Galaxy evolution in compact groups II. Witnessing the influence of major structures in their evolution

• DOI: 10.48550/arxiv.2406.14671
• Publication Date: 2024-01-01
• Authors: Montaguth, Gissel P.; Monachesi, Antonela; Torres-Flores, Se...; Gómez, Facundo A.; Lima-Dias, Ciria; Cortesi, Arianna; de Oliveira, Clau...; Telles, Eduardo; Panda, Swayamtrupta; Grossi, Marco; Lopes, Paulo A. A.; O'Mill, Ana Laura; Hernandez-Jimenez...; Olave-Rojas, D. E.; Demarco, Ricardo; Kanaan, Antonio; Ribeiro, Tiago; Schoenell, William
• Keywords: Astrophysics of Galaxies (astro-ph.GA); FOS: Physical sciences; Astrophysics - Astrophysics of Galaxies

Accepted to A&A, 16 pages, 13 figures<br/>Compact groups (CGs) of galaxies are extreme environments for morphological transformations and the cessation of star formation. Though initially considered isolated, it is now recognised that many CGs are embedded in larger structures. We aim to understand the dynamics of CGs and how their surrounding environments impact their physical properties. We selected 316 CGs in the Stripe 82 region (1011 galaxies) and 2281 field galaxies as a control sample. At least 41% of CGs are part of major structures (non-isolated CGs). We find a bimodal distribution in the effective radius ($R_e$)-Sersic index ($n$) plane for transition galaxies ($(u-r) > 2.3$ and $n<2.5$) in CGs. Transition galaxies in isolated CGs are denser in the $R_e-n$ plane for $n < 1.75$, while those in non-isolated CGs show a smoother increase in $n$, with 62% having $n > 1.5$. This suggests that many have undergone morphological transformation, contributing to the compact galaxy population. Galaxies in CGs have lower mean specific star formation rates (sSFR) than the control sample, with non-isolated CGs showing even lower sSFR, indicating stronger star formation suppression. Non-isolated CGs also have a higher fraction of quenched galaxies. When dividing by morphology, significant differences arise only for early-type galaxies (ETGs; $(u-r) > 2.3$ and $n>2.5$). In isolated CGs, ETGs show lower quenched fractions and higher sSFR in low-mass bins ($\log(M_/M_{\odot}) < 11$), suggesting sustained star formation. In non-isolated CGs, ETGs show higher quenched fractions and lower sSFR in high-mass bins ($\log(M_/M_{\odot}) > 11$), underscoring the environmental suppression of star formation. We propose that major structures accelerate morphological transformations and facilitate preprocessing. Our results highlight the need to consider larger structures when analysing CGs, as they significantly affect galaxy evolution.<br/>