GCD+: a new chemodynamical approach to modelling supernovae and chemical enrichment in elliptical galaxies

Kawata, Daisuke; Gibson, Brad K.

doi:10.1046/j.1365-8711.2003.06356.x

Cited by 218 publications

(295 citation statements)

References 95 publications

(165 reference statements)

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“…Therefore, no metallicity gradient is expected. Brook et al (2005) used the cold dark matter chemodynamical galaxy formation code GCD+ (Kawata & Gibson 2003) to simulate the formation of four Milky-Way-like galaxies. In the four cases, a thick disc appears by accretion of gas-rich building blocks and in-situ (i.e.…”

Section: Discussion: Thick Disc Gradient Versus Formation Scenariosmentioning

confidence: 99%

Probing the Galactic thick disc vertical properties and interfaces

Katz

Soubiran

Cayrel

et al. 2010

A&A

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Aims. This work investigates the properties (metallicity and kinematics) and interfaces of the Galactic thick disc as a function of height above the Galactic plane. The main aim is to study the thick disc in a place where it is the main component of the sample. Methods. We take advantage of former astrometric work in two fields of several square degrees in which accurate proper motions were measured down to V-magnitudes of 18.5 in two directions, one near the north galactic pole and the other at a galactic latitude of 46 • and galactic longitude near 0 • . Spectroscopic observations have been acquired in these two fields for a total of about 400 stars down to magnitude 18.0, at spectral resolutions of 3.5 to 6.25 Å. The spectra have been analysed with the code ETOILE, comparing the target stellar spectra with a grid of 1400 reference stellar spectra. This comparison allowed us to derive the parameters effective temperature, gravity, [Fe/H] and absolute magnitude for each target star. Results. The Metallicity Distribution Function (MDF) of the thin-thick-disc-halo system is derived for several height intervals between 0 and 5 kpc above the Galactic plane. The MDFs show a decrease of the ratio of the thin to thick disc stars between the first and second kilo-parsec. This is consistent with the classical modelling of the vertical density profile of the disc with 2 populations with different scale heights. A vertical metallicity gradient, ∂[Fe/H]/∂z = −0.068 ± 0.009 dex kpc −1 , is observed in the thick disc. It is discussed in terms of scenarios of formation of the thick disc.

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Section: Discussion: Thick Disc Gradient Versus Formation Scenariosmentioning

confidence: 99%

Probing the Galactic thick disc vertical properties and interfaces

Katz

Soubiran

Cayrel

et al. 2010

A&A

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“…Other models incorporate a galaxy formation process that is more similar to the monolithic one (e.g. Kawata & Gibson 2003), 8 With the additional caveat that the stellar value values are robust only in a relative sense. A larger contribution from SNeII may be invoked to explain the observed abundance pattern.…”

Section: Discussionmentioning

confidence: 99%

Abundance ratios in the hot ISM of elliptical galaxies

Pipino

Matteuccí

2011

A&A

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Aims. We constrain possible explanations of the theoretical Fe discrepancy in the hot interstellar medium of elliptical galaxies and simultaneously explain the [α/Fe] ratios. Methods. We use the latest theoretical nucleosynthetic yields, incorporate dust, and explore different SNIa progenitor scenarios by means of a self-consistent chemical evolution model that reproduces the stellar populations properties of elliptical galaxies. Results. Models with Fe-only dust and/or a lower effective SNIa rate achieve a closer agreement with the observed Fe abundance. However, a suitable modification of the SNIa yields relative to the standard W7 model is needed to fully describe the abundance ratio pattern. The 2D explosion model C-DDT by Maeda and collaborator may be capable of reproducing the [Fe/H] and the [α/Fe] ratios.

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“…α-elements scale strongly with mass, between 8 and 40 solar masses, while the iron value does not. If we assume that stars with masses greater than 40 solar masses all have yields the same as stars at 40 solar masses (as in Few et al 2012;Kawata & Gibson 2003), we cannot arrive at a solution for silicon. We therefore only include stars with masses of up to 40 solar masses in our SNII yield tables.…”

Section: Making Chemical Evolution Tracks (Part A)mentioning

confidence: 99%

Reconstructing the star formation history of the Milky Way disc(s) from chemical abundances

Snaith

Haywood

Matteo

et al. 2015

A&A

170

262

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We develop a chemical evolution model to study the star formation history of the Milky Way. Our model assumes that the Milky Way has formed from a closed-box-like system in the inner regions, while the outer parts of the disc have experienced some accretion. Unlike the usual procedure, we do not fix the star formation prescription (e.g. Kennicutt law) to reproduce the chemical abundance trends. Instead, we fit the abundance trends with age to recover the star formation history of the Galaxy. Our method enables us to recover the star formation history of the Milky Way in the first Gyrs with unprecedented accuracy in the inner (R < 7−8 kpc) and outer (R > 9−10 kpc) discs, as sampled in the solar vicinity. We show that half the stellar mass formed during the thick-disc phase in the inner galaxy during the first 4−5 Gyr. This phase was followed by a significant dip in star formation activity (at 8−9 Gyr) and a period of roughly constant lower-level star formation for the remaining 8 Gyr. The thick-disc phase has produced as many metals in 4 Gyr as the thin-disc phase in the remaining 8 Gyr. Our results suggest that a closed-box model is able to fit all the available constraints in the inner disc. A closed-box system is qualitatively equivalent to a regime where the accretion rate maintains a high gas fraction in the inner disc at high redshift. In these conditions the SFR is mainly governed by the high turbulence of the interstellar medium. By z ∼ 1 it is possible that most of the accretion takes place in the outer disc, while the star formation activity in the inner disc is mostly sustained by the gas that is not consumed during the thick-disc phase and the continuous ejecta from earlier generations of stars. The outer disc follows a star formation history very similar to that of the inner disc, although initiated at z ∼ 2, about 2 Gyr before the onset of the thin-disc formation in the inner disc.

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GCD+: a new chemodynamical approach to modelling supernovae and chemical enrichment in elliptical galaxies

Cited by 218 publications

References 95 publications

Probing the Galactic thick disc vertical properties and interfaces

Probing the Galactic thick disc vertical properties and interfaces

Abundance ratios in the hot ISM of elliptical galaxies

Reconstructing the star formation history of the Milky Way disc(s) from chemical abundances

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