A DIVERSITY OF PROGENITORS AND HISTORIES FOR ISOLATED SPIRAL GALAXIES

By M. Martig, Frédéric Bournaud, Darren Croton, A. Dekel, Romain Teyssier. 2012

93 citations recorded by the source corpus.

We analyze a suite of 33 cosmological simulations of the evolution of Milky-Way-mass galaxies in low-density environments. Our sample spans a broad range of Hubble types at z = 0, from nearly bulgeless disks to bulge-dominated galaxies. Despite the fact that a large fraction of the bulge is typically in place by z ∼ 1, we find no significant correlation between the morphology at z = 1 and at z = 0. The z = 1 progenitors of disk galaxies span a range of morphologies, including smooth disks, unstable disks, interacting galaxies, and bulge-dominated systems. By z ∼ 0.5, spiral arms and bars are largely in place and the progenitor morphology is correlated with the final morphology. We next focus on late-type galaxies with a bulge-to-total ratio (B/T) <0.3 at z = 0. These show a correlation between B/T at z = 0 and the mass ratio of the largest merger at z < 2, as well as with the gas accretion rate at z > 1. We find that the galaxies with the lowest B/T tend to have a quiet baryon input history, with no major mergers at z < 2, and with a low and constant gas accretion rate that keeps a stable angular-momentum direction. More violent merger or gas accretion histories lead to galaxies with more prominent bulges. Most disk galaxies have a bulge Sérsic index n ⩽ 2. The galaxies with the highest bulge Sérsic index tend to have histories of intense gas accretion and disk instability rather than active mergers.

Subfields: Astronomy and Astrophysics, Electrical and Electronic Engineering, Instrumentation

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Citations in the corpus

Yule-Simpson’s paradox in Galactic Archaeology (2019, methodology): “In §§2.2-2.5 we make use of the Milky Way chemodynamical model by MCM13, who used a hybrid technique to combine a classical semi-analytical chemical evolution model (Chiappini 2009) with a simulation in the cosmological context (Martig et al. 2012).”
Chemodynamical evolution of the Milky Way disk II: Variations with Galactic radius and height above the disk plane (2014, methodology): “The main features that make this model unique is the fusion between a state-of-theart simulation in the cosmological context (Martig et al., 2009, 2012) and a detailed thin-disk chemical evolution model.”
THE RELATIONSHIP BETWEEN MONO-ABUNDANCE AND MONO-AGE STELLAR POPULATIONS IN THE MILKY WAY DISK (2016, methodology): “The simulation used for the MCM model is part of a suite of numerical experiments presented by Martig et al. (2012), where the authors studied the evolution of 33 simulated galaxies from z = 5 to z = 0 using the zoom-in technique described by Martig et al. (2009).”
THE EPOCH OF DISK SETTLING: z ∼ 1 TO NOW (2012, background): “2009; Ceverino et al. 2010; Brook et al. 2011; Kimm et al. 2011; Martig et al. 2012, and references therein).”
Galaxy Zoo 2: detailed morphological classifications for 304,122 galaxies from the Sloan Digital Sky Survey (2013, background): “Most obviously, merger features reveal ongoing gravitational interactions, but even the presence of a central bulge in a disk galaxy is likely to indicate a history of mass assembly through significant mergers (Martig et al. 2012 and references therein).”
The age structure of stellar populations in the solar vicinity Clues of a two-phase formation history of the Milky Way disk (2013, background): “This epoch is perhaps the transition between an early violent phase of disk formation to a more quiescent one (e.g., Martig et al. 2012; Kraljic et al. 2012).”
The formation of disc galaxies in high-resolution moving-mesh cosmological simulations (2013, background): “…and almost universally too concentrated and massive bulges (e.g. Scannapieco et al. 2009), their rotation curves had unrealistic shapes (e.g. Hummels & Bryan 2012), and in general they were far too luminous (e.g. Martig et al. 2012) as a result of the “overcooling catastrophe” (Balogh et al. 2001).”
Constraining the Milky Way assembly history with Galactic Archaeology (2016, methodology): “The simulation used is part of a suite of numerical experiments presented by Martig et al. (2012), where the authors studied the evolution of 33 simulated galaxies from z = 5 to z = 0 using the zoom-in technique described by Martig et al. (2009).”
Vertical disc heating in Milky Way-sized galaxies in a cosmological context (2015, background): “…simulations are now able to produce thin stellar discs with small bulges (Governato et al. 2010; Agertz et al. 2011; Guedes et al. 2011; Martig et al. 2012; Aumer et al. 2013; Stinson et al. 2013a; Marinacci et al. 2 We note that stars that migrate via satellite interactions are…”
Radial migration does little for Galactic disc thickening (2012, unknown): “27 (C3) by Martig et al. (2012).”
A RADIAL AGE GRADIENT IN THE GEOMETRICALLY THICK DISK OF THE MILKY WAY (2016, background): “Given the variety of formation histories for disk galaxies (e.g., Martig et al. 2012), it is likely that both types of thick disks exist.”
Chemodynamical evolution of the Milky Way disk - I. The solar vicinity (2012, methodology): “27 by Martig et al. 2012).”
The effects of radial migration on the vertical structure of Galactic discs (2012, result): “They support this claim with results from isolated N -body+SPH simulations from the GalMer database (Chilingarian et al. 2010) as well as sticky-particle semicosmological simulations (Martig et al. 2012).”
The Milky Way’s stellar disk (2013, background): “As of 2012, various groups (Agertz et al. 2011; Guedes et al. 2011; Martig et al. 2012; Stinson et al. 2013) have succeeded in running simulations that can result in large, disk-dominated galaxies, resembling the Milky Way in many properties (cf. Figure 4).”
The Dark Matter Crisis: Falsification of the Current Standard Model of Cosmology (2012, background): “Therefore, mergers and encounters between galaxies are logically implied events that shape all larger galaxies (e.g. Bournaud et al. 2011; Martig et al. 2012) such that, by Implication 3 (Section 3.2), type B dwarfs appear in significant numbers.”
Dissecting simulated disc galaxies - I. The structure of mono-age populations (2014, methodology): “The galaxies are drawn from a larger sample of 33 simulated galaxies, described in Martig et al. (2012).”