Galaxy mass-size segregation in the cosmic web from the CAVITY parent sample
Rattachement africain : es, ca, nl. Niveau de preuve : code pays fourni par la source.
Le résumé fourni par la source
Context. The mass-size relation is a fundamental galaxy scaling relation that is intrinsically linked to galaxy formation and evolution. The physical processes involved in galaxy growth leave their particular imprint on the relation between the stellar or total mass and galaxy size. Aims. We aim to explore the effect of the large-scale environment on the stellar mass-size relation using samples and a selection of added-value products from the Calar Alto Void Integral-field Treasury surveY (CAVITY) collaboration. Methods. We analysed the Petrosian R50 and R90 radii from SDSS DR16 images of a sample of ≈14 000 galaxies inhabiting cosmic voids, filaments and walls, and clusters, with a stellar mass range between 108.5 − 1011 M⊙. We investigated the mass-size relation with respect to the galaxy morphology, as well as with the star formation history (SFH), parametrised across a range of different timescales (T50, T70, and T90). Results. We find that, on average, early-type galaxies in voids are approximately 10−20% smaller than their counterparts in denser environments, such as filaments, walls, and clusters, regardless of when they assembled their mass. Additionally, evidence suggests that the mass-size relation for the more massive void galaxies within the early-type sample exhibits a shallower slope, compared to galaxies in denser large-scale environments. In contrast, early-type galaxies in filaments, walls, and clusters exhibit a more consistent mass-size distribution. For stellar masses of log(M⋆/M⊙) = 9 − 10.5, late-type cluster galaxies are smaller and more concentrated than those in lower density environments, such as filaments, walls, and voids; whereas void and filament+wall galaxies exhibit similar size and concentration values. However, for galaxies with masses above 1010.5 M⊙, the sizes of void galaxies become comparable to those in clusters. The trend of smaller low-mass cluster galaxies is primarily driven by galaxies with T50 greater than 7 Gyr. Conclusions. We conclude that the large-scale environment influences the mass-size relation of galaxies. Assuming that early-type galaxies undergo two growth phases, we find that they primarily grow their mass during the first phase of formation. In voids, the subsequent size growth from minor mergers is less pronounced. This is likely due to slower evolution and reduced minor merger activity or the fact that the void environment inherently has fewer accretion events, or even a combination of these effects. The change in slope for high-mass void galaxies suggests a lower rate of minor accretion. This trend is also evident in late-type void galaxies with masses above ≈1010.5 M⊙, where minor mergers contribute to their size growth. In contrast, late-type quenched cluster galaxies are smaller in size due to interactions within the cluster environment, with early infallers being more strongly affected by these environmental interactions.
Ce résumé expose les affirmations des auteurs. BNTIC ne l’interprète pas comme une validation indépendante des résultats.
Le contrôle bibliographique ouvert
DOI retrouvé dans Crossref DOI retrouvé ; titre concordant.
- Titre Crossref
- Galaxy mass-size segregation in the cosmic web from the CAVITY parent sample
- Date Crossref
- 01/03/2025
- Éditeur
- EDP Sciences
- Type
- journal-article
Ce recoupement confirme des métadonnées liées au DOI. Il ne confirme ni la méthode ni les conclusions de l’étude, et il ne compte pas comme une seconde source scientifique indépendante.
Où se fait cette recherche
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Universidad de Granada pays non établi dans la noticeUniversité ou école supérieure
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Universidad de La Laguna pays non établi dans la noticeUniversité ou école supérieure
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Instituto de Astrofísica de Canarias pays non établi dans la noticeStructure de recherche
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Centre for Research in Astrophysics of Québec pays non établi dans la noticeStructure de recherche
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Université Laval Département de Physique pays non établi dans la noticeUniversité ou école supérieure
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Instituto de Astrofísica de Andalucía pays non établi dans la noticeStructure de recherche
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University of Groningen Kapteyn Astronomical Institute pays non établi dans la noticeUniversité ou école supérieure
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Universidad Complutense de Madrid pays non établi dans la noticeUniversité ou école supérieure
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Departamento de Física Teórica y del Cosmos pays non établi dans la noticeInstitution
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Instituto Carlos I de Física Teórica y Computacional pays non établi dans la noticeStructure de recherche
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Departamento de Astrofísica pays non établi dans la noticeInstitution
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Departamento de Física de la Tierra y Astrofísica & IPARCOS pays non établi dans la noticeInstitution
Universidad de Granada, Universidad de La Laguna et Instituto de Astrofísica de Canarias, avec 9 autres affiliations.
Une affiliation ne permet pas de déduire la nationalité d’un auteur.