Simulating the evolution of disc galaxies in a group environment – II. The influence of close encounters between galaxies

Villalobos, Álvaro; Lucia, G. De; Murante, Giuseppe

doi:10.1093/mnras/stu1278

Cited by 27 publications

(18 citation statements)

References 62 publications

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“…This is an idealized assumption useful for most physical configurations, but not representative when more than one satellite interacts with the central galaxy at the same time (see e.g. Villalobos et al 2014). More work in this direction is needed to characterize mass transfers in multiple merger configurations, as a function of the relative masses and orbits.…”

Section: Discussionmentioning

confidence: 99%

On the dependence of galaxy morphologies on galaxy mergers

Fontanot

Macciò

Hirschmann

et al. 2015

Monthly Notices of the Royal Astronomical Society

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The distribution of galaxy morphological types is a key test for models of galaxy formation and evolution, providing strong constraints on the relative contribution of different physical processes responsible for the growth of the spheroidal components. In this paper, we make use of a suite of semi-analytic models to study the efficiency of galaxy mergers in disrupting galaxy discs and building galaxy bulges. In particular, we compare standard prescriptions usually adopted in semi-analytic models, with new prescriptions proposed by Kannan et al., based on results from high-resolution hydrodynamical simulations, and we show that these new implementations reduce the efficiency of bulge formation through mergers. In addition, we compare our model results with a variety of observational measurements of the fraction of spheroid-dominated galaxies as a function of stellar and halo mass, showing that the present uncertainties in the data represent an important limitation to our understanding of spheroid formation. Our results indicate that the main tension between theoretical models and observations does not stem from the survival of purely disc structures (i.e. bulgeless galaxies), rather from the distribution of galaxies of different morphological types, as a function of their stellar mass.

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Section: Discussionmentioning

confidence: 99%

On the dependence of galaxy morphologies on galaxy mergers

Fontanot

Macciò

Hirschmann

et al. 2015

Monthly Notices of the Royal Astronomical Society

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“…Another physical process that works on galaxies in their passage through the deep potential well of the cluster is tidal stripping (e.g. Zwicky 1951;Gnedin 2003a;Villalobos et al 2014). It can induce a central star formation burst (Byrd & Valtonen 2001), bar instabilities (Łokas et al 2016), changes in the pattern of the spiral arms (Semczuk et al 2017), and truncate dark matter haloes (e.g.…”

Section: Introductionmentioning

confidence: 99%

ROGER: Reconstructing orbits of galaxies in extreme regions using machine learning techniques

Ríos¹,

Martínez

Coenda

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We present the ROGER (Reconstructing Orbits of Galaxies in Extreme Regions) code, which uses three different machine learning techniques to classify galaxies in, and around, clusters, according to their projected phase-space position. We use a sample of 34 massive, M200 > 1015h−1M⊙, galaxy clusters in the MultiDark Planck 2 (MDLP2) simulation at redshift zero. We select all galaxies with stellar mass M⋆ ≥ 108.5h−1M⊙, as computed by the semi-analytic model of galaxy formation SAG, that are located in, and in the vicinity of, these clusters and classify them according to their orbits. We train ROGER to retrieve the original classification of the galaxies from their projected phase-space positions. For each galaxy, ROGER gives as output the probability of being a cluster galaxy, a galaxy that has recently fallen into a cluster, a backsplash galaxy, an infalling galaxy, or an interloper. We discuss the performance of the machine learning methods and potential uses of our code. Among the different methods explored, we find the K-Nearest Neighbours algorithm achieves the best performance.

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“…Other mechanisms such as tidal stripping (e.g. Gnedin 2003a;Villalobos et al 2014) and thermal evaporation (Cowie & Songaila 1977) could also affect galaxy evolution. Galaxy-galaxy high-speed interactions (e.g.…”

Section: Introductionmentioning

confidence: 99%

Effects of environment on stellar metallicity profiles of late-type galaxies in the CALIFA survey

Coenda

Mast

Muriel

et al. 2020

A&A

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Aims. We explore the effects of environment in the evolution of late-type galaxies by studying the radial profiles of light- and mass-weighted metallicities of galaxies in two discrete environments: field and groups. Methods. We used a sample of 167 late-type galaxies with stellar masses of 9 ≤ log(M⋆/M⊙) ≤ 12 drawn from the Calar Alto Legacy Integral Field Area (CALIFA) survey. Firstly, we obtained light- and mass-weighted stellar metallicity profiles and stellar mass density profiles of these galaxies using publicly available data. We then classified them according to their environment into field and group galaxies. Finally, we studied the metallicity of galaxies in these two environments, including a comparison of the metallicity as a function of radius, at a characteristic scale, and as a function of stellar mass surface density. As metallicity depends on galaxy mass, we took special care throughout the study to compare, in all cases, subsamples of galaxies in groups and in the field that have similar masses. Results. We find significant differences between group and field late-type galaxies in terms of their metallicity: group galaxies are systematically higher in metallicity than their field counterparts. We find that field galaxies, in general, have metallicity profiles that show a negative gradient in their inner regions and a shallower profile at larger radii. This is in contrast to the metallicity profiles of galaxies in groups, which tend to be flat in the inner regions and to have a negative gradient in the outer parts. Regarding the metallicity at the characteristic radius of the luminosity profiles, we consistently find that it is higher for group galaxies irrespective of galaxy mass. At fixed local stellar surface mass density, group galaxies are again higher in metallicity, also the dependence of metallicity on surface density is less important for group galaxies. Conclusions. The evidence of a clear difference in metallicity between group and field galaxies as a function of mass, spatial scale, and local stellar mass density is indicative of the different evolutionary paths followed by galaxies in groups and in the field. We discuss some possible implications of the observed differences.

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Simulating the evolution of disc galaxies in a group environment – II. The influence of close encounters between galaxies

Cited by 27 publications

References 62 publications

On the dependence of galaxy morphologies on galaxy mergers

On the dependence of galaxy morphologies on galaxy mergers

ROGER: Reconstructing orbits of galaxies in extreme regions using machine learning techniques

Effects of environment on stellar metallicity profiles of late-type galaxies in the CALIFA survey

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