Proto-clusters: searches and studies. Bram Venemans (MPIA)
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1 Proto-clusters: searches and studies Bram Venemans (MPIA) Growing up at high redshift: from proto-clusters to galaxy clusters ESAC Madrid September 2012
2 Overview Introduction Finding proto-clusters Characteristics of proto-clusters Proto-cluster galaxies Summary 13/09/2012 Growing-up at high redshift: from proto-clusters to galaxy clusters 2
3 Progenitors of low z massive clusters Properties of clusters in formation Redshift evolution of large scale structures Emergence of red sequence Influence of environment on galaxy properties Many galaxies at single redshift 13/09/2012 Growing-up at high redshift: from proto-clusters to galaxy clusters 3
4 What is a proto-cluster? 13/09/2012 Growing-up at high redshift: from proto-clusters to galaxy clusters 4
5 What is a proto-cluster? Structure of galaxies that will evolve into massive cluster Cluster of galaxies virialized hot gas 13/09/2012 Growing-up at high redshift: from proto-clusters to galaxy clusters 5
6 What is a proto-cluster? Structure of galaxies that will evolve into massive cluster High density of galaxies, clustered in α,δ, z Minimum size 1 physical Mpc Not virialised no extended X-ray emitting gas Red sequence: still forming? 13/09/2012 Growing-up at high redshift: from proto-clusters to galaxy clusters 6
7 What is a proto-cluster? The grey area: 1 z 2 For example: ISCS cluster Stanford+ (2005): - clustering of galaxies in α,δ and z space - 5 members confirmed high redshift cluster of galaxies 13/09/2012 Growing-up at high redshift: from proto-clusters to galaxy clusters 7
8 What is a proto-cluster? The grey area: 1 z 2 For example: ISCS cluster Stanford+ 2005: - clustering of galaxies in α,δ and z space - 5 members confirmed high redshift cluster of galaxies or proto-cluster? 13/09/2012 Growing-up at high redshift: from proto-clusters to galaxy clusters 8
9 What is a proto-cluster? Do we really care? No We can still study the effects of environment on galaxy properties 13/09/2012 Growing-up at high redshift: from proto-clusters to galaxy clusters 9
10 What is a proto-cluster? Structure of galaxies that will evolve into massive cluster High density of (SF) galaxies, clustered in α,δ δ galaxy 2 Minimum size 1 physical Mpc Volume should contain >10 14 M 13/09/2012 Growing-up at high redshift: from proto-clusters to galaxy clusters 10
11 What is a proto-cluster? Structure of galaxies that will evolve into massive cluster High density of (SF) galaxies, clustered in α,δ δ galaxy 2 Minimum size 1 physical Mpc Volume should contain >10 14 M z 2 13/09/2012 Growing-up at high redshift: from proto-clusters to galaxy clusters 11
12 Ways to find proto-clusters Galaxy overdensities in blank fields Galaxies associated with high density tracers 13/09/2012 Growing-up at high redshift: from proto-clusters to galaxy clusters 12
13 Proto-clusters in blank fields Need to probe large volume - small area cover large z range (photo-z) - large area, small z range (e.g. NB imaging) 13/09/2012 Growing-up at high redshift: from proto-clusters to galaxy clusters 13
14 Overdensities in blank fields (I) Lyman alpha emitters at z=5.7 At least two overdensities δ gal >3 Ouchi /09/2012 Growing-up at high redshift: from proto-clusters to galaxy clusters 14
15 Overdensities in blank fields (II) δ gal ~ 7 Steidel Redshift 13/09/2012 Growing-up at high redshift: from proto-clusters to galaxy clusters 15
16 8 Overdensities in blank fields (II) Toshikawa redshift δ gal =16±7 2 1 N υ(km s 1 ) redshift Redshift = 13/09/2012 Growing-up at high redshift: from proto-clusters to galaxy clusters 16
17 Tracers of galaxy overdensities Progenitors of BCGs / massive galaxies / - Quasars - Radio galaxies - Lyman alpha blobs - Sub-millimeter galaxies (SMGs) - 13/09/2012 Growing-up at high redshift: from proto-clusters to galaxy clusters 17
18 Overdensities around SMGs Walter Capak /09/2012 Growing-up at high redshift: from proto-clusters to galaxy clusters 18
19 Overdensities around Lya blobs Prescott δ gal ~2 13/09/2012 Growing-up at high redshift: from proto-clusters to galaxy clusters 19
20 High redshift radio galaxies D. Stern and J. Vernet s talks: - radio galaxies among most massive galaxies - high SF; surrounded by large halos gas Many objects at z > 2, known redshifts - Lyman alpha imaging - H alpha imaging - Broad band imaging straddling break 13/09/2012 Growing-up at high redshift: from proto-clusters to galaxy clusters 20
21 Overdensities around radio galaxies Some results already presented this week Project: radio galaxies for which Lyman alpha imaging was feasible with VLT/FORS2 - overdensity easy to catch - spectroscopy quick - not much contamination 13/09/2012 Growing-up at high redshift: from proto-clusters to galaxy clusters 21
22 field of 1338 at z= spec. members δ gal > 4 6/8 radio galaxies in overdensities 13/09/2012 Growing-up at high redshift: from proto-clusters to galaxy clusters 22
23 Characteristics of proto-clusters (I) Mass M pc = ρ V (1+δ m ) ρ = mean density V = Volume δ m = mass overdensity - related to δ gal via bias parameter + add redshift space distortions 13/09/2012 Growing-up at high redshift: from proto-clusters to galaxy clusters 23
24 Characteristics of proto-clusters (I) Mass - Steidel et al. pc: ~10 15 M - Kang & Im z~3.7 pc: 2-5 x M - Toshikawa z~6 pc: 3 x M - radio galaxy pc: 2-9 x M enough mass for a massive cluster 13/09/2012 Growing-up at high redshift: from proto-clusters to galaxy clusters 24
25 Characteristics of proto-clusters (II) Number density - 1 z~3 LBG pc per 9 x18 field (Steidel+ 1998) n proto-clusters 3x10-6 Mpc -3 - ~1 LAE pc per S-CAM field (Ouchi+ 2005) n proto-clusters 2x10-6 Mpc LBG pc per S-CAM field (Intema+ 2006) n proto-clusters ~ 5x10-6 Mpc -3 13/09/2012 Growing-up at high redshift: from proto-clusters to galaxy clusters 25
26 Characteristics of proto-clusters (II) Number density - # radio galaxies at z>2 + radio lifetime n proto-clusters 6x10-6 Mpc -3 (BV+ 2007) Various surveys: n = few x 10-6 Mpc -3 Locally: comparable to M cluster 2x10 14 M 13/09/2012 Growing-up at high redshift: from proto-clusters to galaxy clusters 26
27 Characteristics of proto-clusters (III) Sizes Shimasaku+ 03 z= cmpc z= cmpc (e.g. Steidel+ 1998, 2005; Shimasaku+ 2003; Hayashino+ 10 cmpc 2004; Ouchi+ 2005; Douglas+ 2010; Toshikawa+ 2012) 13/09/2012 Growing-up at high redshift: from proto-clusters to galaxy clusters 27
28 Characteristics of proto-clusters (III) Sizes MRC , z=2.92 Surface density 7 comoving Mpc BV Proper 1.0 distance (Mpc) /09/2012 Growing-up at high redshift: from proto-clusters to galaxy clusters 28
29 Characteristics of proto-clusters (III) Sizes LAEs and LBGs around radio galaxies: >6-10 cmpc (e.g. Keel+ 1999; Intema+ 2006; BV+ 2007) sizes up to >10 cmpc (> physical Mpc) Consistent with models (e.g. Overzier+ 2009; Y.-K. Chiang s talk) 13/09/2012 Growing-up at high redshift: from proto-clusters to galaxy clusters 29
30 Simulation, z=6.2 Utsumi Overzier /09/2012 Growing-up at high redshift: from proto-clusters to galaxy clusters 30
31 Characteristics of proto-clusters (IV) Velocity dispersion - Expensive - Contamination (field, subgroups) 13/09/2012 Growing-up at high redshift: from proto-clusters to galaxy clusters 31
32 L.O.S. Velocity Dispersion (km/s) Velocity dispersion (km/s) Characteristics of proto-clusters (IV) 1000 Velocity dispersion Chiang et al. in prep /09/2012 Growing-up at high redshift: from proto-clusters to galaxy clusters 32 z Redshift x x M sun M sun > M sun Radio Galaxy Subgroups X-ray Optical H(z)
33 Linear overdensity Redshift 3 z=2.9 2 z=2.2 δ c 1 0 z=3.1 z=2.3 δ c z=4.1 δ L 2 1 δ c δ c δ c Collapse threshold δ c 0 4 z= δ c z=5.2 δ c z=5.7/5.8 δ c R. Overzier PhD thesis /09/2012 Growing-up at high redshift: from proto-clusters to galaxy clusters Redshift Steidel+ 2005
34 Effect of environment on galaxies Already presented in various talks Higher AGN fraction in proto-clusters (e.g. Pentericci+ 2002; Lehmer+ 2009; Digby-North+ 2010) Galaxies older and more massive (e.g. Steidel+ 2005; Hatch+ 2011) 13/09/2012 Growing-up at high redshift: from proto-clusters to galaxy clusters 34
35 Galaxies older and more massive Steidel Age (Gyr) Stellar Mass 13/09/2012 Growing-up at high redshift: from proto-clusters to galaxy clusters 35
36 Summary Caution linking high-z pc with low-z cluster Differences found between pc / field galaxies - in place at high-z, cluster still forming Need large samples to trace redshift evolution 13/09/2012 Growing-up at high redshift: from proto-clusters to galaxy clusters 36
37 End 13/09/2012 Growing-up at high redshift: from proto-clusters to galaxy clusters 37
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