Galaxy cluster mass reconstruction project – I. Methods and first results on galaxy-based techniques

Old, Lyndsay; Skibba, Ramin; Pearce, Frazer R.; Croton, Darren J.; Muldrew, Stuart I.; Muñoz-Cuartas, J. C.; Gifford, Daniel; Gray, Meghan E.; Linden, Anja von der; Mamon, G. A.; Merrifield, M. R.; Müller, V.; Pearson, Richard; Ponman, T. J.; Saro, A.; Sepp, T.; Sifón, Cristobál; Tempel, Elmo; Tundo, E.; Wang, Yang; Wojtak, Radosław

doi:10.1093/mnras/stu545

Cited by 71 publications

(66 citation statements)

References 101 publications

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“…This is analogous to what is found by most group mass estimation methods when the group center and its velocity are provided (see Old et al 2014, although Old et al 2015 find that a Bayesian fitted slope of the estimated versus true mass relation is typically unity). Figure 15 shows that MAGGIE and Yang do not underestimate the EG masses of primary fragments as frequently as does the FoF algorithm.…”

Section: Mass Accuracysupporting

confidence: 72%

maggie: Models and Algorithms for Galaxy Groups, Interlopers and Environment

Duarte¹,

Mamon²

2015

Mon. Not. R. Astron. Soc.

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Combining our knowledge of halo structure and internal kinematics from cosmological dark matter simulations and the distribution of halo interlopers in projected phase space measured in cosmological galaxy simulations, we develop MAGGIE, a prior-and halo-based, probabilistic, abundance matching (AM) grouping algorithm for doubly complete subsamples (in distance and luminosity) of flux-limited samples. We test MAGGIE-L and MAGGIE-M (in which group masses are derived from AM applied to the group luminosities and stellar masses, respectively) on groups of at least three galaxies extracted from a mock Sloan Digital Sky Survey Legacy redshift survey, incorporating realistic observational errors on galaxy luminosities and stellar masses. In comparison with the optimal Friends-of-Friends (FoF) group finder, groups extracted with MAGGIE are much less likely to be secondary fragments of true groups; in primary fragments, its galaxy memberships (relative to the virial sphere of the realspace group) are much more complete and usually more reliable, and its masses are much less biased and usually with less scatter, as are its group luminosities and stellar masses (computed in MAGGIE using the membership probabilities as weights). FoF outperforms MAGGIE only for high-mass clusters: for the reliability of the galaxy population and the dispersion of its total mass. In comparison with our implementation of the Yang et al. group finder, MAG-GIE reaches much higher completeness and slightly lower group fragmentation and dispersion on group total masses, luminosities and stellar masses, but slightly greater bias in the latter two and lower reliabilities. MAGGIE should therefore lead to sharper trends of environmental effects on galaxies and more accurate mass/orbit modelling.

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Section: Mass Accuracysupporting

confidence: 72%

maggie: Models and Algorithms for Galaxy Groups, Interlopers and Environment

Duarte¹,

Mamon²

2015

Mon. Not. R. Astron. Soc.

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“…The applied FoF group construction method has been tested on mock galaxy surveys in Nurmi et al (2013) and Old et al (2014). Both papers indicate that the used FoF parameters (LL in radial and transversal direction) provide statistically reliable groups.…”

Section: Flux-limited Galaxy Groups/clustersmentioning

confidence: 99%

“…This increase of the mean distance is an expected effect of a fluxlimited survey. A similar LL determination method was used by Old et al (2014), where various group-finding algorithms (including the one presented here) are compared. Old et al (2014) showed that the groups extracted using such LL strategy are statistically correct and the corresponding group properties are meaningful.…”

Section: Flux-limited Galaxy Groups/clustersmentioning

confidence: 99%

“…Thus several other techniques for group and cluster extraction have been developed, well reviewed by Gal (2006) and recently applied by Yang et al (2005), Koester et al (2007), Yang et al (2007), Hao et al (2010), Makarov & Karachentsev (2011), Wen et al (2012), and Muñoz-Cuartas & Müller (2012). However, whether any method is more reliable than the others is still largely a matter of taste and debate (Old et al 2014).…”

Section: Introductionmentioning

confidence: 99%

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Flux- and volume-limited groups/clusters for the SDSS galaxies: catalogues and mass estimation

Tempel

Tamm

Gramann

et al. 2014

A&A

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230

488

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We provide flux-and volume-limited galaxy group and cluster catalogues based on the spectroscopic sample of the galaxies of SDSS data release 10. We used a modified friends-of-friends method with a variable linking length in the transverse and radial directions to identify as many realistic groups as possible. The flux-limited catalogue incorporates galaxies down to m r = 17.77 mag. It includes 588 193 galaxies and 82 458 groups. The volume-limited catalogues are complete for absolute magnitudes down to M r,lim = −18.0, −18.5, −19.0, −19.5, −20.0, −20.5, and −21.0; the completeness is achieved within different spatial volumes. Our analysis shows that flux-and volume-limited group samples are well compatible, especially for the larger groups/clusters. Dynamical mass estimates based on radial velocity dispersions and group extent in the sky were added to the extracted groups.

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“…A similar procedure to calculate the dynamical mass of the supercluster was used in Einasto et al (2015). The reliability of group mass estimation method and mass errors were analysed in Old et al (2014Old et al ( , 2015, where various mass estimation methods were tested on mock galaxy catalogues. The method used in this work performs reasonably well without a clear bias between true and estimated masses.…”

Section: Masses Of Superclustersmentioning

confidence: 99%

Sloan Great Wall as a complex of superclusters with collapsing cores

Einasto

Lietzen

Gramann

et al. 2016

A&A

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Context. The formation and evolution of the cosmic web is governed by the gravitational attraction of dark matter and antigravity of dark energy (cosmological constant). In the cosmic web, galaxy superclusters or their high-density cores are the largest objects that may collapse at present or during the future evolution. Aims. We study the dynamical state and possible future evolution of galaxy superclusters from the Sloan Great Wall (SGW), the richest galaxy system in the nearby Universe. Methods. We calculated supercluster masses using dynamical masses of galaxy groups and stellar masses of galaxies. We employed normal mixture modelling to study the structure of rich SGW superclusters and search for components (cores) in superclusters. We analysed the radial mass distribution in the high-density cores of superclusters centred approximately at rich clusters and used the spherical collapse model to study their dynamical state. Results. The lower limit of the total mass of the SGW is approximately M = 2.5 × 10 16 h −1 M . Different mass estimators of superclusters agree well, the main uncertainties in masses of superclusters come from missing groups and clusters. We detected three high-density cores in the richest SGW supercluster (SCl 027) and two in the second richest supercluster (SCl 019). They have masses of 1.2−5.9 × 10 15 h −1 M and sizes of up to ≈60 h −1 Mpc. The high-density cores of superclusters are very elongated, flattened perpendicularly to the line of sight. The comparison of the radial mass distribution in the high-density cores with the predictions of spherical collapse model suggests that their central regions with radii smaller than 8 h −1 Mpc and masses of up to M = 2 × 10 15 h −1 M may be collapsing. Conclusions. The rich SGW superclusters with their high-density cores represent dynamically evolving environments for studies of the properties of galaxies and galaxy systems.

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Galaxy cluster mass reconstruction project – I. Methods and first results on galaxy-based techniques

Cited by 71 publications

References 101 publications

maggie: Models and Algorithms for Galaxy Groups, Interlopers and Environment

maggie: Models and Algorithms for Galaxy Groups, Interlopers and Environment

Flux- and volume-limited groups/clusters for the SDSS galaxies: catalogues and mass estimation

Sloan Great Wall as a complex of superclusters with collapsing cores

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