Galaxy and mass assembly: luminosity and stellar mass functions in GAMA groups

Vázquez-Mata, J. A.; Loveday, Jon; Riggs, Stephen D; Baldry, I. K.; Davies, Luke J. M.; Robotham, Aaron S. G.; Holwerda, Benne W.; Brown, M. J. I.; Cluver, Michelle; Wang, L.; Alpaslan, Mehmet; Bland‐Hawthorn, J.; Brough, Sarah; Driver, Simon P.; Hopkins, A. M.; Taylor, Edward N.; Wright, Angus H.

doi:10.1093/mnras/staa2889

Cited by 18 publications

(10 citation statements)

References 101 publications

(176 reference statements)

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“…It also provides reliable measurements of absolute magnitudes in a wide wavelength range, stellar masses and SFR. The GAMA survey has been used for various aspects of environmental effects, in particular the impact of group, cluster, local, and large-scale environment on galaxy properties (Wijesinghe et al 2012;Burton et al 2013;Brough et al 2013;McNaught-Roberts et al 2014;Alpaslan et al 2015;Davies et al 2016;Schaefer et al 2017;Grootes et al 2017;Barsanti et al 2018;Wang et al 2018;Davies et al 2019a,b;Schaefer et al 2019;Vázquez-Mata et al 2020).…”

Section: Introductionmentioning

confidence: 99%

Galaxy and Mass Assembly (GAMA)

Sureshkumar

Durkalec

Pollo

et al. 2021

A&A

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Context. Galaxies are biased tracers of the underlying network of dark matter. The strength of this bias depends on various galaxy properties, as well as on redshift. One of the methods used to study these dependences of the bias are measurements of galaxy clustering. Such studies are made using galaxy samples from various catalogues -frequently bearing their own problems related to sample selection methods. It is therefore crucial to understand how sample choice influences the clustering measurements, and which galaxy property is the most direct tracer of the galaxy environment. Aims. We investigate how different galaxy properties -luminosities in u, g, r, J, K-bands, stellar mass, star formation rate and specific star formation rate trace the environment in the local universe. We also study the effect of survey flux limits on galaxy clustering measurements. Methods. We measure the two-point correlation function (2pCF) and marked correlation functions (MCFs) using the aforementioned properties as marks. We use nearly stellar-mass-complete galaxy sample in the redshift range 0.1 < z < 0.16 from the Galaxy And Mass Assembly (GAMA) survey with a flux limit of r < 19.8. Further, we impose a brighter flux limit of r < 17.8 to our sample and repeat the measurements to study how this affects galaxy clustering analysis. We compare our results to measurements from the Sloan Digital Sky Survey (SDSS) with flux limits of r < 17.8 and r < 16.8. Results. We show that the stellar mass is the most direct tracer of galaxy environment, the K-band luminosity being a good substitute, although such a proxy sample misses close pairs of evolved, red galaxies. We also show that the u-band luminosity can be a proxy of star formation rate in the context of galaxy clustering. We observe an effect of the survey flux limit on clustering studies -samples with a higher flux limit (smaller magnitude) miss some information about close pairs of starburst galaxies.

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Section: Introductionmentioning

confidence: 99%

Galaxy and Mass Assembly (GAMA)

Sureshkumar

Durkalec

Pollo

et al. 2021

A&A

Self Cite

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“…As shown in Figure 7, our integrated satellite counts are very tightly bracketed by the corresponding predicted counts in the TNG100 and TNG300 simulations, where we select satellites at projected distances of < 400 kpc for hosts with M200 = 10 13−14 h −1 M . In addition, we compare to the observed satellite mass function from Yang et al (2008Yang et al ( , 2009, based on a sample of spectroscopically-confirmed satellites in ∼ 300,000 low-z groups (see also Vázquez-Mata et al 2020). Overall, our measured satellite mass function is in remarkably good agreement, especially at low masses (or faint magnitudes).…”

Section: Statistical Background Subtractionmentioning

confidence: 68%

A Machine Learning Approach to Measuring the Quenched Fraction of Low-Mass Satellites Beyond the Local Group

Baxter,

Cooper,

Fillingham

2021

Preprint

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Observations suggest that satellite quenching plays a major role in the buildup of passive, low-mass galaxies at late cosmic times. Studies of low-mass satellites, however, are limited by the ability to robustly characterize the local environment and star-formation activity of faint systems. In an effort to overcome the limitations of existing data sets, we utilize deep photometry in Stripe 82 of the Sloan Digital Sky Survey, in conjunction with a neural network classification scheme, to study the suppression of star formation in low-mass satellite galaxies in the local Universe. Using a statistically-driven approach, we are able to push beyond the limits of existing spectroscopic data sets, measuring the satellite quenched fraction down to satellite stellar masses of ∼10 7 M in group environments (M halo = 10 13−14 h −1 M ). At high satellite stellar masses ( 10 10 M ), our analysis successfully reproduces existing measurements of the quenched fraction based on spectroscopic samples. Pushing to lower masses, we find that the fraction of passive satellites increases, potentially signaling a change in the dominant quenching mechanism at M ∼ 10 9 M . Similar to the results of previous studies of the Local Group, this increase in the quenched fraction at low satellite masses may correspond to an increase in the efficacy of ram-pressure stripping as a quenching mechanism in groups.

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“…the linear ratio between the total r-band flux from a Sérsic profile fit cut at 10 effective radii and the r-band AUTO aperture flux (see also, e.g. Taylor et al 2011;Kelvin et al 2014;Lange et al 2016;Vázquez-Mata et al 2020). The stellar masses are calculated by assuming concordance cosmology with the cosmological parameters being Ω m,0 = 0.3, Ω Λ,0 = 0.7, and h = 0.7 (Taylor et al 2011).…”

Section: Gama Surveymentioning

confidence: 99%

The High Fraction of Thin Disk Galaxies Continues to Challenge ΛCDM Cosmology

Haslbauer,

Banik,

Kroupa

et al. 2022

Preprint

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Any viable cosmological framework has to match the observed proportion of early-and late-type galaxies. In this contribution, we focus on the distribution of galaxy morphological types in the standard model of cosmology (Lambda cold dark matter, ΛCDM). Using the latest state-of-the-art cosmological ΛCDM simulations known as Illustris, IllustrisTNG, and EAGLE, we calculate the intrinsic and sky-projected aspect ratio distribution of the stars in subhalos with stellar mass M * > 10 10 M at redshift z = 0. There is a significant deficit of intrinsically thin disk galaxies, which however comprise most of the locally observed galaxy population. Consequently, the sky-projected aspect ratio distribution produced by these ΛCDM simulations disagrees with the Galaxy And Mass Assembly (GAMA) survey and Sloan Digital Sky Survey at ≥ 12.52σ (TNG50-1) and ≥ 14.82σ (EAGLE50) confidence. The deficit of intrinsically thin galaxies could be due to a much less hierarchical mergerdriven build-up of observed galaxies than is given by the ΛCDM framework. It might also arise from the implemented sub-grid models, or from the limited resolution of the above-mentioned hydrodynamical simulations. We estimate that an 8 5 times better mass resolution realization than TNG50-1 would reduce the tension with GAMA to the 5.58σ level. Finally, we show that galaxies with fewer major mergers have a somewhat thinner aspect ratio distribution. Given also the high expected frequency of minor mergers in ΛCDM, the problem may be due to minor mergers. In this case, the angular momentum problem could be alleviated in Milgromian dynamics (MOND) because of a reduced merger frequency arising from the absence of dynamical friction between extended dark matter halos.

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Galaxy and mass assembly: luminosity and stellar mass functions in GAMA groups

Cited by 18 publications

References 101 publications

Galaxy and Mass Assembly (GAMA)

Galaxy and Mass Assembly (GAMA)

A Machine Learning Approach to Measuring the Quenched Fraction of Low-Mass Satellites Beyond the Local Group

The High Fraction of Thin Disk Galaxies Continues to Challenge ΛCDM Cosmology

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