nuclei,extragalactic radio jets,interstellar medium,outflows,spectroscopy,
number = November, pages = 1–10, title = The Many Routes to AGN Feedback,
volume = 4, year = 2017 @articleMisawa2018, abstract = We search for velocity
changes (i.e., acceleration/deceleration) of narrow absorption lines (NALs)
that are intrinsic to the quasars, using spectra of 6 bright quasars that have
been observed more than once with 8-10m class telescopes. While variations in
line strength and profile are frequently reported (especially in broader
absorption lines), definitive evidence for velocity shifts has not been found
with only a few exceptions. Direct velocity shift measurements are valuable
constraints on the acceleration mechanisms. In this study, we determine
velocity shifts by comparing the absorption profiles of NALs at two epochs
separated by more than 10 years in the observed frame, using the cross-
correlation function method and we estimate the uncertainties using Monte
Carlo simulations. We do not detect any significant shifts but we obtain 3$$
upper limits on the acceleration of intrinsic NALs (compared to intervening
NALs in same quasars) of $$0.7 km s$^{-1}$ yr$^{-1}$ ($$0.002 cm s$^{-2}$). We
discuss possible scenarios for non-detection of NAL acceleration/deceleration
and examine resulting constraints on the physical conditions in accretion disk
wind., archivePrefix = arXiv, arxivId = 1809.07476, author = Misawa, Toru and
Eracleous, Michael and Charlton, Jane C. and Kashikawa, Nobunari, eprint =
1809.07476, file = :home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Misawa et al. - 2018 - Direct Measurement of Quasar Outflow
Wind Acceleration.pdf:pdf, title = Direct Measurement of Quasar Outflow Wind
Acceleration, url = http://arxiv.org/abs/1809.07476, year = 2018
@bookNetzer2006, author = Netzer, H, doi = 10.1007/3-540-34621-X, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Netzer - 2006 - Active Galactic Nuclei Basic Physics and
Main Components.pdf:pdf, isbn = 354034621X, pages = 1–38, title = Active
Galactic Nuclei : Basic Physics and Main Components, volume = 38, year = 2006
@articleSolano, author = Solano, C M D, file =
:home/william/Documents/Papers/Plasma_effects_on_quantum_light.pdf:pdf, pages
= 3–4, title = Plasma effects on quantum light @article2013ApJ…763L..18W,
archivePrefix = arXiv, arxivId = 1211.5851, author = Wagner, A.~Y. and
Umemura, M and Bicknell, G.~V., doi = 10.1088/2041-8205/763/1/L18, eprint =
1211.5851, file = :home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Wagner, Umemura, Bicknell - 2013 - Ultrafast outflows
Galaxy-scale active galactic nucleus feedback.pdf:pdf, journal = Apjl,
keywords = ISM: jets and outflows,galaxies: evolution,galaxies:
formation,hydrodynamics,methods: numerical, pages = L18, title = Ultrafast
Outflows: Galaxy-scale Active Galactic Nucleus Feedback, volume = 763, year =
2013 @articleJuneau2021, abstract = There is growing evidence for physical
influence between supermassive black holes and their host galaxies. We present
a case study of nearby galaxy NGC 7582, for which we find evidence that
galactic substructure plays an important role in affecting the collimation of
ionized outflows as well as contributing to the heavy active galactic nucleus
(AGN) obscuration. This result contrasts with a simple, small-scale AGN torus
model, according to which AGN wind collimation may take place inside the torus
itself, at subparsec scale. Using 3D spectroscopy with the MUSE instrument, we
probe the kinematics of the stellar and ionized gas components as well as the
ionization state of the gas from a combination of emission line ratios. We
report for the first time a kinematically distinct core (KDC) in NGC 7582, on
a scale of ~600pc. This KDC coincides spatially with dust lanes and
starbursting complexes previously observed. We interpret it as a circumnuclear
ring of stars and dusty, gas-rich material. We obtain a clear view of the
outflowing cones over kpc scales, and demonstrate that they are predominantly
photoionized by the central engine. We detect the back cone (behind the
galaxy), and confirm previous results of a large nuclear obscuration of both
the stellar continuum and HII regions. While we tentatively associate the
presence of the KDC to a large-scale bar and/or a minor galaxy merger, we
stress the importance of gaining a better understanding of the role of galaxy
substructure in controlling the fueling, feedback and obscuration of AGN.,
archivePrefix = arXiv, arxivId = 2112.08380, author = Juneau, Stéphanie and
Goulding, Andy D. and Banfield, Julie and Bianchi, Stefano and Duc, Pierre-
Alain and Ho, I-Ting and Dopita, Michael A. and Scharw ächter, Julia and
Bauer, Franz E. and Groves, Brent and Alexander, David M. and Davies, Rebecca
L. and Elbaz, David and Freeland, Emily and Hampton, Elise and Kewley, Lisa J.
and Nikutta, Robert and Shastri, Prajval and Shu, Xinwen and Vogt, Frédéric P.
A. and Wang, Tao and Wong, O. Ivy and Woo, Jong-Hak, eprint = 2112.08380, file
= :home/william/Documents/Papers/2112.08380.pdf:pdf, title = The Black Hole-
Galaxy Connection: Interplay between Feedback, Obscuration, and Host Galaxy
Substructure, url = http://arxiv.org/abs/2112.08380, year = 2021
@articleTombesi2017, abstract = We present a spectral analysis of a 200ks
observation of the broad-line radio galaxy 3C120, performed with the high-
energy transmission grating spectrometer on board the Chandra X-ray
Observatory. We find (i) a neutral absorption component intrinsic to the
source with a column density of N log 20.67 0.05 H =  cm −2 ; (ii) no
evidence for a warm absorber (WA) with an upper limit on the column density of
just N log 19.7 H cm −2 , assuming the typical ionization parameter
log$\xi$;2.5 erg s −1 cm; the WA may instead be replaced by (iii) a hot
emitting gas with a temperature kT;0.7 keV observed as soft X-ray emission
from ionized Fe L-shell lines, which may originate from a kiloparsec-scale
shocked bubble inflated by the active galactic nucleus (AGN) wind or jet with
a shock velocity of about 1000 km s −1 determined by the emission line width;
(iv) a neutral Fe K$\alpha$ line and accompanying emission lines indicative of
a Compton-thick cold reflector with a low reflection fraction R;0.2,
suggesting a large opening angle of the torus; (v) a highly ionized Fe XXV
emission feature indicative of photoionized gas with an ionization parameter
log 3.75 0.38 0.27 x = -+ ergs −1 cm and a column density of N log 22 H cm
−2 localized within ∼2pc from the X-ray source; and (vi) possible signatures
of a highly ionized disk wind. Together with previous evidence for intense
molecular line emission, these results indicate that 3C120 is likely a late-
state merger undergoing strong AGN feedback., archivePrefix = arXiv, arxivId =
1703.00516, author = Tombesi, F. and Mushotzky, R. F. and Reynolds, C. S. and
Kallman, T. and Reeves, J. N. and Braito, V. and Ueda, Y. and Leutenegger, M.
A. and Williams, B. J. and Stawarz, Ł. and Cappi, M., doi =
10.3847/1538-4357/aa6342, eprint = 1703.00516, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Tombesi et al. - 2017 - Feeding and Feedback in the
Powerful Radio Galaxy 3C 120.pdf:pdf, issn = 1538-4357, journal = Astrophys.
J., keywords = active,black hole physics,black hole physics,galaxies:
active,line: identifi,galaxies,identi fi cation,line,x-rays, number = 1, pages
= 16, publisher = IOP Publishing, title = Feeding and Feedback in the Powerful
Radio Galaxy 3C 120, url =
http://stacks.iop.org/0004-637X/838/i=1/a=16?key=crossref.5e349d2463f5a93d2b23c77642dabf8a,
volume = 838, year = 2017 @articleMelioli2006a, abstract = In the present
study, considering the physical conditions that are relevant in interactions
between supernova remnants (SNRs) and dense molecular clouds for triggering
star formation we have built a diagram of SNR radius versus cloud density in
which the constraints above delineate a shaded zone where star formation is
allowed. We have also performed fully 3D radiatively cooling numerical
simulations of the impact between SNRs and clouds under different initial
conditions in order to follow the initial steps of these interactions. We
determine the conditions that may lead either to cloud collapse and star
formation or to complete cloud destruction and find that the numerical results
are consistent with those of the SNR-cloud density diagram. Finally, we have
applied the results above to the $\beta$ Pictoris stellar association which is
composed of low-mass post-T Tauri stars with an age of 11 Myr. It has been
recently suggested that its formation could have been triggered by the shock
wave produced by an SN explosion localized at a distance of about 62 pc that
may have occurred either in the Lower Centaurus Crux or in the Upper Centaurus
Lupus which are both nearby older subgroups of that association (Ortega and
co-workers). Using the results of the analysis above we have shown that the
suggested origin for the young association at the proposed distance is
plausible only for a very restricted range of initial conditions for the
parent molecular cloud, that is, a cloud with a radius of the order of 10 pc
and density of the order of 20 cm-3 and a temperature of the order of 50-100
K. 2006 RAS., archivePrefix = arXiv, arxivId = astro-ph/0608207, author =
Melioli, C. and De Gouveia Dal Pino, E. M. and De La Reza, R. and Raga, A.,
doi = 10.1111/j.1365-2966.2006.11076.x, eprint = 0608207, file =
:home/william/Documents/Papers/mnras0373-0811.pdf:pdf, issn = 00358711,
journal = Mon. Not. R. Astron. Soc., keywords = ISM: clouds,Stars:
formation,Supernova remnants, number = 2, pages = 811–818, primaryClass =
astro-ph, title = Star formation triggered by SN explosions: An application to
the stellar association of $\beta$ Pictoris, volume = 373, year = 2006
@articleQiu2020, abstract = Aims. We investigate the physical and chemical
conditions of molecular gas in the circumnuclear disk (CND) region of NGC
1068. Methods. We carried out a spectral line survey with the IRAM 30 m
telescope toward the center of NGC 1068 and mainly focused on the 2 mm band
with a frequency coverage of 160.7–168.6 GHz and 176.5–184.3 GHz. Results.
Fifteen lines are detected in NGC 1068, eight of which are new detections for
this galaxy. We derive the rotation temperatures and column densities of
fourteen molecular species. Conclusions. Based on the [HCO + (2 − 1)]/[HOC +
(2 − 1)] ratio, we obtain a high ionization degree in the CND of NGC 1068. It
is found that HC 3 N is concentrated in the east knot, while 13 CCH, CH 3 CN,
SO, HOC + , CS, CH 3 CCH, and H 2 CO are concentrated in the west knot.
Compared to the star-forming galaxies M 82 and NGC 253, the chemistry of NGC
1068 might be less strongly affected by the UV radiation field, and its
kinetic temperature might be lower. , archivePrefix = arXiv, arxivId =
2001.08697, author = Qiu, Jianjie and Zhang, Jiangshui and Zhang, Yong and
Jia, Lanwei and Tang, Xindi, doi = 10.1051/0004-6361/201935800, eprint =
2001.08697, file = :home/william/Documents/Papers/[Qiu et al.]-2mm
spectroscopy observations toward the circumnuclear.pdf:pdf, issn = 0004-6361,
journal = Astron. Astrophys., keywords =
active,galaxies,individual,ism,molecules,ngc 1068,nuclei, pages = A125, title
= $\lambda$ = 2 mm spectroscopy observations toward the circumnuclear disk of
NGC 1068 , volume = 634, year = 2020 @articleDobbs2011, abstract = We perform
calculations of isolated disc galaxies to investigate how the properties of
the interstellar medium (ISM), the nature of molecular clouds and the global
star formation rate depend on the level of stellar feedback. We adopt a simple
physical model, which includes a galactic potential, a standard cooling and
heating prescription of the ISM and self-gravity of the gas. Stellar feedback
is implemented by injecting energy into dense, gravitationally collapsing gas,
but is independent of the Schmidt-Kennicutt relation. We obtain fractions of
gas, and filling factors for different phases of the ISM in reasonable
agreement with observations. Supernovae are found to be vital to reproduce the
scaleheights of the different components of the ISM, and velocity dispersions.
The giant molecular clouds (GMCs) formed in the simulations display mass
spectra similar to the observations, their normalization depend on the level
of feedback. We find ~40per cent of the clouds exhibit retrograde rotation,
induced by cloud-cloud collisions. The star formation rates we obtain are in
good agreement with the observed Schmidt-Kennicutt relation, and are not
strongly depend on the star formation efficiency we assume, being largely
self-regulated by the feedback. We also investigate the effect of spiral
structure by comparing calculations with and without the spiral component of
the potential. The main difference with a spiral potential is that more
massive GMCs are able to accumulate in the spiral arms. Thus we are able to
reproduce massive GMCs, and the spurs seen in many grand design galaxies, even
with stellar feedback. The presence of the spiral potential does not have an
explicit effect on the star formation rate, but can increase the star
formation rate indirectly by enabling the formation of long-lived, strongly
bound clouds. 2011 The Authors. Monthly Notices of the Royal Astronomical
Society 2011 RAS., archivePrefix = arXiv, arxivId = arXiv:1107.0154v1, author
= Dobbs, C. L. and Burkert, A. and Pringle, J. E., doi =
10.1111/j.1365-2966.2011.19346.x, eprint = arXiv:1107.0154v1, file =
:home/william/Documents/Papers/1107.0154.pdf:pdf, issn = 00358711, journal =
Mon. Not. R. Astron. Soc., keywords = Galaxies: ISM,Hydrodynamics,ISM:
clouds,ISM: evolution,ISM: kinematics and dynamics, number = 2, pages =
1318–1334, title = The properties of the interstellar medium in disc galaxies
with stellar feedback, volume = 417, year = 2011
@articleCacioppoJohnT.;Sandman1978, abstract = An analytical model of a
prestressed concrete reactor vessel (PCRV) for LMFBR and the associated finite
element com- puter code, involving an explicit time integration procedure, is
described. The model is axisymmetric and includes simula- tions of the tensile
cracking of concrete, the reinforcement, and a prestressing capability. The
tensile cracking of concrete and the steel reinforcement are both modeled as
continuously distr~uted within the finite element. The stresses in the rein-
forcement and concrete are computed separately and combined to give an overall
stress state of the composite material. The reinformcement is assumed to be
elastic, perfectly-plastic; the concrete is taken to be elastic, with tensile
and com- pressive stress limits. Cracking of concrete is based on the
criterion of maximum principal stress; a crack is assumed to form normal to
the direction of the maximum principal stress. Attention is also given to the
fact that cracks do not form instan- taneously, but develop gradually. Thus,
after crack initiation the normal stress is reduced to zero gradually as a
function of time. Residual shear resistance of cracks due to aggregate
interlock is also taken into account. An existing crack is permitted to close.
Prestressing of the PCRV is modeled by special structural members which
represent an averaged prestressing layer equivalent to an axisymmetric shell.
The internal prestressing members are superimposed over the reinforced
concrete body of the PCRV; they are permitted to stretch and slide in a
predetermined path, simulating the actual tendons. The validity of the code is
examined by comparison with experimental data. Both static and dynamic data
are com- pared with code predictions, and the agreement is satisfactory. A
preliminary design has been developed for both pool and loop-type PCRVs. The
code was applied to the analysis of these designs. This analysis reveals that
the critical locations in such a design would be the head cover and the
junction between the cover and the vessel wall and indicates the pattern of
crack development. The results show that the development of a design adequate
for current HCDA loads is quite feasible for pool-type or loop-type PCRVs.,
author = Cacioppo, John T.; Sandman, Curt A., file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Unknown - 1978 - No Title.pdf:pdf, isbn = 9789896540821,
number = 3, pages = 377–389, title = No 主観的健康感を中心とした在宅高齢者における
健康関連指標に関する共分散構造分析Title, volume = 2, year = 1978 @articleCox2005, abstract =
The interstellar medium in the vicinity of the Sun is arranged in large-scale
structures of bubble walls, sheets, and filaments of warm gas, within which
close to the midplane there are subsheets and filaments of cold dense
material; the whole occupies roughly half the available volume and extends
with decreasing mean density to at least a kiloparsec off the plane. The
remainder of the volume is in bubble interiors, cavities, and tunnels of much
lower density, with some but not all of those lower density regions hot enough
to be observable via their X-ray emission. This entire system is pervaded by a
rather strong and irregular magnetic field and cosmic rays, the pressures of
which are confined by the weight of the interstellar gas, particularly that
far from the plane where gravity is strong. Observations suggest that the
cosmic rays and magnetic field have an even more extended vertical
distribution than the warm gas, requiring either the weight of additional
coronal material or magnetic tension to confine it to the disk. Adjusting
one’s perception of this medium to embrace the known aspects is difficult.
After this adjustment, there are many problems to solve and prejudices to
overcome - the weak role of thermal instability, the suppression of certain
gravitational instabilities, the problem of determining the state in the low-
density regions, the twin difficulties of not having too much OVI (O +5) and
getting enough diffuse 3/4 keV X-ray emission, the possible importance of
large old-barrel-shaped supernova remnants in clarifying matters, the possible
role of dust evolution in adjusting the heating to make clouds stable, the
factors influencing the magnitudes of the interstellar pressure and scale
height - things that global models of the medium might examine to clarify some
of these matters; attention to these details and more constitute the challenge
of this subject. Copyright 2005 by Annual Reviews. All rights reserved.,
author = Cox, Donald P., doi = 10.1146/annurev.astro.43.072103.150615, file =
:home/william/Documents/Papers/cox2005.pdf:pdf, issn = 00664146, journal =
Annu. Rev. Astron. Astrophys., keywords = Dust,Galaxies,Interstellar
medium,Milky Way,Supernova remnants,X rays, pages = 337–385, title = The
three-phase interstellar medium revisited, volume = 43, year = 2005
@articleFluetsch2019, abstract = We study molecular outflows in a sample of 45
local galaxies, both star forming and active galactic nucleus (AGN), primarily
by using CO data from the Atacama Large Millimeter/submillimeter Array (ALMA)
archive and from the literature. For a subsample, we also compare the
molecular outflow with the ionized and neutral atomic phases. We infer an
empirical analytical function relating the outflow rate simultaneously to the
star formation rate (SFR), L AGN, and galaxy stellar mass; this relation is
much tighter than the relations with the individual quantities. The outflow
kinetic power shows a larger scatter than in previous, more biased studies,
spanning from 0.1 to 5 per cent of L AGN, while the momentum rate ranges from
1 to 30 times L AGN /c, indicating that these outflows can be both energy
driven, but with a broad range of coupling efficiencies with the interstellar
medium (ISM), and radiation pressure driven. For about 10 per cent of the
objects, the outflow energetics significantly exceed the maximum theoretical
values; we interpret these as ’fossil outflows’ resulting from activity of a
past strong AGN, which has now faded. We estimate that, in the stellar mass
range probed here ( 10 10 ,M⊙), less than 5 per cent of the outflowing gas
escapes the galaxy. The molecular gas depletion time associated with the
outflow can be as short as a few million years in powerful AGN; however, the
total gas (H 2 + Hi) depletion times are much longer. Altogether, our findings
suggest that even AGN-driven outflows might be relatively ineffective in
clearing galaxies of their entire gas content, although they are likely
capable of clearing and quenching the central region., author = Fluetsch, A.
and Maiolino, R. and Carniani, S. and Marconi, A. and Cicone, C. and Bourne,
M. A. and Costa, T. and Fabian, A. C. and Ishibashi, W. and Venturi, G., doi =
10.1093/mnras/sty3449, file = :home/william/Documents/Papers/sty3449.pdf:pdf,
issn = 13652966, journal = Mon. Not. R. Astron. Soc., keywords = galaxies:
ISM,galaxies: active,galaxies: evolution,galaxies: star formation,quasars:
general, number = 4, pages = 4586–4614, publisher = Oxford University Press,
title = Cold molecular outflows in the local Universe and their feedback
effect on galaxies, volume = 483, year = 2019 @articleBooth2013a, abstract =
Energetic feedback from supernovae (SNe) and from active galactic nuclei (AGN)
are both important processes that are thought to control how much gas is able
to condense into galaxies and form stars. We show that although both AGN and
SNe suppress star formation, they mutually weaken one another’s effect by up
to an order of magnitude in haloes in the mass range for which both feedback
processes are efficient (). These results demonstrate the importance of the
simultaneous, non-independent inclusion of these two processes in models of
galaxy formation to estimate the total feedback strength. These results are of
particular relevance to the interpretation of results from hydrodynamical
simulations that model only one of the feedback processes, and also to those
semi-analytic models that implicitly assume the effects of the two feedback
processes to be independent., archivePrefix = arXiv, arxivId = 1203.3802,
author = Booth, C. M. and Schaye, Joop, doi = 10.1038/srep01738, eprint =
1203.3802, file = :home/william/Documents/Papers/srep01738.pdf:pdf, issn =
20452322, journal = Sci. Rep., pages = 1–5, title = The interaction between
feedback from active galactic nuclei and supernovae, volume = 3, year = 2013
@articleZhang2020, abstract = The Fermi bubbles are two giant bubbles in gamma
rays lying above and below the Galactic center (GC). Despite numerous studies
on the bubbles, their origin and emission mechanism remain elusive. Here we
use a suite of hydrodynamic simulations to study the scenario where the cosmic
rays (CRs) in the bubbles are mainly accelerated at the forward shocks driven
by a pair of opposing jets from Sgr A*. We find that an active galactic
nucleus (AGN) jet event happened $5-6$ Myr ago can naturally reproduce the
bilobular morphology of the bubbles, and the postshock gas temperature in the
bubbles is heated to $0.4$ keV, consistent with recent X-ray observations. The
forward shocks compress the hot halo gas, and at low latitudes, the compressed
gas shows an X-shaped structure, naturally explaining the biconical X-ray
structure in the ROSAT 1.5 keV map in both morphology and X-ray surface
brightness. CR acceleration is most efficient in the head regions of the
bubbles during the first 2 Myrs. The opposing jets release a total energy of
$10^{55}$ erg with an Eddington ratio of $10^{-3}$, which falls well in the
range of the hot accretion flow mode for black holes. Our simulations further
show that the forward shocks driven by spherical winds at the GC typically
produce bubbles with much wider bases than observed, and could not reproduce
the X-shaped X-ray structure at low latitudes. This suggests that starburst or
AGN winds are unlikely the origin of the bubbles in the shock scenario.,
archivePrefix = arXiv, arxivId = 2003.03625, author = Zhang, Ruiyu and Guo,
Fulai, eprint = 2003.03625, file =
:home/william/Documents/Papers/[Zhang]-SIMULATING THE FERMI BUBBLES AS FORWARD
SHOCKS DRIVEN BY AGN JETS.pdf:pdf, keywords = active,cosmic
rays,galaxies,galaxy,gamma rays,halo,jets, title = Simulating the Fermi
Bubbles as Forward Shocks driven by AGN Jets, url =
http://arxiv.org/abs/2003.03625, year = 2020 @articleBon2018, abstract = Here
we present a critical view of practical problems in the analysis of optical Fe
II emission lines of Type 1 AGN spectra. Besides the very complex and unclear
physical interpretation of the Fe II template shape, there are other issues
that might affect the results of Fe II contribution as well (like the S/N, the
AGN continuum component modelling, the complex shapes of other broad and
narrow emission lines that are blending in the same part of the spectrum, the
galactic host stellar component that could lead to mimicking of the Fe II
template shape on some parts of spectrum, etc.). In this paper we concentrate
particularly on the claims of possibility that in some objects Fe II could be
strongly shifted to the red. We examine the effects in the fitting procedure
that could artificially lead to such results., archivePrefix = arXiv, arxivId
= 1812.05828, author = Bon, E. and Marziani, P. and Berton, M. and Bon, N. and
Antonucci, R. and Gaskell, M. and Ferland, G., eprint = 1812.05828, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley Desktop/Downloaded/Bon
et al. - 2018 - Fe II velocity shifts in optical spectra of type 1
AGN.pdf:pdf, number = April 2018, pages = 0–7, title = Fe II velocity shifts
in optical spectra of type 1 AGN, url = http://arxiv.org/abs/1812.05828, year
= 2018 @miscSilk2017, abstract = Could there be intermediate mass black holes
in essentially all old dwarf galaxies? I argue that current observations of
Active Galactic Nuclei in dwarfs allow such a radical hypothesis which
provides early feedback and potentially provides a unifying explanation for
many if not all of the apparent dwarf galaxy anomalies, such as the abundance,
core-cusp,”too big to fail”, ultra-faint and baryon-fraction issues. I
describe the supporting arguments, which are largely circumstantial in nature,
and discuss a number of tests. There is no strong motivation for modifying the
nature of cold dark matter in order to explain any of the dwarf
galaxy”problems”., archivePrefix = arXiv, arxivId = 1703.08553, author = Silk,
Joseph, booktitle = arXiv, doi = 10.3847/2041-8213/aa67da, eprint =
1703.08553, file = :home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Silk - 2017 - March 28, 2017 FEEDBACK BY MASSIVE BLACK
HOLES IN DWARF GALAXIES.pdf:pdf, issn = 23318422, title = Feedback by massive
black holes in dwarf galaxies, year = 2017 @bookMadejski2016, abstract = This
article reviews the recent observational results regarding $\gamma$ -ray
emission from active galaxies. The most numerous discrete extragalactic
$\gamma$ -ray sources are AGNs dominated by relativistic jets pointing in our
direction (commonly known as blazars), and they are the main subject of the
review. They are de-tected in all observable energy bands and are highly
variable. The advent of the sensitive $\gamma$ -ray observations, afforded by
the launch and continuing op-eration of the Fermi Gamma-ray Space Telescope
and the AGILE Gamma-ray Imaging Detector, as well as by the deployment of
current-generation Air Cerenkov Telescope arrays such as VERITAS, MAGIC, and
HESS-II, con-tinually provides sensitive $\gamma$ -ray data over the energy
range of ∼100 MeV to multi-TeV. Importantly, it has motivated simultaneous,
monitoring obser-vations in other bands, resulting in unprecedented time-
resolved broadband spectral coverage. After an introduction, in Sections 3, 4,
and 5, we cover the current status and highlights of $\gamma$ -ray
observations with (mainly) Fermi but also AGILE and put those in the context
of broadband spectra in Sec-tion 6. We discuss the radiation processes
operating in blazars in Section 7, and we discuss the content of their jets
and the constraints on the loca-tion of the energy dissipation regions in,
respectively, Sections 8 and 9. Sec-tion 10 covers the current ideas for
particle acceleration processes in jets, and Section 11 discusses the coupling
of the jet to the accretion disk in the host galaxy. Finally, Sections 12, 13,
and 14 cover, respectively, the contribution of blazars to the diffuse
$\gamma$ -ray background, the utility of blazars to study the extragalactic
background light, and the insight they provide for study of populations of
supermassive black holes early in the history of the Universe., author =
Madejski, Grzegorz (Greg) and Sikora, Marek, booktitle = Annu. Rev. Astron.
Astrophys., doi = 10.1146/annurev-astro-081913-040044, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Madejski, Sikora - 2016 - Gamma-Ray Observations of Active
Galactic Nuclei.pdf:pdf, isbn = 0819130400, issn = 0066-4146, keywords = agn
jets,gamma-rays,supermassive black holes, number = 1, pages = 725–760, title =
Gamma-Ray Observations of Active Galactic Nuclei, url =
http://www.annualreviews.org/doi/10.1146/annurev-astro-081913-040044, volume =
54, year = 2016 @articleZhuang2020, archivePrefix = arXiv, arxivId =
2007.11283, author = Zhuang, Ming-Yang and Ho, Luis C., doi =
10.3847/1538-4357/ab8f2e, eprint = 2007.11283, file =
:home/william/Documents/Papers/2007.11283.pdf:pdf, issn = 15384357, journal =
Astrophys. J., keywords = active,galaxies,ism,star formation, number = 2,
pages = 108, title = The Interplay between Star Formation and Black Hole
Accretion in Nearby Active Galaxies, volume = 896, year = 2020
@articleCielo2018, 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 rarifies 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, Salvatore and Bieri, Rebekka and
Volonteri, Marta and Wagner, Alexander Y and Dubois, Yohan, doi =
10.1093/mnras/sty708, eprint = 1712.03955, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Cielo et al. - 2018 - AGN feedback compared jets versus
radiation 1 I N T RO D U C T I O N.pdf:pdf, issn = 1365-2966, journal = Mon.
Not. R. Astron. Soc., keywords =
galaxies,ism,jets,methods,numerical,quasars,radiative transfer, pages =
1336–1355, title = AGN Feedback Compared: Jets versus Radiation, volume =
1355, year = 2018 @articleYang2012, abstract = The Fermi Gamma-Ray Space
Telescope reveals two large bubbles in the Galaxy, which extend nearly
symmetrically ~50° above and below the Galactic center. Using three-
dimensional (3D) magnetohydrodynamic simulations that self-consistently
include the dynamical interaction between cosmic rays (CRs) and thermal gas
and anisotropic CR diffusion along the magnetic field lines, we show that the
key characteristics of the observed gamma-ray bubbles and the spatially
correlated X-ray features in the ROSAT 1.5 keV map can be successfully
reproduced by recent jet activity from the central active galactic nucleus. We
find that after taking into account the projection of the 3D bubbles onto the
sky the physical heights of the bubbles can be much smaller than previously
thought, greatly reducing the formation time of the bubbles to about a Myr.
This relatively small bubble age is needed to reconcile the simulations with
the upper limit of bubble ages estimated from the cooling time of high-energy
electrons. No additional physical mechanisms are required to suppress large-
scale hydrodynamic instabilities because the evolution time is too short for
them to develop. The simulated CR bubbles are edge-brightened, which is
consistent with the observed projected flat surface brightness distribution.
Furthermore, we demonstrate that the sharp edges of the observed bubbles can
be due to anisotropic CR diffusion along magnetic field lines that drape
around the bubbles during their supersonic expansion, with suppressed
perpendicular diffusion across the bubble surface. Possible causes of the
slight bends of the Fermi bubbles to the west are also discussed., author =
Yang, H. Y.K. and Ruszkowski, M. and Ricker, P. M. and Zweibel, E. and Lee,
D., doi = 10.1088/0004-637X/761/2/185, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley Desktop/Downloaded/Yang
et al. - 2012 - The Fermi bubbles Supersonic active galactic nucleus jets with
anisotropic cosmic-ray diffusion.pdf:pdf, issn = 15384357, journal =
Astrophys. J., keywords = Galaxy: nucleus,cosmic rays,diffusion,gamma rays:
galaxies,magnetohydrodynamics (MHD),methods: numerical, number = 2, title =
The Fermi bubbles: Supersonic active galactic nucleus jets with anisotropic
cosmic-ray diffusion, volume = 761, year = 2012 @articleFerrari1998, abstract
= ▪ Abstract Extragalactic jets were discovered and initially studied by radio
astronomers in connection with extended radio sources. At present, the
combination of jets and disks is considered the crucial element in unification
models for all active galactic nuclei (AGNs). The acceleration and propagation
conditions of jets, together with the aspect ratio of the disk/jet geometry
with respect to the observer, shape the morphologies of AGNs. However, these
phenomenological models are very complex from the physical and mathematical
point of view, as they involve different elements of the theories of
gravitation, fluid dynamics, and electrodynamics in a highly nonlinear
combination and in conditions not easily reproducible in laboratory plasma or
fluid experiments. In the last ten years, theorists have attacked the subject
with advanced analytical and numerical methods, and some important results
have already been established that confirm the global scenario, although we
are still far from a complete physical…, author = Ferrari, Attilio, doi =
10.1146/annurev.astro.36.1.539, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Ferrari - 1998 - Modeling Extragalactic Jets.pdf:pdf, issn
= 0066-4146, journal = Annu. Rev. Astron. Astrophys., keywords = astrophysical
fluid dynamics,galactic nuclei,radio astronomy, number = 1, pages = 539–598,
title = Modeling Extragalactic Jets, url =
http://www.annualreviews.org/doi/10.1146/annurev.astro.36.1.539, volume = 36,
year = 1998 @articleCresci2018, abstract = Galaxy-scale outflows powered by
actively accreting supermassive black holes are routinely detected, and they
have been associated both with suppression and triggering of star formation.
Recent observational evidence and simulations are favouring a delayed
mechanism that connects outflows and star formation, archivePrefix = arXiv,
arxivId = 1802.10305, author = Cresci, Giovanni and Maiolino, Roberto, doi =
10.1038/s41550-018-0404-5, eprint = 1802.10305, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Cresci, Maiolino - 2018 - Observing positive and negative
AGN feedback.pdf:pdf, issn = 23973366, journal = Nat. Astron., number = 3,
pages = 179–180, title = Observing positive and negative AGN feedback, volume
= 2, year = 2018 @articleYang2014a, abstract = We analyze 60 months of all sky
data from the Fermi-LAT. The Fermi Bubble structures discovered previously are
clearly revealed by our analysis. With more data and, consequently, better
statistics we can now divide each bubble into constant longitude slices to
investigate their gross $$-ray spectral morphology. While the detailed
spectral behaviour of each slice derived within our analysis is somewhat
dependent on the assumed background model, we find, robustly, a relative
deficit of the flux at low energies (i.e., hardening) towards the top of the
South Bubble. In neither Bubble does the spectrum soften with longitude. The
morphology of the Fermi Bubbles is also revealed to be energy dependent: at
high energies they are more extended. We conclude from the gamma-ray spectrum
at high latitudes that a low energy break in the parent cosmic ray population
is required in both leptonic and hadronic models. We briefly discuss possible
leptonic and hadronic interpretation of this phenomenology., archivePrefix =
arXiv, arxivId = 1402.0403, author = Yang, Rui-zhi and Aharonian, Felix and
Crocker, Roland, doi = 10.1051/0004-6361/201423562, eprint = 1402.0403, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Yang, Aharonian, Crocker - 2014 - The Fermi Bubbles
Revisited.pdf:pdf, keywords = cosmic rays,diffuse background,gamma rays,ism,
pages = 1–9, title = The Fermi Bubbles Revisited, url =
http://arxiv.org/abs/1402.0403%0Ahttp://dx.doi.org/10.1051/0004-6361/201423562,
year = 2014 @articleSternberg1989, author = Sternberg, A and Dalgarno, A, file
= :home/william/Documents/Papers/[Sternberg, Dalgarno]-THE INFRARED RESPONSE
OF MOLECULAR HYDROGEN GAS TO ULTRAVIOLET RADIATION$\backslash$:HIGH-DENSITY
REGIONS.pdf:pdf, journal = ApJ, pages = 197–233, title = IR response of
molecular H gas to UV radiation: high density regions, volume = 338, year =
1989 @ARTICLEVeilleux2020, author = Veilleux, Sylvain and Maiolino, Roberto
and Bolatto, Alberto D. and Aalto, Susanne, title = ”Cool outflows in galaxies
and their implications”, journal = , keywords = Galaxies: active, Evolution,
Halo, Kinematics and dynamics, Starburst, Astrophysics - Astrophysics of
Galaxies, year = 2020, month = apr, volume = 28, number = 1, eid = 2, pages =
2, doi = 10.1007/s00159-019-0121-9, archivePrefix = arXiv, eprint =
2002.07765, primaryClass = astro-ph.GA, adsurl =
https://ui.adsabs.harvard.edu/abs/2020A&ARv..28….2V, adsnote = Provided by the
SAO/NASA Astrophysics Data System

@articleMukherjee2019, archivePrefix = arXiv, arxivId = arXiv:1812.08199v1,
author = Mukherjee, Sagnick and Bhattacharjee, Anirban and Chatterjee,
Suchetana and Newman, Jeffrey A. and Yan, Renbin, doi =
10.3847/1538-4357/aaf9b7, eprint = arXiv:1812.08199v1, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Chatterjee et al. - 2019 - X-Ray Surface Brightness
Profiles of Optically Selected Active Galactic Nuclei Comparison with X-Ray
AGNs.pdf:pdf, journal = Astrophys. J., number = 1, pages = 35, title = X-Ray
Surface Brightness Profiles of Optically Selected Active Galactic Nuclei:
Comparison with X-Ray AGNs, volume = 872, year = 2019 @articleMatsushita1999,
abstract = We investigated the physical properties of molecular gas in the
nuclear region of M51 (Seyfert 2). We obtained an aperture synthesis 13 CO(J =
1 - 0) image using the Nobeyama Millimeter Array (NMA), and compared it with
NMA 12 CO(J = 1 - 0) and HCN(J = 1 - 0) maps at similar spatial resolutions.
Within a radius of 180 pc from the center, the 13 CO(1 - 0) integrated
intensity was found to be 3 times weaker than that of HCN(1 - 0). Large-
Velocity-Gradient (LVG) calculations suggest that the observed high HCN(1 -0)/
13 CO(1 - 0) intensity ratio would arise from dense (n H2 ∼ 10 5 cm -3 ) and
hot (T kin ≳ 300 K) molecular clouds in the nuclear molecular disk. We also
observed in the 12 CO(1 - 0), (3 - 2), 13 CO(1 - 0), and (3 - 2) lines using
the Nobeyama 45m and JCMT 15m telescopes. We detected weak 13 CO lines as well
as strong 12 CO lines. The LVG calculations assuming a two-component model
suggest that there is a large amount of low-density (n H2 ∼ 3 - 6 × 10 2 cm -3
), low-temperature (T kin ∼ 20 - 50 K) gas, and a small amount of high-density
(n H2 ≳ 10 4 cm -3 ), high-temperature (T kin ≳ 500 K) gas. The existence of
the high-density and high-temperature component, although having a quite small
beam filling factor, supports the aperture synthesis observation results
mentioned above. Since this dense, hot gas is located in the nuclear molecular
disk around the Active Galactic Nucleus (AGN), it may be heated by the strong
X-ray radiation and/or by the shock induced by the radio jet. @1999 COSPAR.
Published by Elsevier Science Ltd., author = Matsushita, S. and Kohno, K. and
Vila-Vilaro, B. and Tosaki, T. and Kawabe, R., doi =
10.1016/S0273-1177(99)00250-1, file =
:home/william/Documents/Papers/1-s2.0-S0273117799002501-main.pdf:pdf, isbn =
5049484748454, issn = 02731177, journal = Adv. Sp. Res., number = 5-6, pages =
1015–1018, title = High-density and high-temperature molecular gas around the
AGN in M51, volume = 23, year = 1999 @articleStrozzi2017, abstract = The
effects of laser-plasma interactions (LPI) on the dynamics of inertial
confinement fusion hohlraums are investigated via a new approach that self-
consistently couples reduced LPI models into radiation-hydrodynamics numerical
codes. The interplay between hydrodynamics and LPI - specifically stimulated
Raman scatter and crossed-beam energy transfer (CBET) - mostly occurs via
momentum and energy deposition into Langmuir and ion acoustic waves. This
spatially redistributes energy coupling to the target, which affects the
background plasma conditions and thus, modifies laser propagation. This model
shows reduced CBET and significant laser energy depletion by Langmuir waves,
which reduce the discrepancy between modeling and data from hohlraum
experiments on wall x-ray emission and capsule implosion shape., author =
Strozzi, D. J. and Bailey, D. S. and Michel, P. and Divol, L. and Sepke, S. M.
and Kerbel, G. D. and Thomas, C. A. and Ralph, J. E. and Moody, J. D. and
Schneider, M. B., doi = 10.1103/PhysRevLett.118.025002, file =
:home/william/Documents/Papers/PhysRevLett.118.025002.pdf:pdf, issn =
10797114, journal = Phys. Rev. Lett., number = 2, pages = 1–5, pmid =
28128587, title = Interplay of Laser-Plasma Interactions and Inertial Fusion
Hydrodynamics, volume = 118, year = 2017 @articleKeel2021, abstract = We
present a narrowband [O III] imaging survey of 111 AGN hosts and 17 merging-
galaxy systems, in search of distant extended emission-line regions (EELRs)
around AGN (either extant or faded). Our data reach deeper than detection from
the broadband SDSS data, and cover a wider field than some early emission-line
surveys used to study extended structure around AGN. Spectroscopic followup
confirms two new distant AGN-ionized clouds, in the merging systems NGC 235
and NGC 5514, projected at 26 and 75 kpc from the nuclei (respectively). We
also recover the previously-known region in NGC 7252. These results strengthen
the connection between EELRs and tidal features; kinematically quiescent
distant EELRs are virtually always photoionized tidal debris. We see them in
~10% of the galaxies in our sample with tidal tails. Energy budgets suggest
that the AGN in NGC 5514 has faded by 3 times during the extra light-travel
time ~250,000 years from the nucleus to the cloud and then to the observer;
strong shock emission in outflows masks the optical signature of the AGN. For
NGC 235 our data are consistent with but do not unequivocally require
variation over ~85,000 years. In addition to these very distant ionized
clouds, luminous and extensive line emission within four galaxies - IC 1481,
ESO 362-G08, NGC 5514, and NGC 7679. IC 1481 shows apparent ionization cones,
a rare combination with its LINER AGN spectrum. In NGC 5514, we measure a
7-kpc shell expanding at ~370 km/s west of the nucleus., archivePrefix =
arXiv, arxivId = 2112.07084, author = Keel, William C. and Moiseev, Alexei and
Kozlova, D. V. and Ikhsanova, A. I and Oparin, D. V. and Uklein, R. I. and
Smirnova, A. A. and Eselevich, M. V., doi = 10.1093/mnras/stab3656, eprint =
2112.07084, file = :home/william/Documents/Papers/2112.07084.pdf:pdf, keywords
= active,galaxies,interactions,seyfert, number = December, pages = 1–20, title
= The TELPERION Survey for Distant [O III] Clouds around Luminous and
Hibernating AGN, url =
http://arxiv.org/abs/2112.07084%0Ahttp://dx.doi.org/10.1093/mnras/stab3656,
volume = 20, year = 2021 @articleAbeysekara2017, abstract = We present a
search of very high energy gamma-ray emission from the Northern ${Fermi}$
Bubble region using data collected with the High Altitude Water Cherenkov
(HAWC) gamma-ray observatory. The size of the data set is 290 days. No
significant excess is observed in the Northern ${Fermi}$ Bubble region, hence
upper limits above $1\,{TeV}$ are calculated. The upper limits are between
$310^{-7}\,{GeV}\, {cm}^{-2}\, {s}^{-1}\,{sr}^{-1}$ and
$410^{-8}\,{GeV}\,{cm}^{-2}\,{s}^{-1}\,{sr}^{-1}$. The upper limits disfavor a
proton injection spectrum that extends beyond $100\,{TeV}$ without being
suppressed. They also disfavor a hadronic injection spectrum derived from
neutrino measurements., archivePrefix = arXiv, arxivId = 1703.01344, author =
Abeysekara, A. U. and Albert, A. and Alfaro, R. and Alvarez, C. and Álvarez,
J. D. and Arceo, R. and Arteaga-Velázquez, J. C. and Solares, H. A. Ayala and
Barber, A. S. and Bautista-Elivar, N. and Becerril, A. and Belmont-Moreno, E.
and BenZvi, S. Y. and Berley, D. and Braun, J. and Brisbois, C. and Caballero-
Mora, K. S. and Capistrán, T. and Carramiñana, A. and Casanova, S. and
Castillo, M. and Cotti, U. and Cotzomi, J. and de León, S. Coutiño and De
León, C. and De la Fuente, E. and Hernandez, R. Diaz and Dingus, B. L. and
DuVernois, M. A. and Díaz-Vélez, J. C. and Ellsworth, R. W. and Engel, K. and
Fick, B. and Fiorino, D. W. and Fleischhack, H. and Fraija, N. and García-
González, J. A. and Garfias, F. and Gerhardt, M. and Muñoz, A. González and
González, M. M. and Goodman, J. A. and Hampel-Arias, Z. and Harding, J. P. and
Hernandez, S. and Hernandez-Almada, A. and Hinton, J. and Hona, B. and Hui, C.
M. and Hüntemeyer, P. and Iriarte, A. and Jardin-Blicq, A. and Joshi, V. and
Kaufmann, S. and Kieda, D. and Lara, A. and Lauer, R. J. and Lee, W. H. and
Lennarz, D. and Vargas, H. León and Linnemann, J. T. and Longinotti, A. L. and
Raya, G. Luis and Luna-García, R. and López-Coto, R. and Malone, K. and
Marinelli, S. S. and Martinez, O. and Martinez-Castellanos, I. and Martínez-
Castro, J. and Martínez-Huerta, H. and Matthews, J. A. and Miranda-Romagnoli,
P. and Moreno, E. and Mostafá, M. and Nellen, L. and Newbold, M. and Nisa, M.
U. and Noriega-Papaqui, R. and Pelayo, R. and Pretz, J. and Pérez-Pérez, E. G.
and Ren, Z. and Rho, C. D. and Rivière, C. and Rosa-González, D. and
Rosenberg, M. and Ruiz-Velasco, E. and Salazar, H. and Greus, F. Salesa and
Sandoval, A. and Schneider, M. and Schoorlemmer, H. and Sinnis, G. and Smith,
A. J. and Springer, R. W. and Surajbali, P. and Taboada, I. and Tibolla, O.
and Tollefson, K. and Torres, I. and Ukwatta, T. N. and Vianello, G. and
Weisgarber, T. and Westerhoff, S. and Wisher, I. G. and Wood, J. and Yapici,
T. and Yodh, G. B. and Zepeda, A. and Zhou, H., doi =
10.3847/1538-4357/aa751a, eprint = 1703.01344, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Abeysekara et al. - 2017 - Search for Very High Energy
Gamma Rays from the Northern $textit{Fermi}$ Bubble Region with HAWC.pdf:pdf,
keywords = astroparticle physics,diffuse background,galaxy,gamma
rays,general,structure, title = Search for Very High Energy Gamma Rays from
the Northern ${Fermi}$ Bubble Region with HAWC, url =
http://arxiv.org/abs/1703.01344%0Ahttp://dx.doi.org/10.3847/1538-4357/aa751a,
volume = 85, year = 2017 @articleGoyon2021, abstract = Slow and fast light, or
large changes in the group velocity of light, have been observed in a range of
optical media, but the fine optical control necessary to induce an observable
effect has not been achieved in a plasma. Here, we describe how the ion-
acoustic response in a fully ionized plasma can produce large and measurable
changes in the group velocity of light. We show the first experimental
demonstration of slow and fast light in a plasma, measuring group velocities
between 0.12c and -0.34c., author = Goyon, C. and Edwards, M. R. and Chapman,
T. and Divol, L. and Lemos, N. and Williams, G. J. and Mariscal, D. A. and
Turnbull, D. and Hansen, A. M. and Michel, P., doi =
10.1103/PhysRevLett.126.205001, file = :home/william/Documents/Papers/Slow and
Fast Light in Plasma Using Optical Wave Mixing.pdf:pdf, issn = 10797114,
journal = Phys. Rev. Lett., keywords = doi:10.1103/PhysRevLett.126.205001
url:https://doi, number = 20, pages = 205001, pmid = 34110194, publisher =
American Physical Society, title = Slow and Fast Light in Plasma Using Optical
Wave Mixing, url = https://doi.org/10.1103/PhysRevLett.126.205001, volume =
126, year = 2021 @articleAalto2020, abstract = Submillimetre and millimetre
observations are important in probing the properties of the molecular gas and
dust around obscured active galactic nuclei (AGNs) and their feedback. With
very high-resolution (0.”02x0.”03 (2x3 pc)) ALMA 345 GHz observations of CO
3-2, HCO$^+$ 4-3, HCN 4-3 $_2$=1$f$, and continuum we have studied the
molecular outflow and nucleus of the extremely radio-quiet lenticular galaxy
NGC1377. The outflow is resolved, revealing a 150 pc long, clumpy, high-
velocity, collimated molecular jet. The molecular emission is emerging from
the spine of the jet with an average diameter of 3-7 pc. A narrow-angle,
rotating molecular wind surrounds the jet and is enveloped by a larger-scale,
slower CO-emitting structure. The jet and narrow wind are turbulent ($$40
kms$^{-1}$) and have steep radial gas excitation gradients. The jet shows
velocity reversals that we propose are caused by precession, or episodic
directional changes. We suggest that an important process powering the outflow
is magneto-centrifugal driving. In contrast, the large-scale CO-envelope may
be a slow wind, or cocoon that stems from jet-wind interactions. An
asymmetric, nuclear r$$2 pc and hot (180 K) dust structure with a high
molecular column density, N(H$_2$)$1.8 10^{24}$ cm$^{-2}$, is detected in
continuum and vibrationally excited HCN. Its luminosity is likely powered by a
buried AGN. The mass of the supermassive black hole (SMBH) is estimated to
$910^6$ M$_$ and the SMBH of NGC1377 appears to be at the end of an intense
phase of accretion. The nuclear growth may be fuelled by low-angular momentum
gas inflowing from gas ejected in the molecular jet and wind. Such a feedback-
loop of cyclic accretion and outflows would be an effective process in growing
the nuclear SMBH. This result invites new questions as to SMBH growth
processes in obscured, dusty galaxies., archivePrefix = arXiv, arxivId =
2007.07824, author = Aalto, S. and Falstad, N. and Muller, S. and Wada, K. and
Gallagher, J. S. and König, S. and Sakamoto, K. and Vlemmings, W. and
Ceccobello, C. and Dasyra, K. and Combes, F. and García-Burillo, S. and Oya,
Y. and Martín, S. and van der Werf, P. and Evans, A. S. and Kotilainen, J.,
doi = 10.1051/0004-6361/202038282, eprint = 2007.07824, file =
:home/william/Documents/Papers/ALMA resolves the remarkable molecular jet and
rotating wind in.pdf:pdf, issn = 0004-6361, journal = Astron. Astrophys.,
keywords = Galaxies: active,Galaxies: evolution,Galaxies: individual: NGC
1377,Galaxies: nuclei,ISM: jets and outflows,ISM: molecules, month = jul,
pages = A104, publisher = EDP Sciences, title = ALMA resolves the remarkable
molecular jet and rotating wind in the extremely radio-quiet galaxy NGC 1377,
url = https://www.aanda.org/10.1051/0004-6361/202038282
http://arxiv.org/abs/2007.07824 http://dx.doi.org/10.1051/0004-6361/202038282,
volume = 640, year = 2020 @articleDas2007, archivePrefix = arXiv, arxivId =
astro-ph/0611183, author = Das, V. and Crenshaw, D. M. and Kraemer, S. B., doi
= 10.1086/510580, eprint = 0611183, file =
:home/william/Documents/Papers/0611183.pdf:pdf, issn = 0004-637X, journal =
Astrophys. J., number = 2, pages = 699–708, primaryClass = astro-ph, title =
Dynamics of the Narrow‐Line Region in the Seyfert 2 Galaxy NGC 1068, volume =
656, year = 2007 @articleDt1996, abstract = We now turn our attention to the
last term, in which $\Gamma$ ≡ volumetric radiative heating rate [ erg cm −3 s
−1 ] $\Lambda$ ≡ volumetric radiative cooling rate [ erg cm −3 s −1 ].
Unfortunately, due to a shortage of Greek letters, $\Gamma$ is also used to
represent ionization rates. In this section of the course and notes,
therefore, I will denote the radiative heating rate by H, and will reserve
$\Gamma$ for ionization rates., author = Dt, D, file =
:home/william/Documents/Papers/notes8.pdf:pdf, journal = Weinb. al, number =
8, pages = 46–52, title = 8 Radiative Cooling and Heating, volume = 465, year
= 1996 @articleSartori2019, abstract = We present a numerical framework for
the variability of active galactic nuclei (AGN), which links the variability
of AGN over a broad range of timescales and luminosities to the observed
properties of the AGN population as a whole, and particularly the Eddington
ratio distribution function (ERDF). We have implemented our framework on GPU
architecture, relying on previously published time series generating
algorithms. After extensive tests that characterise several intrinsic and
numerical aspects of the simulations, we describe some applications used for
current and future time domain surveys and for the study of extremely variable
sources (e.g., ”changing look” or flaring AGN). Specifically, we define a
simulation setup which reproduces the AGN variability observed in the PTF/iPTF
survey, and use it to forward model longer light curves of the kind that may
be observed within the LSST main survey. Thanks to our effcient
implementations, these simulations are able to cover for example over 1 Myr
with a roughly weekly cadence. We envision that this framework will become
highly valuable to prepare for, and best exploit, data from upcoming time
domain surveys, such as for example LSST., archivePrefix = arXiv, arxivId =
1909.06374, author = Sartori, Lia F. and Trakhtenbrot, Benny and Schawinski,
Kevin and Caplar, Neven and Treister, Ezequiel and Zhang, Ce, doi =
10.3847/1538-4357/ab3c55, eprint = 1909.06374, file =
:home/william/Documents/Papers/1909.06374.pdf:pdf, issn = 15384357, journal =
Astrophys. J., keywords = agn variability - quasars, number = 2, pages = 139,
title = A Forward Modeling Approach to AGN Variability–Method Description and
Early Applications, volume = 883, year = 2019 @articleKing2010a, abstract = I
show that Eddington accretion episodes in active galactic nuclei
(AGN)$\backslash$nare likely to produce winds with velocities v ~ 0.1c and
ionization$\backslash$nparameters up to {$ξ$} ~ 10$^{4}$ (cgs), implying the
presence of$\backslash$nresonance lines of helium- and hydrogen-like iron.
These properties are$\backslash$ndirect consequences of momentum and mass
conservation, respectively, and$\backslash$nagree with recent X-ray
observations of fast outflows from AGN. Because$\backslash$nthe wind is
significantly subluminal, it can persist long after the AGN$\backslash$nis
observed to have become sub-Eddington. The wind creates a
strong$\backslash$ncooling shock as it interacts with the interstellar medium
of the host$\backslash$ngalaxy, and this cooling region may be observable in
an inverse Compton$\backslash$ncontinuum and lower excitation emission lines
associated with lower$\backslash$nvelocities. The shell of matter swept up by
the (‘momentum-driven’)$\backslash$nshocked wind must propagate beyond the
black hole’s sphere of influence$\backslash$non a time-scale of $$~3
{$\backslash$times} 10$^{5}$yr. Outside this radius,$\backslash$nthe shell
stalls unless the black hole mass has reached the value$\backslash$nM$_{σ}$
implied by the M-{$σ$} relation. If the wind shock$\backslash$ndid not cool,
as suggested here, the resulting (‘energy-driven’) outflow$\backslash$nwould
imply a far smaller supermassive black hole mass than
actually$\backslash$nobserved. In galaxies with large bulges the black hole
may grow somewhat$\backslash$nbeyond this value, suggesting that the observed
M-{$σ$} relation may$\backslash$ncurve upwards at large M. Minor accretion
events with small gas$\backslash$nfractions can produce galaxy-wide outflows
with velocities significantly$\backslash$nexceeding {$σ$}, including fossil
outflows in galaxies where there is$\backslash$nlittle current AGN activity.
Some rare cases may reveal the$\backslash$nenergy-driven outflows which sweep
gas out of the galaxy and establish$\backslash$nthe black hole-bulge mass
relation. However, these require the quasar to$\backslash$nbe at the Eddington
luminosity.$\backslash$n, archivePrefix = arXiv, arxivId = 0911.1639, author =
King, A. R., doi = 10.1111/j.1365-2966.2009.16013.x, eprint = 0911.1639, file
= :home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/King - 2010 - Black hole outflows.pdf:pdf, issn = 00358711,
journal = Mon. Not. R. Astron. Soc., keywords = Accretion, accretion
discs,Black hole physics,Galaxies: active,Galaxies: formation, number = 3,
pages = 1516–1522, title = Black hole outflows, volume = 402, year = 2010
@article2041-8205-719-2-L208, author = Wang, Junfeng and Fabbiano, Giuseppina
and Risaliti, Guido and Elvis, Martin and Mundell, Carole G and Dumas, Gaelle
and Schinnerer, Eva and Zezas, Andreas, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley Desktop/Downloaded/Wang
et al. - 2010 - EXTENDED X-RAY EMISSION IN THE H i CAVITY OF NGC 4151 GALAXY-
SCALE ACTIVE GALACTIC NUCLEUS FEEDBACK.pdf:pdf, journal = Astrophys. J. Lett.,
number = 2, pages = L208, title = Extended X-ray Emission in the H I Cavity of
NGC 4151: Galaxy-scale Active Galactic Nucleus Feedback?, url =
http://stacks.iop.org/2041-8205/719/i=2/a=L208, volume = 719, year = 2010
@articleUnknownm, author = رسولی, چاپار, file =
:home/william/Documents/Papers/26060769.pdf:pdf, title = No Titleرساله ی دکتری
دانشگاه شهید بهشتی @articleBieri2016, abstract = The quasar mode of Active
Galactic Nuclei (AGN) in the high-redshift Universe is routinely observed in
gas-rich galaxies together with large-scale AGN-driven winds. It is crucial to
understand how photons emitted by the central AGN source couple to the ambient
interstellar-medium to trigger large-scale outflows. By means of radiation-
hydrodynamical simulations of idealised galactic discs, we study the coupling
of photons with the multiphase galactic gas, and how it varies with gas cloud
sizes, and the radiation bands included in the simulations, which are
ultraviolet (UV), optical, and infrared (IR). We show how a quasar with a
luminosity of $10^{46}$ erg/s can drive large-scale winds with velocities of
$10^2-10^3$ km/s and mass outflow rates around $10^3$ M$_$/yr for times of
order a few million years. Infrared radiation is necessary to efficiently
transfer momentum to the gas via multi-scattering on dust in dense clouds.
However, IR multi-scattering, despite being extremely important at early
times, quickly declines as the central gas cloud expands and breaks up,
allowing the radiation to escape through low gas density channels. The typical
number of multi-scattering events for an IR photon is only about a quarter of
the mean optical depth from the center of the cloud. Our models account for
the observed outflow rates of $$500-1000 M$_$/yr and high velocities of $10^3$
km/s, favouring winds that are energy-driven via extremely fast nuclear
outflows, interpreted here as being IR-radiatively-driven winds.,
archivePrefix = arXiv, arxivId = 1606.06281, author = Bieri, Rebekka and
Dubois, Yohan and Rosdahl, Joakim and Wagner, Alexander Y. and Silk, Joseph
and Mamon, Gary A., doi = 10.1093/mnras/stw2380, eprint = 1606.06281, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Bieri et al. - 2016 - Outflows Driven by Quasars in High-
Redshift Galaxies with Radiation Hydrodynamics.pdf:pdf, keywords =
active,galaxies,high-redshift,ism,methods, number = June, title = Outflows
Driven by Quasars in High-Redshift Galaxies with Radiation Hydrodynamics, url
= http://arxiv.org/abs/1606.06281%0Ahttp://dx.doi.org/10.1093/mnras/stw2380,
volume = 000, year = 2016 @articleZhuravleva2019, abstract = Transport
properties, such as viscosity and thermal conduction, of the hot intergalactic
plasma in clusters of galaxies are largely unknown. Whereas for laboratory
plasmas these characteristics are derived from the gas density and
temperature1, such recipes can be fundamentally different for the
intergalactic plasma2 owing to a low rate of particle collisions and a weak
magnetic field3. In numerical simulations, these unknowns can often be avoided
by modelling these plasmas as hydrodynamic fluids4–6, even though local, non-
hydrodynamic features observed in clusters contradict this assumption7–9.
Using deep Chandra observations of the Coma Cluster10,11, we probe gas
fluctuations in intergalactic medium down to spatial scales where the
transport processes should prominently manifest themselves—provided that
hydrodynamic models12 with pure Coulomb collision rates are indeed adequate.
We do not find evidence of such transport processes, implying that the
effective isotropic viscosity is orders of magnitude smaller than naively
expected. This indicates either an enhanced collision rate in the plasma due
to particle scattering off microfluctuations caused by plasma
instabilities2,13,14 or that the transport processes are anisotropic with
respect to the local magnetic field15. This also means that numerical models
with high Reynolds number appear more consistent with observations. Our
results demonstrate that observations of turbulence in clusters16,17 are
giving rise to a branch of astrophysics that can sharpen theoretical views on
galactic plasmas., author = Zhuravleva, I. and Churazov, E. and Schekochihin,
A. A. and Allen, S. W. and Vikhlinin, A. and Werner, N., doi =
10.1038/s41550-019-0794-z, file =
:home/william/Documents/Papers/10.1038@s41550-019-0794-z.pdf:pdf, issn =
23973366, journal = Nat. Astron., number = 9, pages = 832–837, publisher =
Springer US, title = Suppressed effective viscosity in the bulk intergalactic
plasma, url = http://dx.doi.org/10.1038/s41550-019-0794-z, volume = 3, year =
2019 @articleArav2020, abstract = The Hubble Space Telescope/Cosmic Origins
Spectrograph (COS) has opened a new discovery space for studying quasar
absorption outflows and their contribution to AGN feedback. Specifically, COS
provides high-quality far-ultraviolet (FUV) spectra covering the diagnostic-
rich 500-1050 Angstrom rest frame (hereafter, EUV500) of medium redshift
objects. The quality and quantity of EUV500 diagnostic troughs allow us to
probe the very high-ionization phase, which carries 90% or more of the
outflowing material, as well as to determine the distance of most outflows
from the central source ($R$). The first objective is impossible to achieve
with ground-based spectra, and $R$ can be measured in only $$1% of them. Here,
we summarize the main results of the first dedicated survey of such outflows,
including the following: 1) Measurements of the three most energetic outflows
to date, which can be the main agents for AGN feedback processes in the
environments of the host galaxies. 2) All the outflows have a very high-
ionization component, similar to the one found in warm absorbers, which
carries most of the outflow’s kinetic luminosity. This finding suggests that
all the high-ionization outflows observed from the ground also have a similar
undetected very high-ionization component. 3) Of the 13 studied EUV500
outflows, 9 have $100R2000$ parsecs, 2 have $5R20$ parsecs, 1 has $0.05R50$
parsecs, and in 1 case, $R$ cannot be determined. 4) One of the outflows has
the largest velocity shift (1550 km s$^{-1}$) and acceleration (1.5 cm
s$^{-2}$) measured to date. This outflow is physically similar to the fast
X-ray outflow detected in quasar PG 1211+143., archivePrefix = arXiv, arxivId
= 2003.08688, author = Arav, Nahum and Xu, Xinfeng and Miller, Timothy and
Kriss, Gerard A. and Plesha, Rachel, doi = 10.3847/1538-4365/ab66af, eprint =
2003.08688, file = :home/william/Documents/Papers/[Arav et al.]-HST-COS
OBSERVATIONS OF QUASAR OUTFLOWS IN .pdf:pdf, journal = Astrophys. J. Suppl.
Ser., keywords = 1646,absorption lines,active,galaxies,general,individual,jets
and outflows,kinematics and dynamics,quasars,sdss j1042, number = 2, pages =
37, title = HST /COS Observations of Quasar Outflows in the 500–1050 Å Rest
Frame. I. The Most Energetic Outflows in the Universe and Other Discoveries ,
volume = 247, year = 2020 @articleHeywood2022, abstract = The inner ∼200 pc
region of the Galaxy contains a 4 million M ⊙ supermassive black hole (SMBH),
significant quantities of molecular gas, and star formation and cosmic-ray
energy densities that are roughly two orders of magnitude higher than the
corresponding levels in the Galactic disk. At a distance of only 8.2 kpc, the
region presents astronomers with a unique opportunity to study a diverse range
of energetic astrophysical phenomena, from stellar objects in extreme
environments, to the SMBH and star-formation-driven feedback processes that
are known to influence the evolution of galaxies as a whole. We present a new
survey of the Galactic center conducted with the South African MeerKAT radio
telescope. Radio imaging offers a view that is unaffected by the large
quantities of dust that obscure the region at other wavelengths, and a scene
of striking complexity is revealed. We produce total-intensity and spectral-
index mosaics of the region from 20 pointings (144 hr on-target in total),
covering 6.5 square degrees with an angular resolution of 4″ at a central
frequency of 1.28 GHz. Many new features are revealed for the first time due
to a combination of MeerKAT’s high sensitivity, exceptional u , v -plane
coverage, and geographical vantage point. We highlight some initial survey
results, including new supernova remnant candidates, many new nonthermal
filament complexes, and enhanced views of the Radio Arc bubble, Sagittarius A,
and Sagittarius B regions. This project is a South African Radio Astronomy
Observatory public legacy survey, and the image products are made available
with this article. , archivePrefix = arXiv, arxivId = 2201.10541, author =
Heywood, I. , doi = 10.3847/1538-4357/ac449a, eprint = 2201.10541, file =
:home/william/Documents/Papers/Heywood_2022_ApJ_925_165.pdf:pdf, issn =
0004-637X, journal = Astrophys. J., keywords = Galactic center,Galactic radio
sources,Radio interferometry, number = 2, pages = 165, publisher = IOP
Publishing, title = The 1.28 GHz MeerKAT Galactic Center Mosaic, url =
http://arxiv.org/abs/2201.10541%0Ahttp://dx.doi.org/10.3847/1538-4357/ac449a,
volume = 925, year = 2022 @articleSemenov2021, abstract = Observations of the
$$-ray emission around star clusters, isolated supernova remnants, and pulsar
wind nebulae indicate that cosmic ray (CR) diffusion coefficient near the
acceleration sites can be suppressed by a large factor compared to the Galaxy
average. We explore the effects of such local suppression of CR diffusion on
galaxy evolution using simulations of isolated disk galaxies with regular and
high gas fractions. Our results show that while CR propagation with constant
diffusivity can make gaseous disks more stable by increasing the midplane
pressure, large-scale CR pressure gradients cannot prevent local fragmentation
when the disk is unstable. In contrast, when CR diffusivity is suppressed in
star-forming regions, accumulation of CRs in these regions results in strong
local pressure gradients that prevent formation of massive gaseous clumps. As
a result, the distribution of dense gas and star formation changes
qualitatively: a globally unstable gaseous disk does not violently fragment
into massive star-forming clumps but maintains a regular grand-design spiral
structure. This effect regulates star formation and disk structure and is
qualitatively different from and complementary to the global role of CRs in
vertical hydrostatic support of the gaseous disk and in driving galactic
winds., archivePrefix = arXiv, arxivId = 2012.01427, author = Semenov, Vadim
A. and Kravtsov, Andrey V. and Caprioli, Damiano, doi =
10.3847/1538-4357/abe2a6, eprint = 2012.01427, file =
:home/william/Documents/Papers/2012.01427.pdf:pdf, issn = 0004-637X, journal =
Astrophys. J., keywords = cosmic rays,formation,galaxies,ism,kinematics and
dynamics,methods,stars, number = 2, pages = 126, title = Cosmic-Ray Diffusion
Suppression in Star-forming Regions Inhibits Clump Formation in Gas-rich
Galaxies, volume = 910, year = 2021 @articleMelioli2009b, abstract = The
ejection of the gas out of the disk in late-type galaxies is related to star
formation and is due mainly to Type II supernovae. In this paper we studied in
detail the development of the Galactic fountains in order to understand their
dynamical evolution and their influence in the redistribution of the freshly
delivered metals over the disk. To this aim, we performed a number of 3D
hydrodynamical radiative cooling simulations of the gas in the Milky Way where
the whole Galaxy structure, the Galactic differential rotation and the
supernovae explosions generated by a single OB association are considered. A
typical fountain powered by 100 Type II supernovae may eject material up to
$2$ kpc which than collapses back mostly in form of dense, cold clouds and
filaments. The majority of the gas lifted up by the fountains falls back on
the disk remaining within a radial distance $R=0.5$ kpc from the place where
the fountain originated. This localized circulation of disk gas does not
influence the radial chemical gradients on large scale, as required by the
chemical models of the Milky Way which reproduce the metallicity distribution
without invoking large fluxes of metals. Simulations of multiple fountains
fuelled by Type II supernovae of different OB associations will be presented
in a companion paper., author = Melioli, C. and Brighenti, F. and D’Ercole, A.
and De Gouveia Dal Pino, E. M., doi = 10.1111/j.1365-2966.2009.14725.x, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Melioli et al. - 2009 - Hydrodynamical simulations of
Galactic fountains - II. Evolution of multiple fountains.pdf:pdf, issn =
00358711, journal = Mon. Not. R. Astron. Soc., keywords = Galaxy: disc,Galaxy:
general,Hydrodynamics,ISM: bubbles,ISM: clouds,Methods: numerical, number = 3,
pages = 1089–1105, title = Hydrodynamical simulations of Galactic fountains -
II. Evolution of multiple fountains, volume = 399, year = 2009
@articleZubovas2014, abstract = It is usually assumed that outflows from
luminous active galactic nuclei (AGN) are either in the energy-conserving
(non-radiative) or in the momentum-conserving (radiative) regime. We show that
in a non-spherical geometry the effects of both regimes may manifest at the
same time, and that it is the momentum of the outflow that sets the
MBH-$\sigma$ relation. Considering an initially elliptical distribution of gas
in the host galaxy, we show that a non-radiative outflow opens up a wide
’escape route’ over the paths of least resistance. Most of the outflow energy
escapes in that direction. At the same time, in the directions of higher
resistance, the ambient gas is affected mainly by the incident momentum from
the outflow. Quenching SMBH growth requires quenching gas delivery along the
paths of highest resistance, and therefore, it is the momentum of the outflow
that limits the black hole growth. We present an analytical argument showing
that such energy-conserving feedback bubbles driving leaky ambient shells will
terminate SMBH growth once its mass reaches roughly the M$\sigma$ mass derived
earlier by King for momentum-conserving AGN outflows. Our simulations also
have potentially important implications for observations of AGN jet feedback
and starburst galaxy feedback. The collimation of the wide angle AGN outflow
away from the symmetry plane, as found in our simulations, indicates that
credit for work done by such outflows may sometimes be mistakenly given to AGN
jets or star formation feedback since wide angle $\nu$ ~ 0.1c outflows are
harder to observe and the phase when they are present may be short. 2014 The
Authors Published by Oxford University Press on behalf of the Royal
Astronomical Society., archivePrefix = arXiv, arxivId = 1403.3933, author =
Zubovas, Kastytis and Nayakshin, Sergei, doi = 10.1093/mnras/stu431, eprint =
1403.3933, file =
:home/william/Documents/Papers/MNRAS-2014-Zubovas-2625-35.pdf:pdf, issn =
13652966, journal = Mon. Not. R. Astron. Soc., keywords = Accretion, accretion
discs,Black hole physics,Galaxies: evolution,Quasars: general, number = 3,
pages = 2625–2635, title = Energy- and momentum-conserving AGN feedback
outflows, volume = 440, year = 2014 @articleGarcia-Burillo2014, abstract =
Aims. We investigate the fueling and the feedback of star formation and
nuclear activity in NGC 1068, a nearby (D = 14 Mpc) Seyfert 2 barred galaxy,
by analyzing the distribution and kinematics of the molecular gas in the disk.
We aim to understand if and how gas accretion can self-regulate.Methods. We
have used the Atacama Large Millimeter Array (ALMA) to map the emission of a
set of dense molecular gas (n(H2) ’ 1056 cm3) tracers (CO(3-2), CO(6-5),
HCN(4-3), HCO+(4-3), and CS(7-6)) and their underlying continuum emission in
the central r ∼ 2 kpc of NGC 1068 with spatial resolutions ∼0:3000:500 (∼20-35
pc for the assumed distance of D = 14 Mpc). Results. The sensitivity and
spatial resolution of ALMA give an unprecedented detailed view of the
distribution and kinematics of the dense molecular gas (n(H2) ≈ 1056cm3) in
NGC 1068. Molecular line and dust continuum emissions are detected from a r ∼
200 pc off-centered circumnuclear disk (CND), from the 2.6 kpc-diameter bar
region, and from the r ∼ 1:3 kpc starburst (SB) ring. Most of the emission in
HCO+, HCN, and CS stems from the CND. Molecular line ratios show dramatic
order-of-magnitude changes inside the CND that are correlated with the
UV/X-ray illumination by the active galactic nucleus (AGN), betraying ongoing
feedback. We used the dust continuum fluxes measured by ALMA together with
NIR/MIR data to constrain the properties of the putative torus using CLUMPY
models and found a torus radius of 20+6 10 pc. The Fourier decomposition of
the gas velocity field indicates that rotation is perturbed by an inward
radial flow in the SB ring and the bar region. However, the gas kinematics
from r ∼ 50 pc out to r ∼ 400 pc reveal a massive (Mmol ∼ 2:7+0:9 1:2 × 107 M)
outflow in all molecular tracers. The tight correlation between the ionized
gas outflow, the radio jet, and the occurrence of outward motions in the disk
suggests that the outflow is AGN driven. Conclusions. The molecular outflow is
likely launched when the ionization cone of the narrow line region sweeps the
nuclear disk. The outflow rate estimated in the CND, dM=dt ∼ 63+21 37 M yr1,
is an order of magnitude higher than the star formation rate at these radii,
confirming that the outflow is AGN driven. The power of the AGN is able to
account for the estimated momentum and kinetic luminosity of the outflow. The
CND mass load rate of the CND outflow implies a very short gas depletion
timescale of ≤1 Myr. The CND gas reservoir is likely replenished on longer
timescales by efficient gas inflow from the outer disk. ESO 2014.,
archivePrefix = arXiv, arxivId = 1405.7706, author = García-Burillo, S. and
Combes, F. and Usero, A. and Aalto, S. and Krips, M. and Viti, S. and Alonso-
Herrero, A. and Hunt, L. K. and Schinnerer, E. and Baker, A. J. and Boone, F.
and Casasola, V. and Colina, L. and Costagliola, F. and Eckart, A. and Fuente,
A. and Henkel, C. and Labiano, A. and Martín, S. and Márquez, I. and Muller,
S. and Planesas, P. and Ramos Almeida, C. and Spaans, M. and Tacconi, L. J.
and Van Der Werf, P. P., doi = 10.1051/0004-6361/201423843, eprint =
1405.7706, file = :home/william/Documents/Papers/[Garcia-Burillo, Combes et
al.]-Molecular line emission in NGC 1068 imaged with ALMA.pdf:pdf, issn =
14320746, journal = Astron. Astrophys., keywords = Galaxies: ISM,Galaxies:
Seyfert,Galaxies: individual: NGC 1068,Galaxies: kinematics and
dynamics,Galaxies: nuclei,Radio lines: galaxies, pages = 1–24, title =
Molecular line emission in NGC 1068 imaged with ALMA : I. An AGN-driven
outflow in the dense molecular gas, volume = 567, year = 2014
@articlePeretti2018, abstract = The high rate of star formation and supernova
explosions of starburst galaxies make them interesting sources of high energy
radiation. Depending upon the level of turbulence present in the their
interstellar medium, the bulk of cosmic rays produced inside starburst
galaxies may lose most of their energy before escaping, thereby making these
sources behave as calorimeters, at least up to some maximum energy. Contrary
to previous studies, here we investigate in detail the conditions under which
cosmic ray confinement may be effective for electrons and nuclei and we study
the implications of cosmic ray confinement in terms of multifrequency emission
from starburst nuclei and production of high energy neutrinos. The general
predictions are then specialized to three cases of active starbursts, namely
M82, NGC253 and Arp220. Both primary and secondary electrons, as well as
electron-positron pairs produced by gamma ray absorption inside starburst
galaxies are taken into account. Electrons and positrons produced as secondary
products of hadronic interactions are found to be responsible for most of the
emission of leptonic origin. In particular, synchrotron emission of very high
energy secondary electrons produces an extended emission of hard X-rays that
represent a very interesting signature of hadronic process in starburst
galaxies, potentially accessible to current and future observations in the
X-ray band. A careful understanding of both the production and absorption of
gamma rays in starburst galaxies is instrumental to the assessment of the role
of these astrophysical sources as sources of high energy astrophysical
neutrinos., archivePrefix = arXiv, arxivId = 1812.01996v1, author = Peretti,
Enrico and Blasi, Pasquale and Aharonian, Felix and Morlino, Giovanni, eprint
= 1812.01996v1, file = :home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Peretti et al. - 2018 - Cosmic ray transport and radiative
processes in nuclei of starburst galaxies.pdf:pdf, journal = Mnras, keywords =
Confinement,Cosmic rays-,Starburst galaxy-, number = December, pages = 1–14,
title = Cosmic ray transport and radiative processes in nuclei of starburst
galaxies, url = https://arxiv.org/pdf/1812.01996.pdf, volume = 000, year =
2018 @articleBanda-Barragan2016b, abstract = Filamentary structures are
ubiquitous in the interstellar medium, yet their formation, internal
structure, and longevity have not been studied in detail. We report the
results from a comprehensive numerical study that investigates the
characteristics, formation, and evolution of filaments arising from
magnetohydrodynamic interactions between supersonic winds and dense clouds.
Here, we improve on previous simulations by utilizing sharper density
contrasts and higher numerical resolutions. By following multiple density
tracers, we find that material in the envelopes of the clouds is removed and
deposited downstream to form filamentary tails, while the cores of the clouds
serve as footpoints and late-stage outer layers of these tails. Aspect ratios
≳12, subsonic velocity dispersions ~0.1-0.3 of the wind sound speed, and
magnetic field amplifications ~100 are found to be characteristic of these
filaments. We also report the effects of different magnetic field strengths
and orientations. The magnetic field strength regulates vorticity production:
sinuous filamentary towers arise in non-magnetic environments, while strong
magnetic fields inhibit small-scale perturbations at boundary layers making
tails less turbulent. Magnetic field components aligned with the direction of
the flow favour the formation of pressure-confined flux ropes inside the
tails, whilst transverse components tend to form current sheets. Softening the
equation of state to nearly isothermal leads to suppression of dynamical
instabilities and further collimation of the tail. Towards the final stages of
the evolution, we find that small cloudlets and distorted filaments survive
the break-up of the clouds and become entrained in the winds, reaching
velocities ~0.1 of the wind speed., archivePrefix = arXiv, arxivId =
1510.05356, author = Banda-Barragán, W. E. and Parkin, E. R. and Federrath, C.
and Crocker, R. M. and Bicknel, G. V., doi = 10.1093/mnras/stv2405, eprint =
1510.05356, file = :home/william/Documents/Papers/stv2405.pdf:pdf, issn =
13652966, journal = Mon. Not. R. Astron. Soc., keywords = Galaxies:
starburst,ISM: clouds,ISM: magnetic fields,MHD- methods: numerical,Stars:
winds, outflows, number = 2, pages = 1309–1333, title = Filament formation in
wind-cloud interactions - I. Spherical clouds in uniform magnetic fields,
volume = 455, year = 2016 @articleGuimaraesM.&Silva1985, abstract = er than
those in most current practice; and the use of a variable-size detector
requires even larger sample areas but gives considerably better results. 1. M.
Fuller and P. Griffiths, Anal. Chem. 50, 1906 (1978)., author = Lepp and
McCray, file = :home/william/Documents/Papers/[Leep et al.]-Thermal Phases of
Interestellar and Quasar gas.pdf:pdf, journal = 日本鉄鋼協会 第 109 回(春季)講演大会,
keywords = dorsiflexion - movement initiation,h-reflex - reciprocal
inhibition,la inhibition - ankle, number = 103, pages = 1984, title = Thermal
Phases of the ISM and Quasar gas, volume = 11, year = 1985
@article2005ApJ…618..569M, author = Murray, N and Quataert, E and Thompson,
T.~A., doi = 10.1086/426067, file =
:home/william/Documents/Papers/Murray_2005_ApJ_618_569.pdf:pdf, journal = Apj,
keywords = Galaxies: Formation,Galaxies: Fundamental Parameters,Galaxies:
General,Galaxies: Intergalactic Medium,Galaxies: Starburst, pages = 569–585,
title = On the Maximum Luminosity of Galaxies and Their Central Black Holes:
Feedback from Momentum-driven Winds, volume = 618, year = 2005
@articleNavarro1996, abstract = We use N-body simulations to investigate the
structure of dark halos in the standard Cold Dark Matter cosmogony. Halos are
excised from simulations of cosmologically representative regions and are
resimulated individually at high resolution. We study objects with masses
ranging from those of dwarf galaxy halos to those of rich galaxy clusters. The
spherically averaged density profiles of all our halos can be fit over two
decades in radius by scaling a simple “universal” profile. The characteristic
overdensity of a halo, or equivalently its concentration, correlates strongly
with halo mass in a way which reflects the mass dependence of the epoch of
halo formation. Halo profiles are approximately isothermal over a large range
in radii, but are significantly shallower than $r^{-2}$ near the center and
steeper than $r^{-2}$ near the virial radius. Matching the observed rotation
curves of disk galaxies requires disk mass-to-light ratios to increase
systematically with luminosity. Further, it suggests that the halos of bright
galaxies depend only weakly on galaxy luminosity and have circular velocities
significantly lower than the disk rotation speed. This may explain why
luminosity and dynamics are uncorrelated in observed samples of binary
galaxies and of satellite/spiral systems. For galaxy clusters, our halo models
are consistent both with the presence of giant arcs and with the observed
structure of the intracluster medium, and they suggest a simple explanation
for the disparate estimates of cluster core radii found by previous authors.
Our results also highlight two shortcomings of the CDM model. CDM halos are
too concentrated to be consistent with the halo parameters inferred for dwarf
irregulars, and the predicted abundance of galaxy halos is larger than the
observed abundance of galaxies., archivePrefix = arXiv, arxivId = astro-
ph/9508025, author = Navarro, Julio F. and Frenk, Carlos S. and White, Simon
D. M., doi = 10.1086/177173, eprint = 9508025, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Navarro, Frenk, White - 1996 - The Structure of Cold Dark
Matter Halos.pdf:pdf, isbn = 0792339754, issn = 0004-637X, journal =
Astrophys. J., pages = 563, pmid = 15003161, primaryClass = astro-ph, title =
The Structure of Cold Dark Matter Halos, url =
http://adsabs.harvard.edu/doi/10.1086/177173, volume = 462, year = 1996
@articleFay1967, abstract = Supernova explosions in a cloudy interstellar
medium produce a three-component medium in which a large fraction of the
volume is filled with hot, tenuous gas. In the disk of the galaxy the
evolution of supernova remnants is altered by evaporation of cool clouds
embedded in the hot medium. Radiative losses are enhanced by the resulting
increase in density and by radiation from the conductive interfaces between
clouds and hot gas. Mass balance (cloud evaporation rate = dense shell
formation rate) and energy balance (supernova shock input = radiation loss)
deter- mine the density and temperature of the hot medium with («, T) =
(IO-2-5, 105-7) being repre- sentative values. Very small clouds will be
rapidly evaporated or swept up. The outer edges of “standard” clouds ionized
by the diffuse UV and soft X-ray backgrounds provide the warm (~104 K) ionized
and neutral components. A self-consistent model of the interstellar medium
developed herein accounts for the observed pressure of interstellar clouds,
the galactic soft X-ray background, the O vi absorption line observations, the
ionization and heating of much of the interstellar medium, and the motions of
the clouds. In the halo of the galaxy, where the clouds are relatively
unimportant, we estimate («, T) = (IO-3-3, 106 0) below one pressure scale
height. Energy input from halo supernovae is probably adequate to drive a
galactic wind, author = Christopher F. McKee and Jeremiah P. Ostriker, file =
:home/william/Documents/Papers/1977ApJ…218..148M.pdf:pdf, journal = Astrophys.
Journal, 218148-169, 1977 Novemb. 15, pages = 148–169, title = A THEORY OF THE
INTERSTELLAR MEDIUM: THREE COMPONENTS REGULATED BY SUPERNOVA EXPLOSIONS IN AN
INHOMOGENEOUS SUBSTRATE, year = 1967 @articleEmilia2021, author = Emilia,
Regio, file = :home/william/Documents/Papers/Clavijo-Dal Pino-Melioli.pdf:pdf,
keywords = active galaxies,galactic winds,holes,magneto-hydrodynamical
simulations,star formation,super massive black, title = FEEDBACK IN GALAXIES
HOSTING AGN AND SF WINDS : THE EFFECTS OF THE AGN FLICKERING AND THE, year =
2021 @articleMertsch2017, abstract = The discovery of the Fermi bubbles—a huge
bilobular structure seen in GeV gamma-rays above and below the Galactic
center—implies the presence of a large reservoir of high energy particles at
$10 \, {kpc}$ from the disk. The absence of evidence for a strong shock
coinciding with the edge of the bubbles, and constraints from multi-wavelength
observations point towards stochastic acceleration by turbulence as a likely
mechanism of acceleration. We have investigated the time-dependent
acceleration of electrons in a large-scale outflow from the Galactic centre.
For the first time, we present a detailed numerical solution of the particle
kinetic equation that includes the acceleration, transport and relevant energy
loss processes. We also take into account the addition of shock acceleration
of electrons at the bubble’s blast wave. Fitting to the observed spectrum and
surface brightness distribution of the bubbles allows determining the
transport coefficients, thereby shedding light on the origin of the Fermi
bubbles., archivePrefix = arXiv, arxivId = arXiv:1808.00330v1, author =
Mertsch, Philipp and Petrosian, Vahé, eprint = arXiv:1808.00330v1, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Mertsch, Petrosian - 2017 - The Fermi bubbles from
stochastic acceleration by turbulence in a galactic outflow.pdf:pdf, issn =
18248039, journal = Proc. Sci., keywords = acceleration of particles -,cosmic
rays - ism,gamma rays,ism,jets and outflows -,shock waves - turbulence, pages
= 1–14, title = The Fermi bubbles from stochastic acceleration by turbulence
in a galactic outflow, year = 2017 @articleSullivan2008, abstract = We are
using ”broadband” (4.6 to 43 GHz) multi-frequency VLBA polarization
observations of compact AGN to investigate the 3-D structure of their jet
magnetic (B) fields. Observing at several frequencies, separated by short and
long intervals, enables reliable determination of the distribution of Faraday
Rotation, and thereby the intrinsic B field structure. Transverse Rotation
Measure (RM) gradients were detected in the jets of 0954+658 and 1418+546,
providing evidence for the presence of a helical B field surrounding the jet.
The RM in the core regions of 2200+420 (BL Lac), 0954+658 and 1418+546 display
different signs in different frequency-intervals (on different spatial
scales); we suggest an explanation for this in terms of modest bends in a
helical B field surrounding their jets. In future, polarization observations
with a combination of VSOP-2 at 8, 22 and 43 GHz and ground arrays at
frequencies with corresponding resolution will help map out the distributions
of Faraday rotation, spectral index and the 3-D B field structure both across
the jet and closer to the central engine, providing strong constraints for any
jet B field models., archivePrefix = arXiv, arxivId = 0801.4897, author =
O’Sullivan, Shane P. and Gabuzda, Denise C, eprint = 0801.4897, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Sullivan, Gabuzda - 2008 - The Need For High Resolution In
Studies Of The 3-D Magnetic Field Structure Of AGN Jets.pdf:pdf, pages = 1–4,
title = The Need For High Resolution In Studies Of The 3-D Magnetic Field
Structure Of AGN Jets, url = http://arxiv.org/abs/0801.4897, year = 2008
@articleRathjen2021, abstract = We present simulations of the multiphase
interstellar medium (ISM) at solar neighbourhood conditions including thermal
and non-thermal ISM processes, star cluster formation, and feedback from
massive stars: stellar winds, hydrogen ionizing radiation computed with the
novel treeray radiative transfer method, supernovae (SN), and the injection of
cosmic rays (CR). N-body dynamics is computed with a 4th-order Hermite
integrator. We systematically investigate the impact of stellar feedback on
the self-gravitating ISM with magnetic fields, CR advection and diffusion, and
non-equilibrium chemical evolution. SN-only feedback results in strongly
clustered star formation with very high star cluster masses, a bi-modal
distribution of the ambient SN densities, and low volume-filling factors (VFF)
of warm gas, typically inconsistent with local conditions. Early radiative
feedback prevents an initial starburst, reduces star cluster masses and
outflow rates. Furthermore, star formation rate surface densities of $_{{M}_}
= 1.4-5.9 10^{-3}$${M}_\, {yr}^{-1}\, {kpc}^{-2}$, VFFwarm = 60-80 per cent as
well as thermal, kinetic, magnetic, and cosmic ray energy densities of the
model including all feedback mechanisms agree well with observational
constraints. On the short, 100 Myr, time-scales investigated here, CRs only
have a moderate impact on star formation and the multiphase gas structure and
result in cooler outflows, if present. Our models indicate that at low gas
surface densities SN-only feedback only captures some characteristics of the
star-forming ISM and outflows/inflows relevant for regulating star formation.
Instead, star formation is regulated on star cluster scales by radiation and
winds from massive stars in clusters, whose peak masses agree with solar
neighbourhood estimates., archivePrefix = arXiv, arxivId = 2103.14128, author
= Rathjen, Tim Eric and Naab, Thorsten and Girichidis, Philipp and Walch,
Stefanie and Wünsch, Richard and Dinnbier, František and Seifried, Daniel and
Klessen, Ralf S. and Glover, Simon C.O., doi = 10.1093/mnras/stab900, eprint =
2103.14128, file = :home/william/Documents/Papers/2103.14128.pdf:pdf, issn =
13652966, journal = Mon. Not. R. Astron. Soc., keywords = ISM: evolution,ISM:
structure,cosmic rays,galaxies: ISM,galaxies: star formation,methods:
numerical, number = 1, pages = 1039–1061, title = SILCC VI - Multiphase ISM
structure, stellar clustering, and outflows with supernovae, stellar winds,
ionizing radiation, and cosmic rays, volume = 504, year = 2021
@articleFigureb, author = Henón, M, doi = 10.15713/ins.mmj.3, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Figure - Unknown - No Title No Title_2015.pdf:pdf, isbn =
9789004310087, journal = A&A, number = c, pages = 1–4, pmid = 29982528, title
= Vlasov Equation?, year = 1982 @articleHarfst2006, abstract = We present a
new particle code for modelling the evolution of galaxies. The code is based
on a multi-phase description for the interstellar medium (ISM). We include
star formation (SF), stellar feedback by massive stars and planetary nebulae,
phase transitions, and interactions between gas clouds and ambient diffuse
gas, namely condensation, evaporation, drag, and energy dissipation. The last
is realised by radiative cooling and inelastic cloud-cloud collisions. We
present new schemes for SF and stellar feedback that include a consistent
calculation of the star-formation efficiency (SFE) based on ISM properties, as
well as a detailed redistribution of the feedback energy into the different
ISM phases. As a first test we show a model of the evolution of a present day
Milky-Way-type galaxy. Though the model exhibits a quasi-stationary behaviour
in global properties like mass fractions or surface densities, the evolution
of the ISM is strongly variable locally depending on the local SF and stellar
feedback. We start only with two distinct phases, but a three-phase ISM is
formed soon and consists of cold molecular clouds, a warm gas disk, and a hot
gaseous halo. Hot gas is also found in bubbles in the disk accompanied by type
II supernovae explosions. The volume-filling factor of the hot gas in the disk
is ∼35%. The mass spectrum of the clouds follows a power-law with an index of
$\alpha$ ≈-2. The star-formation rate (SFR) is ∼ 1.6 M⊙ yr-1 on average,
decreasing slowly with time due to gas consumption. In order to maintain a
constant SFR, gas replenishment, e.g. by infall, of the order 1 M⊙ yr-1 is
required. Our model is in fair agreement with Kennicutt’s (1998, ApJ, 498,
541) SF law including the cut-off at ∼10 M⊙ pc-2. Models with a constant SFE,
i.e. no feedback on the SF, fail to reproduce Kennicutt’s law. We performed a
parameter study varying the particle resolution, feedback energy, cloud
radius, SF time scale, and metallicity. In most these cases the evolution of
the model galaxy was not significantly different to our reference model.
Increasing the feedback energy by a factor of 4-5 lowers the SF rate by ∼0.5
M⊙ yr-1, while decreasing the metallicity by a factor of ∼100 increases the
mass fraction of the hot gas from about 10% to 30%. ESO 2006., archivePrefix =
arXiv, arxivId = astro-ph/0511775, author = Harfst, S. and Theis, Ch and
Hensler, G., doi = 10.1051/0004-6361:20042190, eprint = 0511775, file =
:home/william/Documents/Papers/0511775.pdf:pdf, issn = 00046361, journal =
Astron. Astrophys., keywords = Galaxies: ISM,Galaxies: kinematics and
dynamics,Galaxy: evolution,ISM: evolution,Methods: N-body simulations, number
= 2, pages = 509–518, primaryClass = astro-ph, title = Modelling galaxies with
a 3d multi-phase ISM, volume = 449, year = 2006 @articleKing2021, abstract =
The sample of dwarf galaxies with measured central black hole masses M and
velocity dispersions $\sigma$ has recently doubled, and gives a close fit to
the extrapolation of the M-$\sigma$ relation for more massive galaxies. We
argue that this is difficult to reconcile with suggestions that the scaling
relations between galaxies and their central black holes are simply a
statistical consequence of assembly through repeated mergers. This predicts
black hole masses significantly larger than those observed in dwarf galaxies
unless the initial distribution of uncorrelated seed black hole and stellar
masses is confined to much smaller masses than earlier assumed. It also
predicts a noticeable flattening of the M-$\sigma$ relation for dwarfs, to M
$\sigma$2 compared with the observed M $\sigma$4\. In contrast black hole
feedback predicts that black hole masses tend towards a universal M $\sigma$4
relation in all galaxies, and correctly gives the properties of powerful
outflows recently observed in dwarf galaxies. These considerations emphasize
once again that the fundamental physical black hole-galaxy scaling relation is
between M and $\sigma$. The relation of M to the bulge mass Mb is acausal, and
depends on the quite independent connection between Mb and $\sigma$ set by
stellar feedback., archivePrefix = arXiv, arxivId = 2012.06258, author = King,
Andrew and Nealon, Rebecca, doi = 10.1093/mnrasl/slaa200, eprint = 2012.06258,
file = :home/william/Documents/Papers/2012.06258.pdf:pdf, issn = 17453933,
journal = Mon. Not. R. Astron. Soc. Lett., keywords = X-rays: galaxies:
dwarf,black hole physics,galaxies: Active,galaxies: Seyfert,quasars: general,
number = 1, pages = L1–L5, title = Dwarf galaxies and the black hole scaling
relations, volume = 502, year = 2021 @articlePlotnikov2018, abstract =
Perpendicular relativistic ($\gamma$ 0= 10) shocks in magnetized pair plasmas
are investigated using two-dimensional Particle-in-Cell simulations. A
systematic survey, from unmagnetized to strongly magnetized shocks, is
presented accurately capturing the transition from Weibelmediated to magnetic-
reflection-shaped shocks. This transition is found to occur for upstream flow
magnetizations 10-3 $\sigma$ 10-2 at which a strong perpendicular net current
is observed in the precursor, driving the so-called current-filamentation
instability. The global structure of the shock and shock formation time are
discussed. The magnetohydrodynamics shock jump conditions are found in good
agreement with the numerical results, except for 10-4 $\sigma$ 10-2 where a
deviation up to 10 per cent is observed. The particle precursor length
converges towards the Larmor radius of particles injected in the upstream
magnetic field at intermediate magnetizations. For $\sigma$ 10-2, it leaves
place to a purely electromagnetic precursor following from the strong emission
of electromagnetic waves at the shock front. Particle acceleration is found to
be efficient in weakly magnetized perpendicular shocks in agreement with
previous works, and is fully suppressed for $\sigma$ 10-2. Diffusive shock
acceleration is observed only in weakly magnetized shocks, while a dominant
contribution of shock drift acceleration is evidenced at intermediate
magnetizations. The spatial diffusion coefficients are extracted from the
simulations allowing for a deeper insight into the self-consistent particle
kinematics and scale with the square of the particle energy in weakly
magnetized shocks. These results have implications for particle acceleration
in the internal shocks of active galactic nucleus jets and in the termination
shocks of pulsar wind nebulae., archivePrefix = arXiv, arxivId = 1712.02883,
author = Plotnikov, Illya and Grassi, Anna and Grech, Mickael, doi =
10.1093/MNRAS/STY979, eprint = 1712.02883, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Grassi, Grech - 2018 - Perpendicular relativistic shocks in
magnetized pair plasma Illya.pdf:pdf, issn = 13652966, journal = Mon. Not. R.
Astron. Soc., keywords = Acceleration of particles,Plasmas,Relativistic
processes,Shock waves, number = 4, pages = 5238–5260, title = Perpendicular
relativistic shocks in magnetized pair plasma, volume = 477, year = 2018
@articleKataoka2013a, abstract = We present Suzaku X-ray observations along
two edge regions of the Fermi Bubbles, with eight ~20 ksec pointings across
the northern part of the North Polar Spur (NPS) surrounding the north bubble
and six across the southernmost edge of the south bubble. After removing
compact X-ray features, diffuse X-ray emission is clearly detected and is well
reproduced by a three-component spectral model consisting of unabsorbed
thermal emission (temperature kT ~0.1 keV from the Local Bubble (LB), absorbed
kT ~0.3 keV thermal emission related to the NPS and/or Galactic Halo (GH), and
a power-law component at a level consistent with the cosmic X-ray background.
The emission measure (EM) of the 0.3 keV plasma decreases by ~50% toward the
inner regions of the north-east bubble, with no accompanying temperature
change. However, such a jump in the EM is not clearly seen in the south bubble
data. While it is unclear if the NPS originates from a nearby supernova
remnant or is related to previous activity within/around the Galactic Center,
our Suzaku observations provide evidence suggestive of the latter scenario. In
the latter framework, the presence of a large amount of neutral matter
absorbing the X-ray emission as well as the existence of the kT ~ 0.3 keV gas
can be naturally interpreted as a weak shock driven by the bubbles’ expansion
in the surrounding medium, with velocity v_exp ~300 km/s (corresponding to
shock Mach number M ~1.5), compressing the GH gas to form the NPS feature. We
also derived an upper limit for any non-thermal X-ray emission component
associated with the bubbles and demonstrate, that in agreement with the
findings above, the non-thermal pressure and energy estimated from a one-zone
leptonic model of its broad-band spectrum, are in rough equilibrium with that
of the surrounding thermal plasma., author = Kataoka, J. and Tahara, M. and
Totani, T. and Sofue, Y. and Stawarz and Takahashi, Y. and Takeuchi, Y. and
Tsunemi, H. and Kimura, M. and Takei, Y. and Cheung, C. C. and Inoue, Y. and
Nakamori, T., doi = 10.1088/0004-637X/779/1/57, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Kataoka et al. - 2013 - SUZAKU observations of the diffuse
X-ray emission across the Fermi Bubbles’ edges.pdf:pdf, issn = 15384357,
journal = Astrophys. J., keywords = Galaxy: center,Galaxy: halo,X-rays:
ISM,acceleration of particles,cosmic rays, number = 1, title = SUZAKU
observations of the diffuse X-ray emission across the Fermi Bubbles’ edges,
volume = 779, year = 2013 @articleBiernacki2017, abstract = We have recently
improved our model of active galactic nucleus (AGN) by attaching the
supermassive black hole (SMBH) to a massive nuclear star cluster (NSC). Here
we study the effects of this new model in massive, gas-rich galaxies with
several simulations of different feedback recipes with the hydrodynamics code
RAMSES. These simulations are compared to a reference simulation without any
feedback, in which the cooling halo gas is quickly consumed in a burst of star
formation. In the presence of strong supernovae (SN) feedback, we observe the
formation of a galactic fountain that regulates star formation over a longer
period, but without halting it. If only AGN feedback is considered, as soon as
the SMBH reaches a critical mass, strong outflows of hot gas are launched and
prevent the cooling halo gas from reaching the disk, thus efficiently halting
star formation, leading to the so-called ”quenching”. If both feedback
mechanisms act in tandem, we observe a non-linear coupling, in the sense that
the dense gas in the supernovae-powered galactic fountain is propelled by the
hot outflow powered by the AGN at much larger radii than without AGN. We argue
that these particular outflows are able to unbind dense gas from the galactic
halo, thanks to the combined effect of SN and AGN feedback. We speculate that
this mechanism occurs at the end of the fast growing phase of SMBH, and is at
the origin of the dense molecular outflows observed in many massive high-
redshift galaxies., archivePrefix = arXiv, arxivId = 1712.02794, author =
Biernacki, Pawel and Teyssier, Romain, doi = 10.1093/mnras/sty216, eprint =
1712.02794, file = :home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Biernacki, Teyssier - 2017 - The combined effect of AGN and
supernovae feedback in launching massive molecular outflows in high-
redshift.pdf:pdf, issn = 0035-8711, keywords =
active,evolution,galaxies,methods,numerical,quasars,supermas-, pages =
5688–5703, title = The combined effect of AGN and supernovae feedback in
launching massive molecular outflows in high-redshift galaxies, url =
http://arxiv.org/abs/1712.02794%0Ahttp://dx.doi.org/10.1093/mnras/sty216,
volume = 5703, year = 2017 @articleDawson1964, abstract = Calculations are
presented which show that a laser pulse delivering powers of the order of 1010
W to a liquid or solid particle with dimensions of the order of 10-2 cm will
produce a hot plasma with temperatures in the range of several hundred eV. To
a large extent the plasma temperature is held down by its rapid expansion and
cooling. This converts much of the energy supplied into ordered energy of
expansion. This ordered expansion energy can amount to several keV per ion. If
the expanding plasma can be caught in a magnetic field and its ordered motion
converted to random motion this might be utilized as a means for filling
controlled thermonuclear fusion devices with hot plasma. Further, it should
also be possible to do many interesting plasma experiments on such plasmas.,
author = Dawson, John M., doi = 10.1063/1.1711346, file =
:home/william/Documents/Papers/dawson1964.pdf:pdf, issn = 10706631, journal =
Phys. Fluids, number = 7, pages = 981–987, title = On the production of plasma
by giant pulse lasers, volume = 7, year = 1964 @articleChevalier1985, abstract
= Galaxies with highly active star formation regions (starburst galaxies) are
inferred to have high supernova rates in the region of activity. If most of
the supernova energy input is thermalized, a strong wind is driven out of the
active region. The authors present an analytical solution for the wind which
is driven from a region of uniform mass and energy deposition. The solution is
applied to M82 - the best observed case of a starburst galaxy., author =
Chevalier, R. A. and Clegg, A. W., doi = 10.1038/317044a0, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Chevalier, Clegg - 1985 - Wind from a starburst galaxy
nucleus.pdf:pdf, issn = 00280836, journal = Nature, number = 6032, pages =
44–45, title = Wind from a starburst galaxy nucleus, volume = 317, year = 1985
@articleJuranova2022, abstract = Spectral-timing techniques have proven
valuable in studying the interplay between the X-ray corona and the accretion
disc in variable active galactic nuclei (AGN). Under certain conditions,
photo-ionized outflows emerging from central AGN regions also play a role in
the observable spectral-timing properties of the nuclear components. The
variable ionizing flux causes the intervening gas to ionize or recombine,
resulting in a time-dependent absorption spectrum. Understanding the spectral-
timing properties of these outflows is critical for the determination of their
role in the AGN environment, but also the correct interpretation of timing
signatures of other AGN components. In this paper, we test the capabilities of
the Athena X-IFU instrument in studying the spectral and spectral-timing
properties of a black hole system displaying a variable outflow. We take the
narrow-line Seyfert 1 IRAS 13224-3809 as a test case. Our findings show that
while the non-linear response of the absorbing medium can result in complex
behaviour of time lags, the resulting decrease in the coherence can be used to
constrain gas density and distance to the central source. Ultimately,
modelling the coherence spectra of AGN outflows may constitute a valuable tool
in studying the physical properties of the outflowing gas., archivePrefix =
arXiv, arxivId = 2201.02640, author = Juráňová, A. and Costantini, E. and
Uttley, P., eprint = 2201.02640, file =
:home/william/Documents/Papers/2201.02640.pdf:pdf, keywords = absorption
lines,galaxies,individual,iras 13224-3809,methods,numerical,quasars,seyfert,
number = January, pages = 1–11, title = Spectral-timing of AGN ionized
outflows with Athena, url = http://arxiv.org/abs/2201.02640, volume = 11, year
= 2022 @articleLykins2013, abstract = We discuss recent improvements in the
calculation of the radiative cooling in both collisionally ionized and
photoionized plasmas. We are extending the spectral simulation code CLOUDY so
that as much as possible of the underlying atomic data are taken from external
data bases, some created by others and some developed by the CLOUDY team. This
paper focuses on recent changes in the treatment of many stages of ionization
of iron, and discusses its extensions to other elements. The H- and He-like
ions are treated in the isoelectronic approach described previously. Fe II is
a special case treated with a large model atom. Here we focus on Fe III
through Fe XXIV, ions which are important contributors to the radiative
cooling of hot (T ~ 105-107 K) plasmas and for X-ray spectroscopy. We use the
Chianti atomic data base to greatly expand the number of transitions in the
cooling function. Chianti only includes lines that have atomic data computed
by sophisticated methods. This limits the line list to lower excitation,
longer wavelength, transitions.We had previously included lines from the
Opacity Project data base, which tends to include higher energy, shorter
wavelength, transitions. These were combined with various forms of the ’g-bar’
approximation, a highly approximate method of estimating collision rates. For
several iron ions the two data bases are almost entirely complementary.We
adopt a hybrid approach in which we use Chianti where possible, supplemented
by lines from the Opacity Project for shorter wavelength transitions. The
total cooling including the lightest 30 elements differs from some previous
calculations by significant amounts. 2013 The Authors. Published by Oxford
University Press on behalf of the Royal Astronomical Society., author =
Lykins, M. L. and Ferland, G. J. and Porter, Ryan L. and van Hoof, Peter A.M.
and Williams, R. J.R. and Gnat, Orly, doi = 10.1093/mnras/sts570, file =
:home/william/Documents/Papers/sts570.pdf:pdf, issn = 00358711, journal = Mon.
Not. R. Astron. Soc., keywords = Atomic data-plasmas-methods,Numerical, number
= 4, pages = 3133–3143, title = Radiative cooling in collisionally ionized and
photoionized plasmas, volume = 429, year = 2013 @articleHerold2019, abstract =
The Fermi bubbles (FBs) are large gamma-ray emitting lobes extending up to
$55$ in latitude above and below the Galactic center (GC). Although the FBs
were discovered 8 years ago, their origin and the nature of the gamma-ray
emission are still unresolved. Understanding the properties of the FBs near
the Galactic plane may provide a clue to their origin. Previous analyses of
the gamma-ray emission at the base of the FBs, what remains after subtraction
of Galactic foregrounds, have shown an increased intensity compared to the FBs
at high latitudes, a hard power-law spectrum without evidence of a cutoff up
to approximately 1 TeV, and a displacement of the emission to negative
longitudes relative to the GC. We analyze 9 years of Fermi Large Area
Telescope data in order to study in more detail the gamma-ray emission at the
base of the FBs, especially at energies above 10 GeV. We confirm that the
gamma-ray emission at the base of the FBs is well described by a simple power
law up to 1 TeV energies. The 95% confidence lower limit on the cutoff energy
is about 500 GeV. It has larger intensity than the FBs emission at high
latitudes and is shifted to the west (negative longitudes) from the GC. If the
emission at the base of the FBs is indeed connected to the high-latitude FBs,
then the shift of the emission to negative longitudes disfavors models where
the FBs are created by the supermassive black hole at the GC. We find that the
gamma-ray spectrum can be explained either by gamma rays produced in hadronic
interactions or by leptonic inverse Compton scattering. In the hadronic
scenario, the emission at the base of the FBs can be explained either by
several hundred supernova remnants (SNRs) near the Galactic center or by about
10 SNRs at a distance of ~ 1 kpc. In the leptonic scenario, the necessary
number of SNRs is a factor of a few larger than in the hadronic scenario.
(abridged), archivePrefix = arXiv, arxivId = 1904.01454, author = Herold,
Laura and Malyshev, Dmitry, eprint = 1904.01454, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Herold, Malyshev - 2019 - Hard and bright gamma-ray
emission at the base of the Fermi bubbles.pdf:pdf, keywords =
center,galaxy,gamma rays,general,halo,ism,jets and outflows, title = Hard and
bright gamma-ray emission at the base of the Fermi bubbles, url =
http://arxiv.org/abs/1904.01454, year = 2019 @miscCaraveo2020, abstract =
High-energy photons are a powerful tool to understand the most violent
phenomena in our Universe. However, detecting gamma-ray photons is a daunting
task both owing to the overwhelming presence of cosmic rays and to the opacity
of our atmosphere. Thus, direct detection of gamma-ray photons must be done in
space, while instruments on the ground can see very high-energy photons
through the secondary particles they produce in the atmosphere. Mastering
space instruments as well as ground-based ones required decades of relentless
efforts implying hardware and software developments as well as theoretical
studies and extensive simulations. Space instruments, as well as ground-based
ones, are now producing a steady flow of important results often in
conjunction with observatories working at different wavelengths. Multi-
messenger astronomy, which combines the electromagnetic channel with
gravitational waves and neutrinos, is the newly born discipline to which high-
energy gamma-ray detectors provide an essential contribution. Building
instruments to continuously cover the gamma-ray sky is, thus, a priority for
the astronomical community which is looking forward for the Cherenkov
Telescope Array, a new generation ground based gamma-ray observatory designed
to monitor, to study and to unveil the mysteries hidden in the very high
energy sky., author = Caraveo, Patrizia A, booktitle = Riv. del Nuovo Cim.,
doi = 10.1007/s40766-020-00006-3, file =
:home/william/Documents/Papers/Caraveo2020_Article_TheGoldenAgeOfHigh-
energyGamma.pdf:pdf, issn = 18269850, keywords = Cherenkov telescopes,Gamma-
ray astronomy,Gamma-ray missions,Gamma-ray sources,Multi-messenger astronomy,
number = 6, pages = 281–318, publisher = Springer Berlin Heidelberg, title =
The golden age of high-energy gamma-ray astronomy: the Cherenkov Telescope
Array in the multimessenger era, url =
https://doi.org/10.1007/s40766-020-00006-3, volume = 43, year = 2020
@articleRees1984, author = Rees, Martin J, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley Desktop/Downloaded/Rees
- 1984 - Black hole models for active galactic nuclei.pdf:pdf, pages =
471–506, title = Black hole models for active galactic nuclei, year = 1984
@articlePrieto2017a, abstract = By using cosmological hydrodynamical
simulations we study the effect of supernova (SN) and active galactic nuclei
(AGN) feedback on the mass transport of gas on to galactic nuclei and the
black hole (BH) growth down to redshift z~6. We study the BH growth in
relation with the mass transport processes associated with gravity and
pressure torques, and how they are modified by feedback. Cosmological gas
funelled through cold flows reaches the galactic outer region close to free-
fall. Then torques associated to pressure triggered by gas turbulent motions
produced in the circum-galactic medium by shocks and explosions from SNe are
the main source of mass transport beyond the central ~ 100 pc. Due to high
concentrations of mass in the central galactic region, gravitational torques
tend to be more important at high redshift. The combined effect of almost
free-falling material and both gravity and pressure torques produces a mass
accretion rate of order ~ 1 M_sun/yr at ~ pc scales. In the absence of SN
feedback, AGN feedback alone does not affect significantly either star
formation or BH growth until the BH reaches a sufficiently high mass of $10^6$
M_sun to self-regulate. SN feedback alone, instead, decreases both stellar and
BH growth. Finally, SN and AGN feedback in tandem efficiently quench the BH
growth, while star formation remains at the levels set by SN feedback alone
due to the small final BH mass, ~ few 10^5 M_sun. SNe create a more rarefied
and hot environment where energy injection from the central AGN can accelerate
the gas further., archivePrefix = arXiv, arxivId = 1701.06172, author =
Prieto, Joaquin and Escala, Andres and Volonteri, Marta and Dubois, Yohan, doi
= 10.3847/1538-4357/aa5be5, eprint = 1701.06172, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Prieto et al. - 2017 - How AGN and SNe feedback affect mass
transport and black hole growth in high redshift galaxies.pdf:pdf, issn =
1538-4357, journal = Astrophys. J., keywords = formation,galaxies,galaxies:
formation,large-scale structure of the,large-scale structure of the
universe,quasars,quasars: supermassive black holes,stars,stars:
formation,supermassive black holes,turbulence,universe, number = 2, pages =
1–13, publisher = IOP Publishing, title = How AGN and SNe feedback affect mass
transport and black hole growth in high redshift galaxies, url =
http://arxiv.org/abs/1701.06172%0Ahttp://dx.doi.org/10.3847/1538-4357/aa5be5,
volume = 836, year = 2017 @articleMukherjee2018a, abstract = We study the
interactions of a relativistic jet with a dense turbulent gaseous disk of
radius $2$ kpc. We have performed a suite of simulations with different mean
density, jet power and orientation. Our results show that: A) the relativistic
jet couples strongly with the gas in the inner kpc, creating a cavity and
launching outflows. B) The high pressure bubble inflated by the jet and its
back-flow compresses the disk at the outer edges, driving inflows within the
disk. C) Jets inclined towards the disk couple more strongly with the disk and
launch sub-relativistic, wide-angle outflows along the minor axis. D) Shocks
driven directly by the jet and the jet-driven energy bubble raise the velocity
dispersion throughout the disk by several times its initial value. E)
Compression by the jet-driven shocks can enhance the star formation rate in
the disk, especially in a ring-like geometry close to the axis. However,
enhanced turbulent dispersion in the disk also leads to quenching of star
formation. Whether positive or negative feedback dominates depends on jet
power, ISM density, jet orientation with respect to the disc, and the time-
scale under consideration. Qualitatively, our simulations compare favourably
with kinematic and morphological signatures of several observed galaxies such
as NGC 1052, NGC 3079, 3C 326 and 3C 293., archivePrefix = arXiv, arxivId =
1803.08305, author = Mukherjee, Dipanjan and Bicknell, Geoffrey V. and Wagner,
Alexander Y. and Sutherland, Ralph S. and Silk, Joseph, doi =
10.1093/mnras/sty1776, eprint = 1803.08305, file =
:home/william/.local/share/data/Mendeley Ltd./Mendeley
Desktop/Downloaded/Mukherjee et al. - 2018 - Relativistic jet feedback - III.
Feedback on gas discs.pdf:pdf, issn = 0035-8711, journal = Mon. Not. R.
Astron. Soc., keywords = Galaxies: evolution,Galaxies: highredshift,Galaxies:
ism,Galaxies: jets,Hydrodynamics,Methods: numerical, month = oct, number = 4,
pages = 5544–5566, publisher = Oxford University Press, title = Relativistic
jet feedback – III. Feedback on gas discs, url =
https://academic.oup.com/mnras/article/479/4/5544/5049320, volume = 479, year
= 2018 @articleLIMAetal.1982, author = LIMA et al., doi =
10.1016/S0197-0186(13)00110-1, file =
:home/william/Documents/Papers/[Soltan]-Masses of Quasares.pdf:pdf, number =
1981, pages = p.173–203, title = No 主観的健康感を中心とした在宅高齢者における
健康関連指標に関する共分散構造分析Title, year = 1982 @articleBalestra2005, abstract = We
present a 23 ks XMM-Newton observation of the Ultraluminous Infrared Galaxy
(ULIRG) Mrk 273. The hard X-ray spectrum can be modeled by a highly absorbed
(∼7 × 1023 cm-2) power law plus an Fe Ka emission line. The iron line
(detected at more than 99% c.l.) is broad ($\sigma$ = 0.26-0.17+0.37 keV),
suggesting possible superposition of a neutral iron line at 6.4 keV, and a
blend of ionized iron lines from Fe XXV and Fe XXVI. Given the relatively
short exposure, the three line components cannot be individually resolved with
high statistical significance: the neutral component is detected
at∼2.5$\sigma$ and the Fe XXV line at ∼2$\sigma$ c.l., while for the Fe XXVI
line we can only estimate an upper limit. The broad band spectrum requires, in
addition to a highly absorbed power law, at least three collisionally ionized
plasma components, which may be associated with star-forming regions. The
temperatures of the three plasmas are about 0.3, 0.8 and 6 keV, where the
highest of the three is sufficient to produce ionized iron emission lines. An
alternative interpretation for the origin of the soft emission might also be
reflection off photoionized gas, as has been observed in a number of nearby
Compton-thick Seyfert 2 galaxies (e.g. NGC 1068, Circinus, Mrk 3, NGC 4945). A
hot gas, photoionized by the primary, continuum can also produce ionized iron
lines. Unfortunately, given the limited statistics and the lack of high
resolution spectroscopy, it is not possible to distinguish between the two
models investigated. We further compare the XMM-Newton findings with the
Chandra data obtaining consistent spectral results. The absorption-corrected
hard X-ray luminosity of Mrk 273 is L 2-10kev ∼ 7 × 1042 erg s-1,
corresponding to ∼0.2% of the far-IR luminosity, similar to typical values
found in pure starbursts. The thermal contribution to the soft X-ray
luminosity is approximately 0.2-0.7 × 1042 ergs-1, comparable to those found
in NGC 6240 and other starburst-dominated ULIRGs. We also analyze the XMM-
Newton spectrum of Mrk 273x, an unabsorbed Seyfert 2 galaxy at redshift z =
0.458, which lies in the field of view of Mrk 273. ESO 2005., archivePrefix =
arXiv, arxivId = astro-ph/0507321, author = Balestra, I. and Boller, Th and
Gallo, L. and Lutz, D. and Hess, S., doi = 10.1051/0004-6361:20053558, eprint
= 0507321, file = :home/william/Documents/Papers/aa3558-05.pdf:pdf, issn =
00046361, journal = Astron. Astrophys., keywords = Galaxies: Seyfert,Galaxies:
individual: Mrk 273,Galaxies: individual: Mrk 273x,X-rays: galaxies, number =
2, pages = 469–478, primaryClass = astro-ph, title = XMM-Newton spectral
properties of the ultraluminous IRAS galaxy Mrk 273, volume = 442, year = 2005
@articleLonsdale2006a, author = Lonsdale, C J and Farrah, D and Smith, H E,
file = :home/william/Documents/Papers/ultraluminous-infrared-galaxies.pdf:pdf,
journal = Astrophys. Updat., title = Chap.9 Ultraluminous Infrared Galaxies,
year = 2006 @articlePino2012, abstract = The formation of protostellar disks
out of molecular cloud cores is still not fully understood. Under ideal MHD
conditions, the removal of angular momentum from the disk progenitor by the
typically embedded magnetic field may prevent the formation of a rotationally
supported disk during the main protostellar accretion phase of low-mass stars.
This has been known as the magnetic braking problem and the most investigated
mechanism to alleviate this problem and help remove the excess of magnetic
flux during the star formation process, the so-called ambipolar diffusion
(AD), has been shown to be not sufficient to weaken the magnetic braking at
least at this stage of the disk formation. In this work, motivated by recent
progress in the understanding of magnetic reconnection in turbulent
environments, we appeal to the diffusion of magnetic field mediated by
magnetic reconnection as an alternative mechanism for removing magnetic flux.
We investigate numerically this mechanism during the later phases of the
protostellar disk formation and show its high efficiency. By means of fully
three-dimensional MHD simulations, we show that the diffusivity arising from
turbulent magnetic reconnection is able to transport magnetic flux to the
outskirts of the disk progenitor at timescales compatible with the collapse,
allowing the formation of a rotationally supported disk around the protostar
of dimensions 100AU, with a nearly Keplerian profile in the early accretion
phase. Since MHD turbulence is expected to be present in protostellar disks,
this is a natural mechanism for removing magnetic flux excess and allowing the
formation of these disks. This mechanism dismisses the necessity of
postulating a hypothetical increase of the ohmic resistivity as discussed in
the literature. Together with our earlier work which showed that magnetic flux
removal from molecular cloud cores is very efficient, this work calls for
reconsidering the relative role of AD in the processes of star and planet
formation. 2012. The American Astronomical Society. All rights reserved.,
author = Santos-Lima, R. and De Gouveia Dal Pino, E. M. and Lazarian, A, doi =
10.1088/0004-637X/747/1/21, file = :home/william/.local/share/data/Mendeley
Ltd./Mendeley Desktop/Downloaded/Pino, Lazarian - 2012 - THE ROLE OF TURBULENT
MAGNETIC RECONNECTION IN THE FORMATION OF.pdf:pdf, issn = 15384357, journal =
Astrophys. J., keywords = ISM: magnetic fields,accretion,accretion
disks,diffusion,magnetohydrodynamics (MHD),stars: formation,turbulence, number
= 1, title = The role of turbulent magnetic reconnection in the formation of
rotationally supported protostellar disks, volume = 747, year = 2012
@articleBrianYu2020a, abstract = Outflows from starburst galaxies can be
driven by thermal pressure, radiation, and cosmic rays. We present an analytic
phenomenological model that accounts for these contributions simultaneously to
investigate their effects on the hydrodynamical properties of outflows. We
assess the impact of energy injection, wind opacity, magnetic field strength,
and the mass of the host galaxy on flow velocity, temperature, density, and
pressure profiles. For an M82-like wind, a thermally dominated driving
mechanism is found to deliver the fastest and hottest wind. Radiation-driven
winds in typical starburst-galaxy configurations are unable to attain the