LoCuSS: A Legacy Survey of Galaxy Clusters at z=0.2
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1 LoCuSS: A Legacy Survey of Galaxy Clusters at z=0.2 Graham Smith (PI), Chris Haines (Birmingham); Eiichi Egami, Maria Pereira, Tim Rawle, Marie Rex (Arizona); Sean Moran (JHU); Nobuhiro Okabe (Sinica); Alexis Finoguenov (MPIA), Emily Hardegree-Ullman (RPI) and the LoCuSS team ESLAB Herschel First Results Meeting May
2 Local Cluster Substructure Survey (P.I. Graham Smith) AIM: To understand the impact of recent hierarchical infall history of clusters on their baryonic content -- galaxies and hot intracluster gas. - Observable cluster scaling relations show intrinsic scatter from cluster to cluster. How does this scatter relate to their recent assembly history? - Transformation of infalling galaxies through different environments: field / filaments / groups / cluster cores.
3 Local Cluster Substructure Survey (P.I. Graham Smith) LENSING SUBSTRUCTURE ASSEMBLY HISTORY Smith+2005 Okabe+2010 Smith&Taylor 2008
4 Local Cluster Substructure Survey (P.I. Graham Smith) LENSING SUBSTRUCTURE ASSEMBLY HISTORY Smith+2005 Okabe+2010 Smith&Taylor 2008 Maria J. Pereira, Steward Observatory LoCuSS: Herschel First Results Meeting ~ May
5 LoCuSS: Herschel Key Programme A legacy survey of clusters at z=0.2 Summary of ISO/Spitzer results: ~10 clusters, heterogenous selection: depths, FoV order of magnitude variations in IR populations of galaxies. connection between clustercluster mergers and starburst galaxies? (Geach+ 2006; Haines ; Bekki 2001) A(< r) (deg 2 ) N cum (< r) Need: a large wide field homogenous survey of clusters Radius (Mpc) CL MS CL H emitters (Kodama et al. 2004) CL MS Radius (arcmin) Geach+2006
6 LoCuSS: Herschel Key Programme A legacy survey of clusters at z=0.2 Morphologically unbiased sample: 0.15<z<0.3, -70<dec<+70deg, nh<7e-20cm-2 ROSAT All Sky Survey catalogs: BCS, ebcs, REFLEX 165 clusters with LX>2E44erg/s Huge multi-wavelength effort (30-50% complete): Subaru, HST, Keck,VLT, Gemini, Chandra, XMM, SZA, Palomar, Spitzer (24um), GALEX, Herschel, MMT/Hectospec, KPNO, CTIO, UKIRT
7 LoCuSS: Herschel Key Programme A legacy survey of clusters at z=0.2 Morphologically unbiased sample: 0.15<z<0.3, -70<dec<+70deg, nh<7e-20cm-2 ROSAT All Sky Survey catalogs: BCS, ebcs, REFLEX 165 clusters with LX>2E44erg/s Huge multi-wavelength effort (30-50% complete): Subaru, HST, Keck,VLT, Gemini, Chandra, XMM, SZA, Palomar, Spitzer (24um), GALEX, Herschel, MMT/Hectospec, KPNO, CTIO, UKIRT
8 LoCuSS: Herschel Key Programme A legacy survey of clusters at z=0.2 Relative importance of different environmental processes: galaxy-galaxy mergers 2<ρ3D<10Mpc -3 harassment ~ρgal r 2 ram pressure stripping: to strip the MW (Gunn&Gott 1972) Smith+2010
9 LoCuSS: Herschel Key Programme A legacy survey of clusters at z=0.2 Relative importance of different environmental processes: galaxy-galaxy mergers 2<ρ3D<10Mpc -3 harassment ~ρgal r 2 ram pressure stripping: to strip the MW (Gunn&Gott 1972) Δ(z=0.25) = 120 r200 = 0.75rvir Smith+2010
10 LoCuSS: Herschel Key Programme Strategy Large sample of clusters at low redshift 100/160um observations probe SED peak Probe out to 1.5rvirial A bit more detail: Global SFR (gas supply) is ~2-3 lower at z~ than at z~1, but it is not negligible! Observations at z=0.2 are 5 cheaper than at z=0.8! Optical Butcher Oemler effect shows significant cluster-cluster variations at z~0.2 Currently a large statistical sample is only feasible at z~ clusters ~ galaxies with LIR>5 1010L Observations PACS 100um and 160um 25x25arcmin maps 110 sec on-sky per pixel Total 4.8 hours per cluster Status (as of May 2010) 10 clusters observed, 8 analyzed in survey letter (Smith+ 2010, A&A Special Issue) Abell Haines+ 2010, A&A Special Issue Abell Pereira+ 2010, A&A Special Issue
11 LTIR and dust temperature estimates: 100um, 160um probe the peak of the SED
12 LTIR and dust temperature estimates: 100um, 160um probe the peak of the SED fit Rieke+2009 and Chary&Elbaz+2001 templates, integrate from um to obtain LTIR
13 LTIR and dust temperature estimates: 100um, 160um probe the peak of the SED fit Rieke+2009 and Chary&Elbaz+2001 templates, integrate from um to obtain LTIR
14 LTIR and dust temperature estimates: 100um, 160um probe the peak of the SED fit Rieke+2009 and Chary&Elbaz+2001 templates, integrate from um to obtain LTIR
15 LTIR and dust temperature estimates: 100um, 160um probe the peak of the SED fit Rieke+2009 and Chary&Elbaz+2001 templates, integrate from um to obtain LTIR
16 LTIR and dust temperature estimates: 100um, 160um probe the peak of the SED fit Rieke+2009 and Chary&Elbaz+2001 templates, integrate from um to obtain LTIR
17 LTIR and dust temperature estimates: 100um, 160um probe the peak of the SED fit Rieke+2009 and Chary&Elbaz+2001 templates, integrate from um to obtain LTIR fit modified blackbody to 100 and 160um fluxes, temperatures range from 20K - 50K
18 LTIR and dust temperature estimates: 100um, 160um probe the peak of the SED fit Rieke+2009 and Chary&Elbaz+2001 templates, integrate from um to obtain LTIR fit modified blackbody to 100 and 160um fluxes, temperatures range from 20K - 50K
19 LTIR and dust temperature estimates: 100um, 160um probe the peak of the SED fit Rieke+2009 and Chary&Elbaz+2001 templates, integrate from um to obtain LTIR fit modified blackbody to 100 and 160um fluxes, temperatures range from 20K - 50K
20 LTIR and dust temperature estimates: 100um, 160um probe the peak of the SED fit Rieke+2009 and Chary&Elbaz+2001 templates, integrate from um to obtain LTIR fit modified blackbody to 100 and 160um fluxes, temperatures range from 20K - 50K
21 Far IR Luminosities 220 cluster galaxies with PACS detections Smith+2010
22 Far IR Luminosities 220 cluster galaxies with PACS detections Smith+2010
23 Far IR Luminosities 220 cluster galaxies with PACS detections Smith+2010
24 Far IR Luminosities 220 cluster galaxies with PACS detections Typical galaxy: Lk ~Lk *, LTIR ~ 5x10 10 Smith+2010
25 Far IR Luminosities 220 cluster galaxies with PACS detections Typical galaxy: Lk ~Lk *, LTIR ~ 5x10 10 Smith+2010
26 Far IR Luminosities 220 cluster galaxies with PACS detections Typical galaxy: Lk ~Lk *, LTIR ~ 5x % of galaxies are LIRGs Smith+2010
27 Far IR Luminosities 220 cluster galaxies with PACS detections Typical galaxy: Lk ~Lk *, LTIR ~ 5x % of galaxies are LIRGs Smith+2010
28 Far IR Luminosities 220 cluster galaxies with PACS detections Typical galaxy: Lk ~Lk *, LTIR ~ 5x % of galaxies are LIRGs no ULIRGs Smith+2010
29 Far IR Colors of Cluster Galaxies: Pereira+2010
30 Far IR Colors of Cluster Galaxies: Pereira+2010
31 Far IR Colors of Cluster Galaxies: Pereira+2010
32 Far IR Colors of Cluster Galaxies: Pereira+2010
33 Abell 1763 Abell 1835 Abell 1914 Z7160 Abell 1758 Abell 1689 Abell 2219 Abell 2390 Smith+2010
34 Abell 1763 Abell 1835 Abell 1914 Z7160 Abell 1758 Abell 1689 Abell 2219 Abell 2390 Smith+2010
35 Abell 1763 Abell 1835 Abell 1914 Z7160 Abell 1758 Abell 1689 Abell 2219 Abell 2390 Smith+2010
36 Smith+2010
37 Smith+2010
38 LTIR(< rvir)= ±2.8 Mvir 2.0±0.2 Smith+2010
39 LTIR(< rvir)= ±2.8 Mvir 2.0±0.2. M M 1.1 (McBride +2009) Smith+2010
40 LTIR(< rvir)= ±2.8 Mvir 2.0±0.2. M M 1.1 (McBride +2009) σslope = 0.6 (bootstrap) Smith+2010
41 LTIR(< rvir)= ±2.8 Mvir 2.0±0.2. M M 1.1 (McBride +2009) σslope = 0.6 (bootstrap) cool core, relaxed non cool core, disturbed Smith+2010
42 Far IR Luminosities -- radial profiles Smith+2010
43 Far IR Luminosities -- radial profiles cool core non cc Smith+2010
44 Far IR Luminosities -- radial profiles r200 cool core non cc Smith+2010
45 Far IR Luminosities -- radial profiles r200 cool core non cc Smith+2010
46 Merging in Abell 1835 fc : # of companions within δv < 300km/s δr < 50kpc fc 30 % vs 9 % Pereira+2010
47 Abell 1835 T (K)
48 Abell 1835 Δv (km/s)
49 Abell 1835 Δv (km/s)
50 Abell 1835 Pereira+2010 Luminous infrared galaxies dynamically segregated from the cluster population Infall regions of this massive relaxed cluster are extremely active!
51 Abell 1689 B A C Haines+2010
52 Abell 1689 anisotropic distribution: PKS = 0.96 B A C Haines+2010
53 Abell 1689 B A C Haines+2010
54 Abell 1689 B A C Kawaharada Haines+2010
55 Abell 1689 B A C B A C Kawaharada Haines+2010
56 Abell Herschel & 24um δv (km/s) Relative velocity (km/s) r 500 r vir just 24um neither c.f. Fadda+2009 filament in A Clustercentric radius (Mpc) 3 Haines+2010
57 Abell Herschel & 24um δv (km/s) Relative velocity (km/s) r 500 r vir just 24um neither c.f. Fadda+2009 filament in A r500 2 Clustercentric radius (Mpc) 3 rvir Haines+2010
58 Abell Herschel & 24um δv (km/s) Relative velocity (km/s) r 500 r vir just 24um neither c.f. Fadda+2009 filament in A r500 2 Clustercentric radius (Mpc) 3 rvir Haines+2010
59 Herschel & 24um just 24um Abell 1689 neither g-i g i r 500 r500 Maria J. Pereira, Steward 0 Observatory LoCuSS: Herschel First Results Meeting ~ May r vir rvir c.f. A901/2 STAGES Wolf+ 2005,2009 Haines+2010
60 Herschel & 24um just 24um Abell 1689 neither g-i g i r 500 r500 Maria J. Pereira, Steward 0 Observatory LoCuSS: Herschel First Results Meeting ~ May r vir rvir c.f. A901/2 STAGES Wolf+ 2005,2009 Haines+2010
61 Herschel & 24um just 24um Abell 1689 neither Dusty red galaxies -A(Hα) 2 mag -SSFR M / yr / M g-i g i Blue cloud galaxies -A(Hα) 1 mag -SSFR 3x10-10 M / yr /M 0 r 500 r500 Maria J. Pereira, Steward 0 Observatory LoCuSS: Herschel First Results Meeting ~ May r vir rvir c.f. A901/2 STAGES Wolf+ 2005,2009 Haines+2010
62 Conclusions: - FIR colors of cluster galaxies at z=0.2 differ from local galaxy colors, as captured by CE01 and R09 SED templates -- an environmental effect? - no correlation between cluster dynamical state and total infrared luminosity - radial profiles peak at ~rvir for the cool core clusters, indicating merging may be main driver of induced star formation in clusters - LIR is generally anisotropic: the brightest infrared regions in A1835 and A1689 appear to be associated with filaments which are currently feeding the clusters.
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