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Understanding the kinematics of Galactic Centre gas
Open accessAbstract
A coherent picture is constructed of the Galaxy’s H I, CO and CS emissions in the region |$|l|\le10^\circ,\enspace |b|\le0.5^\circ$|. The flow of gas at the Galactic Centre is dominated by a bar that has corotation at r= 2.4 ± 0.5 kpc, which we view at an angle of |$\theta_\text {incl}=16\pm2^\circ$| from its major axis. The first CO emission arises where gas is obliged to switch from x1 orbits to x2 orbits in the notation of Contopoulos. This gives rise to a shock and a clear signature in the (l, v) diagram. The great Galactic Centre molecular clouds such as Sgr B are on x2 orbits. From the structure of the H I terminal velocity envelope we deduce that the central mass density scales as |$\rho \propto r^{-1.75}$| out to at least ∼ 1.2 kpc along the bar’s major axis. Consequently the circular velocity curve is rising significantly through the radius range where naive analysis of the tangent velocity leads to a falling rotation curve. The great ring of molecular material at |$r \simeq 3.5$| kpc is probably associated with the bar’s outer Lindblad resonance, and the region of low gas densities inwards from there with corotation.
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“While an intersecting set of orbits can remain stable in a collisionless system, the gas undergoes a shock at the intersection and loses angular momentum. The gas then flows towards the center and finally settles into a ring-like structure closely following the x 2 orbits and thus forming the CMZ-like rings in galaxies (Binney et al. 1991; Athanassoula 1992; Sormani et al. 2015).”
From The Fermi/eROSITA bubbles: a look into the nuclear outflow from the Milky Way (2024) · cites this paper as Binney et al. 1991
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- Athanassola, E., 1988. In: Proceedings of the Joint VarennaAbastumani International School & Workshop on Plasma Physics, ESA SP-285, vol. I, p. 341, eds Guyenne, T. D. & Hunt, J. J., ESA, Paris.
- Blitz, L. & Spergel, D. N., 1991b. Preprint.
- Matsumoto, T., Hayakawa, S., Koizumi, H., Murakami, H., Uyama, K., Yamagami, T. & Thomas, J. A., 1982. In: The Galactic Center, AIP Conf. No. 83, p. 48, eds Riegler, G. R. & Blandford, R. D., American Institute of Physics, New York.
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Items 301–400 of 621
Stochastic non-circular motion and outflows driven by magnetic activity in the Galactic bulge region
Suzuki, T. K., Fukui, Y., Torii, K., Machida, M., & Matsumoto, R. (2015) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stv2188 · Cited by 25
“In order to interpret the parallelogram in the CMZ, the elliptical orbit in the bar stellar potential has been used as the only viable model (Binney et al. 1991).”
BackgroundMethodBlitz, L. (1997) · Springer eBooks · doi:10.1007/978-94-011-5414-7_2 · Cited by 24
Fraser-McKelvie, A., Merrifield, M. R., & Aragón‐Salamanca, A. (2019) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stz2493 · Cited by 26
“Amelia.Fraser-McKelvie@nottingham.ac.uk with the advent of large-scale photometric and spectroscopic surveys of the Galactic centre employing near-infrared (IR) photometry (Hammersley et al. 1994; Weiland et al. 1994), and gas kinematics (Binney et al. 1991).”
BackgroundSubmillimeter imaging of the Galactic Center starburst Sgr B2
Santa-Maria, M. G., Goicoechea, J. R., Etxaluze, M., Cernicharo, J., & Cuadrado, S. (2021) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202040221 · Cited by 24
Kumar, A., Ghosh, S., Kataria, S. K., et al. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac2302 · Cited by 23
Multiplicity of nuclear dust lanes and dust lane shocks in the Milky Way bar
Liszt, H. S. (2008) · Astronomy and Astrophysics · doi:10.1051/0004-6361:200809748 · Cited by 23
“…understanding of the observations has improved as models of the bar gas flow have matured, from simple recognition of the x2x1 orbit separation in fast bars (Binney et al., 1991) to holistic views of the hydrodynamic gas flow over an entire bar (Fux, 1999; Regan et al., 1999; Regan & Teuben, 2003).”
BackgroundDense Molecular Clouds in the Galactic Center Region
Tsuboi, M., Handa, T., & Ukita, N. (1994) · Springer eBooks · doi:10.1007/978-94-011-0752-5_11 · Cited by 23
Looking for a needle in a haystack: Measuring the length of a stellar bar
Ghosh, S., & Matteo, P. D. (2024) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202347763 · Cited by 22
3-dimensional kinematics in low foreground extinction windows of the Galactic bulge
Soto, M., Kuijken, K. H., & Rich, R. M. (2012) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201116522 · Cited by 21
Sormani, M. C., & Magorrian, J. (2014) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stu2316 · Cited by 21
“These were followed by ballistic models, in which the gas streamlines were approximated by closed orbits in an assumed underlying potential (Gerhard & Vietri 1986; Binney et al. 1991).”
BackgroundMethodEnokiya, R., Torii, K., Schultheis, M., Asahina, Y., Matsumoto, R., Furuhashi, E., Nakamura, K., Dobashi, K., Yoshiike, S., Sato, J., et al. (2013) · The Astrophysical Journal · doi:10.1088/0004-637x/780/1/72 · Cited by 22
“◦4) is mostly from the CMZ.”
MethodInfluentialHoughton, R. C. W., & Thatte, N. (2008) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2008.12893.x · Cited by 21
Hydrodynamic Simulations of the Central Molecular Zone with a Realistic Galactic Potential
Shin, J., Kim, S. S., Baba, J., Saitoh, T. R., Hwang, J.-S., Chun, K., & Hozumi, S. (2017) · The Astrophysical Journal · doi:10.3847/1538-4357/aa7061 · Cited by 20
“They confirmed that the transition of gas motion from X1 to X2 orbits indeed takes place in a bar potential, 2 which was originally suggested by Binney et al. (1991).”
BackgroundISOTOPIC RATIOS OF 18 O/ 17 O IN THE GALACTIC CENTRAL REGION
Zhang, J. S., Sun, L. L., Riquelme, D., et al. (2015) · The Astrophysical Journal Supplement Series · doi:10.1088/0067-0049/219/2/28 · Cited by 20
Interferometric12CO Observations of the Central Disk of NGC 4631: An Energetic Molecular Outflow
Rand, R. J. (2000) · The Astrophysical Journal · doi:10.1086/308869 · Cited by 20
“Furthermore, there is no indication of gas on x 2 orbits perpendicular to the bar, deep in the potential (cf. Figure 1 of Binney et al. 1991).”
BackgroundCOSMOGRAIL: the COSmological MOnitoring of GRAvItational Lenses
Saha, P., Courbin, F., Sluse, D., Dye, S., & Meylan, G. (2006) · Astronomy and Astrophysics · doi:10.1051/0004-6361:20052929 · Cited by 20
“That implies a 3D profile steeper than r−1.5, which is consistent with available estimates from stellar or gas dynamics; for example, Binney et al. (1991) report an r−1.75 profile near the Galactic centre.”
MethodInfluentialMira variables in the Galactic bulge with OGLE-II dataPreprint
Matsunaga, N., Fukushi, H., & Nakada, Y. (2005) · Cited by 20
Riquelme, D., Amo-Baladrón, M. A., Martín-Pintado, J., Mauersberger, R., Martín, S., & Bronfman, L. (2012) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201118288 · Cited by 19
“…can be produced by several phenomena: supernova or hypernova explosions (Tanaka et al. 2007); response of the gas in a barred potential model (Binney et al. 1991); and when the gas in the GMLs flows down their sides along the magnetic field lines, and joins with the gas layer of the Galactic…”
BackgroundInfluentialThe dark matter halo shape of edge-on disk galaxies
O'Brien, J. C., Freeman, K. C., & van der Kruit, P. C. (2010) · Astronomy and Astrophysics · doi:10.1051/0004-6361/200912566 · Cited by 19
GALACTIC WIND IN THE NEARBY STARBURST GALAXY NGC 253 OBSERVED WITH THE KYOTO3DII FABRY-PEROT MODE
Matsubayashi, K., Sugai, H., Hattori, T., et al. (2009) · The Astrophysical Journal · doi:10.1088/0004-637x/701/2/1636 · Cited by 19
“We find that the position of filament C coincides with that of a strong CO emission elongated along the x2 orbit (Binney et al. 1991; Athanassoula 1992), which is made by and is oriented perpendicular to the bar (Peng et al. 1996; Paglione et al. 2004).”
BackgroundTidally Induced Bars in Gas-rich Dwarf Galaxies Orbiting the Milky Way
Gajda, G., Łokas, E. L., & Athanassoula, E. (2018) · The Astrophysical Journal · doi:10.3847/1538-4357/aaea61 · Cited by 19
“In the view of Binney et al. (1991) and Athanassoula (1992b) the creation of shocks is strongly linked to the properties of the underlying periodic orbits.”
BackgroundResultGreve, A., Wills, K. A., Neininger, N., et al. (2002) · Astronomy and Astrophysics · doi:10.1051/0004-6361:20011723 · Cited by 19
“…motion of gas from the far ends of the bar towards the center, shocks at the intersection of the x1 and x2-orbits, accumulation of gas near and inside the x2-orbits, and the formation of dust lanes along the leading x1-orbits (Contopoulos & Mertzanides 1977; Binney et al. 1991; Athanassoula 1992).”
BackgroundStellar populations in the transition region of nuclear star cluster and nuclear stellar disc
Feldmeier-Krause, A. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac1227 · Cited by 18
ABSORPTION FILAMENTS TOWARD THE MASSIVE CLUMP G0.253+0.016
Bally, J., Rathborne, J. M., Longmore, S. N., Jackson, J. M., Alves, J., Bressert, E., Contreras, Y., Foster, J. B., Garay, G., Ginsburg, A. G., et al. (2014) · The Astrophysical Journal · doi:10.1088/0004-637x/795/1/28 · Cited by 18
“The major axis of the bar is oriented between 20 and 45 degrees with respect to our line of sight (Binney et al. 1991; RodriguezFernandez & Combes 2008).”
BackgroundSelf-citationThe 200-pc molecular cylinder in the Galactic Centre
Sofue, Y. (2017) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stx1389 · Cited by 17
“The noncircular motions observed in the GC have been modeled by streaming flows in a bar, and the LV behavior was named parallelogram after the shape of the lowest contours (Binney et al. 1991, 1997).”
MethodHIGH ATOMIC CARBON ABUNDANCE IN MOLECULAR CLOUDS IN THE GALACTIC CENTER REGIONPreprint
Tanaka, K., Oka, T., Matsumura, S., Nagai, M., & Kamegai, K. (2011) · Cited by 18
Theoretical Models of the Galactic Bulge
Shen, J., & Li, Z. (2015) · Astrophysics and space science library · doi:10.1007/978-3-319-19378-6_10 · Cited by 22
“The presence of a triaxial structure in the inner Galaxy was first hinted from gas kinematics (de Vaucouleurs, 1964; Binney et al., 1991; Burton & Liszt, 1993).”
BackgroundRobust inference of the Galactic Centre gamma-ray excess spatial properties
Song, D., Eckner, C., Gordon, C., Calore, F., Macías, O., Abazajian, K. N., Horiuchi, S., Kaplinghat, M., & Pohl, M. (2024) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stae923 · Cited by 29
Chemical evolution of the Galactic bulge with different stellar populations
Molero, M., Matteucci, F., Spitoni, E., Rojas-Arriagada, Á., & Rich, R. M. (2024) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202450418 · Cited by 18
The Effect of Bars on the Ionized ISM: Optical Emission Lines from Milky Way Analogs
Krishnarao, D., Tremonti, C., Fraser-McKelvie, A., Kraljic, K., Boardman, N. F., Masters, K. L., Benjamin, R. A., Haffner, L. M., Jones, A. M., Pace, Z. J., et al. (2020) · The Astrophysical Journal · doi:10.3847/1538-4357/ab9fa3 · Cited by 17
“Because the Milky Way is a prominently barred galaxy (Binney et al. 1991; Weiland et al. 1994; Benjamin et al. 2005; Bland-Hawthorn & Gerhard 2016), it is crucial to understand the impact of bars on the ISM, but doing so from within the Galaxy is limited by our view from within.”
BackgroundInteraction of the galactic-centre super bubbles with the gaseous disc
Sofue, Y., & Kataoka, J. (2021) · Monthly notices of the Royal Astronomical Society · doi:10.1093/mnras/stab1857 · Cited by 11
Bayesian inference of three-dimensional gas maps
Mertsch, P., & Vittino, A. (2021) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202141000 · Cited by 17
Englmaier, P., & Gerhard, O. (2006) · Celestial Mechanics and Dynamical Astronomy · doi:10.1007/s10569-006-9003-3 · Cited by 17
“With some reasonable symmetry assumptions, these methods yield the approximate three-dimensional light distribution of the inner Galaxy on a model grid which can then be analyzed to extract parametric information, such as disk scale length or bar axis ratio and radial extent.”
BackgroundMethodSelf-citationFujishita, M., Torii, K., Kudo, N., Kawase, T., Yamamoto, H., Kawamura, A., Mizuno, N., Onishi, T., Mizuno, A., Machida, M., et al. (2009) · Publications of the Astronomical Society of Japan · doi:10.1093/pasj/61.5.1039 · Cited by 21
“The kinematics with non-circular motions in the nuclear gas disk is explained in terms of the stellar bar driven potential (Binney et al. 1991).”
BackgroundA Dust Lane Leading the Galactic Bar at Negative Galactic Longitudes
Calbet, X., Mahoney, T. J., Hammersley, P. L., et al. (1996) · The Astrophysical Journal · doi:10.1086/309885 · Cited by 17
Rapid Formation of Black Holes in Galaxies: A Self-limiting Growth Mechanism
Li, Z., Sellwood, J. A., & Shen, J. (2017) · The Astrophysical Journal · doi:10.3847/1538-4357/aa9377 · Cited by 16
“We have 9 It is worth noting that the power-law density prolate spheroid bar model used in Binney et al. (1991) is more similar to an N-body bar both in the torque distribution and in the resulting gas flow pattern. found, in common with most other work, that a large fraction of the gas in the bar…”
ResultHigh-speed molecular cloudlets around the Galactic center’s supermassive black hole
Goicoechea, J. R., Pety, J., Chapillon, E., Cernicharo, J., Gérin, M., Herrera, C. N., Requena-Torres, M. A., & Santa-Maria, M. G. (2018) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201833558 · Cited by 21
“…feature at vLSR'−135 km s−1 produced by foreground gas that follows, driven by the barred potential of the Galaxy, non-circular x1 orbits around the Galactic center and produces the characteristic parallelogram on (l, v) longitud-velocity CO maps (e.g., Bally et al. 1988; Binney et al. 1991).”
BackgroundLian, J., Zasowski, G., Hasselquist, S., Neumann, J., Majewski, S. R., Cohen, R. E., Fernández-Trincado, J. G., Lane, R. R., Longa-Peña, P., & Roman–Lopes, A. (2020) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staa3256 · Cited by 16
“The Milky Way ? jianhui.lian@astro.utah.edu is also a barred galaxy, with bar structure identified in both light density profiles (Blitz & Spergel 1991) and kinematics (Binney et al. 1991).”
BackgroundA two-component outer ring and Galactic spiral structure
Melnik, A. M., & Rautiainen, P. (2011) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2011.19641.x · Cited by 16
“This observational feature is sometimes interpreted as a molecular ring (Binney et al. 1991) or as spiral arms emanating from the bar (Fux 1999).”
BackgroundADF22-WEB: A giant barred spiral starburst galaxy in the z = 3.1 SSA22 protocluster core
Umehata, H., Steidel, C. C., Smail, I. R., et al. (2025) · Publications of the Astronomical Society of Japan · doi:10.1093/pasj/psaf010 · Cited by 15
“…of the ISMs is a common feature seen in local barred spiral galaxies and have been reproduced by numerical and analytical calculations, including the cloud-orbit and hydrodynamical shock wave models (Contopoulos & Papayannopoulos 1980, Binney et al. 1991, Athanassoula 1992, Schinnerer et al. 2023).”
Oka, T., & Geballe, T. R. (2020) · The Astrophysical Journal · doi:10.3847/1538-4357/abb1b5 · Cited by 16
“2 of Binney et al. (1991) (from Bally et al. (1988); see also Blitz et al. (1993)) must be incidental and that the face-on view of the CMZ as an ellipse with extremely high eccentricity, which appears for example in Fig.”
BackgroundMethodInfluentialHosek, M. W., Do, T., Lu, J. R., Morris, M., Ghez, A. M., Martinez, G. D., & Anderson, J. (2022) · The Astrophysical Journal · doi:10.3847/1538-4357/ac8bd6 · Cited by 20
“One possibility is that the clusters formed from collisions between gas on the “x1” and “x2” families of orbits found in a barred potential (e.g. Binney et al. 1991).”
BackgroundHigh Excitation Molecular Gas in the Galactic Center Loops; 12CO (J = 2–1 and J = 3–2) Observations
Kudo, N., Torii, K., Machida, M., Davis, T. A., Tsutsumi, K., Fujishita, M., Moribe, N., Yamamoto, H., Okuda, T., Kawamura, A., et al. (2011) · Publications of the Astronomical Society of Japan · doi:10.1093/pasj/63.1.171 · Cited by 17
“Theoretical studies by Binney et al. (1991) showed that the kinematics of the CMZ and EMR can be reproduced by the non-circular motion driven by a stellar bar potential.”
BackgroundAction-based Dynamical Modeling for the Milky Way Disk: The Influence of Spiral Arms
Trick, W. H., Bovy, J., D’Onghia, E., & Rix, H. (2017) · The Astrophysical Journal · doi:10.3847/1538-4357/aa67db · Cited by 14
“The bulge contains a strong bar (Liszt & Burton 1980; Blitz & Spergel 1991; Binney et al. 1991, 1997; Hammersley et al. 2000; Wegg & Gerhard 2013) and the disk itself is threaded by spiral arms (Oort et al. 1958; Georgelin & Georgelin 1976; Churchwell et al. 2009; Reid et al. 2014), and (ring-like)…”
BackgroundSpatial Diffusion of Stars in the Inner Galactic Bulge
Kim, S. S., & Morris, M. (2001) · The Astrophysical Journal · doi:10.1086/321425 · Cited by 15
“For the set of parameters adopted here, the transition from X1 orbits to X2 orbits, which Binney et al. (1991) propose to be responsible for the 180-pc molecular ring, forms atr ≃ 180 pc only wheny0 ≥ 0.9.”
InfluentialLipman, D., Battersby, C., Walker, D. L., Sormani, M. C., Bally, J., Barnes, A. T., Ginsburg, A. G., Glover, S. C. O., Henshaw, J. D., Hatchfield, H. P., et al. (2025) · The Astrophysical Journal · doi:10.3847/1538-4357/adb5ee · Cited by 15
Self-citationGiant H i hole inside the 3 kpc ring and the North Polar Spur—The Galactic crater
Sofue, Y. (2017) · Publications of the Astronomical Society of Japan · doi:10.1093/pasj/psx067 · Cited by 17
“This kinematics problem is not encountered by the bar hypothesis (e.g. Binney et al. 1991), where no energetic explosion is required to produce the non-circular motion.”
BackgroundTowards a three-dimensional distribution of the molecular clouds in the Galactic Centre
YAN, Q.-Z., Walsh, A., Dawson, J. R., Macquart, J., Blackwell, R., Burton, M., Rowell, G. P., Zhang, B., Xu, Y., Tang, Z., et al. (2017) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stx1724 · Cited by 13
“The length and inclination angle of the short bar is about 2.5 kpc and approximately 20◦, respectively (Binney et al. 1991; Dwek et al. 1995; Bissantz & Gerhard 2002; Babusiaux & Gilmore 2005; Cabrera-Lavers et al. 2008), while the half length and inclination angle of the long bar is about 4.5 kpc…”
BackgroundMethodInfluentialPredicted stellar kinematics of a kiloparsec-scale nuclear disc (or ring) in the Milky Way
Debattista, V. P., Earp, S. W. F., Ness, M., et al. (2017) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stx2709 · Cited by 14
“They interpret this variation as resulting from the need to resolve the cusped x1 orbit, at which point the gas shocks and falls inwards on to x2 orbits (Binney et al. 1991; Sormani et al. 2015).”
BackgroundMolecular abundance variations near our galactic center
Minh, Y. C., Kim, S.-J., Pak, S., Lee, S., Irvine, W. M., & Nyman, L.-Å. (2005) · New Astronomy · doi:10.1016/j.newast.2005.03.001 · Cited by 14
“By the interactions with these components, the molecular clouds in our Galactic center show features which are exciting but complex and difficult to interpret (e.g., Scoville, 1972; Burton and Liszt, 1978; Bally et al., 1988; Binney et al., 1991).”
BackgroundA viscous heating mechanism for the hot plasma in the Galactic center region
Bélmont, R., & Tagger, M. (2006) · Astronomy and Astrophysics · doi:10.1051/0004-6361:20054356 · Cited by 14
“Binney et al. (1991) have worked out that the gas dynamics of this Central region is governed by a bar-potential.”
BackgroundGalactic Wind in the Nearby Starburst Galaxy NGC 253 Observed with the Kyoto3DII Fabry-Perot ModePreprint
Matsubayashi, K., Sugai, H., Hattori, T., et al. (2013) · Cited by 14
Horta, D., Petersen, M. S., & Peñarrubia, J. (2025) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staf348 · Cited by 17
Walker, D. L., Battersby, C., Lipman, D., Sormani, M. C., Ginsburg, A. G., Glover, S. C. O., Henshaw, J. D., Longmore, S. N., Klessen, R. S., Immer, K., et al. (2025) · The Astrophysical Journal · doi:10.3847/1538-4357/adb5ef · Cited by 14
Self-citationNamekata, D., & Habe, A. (2011) · The Astrophysical Journal · doi:10.1088/0004-637x/731/1/57 · Cited by 13
“We assume an external gravitational potential of the nuclear region of our Galaxy using the mass distribution derived by Launhardt et al. (2002), who analyzed IRAS3 and COBE4/DIRBE5 data of the central 500 pc of our Galaxy assuming a constant mass-to-light ratio.”
BackgroundInfluentialInvestigation of the Galactic bar based on photometry and stellar proper motions
Bobylev, V. V., Mosenkov, A. V., Bajkova, A. T., et al. (2014) · Astronomy Letters · doi:10.1134/s1063773714030037 · Cited by 13
“These include a study of the gas kinematics (Binney et al. 1991), analysis of the surface brightness (Blitz and Spergel 1991), star counts (Nakada et al. 1991; Stanek et al. 1994), and experiments on searching for microlensing (Udalski et al. 1994).”
BackgroundThe wfc3 galactic bulge treasury program: a first look at resolved stellar population tools
Brown, T. M., Sahu, K. C., Zoccali, M., Renzini, A., Ferguson, H. C., Anderson, J., Smith, E., Bond, H. E., Minniti, D., Valenti, J. A., et al. (2009) · Americanae (AECID Library) · Cited by 11
Liszt, H. S. (1992) · Astrophysics and space science library · doi:10.1007/978-94-011-2813-1_6 · Cited by 13
Photometric Signature of Ultraharmonic Resonances in Barred Galaxies
Krishnarao, D., Pace, Z. J., D’Onghia, E., Aguerri, J. A. L., McClure, R. L., Peterken, T., Fernández-Trincado, J. G., Merrifield, M. R., Masters, K. L., Garma-Oehmichen, L., et al. (2022) · The Astrophysical Journal · doi:10.3847/1538-4357/ac5d55 · Cited by 13
“Observations reveal that 50% to over 70% of nearby disk galaxies host a bar (e.g. Eskridge et al. 2000; Aguerri et al. 2009; Nair & Abraham 2010; Masters et al. 2011) including our own Milky Way (Binney et al. 1991; Weiland et al. 1994; Hammersley et al. 2001; Benjamin et al. 2005).”
BackgroundInfluentialThe Galactic center lobe filled with thermal plasma
Nagoshi, H., Kubose, Y., Fujisawa, K., Sorai, K., Yonekura, Y., Sugiyama, K., Niinuma, K., Motogi, K., & Aoki, T. (2019) · Publications of the Astronomical Society of Japan · doi:10.1093/pasj/psz060 · Cited by 13
“Law et al. (2009) explained the low velocity of the ionized gas in the GCL by the gas dynamics in a barred gravitational potential (Binney et al. 1991).”
BackgroundProper motions for HST observations in three off-axis bulge fields
Soto, M., Zeballos, H., Kuijken, K., et al. (2013) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201117339 · Cited by 12
M Giant Kinematics in Off-Axis Fields between 150 and 300 Parsecs from the Galactic Center
Blum, R., Carr, J. S., Sellgren, K., et al. (1995) · The Astrophysical Journal · doi:10.1086/176084 · Cited by 12
“Dynamical modeling of the observed gas kinematics also indicates that the inner Galaxy is non-axisymmetric (Binney et al. 1991), a result rst suggested by de Vaucouleurs (1964), who compared the non-circular gas motions of the inner Galaxy to those in external barred galaxies.”
BackgroundMethodEnokiya, R., Torii, K., Schultheis, M., Asahina, Y., Matsumoto, R., Furuhashi, E., Nakamura, K., Dobashi, K., Yoshiike, S., Sato, J., et al. (2014) · eScholarship (California Digital Library) · Cited by 12
Gas Motions in the Inner Galaxy and the Dynamics of the Galactic Bulge Region
Gerhard, O. (1992) · Reviews in modern astronomy · doi:10.1007/978-3-642-77543-7_12 · Cited by 12
Self-citationSaha, P., Courbin, F., Sluse, D., Dye, S., & Meylan, G. L. (2006) · arXiv (Cornell University) · doi:10.48550/arxiv.astro-ph/0601370 · Cited by 11
“That implies a 3D profile steeper than r−1.5, which is consistent with available estimates from stellar or gas dynamics; for example, Binney et al. (1991) report an r−1.75 profile near the Galactic centre.”
MethodInfluentialNear-IR Observations of IRAS Sources with SiO Masers at the Inner Galactic Bulge
Deguchi, S., Fujii, T., Matsumoto, S., et al. (2001) · Publications of the Astronomical Society of Japan · doi:10.1093/pasj/53.2.293 · Cited by 12
Proper motions for HST observations in three off-axis bulge fieldsPreprint
Soto, M., Zeballos, H., Kuijken, K. H., et al. (2014) · Cited by 12
Schultheis, M., Sormani, M. C., & Gadotti, D. A. (2025) · The Astronomy and Astrophysics Review · doi:10.1007/s00159-025-00163-6 · Cited by 20
van Donkelaar, F., Mayer, L., Capelo, P. R., Tamfal, T., Quinn, T., & Madau, P. (2024) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stae804 · Cited by 11
Bar-driven dispersal of Galactic substructure
Dillamore, A. M., & Sanders, J. L. (2025) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staf1264 · Cited by 19
Do galactic bars depend on environment?: an information theoretic analysis of Galaxy Zoo 2
Sarkar, S., Pandey, B., & Bhattacharjee, S. (2020) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staa3665 · Cited by 11
Impact of Distance Determinations on Galactic Structure. II. Old Tracers
Kunder, A., Valenti, E., Dall'ora, M., Pietrukowicz, P., Sneden, C., Bono, G., Braga, V., Ferraro, I., Fiorentino, G., Iannicola, G., et al. (2018) · Space Science Reviews · doi:10.1007/s11214-018-0519-0 · Cited by 8
“After then, over the decades, many different tracers - e.g. gas kinematics (Binney et al., 1991), stellar surface profile (Weiland et al., 1994; Dwek et al., 1995; Binney et al., 1997), microlensing experiments (Udalski et al., 2000; Alcock et al., 2000), and OH/IR and SiO maser kinematics (Habing…”
BackgroundRapid Formation of Black Holes in Galaxies: A Self-limiting Growth Mechanism
Li, Z., Sellwood, J. A., & Shen, J. (2018) · Cited by 11
Baryon-driven decontraction in Milky Way-mass haloes
Moreno, V. J. F., Benítez-Llambay, A., Cole, S., & Frenk, C. S. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac312 · Cited by 13
The Nature of Boxy/Peanut Spiral Galaxies: Overview and New Results
Bureau, M., & Freeman, K. C. (1997) · Publications of the Astronomical Society of Australia · doi:10.1071/as97146 · Cited by 11
Kane, S. R., & Sahu, K. C. (2006) · The Astrophysical Journal · doi:10.1086/498402 · Cited by 11
“A number of photometric and dynamic indications also point out the presence of the Galactic bar (Binney et al. 1991;Whitelock et al. 1991;Weinberg 1992).”
BackgroundInvestigation of the Galactic Bar Based on Photometry and Stellar Proper MotionsPreprint
Бобылев, В. В., Mosenkov, A. V., Bajkova, A. T., et al. (2016) · Cited by 11
Blanco DECam Bulge Survey (BDBS)
Marchetti, T., Johnson, C. I., Joyce, M., Rich, R. M., Simion, I. T., Young, M. D., Clarkson, W. I., Pilachowski, C. A., Michael, S. A., Kunder, A., et al. (2022) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202243921 · Cited by 12
Footpoints of the giant molecular loops in the Galactic center region
Riquelme, D., Amo-Baladrón, M. A., Martín-Pintado, J., Mauersberger, R., Martín, S., Burton, M., Cunningham, M., Jones, P. A., Menten, K. M., Bronfman, L., et al. (2017) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201629065 · Cited by 10
“…to its proximity, the central region of the Milky Way allows detailed high resolution studies of the role of a variety of phenomena, namely magnetic loops (Fukui et al. 2006), galactic winds (Bland-Hawthorn & Cohen 2003), gas accretion by for example, a barred Galactic model (Binney et al. 1991).”
BackgroundModeling Turbulence in Galactic Centers
Salas, J. M., Morris, M. R., & Naoz, S. (2021) · The Astronomical Journal · doi:10.3847/1538-3881/abefd3 · Cited by 11
“The gravitational potential we use is adopted from that of Zhao et al. (1994), which is a modified version of the prolate bar potential introduced by Binney et al. (1991).”
MethodMorphological and kinematical analysis of the double-barred galaxy NGC 3504 using ALMA CO (2–1) data
Wu, Y.-T., Trejo, A., Espada, D., & Miyamoto, Y. (2021) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stab1087 · Cited by 10
Living on the edge of the Milky Way's central molecular zone
Busch, L. A., Riquelme, D., Güsten, R., Menten, K. M., Pillai, T., & Kauffmann, J. (2022) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202244870 · Cited by 9
Accelerated phase-mixing in the stellar halo due to a rotating bar
Davies, E. Y., Dillamore, A. M., Vasiliev, E., & Belokurov, V. A. (2023) · Monthly Notices of the Royal Astronomical Society Letters · doi:10.1093/mnrasl/slad017 · Cited by 10
IMAGING CARBON MONOXIDE EMISSION IN THE STARBURST GALAXY NGC 6000
Martín, S., George, M. R., Wilner, D. J., et al. (2010) · The Astronomical Journal · doi:10.1088/0004-6256/139/6/2241 · Cited by 10
“This kinematic signature can be understood as the noncircular motions in the context of a barred potential (Binney et al. 1991).”
BackgroundHercules and Wolf 630 stellar streams and galactic bar kinematics
Бобылев, В. В., & Bajkova, A. T. (2016) · Astronomy Letters · doi:10.1134/s1063773716040010 · Cited by 10
“Binney et al. (1991) and Bissantz et al. (2003) estimated the parameters by comparing the radio observations of central Galactic regions (HI, CO) with various bar models.”
Flattened galactic haloes and baryonic dark matter
Samurović, S., Ćirković, M. M., & Milosevic-Zdjelar, V. (1999) · Monthly Notices of the Royal Astronomical Society · doi:10.1046/j.1365-8711.1999.02799.x · Cited by 10
The Milky Way's Central Molecular ZonePreprint
Mills, E. (2017) · arXiv (Cornell University) · doi:10.48550/arxiv.1705.05332 · Cited by 24
“The resulting large-scale shocks at this orbit intersection along the bar at radii of 200 pc, similar to those observed in other galaxies (54; 55), are believed to convert the gas from primarily neutral to primarily molecular (53), and drive gas inward onto the X2 orbits.”
BackgroundThe Galactic bulge exploration
Prudil, Z., Kunder, A., Silva, L. J. B. E., Gough-Kelly, S., Rejkuba, M., Anderson, S. R., Debattista, V. P., Gerhard, O., Rich, R. M., Nataf, D. M., et al. (2025) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202450620 · Cited by 12
Self-citationNuclear starburst activity induced by elongated bulges in spiral galaxies
Kim, E., Kim, S. S., Choi, Y., Lee, G.-H., de Grijs, R., Lee, M. G., & Hwang, H. S. (2018) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sty1451 · Cited by 9
“To explain gas movement, early studies (Contopoulos & Papayannopoulos 1980; Binney et al. 1991) suggested that gaseous materials move along the stable closed orbits (i.e., x1 orbits) elongated along the bar’s major axis.”
BackgroundHigh-speed molecular cloudlets around the Galactic center’s supermassive black hole
Goicoechea, J. R., Pety, J., Chapillon, E., Cernicharo, J., Gérin, M., Herrera, C. N., Requena-Torres, M. A., & Santa-Maria, M. G. (2018) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361/201833558/pdf · Cited by 13
Long-Period Variables and Carbon Stars in the Galactic Bulge
Whitelock, P. A. (1993) · Springer eBooks · doi:10.1007/978-94-011-0922-2_3 · Cited by 9
AGN activity and nuclear starbursts: Sgr A* activity shapes the Central Molecular Zone
Zubovas, K. (2015) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stv1173 · Cited by 9
“A barred potential leads to vertical as well as radial oscillations of orbits and so could perhaps create the twisted shape required by the first two explanations (Binney et al. 1991; Hasan et al. 1993).”
BackgroundSTAR CLUSTERS IN M31: OLD CLUSTERS WITH BAR KINEMATICS
Morrison, H., Caldwell, N., Schiavon, R. P., et al. (2010) · The Astrophysical Journal Letters · doi:10.1088/2041-8205/726/1/l9 · Cited by 9
“Figure 2 (from Binney et al. 1991) illustrates the spatial and velocity signatures of x1 and x2 orbits.”
BackgroundTHE GALACTIC CENTER: NOT AN ACTIVE GALACTIC NUCLEUS
An, D., Ramírez, S., & Sellgren, K. (2013) · The Astrophysical Journal Supplement Series · doi:10.1088/0067-0049/206/2/20 · Cited by 9
Harris, A. I., Güsten, R., Requena─Torres, M. A., Riquelme, D., Morris, M., Stacey, G. J., Martín-Pintado, J., STUTZKI, J., Simon, R., Higgins, R., et al. (2021) · The Astrophysical Journal · doi:10.3847/1538-4357/ac1863 · Cited by 9
On the Kinematic Signature of a Central Galactic Bar in Observed Star Samples
Vauterin, P., & Dejonghe, H. (1998) · The Astrophysical Journal · doi:10.1086/305724 · Cited by 9
“This theory is supported by the observation of the “parallellogram” structure in the kinematics of the gas (see e.g. Binney et al, 1991), and by the asymmetry in both the integrated light (e.g. Blitz & Spergel, 1991) and the star samples (e.g. Whitelock & Catchpole, 1992).”
ResultThe Evolution of the Galactic Bulge
Rich, R. M. (1992) · Astrophysics and space science library · doi:10.1007/978-94-011-2813-1_3 · Cited by 9
Spergel, D. N. (1992) · Astrophysics and space science library · doi:10.1007/978-94-011-2813-1_4 · Cited by 9
The Central Region of M83 ⋆Preprint
Houghton, R. C. W., & Thatte, N. (2012) · Cited by 9
A non-axisymmetric potential for the Milky Way disk
Khalil, Y. R., Famaey, B., Monari, G., Bernet, M., Siebert, A., Ibata, R., Thomas, G. F., Ramos, P., Antoja, T., Li, C., et al. (2025) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202453077 · Cited by 14
Metadata
- Authors
- Binney, J., Gerhard, O. E., Stark, A. A., Bally, J., & Uchida, K. I.
- Affiliations
- AT&T (United States) (US)
- Venue
- Monthly Notices of the Royal Astronomical Society
- Publisher
- Oxford University Press (OUP)
- Published
- 1991-09-15
- Volume
- 252
- Issue
- 2
- Pages
- 210-218
- ISSN
- 0035-8711 (ISSN-L)
- 1365-2966
- OpenAlex
- W2007725308
- Cited by
- 619
- References
- 0
- Citations by year
- 2026: 18 · 2025: 26 · 2024: 19 · 2023: 11 · 2022: 16 · 2021: 19 · 2020: 22 · 2019: 36 · 2018: 20 · 2017: 24 · 2016: 23 · 2015: 26 · 2014: 14 · 2013: 31 · 2012: 19
- FWCI
- 24.30
- Type
- journal article
- Language
- en
- Open access
- bronze
- doi.org
- Locations
- Monthly Notices of the Royal Astronomical Society (publishedVersion)
- Topics
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Galaxies: Formation, Evolution, Phenomena
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astrophysical Phenomena and Observations
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
- Keywords
- Galactic Center, gas kinematics, bars, corotation, shock, circular velocity curves, outer Lindblad resonance, carbon monoxide emissions, CS emission
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