Stellar population properties of ETGs in compact groups of galaxies

Moura, T. C.; Carvalho, R. R. de; Rembold, Sandro Barboza; Trevisan, M.; Ribeiro, André; Pérez-Villegas, Ángeles; Barbera, F. La; Stalder, D. H.; Rosa, Reinaldo R.

doi:10.1093/mnras/staa386

Cited by 4 publications

(2 citation statements)

References 75 publications

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“…Haynes et al (1984), Gavazzi et al (2006), Boselli et al (2009), andMarasco et al (2016) find that at z = 0, the H i morphology of galaxies are generally perturbed by ram pressure stripping, and that at fixed halo mass, the fraction of satellites devoid of H i decreases as stellar mass increases due to the greater depth of the potential well. Moura et al (2020) infer the loss of ionized gas in galaxies located in compact groups due to their environment, although the effect is small. However, a more recent study in Namiki et al (2021) finds that H i scaling relations are not driven by the environmental density per se.…”

Section: Relationship Between Anomalous Gas and Environmentmentioning

confidence: 99%

A new technique to isolate kinematically anomalous gas in H i data cubes

Randriamiarinarivo

Elson

Baker

2022

Monthly Notices of the Royal Astronomical Society

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H i line observations of nearby galaxies often reveal the presence of extraplanar and/or kinematically anomalous gas that deviates from the general circular flow. In this work, we study the dependence of kinematically anomalous H i gas in galaxies taken from the Simba cosmological simulation on galaxy properties such as H i mass fraction, specific star formation rate, and local environmental density. To identify kinematically anomalous gas, we use a simple yet effective decomposition method to separate it from regularly-rotating gas in the galactic disk; this method is well-suited for application to observational datasets but has been validated here using the simulation. We find that at fixed atomic gas mass fraction, the anomalous gas fraction increases with the specific star formation rate. We also find that the anomalous gas fraction does not have a significant dependence on a galaxy’s environment. Our decomposition method has the potential to yield useful insights from future H i surveys.

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Section: Relationship Between Anomalous Gas and Environmentmentioning

confidence: 99%

A new technique to isolate kinematically anomalous gas in H i data cubes

Randriamiarinarivo

Elson

Baker

2022

Monthly Notices of the Royal Astronomical Society

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“…In this point, López-Cruz et al (2019) applied the stellar population synthesis to disentangle the star formation histories of four galaxy members of the SeyfertâĂŹs Sextet (HCG 79). In that study, they show that it is possible to apply the fossil record to trace the past interactions of galaxy systems by looking into common star formation episodes (Hickson et al 1992;Plauchu-Frayn et al 2012;Moura et al 2020). Hence, the stellar population synthesis is a powerful tool to understand the nature of the galactic systems, uncover their past evolution and demonstrate the past inter-linkage among members of more complex gravitational systems like galaxy groups.…”

Section: Introductionmentioning

confidence: 99%

A spectroscopic study of 14 structures behind Holm15A: Detecting a galaxy group candidate at z=0.58

Ibarra-Medel¹

2022

Preprint

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Holm15A hosts one of the most massive back holes ever known. Hence, it is important to characterize any structure within its core to avoid any wrong association with its central black hole and, therefore, bias any future study. In this work, we present the first identification and characterization of 14 structures hidden behind the surface brightness of Holm15A. We model and subtract the spectral contribution of Holm15A to obtain the spectral information of these structures. We spectroscopically confirm that the 14 objects found are not associated with Holm15A. Ten objects have a well-defined galaxy spectrum from which we implement a fossil record analysis to reconstruct their past evolution. Nine objects are candidates members to be part of a compact galaxy group at redshift 0.5814. We find past mutual interaction among the group candidates that support the scenario of mutual crossings. Furthermore, the fossil reconstruction of the group candidates brings evidence that at least three different merger trees could assemble the galaxy group. We characterize the properties of the galaxy group from which we estimate a lower limit of the scale and mass of this group. We obtain a scale of >146±3 kpc with a dispersion velocity of 622±300 km/s. These estimations consider the lensing effects of the gravitational potential of Holm15A. The other five objects were studied individually. We use public archive data of integral field spectroscopic observations from the Multi-Unit Spectroscopic Explorer instrument.

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Compact groups of galaxies in GAMA

Zandivarez,

Díaz-Giménez,

Taverna

et al. 2024

A&A

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Several compact group catalogues have been constructed over the years using different methods, but most of them are not deep enough to go beyond the very local Universe with a high level of redshift completeness. We build a statistically reliable sample of compact groups to study the influence of its inner extreme environment at intermediate redshifts. We adopted the Galaxy And Mass Assembly (GAMA) redshift survey as a parent galaxy catalogue, complemented with a small sample of galaxies from the Sloan Digital Sky Survey, to identify compact groups using Hickson-like criteria. We explored the parameter space to perform several identifications, with which we built samples with different characteristics. Particularly, we reduced the maximum galaxy separation in the line of sight to 500 km $s^ $, and we implemented different magnitude ranges to define membership: a difference between three, two, or one magnitudes between the brightest galaxy and the other members, and no restriction at all. For comparison, we used control samples extracted from a catalogue of loose groups to compare their properties with those of the compact groups. We built five considerably large compact group samples, ranging from more than 400 up to roughly 2400 systems, and maximum redshifts from 0.2 to 0.4, depending on the selected parameters. The overall properties of each sample agree with previous findings. Moreover, compact groups have a tendency for a larger fraction of quenched galaxies than control loose groups, mainly for galaxies with a low stellar mass in compact groups with short crossing times. In addition, $ 45<!PCT!>$ of the compact groups are embedded in loose galaxy systems and are highly compact, have the shortest crossing times, and the brightest first-ranked galaxies than compact groups that are considered to be non-embedded or isolated. The compact group properties almost do not evolve at all with redshift. Our results confirm previous findings that postulated that compact groups are one of the suitable places in which the suppression of the star formation rate in galaxies that is primarily due to galaxy interactions can be studied. These new Hickson-like compact group samples will be valuable to deepen the analysis of these peculiar galaxy systems in a redshift regime that was poorly explored so far.

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Stellar population properties of ETGs in compact groups of galaxies

Cited by 4 publications

References 75 publications

A new technique to isolate kinematically anomalous gas in H i data cubes

A new technique to isolate kinematically anomalous gas in H i data cubes

A spectroscopic study of 14 structures behind Holm15A: Detecting a galaxy group candidate at z=0.58

Compact groups of galaxies in GAMA

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