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HeCS-SZ: An MMT/Hectospec Survey of SZ-selected Clusters Ken Rines (Western Washington University), Margaret Geller (SAO), Antonaldo Diaferio (Torino),

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Presentation on theme: "HeCS-SZ: An MMT/Hectospec Survey of SZ-selected Clusters Ken Rines (Western Washington University), Margaret Geller (SAO), Antonaldo Diaferio (Torino),"— Presentation transcript:

1 HeCS-SZ: An MMT/Hectospec Survey of SZ-selected Clusters Ken Rines (Western Washington University), Margaret Geller (SAO), Antonaldo Diaferio (Torino), Ho Seong Hwang (KIAS) 5 November 2014 Ken Rines (Western Washington University), Margaret Geller (SAO), Antonaldo Diaferio (Torino), Ho Seong Hwang (KIAS) 5 November 2014

2 Hectospec Cluster Survey (HeCS) Massive clusters Infall regions (FoV is 3-6 Mpc at z=0.1-0.3) SDSS+RASS (BCS/REFLEX) Selection sim. to LoCUSS Survey volume~10 8 Mpc 3 (10x CIRS volume) 58 clusters Target red sequence 22,680 new redshifts 10,145 cluster members Massive clusters Infall regions (FoV is 3-6 Mpc at z=0.1-0.3) SDSS+RASS (BCS/REFLEX) Selection sim. to LoCUSS Survey volume~10 8 Mpc 3 (10x CIRS volume) 58 clusters Target red sequence 22,680 new redshifts 10,145 cluster members Z LXLX CIRS: SDSS+RASS, z<0.1 (Rines & Diaferio 2006, see also Andreon 2010: mass-richness)

3 HeCS Science Goals Scaling relations M vir,  p, M ★, Y X, Y SZ, M lens M vir vs Y SZ (Rines et al. 2010) M vir vs M WL (Geller et al. 2013) Evolution of Cluster Galaxies to 5r 200 Colors, D4000 Mass function (  m,  8 ) BCG Dynamics Lensing: substructure, dilution Mass profiles to 5r 200 Ultimate halo masses (Rines et al. 2013) Scaling relations M vir,  p, M ★, Y X, Y SZ, M lens M vir vs Y SZ (Rines et al. 2010) M vir vs M WL (Geller et al. 2013) Evolution of Cluster Galaxies to 5r 200 Colors, D4000 Mass function (  m,  8 ) BCG Dynamics Lensing: substructure, dilution Mass profiles to 5r 200 Ultimate halo masses (Rines et al. 2013) Hectospec: 300 fibers, 1° diameter MMT 6.5m

4 HeCS: Infall Patterns Clean Infall Regions High contrast Median 200 members  p ~ 500-1200 km/s Ordered by L X Scatter in L X -  p Cooling cores, AGN l.o.s. structure Clean Infall Regions High contrast Median 200 members  p ~ 500-1200 km/s Ordered by L X Scatter in L X -  p Cooling cores, AGN l.o.s. structure vv R p (Mpc/h)

5 HeCS: Infall Patterns vv R p (Mpc/h) Clean Infall Regions High contrast Median 200 members  p ~ 500-1200 km/s Ordered by L X Scatter in L X -  p Cooling cores, AGN l.o.s. structure Double cluster: MS0906/A750 Clean Infall Regions High contrast Median 200 members  p ~ 500-1200 km/s Ordered by L X Scatter in L X -  p Cooling cores, AGN l.o.s. structure Double cluster: MS0906/A750

6 HeCS: Infall Patterns vv R p (Mpc/h) Clean Infall Regions High contrast Median 200 members  p ~ 500-1200 km/s Ordered by L X Scatter in L X -  p Cooling cores, AGN l.o.s. structure Clean Infall Regions High contrast Median 200 members  p ~ 500-1200 km/s Ordered by L X Scatter in L X -  p Cooling cores, AGN l.o.s. structure

7 HeCS: Infall Patterns vv R p (Mpc/h) Clean Infall Regions High contrast Median 200 members  p ~ 500-1200 km/s Ordered by L X Scatter in L X -  p Cooling cores, AGN l.o.s. structure Clean Infall Regions High contrast Median 200 members  p ~ 500-1200 km/s Ordered by L X Scatter in L X -  p Cooling cores, AGN l.o.s. structure

8 HeCS: Infall Patterns vv R p (Mpc/h) Clean Infall Regions High contrast Median 200 members  p ~ 500-1200 km/s Ordered by L X Scatter in L X -  p Cooling cores, AGN l.o.s. structure Clean Infall Regions High contrast Median 200 members  p ~ 500-1200 km/s Ordered by L X Scatter in L X -  p Cooling cores, AGN l.o.s. structure

9 HeCS: Mass Profiles Caustic mass profiles Radii up to 6 Mpc/h  p ~ 500-1200 km/s M ~ 10 15 M  /h Green: M virial (r) for r 500 -r 100 Virial/caustic masses agree (sanity check) Caustic mass profiles Radii up to 6 Mpc/h  p ~ 500-1200 km/s M ~ 10 15 M  /h Green: M virial (r) for r 500 -r 100 Virial/caustic masses agree (sanity check) M(<R) R p (Mpc/h)

10 HeCS: Caustics vs Lensing Neither requires equilibrium Caustics should overestimate at small radius (known systematic) Lensing could overestimate at large radius (l.o.s. structure) 19 clusters (Okabe+10, others) M WL 15-25% low? Neither requires equilibrium Caustics should overestimate at small radius (known systematic) Lensing could overestimate at large radius (l.o.s. structure) 19 clusters (Okabe+10, others) M WL 15-25% low? Geller et al 2013

11 HeCS: Stacked Clusters Projection effects dominate systematics Quartiles by M 200 and L X (no caustics) Works in simulations (Serra et al 2011) Clean Infall Regions Caustic mass profiles Projection effects dominate systematics Quartiles by M 200 and L X (no caustics) Works in simulations (Serra et al 2011) Clean Infall Regions Caustic mass profiles vv R p (Mpc/h)

12 HeCS: Stacked Clusters Density profiles Larger-L X quartiles have larger  Dynamic range of ~10 4  critical at max. radius Singular isothermal sphere ruled out Density profiles Larger-L X quartiles have larger  Dynamic range of ~10 4  critical at max. radius Singular isothermal sphere ruled out  R p (Mpc/h)

13 HeCS: Stacked Clusters Density profiles 4 orders of magnitude Singular isothermal sphere ruled out Agrees well with NFW (even outside r 200 ) Incomplete at R>3 Mpc Comparison to lensing X-ray-selected: NFW c=2.9 (Okabe et al 2010) Lensing-selected: NFW c=6.3 (Umetsu et al 2011) Density profiles 4 orders of magnitude Singular isothermal sphere ruled out Agrees well with NFW (even outside r 200 ) Incomplete at R>3 Mpc Comparison to lensing X-ray-selected: NFW c=2.9 (Okabe et al 2010) Lensing-selected: NFW c=6.3 (Umetsu et al 2011)  R p (Mpc/h)

14 HeCS: Density Profiles Density profiles NFW at R<2 Mpc Steeper at R>2-3 Mpc? Range of >10 3  critical at max. radius Singular isothermal sphere ruled out Cumulative Density profiles Similar to NFW Incomplete at R>3 Mpc Max. bound radius: r 5.6 Density profiles NFW at R<2 Mpc Steeper at R>2-3 Mpc? Range of >10 3  critical at max. radius Singular isothermal sphere ruled out Cumulative Density profiles Similar to NFW Incomplete at R>3 Mpc Max. bound radius: r 5.6  (<r) R p (Mpc/h)  M 200 LXLX

15 Ultimate Halo Mass  CDM cosmology predicts halos stop growing, become increasingly isolated Cluster mass at a=100 is about 2.2 M 200 (a=1) (Busha et al 2005) Limit: r 5.6 (enclosed density = 9  2 /16  critical Prediction seconded (Dunner et al 2006)  CDM cosmology predicts halos stop growing, become increasingly isolated Cluster mass at a=100 is about 2.2 M 200 (a=1) (Busha et al 2005) Limit: r 5.6 (enclosed density = 9  2 /16  critical Prediction seconded (Dunner et al 2006) a=1 a=100a=11 a=100 (comoving) Busha et al 2003

16 Ultimate Halo Mass  CDM cosmology predicts halos stop growing, become increasingly isolated Cluster mass at a=100 is about 2.2 M 200 (a=1) (Busha et al 2005) HeCS measurement 33 clusters have caustics out to r 5.6 M 5.6 /M 200 =1.99±0.11 Similar dispersion  CDM cosmology predicts halos stop growing, become increasingly isolated Cluster mass at a=100 is about 2.2 M 200 (a=1) (Busha et al 2005) HeCS measurement 33 clusters have caustics out to r 5.6 M 5.6 /M 200 =1.99±0.11 Similar dispersion M 5.6 /M 200 M 200 (M  /h)

17 HeCS Science Goals Scaling relations M vir,  p, M ★, Y X, Y SZ, M lens M vir vs Y SZ (Rines et al. 2010) M vir vs M WL (Geller et al. 2013) Evolution of Cluster Galaxies to 5r 200 Colors, D4000 Mass function (  m,  8 ) BCG Dynamics Lensing: substructure, dilution (Coe+2012, Geller+13, Hwang+14) Mass profiles to 5r 200 Ultimate halo masses (Rines et al. 2013) Scaling relations M vir,  p, M ★, Y X, Y SZ, M lens M vir vs Y SZ (Rines et al. 2010) M vir vs M WL (Geller et al. 2013) Evolution of Cluster Galaxies to 5r 200 Colors, D4000 Mass function (  m,  8 ) BCG Dynamics Lensing: substructure, dilution (Coe+2012, Geller+13, Hwang+14) Mass profiles to 5r 200 Ultimate halo masses (Rines et al. 2013) Hectospec: 300 fibers, 1° diameter MMT 6.5m

18 Planck: SZ vs CMB Planck CMB constraints disagree with Planck SZ results Blue: SZ mass function with M HS =0.8M true Red: Planck CMB Black: SZ mass function, free normalization: M HS =0.59M true Alternate explanations: neutrino masses Planck CMB constraints disagree with Planck SZ results Blue: SZ mass function with M HS =0.8M true Red: Planck CMB Black: SZ mass function, free normalization: M HS =0.59M true Alternate explanations: neutrino masses 88 mm Planck Collaboration 2013 XX.

19 HeCS: SZ vs Dynamics Scaling of M vir -Y SZ Published SZA data for 15 clusters (Bonamente+08; Marrone+09) Strong correlation (99.8%) Significant scatter Connection to  8 debate? Larger samples needed Scaling of M vir -Y SZ Published SZA data for 15 clusters (Bonamente+08; Marrone+09) Strong correlation (99.8%) Significant scatter Connection to  8 debate? Larger samples needed Rines et al. 2010 M vir pp Y SZ

20 SZ vs Dynamics: ACT, SPT Scaling of  p -Y SZ VLT/Gemini spectroscopic followup of ACT-detected clusters (Sifon et al 2013) z=0.3-1.1 Cluster evolution? Cluster selection? Scaling of  p -Y SZ VLT/Gemini spectroscopic followup of ACT-detected clusters (Sifon et al 2013) z=0.3-1.1 Cluster evolution? Cluster selection? pp Y SZ Gemini spectroscopic followup of SPT-detected clusters (Ruel et al 2014) z=0.3-1.5 Substantial scatter Velocity bias? (  gxy ~1.1  DM or M vir ~1.3M true ) Gemini spectroscopic followup of SPT-detected clusters (Ruel et al 2014) z=0.3-1.5 Substantial scatter Velocity bias? (  gxy ~1.1  DM or M vir ~1.3M true ) pp M SZ

21 HeCS-SZ: Planck-selected sample Massive clusters Planck clusters with SDSS DR10 imaging Many in HeCS/CIRS 115 clusters (80 in SZ- complete subsample) 8200 new redshifts in 24 clusters (z<0.2) Massive clusters Planck clusters with SDSS DR10 imaging Many in HeCS/CIRS 115 clusters (80 in SZ- complete subsample) 8200 new redshifts in 24 clusters (z<0.2) Z Rines et al. in prep

22 HeCS-SZ: Infall Patterns vv R p (Mpc/h) Clean Infall Regions High contrast Median 200 members  p ~ 500-1200 km/s Ordered by M SZ Scatter in M SZ -  p l.o.s. structure Clean Infall Regions High contrast Median 200 members  p ~ 500-1200 km/s Ordered by M SZ Scatter in M SZ -  p l.o.s. structure

23 HeCS-SZ: Infall Patterns vv R p (Mpc/h) Clean Infall Regions High contrast Median 200 members  p ~ 500-1200 km/s Ordered by M SZ Scatter in M SZ -  p l.o.s. structure Clean Infall Regions High contrast Median 200 members  p ~ 500-1200 km/s Ordered by M SZ Scatter in M SZ -  p l.o.s. structure

24 HeCS-SZ: Infall Patterns vv R p (Mpc/h) Clean Infall Regions High contrast Median 200 members  p ~ 500-1200 km/s Ordered by M SZ Scatter in M SZ -  p l.o.s. structure Clean Infall Regions High contrast Median 200 members  p ~ 500-1200 km/s Ordered by M SZ Scatter in M SZ -  p l.o.s. structure

25 HeCS-SZ: Infall Patterns vv R p (Mpc/h) Clean Infall Regions High contrast Median 200 members  p ~ 500-1200 km/s Ordered by M SZ Scatter in M SZ -  p l.o.s. structure Clean Infall Regions High contrast Median 200 members  p ~ 500-1200 km/s Ordered by M SZ Scatter in M SZ -  p l.o.s. structure

26 HeCS-SZ: Scaling Relation Scaling of  p -Y SZ Published Planck data for 115 clusters (Planck 2013 XXIX) Strong correlation Significant scatter Bayesian fit:  p at fixed Y SZ Scaling of  p -Y SZ Published Planck data for 115 clusters (Planck 2013 XXIX) Strong correlation Significant scatter Bayesian fit:  p at fixed Y SZ pp Y SZ Rines et al. in prep.

27 HeCS-SZ: Scaling Relation Scaling of  p -Y SZ Published Planck data for 115 clusters (Planck 2013 XXIX) Strong correlation Significant scatter Bayesian fit:  p at fixed Y SZ Dotted: Rines+10 ‘shallow’ Y-  no longer good fit Scaling of  p -Y SZ Published Planck data for 115 clusters (Planck 2013 XXIX) Strong correlation Significant scatter Bayesian fit:  p at fixed Y SZ Dotted: Rines+10 ‘shallow’ Y-  no longer good fit pp Y SZ Rines et al. in prep.

28 HeCS-SZ: Scaling Relation Scaling of  p -Y SZ Published Planck data for 115 clusters (Planck 2013 XXIX) Strong correlation Significant scatter Bayesian fit:  p at fixed Y SZ Dashed: Evrard+08 M-  plus Planck Y-M (2013 XX) Scaling of  p -Y SZ Published Planck data for 115 clusters (Planck 2013 XXIX) Strong correlation Significant scatter Bayesian fit:  p at fixed Y SZ Dashed: Evrard+08 M-  plus Planck Y-M (2013 XX) pp Y SZ Rines et al. in prep.

29 HeCS-SZ: Scaling Relation Scaling of  p -Y SZ Published Planck data for 115 clusters (Planck 2013 XXIX) Strong correlation Significant scatter Bayesian fit:  p at fixed Y SZ Dashed: Evrard+08 M-  plus Planck Y-M (2013 XX) Large mass bias (67%) to reconcile w/Planck-CMB not favored Requires  gxy ~0.83  DM or M vir ~0.6M true Scaling of  p -Y SZ Published Planck data for 115 clusters (Planck 2013 XXIX) Strong correlation Significant scatter Bayesian fit:  p at fixed Y SZ Dashed: Evrard+08 M-  plus Planck Y-M (2013 XX) Large mass bias (67%) to reconcile w/Planck-CMB not favored Requires  gxy ~0.83  DM or M vir ~0.6M true pp Y SZ Rines et al. in prep.

30 HeCS-SZ: Scaling Relation Scaling of  p -Y SZ Published Planck data for 115 clusters (Planck 2013 XXIX) Strong correlation Significant scatter Bayesian fit:  p at fixed Y SZ Dashed: Evrard+08 M-  plus Planck Y-M (20113 XX Dashed: Are galaxies biased tracers? Munari+13 Scaling of  p -Y SZ Published Planck data for 115 clusters (Planck 2013 XXIX) Strong correlation Significant scatter Bayesian fit:  p at fixed Y SZ Dashed: Evrard+08 M-  plus Planck Y-M (20113 XX Dashed: Are galaxies biased tracers? Munari+13 pp Y SZ Rines et al. in prep.

31 HeCS-SZ: Scaling Relation Best-fit parameters vs Planck Y-M Green: M HS =M true ; red: M HS =0.59M true Scatter of 0.115 in  p (30%) Best-fit parameters vs Planck Y-M Green: M HS =M true ; red: M HS =0.59M true Scatter of 0.115 in  p (30%) pp Y SZ Slope

32 Future Observations HectoMap 50 deg 2, r~21 z=0.1-0.5 10x denser than BOSS HeCS-red redMapper (optically selected) clusters BigBOSS Subaru-PFS SPIDERS, 4MOST DESpec Euclid, WFIRST HectoMap 50 deg 2, r~21 z=0.1-0.5 10x denser than BOSS HeCS-red redMapper (optically selected) clusters BigBOSS Subaru-PFS SPIDERS, 4MOST DESpec Euclid, WFIRST

33 Science with Wide-Field Cluster Surveys Scaling relations M vir,  p, M ★, Y X, Y SZ, M lens M vir vs Y SZ (Rines et al. 2010) M vir vs M WL (Geller et al. 2013) Evolution of Cluster Galaxies to 5r 200 Mass function (  m,  8 ) BCG Dynamics Lensing: alignment, dilution Mass profiles to 5r 200 Ultimate halo masses Tests of modified gravity? (Lam et al. 2012) Scaling relations M vir,  p, M ★, Y X, Y SZ, M lens M vir vs Y SZ (Rines et al. 2010) M vir vs M WL (Geller et al. 2013) Evolution of Cluster Galaxies to 5r 200 Mass function (  m,  8 ) BCG Dynamics Lensing: alignment, dilution Mass profiles to 5r 200 Ultimate halo masses Tests of modified gravity? (Lam et al. 2012) Hectospec: 300 fibers, 1° diameter MMT 6.5m

34 HeCS: Comparison to X-ray A1835 X-ray HS M(r) Caustic M(r) (blue) Departures from HSE at r>r 500 Estimate P non-th (r)? A1835 X-ray HS M(r) Caustic M(r) (blue) Departures from HSE at r>r 500 Estimate P non-th (r)?  r  R p (Mpc/h)

35 HeCS-SZ: Planck-selected sample Massive clusters Planck clusters with SDSS DR10 imaging Infall regions (FoV is 3-6 Mpc at z=0.1-0.3) 115 clusters (80 in SZ- complete subsample) Target red sequence 8200 new redshifts in 24 clusters (z<0.2) Probes smaller L X at z>0.1 Massive clusters Planck clusters with SDSS DR10 imaging Infall regions (FoV is 3-6 Mpc at z=0.1-0.3) 115 clusters (80 in SZ- complete subsample) Target red sequence 8200 new redshifts in 24 clusters (z<0.2) Probes smaller L X at z>0.1 Z CIRS: SDSS+RASS, z<0.1 (Rines & Diaferio 2006, see also Andreon 2010: mass-richness)

36 HeCS: Color selection Are red-sequence velocity dispersions biased? Few blue members Small differences Quartiles by M 200 and L X (no caustics) Works in simulations (Serra et al 2011) Clean Infall Regions Caustic mass profiles Are red-sequence velocity dispersions biased? Few blue members Small differences Quartiles by M 200 and L X (no caustics) Works in simulations (Serra et al 2011) Clean Infall Regions Caustic mass profiles g-r M r +5 log h

37 HeCS: Color selection Are red-sequence velocity dispersions biased? Few blue members Small differences Quartiles by M 200 and L X (no caustics) Works in simulations (Serra et al 2011) Clean Infall Regions Caustic mass profiles Are red-sequence velocity dispersions biased? Few blue members Small differences Quartiles by M 200 and L X (no caustics) Works in simulations (Serra et al 2011) Clean Infall Regions Caustic mass profiles z M r +5 log h

38 HeCS: Color selection Are red-sequence velocity dispersions biased? Few blue members Small differences Quartiles by M 200 and L X (no caustics) Works in simulations (Serra et al 2011) Clean Infall Regions Caustic mass profiles Are red-sequence velocity dispersions biased? Few blue members Small differences Quartiles by M 200 and L X (no caustics) Works in simulations (Serra et al 2011) Clean Infall Regions Caustic mass profiles vv R p (Mpc/h)

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