The Emergence of the Thick Disk in a Cold Dark Matter Universe

By C. Brook, Daisuke Kawata, B. Gibson, Kenneth C. Freeman. 2004

300 citations recorded by the source corpus.

The disk galaxy simulated using our chemodynamic galaxy formation code, GCD+, is shown to have a thick-disk component. This is evidenced by the velocity dispersion versus age relation for solar neighborhood stars, which clearly shows an abrupt increase in velocity dispersion at a look-back time of approximately 8 Gyr, and is in excellent agreement with observation. These thick-disk stars are formed from gas that is accreted to the galaxy during a chaotic period of hierarchical clustering at high redshift. This formation scenario is shown to be consistent with observations of both the Milky Way and extragalactic thick disks.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/a49c58eff3057ce58397e7b30e2255e2e4b9dd48

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Citations in the corpus

Simulations of minor mergers - I. General properties of thick discs (2008, methodology): “A variant of this model, more in line with modern cosmology, is given by Brook et al. (2004, 2005) and consists of the formation of the thick disk in an epoch of multiple mergers of gas-rich building blocks.”
Evolution of magnetic fields in galaxies and future observational tests with the Square Kilometre Array (2008, background): “Brook et al. (2004) demonstrated that the thick stellar disk was created during an epoch of multiple mergers of gas-rich halos, which were abundant at high redshifts.”
Forming disc galaxies in ΛCDM simulations (2006, methodology): “This early disc could be associated with the thick disc components of present day spiral galaxies (Brook et al. 2004; Seth, Dalcanton & de Jong 2005; Yoachim & Dalcanton 2005).”
The structure and dynamical evolution of the stellar disc of a simulated Milky Way-mass galaxy (2016, background): “This agrees with the picture proposed in Brook et al. (2004).”
THICK DISKS OF EDGE-ON GALAXIES SEEN THROUGH THE SPITZER SURVEY OF STELLAR STRUCTURE IN GALAXIES (S4G): LAIR OF MISSING BARYONS? (2011, background): “Brook et al. (2004) found that thick disk scale lengths are larger than those of thin disks, which is in contradiction with observations (Yoachim & Dalcanton 2006).”
Misaligned angular momentum in hydrodynamic cosmological simulations: warps, outer discs and thick discs (2010, background): “…discs of massive spirals assemble primarily from the quiescent cooling of shock-heated gas after the last major merger (e.g. Fall & Efstathiou 1980; Brook et al. 2004; Robertson et al. 2006), although depending on the mass of the galaxy, cold accretion also plays an important role in providing…”
TRACING CHEMICAL EVOLUTION OVER THE EXTENT OF THE MILKY WAY'S DISK WITH APOGEE RED CLUMP STARS (2014, background): “Numerical simulations in which the early disk forms via a gas-rich merger (Brook et al. 2004), clumpy star-formation (Bournaud et al. 2009), or in situ star formation from a turbulent star-forming gas reservoir (e.g., Bird et al. 2013), all qualitatively match the relatively large velocity…”
Determining the Properties and Evolution of Red Galaxies from the Quasar Luminosity Function (2005, background): “…metallicity with mass or velocity dispersion, deferring a treatment of the chemical enrichment histories of galaxies to future work (but see, e.g. Brook et al. 2004a,b; Robertson et al. 2005d; Font et al. 2005), but note that its addition does not create any conflict between our predictions and…”
OXYGEN ABUNDANCES IN NEARBY FGK STARS AND THE GALACTIC CHEMICAL EVOLUTION OF THE LOCAL DISK AND HALO (2013, background): “One of the most accepted scenarios for the formation of the thick-disk involves mergers with satellite galaxies early in the history of the Galactic disk (e.g., Quinn et al. 1993; Walker et al. 1996; Velazquez & White 1999; Abadi et al. 2003; Brook et al. 2004).”
Impacts of a flaring star-forming disc and stellar radial mixing on the vertical metallicity gradient (2016, background): “…disc population is flaring, although the radial mixing will reduce the strength of the flaring, and it is likely that earlier generations of the thin disc were smaller and thicker as seen in numerical simulations (Brook et al. 2004, 2006; Bird et al. 2013; Minchev et al. 2015; Grand et al. 2016).”
Measuring Radial Orbit Migration in the Galactic Disk (2018, background): “…structure must at some level reflect both the global initial conditions, such as the total angular momentum and distribution of the cold gas, and the hierarchical merging during the early turbulent phases of the Milky Way’s formation (Brook et al. 2004; Bird et al. 2013; Stinson et al. 2013).”
Thin, thick and dark discs in ΛCDM (2008, background): “Despite these difficulties, Abadi et al. (2003) found a thick disc in their simulated Milky Way that formed from a mix of accreted and heated stars, while in a series of papers, Brook et al. (2004) and Brook et al. (2005, 2007) and find thick discs form directly from heated gas in their simulations.”
Numerical simulation of a possible origin of the positive radial metallicity gradient of the thick disk (2013, background): “…thick disk including disk heating (Kroupa 2002), satellite accretion (Abadi et al. 2003; Yoachim & Dalcanton 2005), high redshift gas-rich mergers (Brook et al. 2004), radial migration (Roškar et al. 2008; Schönrich & Binney 2009) and a combination of high redshift gas-rich mergers and radial…”
THE ROLE OF COLD FLOWS IN THE ASSEMBLY OF GALAXY DISKS (2008, background): “This late settling allows the shocked gas to cool to a thin disk before forming stars (see also Brook et al. 2004b).”
The Milky Way’s stellar disk (2013, background): “…can be directly accreted (Abadi et al. 2003), or the disk can be heated through minor mergers (Toth & Ostriker 1992; Quinn et al. 1993; Kazantzidis et al. 2008; Villalobos & Helmi 2008; Moster et al. 2010) or experience a burst of star formation following a gasrich merger (Brook et al. 2004).”
PLATO as it is: a legacy mission for Galactic archaeology (2017, unknown): “…as we see them now, was established, as suggested by many theoretical models (e.g., Abadi et al. 2003; Bird et al. 2013; Bournaud et al. 2009; Brook et al. 2004; Gibson et al. 2009; Guedes et al. 2013; Jones & Wyse 1983; Kawata & Chiappini 2016; Noguchi 1998; Sommer-Larsen et al. 2003;…”
Forming a large disc galaxy from a z < 1 major merger (2008, background): “If feedback is able to suppress star formation (SF) during the merger event (Brook et al. 2004b; Robertson et al. 2006; Zavala, Okamoto & Frenk 2008; Governato et al. 2007), the existing cold gas can settle on a new disc plane and start regrowing a stellar disc.”
The Milky Way Tomography with SDSS. II. Stellar Metallicity (2008, background): “…stars that make up the stellar populations in the Milky Way can be studied in great detail, their characterization will provide clues about the galaxy merging process that cannot be extracted from observations of distant galaxies (e.g., Abadi et al. 2003; Brook et al. 2004; and references therein).”
METALLICITY GRADIENTS IN THE MILKY WAY DISK AS OBSERVED BY THE SEGUE SURVEY (2011, background): “If the thick disk formed rapidly at early times (e.g., Brook et al. 2004, 2005), then the thick disk would be chemically homogeneous and the radial metallicity gradient far from the plane of the disk would be flat.”
Beyond Inside-Out Growth: Formation and Evolution of Disk Outskirts (2007, methodology): “Our simulation should be thought of as modeling disk formation and evolution from the cooling of hot gas after the last gas-rich major merger, as suggested by cosmological simulations (Brook et al. 2004, 2007).”