Upload
elvin-hicks
View
215
Download
0
Tags:
Embed Size (px)
Citation preview
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
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~108 Mpc3
(10x CIRS volume) 58 clusters Target red sequence 22,680 new redshifts 10,145 cluster members
Z
LX
CIRS: SDSS+RASS, z<0.1 (Rines & Diaferio 2006, see also Andreon 2010: mass-richness)
HeCS Science Goals Scaling relations
Mvir, sp, M★, YX, YSZ, Mlens
Mvir vs YSZ (Rines et al. 2010)
Mvir vs MWL (Geller et al. 2013)
Evolution of Cluster Galaxies to 5r200 Colors, D4000
Mass function (Wm,s8) BCG Dynamics Lensing: substructure, dilution
Mass profiles to 5r200 Ultimate halo masses
(Rines et al. 2013)
Hectospec: 300 fibers, 1° diameter
MMT 6.5m
HeCS: Infall Patterns
Clean Infall Regions High contrast Median 200 members p ~ 500-1200 km/s
Ordered by LX Scatter in LX-p
Cooling cores, AGN l.o.s. structure
Dv
Rp (Mpc/h)
HeCS: Infall Patterns
Dv
Rp (Mpc/h)
Clean Infall Regions High contrast Median 200 members p ~ 500-1200 km/s
Ordered by LX Scatter in LX-p
Cooling cores, AGN l.o.s. structure Double cluster:
MS0906/A750
HeCS: Infall Patterns
Dv
Rp (Mpc/h)
Clean Infall Regions High contrast Median 200 members p ~ 500-1200 km/s
Ordered by LX Scatter in LX-p
Cooling cores, AGN l.o.s. structure
HeCS: Infall Patterns
Dv
Rp (Mpc/h)
Clean Infall Regions High contrast Median 200 members p ~ 500-1200 km/s
Ordered by LX Scatter in LX-p
Cooling cores, AGN l.o.s. structure
HeCS: Infall Patterns
Dv
Rp (Mpc/h)
Clean Infall Regions High contrast Median 200 members p ~ 500-1200 km/s
Ordered by LX Scatter in LX-p
Cooling cores, AGN l.o.s. structure
HeCS: Mass Profiles
Caustic mass profiles Radii up to 6 Mpc/h p ~ 500-1200 km/s M ~ 1015 M/h Green: Mvirial(r) for r500-
r100
Virial/caustic masses agree (sanity check)
M(<
R)
Rp (Mpc/h)
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) MWL 15-25% low?
Geller et al 2013
HeCS: Stacked Clusters
Projection effects dominate systematics Quartiles by M200 and LX
(no caustics) Works in simulations
(Serra et al 2011) Clean Infall Regions
Caustic mass profiles Dv
Rp (Mpc/h)
HeCS: Stacked Clusters
Density profiles Larger-LX quartiles have
larger r Dynamic range of ~104
~r rcritical at max. radius Singular isothermal
sphere ruled out
r
Rp (Mpc/h)
HeCS: Stacked Clusters
Density profiles 4 orders of magnitude Singular isothermal
sphere ruled out Agrees well with NFW
(even outside r200) 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
Rp (Mpc/h)
HeCS: Density Profiles
Density profiles NFW at R<2 Mpc Steeper at R>2-3 Mpc? Range of >103
~r rcritical at max. radius Singular isothermal
sphere ruled out Cumulative Density
profiles Similar to NFW Incomplete at R>3 Mpc Max. bound radius: r5.6
r(<r)
Rp (Mpc/h)
r
M200 LX
Ultimate Halo Mass
LCDM cosmology predicts halos stop growing, become increasingly isolated
Cluster mass at a=100 is about 2.2 M200(a=1) (Busha et al 2005) Limit: r5.6 (enclosed
density = 9p2/16 rcritical
Prediction seconded (Dunner et al 2006)
a=1
a=100a=11
a=100 (comoving)
Busha et al 2003
Ultimate Halo Mass
LCDM cosmology predicts halos stop growing, become increasingly isolated
Cluster mass at a=100 is about 2.2 M200(a=1) (Busha et al 2005)
HeCS measurement 33 clusters have
caustics out to r5.6
M5.6/M200=1.99±0.11 Similar dispersion
M5.
6/M
200
M200 (M/h)
HeCS Science Goals Scaling relations
Mvir, sp, M★, YX, YSZ, Mlens
Mvir vs YSZ (Rines et al. 2010)
Mvir vs MWL (Geller et al. 2013)
Evolution of Cluster Galaxies to 5r200 Colors, D4000
Mass function (Wm,s8) BCG Dynamics Lensing: substructure, dilution
(Coe+2012, Geller+13, Hwang+14)
Mass profiles to 5r200 Ultimate halo masses
(Rines et al. 2013)Hectospec: 300 fibers, 1° diameter
MMT 6.5m
Planck: SZ vs CMB Planck CMB constraints
disagree with Planck SZ results Blue: SZ mass function
with MHS=0.8Mtrue
Red: Planck CMB Black: SZ mass function,
free normalization: MHS=0.59Mtrue
Alternate explanations: neutrino masses
s8
Wm
Planck Collaboration 2013 XX.
HeCS: SZ vs Dynamics
Scaling of Mvir-YSZ Published SZA data for 15
clusters (Bonamente+08; Marrone+09)
Strong correlation (99.8%) Significant scatter Connection to s8 debate?
Larger samples needed
Rines et al. 2010
Mvir sp
YSZ
SZ vs Dynamics: ACT, SPT Scaling of sp-YSZ
VLT/Gemini spectroscopic followup of ACT-detected clusters (Sifon et al 2013)
z=0.3-1.1 Cluster evolution? Cluster selection?
sp
YSZ
Gemini spectroscopic followup of SPT-detected clusters (Ruel et al 2014) z=0.3-1.5 Substantial scatter Velocity bias? (sgxy~1.1sDM
or Mvir~1.3Mtrue)
sp
MSZ
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)
Z
MS
Z
Rines et al. in prep
HeCS-SZ: Infall Patterns
Dv
Rp (Mpc/h)
Clean Infall Regions High contrast Median 200 members p ~ 500-1200 km/s
Ordered by MSZ Scatter in MSZ-p
l.o.s. structure
HeCS-SZ: Infall Patterns
Dv
Rp (Mpc/h)
Clean Infall Regions High contrast Median 200 members p ~ 500-1200 km/s
Ordered by MSZ Scatter in MSZ-p
l.o.s. structure
HeCS-SZ: Infall Patterns
Dv
Rp (Mpc/h)
Clean Infall Regions High contrast Median 200 members p ~ 500-1200 km/s
Ordered by MSZ Scatter in MSZ-p
l.o.s. structure
HeCS-SZ: Infall Patterns
Dv
Rp (Mpc/h)
Clean Infall Regions High contrast Median 200 members p ~ 500-1200 km/s
Ordered by MSZ Scatter in MSZ-p
l.o.s. structure
HeCS-SZ: Scaling Relation Scaling of sp-YSZ
Published Planck data for 115 clusters (Planck 2013 XXIX)
Strong correlation Significant scatter Bayesian fit: sp at fixed YSZ
sp
YSZ
Rines et al. in prep.
HeCS-SZ: Scaling Relation Scaling of sp-YSZ
Published Planck data for 115 clusters (Planck 2013 XXIX)
Strong correlation Significant scatter Bayesian fit: sp at fixed YSZ
Dotted: Rines+10 ‘shallow’ Y-s no longer good fit
sp
YSZ
Rines et al. in prep.
HeCS-SZ: Scaling Relation Scaling of sp-YSZ
Published Planck data for 115 clusters (Planck 2013 XXIX)
Strong correlation Significant scatter Bayesian fit: sp at fixed YSZ
Dashed: Evrard+08 M-s plus Planck Y-M (2013 XX)
sp
YSZ
Rines et al. in prep.
HeCS-SZ: Scaling Relation Scaling of sp-YSZ
Published Planck data for 115 clusters (Planck 2013 XXIX)
Strong correlation Significant scatter Bayesian fit: sp at fixed YSZ
Dashed: Evrard+08 M-s plus Planck Y-M (2013 XX)
Large mass bias (67%) to reconcile w/Planck-CMB not favored
Requires sgxy~0.83sDM or Mvir~0.6Mtrue
sp
YSZ
Rines et al. in prep.
HeCS-SZ: Scaling Relation Scaling of sp-YSZ
Published Planck data for 115 clusters (Planck 2013 XXIX)
Strong correlation Significant scatter Bayesian fit: sp at fixed YSZ
Dashed: Evrard+08 M-s plus Planck Y-M (20113 XX
Dashed: Are galaxies biased tracers? Munari+13 sp
YSZ
Rines et al. in prep.
HeCS-SZ: Scaling Relation Best-fit parameters vs Planck Y-M
Green: MHS=Mtrue; red: MHS=0.59Mtrue
Scatter of 0.115 in sp (30%)
sp
YSZ
Slope Slope
Nor
mal
izat
ion
Sca
tter
Future Observations HectoMap
50 deg2, 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
Science with Wide-Field Cluster Surveys
Scaling relations Mvir, sp, M★, YX, YSZ, Mlens
Mvir vs YSZ (Rines et al. 2010)
Mvir vs MWL (Geller et al. 2013)
Evolution of Cluster Galaxies to 5r200
Mass function (Wm,s8) BCG Dynamics Lensing: alignment, dilution
Mass profiles to 5r200 Ultimate halo masses
Tests of modified gravity?(Lam et al. 2012)
Hectospec: 300 fibers, 1° diameter
MMT 6.5m
HeCS: Comparison to X-ray
A1835 X-ray HS M(r) Caustic M(r) (blue) Departures from
HSE at r>r500
Estimate Pnon-th(r)?
(M r)
Rp (Mpc/h)
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 LX at z>0.1
Z
L X
CIRS: SDSS+RASS, z<0.1 (Rines & Diaferio 2006, see also Andreon 2010: mass-richness)
HeCS: Color selection
Are red-sequence velocity dispersions biased?
Few blue members Small differences
Quartiles by M200 and LX (no caustics)
Works in simulations (Serra et al 2011)
Clean Infall Regions Caustic mass profiles
g-r
Mr +5 log h
HeCS: Color selection
Are red-sequence velocity dispersions biased?
Few blue members Small differences
Quartiles by M200 and LX (no caustics)
Works in simulations (Serra et al 2011)
Clean Infall Regions Caustic mass profiles
z
Mr +
5 lo
g h
HeCS: Color selection
Are red-sequence velocity dispersions biased?
Few blue members Small differences
Quartiles by M200 and LX (no caustics)
Works in simulations (Serra et al 2011)
Clean Infall Regions Caustic mass profiles
Dv
Rp (Mpc/h)