Formation of gas discs in merging galaxies

By J. Barnes. 2002

307 citations recorded by the source corpus.

Observations indicate that much of the interstellar gas in merging galaxies may settle into extended gaseous discs. Here, I present simulations of disc formation in mergers of gas-rich galaxies. Up to half of the total gas settles into embedded discs; the most massive instances result from encounters in which both galaxies are inclined to the orbital plane. These discs are often warped, many have rather complex kinematics, and roughly a quarter have counter-rotating or otherwise decoupled central components. Discs typically grow from the inside out; infall from tidal tails may continue disc formation over long periods of time.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/90615765801db57442a73e54ebe8c16bbc2e4d95

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In Astronomy and Astrophysics

1. P. Hopkins
2. L. Hernquist
3. Thomas J. Cox
4. T. Naab
5. R. Somerville
6. M. Cappellari
7. R. Dav'e
8. A. Dekel

Citations in the corpus

• A Merger-driven Scenario for Cosmological Disk Galaxy Formation (2005, background): “The survival of disks in minor merger or infall scenarios have been readily addressed both semianalytically (Toth & Ostriker 1992; Benson et al. 2004) and numerically (Quinn et al. 1993; Walker et al. 1996; Velazquez & White 1999; Font et al. 2001; Barnes 2002).”
• The ATLAS3D project - XIII. Mass and morphology of H I in early-type galaxies as a function of environment (2011, background): “Based on numerical simulations, several authors have argued that it is possible to form an ETG with a disc by merging two gasrich galaxies (e.g. Naab & Burkert 2001; Barnes 2002; Springel & Hernquist 2005; Naab, Jesseit & Burkert 2006; Robertson et al. 2006).”
• The correlation of star formation quenching with internal galaxy properties and environment (2008, background): “Major (near equal mass) mergers can transform spiral galaxies into ellipticals (Toomre & Toomre 1972; cf. Barnes 2002), and may also quench future star formation by ejecting the interstellar medium (ISM) from the galaxy via starburst, active galactic nuclei (AGN) or shock-driven winds (Cox et al.…”
• Dry Mergers in GEMS: The Dynamical Evolution of Massive Early-Type Galaxies (2005, unknown): “…blue star-forming galaxies at z P 1 luminous enough to fade into present-day massive non-star-forming galaxies, but the boxy isophotes and cores in the light distributions of massive early-type galaxies are challenging to reproduce inmergers of disk galaxies (Naab&Burkert 2001, 2003; Barnes 2002).”
• VLA IMAGING OF VIRGO SPIRALS IN ATOMIC GAS (VIVA). I. THE ATLAS AND THE H i PROPERTIES (2009, background): “…morphology could either be the result of a merger between two small systems in which the outer H i is now falling back and forming a new disk (e.g., Barnes 2002), or, alternatively, it could have been pulled out during an encounter with nearby galaxy IC 3605, which is ≈ 150 kpc away with Δv = 300…”
• Metallicity and Nuclear Star Formation in Nearby Galaxy Pairs: Evidence for Tidally Induced Gas Flows (2005, background): “Gas infall is expected to occur after two galaxies undergo their the first close encounter (Barnes 2002; Barnes & Hernquist 1996).”
• THE POPULATION OF VISCOSITY- AND GRAVITATIONAL WAVE-DRIVEN SUPERMASSIVE BLACK HOLE BINARIES AMONG LUMINOUS ACTIVE GALACTIC NUCLEI (2009, background): “The dense nuclear gas around the black hole (BH) binary is expected to cool rapidly, and settle into a rotationally supported, circumbinary disk (e.g., Barnes 2002; Escala et al. 2005).”
• The ATLAS3D project – IV. The molecular gas content of early-type galaxies (2011, background): “Acquisition of molecular gas through major or minor mergers also should be rare, both because the cluster’s high velocity dispersion decreases the merger rate and because mergers tend to fling gas to large radii (Barnes 2002) where it would be highly vulnerable to stripping.”
• Shock-induced star formation in a model of the Mice (2004, background): “A survey of different encounters, along the lines of other surveys without star formation (e.g. Barnes 2002), might establish if widespread star formation at C© 2004 RAS, MNRAS 350, 798–808 Downloaded from https://academic.oup.com/mnras/article-abstract/350/3/798/971619 by guest on 28 July…”
• The influence of gas on the structure of merger remnants (2006, unknown): “In general, gas transport is more effective if the spin and the orbital angular momentum of the disc is aligned (Barnes 2002).”
• The effect of gas fraction on the morphology and time-scales of disc galaxy mergers (2009, background): “The spheroidal remnants of gas-rich mergers can reform small discs out of the remaining gas (Barnes 2002; Cox et al. 2006b; Naab, ⋆ NOAO Leo Goldberg Fellow † W.M. Keck Fellow Jesseit, & Burkert 2006; Khalatyan et al. 2008), while the remnants of extremely gas-rich mergers can preserve discs large…”
• Statistical Properties of Collisionless Equal- and Unequal-Mass Merger Remnants of Disk Galaxies (2001, background): “Barnes (2002) recently presented a first detailed set of equal- and unequal-mass merger simulations of gas-rich galaxies resulting in the formation of extended gas disks.”
• The Magellanic Stream, High-Velocity Clouds, and the Sculptor Group (2002, background): “…stripped off with the gas in the tidal models, the observations show that stellar tails are often completely missing or offset from the gaseous tails in interacting systems (e.g. the M82 group, Yunet al. 1994; Hibbard, Vacca & Young 2000) and this can be reproduced in simulations (Barnes 2002).”
• Theoretical Challenges in Galaxy Formation (2016, background): “As a result, rotating remnants of gas rich mergers can form disk-like subsystems (Barnes 2002; Bekki & Shioya 1997; Bendo & Barnes 2000; Jesseit et al. 2009; Jesseit, Naab & Burkert 2007) and show observed line-of-sight velocity distributions with steep leading wings, which is not the case if gas…”
• The ATLAS3D project - X. On the origin of the molecular and ionized gas in early-type galaxies (2011, background): “…a non-zero cosmological constant (ΛCDM), it is thought that star-formation is shut-off in these galaxies by major mergers that can funnel the cold gas into the centre of the remnant (Barnes 2002), where it may be destroyed by an active galactic nucleus (AGN) or be used up quickly in a starburst.”
• A Population of Short-Period Variable Quasars from PTF as Supermassive Black Hole Binary Candidates (2016, background): “The gas, following the formation of a Keplerian binary, settles in a rotationally supported disc (Barnes 2002), and the binary hardens, as it dissipates energy and angular momentum to the gaseous disc.”