Cosmological Analysis of South Pole Telescope-detected Galaxy Clusters

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1 Cosmological Analysis of South Pole Telescope-detected Galaxy Clusters March 24th Tijmen de Haan (McGill) - Moriond 2014 Photo credit: Keith Vanderlinde

2 Outline The galaxy cluster sample Calibrating the mass scale Cosmological constraints The future of SPT cluster science March 24th Tijmen de Haan (McGill) - Moriond

The South Pole Telescope (SPT) 10-m -> 1 arcminute resolution 2007-2011 SPT-SZ survey

camera observing at 90 GHz, 150 GHz 2016-?

3 The South Pole Telescope (SPT) 10-m -> 1 arcminute resolution SPT-SZ survey Observing at 90 GHz, 150 GHz, 220 GHz SPTpol survey Polarization-sensitive camera observing at 90 GHz, 150 GHz 2016-? SPT-3G survey Polarization-sensitive multichroic ~15000 detector camera Photo credit: Ryan Keisler March 24th Tijmen de Haan (McGill) - Moriond

4 March 24th Tijmen de Haan (McGill) - Moriond

5 Why the South Pole? March 24th Tijmen de Haan (McGill) - Moriond

6 Readout 12x digital frequency multiplexed TES bolometers Custom FPGA-powered readout boards March 24th Tijmen de Haan (McGill) - Moriond

7 2500 square-degree SPT-SZ survey 5 year survey (2007 to 2011) 95 GHz: 40 μk-arcmin 150 GHz: 18 μk-arcmin 220 GHz: 70 μk-arcmin Stephen Padin Zak Staniszewski Keith Vanderlinde Dana Hrubes Erik Shirokoff Ross Williamson Daniel Luong-Van March 24th Tijmen de Haan (McGill) - Moriond

Zak Staniszewski Keith Vanderlinde Dana Hrubes Erik Shirokoff Ross

8 March 24th Tijmen de Haan (McGill) - Moriond

9 March 24th Tijmen de Haan (McGill) - Moriond

10 March 24th Tijmen de Haan (McGill) - Moriond

11 March 24th Tijmen de Haan (McGill) - Moriond

12 Outline The SPT Calibrating the mass scale Cosmological constraints The future of SPT cluster science March 24th Tijmen de Haan (McGill) - Moriond

$(optical depth) * (fractional energy gain per scattering) Illustration: NASA/CXC/M.$

13 Sunyaev-Zel dovich Effect Distortion of the Cosmic Microwave Background from inverse Compton scattering due to high energy electrons Measure Compton y-parameter y = (optical depth) * (fractional energy gain per scattering) Illustration: NASA/CXC/M.Weiss Carlstrom, Holder, Reese (2002) March 24th Tijmen de Haan (McGill) - Moriond

$(optical depth) * (fractional energy gain per scattering) Illustration: NASA/CXC/M.$

14 Extracting Clusters Matched-filter multi-frequency cluster finder (Melin et al. 2006) 95 GHz 150 GHz 220 GHz Spatially filter Linear combination to maximize signal-tonoise March 24th Tijmen de Haan (McGill) - Moriond

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16 March 24th Tijmen de Haan (McGill) - Moriond

17 Selection Function March 24th Tijmen de Haan (McGill) - Moriond

18 Outline The SPT The galaxy cluster sample Cosmological constraints The future of SPT cluster science March 24th Tijmen de Haan (McGill) - Moriond

19 Mass Calibration Poisson errors are very small order 1/ 400 Implies 0.5% on σ 8 compared to current quoted uncertainties (~5%) Even better improvements in extensions to ΛCDM BUT overall scaling of SZ effect with mass dominates uncertainties SZ normalization only known to ~30% from simulation (gas modelling) Need better modelling or multi-wavelength follow-up SZ-Mass Normalization March 24th Tijmen de Haan (McGill) - Moriond

overall scaling of SZ effect with mass dominates uncertainties SZ normalization only known to ~30% from

20 Multi-wavelength mass measurements Chandra Magellan HST XMM Image Credit: ESA/C. Carreau March 24th Tijmen de Haan (McGill) - Moriond

edu/magellan XMM http://spaceflight.nasa.

21 Chandra Observations Awarded 3.2 Ms of Chandra time ~90 clusters ~3k photons - relation was previously calibrated (e.g. Vikhlinin 2006) March 24th Tijmen de Haan (McGill) - Moriond

22 Chandra Observations Relation between integrated compton-y parameter Y SZ and X- ray equivalent Y X agrees with expectation March 24th Tijmen de Haan (McGill) - Moriond

23 Outline The SPT The galaxy cluster sample Calibrating the mass scale The future of SPT cluster science March 24th Tijmen de Haan (McGill) - Moriond

24 Cosmological Analysis Explore cosmological parameter space using MCMC ΛCDM, or add extension parameters like w, w a, Σm ν, f NL, N eff, r Marginalize over nuisance parameters Scaling of SZ signal with cluster mass & evolution with mass, redshift Scaling of X-ray signal with cluster mass & evolution with mass, redshift Intrinsic scatter in the scaling relations, including correlations Likelihood code Bayesian, fully taking into account selection effects, self-consistently incorporating any number of mass proxies, including correlations between them March 24th Tijmen de Haan (McGill) - Moriond Benson et al (2013)

25 ΛCDM Constraints (CMB) March 24th Tijmen de Haan (McGill) - Moriond

26 Constraints on ΛCDM + Σ m ν March 24th Tijmen de Haan (McGill) - Moriond

27 Dark Energy Equation of State w (CMB) March 24th Tijmen de Haan (McGill) - Moriond

28 Coming Soon: Weak lensing Mass Calibration Weak lensing observations & analysis of SPT clusters underway ~100 clusters at low redshift with Magellan/MegaCam ~100 clusters at high redshift with HST Expect major improvements in cosmological constraints Growth-based dark energy constraints from clusters alone Dietrich et al. (in prep) March 24th Tijmen de Haan (McGill) - Moriond

29 Outline The SPT The galaxy cluster sample Calibrating the mass scale Cosmological constraints March 24th Tijmen de Haan (McGill) - Moriond

30 sum diff SPTpol Q Observing since Jan st year SPTpol maps: U March 24th Tijmen de Haan (McGill) - Moriond

31 SPTpol: Cluster Science Small cutout from an SPT-SZ map: March 24th Tijmen de Haan (McGill) - Moriond

32 SPTpol: Cluster Science Small cutout from an SPTpol map: Much deeper data Able to see clusters down to a lower mass March 24th Tijmen de Haan (McGill) - Moriond

33 SPTpol (now) ~ 1600 detectors SPT3G (2016) ~ 16,000 detectors SPT-3G Fabricated by Toki Suzuki March 24th Tijmen de Haan (McGill) - Moriond

34 March 24th Tijmen de Haan (McGill) - Moriond

35 Thanks March 24th Tijmen de Haan (McGill) - Moriond

36 More Slides March 24th Tijmen de Haan (McGill) - Moriond

37 SPTpol: First Detection of B-mode Polarization of the CMB 7.7σ detection of B-mode polarization March 24th Tijmen de Haan (McGill) - Moriond

38 The Most Extreme Clusters A sufficiently massive cluster could falsify our understanding of cosmology and/or clusters SPT-CL J is unlikely at the 95% confidence level Improved constraints on its mass coming soon March 24th Tijmen de Haan (McGill) - Moriond

39 Projections for cluster surveys Current Future Weinberg et al March 24th Tijmen de Haan (McGill) - Moriond

40 Counting Galaxy Clusters Rare extreme peaks in the matter density field at Mpc scales Dark Energy No Dark Energy Borgani and Guzzo 2001 March 24th Tijmen de Haan (McGill) - Moriond

41 Counting Galaxy Clusters Abundance as a function of mass and redshift ( mass function ) is extremely sensitive to cosmological parameters 0.3 ΛCDM σ 8 Ω M Dark energy (w, w a ) Neutrino Masses m ν volume effect dn σ growth effect March 24th Tijmen de Haan (McGill) - Moriond

42 Cosmology Credit: ESA/C. Carreau March 24th Tijmen de Haan (McGill) - Moriond

43 Selection Function March 24th Tijmen de Haan (McGill) - Moriond

44 Log(Observed Mass Proxy) Log(Observed Mass Proxy) Selection Function P M ξ P(ξ M) Log(Cluster Mass) Log(Cluster Mass) Mantz et al (2010) March 24th Tijmen de Haan (McGill) - Moriond

45 March 24th Tijmen de Haan (McGill) - Moriond

Summary of Data Management Principles South Pole Telescope

Summary of Data Management Principles South Pole Telescope Experiment description - Where it is: The South Pole Telescope (SPT) is a 10-meter-diameter telescope located at the Amundsen-Scott South Pole