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Journal articles on the topic 'Dynamics of galaxies'

Author: Grafiati

Published: 4 June 2021

Last updated: 11 March 2023

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1

Bellovary, Jillian M., Sarra Hayoune, Katheryn Chafla, et al. "The origins of off-centre massive black holes in dwarf galaxies." Monthly Notices of the Royal Astronomical Society 505, no. 4 (2021): 5129–41. http://dx.doi.org/10.1093/mnras/stab1665.

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ABSTRACT Massive black holes often exist within dwarf galaxies, and both simulations and observations have shown that a substantial fraction of these may be off-centre with respect to their hosts. We trace the evolution of off-centre massive black holes (MBHs) in dwarf galaxies using cosmological hydrodynamical simulations, and show that the reason for off-centre locations is mainly due to galaxy–galaxy mergers. We calculate dynamical time-scales and show that off-centre MBHs are unlikely to sink to their galaxys’ centres within a Hubble time, due to the shape of the hosts’ potential wells and

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2

Bertin, G., and V. G. Surdin. "Dynamics of Galaxies." Astronomical & Astrophysical Transactions 20, no. 3 (2001): 603–5. http://dx.doi.org/10.1080/10556790108213605.

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3

Bekki, Kenji. "Star cluster dynamics in galaxies." Proceedings of the International Astronomical Union 5, S266 (2009): 219–30. http://dx.doi.org/10.1017/s1743921309991086.

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AbstractI present a review of star cluster (SC) dynamics in galaxies, with special emphasis on the effects of global galactic dynamics on SC formation and evolution. I particularly discuss (i) dynamical friction processes affecting SCs in galaxies of different masses, (ii) formation of stellar galactic nuclei and massive globular clusters (GCs) through multiple merging of SCs, (iii) interactions between giant molecular clouds (GMCs) and SCs, (iv) SC destruction due to the strong tidal fields in galaxy mergers and (v) the formation of low-mass dwarfs from numerous SCs. I also discuss some recen

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Sellwood, J. A., and A. Wilkinson. "Dynamics of barred galaxies." Reports on Progress in Physics 56, no. 2 (1993): 173–256. http://dx.doi.org/10.1088/0034-4885/56/2/001.

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5

Barnes, Joshua E., and Lars Hernquist. "Dynamics of Interacting Galaxies." Annual Review of Astronomy and Astrophysics 30, no. 1 (1992): 705–42. http://dx.doi.org/10.1146/annurev.aa.30.090192.003421.

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6

Merritt, D. "Dynamics of Elliptical Galaxies." Science 259, no. 5103 (1993): 1867–71. http://dx.doi.org/10.1126/science.259.5103.1867.

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7

Chen, Cheng-Yu, and Chorng-Yuan Hwang. "Dynamics of Companion Galaxies of Early-type Galaxies." Astrophysical Journal 903, no. 1 (2020): 38. http://dx.doi.org/10.3847/1538-4357/abb76c.

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8

Giri, Gourab, and Bhargav Vaidya. "Numerical modelling of X-shaped radio galaxies using back-flow model." Proceedings of the International Astronomical Union 16, S362 (2020): 70–75. http://dx.doi.org/10.1017/s1743921322001569.

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AbstractThe focus of this work is to comprehensively understand hydro-dynamical back-flows and their role in dynamics and non-thermal spectral signatures particularly during the initial phase of X-shaped radio galaxies. In this regard, we have performed axisymmetric (2D) and three dimensional (3D) simulations of relativistic magneto-hydrodynamic jet propagation from tri-axial galaxies. High-resolution dynamical modelling of axisymmetric jets has demonstrated the effect of magnetic field strengths on lobe and wing formation. Distinct X-shape formation due to back-flow and pressure gradient of a

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9

Lelli, Federico, Marc Verheijen, and Filippo Fraternali. "Dynamics of starbursting dwarf galaxies." Astronomy & Astrophysics 566 (June 2014): A71. http://dx.doi.org/10.1051/0004-6361/201322657.

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10

Zaritsky, Dennis. "The Dynamics of Satellite Galaxies." Publications of the Astronomical Society of the Pacific 104 (February 1992): 155. http://dx.doi.org/10.1086/132972.

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11

Combes, F. "Comparison with External Galaxies Dynamics." Symposium - International Astronomical Union 169 (1996): 133–43. http://dx.doi.org/10.1017/s0074180900229616.

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Many features of the Milky Way appear weird or unique, because of the peculiar point of view. However the same features are observed more easily and clearly in nearby galaxies. The Milky Way appears to cumulate many dynamical features, such as a bar, a nuclear disk, a perpendicular nuclear bar (?), lopsidedness, an inner ring (molecular ring at 5kpc), a peanut-shape bulge, a warp, and a polar ring. By comparison with external galaxies, and also results from N-body simulations, we can infer the most probable bar angular velocity and length, and interpret the ring features.

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12

Nityananda, Rajaram. "The gravitational dynamics of galaxies." Pramana 73, no. 1 (2009): 193–214. http://dx.doi.org/10.1007/s12043-009-0097-5.

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13

Binney, James. "Symposium summary: dynamics." Proceedings of the International Astronomical Union 3, S245 (2007): 455–58. http://dx.doi.org/10.1017/s1743921308018358.

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AbstractPseudobulges form from unstable disks, while classical bulges form in violent episodes of star formation when a merger sweeps cold gas to a galactic centre. It seems unlikely that smashed disks contribute much to classical bulges. During mergers central black holes make cusps shallower and inflate kinematically decoupled cores. The abundance of galaxies with no detected classical bulge can perhaps be understood if galaxies exchange gas with the IGM more freely than is often supposed.

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14

Bird, Christina M., John M. Dickey, and E. E. Salpeter. "DARK MATTER AND DYNAMICS IN HERCULES CLUSTER." International Journal of Modern Physics D 03, supp01 (1994): 93–100. http://dx.doi.org/10.1142/s021827189400099x.

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We present new 21-cm observations of faint (15.7<mpg<16.5) spiral galaxies in the Abell cluster 2151. These results, when combined with the large body of velocities available in the literature for Hercules, permit us to study the dynamics throughout the cluster core, out to a projected radius of 1.8h−1 Mpc. We calculate the global dynamical mass of Hercules using 3 different but related methods: two versions of the virial theorem and the projected mass estimator. These masses lie in the range 3–6×1014 M⊙. We investigate the importance of subclustering in A2151 using the statistical test

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15

Noguchi, M. "Dynamics and Interactions of High-Redshift Galaxies." Symposium - International Astronomical Union 186 (1999): 431–38. http://dx.doi.org/10.1017/s0074180900113373.

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A large number of high redshift galaxies observed with the Hubble Space Telescope (HST) show anomalous morphology and photometric properties, which may be an indication of evolutionary process in young galaxies. We show here by means of numerical simulations that the copious interstellar gas existing in the disks of rapidly collapsing protogalaxies can bring about these peculiarities. Gravitational instability in a gas-rich disk leads to the formation of massive gas clumps with a typical mass of 109M⊙. These subgalactic clumps make disk galaxy evolution a dynamically energetic and chaotic proc

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16

VAN DE WEYGAERT, RIEN, and ERWIN PLATEN. "COSMIC VOIDS: STRUCTURE, DYNAMICS AND GALAXIES." International Journal of Modern Physics: Conference Series 01 (January 2011): 41–66. http://dx.doi.org/10.1142/s2010194511000092.

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In this contribution we review and discuss several aspects of Cosmic Voids. Voids are a major component of the large scale distribution of matter and galaxies in the Universe. Their instrumental importance for understanding the emergence of the Cosmic Web is clear. Their relatively simple shape and structure makes them into useful tools for extracting the value of a variety cosmic parameters, possibly including even that of the influence of dark energy. Perhaps most promising and challenging is the issue of the galaxies found within their realm. Not only does the pristine environment of voids

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17

Konar, C., M. Jamrozy, M. J. Hardcastle, et al. "The Dynamics of Radio Galaxies and Double–Double Radio Galaxies." Journal of Astrophysics and Astronomy 32, no. 4 (2011): 477–86. http://dx.doi.org/10.1007/s12036-011-9126-0.

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18

Combes, F. "Small Group Dynamics and Extended Gas." International Astronomical Union Colloquium 174 (2000): 148–53. http://dx.doi.org/10.1017/s0252921100054907.

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AbstractInteractions between galaxies have spectacular effects on gas dynamics, and small galaxy groups are a privileged place to investigate them. In particular, they could test the existence of cold H2 gas as dark matter in the outer parts of galaxies. HI observations have revealed that galaxies in small groups are deficient in atomic gas, like in richer galaxy clusters such as Virgo, although in a lesser extent. Galaxy interactions could be the cause of this deficiency, stripping the gas out of galaxies and enriching the inter-cluster medium (ICM) in hot gas, which in turn strips gas throug

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19

Freeman, K. C. "Internal Dynamics of Local Group Galaxies." Symposium - International Astronomical Union 192 (1999): 383–94. http://dx.doi.org/10.1017/s0074180900204403.

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This talk reviews the internal dynamics of some of the different classes of Local Group galaxies. These include the dwarf spheroidal galaxies, the pure disk galaxy M33, the LMC and M31. The talk concludes with some general remarks about bulges and halos.

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20

Smith, Eric P., and Paul Hintzen. "Multi-Color Imaging of Selected Southern Interacting Galaxies." International Astronomical Union Colloquium 124 (1990): 55–58. http://dx.doi.org/10.1017/s0252921100004887.

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We present preliminary results from a study of selected Arp-Madore Southern Hemisphere peculiar galaxies. Broadband CCD images (BVRI) of a subset of these galaxies allow us to study each galaxy’s optical morphology, color, and (in a crude manner) degree of nuclear activity, and to compare them with similar data we possess on other active galaxies. Many of these galaxies have optical morphologies closely resembling those of powerful radio galaxies (Smith and Heckman 1989), yet their radio emission is unremarkable. Accurate positions for subsequent spectroscopic studies have been determined alon

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21

Patsis, P. A., and P. Grosbøl. "Dynamics of Thick Spirals." Symposium - International Astronomical Union 169 (1996): 507–8. http://dx.doi.org/10.1017/s0074180900230180.

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Most studies of spiral structure in galaxies use 2D models, since the motion of the stars is supposed to be confined very close to the plane of symmetry. However, galactic disks have a finite thickness and the vertical variation of spiral perturbations should be considered. The effect of 3D orbits in the dynamics of normal spiral galaxies is examined in this paper. We present the basic orbital behavior of the families of periodic orbits, which support a thick spiral pattern.

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22

J. Romanowsky, Aaron. "Dynamics of Globular Cluster Systems in Elliptical Galaxies." Symposium - International Astronomical Union 207 (2002): 336–38. http://dx.doi.org/10.1017/s0074180900224005.

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One of the most promising avenues for exploring the dynamics of the outer parts of elliptical galaxies involves using bright discrete objects as kinematical tracers: globular clusters and planetary nebulae. As large data sets are becoming available, rigorous dynamical analyses are needed to interpret them. To this end, we have developed an extension of orbit modeling methods, which we apply to the dynamics of the giant ellipticals M87 and M49. We find that a sample of ∼ 200 globular clusters velocities is effective at demonstrating the presence of a dark halo and providing hints about the deta

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23

Nipoti, C., P. Londrillo, H. S. Zhao, and L. Ciotti. "Vertical dynamics of disc galaxies in modified Newtonian dynamics." Monthly Notices of the Royal Astronomical Society 379, no. 2 (2007): 597–604. http://dx.doi.org/10.1111/j.1365-2966.2007.11835.x.

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24

Karachentsev, I. D. "Dynamics of galaxy structures in the Local Volume." Proceedings of the International Astronomical Union 11, S308 (2014): 173–80. http://dx.doi.org/10.1017/s1743921316009807.

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AbstractI consider a sample of ‘Updated Nearby Galaxy Catalog’ that contains eight hundred objects within 11 Mpc. Environment of each galaxy is characterized by a tidal index Θ1 depending on separation and mass of the galaxy Main Disturber (=MD). The UNGC galaxies with a common MD are ascribed to its ‘suite’ and ranked according to their Θ1. Fifteen the most populated suites contain more than half of the UNGC sample. The fraction of MDs among the brightest galaxies is almost 100% and drops to 50% at M_B = -18 mag. The observational properties of galaxies accumulated in UNGC are used to derive

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25

Kroupa, Pavel. "Galaxies as simple dynamical systems: observational data disfavor dark matter and stochastic star formation." Canadian Journal of Physics 93, no. 2 (2015): 169–202. http://dx.doi.org/10.1139/cjp-2014-0179.

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According to modern theory, galactic evolution is driven by the dynamics of dark matter and stochastic star formation, but galaxies are observed to be simple systems. The existence of dark matter particles is a key hypothesis in present-day cosmology and galactic dynamics. Given the large body of high-quality work within the standard model of cosmology (SMoC), the validity of this hypothesis is challenged significantly by two independent arguments: (i) The dual dwarf galaxy theorem must be true in any realistic cosmological model. But the data now available appear to falsify this postulate whe

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26

Östlin, G., R. J. Cumming, P. Amram, et al. "Stellar dynamics of blue compact galaxies." Astronomy & Astrophysics 419, no. 3 (2004): L43—L47. http://dx.doi.org/10.1051/0004-6361:20040139.

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27

Rix, H. W. R., and S. D. M. White. "The dynamics of dumb-bell galaxies." Monthly Notices of the Royal Astronomical Society 240, no. 4 (1989): 941–56. http://dx.doi.org/10.1093/mnras/240.4.941.

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28

Sánchez Almeida, J., C. Muñoz-Tuñón, D. M. Elmegreen, B. G. Elmegreen, and J. Méndez-Abreu. "LOCAL TADPOLE GALAXIES: DYNAMICS AND METALLICITY." Astrophysical Journal 767, no. 1 (2013): 74. http://dx.doi.org/10.1088/0004-637x/767/1/74.

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29

Bertin, G., and M. Stiavelli. "Structure and dynamics of elliptical galaxies." Reports on Progress in Physics 56, no. 4 (1993): 493–556. http://dx.doi.org/10.1088/0034-4885/56/4/001.

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30

de Zeeuw, Tim, and Marijn Franx. "Structure and Dynamics of Elliptical Galaxies." Annual Review of Astronomy and Astrophysics 29, no. 1 (1991): 239–74. http://dx.doi.org/10.1146/annurev.aa.29.090191.001323.

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31

Dobbs, Clare. "Gas dynamics in whole galaxies: SPH." Proceedings of the International Astronomical Union 6, S270 (2010): 459–66. http://dx.doi.org/10.1017/s1743921311000810.

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AbstractI review the progress of SPH calculations for modelling galaxies, and resolving gas dynamics on GMC scales. SPH calculations first investigated the response of isothermal gas to a spiral potential, in the absence of self gravity and magnetic fields. Surprisingly though, even these simple calculations displayed substructure along the spiral arms. Numerical tests indicate that this substructure is still present at high resolution (100 million particles, ~10 pc), and is independent of the initial particle distribution. One interpretation of the formation of substructure is that smaller cl

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32

Sansom, A., J. V. Wall, and W. B. Sparks. "Stellar Dynamics of Radio Elliptical Galaxies." Symposium - International Astronomical Union 127 (1987): 429–30. http://dx.doi.org/10.1017/s0074180900185584.

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Stellar kinematical and dynamical results are presented for 34 radio ellipticals. The radio galaxies we observed were brighter than m(B)=16. The results show that these radio ellipticals are not generally more rapidly rotating than their non-radio counterparts. Evidence for some rotation about the major axis is seen in two cases. These radio ellipticals do not appear to obey the luminosity, velocity dispersion trend seen for normal ellipticals.

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33

El-Zant, A. A., and B. Haßler. "Dynamics of galaxies with triaxial haloes." New Astronomy 3, no. 7 (1998): 493–537. http://dx.doi.org/10.1016/s1384-1076(98)00025-6.

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34

Sakamoto, Kazushi. "Gas dynamics and structure of galaxies." Astrophysics and Space Science 313, no. 1-3 (2007): 245–51. http://dx.doi.org/10.1007/s10509-007-9624-3.

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35

Freeman, K. C. "Dynamics of disk galaxies (invited review)." Astrophysics and Space Science 118, no. 1-2 (1986): 337–42. http://dx.doi.org/10.1007/bf00651147.

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36

Smith, Eric P., T. M. Heckman, and G. D. Illingworth. "Stellar dynamics of powerful radio galaxies." Astrophysical Journal 356 (June 1990): 399. http://dx.doi.org/10.1086/168848.

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37

Cumming, R. J., K. Fathi, G. Östlin, et al. "Stellar dynamics of blue compact galaxies." Astronomy & Astrophysics 479, no. 3 (2008): 725–33. http://dx.doi.org/10.1051/0004-6361:20078916.

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38

Teague, P. F., and D. Carter. "Modelling Clusters of Galaxies." Publications of the Astronomical Society of Australia 6, no. 2 (1985): 198–202. http://dx.doi.org/10.1017/s1323358000018087.

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AbstractThorough investigation of clusters of galaxies involves the complete modelling of their dynamics and structure. Presented here is a description of such a substantial project utilizing a sample of several rich southern clusters of galaxies. Incorporating results from radial velocity analyses of cluster galaxies and X-ray images of the clusters into rigorously constructed models of the cluster potential well and atmosphere will enable the dynamics, structure and evolution of clusters to be tied down.

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39

GURZADYAN, V. G., S. RAUZY, and R. TRIAY. "RECOVERING THE INTERNAL DYNAMICS AND THE SHAPES OF GALAXY CLUSTERS: VIRGO CLUSTER." International Journal of Modern Physics D 11, no. 04 (2002): 581–97. http://dx.doi.org/10.1142/s0218271802001640.

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We describe a method for recovering of the substructure, internal dynamics and geometrical shapes of clusters of galaxies. Applying the method to the Virgo cluster, we first, reveal the substructure of the central 4 arc degree field of the Virgo cluster by means of S-tree technique. The existence of three main subgroups of galaxies is revealed and their dynamical characteristics are estimated. Then, using the previously suggested technique (Ref. 1), the bulk flow velocities of the subgroups are evaluated based on the distribution of the redshifts of the galaxies. The results enable us also to

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40

Quintana, H. "Dynamics of Groups around Interacting Double Ellipticals: Measuring Dark Matter Haloes." International Astronomical Union Colloquium 124 (1990): 37–41. http://dx.doi.org/10.1017/s025292110000484x.

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Binary galaxies, as binary stars, are important to measure masses, as suggested by Page (1952). Because three orbit parameters are measurable for galaxies at one instant of time, severe uncertainties remain in the orbit and mass determinations. These uncertainties can partly be overcome by statistical studies of selected samples and/or n-body simulations. Close double galaxies (and isolated galaxies) could also be useful to estimate dynamical masses if we can find test particles around them.Interacting elliptical pairs or dumb-bell galaxies are found with a large range, between 0-1200 km s-1,

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41

Treu, Tommaso, Léon V. E. Koopmans, David J. Sand, Graham P. Smith, and Richard S. Ellis. "The dark matter halos of spheroidal galaxies and clusters of galaxies." Symposium - International Astronomical Union 220 (2004): 159–64. http://dx.doi.org/10.1017/s0074180900183093.

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We describe the first results from two observational projects aimed at measuring the amount and spatial distribution of dark matter in distant early-type galaxies (E/S0s) and clusters of galaxies. At the galaxy scale, the Lenses Structure and Dynamics (LSD) Survey is gathering kinematic data for distant (up to z ⋐ 1) E/S0s that are gravitational lenses. A joint lensing and dynamical analysis constrains the fraction of dark matter within the Einstein radius, the mass-to-light ratio of the stellar component, and the total slope of the mass density profile. These properties and their evolution wi

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42

Malumuth, Eliot M., Gerard A. Kriss, W. Van Dyke Dixon, Henry C. Ferguson, and Christine Ritchie. "Dynamics of clusters of galaxies with central dominant galaxies. I - Galaxy redshifts." Astronomical Journal 104 (August 1992): 495. http://dx.doi.org/10.1086/116250.

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43

Schweizer, Francois. "Overview: Low-zObservations:Of Interacting and Merging Galaxies." Symposium - International Astronomical Union 186 (1999): 1–10. http://dx.doi.org/10.1017/s0074180900112136.

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Gravitational interactions and mergers affect the morphologies and dynamics of galaxies from our Local Group to the limits of the observable universe. Observations of interacting galaxies at low redshifts (z≲ 0.2) yield detailed information about many of the processes at work. I briefly review these processes and the growing evidence that mergers play a major role in the delayed formation of elliptical and early-type disk galaxies both in the field and in clusters. Low-zobservations clearly contradict the notion of a single epoch of E formation atz≳ 2; instead, E and S0 galaxies continue formi

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Genzel, Reinhard. "Spatially resolved dynamics of high-z star forming galaxies." Proceedings of the International Astronomical Union 4, S254 (2008): 33–34. http://dx.doi.org/10.1017/s174392130802735x.

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AbstractI report on two major programs to study the kinematic properties of galaxies at z ~ 1.5 − 3 with spatially resolved spectroscopy for the first time. Using the adaptive optics assisted, integral field spectrometer SINFONI on the ESO VLT, we have observed more than 70 galaxies and find compelling evidence for large, geometrically thick (turbulent), rotating disk galaxies in a majority of the objects that we can spatially resolve. It appears that these star forming disks are driven by continuous, rapid accretion of gas from their dark matter halos, and that their evolution is strongly inf

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de Oliveira, C. Mendes, and P. Amram. "Dynamics of Galaxies in Compact Groups I." International Astronomical Union Colloquium 174 (2000): 60–69. http://dx.doi.org/10.1017/s0252921100054762.

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AbstractWe describe a long-term program based on Fabry-Perot Hα velocity field data of compact groups taken at the ESO and the CFH 3.6m telescopes. The main goals of our project are: 1) determine the evolutionary stages of the studied groups, 2) search for tidal dwarf galaxy candidates in interacting systems and 3) in combination with photometry available in the literature, determine the Tully-Fisher relation for the group galaxies. In this paper we summarize all the Hα Fabry-Perot data we have obtained to date and present a preliminary discussion of point 1).The sample of 18 systems (with 64

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46

Sanders, R. H. "Modified Newtonian Dynamics: A Falsification of Cold Dark Matter." Advances in Astronomy 2009 (2009): 1–9. http://dx.doi.org/10.1155/2009/752439.

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The only viable alternative to dark matter is one in which Newtonian dynamics or gravity breaks down in the limit of low accelerations, as in modified Newtonian dynamics (MONDs). This hypothesis, suggested by Milgrom, has been successful in explaining systematic properties of spiral and elliptical galaxies and predicting in detail the observed rotation curves of spiral galaxies with only one additional parameter—a critical acceleration which is on the order of the cosmologically interesting value of . MOND may be viewed as an algorithm for calculating the distribution of force in an astronomic

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47

Volonteri, Marta, Tamara Bogdanović, Massimo Dotti, and Monica Colpi. "Massive Black Holes in Merging Galaxies." Proceedings of the International Astronomical Union 11, A29B (2015): 285–91. http://dx.doi.org/10.1017/s1743921316005366.

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AbstractThe dynamics of massive black holes (BHs) in galaxy mergers is a rich field of research that has seen much progress in recent years. In this contribution we briefly review the processes describing the journey of BHs during mergers, from the cosmic context all the way to when BHs coalesce. If two galaxies each hosting a central BH merge, the BHs would be dragged towards the center of the newly formed galaxy. If/when the holes get sufficiently close, they coalesce via the emission of gravitational waves. How often two BHs are involved in galaxy mergers depends crucially on how many galax

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48

van der Marel, Roeland P. "Recent Progress in the Search for Black Holes in Galactic Nuclei." Symposium - International Astronomical Union 171 (1996): 117–20. http://dx.doi.org/10.1017/s0074180900232233.

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Massive nuclear black holes (BHs) of 106–109M⊙ are believed to be responsible for the the energy production in quasars and active galaxies, and are thought to be present in many quiescent galaxies as well. Dynamical evidence for this can be sought by studying the dynamics of gas and stars in galactic nuclei at high spatial resolution. This paper reviews the current evidence, with emphasis on some recent developments and ongoing projects. The evidence from water masers and gas kinematics in the active galaxies NGC 4258 and M87 is compelling. In quiescent galaxies only stellar kinematics are gen

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49

Sanders, R. H. "Missing Mass as Evidence for Modified Newtonian Dynamics at Low Accelerations." Modern Physics Letters A 18, no. 27 (2003): 1861–75. http://dx.doi.org/10.1142/s0217732303011770.

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Milgrom has proposed that the appearance of discrepancies between the Newtonian dynamical mass and the directly observable mass in astronomical systems could be due to a breakdown of Newtonian dynamics in the limit of low accelerations rather than the presence of unseen matter. Milgrom's hypothesis, modified Newtonian dynamics or MOND, has been remarkably successful in explaining systematic properties of spiral and elliptical galaxies and predicting in detail the observed rotation curves of spiral galaxies with only one additional parameter — a critical acceleration which is on the order of th

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Combes, Françoise. "Molecular gas dynamics around nuclei of galaxies." EPJ Web of Conferences 265 (2022): 00047. http://dx.doi.org/10.1051/epjconf/202226500047.

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Recent molecular line observations with ALMA in several nearby Seyferts have revealed the existence of molecular tori, and the nature of gas flows at 10-20 pc scale. At 100 pc scale, or kpc-scale, previous NOEMA work on gravitational torques had shown that only about one third of Seyfert galaxies experienced molecular inflow and central fueling, while in most cases the gas was stalled in rings. At higher resolution, i.e. 10-20 pc scale, it is possible now to see in some cases AGN fueling due to nuclear trailing spirals, influenced by the black hole potential. This brings smoking gun evidence f

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