Erratum: “Compact Groups of Galaxies in Sloan Digital Sky Survey and LAMOST Spectral Survey. I. The Catalogs” (ApJS, 246, 12)

Zheng, Yun-Liang; Shen, Shiyin

doi:10.3847/1538-4365/ab8acb

Cited by 4 publications

(9 citation statements)

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“…Historically, Hickson (1982) identified 100 CGs from Palomar Observatory Sky Survey, introducing a set of photometric based criteria: 1) richness, 2) isolation, 3) compactness. With the follow-up spectroscopic surveys, redshift information has also been absorbed as a criterion (e.g., Hickson et al 1992;Díaz-Giménez et al 2012;Sohn et al 2015) and optimized for CG selection (Díaz-Giménez et al 2018;Zheng & Shen 2020). In Zheng & Shen (2020, hereafter Paper I), we have identified a large spectroscopically confirmed CG sample via modified Hickson criteria: 1.…”

Section: Introductionmentioning

confidence: 99%

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

Zheng

Shen

2020

ApJS

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Compact group (CG) is a kind of special galaxy system where the galaxy members are separated at the distances of the order of galaxy size. The strong interaction between the galaxy members makes CGs ideal labs for studying the environmental effects on galaxy evolution. Traditional photometric selection algorithm biases against the CG candidates at low redshifts, while spectroscopic identification technique is affected by the spectroscopic incompleteness of sample galaxies and typically biases against the high redshift candidates. In this study, we combine these two methods and select CGs in the main galaxy sample of the Sloan Digital Sky Survey, where we also have taken the advantages of the complementary redshift measurements from the LAMOST spectral and GAMA surveys. We have obtained the largest and most complete CG samples to date. Our samples include 6,144 CGs and 8,022 CG candidates, which are unique in the studies of the nature of the CGs and the evolution of the galaxies inside.

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Section: Introductionmentioning

confidence: 99%

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

Zheng

Shen

2020

ApJS

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“…Since ∼ 13, 000 out of ∼ 37, 000 spectroscopically unmeasured galaxies have achieved new redshifts from SDSS-DR16 (Ahumada et al 2020), GAMA-DR2 (Liske et al 2015), and LAMOST-DR7 (Luo et al 2015), the contamination of the group catalog can be significantly reduced (e.g., Shen et al 2016;Feng et al 2019;Zheng & Shen 2020). Here we use these new redshift measurements to update the sample III of Y07 group catalog.…”

Section: Sample: Groups Of Galaxiesmentioning

confidence: 99%

“…On the other hand, like the size of galaxies, the size (or compactness) of galaxy groups might be another observationally accessible parameter encoding the assembly histories of halos. Indeed, it has long been known that there is a special class of galaxy groups, compact groups of galaxies (CGs), which is defined as a group system containing a few galaxies separated by distance of an order of galaxy size (e.g., Hickson 1982; Barton et al 1996;Díaz-Giménez & Zandivarez 2015;Sohn et al 2015Sohn et al , 2016Díaz-Giménez et al 2018;Zheng & Shen 2020). Because of the observational facts that tidal interactions and mergers frequently appear among CG members, (e.g., Barnes 1989;Amram et al 2004;Coziol & Plauchu-Frayn 2007;Torres-Flores et al 2009, CGs are believed to represent the sites for massive members that are about to merge.…”

Section: Introductionmentioning

confidence: 99%

“…However, we can not distinguish whether this lower dynamical mass state is a result of merging process or the dynamical evolution of post-mergers. In this paper, we expand our studies on CGs (Zheng & Shen 2020 and, for the first time, take the compactness of galaxy groups as a general parameter to explore its correlations with other physical properties of galaxy groups and group members when M h is controlled. Moreover, since the X-ray emission from the intra-group medium con-tains rich information of the dynamical status of galaxy groups, we also, as a first time, compare the X-ray properties of galaxy groups with different compactness using a statistical way in this study.…”

Section: Introductionmentioning

confidence: 99%

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The Compactness of Galaxy Groups in the Sloan Digital Sky Survey

Zheng,

Shen,

Feng

2021

Preprint

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We use an updated version of the halo-based galaxy group catalog of Yang et al., and take surface brightness of galaxy group (µ lim ) based on projected positions and luminosities of galaxy members as a compactness proxy to divide groups into sub-systems with different compactness. By comparing various properties, including galaxy conditional luminosity function, stellar population, AGN activity, and X-ray luminosity of intra-cluster medium of carefully controlled high (HC) and low compactness (LC) group samples, we find that the group compactness plays an essential role in characterizing the detailed physical properties of group themselves and their group members, especially for low mass groups with M h 10 13.5 h −1 M . We find that the low mass HC groups have systematically lower magnitude gap ∆m 12 and X-ray luminosity than their LC counterparts, indicating that the high compactness groups are probably in the early stage of group merging. On the other hand, a higher fraction of passive galaxies is found in HC groups, which however is a result of systematically smaller halo-centric distance distribution of their satellite population. After controlling of both M h and halocentric distance, we do not find any differences on both the quenching faction and AGN activity of the member galaxies between the HC and LC groups. Therefore, we conclude that the halo quenching effect, which makes the halo-centric dependence of galaxy population, is a faster process comparing to the dynamical relaxing time-scale of galaxy groups.

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“…Hence, this effect may not affect our results significantly. In recent years, LAMOST survey has produced a complementary galaxy sample (Luo et al 2015;Shen et al 2016;Zheng &Shen 2020), andLim et al 2017 modified the group finder of Yang et al 2007 with a 100% redshift complementary galaxy sample. These efforts might reduce the impact of fiber-collision effect, but in this paper we still use the Yang et al group catalog.…”

Section: Sdss Dr7 Group Catalogmentioning

confidence: 99%

The formation of blue cluster in local Universe

Wen,

Luo,

Kang

2020

Preprint

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It is well known from the Butcher-Oemler effect that galaxies in dense environment are mostly red with little star formation and the fraction of blue galaxies in galaxy groups/clusters also declines rapidly with redshifts. A recent work by Hashimoto et al. reported a local 'blue cluster' with high fraction of blue galaxies (∼ 0.57), higher than the model predictions. They ascribed this blue cluster to the feeding of gas along a filamentary structure around the cluster. In this work we use group catalog from the Sloan Digital Sky Survey Data Release 7 (SDSS DR7) and the state-of-art of semi-analytic model (SAM) to investigate the formation of blue clusters in local Universe. In total, we find four blue clusters with halo mass ∼ 10 14 M at 0.02 < z < 0.082, while only the one found by Hashimoto et al. is in a filamentary structure. The SAM predicts that blue clusters have later formation time and most blue satellite galaxies are recently accreted. We conclude that the formation of blue clusters is mainly governed by newly accreted blue satellites, rather than the effect of large-scale environment.

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Erratum: “Compact Groups of Galaxies in Sloan Digital Sky Survey and LAMOST Spectral Survey. I. The Catalogs” (ApJS, 246, 12)

Cited by 4 publications

References 0 publications

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

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

The Compactness of Galaxy Groups in the Sloan Digital Sky Survey

The formation of blue cluster in local Universe

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