sta,interferometric,ism,jets and out fl,molecules,ows,starburst,techniques,
number = 1, pages = 35, publisher = IOP Publishing, title = The Dual Role of
Starbursts and Active Galactic Nuclei in Driving Extreme Molecular Outflows,
url = http://dx.doi.org/10.3847/1538-4357/aabccc, volume = 859, year = 2018
@articleAvery2022, abstract = This paper investigates the neutral gas phase of
galactic winds via the Na I D$5890,5895${$\backslash$AA} feature within $z
0.04$ MaNGA galaxies, and directly compares their incidence and strength to
the ionized winds detected within the same parent sample. We find evidence for
neutral outflows in 127 galaxies ($5$ per cent of the analysed line-emitting
sample). Na I D winds are preferentially seen in galaxies with dustier central
regions and both wind phases are more often found in systems with elevated SFR
surface densities, especially when there has been a recent upturn in the star
formation activity according to the SFR$_{5Myr}$/SFR$_{800Myr}$ parameter. We
find the ionized outflow kinematics to be in line with what we measure in the
neutral phase. This demonstrates that, despite their small contributions to
the total outflow mass budget, there is value to collecting empirical
measurements of the ionized wind phase to provide information on the bulk
motion in the outflow. Depending on dust corrections applied to the ionized
gas diagnostics, the neutral phase has $1.2 - 1.8$ dex higher mass outflow
rates (${M}_{out}$), on average, compared to the ionized phase. We quantify
scaling relations between ${M}_{out}$ and the strengths of the physical wind
drivers (SFR, $L_{AGN}$). Using a radial-azimuthal stacking method, and by
considering inclination dependencies, we find results consistent with
biconical outflows orthogonal to the disk plane. Our work complements other
multi-phase outflow studies in the literature which consider smaller samples,
more extreme objects, or proceed via stacking of larger samples.,
archivePrefix = arXiv, arxivId = 2201.08079, author = Avery, Charlotte and
Wuyts, Stijn and Schreiber, Natascha M. Förster and Villforth, Carolin and
Bertemes, Caroline and Hamer, Stephen L. and Sharma, Raman and Toshikawa, Jun
and Zhang, Junkai, eprint = 2201.08079, file =
:home/william/Documents/Papers/2201.08079.pdf:pdf, keywords =
evolution,galaxies,ism,jets and outflows,kinematics and dynamics, number =
January, pages = 1–14, title = Cool outflows in MaNGA: a systematic study and
comparison to the warm phase, url = http://arxiv.org/abs/2201.08079, volume =
14, year = 2022 @article1390a, abstract = New results from th Pierre Auger
Observatory could narrow the search for the origin of ultrahigh-energy cosmic
rays, author = Soebur Razzaque, file = :home/william/Documents/Papers/UHeCR-
SBs.pdf:pdf, pages = 145, title = The Anatomy of Ultrahigh-Energy Cosmic Rays,
volume = 13, year = 2020 @articleCosta2020, abstract = We present a new
implementation for active galactic nucleus (AGN) feedback through small-scale,
ultra-fast 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 thermalise, 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 super-winds that break out of the galactic
nucleus, flowing at speeds $ 1000 \, km \, s^{-1}$ out to $10 \, kpc$. 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, eprint = 2006.05997, file =
:home/william/Documents/Papers/2006.05997.pdf:pdf, keywords =
evolution,galaxies,hydrodynamics,methods,numerical,quasars,shock
waves,supermassive black holes, number = June, pages = 1–29, title = Powering
galactic super-winds with small-scale AGN winds, url =
http://arxiv.org/abs/2006.05997, volume = 29, year = 2020
@articleKennicuttJr.1998, abstract = Measurements of H-alpha, HI, and CO
distributions in 61 normal spiral galaxies are combined with published far-
infrared and CO observations of 36 infrared-selected starburst galaxies, in
order to study the form of the global star formation law, over the full range
of gas densities and star formation rates (SFRs) observed in galaxies. The
disk-averaged SFRs and gas densities for the combined sample are well
represented by a Schmidt law with index N = 1.4+-0.15. The Schmidt law
provides a surprisingly tight parametrization of the global star formation
law, extending over several orders of magnitude in SFR and gas density. An
alternative formulation of the star formation law, in which the SFR is
presumed to scale with the ratio of the gas density to the average orbital
timescale, also fits the data very well. Both descriptions provide potentially
useful ”recipes” for modelling the SFR in numerical simulations of galaxy
formation and evolution., archivePrefix = arXiv, arxivId = astro-ph/9712213,
author = Kennicutt, Jr., Robert C., doi = 10.1086/305588, eprint = 9712213,
file = :home/william/Documents/Papers/Kennicutt,_Jr._1998_ApJ_498_541.pdf:pdf,
issn = 0004-637X, journal = Astrophys. J., number = 2, pages = 541–552,
primaryClass = astro-ph, title = The Global Schmidt Law in Star‐forming
Galaxies, volume = 498, year = 1998 @articleMorganti2021a, abstract = Ranging
from a few pc to hundreds of kpc in size, radio jets have, during their
evolution, an impact on their gaseous environment on a large range of scales.
While their effect on larger scales is well established, it is now becoming
clear that they can also strongly affect the interstellar medium (ISM) inside
the host galaxy. Particularly important is the initial phase ((Formula
presented.) years) of the evolution of the radio jet, when they expand into
the inner few kpc of the host galaxy. Here we report on results obtained for a
representative group of young radio galaxies using the cold molecular gas as a
tracer of jet-ISM interactions. The sensitivity and high spatial resolution of
ALMA and NOEMA are ideal to study the details of this process. In many
objects, we find massive molecular outflows driven by the plasma jet, even in
low-power radio sources. However, the observed outflows are limited to the
circumnuclear regions and only a small fraction of the ISM is leaving the
galaxy. Beyond this region, the impact of the jet seems to change. Fast
outflows are replaced by a milder expansion driven by the expanding cocoon
created by the jet-ISM interaction, resulting in dispersing and heating the
ISM. These findings are in line with predictions from simulations of jets
interacting with a clumpy medium and suggest a more complex view of the impact
of AGN than presently implemented in cosmological simulations., archivePrefix
= arXiv, arxivId = 2201.04157, author = Morganti, Raffaella and Oosterloo, Tom
and Murthy, Suma and Tadhunter, Clive, doi = 10.1002/asna.20210037, eprint =
2201.04157, file = :home/william/Documents/Papers/2201.04157.pdf:pdf, issn =
15213994, journal = Astron. Nachrichten, keywords = 1 impact of,active,from
small to large,galaxies,ism,jets and outflow,radio jets,radio
lines,scales,young, number = 9-10, pages = 1135–1139, title = The impact of
young radio jets traced by cold molecular gas, volume = 342, year = 2021a
@article1975PASJ…27..533M, author = Miyamoto, M and Nagai, R, file =
:home/william/Documents/Papers/1975PASJ…27..533M.pdf:pdf, journal = pasj,
keywords = Astronomical Models,Density Distribution,Functions
(Mathematics),Galactic Structure,Globular Clusters,Gravitational Effects,Mass
Distribution,Mathematical Models,Milky Way Galaxy,Potential Theory,Three
Dimensional Models, pages = 533–543, title = Three-dimensional models for the
distribution of mass in galaxies, volume = 27, year = 1975
@inproceedingsDeGouveiaDalPino2005, abstract = Highly collimated supersonic
jets and less collimated outflows are observed to emerge from a wide variety
of astrophysical objects. They are seen in young stellar objects (YSOs),
proto-planetary nebulae, compact objects (like galactic black holes or
microquasars, and X-ray binary stars), and in the nuclei of active galaxies
(AGNs). Despite their different physical scales (in size, velocity, and amount
of energy transported), they have strong morphological similarities. What
physics do they share? These systems are either hydrodynamic or
magnetohydrodynamic (MHD) in nature and are, as such, governed by non-linear
equations. While theoretical models helped us to understand the basic physics
of these objects, numerical simulations have been allowing us to go beyond the
one-dimensional, steady-state approach extracting vital information. In this
lecture, the formation, structure, and evolution of the jets are reviewed with
the help of observational information, MHD and purely hydrodynamical modeling,
and numerical simulations. Possible applications of the models particularly to
YSOs and AGN jets are addressed. 2005 COSPAR. Published by Elsevier Ltd. All
rights reserved., archivePrefix = arXiv, arxivId = astro-ph/0406319, author =
De Gouveia Dal Pino, Elisabete M., booktitle = Adv. Sp. Res., doi =
10.1016/j.asr.2005.03.145, eprint = 0406319, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley Desktop/Downloaded/De
Gouveia Dal Pino - 2005 - Astrophysical jets and outflows.pdf:pdf, issn =
02731177, keywords = Accretion disks,Active galactic nuclei,Astrophysical
jets,Astrophysics,Black holes,Microquasars,Young stellar objects, number = 5,
pages = 908–924, primaryClass = astro-ph, title = Astrophysical jets and
outflows, volume = 35, year = 2005 @articleMay2020, abstract = We report near-
infrared integral field spectroscopic observations of the active galactic
nucleus NGC 4151 with archive data from the NIFS-Gemini North Telescope. We
have selected best-seeing observations (≲0.3 arcsec) that, allied to our
methodology of image processing techniques, show structures with spatial
resolution comparable to those of the HST. The intricate outflow of NGC 4151
is revisited in light of the results found for NGC 1068, in a previous work,
and a very similar dynamic is found: the low-velocity [Fe ii] emission depicts
the glowing walls of an hourglass structure, while the high-velocity gas fills
its volume. From this finding, we show that the misalignment between the jet
and the NLR is not a projection effect, as previously thought. A molecular
outflow is detected for the first time in this galaxy and, just like in NGC
1068, the transition between the molecular and the ionized gas phases comes
from the fragmentation of molecular cavity walls into bullets of ionized gas
exposed to the central source. Furthermore, it is suggestive that the same
geometrical dichotomy between the cones seen in NGC 1068 is found here, with
one side, where the cavity is disrupted by the AGN, being more extended than
the other. Finally, a new spatial correlation between the high-velocity [Fe
ii] and the soft X-ray emission of [Ne ix] is found, which is unexpected given
the difference between their ionization potentials., archivePrefix = arXiv,
arxivId = 2007.07374, author = May, D. and Steiner, J. E. and Menezes, R. B.
and Williams, D R A and Wang, J., doi = 10.1093/mnras/staa1545, eprint =
2007.07374, file = :home/william/Documents/Papers/2007.07374.pdf:pdf, issn =
0035-8711, journal = Mon. Not. R. Astron. Soc., keywords = Galaxies:
Seyfert,Galaxies: individual: (NGC 4151),ISM,ISM: jets and outflows,ISM:
kinematics and dynamics,Nuclei,Techniques: spectroscopic, month = aug, number
= 2, pages = 1488–1516, title = The nuclear architecture of NGC 4151: on the
path toward a universal outflow mechanism in light of NGC 1068, url =
https://academic.oup.com/mnras/article/496/2/1488/5851281, volume = 496, year
= 2020 @articleVeilleux2017, abstract = In Tombesi et al. (2015), we reported
the first direct evidence for a quasar accretion disk wind driving a massive
molecular outflow. The target was F11119+3257, an ultraluminous infrared
galaxy (ULIRG) with unambiguous type-1 quasar optical broad emission lines.
The energetics of the accretion disk wind and molecular outflow were found to
be consistent with the predictions of quasar feedback models where the
molecular outflow is driven by a hot energy-conserving bubble inflated by the
inner quasar accretion disk wind. However, this conclusion was uncertain
because the energetics were estimated from the optically thick OH 119 um
transition profile observed with Herschel. Here, we independently confirm the
presence of the molecular outflow in F11119+3257, based on the detection of
broad wings in the CO(1-0) profile derived from ALMA observations. The broad
CO(1-0) line emission appears to be spatially extended on a scale of at least
~7 kpc from the center. Mass outflow rate, momentum flux, and mechanical power
of (80-200) R_7^{-1} M_sun/yr, (1.5-3.0) R_7^{-1} L_AGN/c, and (0.15-0.40)%
R_7^{-1} L_AGN are inferred from these data, assuming a CO-to-H_2 conversion
factor appropriate for a ULIRG (R_7 is the radius of the outflow normalized to
7 kpc and L_AGN is the AGN luminosity). These rates are time-averaged over a
flow time scale of 7x10^6 yrs. They are similar to the OH-based rates time-
averaged over a flow time scale of 4x10^5 yrs, but about a factor 4 smaller
than the local (”instantaneous”; 10^5 yrs) OH-based estimates cited in Tombesi
et al. The implications of these new results are discussed in the context of
time-variable quasar-mode feedback and galaxy evolution. The need for an
energy-conserving bubble to explain the molecular outflow is also re-
examined., archivePrefix = arXiv, arxivId = 1706.00443, author = Veilleux, S.
and Bolatto, A. and Tombesi, F. and Melendez, M. and Sturm, E. and Gonzalez-
Alfonso, E. and Fischer, J. and Rupke, D. S. N., doi =
10.3847/1538-4357/aa767d, eprint = 1706.00443, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Veilleux et al. - 2017 - Quasar Feedback in the
Ultraluminous Infrared Galaxy F111193257 Connecting the Accretion Disk Wind
with the Lar.pdf:pdf, issn = 1538-4357, journal = Astrophys. J., keywords =
3257,active,evolution,f11119,galaxies,galaxies: active,galaxies:
evolution,ISM: jets and,general,individual,ism,jets and out fl,ows,quasars,
number = 1, pages = 18, publisher = IOP Publishing, title = Quasar Feedback in
the Ultraluminous Infrared Galaxy F11119+3257: Connecting the Accretion Disk
Wind with the Large-Scale Molecular Outflow, url =
http://arxiv.org/abs/1706.00443%0Ahttp://dx.doi.org/10.3847/1538-4357/aa767d,
volume = 843, year = 2017 @articleTully1977, abstract = • גרינבלט, י. (2012).
ענף הקיווי: תמונת מצב 2012, עלון הנוטע שה“מ, מחוז צפון, משרד החקלאות., author
= Tully, R. Brent and Fisher, J. Richard, file =
:home/william/Documents/Papers/[Tully, Fisher]-A New Method to Determine
Distance to Galaxies.pdf:pdf, journal = Astron. Astrophys., pages = 661–673,
title = A New Method of Determining Distances to Galaxies, volume = 54, year =
1977 @articleBell1978, abstract = It is shown that charged particles can be
accelerated to high energies in astrophysical shock fronts. Fast particles are
prevented from streaming away upstream of a shock front by scattering off
Alfven waves which they themselves generate. This scattering confines the
particles to the region around the shock and results in first-order Fermi
acceleration due to the particles crossing the shock many times. The
consequent energy spectrum is a power law with an index close to that observed
for galactic cosmic rays. The discussion relates to particles which are
already relativistic, and their initial acceleration from thermal energies is
not considered., archivePrefix = arXiv, arxivId = arXiv:1011.1669v3, author =
Bell, A. R., doi = 10.1093/mnras/182.3.443, eprint = arXiv:1011.1669v3, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley Desktop/Downloaded/Bell
- 1978 - The acceleration of cosmic rays in shock fronts - II.pdf:pdf, isbn =
9780874216561, issn = 0035-8711, journal = Mon. Not. R. Astron. Soc., number =
3, pages = 443–455, pmid = 25052830, title = The acceleration of cosmic rays
in shock fronts - II, url = https://academic.oup.com/mnras/article-
lookup/doi/10.1093/mnras/182.3.443, volume = 182, year = 1978
@articleYang2021, abstract = In radio-loud active galactic nuclei (AGNs),
ultra-fast outflows (UFOs) were detected at the inclination angle of ∼10°–70°
away from jets. Except for the inclination angle of UFOs, the UFOs in radio-
loud AGNs have similar properties to that in radio-quiet AGNs. The UFOs with
such low inclination cannot be explained in the line-force mechanism. The
magnetic-driving mechanism is suggested to explain the UFOs based on a self-
similar solution with radiative transfer calculations. However, the energetics
of self-similar solution need to be further confirmed based on numerical
simulations. To understand the formation and acceleration of UFOs in radio-
loud AGNs, this paper presents a model of the disk winds driven by both line
force and magnetic field and implements numerical simulations. Initially, a
magnetic field is set to 10 times stronger than the gas pressures at the disk
surface. Simulation results imply that the disk winds driven by both line
force and magnetic field could describe the properties of UFOs in radio-loud
AGNs. Pure magnetohydrodynamics (MHDs) simulation is also implemented. When
the initial conditions are the same, the hybrid models of magnetic fields and
line force are more helpful to form UFOs than the pure MHD models. It is worth
studying the case of a stronger magnetic field to confirm this result.,
archivePrefix = arXiv, arxivId = 2110.10954, author = Yang, Xiao-Hong, doi =
10.3847/1538-4357/ac3236, eprint = 2110.10954, file =
:home/william/Documents/Papers/Yang_2021_ApJ_922_262.pdf:pdf, issn =
0004-637X, journal = Astrophys. J., keywords = Supermassive black holes,Radio
active galactic nuc, number = 2, pages = 262, publisher = IOP Publishing,
title = Magnetohydrodynamic Winds Driven by Line Force from the Standard Thin
Disk around Supermassive Black Holes: II. A Possible Model for Ultra-fast
Outflows in Radio-loud AGNs, url = http://dx.doi.org/10.3847/1538-4357/ac3236,
volume = 922, year = 2021 @articlePonti2019, abstract = Evidence has mounted
in recent decades that outflows of matter and energy from the central few
parsecs of our Galaxy have shaped the observed structure of the Milky Way on a
variety of larger scales1. On scales of 15 parsecs, the Galactic Centre has
bipolar lobes that can be seen in both the X-ray and radio parts of the
spectrum2,3, indicating broadly collimated outflows from the centre, directed
perpendicular to the Galactic plane. On larger scales, approaching the size of
the Galaxy itself, $\gamma$-ray observations have revealed the so-called
‘Fermi bubble’ features4, implying that our Galactic Centre has had a period
of active energy release leading to the production of relativistic particles
that now populate huge cavities on both sides of the Galactic plane. The X-ray
maps from the ROSAT all-sky survey show that the edges of these cavities close
to the Galactic plane are bright in X-rays4–6. At intermediate scales (about
150 parsecs), radio astronomers have observed the Galactic Centre lobe, an
apparent bubble of emission seen only at positive Galactic latitudes7,8, but
again indicative of energy injection from near the Galactic Centre. Here we
report prominent X-ray structures on these intermediate scales (hundreds of
parsecs) above and below the plane, which appear to connect the Galactic
Centre region to the Fermi bubbles. We propose that these structures, which we
term the Galactic Centre ‘chimneys’, constitute exhaust channels through which
energy and mass, injected by a quasi-continuous train of episodic events at
the Galactic Centre, are transported from the central few parsecs to the base
of the Fermi bubbles4., author = Ponti, G. and Hofmann, F. and Churazov, E.
and Morris, M. R. and Haberl, F. and Nandra, K. and Terrier, R. and Clavel, M.
and Goldwurm, A., doi = 10.1038/s41586-019-1009-6, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Ponti et al. - 2019 - An X-ray chimney extending hundreds
of parsecs above and below the Galactic Centre.pdf:pdf, issn = 14764687,
journal = Nature, number = 7748, pages = 347–350, publisher = Springer US,
title = An X-ray chimney extending hundreds of parsecs above and below the
Galactic Centre, url = http://dx.doi.org/10.1038/s41586-019-1009-6, volume =
567, year = 2019 @articleWoo2020, abstract = We investigate the connection
between ionized gas outflows and star formation activity using a large sample
of type 1 and 2 AGNs with far-IR detections or star formation rate (SFR)
estimates. The strength of ionized gas outflows, measured by the velocity
dispersion and velocity shift of the [O iii] emission line, clearly shows a
correlation with SFR. The connection between specific star formation rate
(sSFR) and [O iii] gas velocity dispersion indicates that AGNs with stronger
outflows are hosted by galaxies with higher SFR. Compared to star-forming
galaxies in the main sequence, both type 1 and type 2 AGNs show sSFR similar
to that of non-AGN galaxies, indicating no instantaneous AGN feedback, while
sSFR is higher (lower) for AGNs with stronger (weaker) outflows than that of
main sequence galaxies. These results are consistent with a delayed AGN
feedback scenario. However, it is also possible that a decease/increase of gas
fraction may cause the correlation without AGN feedback. Subject headings:
galaxies: active — galaxies: kinematics and dynamics, archivePrefix = arXiv,
arxivId = 2008.04919, author = Woo, Jong Hak and Son, Donghoon and Rakshit,
Suvendu, doi = 10.3847/1538-4357/abad97, eprint = 2008.04919, file =
:home/william/Documents/Papers/Woo_2020_ApJ_901_66.pdf:pdf, issn = 15384357,
journal = arXiv, title = The correlation of outflow kinematics with star
formation rate - Gas outflows in AGNs. VI, volume = 66, year = 2020
@articleCheung2016, abstract = Quiescent galaxies with little or no ongoing
star formation dominate the galaxy population above $M_{*}2 10^{10}~M_{}$,
where their numbers have increased by a factor of $25$ since $z2$. Once star
formation is initially shut down, perhaps during the quasar phase of rapid
accretion onto a supermassive black hole, an unknown mechanism must remove or
heat subsequently accreted gas from stellar mass loss or mergers that would
otherwise cool to form stars. Energy output from a black hole accreting at a
low rate has been proposed, but observational evidence for this in the form of
expanding hot gas shells is indirect and limited to radio galaxies at the
centers of clusters, which are too rare to explain the vast majority of the
quiescent population. Here we report bisymmetric emission features co-aligned
with strong ionized gas velocity gradients from which we infer the presence of
centrally-driven winds in typical quiescent galaxies that host low-luminosity
active nuclei. These galaxies are surprisingly common, accounting for as much
as $10\%$ of the population at $M_* 2 10^{10}~ M_{}$. In a prototypical
example, we calculate that the energy input from the galaxy’s low-level active
nucleus is capable of driving the observed wind, which contains sufficient
mechanical energy to heat ambient, cooler gas (also detected) and thereby
suppress star formation., archivePrefix = arXiv, arxivId = 1605.07626, author
= Cheung, Edmond and Bundy, Kevin and Cappellari, Michele and Peirani,
Sébastien and Rujopakarn, Wiphu and Westfall, Kyle and Yan, Renbin and
Bershady, Matthew and Greene, Jenny E and Heckman, Timothy M and Drory, Niv
and Law, David R and Masters, Karen L and Thomas, Daniel and Wake, David A and
Weijmans, Anne Marie and Rubin, Kate and Belfiore, Francesco and Vulcani,
Benedetta and Chen, Yan Mei and Zhang, Kai and Gelfand, Joseph D. and Bizyaev,
Dmitry and Roman-Lopes, A. and Schneider, Donald P., doi =
10.1038/nature18006, eprint = 1605.07626, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Cheung et al. - 2016 - Suppressing star formation in
quiescent galaxies with supermassive black hole winds.pdf:pdf, isbn =
1476-4687 (Electronic)$\backslash$r0028-0836 (Linking), issn = 14764687,
journal = Nature, number = 7604, pages = 504–508, pmid = 27225122, publisher =
Nature Publishing Group, title = Suppressing star formation in quiescent
galaxies with supermassive black hole winds, url =
http://dx.doi.org/10.1038/nature18006, volume = 533, year = 2016
@articleYoung1991, author = Young, J. S. and Scoville, N. Z., doi =
10.1146/annurev.aa.29.090191.003053, file =
:home/william/Documents/Papers/annurev.aa.29.090191.003053.pdf:pdf, issn =
00664146, journal = Annu. Rev. Astron. Astrophys., keywords = Galaxy
evolution,Hubble sequence,Interstellar medium,Star formation, number = 1,
pages = 581–625, title = Molecular gas in galaxies, volume = 29, year = 1991
@articleBatista2021, abstract = One of the most promising ways to probe
intergalactic magnetic fields (IGMFs) is through gamma rays produced in
electromagnetic cascades initiated by high-energy gamma rays or cosmic rays in
the intergalactic space. Because the charged component of the cascade is
sensitive to magnetic fields, gamma-ray observations of distant objects such
as blazars can be used to constrain IGMF properties. Ground-based and space-
borne gamma-ray telescopes deliver spectral, temporal, and angular information
of high-energy gamma-ray sources, which carries imprints of the intervening
magnetic fields. This provides insights into the nature of the processes that
led to the creation of the first magnetic fields and into the phenomena that
impacted their evolution. Here we provide a detailed description of how gamma-
ray observations can be used to probe cosmic magnetism. We review the current
status of this topic and discuss the prospects for measuring IGMFs with the
next generation of gamma-ray observatories., archivePrefix = arXiv, arxivId =
2105.12020, author = Batista, Rafael Alves and Saveliev, Andrey, eprint =
2105.12020, file = :home/william/Documents/Papers/2105.12020.pdf:pdf, keywords
= electromagnetic cascades,high-energy gamma rays,intergalactic magnetic
fields, pages = 1–55, title = The Gamma-Ray Window to Intergalactic Magnetism,
url = http://arxiv.org/abs/2105.12020, year = 2021 @article1995ApJ…438…62W,
author = Wilson, A.~S. and Colbert, E.~J.~M., doi = 10.1086/175054, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Wilson, Colbert - 1995 - The difference between radio-loud
and radio-quiet active galaxies.pdf:pdf, journal = Apj, keywords = Active
Galactic Nuclei,Black Holes (Astronomy),Cosmology,Interacting
Galaxies,Luminosity,Quasars,Radio Astronomy,Radio Jets (Astronomy), pages =
62–71, title = The difference between radio-loud and radio-quiet active
galaxies, volume = 438, year = 1995 @articleAbbett2012, abstract = We present
a series of numerical simulations ofthe quiet–Sun plasma threaded by magnetic
fields that extend from the upper convection zone into the low corona.We
discuss an efficient, simplified approximationto thephysics of optically thick
radiative transport through the surface layers, and investigate the effects of
convective turbulence on the magnetic structure of the Sun’s atmosphere in an
initially unipolar (open field) region. We find that the net Poynting flux
below the surface is on average directed toward the interior, while in the
photosphere and chromosphere the net flow of electromagnetic energy is outward
into the solar corona. Overturning convective motions between these layers
driven by rapid radiative cooling appears to be the source of energy for the
oppositely directed fluxes of electromagnetic energy., archivePrefix = arXiv,
arxivId = arXiv:1102.1035v1, author = Abbett, W. P. and Fisher, G. H., doi =
10.1007/s11207-011-9817-3, eprint = arXiv:1102.1035v1, file =
:home/william/Documents/Papers/1102.1035.pdf:pdf, isbn = 9781461437611,
journal = Sol. Flare Magn. Fields Plasmas, keywords =
Convection,Corona,Magnetic fields,Photosphere,Radiative transfer, number =
February 2011, pages = 3–20, title = Radiative coolingin MHD models of the
quiet sun convection zone and corona, year = 2012 @articleJarvis2020, abstract
= We use a sample of powerful z ≈ 0.1 type 2 quasars (’obscured’; log
[LAGN/erg s-1] ≳ 45), which host kpc-scale ionized outflows and jets, to
identify possible signatures of AGN feedback on the total molecular gas
reservoirs of their host galaxies. Specifically, we present Atacama Pathfinder
EXperiment (APEX) observations of the CO(2-1) transition for nine sources and
the CO(6-5) for a subset of three. We find that the majority of our sample
reside in starburst galaxies (average specific star formation rates-sSFR-of
1.7 Gyr-1), with the seven CO-detected quasars also having large molecular gas
reservoirs (average Mgas = 1.3 × 1010 M⊙), even though we had no pre-selection
on the star formation or molecular gas properties. Despite the presence of
quasars and outflows, we find that the molecular gas fractions (Mgas/M* =
0.1-1.2) and depletion times (Mgas/SFR = 0.16-0.95 Gyr) are consistent with
those expected for the overall galaxy population with matched stellar masses
and sSFRs. Furthermore, for at least two of the three targets with the
required measurements, the CO(6-5)/CO(2-1) emission-line ratios are consistent
with star formation dominating the CO excitation over this range of
transitions. The targets in our study represent a gas-rich phase of galaxy
evolution with simultaneously high levels of star formation and nuclear
activity; furthermore, the jets and outflows do not have an immediate
appreciable impact on the global molecular gas reservoirs., archivePrefix =
arXiv, arxivId = 2007.10351, author = Jarvis, M. E. and Harrison, C. M. and
Mainieri, V. and Calistro Rivera, G. and Jethwa, P. and Zhang, Z. Y. and
Alexander, D. M. and Circosta, C. and Costa, T. and De Breuck, C. and Kakkad,
D. and Kharb, P. and Lansbury, G. B. and Thomson, A. P., doi =
10.1093/mnras/staa2196, eprint = 2007.10351, file =
:home/william/Documents/Papers/2007.10351.pdf:pdf, issn = 13652966, journal =
Mon. Not. R. Astron. Soc., keywords = ISM: Jets and outflows,ISM:
Molecules,galaxies: Active,galaxies: Evolution,galaxies: General,galaxies:
ISM, number = 2, pages = 1560–1575, title = High molecular gas content and
star formation rates in local galaxies that host quasars, outflows, and jets,
volume = 498, year = 2020 @article2014A&ARv..22…73F, archivePrefix = arXiv,
arxivId = astro-ph.HE/1407.7615, author = Falomo, R and Pian, E and Treves, A,
doi = 10.1007/s00159-014-0073-z, eprint = 1407.7615, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Falomo, Pian, Treves - 2014 - An optical view of BL
Lacertae objects.pdf:pdf, keywords = BL Lacertae objects: general,Galaxies:
active,Galaxies: jets,Galaxies: nuclei,Quasars: supermassive black
holes,Radiation mechanisms: non-thermal, pages = 73, primaryClass = astro-
ph.HE, title = An optical view of BL Lacertae objects, volume = 22, year =
2014 @articleGrissom2014, abstract = The electron scattering optical depth
constraints on reionization suggest that there may be other sources that
contribute to the ionization of hydrogen aside from observable star forming
galaxies. Often the calculated value of the electron scattering optical depth,
$\tau$es, falls below the measurements derived from observations of the cosmic
microwave background, or an assumption about non-observable sources must be
made in order to reach agreement. Here, we calculate the hydrogen ionization
fraction as a function of redshift and the electron scattering optical depth
from both galaxies and active galactic nuclei (AGN) factoring in the secondary
collisional ionizations from the AGN X-ray emission. In this paper we use the
most current determination of the evolving hard X-ray luminosity function and
extrapolate its evolution beyond z = 6. The AGN spectral energy distributions
include both UV and X-ray ionizing photons. To search for the largest possible
effect, all AGNs are assumed to have $\lambda$Edd = 1.0 and to be completely
unobscured. The results show that AGNs produce a perturbative effect on the
reionization of hydrogen and they remain in agreement with current
constraints. Our calculations find the epoch of reionization still ends at z ≈
6 and only increases the electron scattering optical depth by ~2.3% under
ideal conditions. This can only be moderately increased by assuming a constant
black hole mass of MBH = 105 MâŠ™. As a result, we conclude that there is a
need for other sources beyond observable galaxies and AGNs that contribute to
the reionization of hydrogen at z 6. 2014 ESO., author = Grissom, R. L. and
Ballantyne, D. R. and Wise, J. H., doi = 10.1051/0004-6361/201322637, file =
:home/william/Documents/Papers/aa22637-13.pdf:pdf, issn = 00046361, journal =
Astron. Astrophys., keywords = Dark ages reionization first stars,Galaxies:
active,Galaxies: evolution,Quasars: general, pages = 1–5, title = On the
contribution of active galactic nuclei to reionization, volume = 561, year =
2014 @articlePierce1992, archivePrefix = arXiv, arxivId = arXiv:1011.1669v3,
author = Pierce, Michael J and R. Brent Tully, eprint = arXiv:1011.1669v3,
file = :home/william/Documents/Papers/[Pierce and Tully]-Luminosity-Line width
Relations and the intergalactic Distance Scale. I.Absolute
Calibration.pdf:pdf, journal = J. Chem. Inf. Model., keywords = icle, pages =
47–55, title = Luminosity-Line width Relations and the Extragalatic Distance
Scale. I. Absolute Calibration, volume = 387, year = 1992 @articleAbbott2016,
abstract = On September 14, 2015 at 09:50:45 UTC the two detectors of the
Laser Interferometer Gravitational-Wave Observatory simultaneously observed a
transient gravitational-wave signal. The signal sweeps upwards in frequency
from 35 to 250 Hz with a peak gravitational-wave strain of 1.0×10−21. It
matches the waveform predicted by general relativity for the inspiral and
merger of a pair of black holes and the ringdown of the resulting single black
hole. The signal was observed with a matched-filter signal-to-noise ratio of
24 and a false alarm rate estimated to be less than 1 event per 203 000 years,
equivalent to a significance greater than 5.1$\sigma$. The source lies at a
luminosity distance of 410+160−180 Mpc corresponding to a redshift
z=0.09+0.03−0.04. In the source frame, the initial black hole masses are
36+5−4M⊙ and 29+4−4M⊙, and the final black hole mass is 62+4−4M⊙, with
3.0+0.5−0.5M⊙c2 radiated in gravitational waves. All uncertainties define 90%
credible intervals. These observations demonstrate the existence of binary
stellar-mass black hole systems. This is the first direct detection of
gravitational waves and the first observation of a binary black hole merger.,
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and Schutz, B. F. and Scott, J. and Scott, S. M. and Sellers, D. and Sengupta,
A. S. and Sentenac, D. and Sequino, V. and Sergeev, A. and Serna, G. and
Setyawati, Y. and Sevigny, A. and Shaddock, D. A. and Shaffer, T. and Shah, S.
and Shahriar, M. S. and Shaltev, M. and Shao, Z. and Shapiro, B. and Shawhan,
P. and Sheperd, A. and Shoemaker, D. H. and Shoemaker, D. M. and Siellez, K.
and Siemens, X. and Sigg, D. and Silva, A. D. and Simakov, D. and Singer, A.
and Singer, L. P. and Singh, A. and Singh, R. and Singhal, A. and Sintes, A.
M. and Slagmolen, B. J.J. and Smith, J. R. and Smith, M. R. and Smith, N. D.
and Smith, R. J.E. and Son, E. J. and Sorazu, B. and Sorrentino, F. and
Souradeep, T. and Srivastava, A. K. and Staley, A. and Steinke, M. and
Steinlechner, J. and Steinlechner, S. and Steinmeyer, D. and Stephens, B. C.
and Stevenson, S. P. and Stone, R. and Strain, K. A. and Straniero, N. and
Stratta, G. and Strauss, N. A. and Strigin, S. and Sturani, R. and Stuver, A.
L. and Summerscales, T. Z. and Sun, L. and Sutton, P. J. and Swinkels, B. L.
and Szczepańczyk, M. J. and Tacca, M. and Talukder, D. and Tanner, D. B. and
Tápai, M. and Tarabrin, S. P. and Taracchini, A. and Taylor, R. and Theeg, T.
and Thirugnanasambandam, M. P. and Thomas, E. G. and Thomas, M. and Thomas, P.
and Thorne, K. A. and Thorne, K. S. and Thrane, E. and Tiwari, S. and Tiwari,
V. and Tokmakov, K. V. and Tomlinson, C. and Tonelli, M. and Torres, C. V. and
Torrie, C. I. and Töyrä, D. and Travasso, F. and Traylor, G. and Trifirò, D.
and Tringali, M. C. and Trozzo, L. and Tse, M. and Turconi, M. and Tuyenbayev,
D. and Ugolini, D. and Unnikrishnan, C. S. and Urban, A. L. and Usman, S. A.
and Vahlbruch, H. and Vajente, G. and Valdes, G. and Vallisneri, M. and Van
Bakel, N. and Van Beuzekom, M. and Van Den Brand, J. F.J. and Van Den Broeck,
C. and Vander-Hyde, D. C. and Van Der Schaaf, L. and Van Heijningen, J. V. and
Van Veggel, A. A. and Vardaro, M. and Vass, S. and Vasúth, M. and Vaulin, R.
and Vecchio, A. and Vedovato, G. and Veitch, J. and Veitch, P. J. and
Venkateswara, K. and Verkindt, D. and Vetrano, F. and Viceré, A. and
Vinciguerra, S. and Vine, D. J. and Vinet, J. Y. and Vitale, S. and Vo, T. and
Vocca, H. and Vorvick, C. and Voss, D. and Vousden, W. D. and Vyatchanin, S.
P. and Wade, A. R. and Wade, L. E. and Wade, M. and Waldman, S. J. and Walker,
M. and Wallace, L. and Walsh, S. and Wang, G. and Wang, H. and Wang, M. and
Wang, X. and Wang, Y. and Ward, H. and Ward, R. L. and Warner, J. and Was, M.
and Weaver, B. and Wei, L. W. and Weinert, M. and Weinstein, A. J. and Weiss,
R. and Welborn, T. and Wen, L. and Weßels, P. and Westphal, T. and Wette, K.
and Whelan, J. T. and Whitcomb, S. E. and White, D. J. and Whiting, B. F. and
Wiesner, K. and Wilkinson, C. and Willems, P. A. and Williams, L. and
Williams, R. D. and Williamson, A. R. and Willis, J. L. and Willke, B. and
Wimmer, M. H. and Winkelmann, L. and Winkler, W. and Wipf, C. C. and Wiseman,
A. G. and Wittel, H. and Woan, G. and Worden, J. and Wright, J. L. and Wu, G.
and Yablon, J. and Yakushin, I. and Yam, W. and Yamamoto, H. and Yancey, C. C.
and Yap, M. J. and Yu, H. and Yvert, M. and Zadrożny, A. and Zangrando, L. and
Zanolin, M. and Zendri, J. P. and Zevin, M. and Zhang, F. and Zhang, L. and
Zhang, M. and Zhang, Y. and Zhao, C. and Zhou, M. and Zhou, Z. and Zhu, X. J.
and Zucker, M. E. and Zuraw, S. E. and Zweizig, J., doi =
10.1103/PhysRevLett.116.061102, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley Desktop/Downloaded/Wu
et al. - 2011 - The theoretical basis of oil-coal co-processing and process
optimization.pdf:pdf, issn = 10797114, journal = Phys. Rev. Lett., number = 6,
pages = 1–16, title = Observation of gravitational waves from a binary black
hole merger, volume = 116, year = 2016 @articleYesuf2020, abstract = Active
galactic nucleus (AGN) feedback is expected to impact the amount of cold gas
in galaxies by driving strong galactic winds, by preventing external gas
inflows, or by changing the thermodynamical state of the gas. We use molecular
gas mass estimates based on dust absorption (H$$/H$$) to study gas content of
large samples of type 2 AGN host galaxies in comparison with inactive
galaxies. Using sparse principal component and clustering analysis, we analyze
a suite of stellar and structural parameters of $27,100$ face-on, central
galaxies at redshift $z = 0.02-0.15$ and with stellar mass
$M_10^{10}-210^{11}\,M_$. We identify four galaxy groups of similar mass and
morphology (mass surface density, velocity dispersion, concentration, and
S$\backslash$’{e}rsic index) that can be evolutionarily linked through a
lifecycle wherein gas content mediates their star formation rate (SFR) and
level of AGN activity. Galaxies first consume their gas mostly through bursty
star formation, then enter into a transition phase of intermediate gas
richness in which star formation and AGNs coexist, before settling into
retirement as gas-poor, quiescent systems with residual levels of AGN activity
(LINERs). Strongly accreting black holes (Seyferts) live in gas-rich, star-
forming hosts, but neither their gas reservoir nor their ability to form stars
seem to be impacted $\backslash$emph{instantaneously} (timescales
$0.5$$\backslash$,Gyr) by AGN feedback. Our results are inconsistent with AGN
feedback models that predict that central, bulge-dominated, Seyfert-like AGNs
in massive galaxies have significantly lower molecular gas fractions compared
to inactive galaxies of similar mass, morphology, and SFR., archivePrefix =
arXiv, arxivId = 2007.12026, author = Yesuf, Hassen M. and Ho, Luis C., eprint
= 2007.12026, file = :home/william/Documents/Papers/2007.12026.pdf:pdf,
keywords = dust,evolution,galaxies,ism,molecules,nuclei,seyfert,star
formation, title = Gas Content Regulates the Lifecycle of Star Formation and
Black Hole Accretion in Galaxies, url = http://arxiv.org/abs/2007.12026, year
= 2020 @articleHerrera-Camus2020, abstract = Aims. Our aim is to search for
and characterize inflows and outflows of molecular gas in four ultraluminous
infrared galaxies (ULIRGs; LIR 1012LO ) at z ∼ 0.2-0.3 and one distant quasi-
stellar object (QSO) at z = 6.13. Methods. We used Herschel/PACS and ALMA Band
7 observations of the hydroxyl molecule (OH) line at rest-frame wavelength 119
$\mu$m, which in absorption can provide unambiguous evidence of inflows or
outflows of molecular gas in nuclear regions of galaxies. Our study
contributes to doubling the number of OH 119 $\mu$m observations of luminous
systems at z ∼ 0.2-0.3, and pushes the search for molecular outflows based on
the OH 119 $\mu$m transition to z ∼ 6. Results. We detect OH 119 $\mu$m high-
velocity absorption wings in three of the four ULIRGs. In two cases, IRAS
F20036-1547 and IRAS F13352+6402, the blueshifted absorption profiles indicate
the presence of powerful and fast (∼200-500 km s-1) molecular gas outflows.
Consistent with an inside-out quenching scenario, these outflows are depleting
the central reservoir of star-forming molecular gas at a rate similar to that
of intense star formation activity. For the starburst-dominated system IRAS
10091+4704, we detect an inverted P Cygni profile that is unique among ULIRGs
and indicates the presence of a fast (∼400 km s-1) inflow of molecular gas at
a rate of ∼100 MO yr-1 towards the central region. Finally, we tentatively
detect (∼3$\sigma$) the OH 119 $\mu$m doublet in absorption in the z = 6.13
QSO ULAS J131911+095051. The OH 119 $\mu$m feature is blueshifted with a
median velocity that suggests the presence of a molecular outflow, although
characterized by a modest molecular mass loss rate of ∼200 MO yr-1. This value
is comparable to the small mass outflow rates found in the stacking of the [C
» II] spectra of other z ∼ 6 QSOs and suggests that ejective feedback in this
phase of the evolution of ULAS J131911+095051 has subsided., archivePrefix =
arXiv, arxivId = 1912.05548, author = Herrera-Camus, R. and Sturm, E. and
Graciá-Carpio, J. and Veilleux, S. and Shimizu, T. and Lutz, D. and Stone, M.
and González-Alfonso, E. and Davies, R. and Fischer, J. and Genzel, R. and
Maiolino, R. and Sternberg, A. and Tacconi, L. and Verma, A., doi =
10.1051/0004-6361/201937109, eprint = 1912.05548, file =
:home/william/Documents/Papers/1912.05548.pdf:pdf, isbn = 1342270673, issn =
14320746, journal = Astron. Astrophys., keywords = Galaxies: active,Galaxies:
evolution,Galaxies: high-redshift,Quasars: absorption lines, pages = 1–9,
title = Molecular gas inflows and outflows in ultraluminous infrared galaxies
at z ∼0.2 and one QSO at z = 6.1, volume = 633, year = 2020 @articleDekel2019,
abstract = We address a simple model where the Kennicutt-Schmidt (KS) relation
between the macroscopic densities of star formation rate (SFR, $\rho$sfr) and
gas (n) in galactic discs emerges from self-regulation of the SFR via
supernova feedback. It arises from the physics of supernova bubbles,
insensitive to the microscopic SFR recipe and not explicitly dependent on
gravity. The key is that the filling factor of SFR-suppressed supernova
bubbles self-regulates to a constant, f ∼ 0.5. Expressing the bubble fading
radius and time in terms of n, the filling factor is f ∝ S n−s with s = 1.5,
where S is the supernova rate density. A constant f thus refers to $\rho$sfr ∝
n1.5, with a density-independent SFR efficiency per free-fall time ∼0.01. The
self-regulation to f ∼ 0.5 and the convergence to a KS relation independent of
the local SFR recipe are demonstrated in cosmological and isolated-galaxy
simulations using different codes and recipes. In parallel, the spherical
analysis of bubble evolution is generalized to clustered supernovae,
analytically and via simulations, yielding s = 1.5 ± 0.5. An analysis of
photoionized bubbles about presupernova stars yields a range of KS slopes but
the KS relation is dominated by the supernova bubbles. Superbubble blowouts
may lead to an alternative self-regulation by outflows and recycling. While
the model is oversimplified, its simplicity and validity in the simulations
may argue that it captures the origin of the KS relation., archivePrefix =
arXiv, arxivId = 1903.00962, author = Dekel, Avishai and Sarkar, Kartick C.
and Jiang, Fangzhou and Bournaud, Frederic and Krumholz, Mark R. and Ceverino,
Daniel and Primack, Joel R., doi = 10.1093/mnras/stz1919, eprint = 1903.00962,
file = :home/william/Documents/Papers/stz1919.pdf:pdf, issn = 13652966,
journal = Mon. Not. R. Astron. Soc., keywords = Galaxies: ISM,Galaxies:
evolution,Galaxies: formation,Stars: formation,Supernovae: general, number =
4, pages = 4753–4778, publisher = Oxford University Press, title = The global
star formation law by supernova feedback, volume = 488, year = 2019
@articleCielo2017, abstract = Feedback by Active Galactic Nuclei is often
divided into quasar and radio mode, powered by radiation or radio jets,
respectively. Both are fundamental in galaxy evolution, especially in late-
type galaxies, as shown by cosmological simulations and observations of jet-
ISM interactions in these systems. We compare AGN feedback by radiation and by
collimated jets through a suite of simulations, in which a central AGN
interacts with a clumpy, fractal galactic disc. We test AGN of $10^{43}$ and
$10^{46}$ erg/s, considering jets perpendicular or parallel to the disc.
Mechanical jets drive the more powerful outflows, exhibiting stronger mass and
momentum coupling with the dense gas, while radiation heats and rarefies the
gas more. Radiation and perpendicular jets evolve to be quite similar in
outflow properties and effect on the cold ISM, while inclined jets interact
more efficiently with all the disc gas, removing the densest $20\%$ in $20$
Myr, and thereby reducing the amount of cold gas available for star formation.
All simulations show small-scale inflows of $0.01-0.1$ M$_$/yr, which can
easily reach down to the Bondi radius of the central supermassive black hole
(especially for radiation and perpendicular jets), implying that AGN modulate
their own duty cycle in a feedback/feeding cycle., archivePrefix = arXiv,
arxivId = 1712.03955, author = Cielo, S. and Bieri, R. and Volonteri, M. and
Wagner, A. and Dubois, Y., doi = 10.1093/mnras/sty708, eprint = 1712.03955,
file = :home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Cielo et al. - 2017 - AGN Feedback Compared Jets versus
Radiation.pdf:pdf, issn = 1365-2966, keywords = active,galaxies,high-
redshift,ism,methods, journal = MNRAS, number = December, title = AGN Feedback
Compared: Jets versus Radiation, url =
http://arxiv.org/abs/1712.03955%0Ahttp://dx.doi.org/10.1093/mnras/sty708,
volume = 000, year = 2017 @articleKoudmani2019, abstract = The systematic
analysis of optical large-scale surveys has revealed a population of dwarf
galaxies hosting active galactic nuclei (AGN), which have been confirmed by
X-ray followup 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/Documents/Papers/stz097.pdf:pdf, issn =
13652966, journal = Mon. Not. R. Astron. Soc., keywords = Galaxies:
active,Galaxies: dwarf,Galaxies: formation,Methods: numerical, number = 2,
pages = 2047–2066, publisher = Oxford University Press, title = Fast and
energetic AGN-driven outflows in simulated dwarf galaxies, volume = 484, year
= 2019 @articleKo2019, abstract = Processes of dissipation of energy released
during capture and disruption stars by Galactic central Black hole. This
process should periodically happen in the Galactic center and affect Galactic
center environment as well as Galactic halo. Routine star disruptions by the
central supermassive black hole BH provide enough cumulative energy to form
the Fermi Bubbles. A single star of super-Eddington eruption provide an
subsonic outflow gas whose total energy is about $10^{52}$ erg. The average
rate of disruption events is expected to be $10^{-4}-10^{-5}$yr$^{-1}$ that
provides the average power of energy release in the GC ${W}310^{41}$ erg
s$^{-1}$, just needed to support Fermi Bubbles in the halo. In the exponential
atmosphere the energy from the GC propagates perpendicular to the Galactic
plane and provides symmetric features in the halo., archivePrefix = arXiv,
arxivId = 1904.03958, author = Ko, C. M. and Chernyshov, D. O. and Cheng, H.
and Dai, L. and Dogiel, V. A., eprint = 1904.03958, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley Desktop/Downloaded/Ko
et al. - 2019 - Formation of Fermi Bubbles by Tidal Disruption Events at
Galactic Center.pdf:pdf, keywords = clouds,cosmic rays,gamma rays,ism,mhd,non-
thermal,radiation mechanisms,scattering,turbulence, title = Formation of Fermi
Bubbles by Tidal Disruption Events at Galactic Center, url =
http://arxiv.org/abs/1904.03958, volume = 1, year = 2019 @articleLuminet2003,
abstract = The current ’standard model’ of cosmology posits an infinite flat
universe forever expanding under the pressure of dark energy. First-year data
from the Wilkinson Microwave Anisotropy Probe (WMAP) confirm this model to
spectacular precision on all but the largest scales. Temperature correlations
across the microwave sky match expectations on angular scales narrower than
60° but, contrary to predictions, vanish on scales wider than 60°. Several
explanations have been proposed. One natural approach questions the underlying
geometry of space-namely, its curvature and topology. In an infinite flat
space, waves from the Big Bang would fill the universe on all length scales.
The observed lack of temperature correlations on scales beyond 60° means that
the broadest waves are missing, perhaps because space itself is not big enough
to support them. Here we present a simple geometrical model of a finite space-
the Poincaré dodecahedral space-which accounts for WMAP’s observations with no
fine-tuning required. The predicted density is $\Omega$ 0 ≈ 1.013 1, and the
model also predicts temperature correlations in matching circles on the sky.,
archivePrefix = arXiv, arxivId = astro-ph/0310253, author = Luminet, Jean
Pierre and Weeks, Jeffrey R. and Riazuelo, Alain and Lehoucq, Roland and Uzan,
Jean Philippe, doi = 10.1038/nature01944, eprint = 0310253, file =
:home/william/Documents/Papers/83950 593..640 _ Enhanced Reader.pdf:pdf, issn
= 00280836, journal = Nature, number = 6958, pages = 593–595, primaryClass =
astro-ph, title = Dodecahedral space topology as an explanation for weak wide-
angle temperature correlations in the cosmic microwave background, volume =
425, year = 2003 @articleYang2018b, abstract = The Fermi bubbles, two giant
structures above and below the Galactic center (GC), are among the most
important discoveries of the Fermi Gamma-ray Space Telescope. Studying their
physical origin has been providing valuable insights into cosmic-ray
transport, the Galactic magnetic field, and past activity at the GC in the
Milky Way galaxy. Despite their importance, the formation mechanism of the
bubbles is still elusive. Over the past few years there have been numerous
efforts, both observational and theoretical, to uncover the nature of the
bubbles. In this article, we present an overview of the current status of our
understanding of the bubbles’ origin, and discuss possible future directions
that will help to distinguish different scenarios of bubble formation.,
archivePrefix = arXiv, arxivId = 1802.03890, author = Yang, H. -Y. K. and
Ruszkowski, M. and Zweibel, E. G., doi = 10.3390/galaxies6010029, eprint =
1802.03890, file = :home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Yang, Ruszkowski, Zweibel - 2018 - Unveiling the Origin of
the Fermi Bubbles.pdf:pdf, issn = 20754434, keywords = cosmic
rays,galaxy,gamma rays, pages = 1–9, title = Unveiling the Origin of the Fermi
Bubbles, url =
http://arxiv.org/abs/1802.03890%0Ahttp://dx.doi.org/10.3390/galaxies6010029,
year = 2018 @articleHayashi2021, abstract = We present the results of our
multifrequency observations for 10 ultraluminous infrared galaxies (ULIRGs)
made by the Karl G. Jansky Very Large Array at 1.4, 5.5, 9.0, and 14.0 GHz.
Our sample is selected from ULIRGs whose active galactic nuclei (AGNs) are not
found at optical wavelengths (∼70 per cent of the total ULIRGs), but whose
presence is suggested by mid-infrared or submillimetre observations (50 per
cent of the non-AGN ULIRGs at optical wavelengths). The statistical properties
of the targets are similar to those of the entire ULIRG sample, which implies
that ULIRGs have common radiative processes regardless of the presence of
optical AGNs, and thus AGNs might equally contribute to the radio emission of
every ULIRG. Although their spectra are mainly explained by starbursts and/or
merger activity, some individual sources suggest contributions from AGNs. IRAS
00188-0856, whose optical morphology is not disturbed, shows a large non-
thermal fraction and a spectral break at high frequency, which can be
explained by synchrotron ageing of non-thermal plasma emitted from AGNs. In
addition, we find 100-kpc-scale extended emission associated with IRAS
01004-2237. The two-sided morphology and absence of extended X-ray emission
suggest that this system is not induced by a merger in a cluster but
originates from AGN activity., archivePrefix = arXiv, arxivId = 2101.12058,
author = Hayashi, Takayuki J. and Hagiwara, Yoshiaki and Imanishi, Masatoshi,
doi = 10.1093/mnras/stab1084, eprint = 2101.12058, file =
:home/william/Documents/Papers/2101.12058.pdf:pdf, issn = 13652966, journal =
Mon. Not. R. Astron. Soc., keywords = galaxies: active,galaxies: nuclei,radio
continuum: galaxies,techniques: interferometric, number = 2, pages =
2675–2686, title = Radio properties of 10 nearby ultraluminous infrared
galaxies with signatures of luminous buried active galactic nuclei, url =
http://arxiv.org/abs/2101.12058, volume = 504, year = 2021

@articleMorganti2013b, abstract = High-resolution (0.5 arcsec) CO(2-1)
observations performed with the Atacama Large Millimetre/submillimetre Array
have been used to trace the kinematics of the molecular gas in the Seyfert 2
galaxy{IC~5063}. Although one of the most radio-loud Seyfert galaxy, IC~5063
is a relatively weak radio source (P_1.4GHz = 3 x 10^23 W Hz^-1). The data
reveal that the kinematics of the gas is very complex. A fast outflow of
molecular gas extends along the entire radio jet (~ 1 kpc), with the highest
outflow velocities about 0.5 kpc from the nucleus, at the location of the
brighter hot-spot in the W lobe. All the observed characteristics can be
described by a scenario of a radio plasma jet expanding into a clumpy medium,
interacting directly with the clouds and inflating a cocoon that drives a
lateral outflow into the interstellar medium. This suggests that most of the
observed cold molecular outflow is due to fast cooling of the gas after the
passage of a shock and that it is the end product of the cooling process.,
archivePrefix = arXiv, arxivId = 1504.04694, author = Morganti, Raffaella and
Fogasy, Judit and Paragi, Zsolt and Oosterloo, Tom and Orienti, Monica, doi =
10.1126/science.1240436, eprint = 1504.04694, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Morganti et al. - 2013 - Radio jets clearing the way
through a galaxy Watching feedback in action.pdf:pdf, isbn = 0036-8075, issn =
10959203, journal = Science (80-. )., number = 6150, pages = 1082–1085, pmid =
24009387, title = Radio jets clearing the way through a galaxy: Watching
feedback in action, volume = 341, year = 2013 @articleKaaret2022, abstract =
Chandra observations of the nearby, candidate Lyman-continuum (LyC) emitting
galaxy Tol 0440-381 show brightening of an X-ray source by at least a factor
of 4 to a luminosity of 1.6E40 erg/s over 3.8~days. The X-ray emission likely
arises from either a low-luminosity AGN or an ultraluminous X-ray source. The
properties of the X-ray source are similar to those found in Haro 11 and
Tololo 1247-232, the only other LyC-emitting galaxies that have been resolved
in X-rays. All three galaxies host luminous, variable, and hard spectrum X-ray
sources that are likely accretion-powered. Accretion onto compact objects
produces powerful outflows and ionizing radiation that could help enable LyC
escape., archivePrefix = arXiv, arxivId = 2201.03138, author = Kaaret, P. and
Bluem, J. and Prestwich, A. H., doi = 10.1093/mnrasl/slab127, eprint =
2201.03138, file = :home/william/Documents/Papers/2201.03138.pdf:pdf, keywords
= binaries,galaxies,individual,star formation,tol 0440-381,x-rays, number =
January, pages = 1–5, title = Rapid turn-on of a luminous X-ray source in the
candidate Lyman continuum emitting galaxy Tol 0440-381, url =
http://arxiv.org/abs/2201.03138%0Ahttp://dx.doi.org/10.1093/mnrasl/slab127,
volume = 5, year = 2022 @articleEdgar2004, abstract = If a point mass moves
through a uniform gas cloud, at what rate does it accrete material? This is
the question studied by Bondi, Hoyle and Lyttleton. This paper draws together
the work performed in this area since the problem was first studied. Time has
shown that, despite the simplifications made, Bondi, Hoyle and Lyttleton made
quite accurate predictions for the accretion rate. Bondi- Hoyle-Lyttleton
accretion has found application in many fields of astronomy, and these are
also discussed. 2004 Elsevier B.V. All rights reserved., archivePrefix =
arXiv, arxivId = astro-ph/0406166, author = Edgar, Richard, doi =
10.1016/j.newar.2004.06.001, eprint = 0406166, file =
:home/william/Documents/Papers/[Edgar R,.]-A Review of
Bondi–Hoyle–Lyttleton.pdf:pdf, issn = 13876473, journal = New Astron. Rev.,
keywords = Accretion, number = 10, pages = 843–859, primaryClass = astro-ph,
title = A review of Bondi-Hoyle-Lyttleton accretion, volume = 48, year = 2004
@articleGraur2015, abstract = Using a method to discover and classify
supernovae (SNe) in galaxy spectra, we detect 91 Type Ia SNe (SNe Ia) and 16
Type II SNe (SNe II) among ~740 000 galaxies of all types and ~215 000 star-
forming galaxies without active galactic nuclei, respectively, in Data Release
9 of the Sloan Digital Sky Survey. Of these SNe, 15 SNe Ia and eight SNe II
are new discoveries reported here for the first time. We use our SN samples to
measure SN rates per unit mass as a function of galaxy stellar mass, star-
formation rate (SFR), and specific SFR (sSFR), as derived by the MPA-JHU
Galspec pipeline. We show that correlations between SN Ia and SN II rates per
unit mass and galaxy stellar mass, SFR, and sSFR can be explained by a
combination of the respective SN delay-time distributions (the distributions
of times that elapse between the formation of a stellar population and all
ensuing SNe), the ages of the surveyed galaxies, the redshifts at which they
are observed, and their star formation histories. This model was first
suggested by Kistler et al. for the SN Ia rate-mass correlation, but is
expanded here to SNe II and to correlations with galaxy SFR and sSFR. Finally,
we measure a volumetric SN II rate at redshift 0.075 of RII, V =
0.621-0.154+0.197 (stat)-0.063+0.024 (sys) × 10-4 yr-1 Mpc-3. Assuming that
SNe IIP and IIL account for 60 per cent of all core-collapse (CC) SNe, the CC
SN rate is RCC, V = 1.04-0.26+0.33 (stat)-0.11+0.04 (sys) × 10-4 yr-1 Mpc-3.,
archivePrefix = arXiv, arxivId = 1412.7991, author = Graur, Or and Bianco,
Federica B. and Modjaz, Maryam, doi = 10.1093/mnras/stv713, eprint =
1412.7991, file = :home/william/Documents/Papers/1412.7991.pdf:pdf, issn =
13652966, journal = Mon. Not. R. Astron. Soc., keywords = Methods:
observational,Supernovae: general,Surveys, number = 1, pages = 905–925, title
= A unified explanation for the supernova rate-galaxy mass dependence based on
supernovae detected in Sloan galaxy spectra, volume = 450, year = 2015
@articleMcGaugh2012, abstract = The baryonic Tully-Fisher relation (BTFR) is
an empirical relation between baryonic mass and rotation velocity in disk
galaxies. It provides tests of galaxy formation models in $\Lambda$CDM and of
alternative theories like modified Newtonian dynamics (MOND). Observations of
gas-rich galaxies provide a measure of the slope and normalization of the BTFR
that is more accurate (if less precise) than that provided by star-dominated
spirals, as their masses are insensitive to the details of stellar population
modeling. Recent independent data for such galaxies are consistent with M b =
AV 4f with A = 47 6 M km -4 s 4. This is equivalent to MOND with a 0 = 1.3 0.3
s -2. The scatter in the data is consistent with being due entirely to
observational uncertainties. It is unclear why the physics of galaxy formation
in $\Lambda$CDM happens to pick out the relation predicted by MOND. We
introduce a feedback efficacy parameter to relate halo properties to those of
the galaxies they host. correlates with star formation rate and gas fraction
in the sense that galaxies that have experienced the least star formation have
been most impacted by feedback. 2012. The American Astronomical Society. All
rights reserved., archivePrefix = arXiv, arxivId = 1107.2934, author =
McGaugh, Stacy S., doi = 10.1088/0004-6256/143/2/40, eprint = 1107.2934, file
= :home/william/Documents/Papers/[McGaugh]-The Baryonic Tully-Fisher Relation
of Gas-rich Galaxies as a Test of $\Lambda$CDM and MOND.pdf:pdf, issn =
00046256, journal = Astron. J., keywords = galaxies: dwarf,galaxies:
irregular,galaxies: kinematics and dynamics,galaxies: spiral, number = 2,
title = The baryonic tully-fisher relation of gas-rich galaxies as a test of
$\Lambda$cDM and MOND, volume = 143, year = 2012 @articlePaulM.Muchinsky2012,
abstract = Predicting the binding mode of flexible polypeptides to proteins is
an important task that falls outside the domain of applicability of most small
molecule and protein−protein docking tools. Here, we test the small molecule
flexible ligand docking program Glide on a set of 19 non-$\alpha$-helical
peptides and systematically improve pose prediction accuracy by enhancing
Glide sampling for flexible polypeptides. In addition, scoring of the poses
was improved by post-processing with physics-based implicit solvent MM- GBSA
calculations. Using the best RMSD among the top 10 scoring poses as a metric,
the success rate (RMSD ≤ 2.0 Å for the interface backbone atoms) increased
from 21% with default Glide SP settings to 58% with the enhanced peptide
sampling and scoring protocol in the case of redocking to the native protein
structure. This approaches the accuracy of the recently developed Rosetta
FlexPepDock method (63% success for these 19 peptides) while being over 100
times faster. Cross-docking was performed for a subset of cases where an
unbound receptor structure was available, and in that case, 40% of peptides
were docked successfully. We analyze the results and find that the optimized
polypeptide protocol is most accurate for extended peptides of limited size
and number of formal charges, defining a domain of applicability for this
approach., archivePrefix = arXiv, arxivId = arXiv:1011.1669v3, author =
Hollenbach, D., doi = 10.1017/CBO9781107415324.004, eprint =
arXiv:1011.1669v3, file =
:home/william/Documents/Papers/1979ApJS…41..555H.pdf:pdf, isbn =
9788578110796, issn = 1098-6596, journal = Astrophys. J., keywords = icle,
number = 9, pages = 1689–1699, pmid = 25246403, title = MOLECULE FORMATION AND
INFRARED EMISSION IN FAST INTERESTELLAR SHOCK. I-PHYSICAL PROCESSES, volume =
53, year = 1979 @articleChen2020, 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] $\lambda$5007 outflow with one of the highest energy-ejection rates at
z 1.6. 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 3.0 × 1043 erg s−1 assuming Compton-thick obscuration (NH = 1.5 ×
1024 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/Chen_2020_ApJL_905_L2.pdf:pdf, issn = 23318422,
journal = arXiv, keywords = Active galaxies,ULIRG,X-ray AGN, number = 1, pages
= L2, publisher = IOP Publishing, title = NuSTAR Non-detection of a faint
active galactic nucleus in an ultraluminous IR galaxy with Kpc-scale fast
wind, url = http://dx.doi.org/10.3847/2041-8213/abca30, volume = 905, year =
2020 @articleLopez-Rodriguez2019, abstract = We report the first detection of
galactic spiral structure by means of thermal emission from magnetically
aligned dust grains. Our 89 µm polarimetric imaging of NGC 1068 with the High-
resolution Airborne Wideband Camera/Polarimeter (HAWC+) on NASAs Stratospheric
Observatory for Infrared Astronomy (SOFIA) also sheds light on magnetic field
structure in the vicinity of the galaxys inner-bar and active galactic nucleus
(AGN). We find correlations between the 89 µm magnetic field vectors and other
tracers of spiral arms, and a symmetric polarization pattern as a function of
the azimuthal angle arising from the projection and inclination of the disk
field component in the plane of the sky. The observations can be fit with a
logarithmic spiral model with pitch angle of 16.9−+22..78◦ and a disk
inclination of 48 ± 2◦. We infer that the bulk of the interstellar medium from
which the polarized dust emission originates is threaded by a magnetic field
that closely follows the spiral arms. Inside the central starburst disk ( 1.6
kpc), the degree of polarization is found to be lower than for far-infrared
sources in the Milky Way, and has minima at the locations of most intense star
formation near the outer ends of the inner-bar. Inside the starburst ring, the
field direction deviates from the model, becoming more radial along the
leading edges of the inner-bar. The polarized flux and dust temperature peak ∼
3 − 600 NE of the AGN at the location of a bow shock between the AGN outflow
and the surrounding interstellar medium, but the AGN itself is weakly
polarized ( 1%) at both 53 and 89 µm., archivePrefix = arXiv, arxivId =
1907.06648, author = Lopez-Rodriguez, Enrique and Dowell, C. Darren and Jones,
Terry J. and Harper, Doyal A. and Berthoud, Marc and Chuss, David and Dale,
Daniel A. and Guerra, Jordan A. and Hamilton, Ryan T. and Looney, Leslie W.
and Michail, Joseph M. and Nikutta, Robert and Novak, Giles and Santos, Fabio
P. and Sheth, Kartik and Siah, Javad and Staguhn, Johannes and Stephens, Ian
W. and Tassis, Konstantinos and Trinh, Christopher Q. and Ward-Thompson, Derek
and Werner, Michael and Wollack, Edward J. and Zweibel, Ellen G., doi =
10.3847/1538-4357/ab5849, eprint = 1907.06648, file =
:home/william/Documents/Papers/1907.06648.pdf:pdf, issn = 23318422, journal =
arXiv, keywords = Galaxies - techniques,Individual (NGC 1068) -
galaxies,Infrared,Magnetic fields,Polarimetric - galaxies, title = SOFIA/HAWC+
traces the magnetic fields in NGC 1068, year = 2019 @articleCorrea2019,
abstract = Ultra-Luminous Infrared Galaxies (ULIRGs) are the most luminous
objects in the infrared sky. With infrared luminosities exceeding 1012 solar
luminosities, ULIRGs contain strong star formation regions which could power
hadronic acceleration. Moreover, a significant fraction of ULIRGs have been
found to host Active Galactic Nuclei, which could also be a source of hadronic
acceleration. Furthermore, such high infrared luminosities indicate that large
amounts of dust are present in these objects. In the presence of hadronic
acceleration, this dust not only represents an excellent target for high-
energy neutrino production through the pp-channel, but it could also attenuate
a significant fraction of the gamma rays that are produced in this process.
This could relieve the apparent tension between the diffuse IceCube neutrino
flux and the diffuse gamma-ray flux measured by Fermi-LAT. We present our
source selection criteria and IceCube sensitivities in view of a search for
high-energy neutrinos from these so far unexplored objects., archivePrefix =
arXiv, arxivId = 1908.05137, author = Correa, Pablo and De Vries, Krijn D. and
Van Eijndhoven, Nick, doi = 10.22323/1.358.0860, eprint = 1908.05137, file =
:home/william/Documents/Papers/1908.05137.pdf:pdf, issn = 23318422, journal =
arXiv, title = Investigation of Ultra-Luminous Infrared Galaxies as obscured
high-energy neutrino source candidates, year = 2019 @articleLonginotti2018,
abstract = We report on the coexistence of powerful gas outflows observed in
millimeter and X-ray data of the Radio-Loud Narrow Line Seyfert 1 Galaxy IRAS
17020+4544. Thanks to the large collecting power of the Large Millimeter
Telescope, a prominent line arising from the 12CO(1-0) transition was revealed
in recent observations of this source. The complex profile is composed by a
narrow double-peak line and a broad wing. While the double-peak structure may
be arising in a disk of molecular material, the broad wing is interpreted as
the signature of a massive outflow of molecular gas with an approximate bulk
velocity of -660 km/s. This molecular wind is likely associated to a multi-
component X-ray Ultra-Fast Outflow with velocities reaching up to ~0.1c and
column densities in the range 10^{21-23.9} cm^-2 that was reported in the
source prior to the LMT observations. The momentum load estimated in the two
gas phases indicates that within the observational uncertainties the outflow
is consistent with being propagating through the galaxy and sweeping up the
gas while conserving its energy. This scenario, which has been often
postulated as a viable mechanism of how AGN feedback takes place, has so far
been observed only in ULIRGs sources. IRAS 17020+4544 with bolometric and
infrared luminosity respectively of 5X10^{44} erg/s and 1.05X10^{11} L_sun
appears to be an example of AGN feedback in a NLSy1 Galaxy (a low power AGN).
New proprietary multi-wavelength data recently obtained on this source will
allow us to corroborate the proposed hypothesis., archivePrefix = arXiv,
arxivId = 1810.01941, author = Longinotti, A. L. and Vega, O. and Krongold, Y.
and Aretxaga, I. and Yun, M. and Chavushyan, V. and Feruglio, C. and Gomez-
Ruiz, A. and Montaña, A. and Leon-Tavares, J. and Olguın-Iglesias, A. and
Giroletti, M. and Guainazzi, M. and Kotilainen, J. and Panessa, F. and Zapata,
L. A. and Cruz-Gonzalez, I. and Patiño-Alvarez, V. M. and Rosa-Gonzalez, D.
and Carramiñana, A. and Carrasco, L. and Costantini, E. and Dultzin, D. and
Guichard, J. and Puerari, I. and Santos-Lleo, M., eprint = 1810.01941, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Longinotti et al. - 2018 - Early Science with the Large
Millimeter Telescope an energy-driven wind revealed by massive molecular and
fas.pdf:pdf, pages = 1–9, title = Early Science with the Large Millimeter
Telescope: an energy-driven wind revealed by massive molecular and fast X-ray
outflows in the Seyfert Galaxy IRAS 17020+4544, url =
http://arxiv.org/abs/1810.01941, year = 2018 @articleRiffel2021, abstract = We
present maps for the electron temperature in the inner kpc of three luminous
Seyfert galaxies: Mrk 79, Mrk 348, and Mrk 607 obtained from Gemini Multi-
Object Spectrograph-integral field unit observations at spatial resolutions of
∼110–280 pc. We study the distributions of electron temperature in active
galaxies and find temperatures varying in the range from ∼8000 to 30 000 K.
Shocks due to gas outflows play an important role in the observed temperature
distributions of Mrk 79 and Mrk 348, while standard photoionization models
reproduce the derived temperature values for Mrk 607. In Mrk 79 and Mrk 348,
we find direct evidence for shock ionization with overall orientation
orthogonal to the ionization axis, where shocks can be easily observed as the
active galactic nuclei radiation field is shielded by the nuclear dusty torus.
This also indicates that even when the ionization cones are narrow, the shocks
can be much wider angle., archivePrefix = arXiv, arxivId = 2012.02013, author
= Riffel, R. A. and Dors, O. L. and Armah, M. and Storchi-Bergmann, T. and
Feltre, A. and Hägele, G. F. and Cardaci, M. V. and Ruschel-Dutra, D. and
Krabbe, A. C. and Pérez-Montero, E. and Zakamska, N. L. and Freitas, I. C.,
doi = 10.1093/mnrasl/slaa194, eprint = 2012.02013, file =
:home/william/Documents/Papers/2021MNRAS.501L..54R.pdf:pdf, issn = 17453933,
journal = Mon. Not. R. Astron. Soc. Lett., keywords = Galaxies: ISM,Galaxies:
Seyfert,Galaxies: abundances,Galaxies: active, number = 1, pages = L54–L59,
title = Chemical abundances in Seyfert galaxies – V. The discovery of shocked
emission outside the AGN ionization axis, volume = 501, year = 2021
@articleSutherland2017, abstract = In this paper we treat the pre-ionisation
problem in shocks over the velocity range $10 v_{s} 1500$$\backslash$,km/s in
a self-consistent manner. We identify four distinct classes of solution
controlled by the value of the shock precursor parameter, $= {Q}/v_s$, where
${Q}$ is the ionization parameter of the UV photons escaping upstream. This
parameter determines both the temperature and the degree of ionisation of the
gas entering the shock. In increasing velocity the shock solution regimes are
cold neutral precursors ($v_s 40$$\backslash$,km/s), warm neutral precursors
($40 v_s 75$$\backslash$,km/s), warm partly-ionized precursors ($75 v_s
120$$\backslash$,km/s), and fast shocks in which the pre-shock gas is in
photoionisation equilibrium, and is fully ionized. The main effect of a
magnetic field is to push these velocity ranges to higher values, and to limit
the post-shock compression. In order to facilitate comparison with
observations of shocks, we provide a number of convenient scaling
relationships for parameters such as post-shock temperature, compression
factors, cooling lengths, and H$$ and X-ray luminosity., archivePrefix =
arXiv, arxivId = 1702.07453, author = Sutherland, Ralph S. and Dopita, Michael
A., doi = 10.3847/1538-4365/aa6541, eprint = 1702.07453, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Sutherland, Dopita - 2017 - Effects of Pre-ionisation in
Radiative Shocks I Self-Consistent Models.pdf:pdf, issn = 1538-4365, journal =
Astrophys. J. Suppl. Ser., keywords = atomic data,atomic data,atomic
processes,radiative transfer,sh,atomic processes,machine-readable
tables,radiative transfer,shock waves,supporting material, number = 2, pages =
34, publisher = IOP Publishing, title = Effects of Pre-ionisation in Radiative
Shocks I: Self-Consistent Models, url =
http://arxiv.org/abs/1702.07453%0Ahttp://dx.doi.org/10.3847/1538-4365/aa6541,
volume = 229, year = 2017 @articlePereira-Santaella2020, abstract = We used
high-spatial resolution (70 pc; 0$ {{{}{.}}} $3) CO multi-transition (J = 1-0,
2-1, 4-3, and 6-5) ALMA data to study the physical conditions and kinematics
of the cold molecular outflow in the local luminous infrared galaxy (LIRG) ESO
320-G030 (d = 48 Mpc, LIR/L = 1011.3). ESO 320-G030 is a double-barred
isolated spiral, but its compact and obscured nuclear starburst (SFR ∼15 M
yr-1; AV ∼40 mag) resembles those of ultra-luminous infrared galaxies (LIR/L
1012). In the outflow, the CO(1-0)/CO(2-1) ratio is enhanced with respect to
the rest of the galaxy and the CO(4-3) transition is undetected. This
indicates that the outflowing molecular gas is less excited than the molecular
gas in the nuclear starburst (i.e., outflow launching site) and in the galaxy
disk. Non-local thermodynamic equilibrium radiative transfer modeling reveals
that the properties of the molecular clouds in the outflow differ from those
of the nuclear and disk clouds: The kinetic temperature is lower (Tkin ∼ 9 K)
in the outflow, and the outflowing clouds have lower column densities.
Assuming a 10-4 CO abundance, the large internal velocity gradients, 60-45+250
km s-1 pc-1, imply that the outflowing molecular clouds are not bound by self-
gravity. All this suggests that the life-cycle (formation, collapse,
dissipation) of the galaxy disk molecular clouds might differ from that of the
outflowing molecular clouds which might not be able to form stars. The low
kinetic temperature of the molecular outflow remains constant at radial
distances between 0.3 and 1.7 kpc. This indicates that the heating by the
hotter ionized outflow phase is not efficient and may favor the survival of
the molecular gas phase in the outflow. The spatially resolved velocity
structure of the outflow shows a 0.8 km s-1 pc-1 velocity gradient between 190
pc and 560 pc and then a constant maximum outflow velocity of about 700-800 km
s-1 up to 1.7 kpc. This could be compatible with a pure gravitational
evolution of the outflow, which would require coupled variations of the mass
outflow rate and the outflow launching velocity distribution. Alternatively, a
combination of ram pressure acceleration and cloud evaporation could explain
the observed kinematics and the total size of the cold molecular phase of the
outflow., archivePrefix = arXiv, arxivId = 2009.08481, author = Pereira-
Santaella, M. and Colina, L. and García-Burillo, S. and González-Alfonso, E.
and Alonso-Herrero, A. and Arribas, S. and Cazzoli, S. and Piqueras-López, J.
and Rigopoulou, D. and Usero, A., doi = 10.1051/0004-6361/202038838, eprint =
2009.08481, file = :home/william/Documents/Papers/2009.08481.pdf:pdf, issn =
14320746, journal = Astron. Astrophys., keywords = Galaxies: ISM,Galaxies:
nuclei,ISM: molecules,Infrared: galaxies, title = Excitation and acceleration
of molecular outflows in LIRGs: The extended ESO 320-G030 outflow on 200-pc
scales, volume = 643, year = 2020 @articleChoi2014, abstract = Quantum
dynamics of light waves traveling through a time-varying turbulent plasma is
investigated via the SU(1,1) Lie algebraic approach. Plasma oscillations that
accompany time-dependence of electromagnetic parameters of the plasma are
considered. In particular, we assume that the conductivity of plasma involves
a sinusoidally varying term in addition to a constant one. Regarding the time
behavior of electromagnetic parameters in media, the light fields are modeled
as a modified CK (Caldirola-Kanai) oscillator that is more complex than the
standard CK oscillator. Diverse quantum properties of the system are analyzed
under the consideration of time-dependent characteristics of electromagnetic
parameters. Quantum energy of the light waves is derived and compared with the
counterpart classical energy. Gaussian wave packet of the field whose
probability density oscillates with time like that of classical states is
constructed through a choice of suitable initial condition and its quantum
behavior is investigated in detail. Our development presented here provides a
useful way for analyzing time behavior of quantized light in complex plasma.,
author = Choi, Jeong Ryeol, doi = 10.1038/srep06880, file =
:home/william/Documents/Papers/may.srep06880.pdf:pdf, issn = 20452322, journal
= Sci. Rep., pages = 1–7, title = A novel method for analyzing complicated
quantum behaviors of light waves in oscillating turbulent plasma, volume = 4,
year = 2014 @articleHarrison2018a, abstract = It is the twentieth anniversary
of the publication of the seminal papers by Magorrian et al. and Silk & Rees
which, along with other related work, ignited an explosion of publications
connecting active galactic nuclei (AGN)-driven outflows to galaxy evolution.
With a surge in observations of AGN outflows, studies are attempting to
directly test AGN feedback models using the outflow properties. With a focus
on outflows traced by optical and CO emission lines, we discuss significant
challenges which greatly complicate this task from both an observational and
theoretical perspective. We highlight observational uncertainties involved,
and the assumptions required, when deriving kinetic coupling efficiencies
(i.e., outflow kinetic power as a fraction of AGN luminosity) from typical
observations. Based on recent models we demonstrate that extreme caution
should taken when comparing observationally-derived kinetic coupling
efficiencies to coupling efficiencies from fiducial feedback models.,
archivePrefix = arXiv, arxivId = 1802.10306, author = Harrison, C. M. and
Costa, T. and Tadhunter, C. N. and Flütsch, A. and Kakkad, D. and Perna, M.
and Vietri, G., doi = 10.1038/s41550-018-0403-6, eprint = 1802.10306, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Harrison et al. - 2018 - AGN outflows and feedback twenty
years on.pdf:pdf, issn = 23973366, journal = Nat. Astron., number = 3, pages =
198–205, title = AGN outflows and feedback twenty years on, volume = 2, year =
2018 @articleDrzazga2011, abstract = Aims. Violent gravitational interactions
can change the morphologies of galaxies and, by means of merging, transform
them into elliptical galaxies. We aim to investigate how they affect the
evolution of galactic magnetic fields. Methods. We selected 16 systems of
interacting galaxies with available VLA archive radio data at 4.86 and 1.4 GHz
and compared their radio emission and estimated magnetic field strengths with
their star-forming activity, far-infrared emission, and the stage of tidal
interaction. Results. The estimated mean of total magnetic field strength for
our sample of interacting galaxies is 14 ± 5 $\mu$G, which is larger than for
the non-interacting objects. The field regularity (of 0.27 ± 0.09) is lower
than in typical spirals and indicates enhanced production of random magnetic
fields in the interacting objects. We find a general evolution of magnetic
fields: for weak interactions the strength of magnetic field is almost
constant (10−15 $\mu$G) as interaction advances, then it increases up to 2×,
peaks at the nuclear coalescence (25 $\mu$G), and decreases again, down to 5−6
$\mu$G, for the post-merger remnants. The main production of magnetic fields
in colliding galaxies thus terminates somewhere close to the nuclear
coalescence, after which magnetic field diffuses. The magnetic field strength
for whole galaxies is weakly affected by the star formation rate (SFR), while
the dependence is higher for galactic centres. We show that the morphological
distortions visible in the radio total and polarized emission do not depend
statistically on the global or local SFRs, while they do increase (especially
in the polarization) with the advance of interaction. The constructed radio-
far-infrared relations for interacting and non-interacting galaxies display a
similar balance between the generation of cosmic rays, magnetic fields, and
the production of the thermal energy and dust radiation. Conclusions. The
regular magnetic fields are much more sensitive to morphological distortions
induced by tidal interactions than are the random fields. As a result the
polarized emission could be yet another indicator of an ongoing merging
process. The found evolution of magnetic field with advancing interaction
would definitely imply a stronger effect of magnetic fields on the galaxy
surroundings in the earlier cosmological epochs. The process of strong
gravitational interactions can efficiently magnetize the merger’s
surroundings, having a similar magnetizing effect on intergalactic medium as
supernova explosions or galactic winds. If interacting galaxies generate some
ultra-high energy cosmic rays (UHECRs), the disk or magnetized outflows can
deflect them (up to 23 •), and make an association of the observed UHECRs with
the sites of their origin very uncertain., author = Drzazga, R T and Chy˙, K T
and Jurusik, W and Wiórkiewicz, K, file =
:home/william/Documents/Papers/aa16092-10.pdf:pdf, journal = a&a, keywords =
galaxies,general – galaxies,interactions – radio continuum,magnetic fields –
galaxies, title = Magnetic field evolution in interacting galaxies, url =
https://www.aanda.org/articles/aa/pdf/2011/09/aa16092-10.pdf, volume = 533,
year = 2011 @incollectionPeterson2006, abstract = Reverberation mapping is a
proven technique that is used to measure the size of the broad emission-line
region and central black hole mass in active galactic nuclei. More ambitious
reverberation mapping programs that are well within the capabilities of Hubble
Space Telescope could allow us to determine the nature and flow of line-
emitting gas in active nuclei and to assess accurately the systematic
uncertainties in reverberation-based black hole mass measurements.,
archivePrefix = arXiv, arxivId = astro-ph/0407538, author = Peterson, B. M.
and Horne, K., booktitle = Planets to Cosmol. Essent. Sci. Final Years Hubble
Sp. Telesc., doi = 10.1017/CBO9780511536328.009, eprint = 0407538, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Peterson, Horne - 2006 - Reverberation mapping of active
galactic nuclei.pdf:pdf, isbn = 9780511536328, issn = 0004-6280, pages =
89–98, pmid = 15003161, primaryClass = astro-ph, title = Reverberation mapping
of active galactic nuclei, volume = 9780521847, year = 2006
@articleSchawinski2015, abstract = We present an observational constraint for
the typical active galactic nucleus (AGN) phase lifetime. The argument is
based on the time lag between an AGN central engine switching on and becoming
visible in X-rays, and the time the AGN then requires to photoionize a large
fraction of the host galaxy. Based on the typical light travel time across
massive galaxies, and the observed fraction of X-ray-selected AGN without AGN-
photoionized narrow lines, we estimate that the AGN phase typically lasts ~105
yr. This lifetime is short compared to the total growth time of 107-109 yr
estimated from e.g. the Soltan argument and implies that black holes grow via
many such short bursts and that AGN therefore ’flicker’ on and off. We discuss
some consequences of this flickering behaviour for AGN feedback and the
analogy of X-ray binaries and AGN lifecycles., archivePrefix = arXiv, arxivId
= 1505.06733, author = Schawinski, Kevin and Koss, Michael and Berney, Simon
and Sartori, Lia F., doi = 10.1093/mnras/stv1136, eprint = 1505.06733, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Schawinski et al. - 2015 - Active galactic nuclei flicker
An observational estimate of the duration of black hole growth phases of
~105.pdf:pdf, issn = 13652966, journal = Mon. Not. R. Astron. Soc., keywords =
Galaxies: Seyfert,Galaxies: active,Quasars: general, number = 3, pages =
2517–2523, title = Active galactic nuclei flicker: An observational estimate
of the duration of black hole growth phases of ~10⁵ yr, volume = 451, year =
2015 @articlePogge2011, author = Pogge, Richard W, file =
:home/william/Documents/Papers/Intro.pdf:pdf, journal = Osu Ast871, pages =
1–25, title = Ch. 1 - Introduction to the Interstellar Medium, url =
http://www.astronomy.ohio-state.edu/
pogge/Ast871/Notes/Intro.pdf%5Cnpapers2://publication/uuid/0A47944A-0ACC-4021-B7A0-641FA416EC18,
year = 2011 @articleMorganti2021, abstract = We present an update of our
ongoing project to characterise the impact of radio jets on the interstellar
medium (ISM). This is done by tracing the distribution, kinematics and
excitation of the molecular gas at high spatial resolution using ALMA. The
radio active galactic nuclei (AGN) studied are in the interesting phase of
having a recently born radio jet. In this stage, the plasma jets can have the
largest impact on the ISM, as also predicted by state-of-the-art simulations.
The two targets we present have quite different ages, allowing us to get
snapshots of the effects of radio jets as they grow and evolve. Interestingly,
both also host powerful quasar emission, making them ideal for studying the
full impact of AGN. The largest mass outflow rate of molecular gas is found in
a radio galaxy () hosting a newly born radio jet still in the early phase of
emerging from an obscuring cocoon of gas and dust. Although the molecular mass
outflow rate is high (few hundred), the outflow is limited to the inner few
hundred pc region. In a second object (), the jet is larger (a few kpc) and is
in a more advanced evolutionary phase. In this object, the distribution of the
molecular gas is reminiscent of what is seen, on larger scales, in cool-core
clusters hosting radio galaxies. Interestingly, gas deviating from quiescent
kinematics (possibly indicating an outflow) is not very prominent, limited
only to the very inner region, and has a low mass outflow rate. Instead, on
kpc scales, the radio lobes appear associated with depressions in the
distribution of the molecular gas. This suggests that the lobes have broken
out from the dense nuclear region. However, the AGN does not appear to be
able, at present, to stop the star formation observed in this galaxy. These
results support the idea that the effects of the radio source start in the
very first phases by producing outflows which, however, tend to be limited to
the kpc region. After that, the effects turn into producing large-scale
bubbles which could, in the long term, prevent the surrounding gas from
cooling. Thus, our results provide a way to characterise the effect of radio
jets in different phases of their evolution and in different environments,
bridging the studies done for radio galaxies in clusters., archivePrefix =
arXiv, arxivId = 2005.04765, author = Morganti, Raffaella and Oosterloo, Tom
and Tadhunter, Clive N., doi = 10.1017/S1743921320001775, eprint = 2005.04765,
file = :home/william/Documents/Papers/2109.13516.pdf:pdf, issn = 17439221,
journal = Proc. Int. Astron. Union, keywords = ISM: jets and
outflows,galaxies: active,galaxies: jets,radio continuum: galaxies, pages =
243–248, title = Taking snapshots of the jet-ISM interplay with ALMA, volume =
359, year = 2021

@article2002A&A…392..267R, author = Raga, A.~C. and de Gouveia Dal Pino, E.~M.
and Noriega-Crespo, A and Mininni, P.~D. and Velázquez, P.~F., doi =
10.1051/0004-6361:20020851, file = :home/william/.local/share/data/Mendeley
Ltd./Mendeley Desktop/Downloaded/Raga et al. - 2002 - Jetcloud collision, 3D
gasdynamic simulations of HH 110.pdf:pdf, journal = aap, keywords = ISM:
Herbig-Haro objects,ISM: individual (HH 110),ISM: jets and outflows,ISM:
kinematics and dynamics,shock waves, pages = 267–276, title = Jet/cloud
collision, 3D gasdynamic simulations of HH 110, volume = 392, year = 2002
@articleYoon2019, abstract = In AGN feedback study, it is crucial to precisely
determine the accretion rate of AGN and properly adopt the AGN physics, since
they determine the AGN radiation and wind outputs. One key feature of such an
AGN physics is that, depending on the value of the accretion rate, accretion
is divided into two modes, namely hot and cold, corresponding to below and
above $2\% L_{Edd}$ respectively. In this paper we investigate the role of the
hot mode by performing hydrodynamical numerical simulations of AGN feedback in
an isolated elliptical galaxy. We have run two test models. In one model, we
always adopt the cold mode accretion physics no matter what value the
accretion rate is; in another model, we turn off the AGN outputs once the
accretion is in the hot mode. We have calculated the AGN light curves, black
hole growth, star formation, and AGN energy duty-cycle and compared the
results of these two models with the model in which the two modes are
correctly taken into account. Important differences are found. For example, if
we would adopt only the cold mode, compared to the model considering both
modes, the AGN luminosity would become significantly smaller, the total mass
of newly formed stars would become two orders of magnitude smaller, and the
fraction of energy ejected within the high accretion regime (i.e., $L_{BH} 2\%
L_{Edd}$) would be very small ($10^{-3}$), inconsistent with observations.
These results strongly indicate the importance of hot mode feedback, which is
because the time fraction of being in this mode is very large. We have also
investigated the roles of wind and radiation in the hot mode and found that
usually wind is more important than radiation; but, depending on the problem,
radiation also cannot be neglected., archivePrefix = arXiv, arxivId =
1901.07570, author = Yoon, Doosoo and Yuan, Feng and Ostriker, Jeremiah P. and
Ciotti, Luca, eprint = 1901.07570, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley Desktop/Downloaded/Yoon
et al. - 2019 - On the Role of Hot Feedback Mode in Active Galactic Nuclei
Feedback in an Elliptical Galaxy.pdf:pdf, keywords = accretion,accretion disks
- black,active - galaxies,evolution -,hole physics - galaxies, title = On the
Role of Hot Feedback Mode in Active Galactic Nuclei Feedback in an Elliptical
Galaxy, url = http://arxiv.org/abs/1901.07570, year = 2019
@articleOrienti2017, author = Orienti, Monica, doi =
10.1164/rccm.200806-848OC, file = :home/william/.local/share/data/Mendeley
Ltd./Mendeley Desktop/Downloaded/King et al. - 2017 - Fo r R iew On Fo r R iew
On ly.pdf:pdf, isbn = 9781509037582, journal = Proocedings, Perseus in Sicily,
pages = 1–60, title = Extragalactic relativistic jets, year = 2017
@articleMarchiolli1997, abstract = We begin by revisiting the so-called
Caldirola-Kanai Hamiltonian and discuss its inherent ambiguity: does it
represent a dissipative harmonic oscillator (HO) subject to a friction force,
or does it describe an HO with a time-dependent mass (TDM)? Although
classically both descriptions do coexist, in the quantum domain the solution
of the Schrödinger equation (or Heisenberg equations of motion) with a TDM
does not present inconsistencies, however, the dissipative Hamiltonian shows
violation of the Heisenberg uncertainty principle. This violation is avoided
by introducing a stochastic force in the equations of motion, which will take
care of the fluctuations due to the environment. Once the distinction between
the dissipative and amplifying Hamiltonian is made clear, we consider the
problem of the quantum TDM HO subject to dissipation, showing that both
phenomena may be merged and described by a single Hamiltonian, the amplifying-
dissipative Hamiltonian. We obtain the solutions of the Heisenberg equations
of motion for the canonical momentum and position; next, we specialize on the
weak damping limit and analyse the effects of the amplifying-dissipative
process on the mean values of the physical variables., author = Marchiolli,
Marcelo A. and Mizrahi, Salomon S., doi = 10.1088/0305-4470/30/8/011, file =
:home/william/Documents/Papers/marchiolli1997.pdf:pdf, issn = 03054470,
journal = J. Phys. A. Math. Gen., number = 8, pages = 2619–2635, title =
Dissipative mass-accreting quantum oscillator, volume = 30, year = 1997
@articleWagner2011, abstract = Over cosmic time, galaxies grow through the
hierarchical merging of smaller galaxies. However, the bright region of the
galaxy luminosity function is incompatible with the simplest version of
hierarchical merging, and it is believed that feedback from the central black
hole in the host galaxies reduces the number of bright galaxies and regulates
the co-evolution of the black hole and host galaxy. Numerous simulations of
galaxy evolution have attempted to include the physical effects of such
feedback with a resolution usually exceeding a kiloparsec. However,
interactions between jets and the interstellar medium involve processes
occurring on less than kiloparsec scales. In order to further the
understanding of processes occurring on such scales, we present a suite of
simulations of relativistic jets interacting with a fractal two-phase
interstellar medium with a resolution of two parsecs and a largest scale of
one kiloparsec. The transfer of energy and momentum to the interstellar medium
is considerable, and we find that jets with powers in the range of 10 43-1046
erg s-1 can inhibit star formation through the dispersal of dense gas in the
galaxy core. We determine the effectiveness of this process as a function of
the ratio of the jet power to the Eddington luminosity of the black hole, the
pressure of the interstellar medium, and the porosity of the dense gas. 2011.
The American Astronomical Society., archivePrefix = arXiv, arxivId = astro-
ph.CO/1012.1092, author = Wagner, A. Y. and Bicknell, G. V., doi =
10.1088/0004-637X/728/1/29, eprint = 1012.1092, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Wagner, Bicknell - 2011 - Relativistic jet feedback in
evolving galaxies.pdf:pdf, isbn = 0004-637X, issn = 15384357, journal =
Astrophys. J., keywords = Galaxies: evolution,Galaxies: formation,Galaxies:
jets,Hydrodynamics,ISM: jets and outflows,Methods: numerical, number = 1,
primaryClass = astro-ph.CO, title = Relativistic jet feedback in evolving
galaxies, volume = 728, year = 2011 @articleDeconto-Machado2022, abstract = We
analyse the kinematics of 170 AGN host galaxies as compared to those of a
matched control sample of non-active galaxies from the MaNGA survey in order
to characterise and estimate the extents of the Narrow Line Region (NLR) and
of the kinematically disturbed region (KDR) by the AGN. We define the observed
NLR radius as the farthest distance from the nucleus within which both
[Oiii]/H$\backslash$beta and [Nii]/H$\backslash$alpha ratios fall in the AGN
region of the BPT diagram and the H$\backslash$alpha equivalent width is
required to be larger than 3.0$\backslash$AA. The extent of the KDR is defined
as the distance from the nucleus within which the AGN hosts galaxies shows a
more disturbed gas kinematics than the control galaxies. The kinematics
derived from the [Oiii] line profiles reveal that, on average, the most
luminous AGN (L[Oiii] 3.8 * 10^40 erg s^-1) possess higher residual difference
between the gaseous and stellar velocities and velocities dispersion than
their control galaxies. Spatially resolved NLR’s and KDR’s were found in 55
and 46 AGN host galaxies, with corrected radii 0.2 r_KDR,c 2.3 kpc and 0.4
r_NLR,c 10.1 kpc, with a relation between the two given by log r_KDR,c =
(0.53$\backslash$pm0.12) log r_NLR,c + (1.07$\backslash$pm0.22), respectively.
The extension of the KDR corresponds to about 30 per cent of that of the NLR.
Assuming that the KDR is due to an AGN outflow, we have estimated ionised gas
mass outflow rates that range between 10^-5 and $\backslash$approx 1 Myr^-1,
and kinetic powers that range from 10^34 to 10^40 erg s^-1. Comparing the
power of the AGN ionised outflows with the AGN luminosities, they are always
below the 0.05 L_AGN model threshold for having an important feedback effect
on their respective host galaxies. The mass outflow rates (and power) of our
AGN sample correlate with their luminosities, populating the lowest AGN
luminosity range of the correlations previously found for more powerful
sources., archivePrefix = arXiv, arxivId = 2201.01690, author = Deconto-
Machado, A. and Riffel, R. A. and Ilha, G. S. and Rembold, S. B. and Storchi-
Bergmann, T. and Riffel, R. and Schimoia, J. S. and Schneider, D. P. and
Bizyaev, D. and Feng, S. and Wylezalek, D. and da Costa, L. N. and do
Nascimento, J. C. and Maia, M. A. G., doi = 10.1051/0004-6361/202140613,
eprint = 2201.01690, file = :home/william/Documents/Papers/2201.01690.pdf:pdf,
issn = 0004-6361, keywords = active,galaxies,general,kinematics and dynamics,
title = Ionised Gas Kinematics in MaNGA AGN. Extents of the Narrow Line and
Kinematically Disturbed regions, url = http://arxiv.org/abs/2201.01690, year =
2022 @articleBruggen2002, abstract = Hot, X-ray-emitting plasma permeates
clusters of galaxies. The X-ray surface brightness often shows a peak near the
centre of the duster that is coincident with a drop in the entropy of the gas.
This has been taken as evidence for a ’cooling flow’, where the gas cools by
radiating away its energy, and then falls to the centre. Searches for this
cool gas have revealed significantly less than predicted, indicating that the
mass deposition rate is much lower than expected. Most clusters with cooling
flows, however, also host an active galactic nucleus at their centres. These
active galactic nuclei can inflate large bubbles of hot plasma that
subsequently rise through the cluster ’atmosphere’, thus stirring the cooling
gas and adding energy. Here we report highly resolved hydrodynamic simulations
which show that buoyant bubbles increase the cooling time in the inner regions
of clusters and significantly reduce the deposition of cold gas., author =
Brüggen, Marcus and Kaiser, Christian R., doi = 10.1038/nature00857, file =
:home/william/Documents/Papers/10.1038@nature00857.pdf:pdf, issn = 00280836,
journal = Nature, number = 6895, pages = 301–303, title = Hot bubbles from
active galactic nuclei as a heat source in cooling-flow clusters, volume =
418, year = 2002 @articleBaron2020a, abstract = Post-starburst E+A galaxies
are systems that hosted a powerful starburst that was quenched abruptly.
Simulations suggest that these systems provide the missing link between major
merger ULIRGs and red and dead ellipticals, where AGN feedback is responsible
for the expulsion or destruction of the molecular gas. However, many details
remain unresolved and little is known about AGN-driven winds in this short-
lived phase. We present spatially resolved IFU spectroscopy with MUSE/VLT of
SDSS J124754.95-033738.6, a post-starburst E+A galaxy with a recent starburst
that started 70 Myr ago and ended 30 Myr ago, with a peak SFR of $150\,
{M_{}\,yr^{ -1}}$. We detect disturbed gas throughout the entire field of
view, suggesting triggering by a minor merger. We detect fast-moving
multiphased gas clouds, embedded in a double-cone face-on outflow, which are
traced by ionized emission lines and neutral NaID emission and absorption
lines. We find remarkable similarities between the kinematics, spatial
extents, and line luminosities of the ionized and neutral gas phases, and
propose a model in which they are part of the same outflowing clouds, which
are exposed to both stellar and AGN radiation. Our photoionization model
provides consistent ionized line ratios, NaID absorption optical depths and
EWs, and dust reddening. Using the model, we estimate, for the first time, the
neutral-to-ionized gas mass ratio (about 20), the sodium neutral fraction, and
the size of the outflowing clouds. This is one of the best ever observed
direct connections between the neutral and ionized outflow phases in AGN.,
archivePrefix = arXiv, arxivId = 2004.04749, author = Baron, Dalya and Netzer,
Hagai and Davies, Ric I and Xavier Prochaska, J, doi = 10.1093/mnras/staa1018,
eprint = 2004.04749, file = :home/william/Documents/Papers/staa1018.pdf:pdf,
issn = 0035-8711, journal = Mon. Not. R. Astron. Soc., keywords = 1 i n
t,active,correlations between the
masses,evolution,galaxies,general,interactions,of super,ro d u c,star
formation,t i o n,the discovery of strong, number = 4, pages = 5396–5420,
publisher = Oxford University Press, title = Multiphase outflows in post-
starburst E+A galaxies - II. A direct connection between the neutral and
ionized outflow phases, volume = 494, year = 2020 @articleMiyoshi2005,
abstract = A new multi-state Harten-Lax-van Leer (HLL) approximate Riemann
solver for the ideal magnetohydrodynamic (MHD) equations is developed based on
the assumption that the normal velocity is constant over the Riemann fan. This
assumption is same as that used in the HLLC (”C” denotes Contact) approximate
Riemann solver for the Euler equations. From the assumption, it is naturally
derived that the Riemann fan should consist of four intermediate states for
Bx≠ 0, whereas the number of the intermediate states is reduced to two when
Bx= 0. Since the intermediate states satisfied with all jump conditions in
this approximate Riemann system are analytically obtained, the multi-state HLL
Riemann solver can be constructed straightforwardly. It is shown that this
solver can exactly resolve isolated discontinuities formed in the MHD system,
and hence named as HLLD Riemann solver. (Here, ”D” stands for
Discontinuities.) It is also analytically proved that the HLLD Riemann solver
is positively conservative like the HLLC Riemann solver. Indeed, the HLLD
Riemann solver corresponds to the HLLC Riemann solver when the magnetic field
vanishes. Numerical tests demonstrate that the HLLD Riemann solver is more
robust and efficient than the linearized Riemann solver, and its resolution is
equally good. It indicates that the HLLD solver must be useful in practical
applications for the ideal MHD equations. 2005 Elsevier Inc. All rights
reserved., archivePrefix = arXiv, arxivId = 0501557, author = Miyoshi,
Takahiro and Kusano, Kanya, doi = 10.1016/j.jcp.2005.02.017, eprint = 0501557,
file = :home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Miyoshi, Kusano - 2005 - A multi-state HLL approximate
Riemann solver for ideal magnetohydrodynamics.pdf:pdf, isbn = 0021-9991, issn
= 00219991, journal = J. Comput. Phys., keywords = Approximate Riemann
solver,HLL,HLLC,HLLD,Magnetohydrodynamics,Positivity, number = 1, pages =
315–344, title = A multi-state HLL approximate Riemann solver for ideal
magnetohydrodynamics, volume = 208, year = 2005 @articleSoc2018, author = Soc,
R, doi = 00.0000/X000000000000000X, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley Desktop/Downloaded/Soc
- 2018 - Fo r R iew On Fo r R iew On ly.pdf:pdf, isbn = 0000000000000,
keywords = cd,elliptical and
lenticular,galaxies,hydrodynam-,ics,ism,nuclei,stellar dynamics, title = Fo r
R iew On Fo r R iew On ly, year = 2018 @articleBelan2013, abstract = Context.
In this paper we study the propagation of hypersonic hydrodynamic jets (Mach
number 5) in a laboratory vessel and make comparisons with numerical
simulations of axially symmetric flows with the same initial and boundary
conditions. The astrophysical context is that of the jets originating around
young stellar objects (YSOs). Aims. In order to gain a deeper insight into the
phenomenology of YSO jets, we performed a set of experiments and numerical
simulations of hypersonic jets in the range of Mach numbers from 10 to 20 and
for jet-to-ambient density ratios from 0.85 to 5.4, using different gas
species and observing jet lengths of the order of 150 initial radii or more.
Exploiting the scalability of the hydrodynamic equations, we intend to
reproduce the YSO jet behaviour with respect to jet velocity and elapsed
times. In addition, we can make comparisons between the simulated, the
experimental, and the observed morphologies. Methods. In the experiments the
gas pressure and temperature are increased by a fast, quasi-isentropic
compression by means of a piston system operating on a time scale of tens of
milliseconds, while the gas density is visualized and measured by means of an
electron beam system. We used the PLUTO software for the numerical solution of
mixed hyperbolic/parabolic conservation laws targeting high Mach number flows
in astrophysical fluid dynamics. We considered axisymmetric initial conditions
and carried out numerical simulations in cylindrical geometry. The code has a
modular flexible structure whereby different numerical algorithms can be
separately combined to solve systems of conservation laws using the finite
volume or finite difference approach based on Godunov-type schemes. Results.
The agreement between experiments and numerical simulations is fairly good in
most of the comparisons. The resulting scaled flow velocities and elapsed
times are close to the ones shown by observations. The morphologies of the
density distributions agree with the observed ones as well. Conclusions. The
laboratory and the simulated hypersonic jets are all pressure matched, i.e.
their axial regions are almost isentropic at the nozzle exit. They maintain
their collimation for long distances in terms of the initial jet radii,
without including magnetic confinement effects. This yields a qualitatively
good agreement with the observed YSO jet morphologies. It remains to be seen
what happens when non-axially symmetric perturbations of the flow are imposed
at the nozzle, both in the experiment and in the simulation. ESO, 2013.,
author = Belan, M. and Massaglia, S. and Tordella, D. and Mirzaei, M. and De
Ponte, S., doi = 10.1051/0004-6361/201321040, file =
:home/william/Documents/Papers/hyperjets.pdf:pdf, issn = 00046361, journal =
Astron. Astrophys., keywords = Herbig-Haro objects,Hydrodynamics,ISM: jets and
outflows,Shock waves,Stars: winds,outflows, number = June 2014, title = The
hydrodynamics of astrophysical jets: Scaled experiments and numerical
simulations, volume = 554, year = 2013 @articleNguyen2021, abstract = Cool
clouds are expected to be destroyed and incorporated into hot supernova-driven
galactic winds. The mass-loading of a wind by the cool medium modifies the
bulk velocity, temperature, density, entropy, and abundance profiles of the
hot phase relative to an un-mass-loaded outflow. We provide general equations
and limits for this physics that can be used to infer the rate of cool gas
entrainment from X-ray observations, accounting for non-spherical expansion.
In general, mass-loading flattens the density and temperature profiles,
decreases the velocity and increases the entropy if the Mach number is above a
critical value. We first apply this model to a recent high-resolution galactic
outflow simulation where the mass-loading can be directly inferred. We show
that the temperature, entropy, and composition profiles are well-matched,
providing evidence that this physics sets the bulk hot gas profiles. We then
model the diffuse X-ray emission from the local starburst M82. The non-
spherical (more cylindrical) outflow geometry is directly taken from the
observed X-ray surface brightness profile. These models imply a total mass-