Cosmological Constraints from the XMM Cluster Survey (XCS) Martin Sahlén, for the XMM Cluster Survey Collaboration The Oskar Klein Centre for

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1 Cosmological Constraints from the XMM Cluster Survey (XCS) Martin Sahlén, for the XMM Cluster Survey Collaboration The Oskar Klein Centre for Cosmoparticle Physics Stockholm University

2 Key Points The XCS is the XMM-Newton equivalent of the ROSAT 400d survey; largest X-ray cluster survey to date (factor 4) Major potential for e.g. Cluster discovery Scaling relations Cosmology: ~2x on Ω m, σ 8, Σm ν & f NL > 30 might be testable Calibration of future surveys First data release (XCS-DR1) available Upcoming x2 Cosmological constraints constraints on e.g. from Ωthe M XCS, σ 8 /, M. w, Sahlén m ν, / γ, msa@fysik.su.se f NL 2/26

3 Complete XMM-Newton archive (serendipitous) >6000 observations, ~600 sq. deg. Science goals Find galaxy clusters Constrain cosmology using galaxy clusters Study redshift evolution of cluster gas (scaling relations) Study galaxy evolution in clusters Study properties of unusual X-ray sources, e.g. high-redshift quasars and isolated neutron stars Cosmological constraints from the XCS / M. Sahlén / msa@fysik.su.se 3/26

4 Cluster Finding X-ray temperature, flux, redshift, spatial parameters Flux limit: ~5 x erg s -1 cm -2 z max = 1.46 (so far) Final area: ~500 sq. deg. Several thousand clusters expected (3675 extended-source candidates so far) Targeted pointings excluded for cosmology (but useful for mass calibration) Cosmological constraints from the XCS / M. Sahlén / msa@fysik.su.se 4/26

5 Lloyd-Davies et al., arxiv: XMM observation pointings Green = DES footprint Area within red dashed lines (Galactic plane + Magellanic clouds) not used for clusters Cosmological constraints from the XCS / M. Sahlén / msa@fysik.su.se 5/26

6 XCS Data Release 1 Mehrtens et al. (2011) MNRAS submitted, arxiv: optically confirmed clusters (largest homogeneous X-ray cluster sample) 464 with redshift estimate 402 with temperature measurement 255 previously unknown clusters, 356 new to X-ray z>1: 10, T>5 kev: 67 Cosmological constraints from the XCS / M. Sahlén / msa@fysik.su.se 6/26

7 Current X-Ray Cluster Surveys Cosmological constraints from the XCS / M. Sahlén / msa@fysik.su.se 7/26

8 Current X-Ray Cluster Surveys Cosmological constraints from the XCS / M. Sahlén / msa@fysik.su.se 8/26

9 XCS-DR1 L T Relation 402 clusters Selection not included (L X -T X data not yet public) Most accurate L-T measurement to date valuable calibration for other surveys Lloyd-Davies et al, in prep. Cosmological constraints from the XCS / M. Sahlén / msa@fysik.su.se 9/26

10 0.1 < z < 0.3 T > 2 kev >300 counts 121 sq. deg. Measurement errors ignored First comparison: SDSS DR7 XCS-DR1 overlap Observed clusters (SDSS DR7 overlap) Expected means, WMAP7 cosmology 41 6 observed, 36 expected mean 5 M.S. et al., in prep z Cosmological constraints from the XCS / M. Sahlén / msa@fysik.su.se 10/26

11 0.1 < z < 0.3 T > 2 kev >300 counts 121 sq. deg. Measurement errors ignored First comparison: SDSS DR7 XCS-DR1 overlap Observed clusters (SDSS DR7 overlap) Expected means, WMAP7 cosmology 41 6 observed, 36 expected mean 5 M.S. et al., in prep T X [kev] Cosmological constraints from the XCS / M. Sahlén / msa@fysik.su.se 11/26

12 FORECASTS WORK IN PROGRESS Cosmological constraints from the XCS / M. Sahlén / msa@fysik.su.se 12/26

13 Predicted Detected Distributions XCS 500 Flat ΛCDM, Ω m = 0.3, σ 8 =0.8 T>2 kev, >500 photons M.S., P. Viana, A. Liddle, K. Romer et al Cosmological constraints from the XCS / M. Sahlén / msa@fysik.su.se 13/26

14 Forecast Constraints Self-Calibrated L-T Relation w/ Scatter XCS 500 Results Self-calibration σ(ω of L-T m ) < 0.03 σ(σ 8 ) < 0.05 Note: not using flux measurements Fixed M-T (HIFLUGCS), 0.1 < z < 1 4 L-T parameters marginalized over Number counts only (serendipitous) M.S., P. Viana, A. Liddle, K. Romer et al Cosmological constraints from the XCS / M. Sahlén / msa@fysik.su.se 14/26

15 Mean # clusters in bin ( z=0.05) Predicted Detected Distributions XCS 300 Self-similar L-T relation Constant L-T relation Flat ΛCDM, Ω m = 0.266, σ 8 =0.801 T>2 kev, >300 photons ~300 photons limit for small T (hence M) uncertainties ~3/4 increase in clusters by lowering the threshold z Cosmological constraints from the XCS / M. Sahlén / msa@fysik.su.se 15/26 M.S. et al., in prep.

16 XCS 300 Forecast: ΛCDM Fiducial model Ω M = Ω b = h = 0.71 σ 8 = n S = σ(α M-T ) = 15% σ8 = 0.80 ± 0.01, ±0.02 Ω M = ± 0.005, ±0.010 Varying σ 8 Ω M α M-T m m α M-T is the normalization of the mass temperature (M T) relation, here used to illustrate many possible mass-calibration uncertainties M.S. et al., in prep. Cosmological constraints from the XCS / M. Sahlén / msa@fysik.su.se 16/26

17 Comparison to Current Results Works of 400d (Vikhlinin et al. 2009) and Allen group (Mantz et al. 2010) set a gold standard In a like-for-like comparison, we expect an improvement in constraints by a factor ~2 (based on numbers) or more (redshift coverage) Mantz et al. find σ(ω M ) = 0.04, σ(σ 8 ) = 0.05, which matches this expectation quite well Cosmological constraints from the XCS / M. Sahlén / msa@fysik.su.se 17/26

18 Forecast: m /ev XCS 300 Neutrino masses Σm ν /ev < 0.86 (0.95), 95% CL σ 8 = 0.80 ± 0.01, ±0.02 Ω M = 0.27 ± 0.01, ±0.02 Fiducial model Ω M = Ω b = Σm ν = 0.0 ev h = 0.71 σ 8 = n S = σ(α M-T ) = 15% Fitting σ 8 Ω M Σm ν α M-T m Work in progress, ultimately expect x2 improvement on CMB+clusters constraint m m /ev M.S. et al., in prep. Cosmological constraints from the XCS / M. Sahlén / msa@fysik.su.se 18/26

19 Forecast: Neutrino masses m /ev XCS Σm ν /ev= 1.00 ± 0.40, ±0.43 σ 8 = 0.80 ± 0.02, ±0.03 Ω M = 0.27 ± 0.02, ±0.03 Fiducial model Ω M = Ω b = Σm ν = 1.0 ev h = 0.71 σ 8 = n S = σ(α M-T ) = 15% Fitting σ 8 Ω M Σm ν α M-T m Work in progress, ultimately expect x2 improvement on CMB+clusters constraint m m /ev M.S. et al., in prep. Cosmological constraints from the XCS / M. Sahlén / msa@fysik.su.se 19/26

20 XCS 300 Forecast: Non-Gaussianity f NL = 0 ± 16, ±51 f NL = 90 ± 16, ±52 Fiducial model Ω M = Ω b = h = 0.71 σ 8 = n S = f NL = 0 and 90 σ(α M-T ) = 15% Fitting f NL α M-T local f NL Here using XCS 300 clusters up to z = local f NL M.S. et al., in prep. Cosmological constraints from the XCS / M. Sahlén / msa@fysik.su.se 20/26

21 Other work in preparation: The Bayes Diet Bias! for overweight galaxy clusters M obs = 7.7 ± 1.1 x h -1 M solar Can t idealize selection! M obs = 7.7 ± 3.7 x h -1 M solar M t ~ 5.8 x h -1 M solar Mass [10 15 h -1 M solar ] Mass [10 15 h -1 M solar ] M.S., in prep. Cosmological constraints from the XCS / M. Sahlén / msa@fysik.su.se 21/26

22 Conclusions The XMM Cluster Survey has released XCS- DR1, publicly available at It is the largest homogeneous X-ray cluster sample to date, with 503 clusters, extending to high redshifts We find (in SDSS DR7 overlap) a distribution of clusters that agrees with a WMAP7 ΛCDM cosmology Cosmological constraints from the XCS / M. Sahlén / msa@fysik.su.se 22/26

23 Conclusions First cosmological constraints this year; next year considerable improvement [σ 8, Ω m, w, m ν, f NL, γ, ] With strong priors on Ω b, h, n S : Parameter Best-case σ Worst-case(?) σ Ω m ~ 0.02 ~ 0.03 σ 8 ~ 0.01 ~ 0.03 Σm ν * ~ 0.4 ev ~ 0.5 ev * but using e.g. full CMB covariance considerably better Cosmological constraints from the XCS / M. Sahlén / msa@fysik.su.se 23/26

24 Conclusions With strong priors on Ω b, h, Ω M & σ 8, n S : Parameter Best-case σ Worst-case(?) σ f NL ~ 15 ~ 50 Detailed constraints and forecasts in prep. Claims of too massive clusters often based on heavily biased mass estimates; in my opinion most likely no tension with ΛCDM Cosmological constraints from the XCS / M. Sahlén / msa@fysik.su.se 24/26

25 Other ideas Forecasts for e.g. XXL, erosita Quintessence models Public CosmoMC cluster module Cosmological constraints from the XCS / M. Sahlén / msa@fysik.su.se 25/26

26 THANK YOU Cosmological constraints from the XCS / M. Sahlén / msa@fysik.su.se 26/26

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