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

Old, Lyndsay; Skibba, R.A.; Pearce, Frazer R.; Croton, D.; Muldrew, Stuart I.; Muñoz-Cuartas, J.C.; Gifford, D.; Gray, M.; der Linden, A. von; Mamon, G.A.; Merrifield, Michael R.; Müller, V.; Pearson, R.J.; Ponman, T.J.; Saro, Alexandro; Sepp, T.; Sifón, C.; Tempel, E.; Tundo, E.; Wang, Y.O.; Wojtak, R.

Authors

Lyndsay Old

R.A. Skibba

D. Croton

Stuart I. Muldrew

J.C. Muñoz-Cuartas

D. Gifford

A. von der Linden

G.A. Mamon

V. Müller

R.J. Pearson

T.J. Ponman

Alexandro Saro

T. Sepp

C. Sifón

E. Tempel

E. Tundo

Y.O. Wang

R. Wojtak



Abstract

This paper is the first in a series in which we perform an extensive comparison of various galaxy-based cluster mass estimation techniques that utilize the positions, velocities and colours of galaxies. Our primary aim is to test the performance of these cluster mass estimation techniques on a diverse set of models that will increase in complexity. We begin by providing participating methods with data from a simple model that delivers idealized clusters, enabling us to quantify the underlying scatter intrinsic to these mass estimation techniques. The mock catalogue is based on a Halo Occupation Distribution (HOD) model that assumes spherical Navarro, Frenk and White (NFW) haloes truncated at R₂₀₀, with no substructure nor colour segregation, and with isotropic, isothermal Maxwellian velocities. We find that, above 1014Mʘ, recovered cluster masses are correlated with the true underlying cluster mass with an intrinsic scatter of typically a factor of 2. Below 1014Mʘ, the scatter rises as the number of member galaxies drops and rapidly approaches an order of magnitude. We find that richness-based methods deliver the lowest scatter, but it is not clear whether such accuracy may simply be the result of using an over-simplistic model to populate the galaxies in their haloes. Even when given the true cluster membership, large scatter is observed for the majority non-richness-based approaches, suggesting that mass reconstruction with a low number of dynamical tracers is inherently problematic.

Journal Article Type Article
Publication Date Jun 21, 2014
Journal Monthly Notices of the Royal Astronomical Society
Print ISSN 0035-8711
Electronic ISSN 1365-2966
Publisher Oxford University Press
Peer Reviewed Peer Reviewed
Volume 441
Issue 2
Pages 1513-1536
APA6 Citation Old, L., Skibba, R., Pearce, F. R., Croton, D., Muldrew, S. I., Muñoz-Cuartas, J., …Wojtak, R. (2014). Galaxy cluster mass reconstruction project – I. Methods and first results on galaxy-based techniques. Monthly Notices of the Royal Astronomical Society, 441(2), 1513-1536. https://doi.org/10.1093/mnras/stu545
DOI https://doi.org/10.1093/mnras/stu545
Keywords Methods: numerical - methods: statistical - galaxies: clusters: general - galaxies: haloes - galaxies: kinematics and dynamics - cosmology: observations
Publisher URL http://mnras.oxfordjournals.org/content/441/2/1513
Copyright Statement Copyright information regarding this work can be found at the following address: http://eprints.nottingh.../end_user_agreement.pdf
Additional Information This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.

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Copyright Statement
Copyright information regarding this work can be found at the following address: http://eprints.nottingham.ac.uk/end_user_agreement.pdf





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