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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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Research works printed but not linked: 3
- 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.
Cited by
Sorted by citations
Secular Evolution and the Formation of Pseudobulges in Disk Galaxies
Kormendy, J., & Kennicutt, R. C. (2004) · Annual Review of Astronomy and Astrophysics · doi:10.1146/annurev.astro.42.053102.134024 · Cited by 1,737
“If the inner bar has a radius of 1 - 2 kpc (Binney et al. 1991; Blitz & Spergel 1991; Binney & Gerhard 1993; Sellwood 1993b; cf. Dwek et al. 1995), then it is more nearly the length of typical nuclear bars than of typical main bars.”
BackgroundThe Galaxy in Context: Structural, Kinematic, and Integrated Properties
Bland-Hawthorn, J., & Gerhard, O. (2016) · Annual Review of Astronomy and Astrophysics · doi:10.1146/annurev-astro-081915-023441 · Cited by 1,656
“This corroborates long-standing evidence for a barred potential in the bulge region from noncircular motions seen in HI and CO longitudevelocity (lv) diagrams (Binney et al. 1991, Englmaier & Gerhard 1999).”
BackgroundSelf-citationSECULAR EVOLUTION AND THE FORMATION OF PSEUDOBULGES IN DISK GALAXIESPreprint
Kormendy, J., Kennicutt, R. C., & words, K. (2004) · Cited by 1,152
THE GALACTIC CENTER ENVIRONMENT
Morris, M., & Serabyn, E. (1996) · Annual Review of Astronomy and Astrophysics · doi:10.1146/annurev.astro.34.1.645 · Cited by 930
“The kinematics of this ring (hereafter referred to as the “180-pc molecular ring”) and its tilt relative to the Galactic plane are continuous with those of the exterior H I nuclear disk, indicating that this structure likely marks the location of an H I/H2 transition (Binney et al 1991).”
BackgroundInfluentialRotation Curves of Spiral Galaxies
Sofue, Y., & Rubin, V. (2001) · Annual Review of Astronomy and Astrophysics · doi:10.1146/annurev.astro.39.1.137 · Cited by 1,011
“A few percent exhibits non-circular ’forbidden’ velocities, which could be due to non-circular motion in an oval potential (Binney et al. 1991), whereas a question remains why the majority of the gas is regularly rotating.”
Background
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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