On the weak-lensing masses of a new sample of galaxy groups

González, Elizabeth Hernández; Rodríguez, Facundo; Merchán, Manuel; Lambas, D. García; Makler, M.; Chalela, Martín; Pereira, M. E. S.; Moraes, Bruno; Shan, Huanyuan

doi:10.1093/mnras/stab1168

Cited by 9 publications

(12 citation statements)

References 97 publications

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“…We also compare our results with a recent study of (Gonzalez et al 2021) who identify groups using spectroscopic galaxies from the SDSS-DR12 survey (Rodriguez & Merchán 2020) and carry out a weak lensing study using a heterogenous collection of shear catalogues -CFHTLenS, CS82, RCSLens and KiDS. The green data points represent their median halo-mass constraints with 1𝜎 error bars at a median velocity dispersion value in the corresponding bin.…”

Section: Velocity Dispersion and Halo Mass Relationmentioning

confidence: 76%

“…In their 2015) who used SDSS source galaxies around GAMA groups with at least three members. The green points correspond to more recent weak lensing mass estimates from (Gonzalez et al 2021) for galaxy group sample constructed from the galaxies in SDSS-DR12 and having at least four member galaxies. study, Viola et al (2015) argue that the shallow slope of the scaling relation could be a result of the apparent richness cut of five or more member galaxies that we have used for the selection of GAMA groups to perform such an analysis.…”

Section: Velocity Dispersion and Halo Mass Relationmentioning

confidence: 99%

“…They are an important laboratory to study how different baryonic processes shape the properties of galaxies that reside in these galaxy groups (McCarthy et al 2010;Le Brun et al 2014;Gu et al 2020). Scaling relations between the observable properties of galaxy groups such as their total group luminosity or group velocity dispersion with the halo mass are crucial to develop a phenomenological understanding of galaxy formation within groups (see e.g., Yang et al 2003;Eke et al 2004b;Yang et al 2007;Sheldon et al 2009;Eckmiller et al 2011;Han et al 2015;Viola et al 2015;Lovisari et al 2020Lovisari et al , 2021Gonzalez et al 2021;Yang et al 2021).…”

Section: Introductionmentioning

confidence: 99%

“…The purple data points denote the scaling relation measurements from fig.4ofHan et al (2015) who used SDSS source galaxies around GAMA groups with at least three members. The green points correspond to more recent weak lensing mass estimates from(Gonzalez et al 2021) for galaxy group sample constructed from the galaxies in SDSS-DR12 and having at least four member galaxies.…”

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confidence: 99%

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The Subaru HSC weak lensing mass-observable scaling relations of spectroscopic galaxy groups from the GAMA survey

Rana,

More,

Miyatake

et al. 2021

Preprint

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We utilize the galaxy shape catalogue from the first year data release of the Subaru Hyper Suprime-cam Survey (HSC) to study the dark matter content of galaxy groups in the Universe using weak gravitational lensing. As our lens sample, we use galaxy groups that have been spectroscopically selected from the Galaxy Mass and Assembly (GAMA) galaxy survey in approximately 100 sq. degrees of the sky that overlap with the HSC survey. We restrict our analysis to the 1587 groups with at least five group members. We divide these galaxy groups into six bins each of galaxy group luminosity and group member velocity dispersion and measure the coherent tangential ellipticity pattern on background HSC galaxies imprinted by weak gravitational lensing. We measure the weak lensing signal with a total signal-to-noise ratio of 55 and 51 for these two different selections, respectively. We use a Bayesian halo model framework to infer the halo mass distribution of our galaxy groups binned in the two different observable properties and obtain constraints on the power law scaling relation between mean halo masses and the two group observable properties. We obtain a 5 percent constraint on the amplitude of the scaling relation between halo mass and group luminosity with 𝑀 = (0.81 ± 0.04) × 10 14 ℎ −1 𝑀 for 𝐿 grp = 10 11.5 ℎ −2 𝐿 , and a power law index of 𝛼 = 1.01 ± 0.07. We also obtain a 5 percent constraint on the amplitude of the scaling relation between halo mass and velocity dispersion with 𝑀 = (0.93 ± 0.05) × 10 14 ℎ −1 𝑀 for 𝜎 = 500km s −1 and a power law index 𝛼 = 1.52 ± 0.10, although these scaling relations are sensitive to the exact cuts applied to the number of group members. Comparisons with similar scaling relations from the literature indicate that our results are consistent, but have significantly reduced errors.

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Section: Velocity Dispersion and Halo Mass Relationmentioning

confidence: 76%

Section: Velocity Dispersion and Halo Mass Relationmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

mentioning

confidence: 99%

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The Subaru HSC weak lensing mass-observable scaling relations of spectroscopic galaxy groups from the GAMA survey

Rana,

More,

Miyatake

et al. 2021

Preprint

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“…The galaxy group finder algorithm presented in Rodriguez & Merchán (2020) allows identification systems in large galaxy surveys. This algorithm combines the friends-of-friends (FOF; Huchra & Geller 1982) and halo-based methods (Yang et al 2006) showing a high performance in the study of scaling relations dividing between central and satellite galaxies (Rodriguez et al 2021), in the mass assignment of the dark matter halos of the groups when compared with those got by weak gravitational lensing Gonzalez et al (2021a) and in the studies of the halo occupation distribution in different environments (Alfaro et al 2022). In this work, we propose to identify a new galaxy group sample using the data provided by Sloan Digital Sky Survey Data Release 16 (SDSS DR16, Ahumada et al 2020) to study the alignment following the techniques introduced by Yang et al (2006) and Paz et al (2008) and to compare the results with each other and with other authors.…”

Section: Introductionmentioning

confidence: 99%

Alignment of the central galaxies with the environment

Rodriguez,

Merchán,

Artale

2022

Preprint

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In this work, we combine ellipticity and major axis position angle measurements from the Sloan Digital Sky Server Data Release 16 (SDSS DR16) with the group finder algorithm of Rodriguez & Merchán to determine the alignment of the central galaxies with the surrounding structures and satellite galaxies lying in their group. We use two independent methods: A modified version of the two-point cross-correlation function and the angle between the central galaxy orientation and the satellite galaxies relative position. The first method allows us to study the inner and outer regions of the cluster, while the second method provides information within the halos. Our results show that central galaxies present anysotropy in the correlation function up to ∼ 10ℎ −1 𝑀 𝑝𝑐, which becomes ∼10% stronger for the brightest ones ( 0.1 𝑀 𝑟 < −21.5). When we split the galaxy sample by colour, we find that red central galaxies are the main contributors to this anisotropy. We also show that this behaviour does not depend on the group mass or central galaxy ellipticity. Finally, our results are in agreement with previous findings, showing that the two-point cross-correlation function is a best tracer of the galaxy alignments using all galaxies and not only those of the group to which it belongs. In addition, this feature allows us to explore the behaviour of the alignment on larger scales.

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How galaxies populate halos in extreme density environments: An analysis of the halo occupation distribution in SDSS

Alfaro

Rodríguez

Ruiz

et al. 2022

A&A

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Context. Recent works have shown that the properties of galaxy populations in simulated dark matter halos vary with large-scale environments. These results suggest a variation in the halo occupation distribution (HOD) in extreme density environments since the dynamical and astrophysical conditions prevailing in these regions may significantly affect the formation and evolution of their halos and residing galaxies, influencing the mean number of satellite galaxies. To analyze these effects, we identify cosmic voids and future virialized structures (FVSs) in the Sloan Digital Sky Server Data Release 12 (SDSS-DR12) and estimate the HOD within these super-structures using group catalogs as dark matter halo proxies. Aims. Our goal is to use observational galaxy data to characterize the HOD within cosmic voids and FVSs, explore the different properties of these galaxies' populations, and compare them with the general results outside of these super-structures. Methods. We used a publicly available observational galaxy catalog with information on redshifts, positions, magnitudes, and other astrophysical features to build a volume complete galaxy sample and identify cosmic voids and FVSs. Using a publicly available galaxy group catalog as a proxy to dark matter halos, we computed the HOD within both types of super-structures for different absolute magnitude thresholds. We also studied the dependence of the results on the main void and FVS properties, density, and volume. We also analyzed the main characteristics of the stellar content of galaxies inside these extreme-density regions such as the mean stellar age and the stellar mass. In all cases, we compared the results with those derived from the field sample, defined by objects outside of both types of environments. Results. Inside cosmic voids, we find a strong decrease in the HOD concerning the field results. In the most extreme cases, that is to say groups with masses above ∼ 10 13 h −1 M , the mean number of satellites fall to ∼ 50 percent. Inside FVSs, the HOD shows a significant increase to the field, with a ∼ 40 percent excess in the mean number of satellites for groups with masses around 10 14 h −1 M . These results are present for the different galaxy luminosity ranges explored. In both environments, the differences with respect to the field increases for the extreme values of the density environments. However, we obtain no signs of variations related to intrinsic characteristics of the super-structures, indicating that the effects mainly depend on the density of the large-scale environment. In addition, we find that the cumulative distribution of the mean age of stars of the central galaxy also varies in the different regions; this suggests that the history of the formation of the dark matter halos may be different. Finally, we explore the HOD for the 25% youngest (oldest) galaxies, based on the mean age of their stars. We find that for the low-mass groups the youngest galaxies are only present inside voids, and they are generally central galaxies. On the othe...

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On the weak-lensing masses of a new sample of galaxy groups

Cited by 9 publications

References 97 publications

The Subaru HSC weak lensing mass-observable scaling relations of spectroscopic galaxy groups from the GAMA survey

The Subaru HSC weak lensing mass-observable scaling relations of spectroscopic galaxy groups from the GAMA survey

Alignment of the central galaxies with the environment

How galaxies populate halos in extreme density environments: An analysis of the halo occupation distribution in SDSS

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