Galaxy evolution in compact groups II. Witnessing the influence of major structures in their evolution
Date
2024-06-24Author
Parado Montaguth, Gissel Dayana
Antonela, Monachesi
Sergio, Torres-Flores
Gomez, Facundo Ariel
Ciria, Lima-Dias
Claudia, Mendes de Oliveira
Eduardo, Telles
Marco, Grossi
Augusto Lopes, Paulo Afrânio
O’Mill, Ana Laura
Hernandez-Jimenez, Jose A.
Olave-Rojas, Daniela E.
Ricardo, Demarco
Antonio, Kanaan
Tiago, Ribeiro
William, Schoenell
Cortesi, Arianna
Swayamtrupta, Panda
ORCID
https://orcid.org/0009-0003-1364-3590https://orcid.org/0000-0003-2325-9616
https://orcid.org/0000-0003-4232-8584
https://orcid.org/0000-0002-5854-7426
https://orcid.org/0000-0003-4675-3246
https://orcid.org/0000-0002-6656-5333
https://orcid.org/0000-0002-2925-1861
https://orcid.org/0000-0001-9243-3425
https://orcid.org/0000-0003-3921-2177
https://orcid.org/0009-0007-8005-4541
https://orcid.org/0000-0002-4064-7234
https://orcid.org/0000-0002-0620-136X
Metadata
Show full item recordAbstract
Compact groups (CGs) of galaxies are an extreme environment for the morphological transformations and the cessation of star
formation in galaxies. However, despite initially being conceived as isolated systems, it is now widely recognised that many of them
are not as isolated as expected. Our objective is to understand the dynamics of CGs, as well as how the environment surrounding
CGs impacts their morphological and physical properties. To achieve this, we selected a sample of 340 CGs in the Stripe 82 region,
with a total of 1083 galaxies, and a sample of 2281 field galaxies as a control sample. We find that at least 27% of our sample of
CGs are part of major structures, i.e. non-isolated CGs. We find a bimodality in the effective radius (Re)-Sérsic index (n) plane for
all transition galaxies (those with (u − r) > 2.3 and n < 2.5) in CGs. Additionally, transition galaxies in isolated CGs populate
more densely the Re − n plane for n < 1.75. In contrast, transition galaxies in non-isolated CGs have smoothly increasing n values,
suggesting these galaxies have already suffered morphological transformation, and primarily contribute to the distribution of more
compact galaxies in the Re−n plane for all transition galaxies in CGs. We also find significant differences in the specific star-formation
rate (sSFR) distribution between the late-type galaxies (LTGs) (those with (u − r) < 2.3 and n < 2.5) in non-isolated CGs and the
same type of galaxies in the control sample, suggesting that the evolution of LTGs differs in non-isolated CGs. Moreover, Early-type
galaxies (those with (u − r) > 2.3 and n > 2.5) and transition galaxies in non-isolated CGs have lower sSFR values and a higher
fraction of quenched galaxies, compared to those in isolated CGs. Based on our results, we propose an evolutionary scenario where
the major structures in which the CGs are embedded accelerate the morphological transformations of their galaxy members, and also
facilitates preprocessing. Our findings highlight the importance of considering the larger structures in which CGs may be located,
when analysing the properties of their galaxy members, as this can significantly affect the evolution of CGs and their galaxies.
xmlui.dri2xhtml.METS-1.0.item-citation
Montaguth, G. P., Monachesi, A., Torres-Flores, S., Gómez, F. A., Lima-Dias, C., Cortesi, A., ... & Schoenell, W. (2024). Galaxy evolution in compact groups II. Witnessing the influence of major structures in their evolution. arXiv preprint arXiv:2406.14671
Other links
https://arxiv.org/abs/2406.14671Collections
The following license files are associated with this item: