1. Using Spectroscopic Data of Galaxies within and around Galaxy Clusters to Test Structure Formation
Doron Lemze (Johns Hopkins University)
Amata Mercurio, Andrea Biviano, Italo Balestra, Piero Rosati (PI: CLASH-VLT), Mario Nonino, Elinor Medezinski, Marc Postman (PI: CLASH), Thomas Richardson, Holland Ford, Massimo Meneghetti, Keiichi Umetsu, Daniel Kelson, Marisa Girardi, Maria Pereira, Eiichi Egami, with the CLASH and CLASH-VLT teams
Acknowledgement: We thank Margaret J. Geller, Kenneth Rines, Michael Kurtz, and Antonaldo Diaferio for genorusly providing their redshift data in advance of publication.
JHU/STScI HotSci - August 2014

2. JHU/STScI HotSci - August 2014
Outline
Two different tests for structure formation using galaxy clusters:
The mass density profile of clusters - the concentration-mass (C-M) relation (Lemze et al., in preparation).
we provided a new observational test for a key prediction of the ΛCDM cosmological model: the contributions of mergers with different halo-to-cluster mass ratios to cluster-sized halo growth (Lemze et al. 2013).
JHU/STScI HotSci - August 2014

3. Clusters of galaxies Subaru 5 bands composite color image
MACS1206 at z=0.44
Umetsu et al. 2012
Galaxy clusters are the largest gravitationally bound structures in the universe.
mass contours from joint strong- and weak-lensing analysis

4. 20 CLASH clusters were X-ray selected
Selected to be:
“relaxed”
Tx > 5 keV
have Subaru imaging
MACS
Abell 383
Abell 611
Abell 963
Abell 2261
CLJ
MACS
MACS
MACS
RXJ
RXJ
MS-2137
RXJ
RXJ
MACS
MACS
RXJ
MACS
RXJ
Abell 209
To avoid lensing bias toward high concentrations
20 are selected to be “relaxed” clusters (based on their X-ray properties, i.e. smooth and regular surface brightness, and small separation between the BCG and the X-ray peak).
Candidates were taken from:
Allen et al. 2004; Schmidt & Allen 2007; Allen et al. 2008;
Mantz et al. 2010
Images were taken from the Megan Donahue ACCEPT database, see also Donahue et al. 2014

5. JHU/STScI HotSci - August 2014
NFW mass profile
Navarro, Frenk, & White 1996,1997
Navarro et al. 2004
JHU/STScI HotSci - August 2014
log r (kpc)

6. In agreement with observations
X-ray
Vikhlinin et al. 2006
In agreement with observations
Lensing
Galaxy dynaimcs
Diaferio, Geller, & Rines 2005
Broadhurst et al. 2005

7. C-M ratio - predicted
Ludlow et al. 2014

8. C-M ratio - observed vs. predicted
Newman et al. 2013
Oguri et al. 2012

9. JHU/STScI HotSci - August 2014
Concentration values
Comerford & Natarajan 2007
A1689
MS2137
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10. JHU/STScI HotSci - August 2014
Jeans analysis
Jeans eq.
Velocity anisotropy
All the 4 free unknowns ( , , , and ) are functions, where M is taken to be NFW.
Galaxy surface number density
Projected velocity dispersion
JHU/STScI HotSci - August 2014

11. The kurtosis

12. Removing interlopers using the caustics method
Diaferio & Geller 1997
Diaferio 1999
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16. C – M relation using galaxy kinematics vs. the theoretical expectation

17. CLASH Characterization
Theoretical predictions from about 1,400 clusters simulated at high spatial and mass resolution by Meneghetti et al. 14 (MUSIC-2: DM + adiabatic gas)
(M200, c200) measured both in 3D and 2D, taking into account projection effects
The CLASH selection function gives a heterogeneous sample of relaxed (70%) and unrelaxed (30%) clusters
CLASH X-ray selection function taken into account using Chandra X-ray image simulator (X-MAS)
 c200 recovered from the lensing analysis of the CLASH clusters are c=[3-6], with an average value of 3.9 and a standard deviation of 0.6. 
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18. The selection function
X is a combination of 5 X-ray morphological parameters.
P(X) X
Meneghetti et al. 2014
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19. The C – M relation using weak lensing
Umetsu et al. 2014
JHU/STScI HotSci - August 2014

20. The C – M relation using strong and weak lensing
Merten et al. 2014

21. Bound galaxies
Identified halos – overdensity halo finder
Identified halos – FoF halo finder
X-ray peak
Virial radius
Lemze et al. 2013

22. The differential fraction of cluster mass accreted
Data – Overdensity HF
Data – FoF HF
MS - Genel et al. 2010,WMAP7
MS - Genel et al. 2010,WMAP1
WMAP1: Omega_m = 0.25, sigma8 = 0.9
WMAP7: Omega_m = 0.272, sigma8 = 0.807
Sigma8 = 0.82 Bennett et al
Sigma8 = 0.83 Planck
Lemze et al. 2013

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Conclusions
Except for one outlying cluster, our results for the mass-concentration relation derived by using galaxy dynamics are in ∼1σ agreement with the expected relation in ΛCDM cosmology (Lemze et al. 2014, in preparation). The mass-concentration relation based on lensing analysis is in excellent agreement with ΛCDM cosmology.
For the first time, we tested a key outcome in the canonical cosmological model: the contributions of mergers with different mass ratios to cluster-size halos growth. We found ∼1σ agreement with the canonical cosmological model (Lemze et al. 2013).
JHU/STScI HotSci - August 2014

24. JHU/STScI HotSci - August 2014
Future prospects
Comparing (cluster to cluster) dynamical masses with lensing masses
(Merten et al. 2014; Umetsu et al. 2014) and using realistic simulations
(Meneghetti et al. 2014) to better understand the systematics of both
methods.
Apply dynamical and lensing analyses to surveys with a larger number of
clusters, and constrain the cosmological model using the cluster mass
function (i.e. number of clusters in a given mass range).
JHU/STScI HotSci - August 2014

25. JHU/STScI HotSci - August 2014
The CLASH Science Team:
Marc Postman, P.I.
Timo Anguita
Begona Ascaso
Italo Balestra
Matthias Bartelmann
Narciso “Txitxo” Benitez
Andrea Biviano
Rychard Bouwens
Larry Bradley
Thomas Broadhurst
Justice Bruursema
Dan Coe
Mauricio Carrasco
Nicole Czakon
Megan Donahue
Thomas Eicher
Kevin Fogarty
Holland Ford
Brenda Frye
Or Graur
Genevieve Graves
Claudio Grillo
Sunil Golwala
Aaron Hoffer
Øle Host
Leopoldo Infante
Saurubh Jha
Yolanda Jimenez-Teja
Stéphanie Jouvel
Daniel Kelson
Anton Koekemoer
Ulricke Kuchner
Ofer Lahav
Ruth Lazkoz
Doron Lemze
Dan Maoz
Curtis McCully
Elinor Medezinski
Space Telescope Science Institute (STScI)
Universidad Catolica de Chile
Instituto de Astrofisica de Andalucia (IAA)
Max Plank Institut fur Extraterrestrivhe Physik
(MPE)
Universität Heidelberg
INAF - OATS
Leiden University
STScI
University of the Basque Country
The Johns Hopkins University (JHU)
ASIAA
Michigan State University
Universitas Sternwarte Munchen
JHU
Steward Observatory / U. Arizona
Tel Aviv University (TAU)
University of California, Berkeley
Dark Cosmology Center
California Institute of Technology
Universidad Católica de Chile
Rutgers University
IAA
UCL
Carnegie Institute of Washington
Universitat Wien
TAU
Chile
Germany
Israel
Italy
Netherlands
Spain
Switzerland
Taiwan
U.K.
U.S.A.
Part 1
JHU/STScI HotSci - August 2014
To be continue…

26. JHU/STScI HotSci - August 2014
The CLASH Science Team:
Peter Melchior
Massimo Meneghetti
Amata Mercurio
Julian Merten
Anna Monna
Alberto Molino
John Moustakas
Leonidas Moustakas
Mario Nonimo
Sara Ogaz
Brandon Patel
Enikö Regös
Adam Riess
Steve Rodney
Piero Rosati P.I. VLT
Jack Sayers
Irene Sendra
Stella Seitz
Renke Smit
Leonardo Ubeda
Keiichi Umetsu
Alex Viana
Arjen van der Wel
Bingxiao Xu
Wei Zheng
Adi Zitrin
The Ohio State University
INAF / Osservatorio Astronomico di Bologna
INAF - OAC
Universität Heidelberg
Universitas Sternwarte Munchen/MPE
IAA
Siena College
JPL/Caltech
Space Telescope Science Institute
Rutgers University
European Laboratory for Particle Physics (CERN)
STScI / JHU
JHU
University of Ferrara
California Institute of Technology
University of the Basque Country
Universitas Sternwarte München
Leiden University
STScI
Academia Sinica, Institute of Astronomy &
Astrophysics
Max Planck Institüt für Astronomie
Caltech
Chile
Germany
Israel
Italy
Netherlands
Spain
Switzerland
Taiwan
U.K.
U.S.A.
And friends:
Thomas Richardson, Shy Genel, Andrew Newman, David Sand,
Maria Pereira, Eiichi Egami
Part 2
JHU/STScI HotSci - August 2014

27. JHU/STScI HotSci - August 2014
The End
JHU/STScI HotSci - August 2014
Thanks for the CLASH team for a few of the slides.

28. DM universal density profiles found in simulations
Generalized NFW, Zhao 1996
NFW Navarro, Frenk, White 1996, 1997
Moore et al. 1999
Einasto 1965
JHU/STScI HotSci - August 2014