Compact Groups of Galaxies in Sloan Digital Sky Survey and LAMOST Spectral Survey. I. The Catalogs

Zheng, Yun-Liang; Shen, Shiyin

doi:10.3847/1538-4365/ab5c26

Cited by 19 publications

(9 citation statements)

References 104 publications

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“…The WAVES-WIDE(-DEEP) surveys aiming to cover an area of ∼70 (1200) deg 2 , identifying ∼50,000 (20,000) dark matter halos down to a mass of 10 14 (10 11 ) M and out to a redshift of z phot 0.2 (0.8). As with X-ray selected objects, optically selected groups are physically heterogenous systems (e.g., see the dynamical analysis by Zheng and Shen [239] for a sample of compact groups). However, it is possible that the physical processes at work in the IGrM of optically-and X-ray-selected systems are different.…”

Section: Galaxy Groups With the Next-generation Instrumentsmentioning

confidence: 99%

Scaling Properties of Galaxy Groups

et al. 2021

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Galaxy groups and poor clusters are more common than rich clusters, and host the largest fraction of matter content in the Universe. Hence, their studies are key to understand the gravitational and thermal evolution of the bulk of the cosmic matter. Moreover, because of their shallower gravitational potential, galaxy groups are systems where non-gravitational processes (e.g., cooling, AGN feedback, star formation) are expected to have a higher impact on the distribution of baryons, and on the general physical properties, than in more massive objects, inducing systematic departures from the expected scaling relations. Despite their paramount importance from the astrophysical and cosmological point of view, the challenges in their detection have limited the studies of galaxy groups. Upcoming large surveys will change this picture, reassigning to galaxy groups their central role in studying the structure formation and evolution in the Universe, and in measuring the cosmic baryonic content. Here, we review the recent literature on various scaling relations between X-ray and optical properties of these systems, focusing on the observational measurements, and the progress in our understanding of the deviations from the self-similar expectations on groups’ scales. We discuss some of the sources of these deviations, and how feedback from supernovae and/or AGNs impacts the general properties and the reconstructed scaling laws. Finally, we discuss future prospects in the study of galaxy groups.

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Section: Galaxy Groups With the Next-generation Instrumentsmentioning

confidence: 99%

Scaling Properties of Galaxy Groups

et al. 2021

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“…However, when radial velocities became available, concordant triplets were allowed in the sample (Hickson et al 1992). Also, McConnachie et al (2009) and Zheng & Shen (2020) have introduced CG catalogues including triplets. Following these works and allowing to have triplets among the CGs, we adopted a minimum number of three galaxies and a maximum of ten.…”

Section: Compact Groupsmentioning

confidence: 99%

Galaxy clustering in the VVV Near-IR Galaxy Catalogue

Soto,

Sgró,

Baravalle

et al. 2022

Preprint

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Mapping galaxies at low Galactic latitudes and determining their clustering status are fundamental steps in defining the large-scale structure in the nearby Universe. The VVV Near-IR Galaxy Catalogue (VVV NIRGC) allows us to explore this region in great detail. Our goal is to identify galaxy overdensities and characterize galaxy clustering in the Zone of Avoidance. We use different clustering algorithms to identify galaxy overdensities: the Voronoi tessellations, the Minimum Spanning Tree and the Ordering Points To Identify the Clustering Structure. We studied the membership, isolation, compactness, and flux limits to identify compact groups of galaxies. Each method identified a variety of galaxy systems across the Galactic Plane that are publicly available. We also explore the probability that these systems are formed by concordant galaxies using mock catalogues. Nineteen galaxy systems were identified in all of the four methods. They have the highest probability to be real overdensities. We stress the need for spectroscopic follow-up observations to confirm and characterize these new structures.

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“…To perform statistical studies of these peculiar systems, until today astronomers apply similar criteria to different observational samples of galaxies but using automatic algorithms (Prandoni et al 1994;Iovino 2002; Iovino et al 2003;Lee et al 2004;de Carvalho et al 2005;McConnachie et al 2009;Díaz-Giménez et al 2012;Sohn et al 2015;Díaz-Giménez et al 2018;Zheng & Shen 2020). Other authors identified compact groups using percolation algorithms (for example the friends-of-friends algorithm) but trying to mimic the main characteristics of the Hickson CGs ( Barton et al 1996;Allam & Tucker 2000;Focardi & Kelm 2002;Hernández-Fernández & Mendes de Oliveira 2015;Sohn et al 2016).…”

Section: Introductionmentioning

confidence: 99%

“…They found that only 44% of the SHONCGs are also in HMCG sample. Recently, Zheng & Shen (2020) identified a large sample of CGs with redshifts information also in SDSS-DR12 survey, using a relaxed Hickson-like criteria. The percentage of groups in common with previous samples is very poor and suggests that the population of CGs identified by different authors is different.…”

Section: Introductionmentioning

confidence: 99%

Compact groups from semi-analytical models of galaxy formation -- III: purity and completeness of Hickson-like catalogues

Taverna,

Diaz-Gimenez,

Zandivarez

et al. 2022

Preprint

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Many catalogues of isolated compact groups of galaxies (CGs) have been extracted using Hickson's criteria to identify isolated, dense systems of galaxies, with at least three or four galaxies concordant in magnitude and redshift. But is not clear to what extent the catalogues of CGs are complete and reliable, relative to 3D truly isolated, dense groups. Using five different semi-analytical models of galaxy formation (SAMs), we identify isolated dense groups in 3D real space, containing at least three galaxies. We then build mock redshift space galaxy catalogues and run a Hickson-like CG finder. We find that the Hickson-like algorithm in redshift space is poor at recovering 3D CGs of at least 3 galaxies, with a purity of ∼ 10% and a completeness of ∼ 22%. Among the ∼ 90% of spurious systems, typically 60% are dense structures that failed the 3D isolation criteria, while the remaining 40% are chance alignments of galaxies along the line of sight, nearly all of which are within regular groups, with some variation with the SAM used for the analysis. In other words, while only 10% of CGs are isolated dense groups, as intended, half are dense structures embedded within larger groups, and one-third are chance alignments within larger groups. The low completeness of the extracted CG sample is mainly due to the flux limits of the selection criteria. Our results suggest that a new observational algorithm to identify compact groups in redshift space is required to obtain dense isolated galaxy systems.

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Compact Groups of Galaxies in Sloan Digital Sky Survey and LAMOST Spectral Survey. I. The Catalogs

Cited by 19 publications

References 104 publications

Scaling Properties of Galaxy Groups

Scaling Properties of Galaxy Groups

Galaxy clustering in the VVV Near-IR Galaxy Catalogue

Compact groups from semi-analytical models of galaxy formation -- III: purity and completeness of Hickson-like catalogues

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