On the accretion of a new group of galaxies on to Virgo – II. The effect of pre-processing on the stellar population content of dEs

Bidaran, Bahar; Barbera, F. La; Pasquali, A.; Peletier, Reynier F.; Ven, Glenn van de; Grebel, Eva K.; Falcón-Barroso, J.; Sybilska, Agnieszka; Gadotti, Dimitri A.; Coccato, L.

doi:10.1093/mnras/stac2005

Cited by 9 publications

(10 citation statements)

References 174 publications

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“…These previous results are in agreement with stellar populations from other works on dwarfs spheroidal in galaxy clusters like Virgo (Sybilska et al 2017 ;S ¸en et al 2018 ;Bidaran et al 2022 ) or Coma (Smith et al 2009 ). Putting our sample and ATLAS 3 D together, a clear mass-metallicity relation is visible.…”

Section: Ages and Metallicitiessupporting

confidence: 92%

“…5 . Such analysis, ho we ver, is dif ficult to perform in low-mass galaxies because of their low surface brightness and therefore objects with σ < 30 km s −1 have rarely been studied up to now outside the Local Group (S09; Sybilska et al 2017 ;S ¸en et al 2018 ;Bidaran et al 2022 ). Our SAMI-Fornax dwarfs are the first sample of more than a few galaxies to reach as low as 10 km s −1 .…”

Section: Age and Metallicities Of Dwarfs Galaxiesmentioning

confidence: 93%

“…Because of this, the exact stellar population parameters of their dwarfs are not directly comparable to ours due to the different MNRAS 522, 130-150 (2023) methodologies. Generally, there is an offset in age and metallicity between using FSF and index-fitting (Mentz et al 2016 ;Bidaran et al 2022 ; see also the comparison with the populations derived from inde x-inde x diagrams for the ATLAS 3 D sample in Fig. A2 ).…”

Section: Age and Metallicities Of Dwarfs Galaxiesmentioning

confidence: 97%

“…To understand better how galaxies are enriched in α-elements, we now study the distribution of α-enhancement for dwarf galaxies as a function of clustercentric radius, and, for the Local Group, as a function of distance to the Milky W ay. W e use here our SAMI-Fornax dwarfs, the Coma dwarfs of S09, and the Local Group dwarfs that are satellites of the Milky Way and the dwarfs in the Virgo Cluster from Liu et al ( 2016a ), Sybilska et al ( 2017 ), andBidaran et al ( 2022 ). In the Milky Way, we use [Mg/Fe], and for objects in the Fornax A group, we use the distance to Fornax A.…”

Section: Environmentmentioning

confidence: 99%

“…Their sample, ho we ver, was composed of fairly bright, M r > −19, and massive, 10 9 M < M < 5 × 10 9 M , galaxies, which we will not consider in this paper. Also Sybilska et al ( 2017 ; with 20 dwarfs of 10 9 M < M < 10 10 M ) and Bidaran et al ( 2022 ; with 9 dwarf galaxies of M ∼ 10 9 M ) used FSF, indicating that this is a feasible method nowadays.…”

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confidence: 99%

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The SAMI–Fornax Dwarfs Survey – III. Evolution of [α/Fe] in dwarfs, from Galaxy Clusters to the Local Group

Romero-Gómez

Peletier

Aguerri

et al. 2023

Monthly Notices of the Royal Astronomical Society

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Using very deep, high spectral resolution data from the SAMI Integral Field Spectrograph we study the stellar population properties of a sample of dwarf galaxies in the Fornax Cluster, down to a stellar mass of 107 M⊙, which has never been done outside the Local Group. We use full spectral fitting to obtain stellar population parameters. Adding massive galaxies from the ATLAS3D project, which we re-analysed, and the satellite galaxies of the Milky Way, we obtained a galaxy sample that covers the stellar mass range 104 to 1012M⊙. Using this large range we find that the mass – metallicity relation is not linear. We also find that the [α/Fe]-stellar mass relation of the full sample shows a U-shape, with a minimum in [α/Fe] for masses between 109 − 1010M⊙. The relation between [α/Fe] and stellar mass can be understood in the following way: When the faintest galaxies enter the cluster environment, a rapid burst of star formation is induced, after which the gas content is blown away by various quenching mechanisms. This fast star formation causes high [α/Fe] values, like in the Galactic halo. More massive galaxies will manage to keep their gas longer and form several bursts of star formation, with lower [α/Fe] as a result. For massive galaxies, stellar populations are regulated by internal processes, leading to [α/Fe] increasing with mass. We confirm this model by showing that [α/Fe] correlates with clustercentric distance in three nearby clusters, and also in the halo of the Milky Way.

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Section: Ages and Metallicitiessupporting

confidence: 92%

Section: Age and Metallicities Of Dwarfs Galaxiesmentioning

confidence: 93%

Section: Age and Metallicities Of Dwarfs Galaxiesmentioning

confidence: 97%

Section: Environmentmentioning

confidence: 99%

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confidence: 99%

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The SAMI–Fornax Dwarfs Survey – III. Evolution of [α/Fe] in dwarfs, from Galaxy Clusters to the Local Group

Romero-Gómez

Peletier

Aguerri

et al. 2023

Monthly Notices of the Royal Astronomical Society

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Preprocessing in small groups: Three simulated galaxies interacting prior to cluster infall

Łokas

2023

A&A

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The formation of galaxy clusters is a complicated process that probably involves the accretion of galaxies in groups, as observed in nearby clusters, such as Virgo and Fornax. The members of the groups undergo “preprocessing” prior to cluster infall, which affects their stellar populations and morphology. In this paper, I present an extreme example of such an accretion event selected from the IllustrisTNG100 simulation. The group, composed of three full-sized disky galaxies and a number of smaller satellites, is accreted early, with the first pericenter around the cluster at redshift z = 1.3. Before the infall, the three galaxies interact strongly in pairs within the group, which produces tidally induced bars in the two more massive ones. The interactions also lead to mass exchange and trigger some star formation activity resulting in temporary rejuvenation of their stellar populations. After infall, they all undergo seven pericenter passages around the cluster, experiencing strong mass loss in the dark matter and gas components, as well as reddening of the stellar populations. Their tidally induced bars are, however, preserved and even enhanced probably due to the loss of gas via ram-pressure stripping in the intracluster medium. The study demonstrates that group accretion can happen very early in cluster formation and proposes another scenario for the formation of tidally induced bars.

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Large-scale structure around the Fornax-Eridanus complex

Raj,

Awad,

Peletier

et al. 2024

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Our objectives are to map the filamentary network around the Fornax-Eridanus complex and probe the influence of the local environment on galaxy morphology. We employed the novel machine-learning tool, named, 1-Dimensional, Recovery, Extraction, and Analysis of Manifolds (1-DREAM) to detect and model filaments around the Fornax cluster. We then used the morphology-density relation of galaxies to examine the variation in the galaxies' morphology with respect to their distance from the central axis of the detected filaments. We detected 27 filaments that vary in length and galaxy-number density around the Fornax-Eridanus complex. We find that 81<!PCT!> of galaxies in our catalogue belong to filaments and 19<!PCT!> of galaxies are located outside filaments. The filaments around the Fornax-Eridanus complex showcase a variety of environments:\ some filaments encompass groups and clusters, while others are only inhabited by galaxies in pristine filamentary environments. In this context, we reveal a well-known structure, namely:\ the Fornax Wall, which passes through the Dorado group, Fornax cluster, and Eridanus supergroup. With regard to the morphology of galaxies, we find that early-type galaxies (ETGs) populate high-density filaments and high-density regions of the Fornax Wall. Furthermore, the fraction of the ETG-population decreases as the distance to the central axis of the filament increases. The fraction of late-type galaxies (LTGs; 8<!PCT!>) is lower than that of ETGs (12<!PCT!>) at 0.5 Mpc/$h$ from the filament spine. Of the total galaxy population in filaments around the Fornax-Eridanus complex, sim 7<!PCT!> are ETGs and sim 24<!PCT!> are LTGs located in pristine environments of filaments, while sim 27<!PCT!> are ETGs and sim 42<!PCT!> are LTGs in groups and clusters within filaments. Among the galaxies in the filamentary network around the Fornax-Eridanus complex, 44<!PCT!> of them belong to the Fornax Wall. This study reveals the cosmic web around the Fornax cluster, which exhibits a variety of filamentary environments. With this, our research asserts that filamentary environments are heterogeneous in nature. When investigating the role of the environment on galaxy morphology, it is essential to consider both the local number-density and a galaxy's proximity to the filament spine (i.e. the filament core). Within this framework, we ascribe the observed morphological segregation in the Fornax Wall to the pre-processing of galaxies among groups embedded in it.

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On the accretion of a new group of galaxies on to Virgo – II. The effect of pre-processing on the stellar population content of dEs

Cited by 9 publications

References 174 publications

The SAMI–Fornax Dwarfs Survey – III. Evolution of [α/Fe] in dwarfs, from Galaxy Clusters to the Local Group

The SAMI–Fornax Dwarfs Survey – III. Evolution of [α/Fe] in dwarfs, from Galaxy Clusters to the Local Group

Preprocessing in small groups: Three simulated galaxies interacting prior to cluster infall

Large-scale structure around the Fornax-Eridanus complex

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