Results from the 2500d SPT-SZ Survey

Transcription

1 Results from the 2500d SPT-SZ Survey Lindsey Bleem Argonne National Laboratory! March 15, 2015 SnowCluster 2015

2 The South Pole Telescope Collaboration Funded By: Funded by: 2

3 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 2016: SPT-3G! ~15,200 detectors! 100,150,220 GHz! +Polarization Funded by: Funded By:

4 WMAP! 94 GHz! 50 deg 2

5 Planck! 143 GHz! 50 deg 2 2x finer angular resolution!! 7x deeper

6 SPT! 150 GHz! 50 deg 2 13x finer angular resolution!! 17x deeper

7 SPT! 150 GHz! 50 deg 2

8 SPT! 150 GHz! 50 deg 2 CMB Anisotropy Primordial and secondary anisotropy in the CMB

9 SPT! 150 GHz! 50 deg 2 Point Sources Active galactic nuclei, and the most distant, star-forming galaxies

10 SPT! 150 GHz! 50 deg 2 Clusters of Galaxies Shadows in the microwave background from clusters of galaxies

11 The 2500 deg 2 SPT-SZ Survey ( ): 4h 2h 0h 22h 6h Final survey depths of:! 90 GHz: 40 ukcmb-arcmin! 150 GHz: 17 ukcmb-arcmin! 220 GHz: 80 ukcmb-arcmin!

12 The Sunyaev Zel dovich (SZ) Effect Adapted from L. Van Speybroeck CMB Spectrum The SPT-SZ survey SZ Spectrum imaged the sky at 100, 150 and 220 GHz.!

13 90 o 1 o 10 Angular Scale Planck SPT 220 GHz SPT - S13 SPT 150 GHz 1000 SPT 95 GHz 100 Everything Else! (astrophysics, cosmology) primary CMB! (cosmology) George et al., ApJ, 799, 177 (2015)

14 x95 150x x x150 95x x Total tsz DSFG Poisson Radio Poisson CMB ksz DSFG Clustering Gal. Cirrus George et al., ApJ, 799, 177 (2015)

15 Finding Clusters in the SPT Survey 95 GHz 150 GHz Matched Filter S/N= GHz Matched-filter multi-frequency cluster finder (Melin et al. 2006)

16 First Blind SZ detection : 2008! 150 GHz Raw 150 GHz filtered 90 GHz filtered 220 GHz filtered Staniszewski et al. 2009

17 > 500 Clusters in SPT-SZ sample

18 Swope Spitzer Multiple-facility Imaging Campaign Magellan for Cluster Confirmation Blanco 2.2 m MPG/ESO NTT

19 The 2500d SPT-SZ Cluster Sample ] M 500c [ M O h SPT-SZ 2500 deg 2 ROSAT-All sky Planck-2015 ACT Redshift Median M500 ~ 3x10 14 Msun zmedian =0.55 Bleem et al, ApJS, 216, 27 (2015)

20 The 2500d SPT-SZ Cluster Sample ] M 500c [ M O h Area (deg Redshift Depth (uk-arcmin) SPT-SZ 2500 deg 2 ROSAT-All sky Planck-2015 ACT Planck All-sky N SPT ACT The SZ effect uniquely finds the most massive, high-redshift clusters in the Universe.!! First SZ-discovered cluster found in 2008; 5 years later there are >1400 SZ-identified clusters!

21 ACT-CL/SPT-CL J : El-Gordo Rarest cluster in universe; only ~1 expected in universe above its mass and redshift of M200 Phoenix ~ 3 x Msun/ h70 at z=0.87 Cluster McDonald et al, 2012, Nature Chandra/ACIS Menanteau et al. (2011) Galaxy Density Foley et al 2011

22 SPT-CL J : The Phoenix Cluster Phoenix Cluster! z=0.596 SZ + Optical 5 20 kpc Phoenix Cluster Most X-ray luminous cluster known in the Universe! Largest star formation rate observed in a cluster s brightest central McDonald galaxy: et al, (~800 +/- 40 Msun 2012, / year) Nature! 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

23 Multi-wavelength Observations: Multi-wavelength mass calibration campaign, including:! Mass Calibration Gemini S 1. X-ray with Chandra! 2. Weak lensing from Magellan (0.3 < z < 0.6) and HST (z > 0.6)! Hubble Magellan 3. Dynamical masses from NOAO 3-year survey on Gemini (0.3 < z < 0.8 ), VLT, Magellan at (z > 0.8)

24 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)! 3. Dynamical masses from NOAO 3-year survey on Gemini (0.3 < z < 0.8 ), VLT, Magellan at (z > 0.8) + 40 more XMM (X-ray)! ~40 more HST snapshot High et al ApJ 758 (2012), 68 21

25 Multi-wavelength Observations: 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) Mass Calibration Weak Lensing Sample + 40 more XMM (X-ray)! ~40 more HST snapshot See Doug Applegate s Talk Tomorrow! High et al ApJ 758 (2012), 68 21

26 Multi-wavelength Observations: Multi-wavelength mass calibration campaign, including:! Mass Calibration Gemini S 1. X-ray with Chandra! 2. Weak lensing from Magellan (0.3 < z < 0.6) and HST (z > 0.6)! Hubble Magellan 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)

27 CMB Cluster Lensing with SPT-SZ Lensed-Unlensed On cluster Off cluster Combined off cluster Likelihood A ~few uk dimple! in the CMB caused by! lensing of a ~10 15! solar mass cluster M 200 (10 14 M O ) A 3.1-σ detection of CMB lensing using ~500 clusters measured by SPT-SZ! (Baxter et al. 2014, arxiv: ) See also Planck Collab. XXIV, 2015 (arxiv: )

28 Ysz-Yx Relation: Fit using 83 Clusters with Chandra X-ray Observations Y SZ (r 500 ) [10 14 M sun kev] 10 1 Andersson et al SPT-Chandra Y SZ = Y X Slope (0.97+/-0.04)! 1:1 relation with no tilt! Redshift Evolution (0.03+/-0.25)! Normalization doesn t evolve with redshift! Scatter (0.12+/-0.04)! Assume universal profile to measure Ysz; this assumption likely dominates scatter! Normalization (0.98+/-0.03)! Expect (Ysz/Yx) =1 for isothermal cluster, 0.92 for Arnaud et al pressure profile! Systematic uncertainty likely larger than statistical uncertainty quoted above:! 1 10 Y X (r 500 ) [10 14 M sun kev] (dysz/ysz) ~ 4% systematic due to pressure profile! (dyx/yx) ~ 10% systematic due to Chandra calibration Benson et al., (2015), in prep 28

29 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! - Ω m h 2, Ω b h 2, A s, n s, θ s Extension Cosmology! - w, Σmν, fnl, Neff D) scatter,! F) correlated scatter! Benson et al,! ApJ 763, 147 (2013)!

30 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 ~ M 1.75+/-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)

31 Yx-M Weak Lensing (WL) Calibration: Updating calibration to new Hoekstra+15 calibration M WL(CCCP) (r 500 ) [10 14 M sun /h 70 ] M(WL)-M(Yx) 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+/ M Yx (r 500 ) [10 14 M sun /h 70 ] M(WL, Hoekstra+15) = (1.25+/-0.14) M(Yx) Hoekstra et al arxiv:

32 ΛCDM Constraints: SPT data using Vikhlinin+09 Yx mass calibration Statistical (Cluster Counts) Mass Function Shape, Redshift Evolution Systematic (Mass Calibration) From Benson+13 to de Haan+15, area in σ 8 -Ωm likelihood space reduced by ~4x! Biggest improvement is in direction of parameter space helped by cluster counts Benson et al., ApJ 763, 147 (2013)! Reichardt et al., ApJ 763, 127 (2013)! de Haan et al., (2015), in prep 32

33 ΛCDM Constraints: SPT data using Vikhlinin+09 Yx mass calibration Statistical (Cluster Counts) Mass Function Shape, Redshift Evolution Systematic (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

34 ΛCDM Constraints: SPT data using Vikhlinin+09 Yx mass calibration Statistical (Cluster Counts) Mass Function Shape, Redshift Evolution Consistent with CMB cosmological measurements! As well as constraints from other cluster surveys (Adam Mantz s talk)! de Haan et al., (2015), in prep

35 37 SPT-discovered massive clusters at z>1. SPT-CL J : z > 1.5 M500 ~ 3 x M Bleem et al, ApJS, 216, 27 (2015)

36 z = 1.07 z = 1.13 SPT-CL J First spec-z confirmed z > 1 SZ-selected cluster (Brodwin et al. 2010) z = 1.32 SPT-CL J Most massive cluster (M500 ~8 x10 14 M ) known at z > 1 (Foley et al. 2011) z = SPT-CL J z spec = 1.32, M500 = 5 x M (Stalder et al. 2012) SPT-CL J Most distant spectroscopically-confirmed SZ-selected cluster (z spec = 1.478; M500 = 5 x M ) (Bayliss et al. 2013)

37 SPT-CLJ Spitzer/IRAC 3.6 micron + i-band + r-band SPT-CLJ detected at significance of 6.3 (M500,SZ ~ 7 x ) in the first 720 deg 2 of the SPT survey area 15 (!) galaxies with O[II] 3727! emission (yellow) within! ~4000 km/s of z= Bayliss et al ApJ 794, 12

38 FourStar Imaging (H/Ks) First Look 40 High-z clusters observed with FourStar (complete above z ~1.0)

39 The SPT Strong Lensing sample can be used to probe DM halos.

40 Contrasting Simulations with Observations Li et al (in prep)

41 The SPT-SZ Strong Lensing Sample Expect >100 strong lenses to be detected in SPT cosmology sample with reasonable (<0.75 ) ground-based imaging. Will be possible to measure the mean mass-concentration relation of massive halos to 5%, and constrain its scatter to 10% precision.! On-going simulation efforts to interpret observations: - Outer Rim simulation (HACC code) trillion particles with mass 2.6x10 9 M Gpc 3 Volume!!! Fig by Nan Li

42 h The SPT Surveys 4h 2h 0h 6h SPT-SZ SPT-E, SPT-W SPTpol deep SPTpol SPTpol-Summer Freq! (GHz) SPT-SZ SPTpol! deep SPTpol! Summer SPTpol Area Status Complete Complete Complete In Progress 4000 deg 2 surveyed in total by SPT-SZ and SPTpol! GHz depths between 6-30 uk-arcmin (from ~Planck depth,! to ~5 times deeper)

43 SPT Footprints! 4000 deg 2 between! SPT-SZ, SPTpol DES Footprint! SPT Footprint 22h 0h 2h 4h 6h -15d -30d SPT-SZ SPT-E, SPT-W SPTpol deep SPTpol SPTpol-Summer -65d ~3400 deg 2 overlap with Dark Energy Survey

44 Whats next? Evolution of CMB Focal Planes 2001: ACBAR! 16 detectors 2007: SPT! 960 detectors Stage : SPTpol! ~1600 detectors Pol Pol CMB Stage-4 Experiment! Described in Snowmass CF5:! Neutrinos: arxiv: ! Inflation: arxiv: Stage : SPT-3G! ~15,200 detectors Stage ?: CMB-S4! 100,000+ detectors Detector sensitivity has been limited by photon shot noise for last ~15 years; further improvements are made only by making more detectors! Pol

45 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)

46 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

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49 Redshift Measurements of SPT Clusters J. Hao 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)

50 CMB-S4 Stage 4 CMB experiment (footprint overlap with DES, LSST, MS-DESI, etc) - 200, ,000 detectors on multiple platforms - span 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