Understanding the kinematics of Galactic Centre gas

Binney, James; Gerhard, Ortwin; Stark, A. A.; Bally, John; Uchida, K. I.

doi:10.1093/mnras/252.2.210

Cited by 595 publications

(686 citation statements)

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“…This is illustrated in Figure 3. The gas orbital motions in this way in a CMZ (or a nuclear ring) has been theoretically predicted (Athanassoula 1992) and suggested from observations of the Galactic CMZ (Binney et al 1991) and extragalactic nuclear rings (Kenney et al 1992). The middle panels in Figure 3 show CO line profiles at one of the regions with large line widths.…”

Section: M83supporting

confidence: 58%

Kinematics and dynamics of molecular gas in galactic centers

Sakamoto

2013

Proc. IAU

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Abstract. The central molecular zone (CMZ) in the central half kpc of the Milky Way is a massive concentration of molecular gas in the center of a barred spiral galaxy. Current and past activities in the Galactic center include the formation of massive stars/clusters, AGN feeding, and feedback. At the same time, observations of molecular gas in external galaxies show that many disk galaxies have similar condensations of molecular gas in their central kpc or so. They also have CMZs, or nuclear molecular rings or concentrations in more common terms among extragalactic observers. The formation of the CMZs are often, but not always, related to stellar bars. The centers of nearby galaxies can provide valuable information on the general properties of galactic centers and CMZs through comparative studies of multiple galactic centers of different characteristics from various viewing angles. Linear resolutions achieved toward nearby extragalactic CMZs with modern radio interferometers are now comparable to those achieved toward the Galactic CMZ with small single-dish telescopes. I review and present work on the formation mechanism and properties of the CMZs in external galaxies with some comparisons with the CMZ of our Galaxy.

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Section: M83supporting

confidence: 58%

Kinematics and dynamics of molecular gas in galactic centers

Sakamoto

2013

Proc. IAU

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“…On the one hand, many lines of evidence now point to the fact that the Milky Way hosts a bar (de Vaucouleurs 1964;Peters 1975;Cohen & Few 1976;Liszt & Burton 1980;Gerhard & Vietri 1986;Mulder & Liem 1986;Binney et al 1991;Nakada et al 1991;Whitelock & Catchpole 1992;Weiland et al 1994;Paczynski et al 1994; of a peanut-shaped bulge (e.g. Li & Shen 2012).…”

Section: Introductionmentioning

confidence: 99%

Separation of stellar populations by an evolving bar: implications for the bulge of the Milky Way

Debattista

Ness

Gonzalez

et al. 2017

Monthly Notices of the Royal Astronomical Society

146

255

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We present a novel interpretation of the previously puzzling different behaviours of stellar populations of the Milky Way's bulge. We first show, by means of pure N -body simulations, that initially co-spatial stellar populations with different in-plane random motions separate when a bar forms. The radially cooler populations form a strong bar, and are vertically thin and peanut-shaped, while the hotter populations form a weaker bar and become a vertically thicker box. We demonstrate that it is the radial, not the vertical, velocity dispersion that dominates this evolution. Assuming that early stellar discs heat rapidly as they form, then both the in-plane and vertical random motions correlate with stellar age and chemistry, leading to different density distributions for metal-rich and metal-poor stars. We then use a high-resolution simulation, in which all stars form out of gas, to demonstrate that this is what happens. When we apply these results to the Milky Way we show that a very broad range of observed trends for ages, densities, kinematics and chemistries, that have been presented as evidence for contradictory paths to the formation of the bulge, are in fact consistent with a bulge which formed from a continuum of disc stellar populations which were kinematically separated by the bar. For the first time we are able to account for the bulge's main trends via a model in which the bulge formed largely in situ. Since the model is generic, we also predict the general appearance of stellar population maps of external edge-on galaxies.

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“…However, this study suggests that the rate at which high-velocity clouds could migrate inwards from larger GC distances is not well constrained. Candidates for such a collision are clouds on x1 orbits following the bar's major axis outside the x2 (minor axis) orbital zone, as already suggested by Binney et al 1991, or clouds falling in from the outer parts of the Galaxy (Crawford et al 2002). A collision between an x1 and an x2 orbit cloud is particularly intriguing, as x1 clouds display line-of-sight velocities of up to 270 km/s (Dame et al 2001), which could account for the orbital velocity of 232 km/s observed for the Arches today.…”

Section: Formation Scenarios For the Archesmentioning

confidence: 65%

The orbital motion of the Arches cluster — clues on cluster formation near the galactic center

Stolte

Ghez

Morris³

et al. 2008

J. Phys.: Conf. Ser.

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Abstract. The Arches cluster is one of the most massive, young clusters in the Milky Way. Located inside the central molecular zone in the inner 200 pc of the Galactic center, it formed in one of the most extreme star-forming environments in the present-day Galaxy. Its young age of only 2.5 Myr allows us to observe the cluster despite the strong tidal shear forces in the inner Galaxy. The orbit of the cluster determines its dynamical evolution, tidal stripping, and hence its fate. We have measured the proper motion of the Arches cluster relative to the ambient field from Keck/NIRC2 LGS-AO and VLT/NAOS-CONICA NGS-AO observations taken 4.3 years earlier. When combined with the radial velocity, we derive a 3D space motion of 232 ± 30 km/s for the Arches. This motion is exceptionally large when compared to molecular cloud orbits in the GC, and places stringent constraints on the formation scenarios for starburst clusters in dense, nuclear environments.

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Understanding the kinematics of Galactic Centre gas

Cited by 595 publications

References 0 publications

Kinematics and dynamics of molecular gas in galactic centers

Kinematics and dynamics of molecular gas in galactic centers

Separation of stellar populations by an evolving bar: implications for the bulge of the Milky Way

The orbital motion of the Arches cluster — clues on cluster formation near the galactic center

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