Hydrodynamical Simulations of Nuclear Rings in Barred Galaxies

Li, Zhi; Shen, Juntai; Kim, Woong-Tae

doi:10.1088/0004-637x/806/2/150

Cited by 77 publications

(93 citation statements)

References 86 publications

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“…Foremost of the limitations is that the resolution used for the gas is still too large to properly resolve the gas ring size. Sormani et al (2015) show, using two-dimensional grid calculations with a fixed bar potential, that the size of the gas ring that forms is dependent on the grid cell size, varying by a factor of ∼ 2 when this cell size is changed from 40 pc to 10 pc (see also Li et al 2015). They interpret this variation as resulting from the need to resolve the cusped x1 orbit, at which point the gas shocks and falls inwards onto x2 orbits (Binney et al 1991;Sormani et al 2015).…”

Section: Limitations Of the Modelmentioning

confidence: 97%

Predicted stellar kinematics of a kiloparsec-scale nuclear disc (or ring) in the Milky Way

Debattista

Earp

Ness

et al. 2017

Monthly Notices of the Royal Astronomical Society

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In Debattista et al. (2015), we proposed that a kiloparsec-scale nuclear disc is responsible for the high-velocity secondary peak in the stellar line-of-sight velocity distributions (LOSVDs) seen at positive longitudes in the bulge by the Apache Point Observatory Galactic Evolution Experiment (APOGEE). Here, we make further qualitative but distinctive predictions of the kinematic properties of a nuclear disc, including for the LOSVDs at negative longitudes (which APOGEE-2 will observe) and examine the proper motions throughout the disc. Since a nuclear ring is also able to produce similar high-velocity LOSVD peaks, we present predictions for the proper motion signatures which distinguish between a nuclear disc and a nuclear ring. We also demonstrate that the stars in a nuclear disc, which would be on x2 orbits perpendicular to the bar, can remain on these orbits for a long time and can therefore be old. We show that such (old) nuclear discs of comparable size exist in external galaxies.

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Section: Limitations Of the Modelmentioning

confidence: 97%

Predicted stellar kinematics of a kiloparsec-scale nuclear disc (or ring) in the Milky Way

Debattista

Earp

Ness

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…High spatial resolution is necessary to capture the turbulent gas motions in the central region of galaxies, as demonstrated in previous works (e.g. Sormani et al 2015a;Li et al 2015;Few et al 2016 We set up the initial rotating gaseous disk with an exponential surface density profile Σ gas = Σ 0 exp (−R/R d ), where Σ 0 = 76.7 M pc −2 and R d = 4.8 kpc. The gas disk then has a surface density around 13 M pc −2 at solar neighbourhood to match the observed value roughly (Bovy & Rix 2013).…”

Section: Numerical Schemementioning

confidence: 99%

Testing the Prediction of Fuzzy Dark Matter Theory in the Milky Way Center

Shen

Schive

2020

ApJ

Self Cite

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The fuzzy dark matter model (FDM, also known as quantum wave dark matter model) argues that light bosons with a mass of ∼ 10 −22 eV are a possible candidate for dark matter in the Universe. One of the most important predictions of FDM is the formation of a soliton core instead of a density cusp at the center of galaxies. If FDM is the correct theory of dark matter, then the predicted soliton core can help to form the Central Molecular Zone (CMZ) in the Milky Way. We present high-resolution hydrodynamical simulations of gas flow patterns to constrain the properties of the soliton core based on a realistic Milky Way potential. We find that a dense center is required to form a reasonable CMZ. The size and kinematics of the CMZ offer a relatively strong constraint on the inner enclosed mass profile of the Galaxy. If a soliton core is not considered, a compact nuclear bulge alone with a radially varying mass-to-light ratio can match the observed size and kinematics of the CMZ. A soliton core model with a mass of ≈ 4.0 × 10 8 M and a core radius of ≈ 0.05 kpc, together with a less massive nuclear bulge with a constant mass-to-light ratio, also agrees nicely with the current data. Such a FDM soliton core corresponds to a boson mass of ∼ 2 − 7 × 10 −22 eV, which could be further constrained by the improved determination of the mass-to-light ratio in the Galactic center.

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“…However, the distribution of stellar populations is influenced by more factors. From hydrodynamical simulations of gas dynamics in barred galaxies, we know that gas flows inwards in thin stream lines along the leading edges 1 of rotating bars (Athanassoula 1992;Piner et al 1995;Kim et al 2012;Li et al 2015;Renaud et al 2015;Sormani et al 2015;Fragkoudi et al 2016). If gas is present and star formation is not suppressed by shear, star formation is expected to happen along the leading edges of the bar.…”

Section: Introductionmentioning

confidence: 99%

Stellar populations across galaxy bars in the MUSE TIMER project

Neumann

Fragkoudi

Pérez

et al. 2020

A&A

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Stellar populations in barred galaxies save an imprint of the influence of the bar on the host galaxy's evolution. We present a detailed analysis of star formation histories (SFHs) and chemical enrichment of stellar populations in nine nearby barred galaxies from the TIMER project. We use integral field observations with the MUSE instrument to derive unprecedented spatially resolved maps of stellar ages, metallicities, [Mg/Fe] abundances and SFHs, as well as Hα as a tracer of ongoing star formation. We find a characteristic V-shaped signature in the SFH perpendicular to the bar major axis which supports the scenario where intermediate age stars (∼ 2-6 Gyr) are trapped on more elongated orbits shaping a thinner part of the bar, while older stars (> 8 Gyr) are trapped on less elongated orbits shaping a rounder and thicker part of the bar. We compare our data to state-of-the-art cosmological magneto-hydrodynamical simulations of barred galaxies and show that such V-shaped SFHs arise naturally due to the dynamical influence of the bar on stellar populations with different ages and kinematic properties. Additionally, we find an excess of very young stars (< 2 Gyr) on the edges of the bars, predominantly on the leading side, confirming typical star formation patterns in bars. Furthermore, mass-weighted age and metallicity gradients are slightly shallower along the bar than in the disc likely due to orbital mixing in the bar. Finally, we find that bars are mostly more metal-rich and less [Mg/Fe]-enhanced than the surrounding discs. We interpret this as a signature that the bar quenches star formation in the inner region of discs, usually referred to as star formation deserts. We discuss these results and their implications on two different scenarios of bar formation and evolution.

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Hydrodynamical Simulations of Nuclear Rings in Barred Galaxies

Cited by 77 publications

References 86 publications

Predicted stellar kinematics of a kiloparsec-scale nuclear disc (or ring) in the Milky Way

Predicted stellar kinematics of a kiloparsec-scale nuclear disc (or ring) in the Milky Way

Testing the Prediction of Fuzzy Dark Matter Theory in the Milky Way Center

Stellar populations across galaxy bars in the MUSE TIMER project

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