Mild evolution of the stellar metallicity gradients of disc galaxies

Tissera, Patricia B.; Machado, Rubens E. G.; Vı́lchez, J. M.; Pedrosa, Susana; Sánchez‐Blázquez, P.; Varela, S.

doi:10.1051/0004-6361/201628915

Cited by 13 publications

(19 citation statements)

References 66 publications

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“…We have analysed the properties of simulated galaxies dominated by the spheroid components in a Λ-CDM universe with the aim to investigate to what extent these systems are consistent with the observations. In previous works, the dynamical and chemical properties of disc-dominated galaxies have been studied in great detail, finding very good agreement with observations Tissera et al 2016aTissera et al ,b, 2017. Since the evolutionary paths of spheroid-dominated galaxies are expected to be different, it is of relevance to assess to what extent the same models and simulations reproduce the two kinds of systems.…”

Section: Discussionsupporting

confidence: 66%

Field spheroid-dominated galaxies in a Λ-CDM Universe

Rosito

Pedrosa

Tissera

et al. 2018

A&A

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Context. Understanding the formation and evolution of early-type, spheroid-dominated galaxies is an open question within the context of the hierarchical clustering scenario, particularly in low-density environments. Aims. Our goal is to study the main structural, dynamical, and stellar population properties and assembly histories of field spheroiddominated galaxies formed in a Λ−CDM scenario to assess to what extent they are consistent with observations. Methods. We selected spheroid-dominated systems from a Λ-CDM simulation that includes star formation, chemical evolution, and supernova feedback. The sample is made up of 18 field systems with M Star 6 × 10 10 M that are dominated by the spheroid component. For this sample we estimated the fundamental relations of ellipticals and compared them with current observations. Results. The simulated spheroid galaxies have sizes that are in good agreement with observations. The bulges follow a Sersic law with Sersic indexes that correlate with the bulge-to-total mass ratios. The structural-dynamical properties of the simulated galaxies are consistent with observed Faber-Jackson, fundamental plane, and Tully-Fisher relations. However, the simulated galaxies are bluer and with higher star formation rates than the observed isolated early-type galaxies. The archaeological mass growth histories show a slightly delayed formation and more prominent inside-out growth mode than observational inferences based on the fossil record method.Conclusions. The main structural and dynamical properties of the simulated spheroid-dominated galaxies are consistent with observations. This is remarkable since our simulation has not been calibrated to match them. However, the simulated galaxies are blue and star-forming, and with later stellar mass growth histories compared to observational inferences. This is mainly due to the persistence of extended discs in the simulations. The need for more efficient quenching mechanisms able to avoid further disc growth and star formation is required in order to reproduce current observational trends.

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Section: Discussionsupporting

confidence: 66%

Field spheroid-dominated galaxies in a Λ-CDM Universe

Rosito

Pedrosa

Tissera

et al. 2018

A&A

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“…Cosmological hydrodynamical simulations are powerful tool to study the chemical evolution of galaxies (Taylor & Kobayashi 2017). Tissera et al (2016Tissera et al ( , 2017 analysed the radial oxygen gradients in cosmological simulations, finding that if the discs formed inside out then, negative metallicity gradients are detected in the gas-phase, in agreement with previous results (Pilkington et al 2012).…”

Section: Discussionsupporting

confidence: 79%

“…Gibson et al 2013 andMa et al 2018) while weaker stellar feedback shows a slight trend with redshift (e.g. Tissera et al 2017). As shown in Figure 1, the metallicity gradients obtained from the EAGLE project (Schaye et al 2015) are consistent with the observed large dispersion and show no clear evolution in time (Tissera et al in prep).…”

Section: P B Tisseramentioning

confidence: 76%

Galaxy Evolution in the context of radial metallicity gradients

Tissera

2018

Proc. IAU

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The chemical abundances of the gas-phase and stellar components of disc galaxies are relevant to understand their formation and evolution. It has been shown that an inside-out disc formation yields negative chemical profiles. However, a large spread in metallicity gradients, including positive ones, has been reported by recent and more precise observations, suggesting the action of other physics processes such as gas outflows and inflows, radial migration, and mergers and interactions. Cosmological simulations that includes chemical models provide a tools to tackle the origin of the metallicity profiles and the action of those processes that might affect them as a function of time. I present a summary of the current state-of-knowledge from a numerical point of view and discuss the main results from the analysis of the EAGLE simulations.

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“…The novelty in the METGRAD model relies on the assumption of a (negative) metallicity gradient in satellites 2 (see, e.g. Tissera et al 2017), such that the fraction of metals stripped is different from the fraction of stellar mass stripped. In this model, at each episode of stripping we assume that metals in the satellite galaxies follow an exponential profile with R sl,metals = f R · R sl , where R sl,metals is the scale lenght of the distribution of metals, and f R is a random fraction assumed to be between 0.5 and 1.…”

Section: Methodsmentioning

confidence: 99%

Theoretical Predictions of Colors and Metallicity of the Intracluster Light

Contini

Yi²,

Kang

2019

ApJ

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We study colors and metallicities of the Brightest Cluster Galaxies (BCGs) and Intra-Cluster Light (ICL) in galaxy groups and clusters, as predicted by a semi-analytic model of galaxy formation, coupled with a set of high-resolution N-body simulations. The model assumes stellar stripping and violent relaxation processes during galaxy mergers to be the main channels for the formation of the ICL. We find that BCGs are more metal-rich and redder than the ICL, at all redshifts since the ICL starts to form (z ∼ 1). In good agreement with several observed data, our model predicts negative radial metallicity and color gradients in the BCG+ICL system. By comparing the typical colors of the ICL with those of satellite galaxies, we find that mass and metals in the ICL come from galaxies of different mass, depending on the redshift. Stripping of low mass galaxies, 9 < log M * < 10, is the most important contributor in the early stage of the ICL formation, but the bulk of the mass/metals contents are given by intermediate/massive galaxies, 10 < log M * < 11, at lower redshift. Our analysis supports the idea that stellar stripping is more important than galaxy mergers in building-up the ICL, and highlights the importance of colors/metallicity measurements for understanding the formation and evolution of the ICL.

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Mild evolution of the stellar metallicity gradients of disc galaxies

Cited by 13 publications

References 66 publications

Field spheroid-dominated galaxies in a Λ-CDM Universe

Field spheroid-dominated galaxies in a Λ-CDM Universe

Galaxy Evolution in the context of radial metallicity gradients

Theoretical Predictions of Colors and Metallicity of the Intracluster Light

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