Galaxy groups in the low-redshift Universe

Lim, Sangsoo; Mo, H. J.; Lu, Yi; Wang, Huiyuan; Yang, Xiaohu

doi:10.1093/mnras/stx1462

Cited by 133 publications

(195 citation statements)

References 54 publications

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“…Huchra & Geller 1982;Eke et al 2004;Crook et al 2007;Berlind et al 2006;Tempel et al 2014) and iterative halo-based group finders (e.g. Yang et al 2007;Lu et al 2016;Lim et al 2017). Friends-of-friends uses linking lengths: one in sky projection and one in redshift to associate nearby galaxies with one another.…”

Section: Group Cataloguesmentioning

confidence: 99%

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The H i mass function of group galaxies in the ALFALFA survey

Jones

Hess

Adams

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We estimate the H i mass function (HIMF) of galaxies in groups based on thousands of ALFALFA (Arecibo Legacy Fast ALFA survey) H i detections within the galaxy groups of four widely used SDSS (Sloan Digital Sky Survey) groups catalogues. Although differences between the catalogues mean that there is no one definitive group galaxy HIMF, in general we find that the low-mass slope is flat, in agreement with studies based on small samples of individual groups, and that the 'knee' mass is slightly higher than that of the global HIMF of the full ALFALFA sample. We find that the observed fraction of ALFALFA galaxies in groups is approximately 22 per cent. These group galaxies were removed from the full ALFALFA source catalogue to calculate the field HIMF using the remaining galaxies. Comparison between the field and group HIMFs reveals that group galaxies make only a small contribution to the global HIMF as most ALFALFA galaxies are in the field, but beyond the HIMF 'knee' group galaxies dominate. Finally we attempt to separate the group galaxy HIMF into bins of group halo mass, but find that too few low-mass galaxies are detected in the most massive groups to tightly constrain the slope, owing to the rarity of such groups in the nearby Universe where low-mass galaxies are detectable with existing H i surveys.

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Section: Group Cataloguesmentioning

confidence: 99%

“…In this case we restrict the catalogue to 3600 < cz cmb /km s −1 < 15000. Lim et al (2017), hereafter L17, is a improvement on the methodology developed by Y07 to extend it to poor and low mass groups. The paper provides group catalogues for four spectroscopic surveys: 2MRS, 6dFGS (6 degree Field Galaxy Survey), SDSS and 2dFGRS.…”

Section: Yang Et Al Groupsmentioning

confidence: 99%

The H i mass function of group galaxies in the ALFALFA survey

Jones

Hess

Adams

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…where α 0 , α , γ a , γ b and z c are time-independent model parameters. In L14 and L15, both α and γ are chosen to be time-dependent to make the model compatible with the observed galaxy stellar mass functions (GSMFs) at different redshifts and the composite conditional luminosity function of cluster galaxies at redshift z = 0 (see also Lim et al 2017b). All the model parameters are determined by fitting the model predictions to a set of observational data (see the original papers for details).…”

Section: The Empirical Model Of Galaxy Formationmentioning

confidence: 99%

ELUCID. VI. Cosmic Variance of the Galaxy Distribution in the Local Universe

Chen

et al. 2019

ApJ

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Halo merger trees are constructed from ELUCID, a constrained N -body simulation in the Sloan Digital Sky Survey (SDSS) volume. These merger trees are used to populate dark matter halos with galaxies according to an empirical model of galaxy formation. Mock catalogs in the SDSS sky coverage are constructed, which can be used to study the spatial distribution of galaxies in the low-z Universe. These mock catalogs are used to quantify the cosmic variance in the galaxy stellar mass function (GSMF) measured from the SDSS survey. The GSMF estimated from the SDSS magnitude-limited sample can be affected significantly by the presence of the under-dense region at z < 0.03, so that the low-mass end of the function can be underestimated significantly. Several existing methods designed to deal with the effects of the cosmic variance in the estimate of GSMF are tested, and none is found to be able to fully account for the cosmic variance. We propose a method based on the conditional stellar mass functions in dark matter halos, which can provide an unbiased estimate of the global GSMF. The application of the method to the SDSS data shows that the GSMF has a significant upturn at M * < 10 9.5 h −1 M , which has been missed in many earlier measurements of the local GSMF. Subject headings: dark matter -large-scale structure of the universe -galaxies: halos -methods: statistical

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“…To investigate different pathways leading to kinematic misalignment, we must separate galaxies into centrals and satellites. We identify groups with an adaptive halo-based group finder of Yang et al (2005Yang et al ( , 2007 and with improved halo mass assigning techniques (see; Lim et al 2017, for details and application to SDSS). In a nutshell, the group finder uses either the stellar mass or luminosity of central galaxies in addition with the n th brightest/most massive satellite as proxies for halo mass.…”

Section: Group Membershipmentioning

confidence: 99%

“…Galaxies are assigned to groups through an iterative process, where halo properties such as halo size and velocity dispersion are updated until membership converges. Lim et al (2017) do not apply the group finder to the thin strips in the Southern Galatic Cap of SDSS main due to incomplete groups resulting from close proximity to borders. MaNGA galaxies in these strips are therefore unclassified by the group finder, resulting in 5088 matched galaxies with group membership classifications into central or satellite.…”

Section: Group Membershipmentioning

confidence: 99%

Decoupling the rotation of stars and gas – I. The relationship with morphology and halo spin

Duckworth

Tojeiro

Kraljic

2019

Monthly Notices of the Royal Astronomical Society

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We use a combination of data from the MaNGA survey and MaNGA-like observations in IllustrisTNG100 to determine the prevalence of misalignment between the rotational axes of stars and gas. This census paper outlines the typical characteristics of misaligned galaxies in both observations and simulations to determine their fundamental relationship with morphology and angular momentum. We present a sample of ∼ 4500 galaxies from MaNGA with kinematic classifications which we use to demonstrate that the prevalence of misalignment is strongly dependent on morphology. The misaligned fraction sharply increases going to earlier morphologies (28±3% of 301 early-type galaxies, 10±1% of 677 lenticulars and 5.4±0.6% of 1634 pure late-type galaxies). For early-types, aligned galaxies are less massive than the misaligned sample whereas this trend reverses for lenticulars and pure late-types. We also find that decoupling depends on group membership for early-types with centrals more likely to be decoupled than satellites. We demonstrate that misaligned galaxies have similar stellar angular momentum to galaxies without gas rotation, much lower than aligned galaxies. Misaligned galaxies also have a lower gas mass than the aligned, indicative that gas loss is a crucial step in decoupling star-gas rotation. Through comparison to a mock MaNGA sample, we find that the strong trends with morphology and angular momentum hold true in IllustrisTNG100. We demonstrate that the lowered angular momentum is, however, not a transient property and that the likelihood of star-gas misalignment at z = 0 is correlated with the spin of the dark matter halo going back to z = 1.

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Galaxy groups in the low-redshift Universe

Cited by 133 publications

References 54 publications

The H i mass function of group galaxies in the ALFALFA survey

The H i mass function of group galaxies in the ALFALFA survey

ELUCID. VI. Cosmic Variance of the Galaxy Distribution in the Local Universe

Decoupling the rotation of stars and gas – I. The relationship with morphology and halo spin

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