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

1JHU/STScI HotSci - August 2014

Acknowledgement: We thank Margaret J. Geller, Kenneth Rines, Michael Kurtz, and Antonaldo Diaferio for genorusly providing their redshift data in advance of publication.

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Two different tests for structure formation using galaxy clusters:

1) The mass density profile of clusters - the concentration-mass (C-M) relation (Lemze et al., in preparation).

2) 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).

Outline

3

Clusters of galaxies

sun15142

virvir

gasB

vir

10~/2~)(

km/s1300800 keV,103~

Mpc21~

1000100

MGRRM

Tk

R

N

v

v

MACS1206 at z=0.44Umetsu et al. 2012 Galaxy clusters are the largest

gravitationally bound structures in the universe.

mass contours from joint strong- and weak-lensing analysis

Subaru 5 bands composite color image

4

MACS 0329-0211

Abell 383 Abell 611 Abell 963 Abell 2261

CLJ1226+3332

MACS 0744+3927 MACS 1115+0129 MACS 1206-0847

RXJ 1347-1145 RXJ 1423+2404

MS-2137RXJ 1720+3536 RXJ 2129+0005

MACS 0429-0253

MACS 1311-0310 RXJ 1532+3020

MACS 1931-2634 RXJ 2248-4431

Abell 209

Candidates were taken from:Allen et al. 2004; Schmidt & Allen 2007; Allen et al. 2008; Mantz et al. 2010

Selected to be:- “relaxed”- Tx > 5 keV- have Subaru imaging

20 CLASH clusters were X-ray selected

Images were taken from the Megan Donahue ACCEPT database, see also Donahue et al. 2014

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).

To avoid lensing biastoward high concentrations

JHU/STScI HotSci - August 2014 5

NFW mass profile Navarro, Frenk, & White 1996,1997 2/1/

)(ss

s

rrrrr

Navarro et al. 2004

log r (kpc)

2log

log

srrrd

d

6

In agreement with observations

X-ray Vikhlinin et al. 2006

Galaxy dynaimcs

Lensing

Diaferio, Geller, & Rines 2005Broadhurst et al. 2005

7

s

virvirss r

rCMr ,,

Ludlow et al. 2014

C-M ratio - predicted

8

C-M ratio - observed vs. predicted

Newman et al. 2013

Oguri et al. 2012

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A1689 MS2137

Concentration values

Comerford & Natarajan 2007

JHU/STScI HotSci - August 2014 10

Jeans analysis

)(

)(1)(

2

2

r

rr

r

t

Jeans eq.

Velocity anisotropy

2

22 )()()()(

)(2)()(

r

rnrGMrrn

r

rrrn

dr

d galrgalrgal

R

galgal

Rr

rdrrnR

22

)(2)(

Galaxy surface number density

Projected velocity dispersion

R

rgal

galp

Rr

rdrr

Rrrrn

R22

2

22

2))(1)(()(2

)(

All the 4 free unknowns ( , , , and ) are functions, where M is taken to be NFW.

)(rngal )(rr )(r )( rM

11

The kurtosis

4

4

p

pp

vk

JHU/STScI HotSci - August 2014 12

Removing interlopers using the caustics method

Diaferio & Geller 1997Diaferio 1999

JHU/STScI HotSci - August 2014 13

JHU/STScI HotSci - August 2014 14

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16

C – M relation using galaxy kinematics vs. the theoretical expectation

JHU/STScI HotSci - August 2014

CLASH CharacterizationTheoretical 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.

17

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The selection function

X is a combination of 5 X-ray morphological parameters.

Meneghetti et al. 2014

X

P(X)

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The C – M relation using weak lensing

Umetsu et al. 2014

20

The C – M relation using strong and weak lensing

simobs CC /

Merten et al. 2014

21

Identified halos – overdensity halo finderIdentified halos – FoF halo finder

X-ray peakVirial radius

Bound galaxies

Lemze et al. 2013

22

The differential fraction of cluster mass accreted

Data – Overdensity HFData – FoF HFMS - Genel et al. 2010,WMAP7MS - Genel et al. 2010,WMAP1

Lemze et al. 2013

cluster

halo

M

M

JHU/STScI HotSci - August 2014 23

Conclusions

1) Except for one outlying cluster, our results for the mass-concentration relation derived by using galaxy dynamics are in 1∼ σ 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.

2) 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 1∼ σ agreement with the canonical cosmological model (Lemze et al. 2013).

24JHU/STScI HotSci - August 2014

Future prospects

1) 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.

2) 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

Marc Postman, P.I. Timo AnguitaBegona AscasoItalo Balestra

Matthias BartelmannNarciso “Txitxo” BenitezAndrea BivianoRychard BouwensLarry BradleyThomas BroadhurstJustice BruursemaDan CoeMauricio CarrascoNicole CzakonMegan DonahueThomas EicherKevin FogartyHolland FordBrenda FryeOr GraurGenevieve GravesClaudio GrilloSunil GolwalaAaron HofferØle HostLeopoldo InfanteSaurubh JhaYolanda Jimenez-TejaStéphanie JouvelDaniel KelsonAnton KoekemoerUlricke KuchnerOfer LahavRuth LazkozDoron LemzeDan MaozCurtis McCullyElinor Medezinski

Space Telescope Science Institute (STScI)Universidad Catolica de ChileInstituto de Astrofisica de Andalucia (IAA)Max Plank Institut fur Extraterrestrivhe Physik (MPE)Universität HeidelbergInstituto de Astrofisica de Andalucia (IAA)INAF - OATSLeiden UniversitySTScIUniversity of the Basque CountryThe Johns Hopkins University (JHU)STScIUniversidad Catolica de ChileASIAAMichigan State UniversityUniversitas Sternwarte MunchenThe Johns Hopkins University (JHU)JHUSteward Observatory / U. ArizonaTel Aviv University (TAU)University of California, BerkeleyDark Cosmology CenterCalifornia Institute of TechnologyMichigan State UniversityDark Cosmology CenterUniversidad Católica de ChileRutgers UniversityIAAUCLCarnegie Institute of WashingtonSTScIUniversitat WienUCLUniversity of the Basque CountryJHUTAURutgers UniversityJHU

The CLASH Science Team:

ChileGermanyIsraelItalyNetherlandsSpainSwitzerlandTaiwanU.K.U.S.A.

Part 1

To be continue…

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Peter MelchiorMassimo MeneghettiAmata MercurioJulian MertenAnna MonnaAlberto MolinoJohn MoustakasLeonidas MoustakasMario NonimoSara OgazBrandon PatelEnikö RegösAdam RiessSteve RodneyPiero Rosati P.I. VLTJack SayersIrene SendraStella SeitzRenke SmitLeonardo UbedaKeiichi Umetsu

Alex VianaArjen van der WelBingxiao XuWei ZhengAdi Zitrin

The Ohio State UniversityINAF / Osservatorio Astronomico di BolognaINAF - OACUniversität HeidelbergUniversitas Sternwarte Munchen/MPEIAASiena CollegeJPL/CaltechINAF / Osservatorio Astronomico di BolognaSpace Telescope Science InstituteRutgers UniversityEuropean Laboratory for Particle Physics (CERN)STScI / JHUJHUUniversity of FerraraCalifornia Institute of TechnologyUniversity of the Basque CountryUniversitas Sternwarte MünchenLeiden UniversitySTScIAcademia Sinica, Institute of Astronomy & AstrophysicsSpace Telescope Science InstituteMax Planck Institüt für AstronomieJHUJHUCaltech

The CLASH Science Team:

ChileGermanyIsraelItalyNetherlandsSpainSwitzerlandTaiwanU.K.U.S.A.

Part 2

And friends: Thomas Richardson, Shy Genel, Andrew Newman, David Sand,Maria Pereira, Eiichi Egami

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The End

Thanks for the CLASH team for a few of the slides.

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DM universal density profiles found in simulations

1//2exp)( ss rrr

//1/

)(

ss

s

rrrrr

1,3,1,, NFW Navarro, Frenk, White 1996, 1997

Moore et al. 1999

Generalized NFW, Zhao 1996

Einasto 1965

5.1,3,5.1,,