
investigate the molecular gas properties of a representative sample of 40 z
0.3 Palomar-Green quasars, the largest and most sensitive study of molecular
gas emission to date for nearby quasars. We find that the AGN luminosity
correlates with both the CO luminosity and black hole mass, suggesting that
AGN activity is loosely coupled to the cold gas reservoir of the host. The
observed strong correlation between host galaxy total infrared luminosity and
AGN luminosity arises from their common dependence on the molecular gas. We
argue that the total infrared luminosity, at least for low-redshift quasars,
can be used to derive reliable star formation rates for the host galaxy. The
host galaxies of low-redshift quasars have molecular gas content similar to
that of star-forming galaxies of comparable stellar mass. Moreover, they share
similar gas kinematics, as evidenced by their CO Tully-Fisher relation and the
absence of detectable molecular outflows down to sensitive limits. There is no
sign that AGN feedback quenches star formation for the quasars in our sample.
On the contrary, the abundant gas supply forms stars prodigiously, at a rate
that places most of them above the star-forming main sequence and with an
efficiency that rivals that of starburst systems., archivePrefix = arXiv,
arxivId = 2007.11286, author = Shangguan, Jinyi and Ho, Luis C. and Bauer,
Franz E. and Wang, Ran and Treister, Ezequiel, doi = 10.3847/1538-4357/aba8a1,
eprint = 2007.11286, file =
:home/william/Documents/Papers/Shangguan_2020_ApJ_899_112.pdf:pdf, issn =
1538-4357, journal = arXiv, keywords = (Galaxies:) quasars: general,Galaxies:
ISM,Galaxies: active,Galaxies: evolution,Galaxies: seyfert,Submillimeter:
galaxies, number = 2, pages = 112, publisher = IOP Publishing, title = AGN
feedback and star formation of quasar host galaxies: Insights from the
molecular gas, url = http://dx.doi.org/10.3847/1538-4357/aba8a1, volume = 899,
year = 2020 @articleIbanez-Mejia2015, abstract = Molecular cloud observations
show that clouds have non-thermal velocity dispersions that scale with the
cloud size as $R^{1/2}$ at constant surface density, and for varying surface
density scale with both the cloud‘s size and surface density, $^2 R $. The
energy source driving these chaotic motions remains poorly understood. We
describe the velocity dispersions observed in a cloud population formed in a
kiloparsec-scale numerical simulation of a magnetized, supernova-driven, self-
gravitating, interstellar medium, including diffuse heating and radiative
cooling. We compare the relationships between velocity dispersion, size, and
surface density measured in the simulated cloud population to those found in
observations of Galactic molecular clouds. We find that external supernova
explosions can not drive turbulent motions of the observed magnitudes within
dense clouds. On the other hand, self-gravity also induces non-thermal motions
as gravitationally bound clouds begin to collapse in our model, and by doing
so their internal velocity dispersions recover the observed relations. Energy
conservation suggests that the observed behavior is consistent with the
kinetic energy being proportional to the gravitational energy. However, the
clouds in our model show no sign of reaching a stable equilibrium state at any
time, even for strongly magnetized clouds. We conclude that gravitationally
bound molecular clouds are always in a state of gravitational collapse and
their properties are a natural result of this chaotic collapse. In order to
agree with observed star formation efficiencies, this process must be
terminated by the early destruction of the clouds, presumably from internal
stellar feedback., archivePrefix = arXiv, arxivId = 1511.05602, author =
Ibáñez-Mejía, Juan C. and Mac Low, Mordecai-Mark and Klessen, Ralf S. and
Baczynski, Christian, doi = 10.3847/0004-637X/824/1/41, eprint = 1511.05602,
file = :home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Ibáñez-Mejía et al. - 2015 - Gravitational contraction
versus Supernova driving and the origin of the velocity dispersion-size
relati.pdf:pdf, issn = 1538-4357, journal = Astrophys. J., keywords = ISM:
clouds,ISM: kinematics and dynamics,ISM: structure,clouds,ism,kinematics and
dynamics,magnetohydrodynamics,magnetohydrodynamics
(MHD),mhd,structure,turbulence, number = 1, pages = 1–15, publisher = IOP
Publishing, title = Gravitational contraction versus Supernova driving and the
origin of the velocity dispersion-size relation in molecular clouds, url =
http://arxiv.org/abs/1511.05602%0Ahttp://dx.doi.org/10.3847/0004-637X/824/1/41,
volume = 824, year = 2015 @articleGoosmann2011, abstract = We model the
expected X-ray polarization induced by complex reprocessing in the active
nucleus of the Seyfert 2 galaxy NGC 1068. Recent analysis of infrared
interferometry observations suggests that the ionized outflows ejected by the
central engine are not aligned with the symmetry axis of the obscuring torus.
This conclusion was obtained by extrapolating the apparent orientation of the
narrow-line region to the inner parts of the ionization cones. We show that
future measurements of the soft X-ray polarization vector unambiguously
determine the orientation of the ionization cones. Furthermore, X-ray
polarimetry across a broad photon energy range may independently verify the
misalignment between the ionization cones and the axis of the torus. To model
the expected polarization percentage and position angle, we apply the
radiative transfer code stokes. Reprocessing of the primary X-ray radiation
takes place in the accretion disc, the surrounding equatorial torus and the
inclined, ionized outflows. We also examine additional equatorial scattering
occurring in between the accretion disc and the inner surfaces of the torus.
Radiative coupling between the different reprocessing components is computed
coherently. The resulting polarization properties depend on the optical depth
of the reprocessing regions and on the viewing angle of the observer. We show
that even under unfavourable conditions the misalignment of the outflows with
respect to the torus axis can be determined from a rotation of the
polarization position angle between softer and harder X-rays. We argue that
the misalignment of the outflows with respect to the torus axis in NGC 1068
may be constrained by a future X-ray mission if equipped with a broad-band
polarimeter. 2011 The Authors Monthly Notices of the Royal Astronomical
Society 2011 RAS., archivePrefix = arXiv, arxivId = 1012.4652, author =
Goosmann, R. W. and Matt, G., doi = 10.1111/j.1365-2966.2011.18923.x, eprint =
1012.4652, file = :home/william/Documents/Papers/1012.4652.pdf:pdf, issn =
00358711, journal = Mon. Not. R. Astron. Soc., keywords = Galaxies:
Seyfert,Galaxies: individual: NGC 1068,Polarization,Radiative
transfer,Techniques: polarimetric,X-rays: galaxies, number = 4, pages =
3119–3128, title = Spotting the misaligned outflows in NGC 1068 using X-ray
polarimetry, volume = 415, year = 2011 @articleTombesi2013a, abstract = The
existence of ionized X-ray absorbing layers of gas along the line of sight to
the nuclei of Seyfert galaxies is a well established observational fact. This
material is systematically outflowing and shows a large range in parameters.
However, its actual nature and dynamics are still not clear. In order to gain
insights into these important issues we performed a literature search for
papers reporting the parameters of the soft X-ray warm absorbers (WAs) in 35
type 1 Seyferts and compared their properties to those of the ultra-fast
outflows (UFOs) detected in the same sample. The fraction of sources with WAs
is 60%, consistent with previous studies. The fraction of sources with UFOs is
34%, 67% of which also show WAs. The large dynamic range obtained when
considering all the absorbers together allows us, for the first time, to
investigate general relations among them. In particular, we find significant
correlations indicating that the closer the absorber is to the central black
hole, the higher the ionization, column, outflow velocity and consequently the
mechanical power. The absorbers continuously populate the whole parameter
space, with the WAs and the UFOs lying always at the two ends of the
distribution. This strongly suggest that these absorbers, often considered of
different types, could actually represent parts of a single large-scale
stratified outflow observed at different locations from the black hole. The
observed parameters and correlations are consistent with both radiation
pressure through Compton scattering and MHD processes contributing to the
outflow acceleration, the latter playing a major role. Most of the absorbers,
especially the UFOs, have a sufficiently high mechanical power to
significantly contribute to AGN feedback., archivePrefix = arXiv, arxivId =
1212.4851, author = Tombesi, F and Cappi, M and Reeves, J N and Nemmen, R S
and Braito, V and Gaspari, M and Reynolds, C S, doi = 10.1093/mnras/sts692,
eprint = 1212.4851, file = :home/william/.local/share/data/Mendeley
Ltd./Mendeley Desktop/Downloaded/Tombesi et al. - 2013 - Unification of X-ray
winds in Seyfert galaxies From ultra-fast outflows to warm absorbers.pdf:pdf,
issn = 00358711, journal = Mon. Not. R. Astron. Soc., keywords =
Accretion,Black hole physics,Galaxies: Seyfert,Galaxies: active,X-rays:
galaxies,accretion discs, number = 2, pages = 1102–1117, title = Unification
of X-ray winds in Seyfert galaxies: From ultra-fast outflows to warm
absorbers, volume = 430, year = 2013 @articleFluetsch2021, abstract = Galactic
outflows are known to consist of several gas phases; however, the connection
between these phases has been investigated little and only in a few objects.
In this paper, we analyse Multi Unit Spectroscopic Explorer (MUSE)/Very Large
Telescope (VLT) data of 26 local (U)LIRGs and study their ionized and neutral
atomic phases. We also include objects from the literature to obtain a sample
of 31 galaxies with spatially resolved multiphase outflow information. We find
that the ionized phase of the outflows has on average an electron density
three times higher than the disc (ne,disc ∼145 cm-3 versus ne,outflow ∼500
cm-3), suggesting that cloud compression in the outflow is more important than
cloud dissipation. We find that the difference in extinction between outflow
and disc correlates with the outflow gas mass. Together with the analysis of
the outflow velocities, this suggests that at least some of the outflows are
associated with the ejection of dusty clouds from the disc. This may support
models where radiation pressure on dust contributes to driving galactic
outflows. The presence of dust in outflows is relevant for potential formation
of molecules inside them. We combine our data with millimetre data to
investigate the molecular phase. We find that the molecular phase accounts for
more than 60 per cent of the total mass outflow rate in most objects and this
fraction is higher in active galactic nuclei (AGN)-dominated systems. The
neutral atomic phase contributes of the order of 10 per cent, while the
ionized phase is negligible. The ionized-to-molecular mass outflow rate
declines slightly with AGN luminosity, although with a large scatter.,
archivePrefix = arXiv, arxivId = 2006.13232, author = Fluetsch, A. and
Maiolino, R. and Carniani, S. and Arribas, S. and Belfiore, F. and Bellocchi,
E. and Cazzoli, S. and Cicone, C. and Cresci, G. and Fabian, A. C. and
Gallagher, R. and Ishibashi, W. and Mannucci, F. and Marconi, A. and Perna, M.
and Sturm, E. and Venturi, G., doi = 10.1093/mnras/stab1666, eprint =
2006.13232, file = :home/william/Documents/Papers/2006.13232.pdf:pdf, issn =
13652966, journal = Mon. Not. R. Astron. Soc., keywords = ISM:
evolution,galaxies: ISM,galaxies: active,galaxies: evolution, number = 4,
pages = 5753–5783, title = Properties of the multiphase outflows in local
(ultra)luminous infrared galaxies, volume = 505, year = 2021
@articleStrickland2009a, abstract = We measure the net energy efficiency of
supernova (SN) and stellar wind feedback in the starburst galaxy M82 and the
degree of mass loading of the hot gas piston driving its superwind by
comparing a large suite of one and two-dimensional hydrodynamical models to a
set of observational constraints derived from hard X-ray observations of the
starburst region (the fluxes of the He$\alpha$ and Ly$\alpha$-like lines of S,
Ar, Ca, and Fe, along with the total diffuse E = 2-8keV X-ray luminosity).
These are the first direct measurements of the feedback efficiency and mass
loading of SN-heated and enriched plasma in a starburst galaxy. We consider a
broad range of plausible parameters for the M82 starburst, varying the age and
mode of star formation, the starburst region size and geometry, and SN metal
yields. Over all these varied input parameters all the models that satisfy the
existing observational constraints have medium to high thermalization
efficiencies (30% ≤$\epsilon$ ≤ 100%) and the volume-filling wind fluid that
flows out of the starburst region is only mildly centrally mass loaded (1.0 ≤
$\beta$ ≤ 2.8). These results imply a temperature of the plasma within the
starburst region in the range 30-80 million Kelvin, a mass-flow rate of the
wind fluid out of the starburst region of and a terminal velocity of the wind
in the range v ∞ = 1410 - 2240 km s-1 . This velocity is considerably larger
than the escape velocity from M82 (v esc ≲ 460 km s-1 ) and the velocity of
the H$\alpha$ emitting clumps and filaments within M82’s wind (v H$\alpha$ 600
km s-1 ). Drawing on these results we provide a prescription for implementing
starburst-driven superwinds in cosmological models of galaxy formation and
evolution that more accurately represents the energetics of the hot metal-
enriched phases than the existing recipes do. 2009. The American Astronomical
Society. All rights reserved., archivePrefix = arXiv, arxivId = 0903.4175,
author = Strickland, David K. and Heckman, Timothy M., doi =
10.1088/0004-637X/697/2/2030, eprint = 0903.4175, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Strickland, Heckman - 2009 - Supernova feedback efficiency
and mass loading in the starburst and galactic superwind exemplar M82.pdf:pdf,
isbn = bibcode:2009ApJ…697.2030S, issn = 15384357, journal = Astrophys. J.,
keywords = Galaxies: halos,Galaxies: individual (NGC 3034 (M82)),Galaxies:
starburst,ISM: bubbles,Intergalactic medium,X-rays: galaxies, number = 2,
pages = 2030–2056, title = Supernova feedback efficiency and mass loading in
the starburst and galactic superwind exemplar M82, volume = 697, year = 2009
@articleSu2010, abstract = Data from the Fermi-LAT reveal two large gamma-ray
bubbles, extending 50 degrees above and below the Galactic center, with a
width of about 40 degrees in longitude. The gamma-ray emission associated with
these bubbles has a significantly harder spectrum (dN/dE ~ E^-2) than the IC
emission from electrons in the Galactic disk, or the gamma-rays produced by
decay of pions from proton-ISM collisions. There is no significant spatial
variation in the spectrum or gamma-ray intensity within the bubbles, or
between the north and south bubbles. The bubbles are spatially correlated with
the hard-spectrum microwave excess known as the WMAP haze; the edges of the
bubbles also line up with features in the ROSAT X-ray maps at 1.5-2 keV. We
argue that these Galactic gamma-ray bubbles were most likely created by some
large episode of energy injection in the Galactic center, such as past
accretion events onto the central massive black hole, or a nuclear starburst
in the last ~10 Myr. Dark matter annihilation/decay seems unlikely to generate
all the features of the bubbles and the associated signals in WMAP and ROSAT;
the bubbles must be understood in order to use measurements of the diffuse
gamma-ray emission in the inner Galaxy as a probe of dark matter physics.
Study of the origin and evolution of the bubbles also has the potential to
improve our understanding of recent energetic events in the inner Galaxy and
the high-latitude cosmic ray population., author = Su, Meng and Slatyer, Tracy
R. and Finkbeiner, Douglas P., doi = 10.1088/0004-637X/724/2/1044, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley Desktop/Downloaded/Su,
Slatyer, Finkbeiner - 2010 - Giant gamma-ray bubbles from Fermi-LAT Active
Galactic nucleus activity or bipolar Galactic wind.pdf:pdf, issn = 15384357,
journal = Astrophys. J., keywords = Galaxies: active,Galaxies: starburst,Gamma
rays: diffuse background,Ism: jets and outflows, number = 2, pages =
1044–1082, title = Giant gamma-ray bubbles from Fermi-LAT: Active Galactic
nucleus activity or bipolar Galactic wind?, url =
http://stacks.iop.org/0004-637X/724/i=2/a=1044?key=crossref.5aa3963ec8c1c799c748f54d6037d4e5,
volume = 724, year = 2010 @articleTrebitsch2019, archivePrefix = arXiv,
arxivId = 1901.01261, author = Trebitsch, Maxime and Volonteri, Marta and
Dubois, Yohan, eprint = 1901.01261, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Trebitsch, Volonteri, Dubois - 2019 - Black hole
obscuration and duty cycles mediated by AGN feedback in high redshift
galaxies.pdf:pdf, isbn = 1901.01261v1, keywords = ages,dark,first
stars,formation,galaxies,high-
redshift,nuclei,quasars,reionization,supermassive black holes, number =
January, pages = 1–13, title = Black hole obscuration and duty cycles mediated
by AGN feedback in high redshift galaxies, url =
https://arxiv.org/abs/1901.01261, volume = 13, year = 2019
@articledoi:10.1146/annurev-astro-082214-122316, author = King, Andrew and
Pounds, Ken, doi = 10.1146/annurev-astro-082214-122316, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/King, Pounds - 2015 - Powerful Outflows and Feedback from
Active Galactic Nuclei.pdf:pdf, journal = Annu. Rev. Astron. Astrophys.,
number = 1, pages = 115–154, title = Powerful Outflows and Feedback from
Active Galactic Nuclei, url = https://doi.org/10.1146/annurev-
astro-082214-122316, volume = 53, year = 2015 @articlePudritz2003, author =
Pudritz, Ralph E and Ouyed, Rachid and Fendt, Christian and Brandenburg, Axel,
file = :home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Pudritz et al. - 2003 - DISK WINDS , JETS , AND
OUTFLOWS.pdf:pdf, title = DISK WINDS , JETS , AND OUTFLOWS :, year = 2003
@articleRicci2017, abstract = The majority of the accreting supermassive black
holes in the Universe are obscured by large columns of gas and dust1,2,3. The
location and evolution of this obscuring material have been the subject of
intense research in the past decades4,5, and are still debated. A decrease in
the covering factor of the circumnuclear material with increasing accretion
rates has been found by studies across the electromagnetic spectrum1,6,7,8.
The origin of this trend may be driven by the increase in the inner radius of
the obscuring material with incident luminosity, which arises from the
sublimation of dust9; by the gravitational potential of the black hole10; by
radiative feedback11,12,13,14; or by the interplay between outflows and
inflows15. However, the lack of a large, unbiased and complete sample of
accreting black holes, with reliable information on gas column density,
luminosity and mass, has left the main physical mechanism that regulates
obscuration unclear. Here we report a systematic multi-wavelength survey of
hard-X-ray-selected black holes that reveals that radiative feedback on dusty
gas is the main physical mechanism that regulates the distribution of the
circumnuclear material. Our results imply that the bulk of the obscuring dust
and gas is located within a few to tens of parsecs of the accreting
supermassive black hole (within the sphere of influence of the black hole),
and that it can be swept away even at low radiative output rates. The main
physical driver of the differences between obscured and unobscured accreting
black holes is therefore their mass-normalized accretion rate., archivePrefix
= arXiv, arxivId = 1709.09651, author = Ricci, Claudio and Trakhtenbrot, Benny
and Koss, Michael J. and Ueda, Yoshihiro and Schawinski, Kevin and Oh, Kyuseok
and Lamperti, Isabella and Mushotzky, Richard and Treister, Ezequiel and Ho,
Luis C. and Weigel, Anna and Bauer, Franz E. and Paltani, Stephane and Fabian,
Andrew C. and Xie, Yanxia and Gehrels, Neil, doi = 10.1038/nature23906, eprint
= 1709.09651, file = :home/william/Documents/Papers/ricci2017.pdf:pdf, issn =
14764687, journal = Nature, number = 7673, pages = 488–491, publisher = Nature
Publishing Group, title = The close environments of accreting massive black
holes are shaped by radiative feedback, url =
http://dx.doi.org/10.1038/nature23906, volume = 549, year = 2017
@articleSpacek2017a, abstract = Energetic feedback from active galactic nuclei
(AGNs) is difficult to observe, but often used in simulations to resolve
several outstanding issues in galaxy formation. Here we derive new constraints
on AGN feedback by comparing observations and simulations of the thermal
Sunyaev-Zel’dovich (tSZ) effect, which causes spectral distortions in the
cosmic microwave background with signal strengths that are proportional to the
total energy deposited into the medium surrounding large galaxies. We draw on
observational results presented in Spacek et al. (2016, 2017) who used data
from the South Pole Telescope (SPT) and Atacama Cosmology Telescope (ACT) to
measure the tSZ signal from = 10^11 M_Sun and = 1 Gyr galaxies in the redshift
ranges of z=0.5-1.0 (low-z) and z=1.0-1.5 (high-z). Using two large-scale
cosmological hydrodynamical simulations, one with AGN feedback (Horizon-AGN)
and one without (Horizon-NoAGN), we extract simulated tSZ measurements around
a population of galaxies equivalent to those observed. We find that the
Horizon-AGN results only differ from the SPT measurements at levels of 0.4
sigma at low-z and 0.5 sigma at high-z, but they differ from the ACT
measurements at levels of 6.9 sigma at low-z and 14.6 sigma at high-z. The
Horizon-NoAGN results provide a slightly worse fit to the SPT measurements at
levels of 1.8 sigma at low-z and 0.6 sigma at high-z, but a drastically better
match to the ACT measurements at levels of 0.8 sigma at low-z and 1.9 sigma at
high-z. We conclude that, while the lower-mass (~ 5 x 10^11 M_Sun) SPT results
show a hint of AGN feedback energy, the higher-mass (~ 5 x 10^11 M_Sun) ACT
results show significantly less energy than predicted in the simulation
including feedback, indicating that AGN feedback may be milder than often
predicted., archivePrefix = arXiv, arxivId = 1711.05304, author = Spacek,
Alexander and Richardson, Mark and Scannapieco, Evan, doi =
10.3847/1538-4357/aada01, eprint = 1711.05304, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Spacek, Richardson, Scannapieco - 2017 - Using Real and
Simulated Measurements of the Thermal Sunyaev-Zel’dovich Effect to Constrain
Mod.pdf:pdf, issn = 15384357, journal = Astrophys. J., keywords = cosmic
background radiation,cosmic background radiation,galaxies:
evolution,in,evolution,galaxies,general,intergalactic medium,large-scale
structure of,quasars,universe, number = 2, pages = 109, pmid = 900, publisher
= IOP Publishing, title = Using Real and Simulated Measurements of the Thermal
Sunyaev-Zel’dovich Effect to Constrain Models of AGN Feedback, url =
http://arxiv.org/abs/1711.05304, volume = 865, year = 2017 @articleWehrle2009,
author = a.~E. Wehrle and Zacharias, Norbert and Johnston, Kenneth and
Boboltz, David and Fey, A.~L. and Gaume, Ralph and Ojha, R and Meier, D.~L.
and Murphy, D.~W. and Jones, D.~L. and Unwin, S.~C. and Piner, B.~G., file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Wehrle et al. - 2009 - What is the Structure of
Relativistic Jets in AGN on Scales of Light Days.pdf:pdf, journal = astro2010
Astron. Astrophys. Decad. Surv., pages = 310–+, title = What is the Structure
of Relativistic Jets in AGN on Scales of Light Days?, volume = 2010, year =
2009 @articleVanMarle2011, abstract = Energy loss through optically thin
radiative cooling plays an important part in the evolution of astrophysical
gas dynamics and should therefore be considered a necessary element in any
numerical simulation. Although the addition of this physical process to the
equations of hydrodynamics is straightforward, it does create numerical
challenges that have to be overcome in order to ensure the physical
correctness of the simulation. First, the cooling has to be treated
(semi-)implicitly, owing to the discrepancies between the cooling timescale
and the typical timesteps of the simulation. Secondly, because of its
dependence on a tabulated cooling curve, the introduction of radiative cooling
creates the necessity for an interpolation scheme. In particular, we will
argue that the addition of radiative cooling to a numerical simulation creates
the need for extremely high resolution, which can only be fully met through
the use of adaptive mesh refinement. 2010 Elsevier Ltd., archivePrefix =
arXiv, arxivId = 1011.2610, author = van Marle, Allard Jan and Keppens, Rony,
doi = 10.1016/j.compfluid.2010.10.022, eprint = 1011.2610, file =
:home/william/Documents/Papers/[van Marle, et al.]-Radiative cooling in
numerical astrophysics$\backslash$: the need.pdf:pdf, issn = 00457930, journal
= Comput. Fluids, keywords = Circumstellar envelopes,Computational techniques:
fluid dynamics,Radiative recombination,Radiative transfer in
astrophysics,Stellar winds, number = 1, pages = 44–53, title = Radiative
cooling in numerical astrophysics: The need for adaptive mesh refinement,
volume = 42, year = 2011 @articleLakehal2016a, abstract = A simple elegant
expression of nonadiabatic light wave evolution is necessary in order to have
a deeper insight for complicated optical phenomena in light science as well as
in everyday life. Light wave propagation in linear media which have time-
dependent electromagnetic parameters is investigated by utilizing a quadratic
invariant of the system. The time behavior of the nonadiabatic geometric phase
of the waves that yield a cyclic nonadiabatic evolution is analyzed in detail.
Various quantum properties of light waves in this situation, such as variances
of electric and magnetic fields, uncertainty product, coherent and squeezed
states, and their classical limits, are developed. For better understanding of
our research, we applied our analysis in a particular case. The variances of
the fields D and B are illustrated and their time behaviors are addressed.
Equivalent results for the corresponding classical systems are deduced from
the study of the time evolution of the appropriate coherent and squeezed
states., author = Lakehal, Halim and Maamache, Mustapha and Choi, Jeong Ryeol,
doi = 10.1038/srep19860, file =
:home/william/Documents/Papers/may.srep19860.pdf:pdf, issn = 20452322, journal
= Sci. Rep., number = December 2015, pages = 1–10, publisher = Nature
Publishing Group, title = Novel quantum description for nonadiabatic evolution
of light wave propagation in time-dependent linear media, url =
http://dx.doi.org/10.1038/srep19860, volume = 6, year = 2016
@articleOrszag1992, abstract = A Comment on the Letter by J. Janszky and An.
V. Vinogradov, Phys. Rev. Lett. 64, 2771 (1990). 1992 The American Physical
Society., author = Orszag, M. and Ramírez, R. and Retamal, J. C. and Saavedra,
C., doi = 10.1103/PhysRevLett.68.3815, file =
:home/william/Documents/Papers/PhysRevA.45.6570.pdf:pdf, issn = 00319007,
journal = Phys. Rev. Lett., number = 25, pages = 3815, title = Superposition
of coherent states and squeezing, volume = 68, year = 1992 @articleBaron2018d,
abstract = Large scale outflows of different gas phases are ubiquitous in the
host galaxies of active galactic nuclei (AGN). Despite their many differences,
they share a common property - they all contain dust. The dust is carried with
the outflow, heated by the AGN, and emits at infrared wavelengths. This paper
shows that the infrared emission of this dust can be used to detect AGN
outflows and derive their properties. We use a sample of about 4000 type II
AGN and compare the infrared properties of systems that show spectroscopic
signature of ionized gas outflows to systems that do not. We detect an
additional mid-infrared emission component in galaxies with spectroscopically
discovered winds, and attribute it to the dust in the outflow. This new
component offers novel constraints on the outflow properties, such as its mean
location and covering factor. We measure the location of the outflow for
roughly 1700 systems, with the distribution showing a prominent peak around
500 pc, a tail that extends to large distances (10 kpc), and no objects with a
location smaller than 50 pc. The covering factor of the wind shows a wide
distribution which is centered around 0.1, with 24$\%$ (8$\%$) of the winds
showing covering factors larger than 0.2 (0.5). The dust emission is not
sensitive to various systematics affecting optically-selected outflows, and
can be used to estimate the mass outflow rate in thousands of galaxies with
only 1D spectra., archivePrefix = arXiv, arxivId = 1810.06562, author = Baron,
Dalya and Netzer, Hagai, doi = 10.1093/mnras/sty2935, eprint = 1810.06562,
file = :home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Baron, Netzer - 2018 - Discovering AGN-driven winds through
their infrared emission I. General method and wind location.pdf:pdf, keywords
= active,evolution,galaxies,general,interactions,star formation,supermassive
black holes, journal = MNRAS, number = October, title = Discovering AGN-driven
winds through their infrared emission: I. General method and wind location,
url =
http://arxiv.org/abs/1810.06562$\%$0Ahttp://dx.doi.org/10.1093/mnras/sty2935,
volume = 000, year = 2018

@articleOzaki2009, abstract = We investigated the kinematic and excitation
structure of the NGC 1068 narrow-line region (NLR). We obtained profiles of
several emission lines ([O in] A 5007, H/$\beta$, [O I] A 6300, and [Fe VII]
$\lambda$ 6087) at high-velocity resolution (R ̵̃ 7500-11000), and confirmed
that they showed different profiles. These profiles are useful for
understanding the NLR structure, since they cover a wide ionization-potential
range. By comparing the results with a photoioniza-tion model, we found that:
(1) blueshifted components at the center are very dense, (2) those in the
northeast region have slightly lower densities than those in the center, and
(3) the ionization parameters of the blueshifted components increase with
increasing velocity with respect to the systemic velocity. We investigated the
NLR structure in NGC 1068 based on these results. We show that both the
observed velocity dependence of the ionization parameter and the gradually
increasing velocity field can be reproduced by varying the ionizing continuum
attenuation, assuming a hollowed biconical geometry and varying the column
densities of outflowing clouds. 2009 Astronomical Society of Japan.,
archivePrefix = arXiv, arxivId = 0901.1704, author = Ozaki, Shinobu, doi =
10.1093/pasj/61.2.259, eprint = 0901.1704, file =
:home/william/Documents/Papers/0901.1704.pdf:pdf, issn = 00046264, journal =
Publ. Astron. Soc. Japan, keywords = Galaxies: Seyfert,Galaxies: individual
(NGC 1068),Galaxies: kinematics and dynamics, number = 2, pages = 259–274,
title = Kinematic and excitation structure of the NGC 1068 narrow-line region,
volume = 61, year = 2009 @articleRuffa2019, abstract = This is the first paper
of a series exploring the multi-frequency properties of a sample of eleven
nearby low excitation radio galaxies (LERGs) in the southern sky. We are
conducting an extensive study of different galaxy components (stars, warm and
cold gas, radio jets) with the aim of improving our understanding of the AGN
fuelling/feedback cycle in LERGs. We present ALMA Band 6 $^{12}$CO(2-1) and
continuum observations of nine sources. Continuum emission from the radio
cores was detected in all objects. Six sources also show mm emission from jets
on kpc/sub-kpc scales. The jet structures are very similar at mm and cm
wavelengths. We conclude that synchrotron emission associated with the radio
jets dominates the continuum spectra up to 230 GHz. The $^{12}$CO(2-1) line
was detected in emission in six out of nine objects, with molecular gas masses
ranging from $2 10^{7}$ to $2 10^{10}$ M$_{}$. The CO detections show disc-
like structures on scales from $$0.2 to $$10 kpc. In one case (NGC 3100) the
CO disc presents some asymmetries and is disrupted in the direction of the
northern radio jet, indicating a possible jet/disc interaction. In IC 4296, CO
is detected in absorption against the radio core, as well as in emission. In
four of the six galaxies with CO detections, the gas rotation axes are roughly
parallel to the radio jets in projection; the remaining two cases show large
misalignments. In those objects where optical imaging is available, dust and
CO appear to be co-spatial., archivePrefix = arXiv, arxivId = 1901.07513,
author = Ruffa, Ilaria and Prandoni, Isabella and Laing, Robert A. and
Paladino, Rosita and Parma, Paola and de Ruiter, Hans and Mignano, Arturo and
Davis, Timothy A. and Bureau, Martin and Warren, Joshua, eprint = 1901.07513,
file = :home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Ruffa et al. - 2019 - The AGN fuellingfeedback cycle in
nearby radio galaxies - I. ALMA observations and early results.pdf:pdf,
keywords = active,cd,elliptical and lenticular,galaxies,ism,jets,nuclei,
number = January, pages = 1–25, title = The AGN fuelling/feedback cycle in
nearby radio galaxies - I. ALMA observations and early results, url =
http://arxiv.org/abs/1901.07513, volume = 25, year = 2019 @articleLeao2008,
abstract = Considering that the main source of turbulence in the ISM medium
are the explosions of supernovae (SNe), we explore here the role of SN shock
front interactions with clouds on the star formation triggering in presence
and in absence of magnetic field., archivePrefix = arXiv, arxivId = 0810.5374,
author = Leão, M. R. M. and de Gouveia Dal Pino, E. M. and Falceta-Gonçalves,
D. and Melioli, C. and Geraissate, F. G., doi = 10.1017/s1743921309030191,
eprint = 0810.5374, file = :home/william/Documents/Papers/0810.5374.pdf:pdf,
issn = 1743-9213, journal = Proc. Int. Astron. Union, keywords = clouds,from
laboratory and stars,ism,magnetic fields,magnetics fields in the,star,star
formation,supernova remnant,to appear in,to the primordial structure,universe
ii, number = S259, pages = 105–106, title = Local star formation triggered by
SN shocks in magnetized diffuse neutral clouds, volume = 4, year = 2008
@articleTremblay2010, abstract = We present Hubble Space Telescope Advanced
Camera for Surveys and STIS FUV/NUV/optical imaging of the radio galaxy 3C
236, whose relic ∼ 4 Mpc radio jet lobes and inner 2 kpc compact steep
spectrum (CSS) radio source are evidence of multiple epochs of active galactic
nucleus (AGN) activity. Consistent with previous results, our data confirm the
presence of four bright knots of FUV emission in an arc along the edge of the
inner circumnuclear dust disk in the galaxy’s nucleus, as well as FUV emission
cospatial with the nucleus itself. We interpret these to be sites of recent or
ongoing star formation. We present photometry of these knots, as well as an
estimate for the internal extinction in the source using line ratios from
archival ground-based spectroscopy. We estimate the ages of the knots by
comparing our extinction-corrected photometry with stellar population
synthesis models. We find the four knots cospatial with the dusty disk to be
young, of order ∼ 107 yr old. The FUV emission in the nucleus, to which we do
not expect scattered light from the AGN to contribute significantly, is likely
due to an episode of star formation triggered ∼ 109 yr ago. We argue that the
young ∼ 107 yr old knots stem from an episode of star formation that was
roughly coeval with the event resulting in reignition of radio activity,
creating the CSS source. The ∼ 109 yr old stars in the nucleus may be
associated with the previous epoch of radio activity that generated the 4 Mpc
relic source, before being cut off by exhaustion or interruption. The ages of
the knots, considered in the context of both the disturbed morphology of the
nuclear dust and the double-double morphology of the ”old” and ”young” radio
sources, present evidence for an AGN/starburst connection that is possibly
episodic in nature. We suggest that the AGN fuel supply was interrupted for ∼
107 yr due to a minor merger event and has now been restored. The resultant
nonsteady flow of gas in the disk is likely responsible for both the new
episode of infall-induced star formation and also the multiple epochs of radio
activity. 2010. The American Astronomical Society. All rights reserved.,
author = Tremblay, Grant R. and O’Dea, Christopher P. and Baum, Stefi A. and
Koekemoer, Anton M. and Sparks, William B. and De Bruyn, Ger and Schoenmakers,
Arno P., doi = 10.1088/0004-637X/715/1/172, file =
:home/william/Documents/Papers/[Tremblay et al.]-EPISODIC STAR FORMATION
COUPLED TO REIGNITION OF RADIO ACTIVITY IN 3C 236.pdf:pdf, issn = 15384357,
journal = Astrophys. J., keywords = Galaxies: active,Galaxies: individual (3C
236),Galaxies: jets,Galaxies: starburst, number = 1, pages = 172–185, title =
Episodic star formation coupled to reignition of radio activity in 3C 236,
volume = 715, year = 2010 @articleMartizzi2016, abstract = We use local
Cartesian simulations with a vertical gravitational potential to study how
supernova (SN) feedback in stratified galactic discs drives turbulence and
launches galactic winds. Our analysis includes three disc models with gas
surface densities ranging from Milky Way-like galaxies to gas-rich
ultraluminous infrared galaxies (ULIRGs), and two different SN driving schemes
(random and correlated with local gas density). In order to isolate the
physics of SN feedback, we do not include additional feedback processes. We
find that, in these local box calculations, SN feedback excites relatively low
mass-weighted gas turbulent velocity dispersions ≈3-7 km s-1 and low wind mass
loading factors $\eta$ ≲ 1 in all the cases we study. The low turbulent
velocities and wind mass loading factors predicted by our local box
calculations are significantly below those suggested by observations of gas-
rich and rapidly star-forming galaxies; they are also in tension with global
simulations of disc galaxies regulated by stellar feedback. Using a
combination of numerical tests and analytic arguments, we argue that local
Cartesian boxes cannot predict the properties of galactic winds because they
do not capture the correct global geometry and gravitational potential of
galaxies. The wind mass loading factors are in fact not well defined in local
simulations because they decline significantly with increasing box height.
More physically realistic calculations (e.g. including a global galactic
potential and disc rotation) will likely be needed to fully understand disc
turbulence and galactic outflows, even for the idealized case of feedback by
SNe alone., archivePrefix = arXiv, arxivId = 1601.03399, author = Martizzi,
Davide and Fielding, Drummond and Faucher-Giguère, Claude André and Quataert,
Eliot, doi = 10.1093/mnras/stw745, eprint = 1601.03399, file =
:home/william/Documents/Papers/1601.03399.pdf:pdf, issn = 13652966, journal =
Mon. Not. R. Astron. Soc., keywords = Galaxies: ISM,Galaxies:
evolution,Galaxies: formation,Galaxies: general,ISM: supernova
remnants,Methods: numerical, number = 3, pages = 2311–2326, title = Supernova
feedback in a local vertically stratified medium: Interstellar turbulence and
galactic winds, volume = 459, year = 2016 @articleKoudmani2018, abstract = The
systematic analysis of optical large-scale surveys has revealed a population
of dwarf galaxies hosting AGN, which have been confirmed by X-ray follow-up
observations. Recently, the MaNGA survey identified six dwarf galaxies that
appear to have an AGN that is preventing on-going star formation. It is
therefore timely to study the physical properties of dwarf galaxies, in
particular whether the presence of an AGN can affect their evolution. Using
the moving mesh code AREPO, we have investigated different models of AGN
activity, ranging from simple energy-driven spherical winds to collimated,
mass-loaded, bipolar outflows in high resolution simulations of isolated dwarf
galaxies hosting an active black hole. Our simulations also include a novel
implementation of star formation and mechanical supernova (SN) feedback. We
find that AGN outflows have a small but systematic effect on the central star
formation rates (SFRs) for all set-ups explored, while substantial effects on
the global SFR are only obtained with strong SNe and a sustained high-
luminosity AGN with an isotropic wind. This suggests that AGN feedback in
dwarf galaxies is unlikely to directly regulate their global SFRs. There is,
however, a significant effect on outflow properties, which are notably
enhanced by the AGN to much higher outflow temperatures and velocities, in
agreement with kinematic signatures from the MaNGA survey. This indicates that
AGN may play an indirect role in regulating the baryon cycle in dwarf galaxies
by hindering cosmic gas inflows., archivePrefix = arXiv, arxivId = 1812.04629,
author = Koudmani, Sophie and Sijacki, Debora and Bourne, Martin A. and Smith,
Matthew C., doi = 10.1093/mnras/stz097, eprint = 1812.04629, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Koudmani et al. - 2018 - Fast and energetic AGN-driven
outflows in simulated dwarf galaxies.pdf:pdf, keywords =
active,dwarf,formation,galaxies,methods,numerical, number = January, title =
Fast and energetic AGN-driven outflows in simulated dwarf galaxies, url =
http://arxiv.org/abs/1812.04629%0Ahttp://dx.doi.org/10.1093/mnras/stz097,
volume = 000, year = 2018 @article2005A&A…444L…9M, author = Morganti, R and
Tadhunter, C.~N. and Oosterloo, T.~A., doi = 10.1051/0004-6361:200500197, file
= :home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Morganti, Tadhunter, Oosterloo - 2005 - Fast neutral
outflows in powerful radio galaxies a major source of feedback in massive
galaxies.pdf:pdf, journal = aap, keywords = galaxies: ISM,galaxies: active,
pages = L9–L13, title = Fast neutral outflows in powerful radio galaxies: a
major source of feedback in massive galaxies, volume = 444, year = 2005
@articleCosta2020a, abstract = We present a new implementation for active
galactic nucleus (AGN) feedback through small-scale, ultrafast winds in the
moving-mesh hydrodynamic code arepo. The wind is injected by prescribing mass,
momentum, and energy fluxes across a spherical boundary centred on a
supermassive black hole according to available constraints for accretion disc
winds. After sweeping-up a mass equal to their own, small-scale winds
thermalize, powering energy-driven outflows with dynamics, structure, and
cooling properties in excellent agreement with those of analytic wind
solutions. Momentum-driven solutions do not easily occur, because the Compton
cooling radius is usually much smaller than the free-expansion radius of the
small-scale winds. Through various convergence tests, we demonstrate that our
implementation yields wind solutions, which are well converged down to the
typical resolution achieved in cosmological simulations. We test our model in
hydrodynamic simulations of isolated Milky Way-mass galaxies. Above a critical
AGN luminosity, initially spherical, small-scale winds power bipolar, energy-
driven superwinds that break out of the galactic nucleus, flowing at speeds gt
1000 $\backslash$rm km s-1 out to sim 10 $\backslash$rm kpc. These energy-
driven outflows result in moderate, but long-term, reduction in star
formation, which becomes more pronounced for higher AGN luminosities and
faster small-scale winds. Suppression of star formation proceeds through a
rapid mode that involves the removal of the highest density, nuclear gas, and
through a slower mode that effectively halts halo gas accretion. Our new
implementation makes it possible to model AGN-driven winds in a physically
meaningful and validated way in simulations of galaxy evolution, the
interstellar medium and black hole accretion flows., archivePrefix = arXiv,
arxivId = 2006.05997, author = Costa, Tiago and Pakmor, Rüdiger and Springel,
Volker, doi = 10.1093/mnras/staa2321, eprint = 2006.05997, file =
:home/william/Documents/Papers/staa2321.pdf:pdf, issn = 13652966, journal =
Mon. Not. R. Astron. Soc., keywords = galaxies:
evolution,hydrodynamics,methods: numerical,quasars: supermassive black
holes,shock waves, number = 4, pages = 5229–5255, title = Powering galactic
superwinds with small-scale AGN winds, volume = 497, year = 2020
@articleDalgarno, author = Dalgarno, A. and McCray, R. A., file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Dalgarno, McCray - Unknown - Heating and ionization of HI
regions.pdf:pdf, title = Heating and ionization of HI regions
@miscKrawczynski2013, abstract = In this paper we give a brief review of the
astrophysics of active galactic nuclei (AGNs). After a general introduction
motivating the study of AGNs, we discuss our present understanding of the
inner workings of the central engines, most likely accreting black holes with
masses between 106 and 1010 M ⊙. We highlight recent results concerning the
jets (collimated outflows) of AGNs derived from X-ray observations (Chandra)
of kpc-scale jets and $\gamma$-ray observations of AGNs (Fermi, Cherenkov
telescopes) with jets closely aligned with the lines of sight (blazars), and
discuss the interpretation of these observations. Subsequently, we summarize
our knowledge about the cosmic history of AGN formation and evolution. We
conclude with a description of upcoming observational opportunities. 2013
Higher Education Press and Springer-Verlag Berlin Heidelberg., archivePrefix =
arXiv, arxivId = 1301.4179, author = Krawczynski, Henric and Treister,
Ezequiel, booktitle = Front. Phys., doi = 10.1007/s11467-013-0310-3, eprint =
1301.4179, file = :home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Krawczynski, Treister - 2013 - Active Galactic Nuclei – the
Physics of Individual Sources and the Cosmic History of Formation and
Evol.pdf:pdf, issn = 20950462, keywords = active galactic nuclei (AGNs),black
hole accretion,cosmological evolution,relativistic jets, number = 6, pages =
609–629, title = Active galactic nuclei - the physics of individual sources
and the cosmic history of formation and evolution, volume = 8, year = 2013
@articleIshibashi2018, abstract = Galactic outflows are now commonly observed
in starburst and active galactic nuclei (AGN) host galaxies. Yet, there is no
clear consensus on their physical driving mechanism(s). We have previously
shown that AGN radiative feedback, driven by radiation pressure on dust, can
account for the observed dynamics and energetics of galactic outflows,
provided that radiation trapping is taken into account. Here we generalise our
model results by explicitly considering the temporal evolution of the central
AGN luminosity, and the shell mass evolution in different ambient density
distributions. In the case of fixed-mass shells, the high observed values of
the momentum ratio ($= {p}/(L/c)$) and energy ratio ($_k = {E}_{k}/L$) may be
attributed to either radiation trapping or AGN luminosity decay. In contrast,
for expanding shells sweeping up mass from the surrounding environment, a
decay in AGN luminosity cannot account for the observed high energetics, and
radiation trapping is necessarily required. Indeed, strong radiation trapping,
e.g. due to high dust-to-gas ratios, can considerably boost the outflow
energetics. We obtain a distinct radial dependence for the outflow energetics
($(r)$, $_k(r)$) in the case of radiation trapping and luminosity decay, which
may help discriminate between the two scenarios. In this framework, the
recently discovered ‘fossil’ outflows, with anomalously high values of the
energetics, may be interpreted as relics of past AGN activity. The observed
outflow properties may therefore provide useful constraints on the past
history of AGN activity and/or the physical conditions of the outflow launch
region., author = Ishibashi, W. and Fabian, A. C., doi =
10.1093/mnras/sty2617, file = :home/william/.local/share/data/Mendeley
Ltd./Mendeley Desktop/Downloaded/Ishibashi, Fabian - 2018 - Variations on a
theme of AGN-driven outflows luminosity evolution and ambient density
distribution.pdf:pdf, issn = 13652966, journal = Mon. Not. R. Astron. Soc.,
keywords = Black hole physics,Galaxies: active,Galaxies: evolution, number =
4, pages = 4522–4531, publisher = Oxford University Press, title = Variations
on a theme of AGN-driven outflows: Luminosity evolution and ambient density
distribution, volume = 481, year = 2018 @articleMcMillan2017, abstract = We
present mass models of the Milky Way created to fit observational constraints
and to be consistent with expectations from theoretical modelling. The method
used to create these models is that demonstrated in our previous study, and we
improve on those models by adding gas discs to the potential, considering the
effects of allowing the inner slope of the halo density profile to vary, and
including new observations of maser sources in the Milky Way amongst the new
constraints. We provide a best-fitting model, as well as estimates of the
properties of the Milky Way. Under the assumptions in our main model, we find
that the Sun is R0 = 8.20 ± 0.09 kpc from the Galactic Centre, with the
circular speed at the Sun being v0 = 232.8 ± 3.0 kms-1; and that the Galaxy
has a total stellar mass of (54.3 ± 5.7) × 109 M⊙, a total virial mass of
(1.30 ± 0.30) × 1012M⊙ and a local dark-matter density of 0.40 ± 0.04 GeV
cm-3, where the quoted uncertainties are statistical. These values are
sensitive to our choice of priors and constraints. We investigate systematic
uncertainties, which in some cases may be larger. For example, if we weaken
our prior on R0, we find it to be 7.97 ± 0.15 kpc and that v0 = 226.8 ± 4.2
kms-1.We find that most of these properties, including the local dark-matter
density, are remarkably insensitive to the assumed power-law density slope at
the centre of the dark-matter halo. We find that it is unlikely that the local
standard of rest differs significantly from that found under assumptions of
axisymmetry. We have made code to compute the force from our potential, and to
integrate orbits within it, publicly available., archivePrefix = arXiv,
arxivId = 1608.00971, author = McMillan, Paul J., doi = 10.1093/mnras/stw2759,
eprint = 1608.00971, file = :home/william/Documents/Papers/[McMillan et
al.]-The mass distribution and gravitational potential of the Milky
Way.pdf:pdf, issn = 13652966, journal = Mon. Not. R. Astron. Soc., keywords =
Galaxy: fundamental parameters,Galaxy: kinematics and dynamics,Galaxy:
structure,Methods: statistical, number = 1, pages = 76–94, title = The mass
distribution and gravitational potential of the Milky Way, volume = 465, year
= 2017 @articleNardini2018, abstract = Powerful outflows with a broad range of
properties (such as velocity, ionization, radial scale and mass-loss rate)
represent a key feature of active galactic nuclei (AGN), even more so since
they have been simultaneously revealed also in individual objects. Here we
revisit in a simple analytical framework the recent remarkable cases of two
ultraluminous infrared quasars, IRAS F11119+3257 and Mrk 231, which allow us
to investigate the physical connection between multi-phase AGN outflows across
the ladder of distance from the central supermassive black hole (SMBH). We
argue that any major deviations from the standard outflow propagation models
might encode unique information on the past SMBH accretion history, and
briefly discuss how this could help address some controversial aspects of the
current picture of AGN feedback., archivePrefix = arXiv, arxivId = 1805.00040,
author = Nardini, Emanuele and Zubovas, Kastytis, doi = 10.1093/mnras/sty1144,
eprint = 1805.00040, file = :home/william/Documents/Papers/sty1144.pdf:pdf,
issn = 13652966, journal = Mon. Not. R. Astron. Soc., keywords = Galaxies:
active,Galaxies: evolution,ISM: jets and outflows,Quasars: general,Quasars:
individual: supermassive black holes, number = 2, pages = 2274–2280, publisher
= Oxford University Press, title = Multi-phase outflows as probes of AGN
accretion history, volume = 478, year = 2018 @article2000MNRAS.314..511S,
author = Strickland, D.~K. and Stevens, I.~R., doi =
10.1046/j.1365-8711.2000.03391.x, file =
:home/william/Documents/Papers/2000MNRAS.314..511S.pdf:pdf, journal = MNRAS,
keywords = GALAXIES: INDIVIDUAL: M82,GALAXIES: STARBURST,ISM: BUBBLES,ISM:
JETS AND OUTFLOWS,METHODS: NUMERICAL,X-RAYS: GALAXIES, pages = 511–545, title
= Starburst-driven galactic winds - I. Energetics and intrinsic X-ray
emission, volume = 314, year = 2000 @articleDeGouveiadalPino1995, abstract =
After a summary of the observations of cosmic magnetic fields, I briefly
discuss the status of dynamos, the use of electric circuits, the physics of
magnetic explosions, the role of magnetic tension and our strongest magnet
known, the radio pulsar. Finally I mention a few problem areas which may show
a breakthrough in the near future. 1995., archivePrefix = arXiv, arxivId =
astro-ph/0603065, author = de Gouveia dal Pino, Elisabete M, doi =
10.1016/0921-4526(94)01048-6, eprint = 0603065, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley Desktop/Downloaded/de
Gouveia dal Pino - 1995 - Cosmic magnetic fields.pdf:pdf, isbn = 0735403759,
issn = 09214526, journal = Phys. B Phys. Condens. Matter, keywords =
-b,-r,10,12,35,38,52,54,58,62,65,80,96,97,98,and in the early,bp,clusters of
galaxies,cm,dq,eg,en,fs,galaxies,gz,hb,hg,interstellar medium,intracluster and
inter-galactic medium,jets and accretion disks,kh,ld,magnetic fields
in,mj,pacs,stars,universe, number = 1-4, pages = 306–315, primaryClass =
astro-ph, title = Cosmic magnetic fields, volume = 211, year = 1995
@articlePereira-Santaella2018a, abstract = We present new CO(2-1) observations
of three low-z (d ∼350 Mpc) ultra-luminous infrared galaxy (ULIRG) systems
(six nuclei) observed with the Atacama large millimeter/submillimeter array
(ALMA) at high spatial resolution (∼500 pc). We detect massive cold molecular
gas outflows in five out of six nuclei (Mout ∼ (0.3-5) × 108 M⊙). These
outflows are spatially resolved with deprojected effective radii between 250
pc and 1 kpc although high-velocity molecular gas is detected up to Rmax ∼
0.5-1.8 kpc (1-6 kpc deprojected). The mass outflow rates are 12-400 M⊙ yr-1
and the inclination corrected average velocity of the outflowing gas is
350-550 km s-1 (vmax = 500-900 km s-1). The origin of these outflows can be
explained by the strong nuclear starbursts although the contribution of an
obscured active galactic nucleus cannot be completely ruled out. The position
angle (PA) of the outflowing gas along the kinematic minor axis of the nuclear
molecular disk suggests that the outflow axis is perpendicular to the disk for
three of these outflows. Only in one case is the outflow PA clearly not along
the kinematic minor axis, which might indicate a different outflow geometry.
The outflow depletion times are 15-80 Myr. These are comparable to, although
slightly shorter than, the star-formation (SF) depletion times (30-80 Myr).
However, we estimate that only 15-30% of the outflowing molecular gas will
escape the gravitational potential of the nucleus. The majority of the
outflowing gas will return to the disk after 5-10 Myr and become available to
form new stars. Therefore, these outflows will not likely completely quench
the nuclear starbursts. These star-forming powered molecular outflows would be
consistent with being driven by radiation pressure from young stars (i.e.,
momentum-driven) only if the coupling between radiation and dust increases
with increasing SF rates. This can be achieved if the dust optical depth is
higher in objects with higher SF. This is the case in at least one of the
studied objects. Alternatively, if the outflows are mainly driven by
supernovae (SNe), the coupling efficiency between the interstellar medium and
SNe must increase with increasing SF levels. The relatively small sizes (1
kpc) and dynamical times (3 Myr) of the cold molecular outflows suggests that
molecular gas cannot survive longer in the outflow environment or that it
cannot form efficiently beyond these distances or times. In addition, the
ionized and hot molecular phases have been detected for several of these
outflows, so this suggests that outflowing gas can experience phase changes
and indicates that the outflowing gas is intrinsically multiphase, likely
sharing similar kinematics, but different mass and, therefore, different
energy and momentum contributions., archivePrefix = arXiv, arxivId =
1805.03667, author = Pereira-Santaella, M. and Colina, L. and García-Burillo,
S. and Combes, F. and Emonts, B. and Aalto, S. and Alonso-Herrero, A. and
Arribas, S. and Henkel, C. and Labiano, A. and Muller, S. and Piqueras López,
J. and Rigopoulou, D. and Van Der Werf, P., doi = 10.1051/0004-6361/201833089,
eprint = 1805.03667, file = :home/william/Documents/Papers/aa33089-18.pdf:pdf,
issn = 14320746, journal = Astron. Astrophys., keywords = Galaxies:
ISM,Galaxies: active,Galaxies: kinematics and dynamics,Galaxies:
nuclei,Galaxies: starburst, pages = 1–20, title = Spatially resolved cold
molecular outflows in ULIRGs, volume = 616, year = 2018 @articleTombesi2015a,
abstract = Powerful winds driven by active galactic nuclei are often thought
to affect the evolution of both supermassive black holes and their host
galaxies, quenching star formation and explaining the close relationship
between black holes and galaxies. Recent observations of large-scale molecular
outflows in ultraluminous infrared galaxies support this quasar-feedback idea,
because they directly trace the gas from which stars form. Theoretical models
suggest that these outflows originate as energy-conserving flows driven by
fast accretion-disk winds. Proposed connections between large-scale molecular
outflows and accretion-disk activity in ultraluminous galaxies were incomplete
because no accretion-disk wind had been detected. Conversely, studies of
powerful accretion-disk winds have until now focused only on X-ray
observations of local Seyfert galaxies and a few higher-redshift quasars. Here
we report observations of a powerful accretion-disk wind with a mildly
relativistic velocity (a quarter that of light) in the X-ray spectrum of IRAS
F11119+3257, a nearby (redshift 0.189) optically classified type 1
ultraluminous infrared galaxy hosting a powerful molecular outflow. The active
galactic nucleus is responsible for about 80 per cent of the emission, with a
quasar-like luminosity of 1.5 × 10(46) ergs per second. The energetics of
these two types of wide-angle outflows is consistent with the energy-
conserving mechanism that is the basis of the quasar feedback in active
galactic nuclei that lack powerful radio jets (such jets are an alternative
way to drive molecular outflows)., archivePrefix = arXiv, arxivId =
1501.07664, author = Tombesi, F and Meléndez, M. and Veilleux, S and Reeves, J
N and González-Alfonso, E. and Reynolds, C S, doi = 10.1038/nature14261,
eprint = 1501.07664, file = :home/william/.local/share/data/Mendeley
Ltd./Mendeley Desktop/Downloaded/Tombesi et al. - 2015 - Wind from the black-
hole accretion disk driving a molecular outflow in an active galaxy.pdf:pdf,
isbn = 9780874216561, issn = 14764687, journal = Nature, number = 7544, pages
= 436–438, pmid = 25810204, title = Wind from the black-hole accretion disk
driving a molecular outflow in an active galaxy, volume = 519, year = 2015
@articleTampo2020, abstract = We report photometric and spectroscopic
observations and analysis of the 2019 superout- burst of TCP
J21040470+4631129. This object showed a 9-mag superoutburst with early
superhumps and ordinary superhumps, which are the features of WZ Sge-type
dwarf novae. Five rebrightenings were observed after the main superoutburst.
The spectra during the post- superoutburst stage showed the Balmer, He I and
possible sodium doublet features. The mass ratio is derived as 0.0880(9) from
the period of the superhump. During the third and fifth re- brightenings,
growing superhumps and superoutbursts were observed, which have never been
detected during a rebrightening phase among WZ Sge-type dwarf novae with
multiple rebright- enings. To induce a superoutburst during the brightening
phase, the accretion disk was needed to expand beyond the 3:1 resonance radius
of the system again after the main superoutburst.These peculiar phenomena can
be explained by the enhanced viscosity and large radius of the disk suggested
by the higher luminosity and the presence of late-stage superhumps during the
post-superoutburst stage, plus by more mass supply from the cool mass
reservoir and/or from the secondary because of the enhanced mass transfer than
those of other WZ Sge-type dwarf novae., archivePrefix = arXiv, arxivId =
arXiv:2004.10508v1, author = Tampo, Yusuke and Kojiguchi, Naoto and Isogai,
Keisuke and Kato, Taichi and Kimura, Mariko and Wakamatsu, Yasuyuki and
Nogami, Daisaku, doi = 10.1093/pasj/xxx000, eprint = arXiv:2004.10508v1, file
= :home/william/Documents/Papers/1901.05618.pdf:pdf, journal = Publ. Astron.
Soc. Japan, keywords = accretion,accretion disks-stars: novae,cataclysmic
variables-stars: dwarf novae-stars: in, number = 0, pages = 1–6, title = First
Detection of Two Superoutbursts during Rebrightening Phase of a WZ Sge-type
Dwarf Nova: TCP J21040470+4631129, url = http://www.aavso.org/data-download,
volume = 00, year = 2020 @articleNakamura2004, abstract = Non-relativistic
three-dimensional magnetohydrodynamic simulations of Poynting-flux-dominated
(PFD) jets are presented. Our study focuses on the propagation of strongly
magnetized hypersonic but sub-Alfvénic flow (Cs2 Vjet2 VA2) and the
development of a current-driven (CD) kink instability. This instability may be
responsible for the ”wiggled” structures seen in VLBI-scale AGN jets. In the
present paper we investigate the nonlinear behavior of PFD jets in a variety
of external ambient magnetized gas distributions, including those with
density, pressure, and temperature gradients. Our numerical results show that
PFD jets can develop kink distortions in the trans-Alfvénic flow case, even
when the flow itself is still strongly magnetically dominated. In the
nonlinear development of the instability, a non-axisymmetric mode grows on
time scales of order the Alfvén crossing time (in the jet frame) and proceeds
to disrupt the kinematic and magnetic structure of the jet. Because of a large
scale poloidal magnetic field in the ambient medium, the growth of surface
modes (i.e., MHD Kelvin-Helmholtz instabilities) is suppressed. The CD kink
mode (m = 1) grows faster than the other higher order modes (m 1), driven in
large part by the radial component of the Lorentz force., archivePrefix =
arXiv, arxivId = arXiv:astro-ph/0312055v1, author = Nakamura, M. and Meier, D.
L., doi = 10.1063/1.1718472, eprint = 0312055v1, file =
:home/william/Documents/Papers/3-D_Simulations_of_MHD_Jets_-
_The_Stability_Proble.pdf:pdf, isbn = 0735401764, issn = 15517616, journal =
AIP Conf. Proc., number = December 2003, pages = 308–313, primaryClass =
arXiv:astro-ph, title = 3-D simulations of MHD Jets - The stability problem,
volume = 703, year = 2004 @articleSilpa2021, abstract = We present the results
of a multi-frequency, multi-scale radio polarimetric study with the Very Large
Array (VLA) of the Seyfert 1 galaxy and BALQSO, Mrk 231. We detect complex
total and polarized intensity features in the source. Overall, the images
indicate the presence of a broad, one-sided, curved outflow towards the south
which consists of a weakly collimated jet with poloidal inferred magnetic
fields, inside a broader magnetized “wind” or “sheath” component with toroidal
inferred magnetic fields. The model of a kpc-scale weakly collimated jet/lobe
in Mrk 231 is strengthened by its C-shaped morphology, steep spectral index
throughout, complexities in the magnetic field structures, and the presence of
self-similar structures observed on the 10-parsec-scale in the literature. The
“wind” may comprise both nuclear starburst (close to the core) and AGN winds,
where the latter maybe the primary contributor. Moving away from the core, the
“wind” component may also comprise the outer layers (or “sheath”) of a
broadened jet. The inferred value of the (weakly collimated) jet production
efficiency, $\eta$jet ∼ 0.01 is consistent with the estimates in the
literature. The composite jet and wind outflow in Mrk 231 appears to be low-
power and matter-dominated, and oriented at a small angle to our line of
sight., archivePrefix = arXiv, arxivId = 2107.09466, author = Silpa, S and
Kharb, P and O’Dea, C P and Baum, S A and Sebastian, B and Mukherjee, D and
Harrison, C M, doi = 10.1093/mnras/stab2110, eprint = 2107.09466, file =
:home/william/Documents/Papers/2107.09466.pdf:pdf, issn = 0035-8711, journal =
Mon. Not. R. Astron. Soc., keywords = galaxies,general,individual,mrk
231,polarimetric,quasars,radio continuum,techniques, number = July, pages =
1–12, title = AGN jets and winds in polarised light: The case of Mrk 231,
volume = 12, year = 2021 @articleNawaz2016a, abstract = We present three
dimensional relativistic hydrodynamical simulations of a precessing jet
interacting with the intracluster medium and compare the simulated jet
structure with the observed structure of the Hydra A northern jet. For the
simulations, we use jet parameters obtained in the parameter space study of
the first paper in this series and probe different values for the precession
period and precession angle. We find that for a precession period P = 1 Myr
and a precession angle = 20 degree the model reproduces i) the curvature of
the jet, ii) the correct number of bright knots within 20 kpc at approximately
correct locations, and iii) the turbulent transition of the jet to a plume.
The Mach number of the advancing bow shock = 1.85 is indicative of gentle
cluster atmosphere heating during the early stages of the AGN’s activity.,
author = Nawaz, M. A. and Bicknell, G. V. and Wagner, A. Y. and Sutherland, R.
S. and McNamara, B. R., doi = 10.1093/mnras/stw330, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Nawaz et al. - 2016 - Jet-intracluster medium interaction
in hydra A - II. The effect of jet precession.pdf:pdf, issn = 13652966,
journal = Mon. Not. R. Astron. Soc., keywords = Galaxies: active,Galaxies:
clusters: individual: Hydra A,Galaxies: clusters: intracluster
medium,Galaxies: jets, number = 1, pages = 802–815, title = Jet-intracluster
medium interaction in hydra A - II. The effect of jet precession, volume =
458, year = 2016 @articleCrenshaw2015, abstract = We present a detailed study
of AGN feedback in the narrow-line region (NLR) of the Seyfert 1 galaxy NGC
4151. We illustrate the data and techniques needed to determine the mass
outflow rate and kinetic luminosity of the outflowing ionized gas as a
function of position in the NLR. We find that the mass outflow rate peaks at a
value of 3 solar masses per year at a distance of 70 pc from the central
supermassive black hole (SMBH), which is about 10 times the outflow rate
coming from inside 13 pc, and 230 times the mass accretion rate inferred from
the bolometric luminosity of NGC 4151. Thus, most of the outflow must arise
from ”in situ” acceleration of ambient gas throughout the NLR. The kinetic