The Seeds of Galaxy Clusters and their Galaxies
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1 The Seeds of Galaxy Clusters and their Galaxies Roderik Overzier Max-Planck Institute for Astrophysics IPMU, Kashiwa, June 28 - July
2 Talk Overview Motivation for Cluster Studies at z>2 Overview of Galaxy Overdensities Observed at High Z Some Successes / Questions Are we missing Progenitors of Massive z~1 clusters? A Simulations Perspective Cosmic Variance and the Progenitor Halos of Clusters Expectations for High Redshift Overdensities Simulating Field and Quasar Environments at z=6 Future Directions
3 Introduction / Motivation Cluster evolution studies limited to z<2, while galaxy studies are at z~8 Cosmological Parameters (Massive) Galaxy Formation (when & how) In General (clusters contain large numbers) Dependence on Environment? Pre-processing? Brightest Cluster Galaxies Assembly History Intra-Cluster Light Supermassive Black Hole & Feedback Metal Enrichment History of the ICM
4 Introduction / Motivation Cluster evolution studies limited to z<2, while galaxy studies are at z~8 Cosmological Parameters (Massive) Galaxy Formation (when & how) In General (clusters contain large numbers) Dependence on Environment? Pre-processing? Brightest Cluster Galaxies Assembly History Intra-Cluster Light Supermassive Black Hole & Feedback Metal Enrichment History of the ICM
5 Introduction / Motivation Cluster evolution studies limited to z<2, while galaxy studies are at z~8 Cosmological Parameters (Massive) Galaxy Formation (when & how) In General (clusters contain large numbers) Dependence on Environment? Pre-processing? Brightest Cluster Galaxies Assembly History Intra-Cluster Light Supermassive Black Hole & Feedback Metal Enrichment History of the ICM
6 Introduction / Motivation Cluster evolution studies limited to z<2, while galaxy studies are at z~8 Cosmological Parameters Massive Galaxy Formation (when & how) In General (clusters contain large numbers) Dependence on Environment? Pre-processing? Brightest Cluster Galaxies Assembly History Intra-Cluster Light Supermassive Black Hole & Feedback Metal Enrichment History of the ICM
7 Introduction / Motivation Cluster evolution studies limited to z<2, while galaxy studies are at z~8 Cosmological Parameters Massive Galaxy Formation (when & how) In General (clusters contain large numbers) Dependence on Environment? Pre-processing? Brightest Cluster Galaxies Assembly History Intra-Cluster Light Supermassive Black Hole & Feedback Metal Enrichment History of the ICM RDCSJ at z = 1.11 [Mei et al. 2006]
8 Introduction / Motivation Cluster evolution studies limited to z<2, while galaxy studies are at z~8 Cosmological Parameters Massive Galaxy Formation (when & how) In General (clusters contain large numbers) Dependence on Environment? Pre-processing? Brightest Cluster Galaxies Assembly History Intra-Cluster Light Supermassive Black Hole & Feedback Metal Enrichment History of the ICM [Rettura et al. 2010ab] RDCSJ at z = 1.11 [Mei et al. 2006]
9 Introduction / Motivation Cluster evolution studies limited to z<2, while galaxy studies are at z~8 [Dekel et al. 2009] Cosmological Parameters Massive Galaxy Formation (when & how) In General (clusters contain large numbers) Dependence on Environment? Pre-processing? Brightest Cluster Galaxies Assembly History Intra-Cluster Light Supermassive Black Hole & Feedback Metal Enrichment History of the ICM RDCSJ at z = 1.11 [Mei et al. 2006]
10 Introduction / Motivation Cluster evolution studies limited to z<2, while galaxy studies are at z~8 Cosmological Parameters Massive Galaxy Formation (when & how) In General (clusters contain large numbers) Dependence on Environment? Pre-processing? Brightest Cluster Galaxies Assembly History Intra-Cluster Light Supermassive Black Hole & Feedback Metal Enrichment History of the ICM [Gonzalez et al. 2005, Tran et al. 2007, Kautsch et al. 2008]
11 Introduction / Motivation Cluster evolution studies limited to z<2, while galaxy studies are at z~8 Cosmological Parameters (Massive) Galaxy Formation (when & how) In General (clusters contain large numbers) Dependence on Environment? Pre-processing? Brightest Cluster Galaxies Assembly History Intra-Cluster Light Supermassive Black Hole & Feedback Metal Enrichment History of the ICM
12 Introduction / Motivation Cluster evolution studies limited to z<2, while galaxy studies are at z~8 Cosmological Parameters (Massive) Galaxy Formation (when & how) In General (clusters contain large numbers) Dependence on Environment? Pre-processing? Brightest Cluster Galaxies Assembly History Intra-Cluster Light Supermassive Black Hole & Feedback Metal Enrichment History of the ICM Forming ICL & Multi-Mergers at z=2.2? [Pentericci et al. 1997; Miley, RO, et al. 2006; Hatch, RO, et al. 2008, 2009]
13 Introduction / Motivation Cluster evolution studies limited to z<2, while galaxy studies are at z~8 Cosmological Parameters (Massive) Galaxy Formation (when & how) In General (clusters contain large numbers) Dependence on Environment? Pre-processing? Brightest Cluster Galaxies Assembly History Intra-Cluster Light Supermassive Black Hole & Feedback Metal Enrichment History of the ICM
14 Introduction / Motivation Cluster evolution studies limited to z<2, while galaxy studies are at z~8 Cosmological Parameters (Massive) Galaxy Formation (when & how) In General (clusters contain large numbers) [Ettori 2005] Dependence on Environment? Pre-processing? Brightest Cluster Galaxies Assembly History Intra-Cluster Light Supermassive Black Hole & Feedback Metal Enrichment History of the ICM
15 Introduction / Motivation Cluster evolution studies limited to z<2, while galaxy studies are at z~8 Cosmological Parameters (Massive) Galaxy Formation (when & how) In General (clusters contain large numbers) [Ettori 2005] Dependence on Environment? Pre-processing? Brightest Cluster Galaxies Assembly History Intra-Cluster Light Supermassive Black Hole & Feedback Metal Enrichment History of the ICM For all of these issues, some very interesting observables lie at much higher redshifts (z>2) than probed with any of the known clusters at z~1
16 Galaxy Overdensities at High Redshift (z=2-6) [Francis+97; Venemans+02,04,05,07; Kurk+02,04; Miley+04,06; Bornancini+06; Intema+06; RO+05,08,09; Kuiper+09; Hatch+09; Steidel+98; Steidel+05; Ota+08; Ouchi+05; Shimasaku+04,05; Matsuda+05; Kodama+07; Kajisawa+06; Zirm+08; Stiavelli+05; Ajiki+06; Kim+08; Zheng+06; Daddi09; Lemaux+09; Utsumi+10,...] Narrow velocity distribution of SF galaxies Evidence for Environmental Effects? [but keep in mind Gabriella De Lucia s comments on nature vs nurture ]
17 Galaxy Overdensities at High Redshift (z=2-6) [Francis+97; Venemans+02,04,05,07; Kurk+02,04; Miley+04,06; Bornancini+06; Intema+06; RO+05,08,09; Kuiper+09; Hatch+09; Steidel+98; Steidel+05; Ota+08; Ouchi+05; Shimasaku+04,05; Matsuda+05; Kodama+07; Kajisawa+06; Zirm+08; Stiavelli+05; Ajiki+06; Kim+08; Zheng+06; Daddi09; Lemaux+09; Utsumi+10,...] Narrow velocity distribution of SF galaxies Evidence for Environmental Effects? [but keep in mind Gabriella De Lucia s comments on nature vs nurture ] Excess AGN? [Pentericci+02; Carilli+02; Overzier+05,Lehmer +09,Digby-North+10]
18 Galaxy Overdensities at High Redshift (z=2-6) [Francis+97; Venemans+02,04,05,07; Kurk+02,04; Miley+04,06; Bornancini+06; Intema+06; RO+05,08,09; Kuiper+09; Hatch+09; Steidel+98; Steidel+05; Ota+08; Ouchi+05; Shimasaku+04,05; Matsuda+05; Kodama+07; Kajisawa+06; Zirm+08; Stiavelli+05; Ajiki+06; Kim+08; Zheng+06; Daddi09; Lemaux+09; Utsumi+10,...] Narrow velocity distribution of SF galaxies Evidence for Environmental Effects? [but keep in mind Gabriella De Lucia s comments on nature vs nurture ] Excess AGN? Excess Age? [Pentericci+02; Carilli+02; Overzier+05,Lehmer +09,Digby-North+10] [Steidel et al. 2005]
19 Galaxy Overdensities at High Redshift (z=2-6) [Francis+97; Venemans+02,04,05,07; Kurk+02,04; Miley+04,06; Bornancini+06; Intema+06; RO+05,08,09; Kuiper+09; Hatch+09; Steidel+98; Steidel+05; Ota+08; Ouchi+05; Shimasaku+04,05; Matsuda+05; Kodama+07; Kajisawa+06; Zirm+08; Stiavelli+05; Ajiki+06; Kim+08; Zheng+06; Daddi09; Lemaux+09; Utsumi+10,...] Narrow velocity distribution of SF galaxies Evidence for Environmental Effects? [but keep in mind Gabriella De Lucia s comments on nature vs nurture ] Excess AGN? Excess Age? Emerging red sequence? [Pentericci+02; Carilli+02; Overzier+05,Lehmer +09,Digby-North+10] [Steidel et al. 2005] [Kurk+04,Kajisawa+06,Kodama+07, Zirm+08, Doherty +10, Galametz+10, Hatch+10,Tanaka+10]
20 Overview of High Redshift Overdensities Number Number Typical error = δgal Redshift
21 Overview of High Redshift Overdensities 7 Number Typical error = Samples: Lyα, LBG, DRG, sub-mm, AGN,... Redshifts: Photo-z or spec-z Areas: ~1-30 arcmin 2 (~1-50 Mpc) MCluster (z=0): ~1-15 x Msun Number δgal Redshift Radio Galaxies Number Quasars Sub-mm Targeted Fields Random
22 Linear Theory Estimates for Evolution Overdensities [RO 2006,2010]
23 Linear Theory Estimates for Evolution Overdensities [RO 2006,2010] Some Conclusions: Large uncertainties Some high-z overdensities turn into virialized clusters at z<1 some not even by z~0... almost none are virialized by z~1 z=1 z=1 z=1
24 Stellar mass budget at z = 4 compared to z = 1.2 Large overdensity TN1338 at z=4: [Overzier et al. 2009] Assumptions: 1. all LBGs in the TN1338 field end up in a cluster 2. LF of LBGs extrapolated faintward to ~0.04L * 3. the UV-selection misses only ~10% at z~4 (Bouwens et al. 2009) Then: TN1338 has MStars! 1x10 12 Mo at z ~ 4
25 Stellar mass budget at z = 4 compared to z = 1.2 Large overdensity TN1338 at z=4: Cluster Cl1252 at z=1.24: versus [Overzier et al. 2009] [Rettura et al. 2010ab] Assumptions: 1. all LBGs in the TN1338 field end up in a cluster 2. LF of LBGs extrapolated faintward to ~0.04L * 3. the UV-selection misses only ~10% at z~4 (Bouwens et al. 2009) Then: TN1338 has MStars! 1x10 12 Mo at z ~ 4
26 Stellar mass budget at z = 4 compared to z = 1.2 Large overdensity TN1338 at z=4: Cluster Cl1252 at z=1.24: formed at z > 4 versus [Overzier et al. 2009] [Rettura et al. 2010ab] Assumptions: 1. all LBGs in the TN1338 field end up in a cluster 2. LF of LBGs extrapolated faintward to ~0.04L * 3. the UV-selection misses only ~10% at z~4 (Bouwens et al. 2009) Then: TN1338 has MStars! 1x10 12 Mo at z ~ 4
27 Stellar mass budget at z = 4 compared to z = 1.2 Large overdensity TN1338 at z=4: Cluster Cl1252 at z=1.24: formed at z > 4 versus [Overzier et al. 2009] [Rettura et al. 2010ab] Assumptions: 1. all LBGs in the TN1338 field end up in a cluster 2. LF of LBGs extrapolated faintward to ~0.04L * 3. the UV-selection misses only ~10% at z~4 (Bouwens et al. 2009) Then: TN1338 has MStars! 1x10 12 Mo at z ~ 4 vs. Cl1252: MStars! 4x10 12 Mo at z > 4 We can account for no more than ~30% of the Cl1252 (stellar) mass
![2005] Millennium Run Simulations 10 10 dark matter particles in a 500 3 h -3 Mpc](/docs-images/81/84518676/images/28-2.jpg "3 box, 64 snapshots between z=127 and z=0 Semi-analytic galaxy formation")
28 Data-mining Clusters in Cosmological Simulations [RO et al. 2009, RO 2010a,b in prep.] z=18 z=6 z=1.4 z=0 [Springel et al. 2005] Millennium Run Simulations dark matter particles in a h -3 Mpc 3 box, 64 snapshots between z=127 and z=0 Semi-analytic galaxy formation [cooling, SF, SN+AGN feedback, chem. enrichment,...] [De Lucia+04, Springel+05, Croton+05, DeLuciaBlaizot07, Guo+10] Ideal for High-z Galaxies: BX/BM galaxies at z~2 [Guo et al. 2009] LBGs at z~3 DRGs at 2<z<4 i -dropouts at z~6 [Overzier et al. 2009] Ideal for Clusters: 2800 Mhalo! h -1 M o clusters 23 Mhalo! h -1 M o clusters Ideal for High-z Galaxy Overdensities
29 The Progenitor Halos of Galaxy Clusters [see also De Lucia & Blaizot 2007]
30 The Progenitor Halos of Galaxy Clusters [see also De Lucia & Blaizot 2007]
31 The Progenitor Halos of Galaxy Clusters Important for Interpretation of the Red Sequence already at z~1! [Sagnard & RO, in prep.] [see also De Lucia & Blaizot 2007]
32 The Progenitor Halos of Galaxy Clusters Important for Interpretation of the Red Sequence already at z~1! [Sagnard & RO, in prep.] Important for Interpretation of High Redshift Galaxy Overdensities! [see also De Lucia & Blaizot 2007]
33 The most massive cluster in the Millennium X-coordinate versus Redshift Projection on the sky at z = 2.07 Redshift 2 1 Y (Mpc/h) 27 x X (Mpc/h) (~3x10 15 Msun at z=0) X (Mpc/h) Create Simulated Multi-Filter Images in prep (in my basement)
34 The Progenitor Overdensities of Galaxy Clusters z = 3.0 Fraction of Regions Field Clusters δgal (Galaxy Overdensity) δm (Dark Matter Overdensity) b = δgal / δm δm Mhalo [see also Suwa, Habe & Yoshikawa 2006]
35 The Progenitor Overdensities of Galaxy Clusters z = 3.0 δgal (Galaxy Overdensity) δm (Mass Overdensity) b = δgal / δm δm Mhalo [see also Suwa, Habe & Yoshikawa 2006]
36 The Progenitor Overdensities of Galaxy Clusters z = 3.0 δgal (Galaxy Overdensity) > MO > MO > MO Field δm (Mass Overdensity) b = δgal / δm δm Mhalo [see also Suwa, Habe & Yoshikawa 2006]
37 The Progenitor Overdensities of Galaxy Clusters z = 3.0 δgal (Galaxy Overdensity) > MO > MO > MO Field Fraction of Real Clusters > MO > MO δm (Mass Overdensity) δgal (Galaxy Overdensity) b = δgal / δm δm Mhalo [see also Suwa, Habe & Yoshikawa 2006]
38 Adjusting selection criteria help to constrain descendant cluster mass SFR-selected galaxies at z=2.5 mass-selected galaxies at z=2.5
39 Adjusting selection criteria help to constrain descendant cluster mass SFR-selected galaxies at z=2.5 mass-selected galaxies at z=2.5 δgal (Galaxy Overdensity) δgal (Galaxy Overdensity)
40 Probability that Structure X evolves into a z=0 cluster of mass Mhalo > Msun, or >10 15 Msun Conclusion: some regions seem alright (Probability = %) while many seem not overdense enough (P = 1-50%)
41 Large Simulated Survey of z~6 i -dropouts [RO+09] z < 27 (AB) i - z > galaxies in 4x4 degrees! gal = [-2, -1, -0.5, 0, +0.5, +1, +2] Contours of surface density contrast "=!- #!$ / #!$ Highlighted are all dropouts that are in the halo merger tree of clusters at z= proto-cluster galaxies (~1/5) UDF GOODS SuprimeCam
42 Large Simulated Survey of z~6 i -dropouts [RO+09] z < 27 (AB) i - z > galaxies in 4x4 degrees! gal = [-2, -1, -0.5, 0, +0.5, +1, +2] Contours of surface density contrast "=!- #!$ / #!$ Highlighted are all dropouts that are in the halo merger tree of clusters at z= proto-cluster galaxies (~1/5) UDF GOODS SuprimeCam
![Large Simulated Survey of z~6 i -dropouts [RO+09] z < 27 (AB) i - z > 1.3 32098 galaxies in 4x4 degrees Contours of surface density contrast "=!- #!$ / #!$! gal = [-2, -1, -0.5, 0, +0.](/docs-images/81/84518676/images/43-2.jpg "5, +1, +2] Hyper- Suprime- Cam Hyper- Suprime- Cam Highlighted are all dropouts that are in the halo merger tree of clusters at z=0 5607 proto-cluster galaxies (~1/5) Hyper- Suprime- Cam Hyper-")
43 Large Simulated Survey of z~6 i -dropouts [RO+09] z < 27 (AB) i - z > galaxies in 4x4 degrees Contours of surface density contrast "=!- #!$ / #!$! gal = [-2, -1, -0.5, 0, +0.5, +1, +2] Hyper- Suprime- Cam Hyper- Suprime- Cam Highlighted are all dropouts that are in the halo merger tree of clusters at z= proto-cluster galaxies (~1/5) Hyper- Suprime- Cam Hyper- Suprime- Cam UDF GOODS SuprimeCam
44 Near Future Strategies for Finding New High-z (Proto-)Clusters for Cosmology and Cluster Galaxy Evolution Studies 1. Large Area Surveying with Matched Filter Techniques X-ray Notes: currently no survey capability (e-rosita,ixo) only virialized cores Optical/IR Wide-Field Imaging Notes: an LBG survey at z~4 with HST covering an area of 300 arcmin 2 (GOODS) will contain about 1 progenitor of a M~5x10 14 Msun z~0 cluster a ~50 square degree survey sensitive to z=2 with Δz~1 will contain about 10 progenitors of z~0 clusters of M~10 15 Msun Sunyaev-Z eldovich Surveys Note: deep enough for (proto-)cluster cores of Mhalo ~ few times Msun at z ~ 2? 2. Suggested Improvements on Targeted Snapshots of Biased Regions Notes: talk to me
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