Results from the 2500d SPT-SZ Survey

Results from the 2500d SPT-SZ Survey
Lindsey Bleem
Argonne National Laboratory
!
March 15, 2015
SnowCluster 2015
The South Pole Telescope Collaboration
Funded By:
Funded by:
2
The South Pole
Telescope
(SPT)
!
10-meter sub-mm quality
wavelength telescope!
100, 150, 220 GHz and
1.6, 1.2, 1.0 arcmin resolution
2007: SPT-SZ!
960 detectors!
100,150,220 GHz
2012: SPTpol!
1600 detectors!
100,150 GHz!
+Polarization
Funded By:
2016: SPT-3G!
~15,200 detectors!
100,150,220 GHz!
+Polarization
Funded by:
WMAP!
94 GHz!
50 deg2
Planck!
143 GHz!
50 deg2
2x finer angular
resolution!
!
7x deeper
SPT!
150 GHz!
50 deg2
13x finer angular
resolution!
!
17x deeper
SPT!
150 GHz!
50 deg2
SPT!
150 GHz!
50 deg2
CMB Anisotropy
Primordial and
secondary anisotropy in
the CMB
SPT!
150 GHz!
50 deg2
Point Sources Active galactic nuclei, and the most
distant, star-forming galaxies
SPT!
150 GHz!
50 deg2
Clusters of Galaxies “Shadows” in the microwave
background from clusters of
galaxies
The 2500 deg2 SPT-SZ Survey (2007-2011):
2h
0h
4h
22
6h
h
-40
-50
-60
Final survey depths of:!
90 GHz: 40 uKCMB-arcmin !
150 GHz: 17 uKCMB-arcmin!
220 GHz: 80 uKCMB-arcmin!
Adapted from L. Van Speybroeck
The Sunyaev Zel’dovich (SZ) Effect
CMB Spectrum
SZ Spectrum
The SPT-SZ survey
imaged the sky at 100,
150 and 220 GHz. !
90o
1o
Angular Scale
5
2
10
1
Planck
SPT 220 GHz
SPT - S13
SPT 150 GHz
SPT 95 GHz
1000
Everything Else!
(astrophysics, cosmology)
100
primary CMB!
(cosmology)
10
10
500
1500
2500
6000
10000
George et al., ApJ, 799, 177 (2015)
1000
95x95
150x150
220x220
95x150
95x220
150x220
100
10
1
1000
100
10
1
2000 4000 6000 8000 10000
4000 6000 8000 10000
4000 6000 8000 10000
Total
tSZ
DSFG Poisson
Radio Poisson
CMB
kSZ
DSFG Clustering
Gal. Cirrus
George et al., ApJ, 799, 177 (2015)
Finding Clusters in the SPT Survey
95 GHz
150 GHz
Matched
Filter
S/N=6.3
220 GHz
• Matched-filter multi-frequency cluster
finder (Melin et al. 2006)
First “Blind” SZ detection : 2008!
150 GHz
“Raw”
150 GHz
filtered
90 GHz
filtered
220 GHz
filtered
Staniszewski et al. 2009
> 500 Clusters in SPT-SZ sample
Swope
Spitzer
Multiple-facility Imaging Campaign
for Cluster Confirmation
Magellan
Blanco
2.2 m MPG/ESO
NTT
M500c [1014 MO• h-1
70 ]
The 2500d SPT-SZ Cluster Sample
SPT-SZ 2500 deg2
ROSAT-All sky
Planck-2015
ACT
10
1
0.0
0.5
1.0
1.5
Redshift
• Median M500 ~ 3x1014 Msun
• zmedian =0.55
Bleem et al, ApJS, 216, 27 (2015)
M500c [1014 MO• h-1
70 ]
The 2500d SPT-SZ Cluster Sample
SPT-SZ 2500 deg2
ROSAT-All sky
Planck-2015
ACT
10
• The SZ effect uniquely
finds the most massive,
high-redshift clusters in
the Universe.!
1
0.0
0.5
1.0
1.5
• First SZ-discovered
Redshift
Area
(deg
Depth
(uK-arcmin)
!
N
Planck All-sky
45
1203
SPT
2500
17
516
ACT
950
23-40
91
cluster found in 2008;
5 years later there are
>1400 SZ-identified
clusters!
ACT-CL/SPT-CL J0102-4915: “El-Gordo”
“Rarest” cluster in universe; only ~1 expected in
universe above its mass and redshift of M200 “Phoenix”
~ 3 x 1015 Msun/
Cluster
h70 at z=0.87
McDonald et al,
2012, Nature
Chandra/ACIS
Menanteau et al. (2011)
Galaxy Density
Foley et al
2011
SPT-CL J2344-4243: The “Phoenix Cluster”
Phoenix Cluster!
z=0.596
• Most X-ray “Phoenix”
luminous cluster
known in theCluster
Universe
!
• Largest star formation rate
observed in a cluster’s
brightest central
galaxy: et al,
McDonald
(~800 +/- 40 Msun
/ year)
2012,
Nature
5’
SZ +
Optical
20 kpc
!
• Star formation efficiency of
~30%; “classical” X-ray cooling
rate of 2850 Msun / year is
efficiently turning into stars
Hubble
McDonald et al. !
Nature 488 (2012), 349!
! Foley et al
2011
Multi-wavelength Observations:
Mass Calibration
Gemini S
• Multi-wavelength mass
calibration campaign,
including:!
1. X-ray with Chandra !
2. Weak lensing from
Magellan (0.3 < z < 0.6) and
HST (z > 0.6) !
3. Dynamical masses from
NOAO 3-year survey on
Gemini (0.3 < z < 0.8 ), VLT,
Magellan at (z > 0.8)
Hubble
Magellan
Multi-wavelength Observations:
Mass Calibration
• Multi-wavelength mass
calibration campaign,
including:!
Weak Lensing Sample
1. X-ray with Chandra !
2. Weak lensing from
Magellan (0.3 < z < 0.6) and
HST (z > 0.6) !
XMM (X-ray)
!
+ 40 more
~40 more
HST snapshot
3. Dynamical masses from
NOAO 3-year survey on
Gemini (0.3 < z < 0.8 ), VLT,
Magellan at (z > 0.8)
High et al ApJ 758 (2012), 68
21
Multi-wavelength Observations:
Mass Calibration
• Multi-wavelength mass
calibration campaign,
including:!
Weak Lensing Sample
!
w
rro
k
l
a
T
s
’
1. X-ray with Chandra !
e
t
a
leg
2. Weak lensing from
p
p
Magellan (0.3 < z < 0.6)A
and
g
u
HST (z > 0.6) ! Do
e
e
S
o
m
To
XMM (X-ray)
!
+ 40 more
~40 more
HST snapshot
3. Dynamical masses from
NOAO 3-year survey on
Gemini (0.3 < z < 0.8 ), VLT,
Magellan at (z > 0.8)
High et al ApJ 758 (2012), 68
21
Multi-wavelength Observations:
Mass Calibration
Gemini S
• Multi-wavelength mass
calibration campaign,
including:!
1. X-ray with Chandra !
2. Weak lensing from
Magellan (0.3 < z < 0.6) and
HST (z > 0.6) !
3. Dynamical masses from
NOAO 3-year survey on
Gemini (0.3 < z < 0.8 ), VLT,
Magellan at (z > 0.8)
Bocquet et al. ApJ, 799, 214 (2015)
Hubble
Magellan
CMB Cluster Lensing with SPT-SZ
Lensed-Unlensed
1.0
On cluster
Off cluster
Combined off cluster
Likelihood
0.8
0.6
0.4
0.2
0.0
-10.0
A ~few uK “dimple” !
in the CMB caused by !
lensing of a ~1015 !
solar mass cluster
-5.0
0.0
5.0
M200 (1014 MO• )
10.0
15.0
20.0
A 3.1-𝝈 detection of CMB lensing
using ~500 clusters measured by
SPT-SZ !
(Baxter et al. 2014, arXiv:1412.7521)
See also Planck Collab. XXIV, 2015 (arXiv:1502.01597)
Ysz-Yx Relation:
YSZ (r500) [1014 Msun keV]
Fit using 83 Clusters with Chandra X-ray Observations
Andersson et al. 2011
SPT-Chandra
YSZ = YX
• Slope (0.97+/-0.04)!
• 1:1 relation with no tilt!
• Redshift Evolution (0.03+/-0.25)!
• Normalization doesn’t evolve with redshift!
10
• Scatter (0.12+/-0.04)!
• Assume universal profile to measure Ysz;
this assumption likely dominates scatter!
• Normalization (0.98+/-0.03)!
1
• Expect (Ysz/Yx) =1 for isothermal cluster,
1
10
YX (r500) [1014 Msun keV]
Benson et al., (2015), in prep
0.92 for Arnaud et al. 2009 pressure profile!
• Systematic uncertainty likely larger than
statistical uncertainty quoted above:!
• (dYsz/Ysz) ~ 4% systematic due to
pressure profile!
• (dYx/Yx) ~ 10% systematic due to
Chandra calibration
28
Cosmological Analysis:
Combine X-ray Observables with SPT Cluster Survey
Use Markov-Chain Monte Carlo (MCMC) method to vary
cosmology and cluster observable-mass relation simultaneously,
while accounting for SZ selection in a self-consistent way
9 Scaling Relation Parameters!
• X-ray (Yx-M) and SZ (𝞯-M)
relations (4 and 5 parameters): A) normalization, !
B) slope, !
C) redshift evolution, !
6 Cosmology Parameters
(plus extension parameters)!
• 𝚲CDM Cosmology !
2, Ω h2, A , n , 𝜽 Ω
h
- m
b
s
s
s
• Extension Cosmology !
- w, 𝚺m𝝂, fNL, Neff
D) scatter, !
F) correlated scatter!
Benson et al, !
ApJ 763, 147 (2013) !
Cosmological Analysis:
Combine X-ray Measurements with SZ Cluster Survey
9 Scaling Relation Parameters!
• X-ray (Yx-M) and SZ (𝞯-M) relations (4 and 5 parameters): A) Normalization:!
- Effectively set by weak-lensing calibration (see next slide)!
B) Slope:!
- Effectively set by prior based on Vikhlinin+09 (Yx ~ M1.75+/-0.10)!
C) Redshift evolution:!
- Prior of self-similar evolution, with an uncertainty
corresponding to an additional ~10% mass uncertainty at z=1.0!
D) Scatter:!
- Log-normal scatter of (0.12+/-0.08) in mass given Yx !
F) Correlated scatter:!
- Uniform prior from -1 to 1 (not important for constraints)
Yx-M Weak Lensing (WL) Calibration:
Updating calibration to new Hoekstra+15 calibration
M(WL)-M(Yx)
MWL(CCCP) (r500) [1014 Msun/h70]
20
15
10
5
• Vikhlinin+09 Yx-M used weak-lensing
measurements of 10 clusters from
Hoekstra07 to check overall mass
calibration!
• Hoekstra-measured WL masses
have been updated as data sets and
methods have improved!
• Re-fitting normalization, we should
multiply Vikhlinin+09 Yx-masses by:!
• Hoekstra+12: 1.03+/-0.15!
• Hoekstra+15: 1.25+/-0.14
0
0
5
10
15
MYx (r500) [1014 Msun/h70]
20
M(WL, Hoekstra+15)
= (1.25+/-0.14) M(Yx)
Hoekstra et al. 2015 arXiv:1502.01883
𝚲CDM Constraints:
St
a
Ma tisti
Re ss F cal (
C
ds
u
hif nct lus
t E ion ter
C
vo
lut Shap oun
ion e,
ts)
Benson et al., ApJ 763, 147 (2013)!
Reichardt et al., ApJ 763, 127 (2013)!
de Haan et al., (2015), in prep
Sy
(M stem
as
s C atic
al
ib
ra
tio
n)
SPT data using Vikhlinin+09 Yx mass calibration
• From Benson+13 to
de Haan+15, area in
σ8-Ωm likelihood space
reduced by ~4x!
• Biggest improvement
is in direction of
parameter space
helped by cluster
counts
32
𝚲CDM Constraints:
St
a
Ma tisti
Re ss F cal (
C
ds
u
hif nct lus
t E ion ter
C
vo
lut Shap oun
ion e,
ts)
Sy
(M stem
as
s C atic
al
ib
ra
tio
n)
SPT data using Vikhlinin+09 Yx mass calibration
• Hoekstra+15 weak lensing
calibration increases mass
calibration by 25% (relative
to Vikhlinin+09)!
• Mass calibration assumes
a 14% uncertainty in mass
at z=0!
• Limited by small sample (10
clusters) in Vikhlinin+09,
Hoekstra+15 comparison!
• Next step is to increase
sample and extend to higher
redshift
Benson et al., ApJ 763, 147 (2013)!
Reichardt et al., ApJ 763, 127 (2013)!
de Haan et al., (2015), in prep
33
𝚲CDM Constraints:
SPT data using Vikhlinin+09 Yx mass calibration
• Consistent with CMB
cosmological
measurements !
St
a
Ma tisti
Re ss F cal (
C
ds
u
hif nct lus
t E ion ter
C
vo
lut Shap oun
ion e,
ts)
• As well as constraints from
other cluster surveys
(Adam Mantz’s talk)
!
de Haan et al., (2015), in prep
37 SPT-discovered massive clusters at z>1.
SPT-CL J0459-4947: z > 1.5
M500 ~ 3 x 1014 M⊙
Bleem et al, ApJS, 216, 27 (2015)
z = 1.07
SPT-CL J0546-5345 – First spec-z confirmed z
> 1 SZ-selected cluster (Brodwin et al. 2010)
z = 1.32
SPT-CL J0205-5829
zspec = 1.32, M500 = 5 x 1014 M⊙
(Stalder et al. 2012)
z = 1.13
SPT-CL J2106-5844 – Most massive cluster
(M500 ~8 x1014 M⊙) known at z > 1 (Foley et al. 2011)
z = 1.478
SPT-CL J2040-4451 – Most distant spectroscopically-confirmed
SZ-selected cluster (zspec = 1.478; M500 = 5 x 1014 M⊙)
(Bayliss et al. 2013)
SPT-CLJ2040-4451
Spitzer/IRAC 3.6 micron + i-band + r-band
•
SPT-CLJ2040-4451 detected at
significance of 6.3 (M500,SZ ~ 7 x
1014) in the first 720 deg2 of the SPT
survey area
15 (!) galaxies with O[II] 3727 !
emission (yellow) within !
~4000 km/s of z=1.4765
Bayliss et al. 2014. ApJ 794, 12
FourStar Imaging (H/Ks) First Look
40 High-z
clusters observed with FourStar (complete above z ~1.0)
The SPT Strong Lensing sample can be used to probe DM halos.
Contrasting Simulations with
Observations
Li et al (in prep)
The SPT-SZ Strong Lensing Sample
• Expect >100 strong lenses to be
14detected in SPT cosmology sample with
reasonable (<0.75”) ground-based
12
imaging. 20
10
15
• Will be possible to measure the mean
8
mass-concentration relation of massive
6halos to ∼5%, and constrain its scatter to
∼10% precision.
4
!
2• On-going simulation efforts to interpret
0observations:
“Outer
code)
0.0 - 0.2
0.4Rim”
0.6simulation
0.8 1.0 (HACC
1.2 1.4
- 1.1 trillion particles with mass
2.6x109 M⊙
- 9.14 Gpc3 Volume
!
!
!
10
5
0
0.0
0.2
0.4
0.6
0.8
1.0
1.2
1.4
Fig by Nan Li
The SPT Surveys
2h
0h
4h
22
6h
h
-40
-50
SPT-SZ
SPT-E, SPT-W
SPTpol deep
SPTpol
SPTpol-Summer
Freq!
(GHz)
-60
SPTpol! SPTpol!
SPT-SZ
deep
Summer
SPTpol
95
40
15
70
15
150
17
6
30
6
220
80
40
-
2500
100
1500
500
Complete
In Progress
Area
Status
Complete Complete
4000 deg2 surveyed in total by SPT-SZ and SPTpol!
- 150 GHz depths between 6-30 uK-arcmin (from ~Planck depth, !
to ~5 times deeper)
SPT Footprints!
DES Footprint!
SPT Footprint
4000 deg2 between !
SPT-SZ, SPTpol
22h
0h
2h
-15d
-30d
SPT-SZ
SPT-E, SPT-W
SPTpol deep
SPTpol
SPTpol-Summer
-65d
~3400 deg2 overlap with Dark Energy Survey
4h
6h
Whats next? Evolution of CMB Focal Planes
2001: ACBAR!
16 detectors
2007: SPT!
960 detectors
CMB Stage-4 Experiment!
Described in Snowmass CF5: !
Neutrinos: arxiv:1309.5383 !
Inflation: arxiv:1309.5381
Stage-2
2012: SPTpol!
~1600 detectors
Stage-3
2016: SPT-3G!
~15,200 detectors
Stage-4
2020?: CMB-S4!
100,000+ detectors
Pol
Pol
Detector sensitivity has been limited by
photon “shot” noise for last ~15 years;
further improvements are made only by
making more detectors!
Pol
Future SZ Cluster Surveys
Cluster counts scale roughly
as number of detectors:
SPT-SZ/pol:
Nclust ~ 1,000!
SPT-3G:
Nclust ~ 10,000!
CMB-S4: Nclust ~ 100,000+
Deep CMB data also enables
CMB cluster lensing as a
competitive mass calibration
tool for cluster DE science:!
SPT-3G: 𝝈(M) ~ 3%!
CMB-S4: 𝝈(M) < ~0.1%!
Especially promising tool for
cluster masses at z > 1
*eRosita 50 cts threshold
(Pillepich et al 2012)
Summary
•
SPT has found hundreds of massive galaxy clusters
spanning a redshift range 0.05 < z< 1.7.
•
Clean, mass-limited selection leads to a fantastic sample
for cosmological and astrophysical studies.
•
Cosmological analysis consistent with other cluster
studies & CMB Cosmology
•
Better mass calibration required to tighten constraints
(and work is ongoing!).
•
Rapid growth of SZ cluster samples will continue with
SPTpol, SPT-3G
Redshift Measurements of SPT Clusters
1.4
1.2
1.0
0.8
0.6
0.4
0.2
0.0
3
2
1
0
-1
-2
-3
0.0
0.2
0.4
0.6
0.8
1.0
1.2
1.4
J. Hao
• 134
spectroscopic redshifts (26%)
• σz ~ 0.02(1+z) optical (Red-Sequence)
• σz ~ 0.04(1+z) NIR (1.6 μm Stellar “Bump”)
Bleem et al, ApJS, 216, 27 (2015)
‘CMB-S4’ Stage 4 CMB experiment
(footprint overlap with DES, LSST, MS-DESI, etc)
- 200,000 - 500,000 detectors on multiple platforms
- span 40 - 240 GHz for foreground removal
- target noise of ~1 uK-arcmin depth over half the sky
- start ~2022
Primary technical challenge will be the
scaling of the detector arrays