This website hosts data products associated with the sample of massive galaxy clusters selected via their Sunyaev-Zel'dovich effect signature from the 2500d SPT-SZ survey, the SPTpol 100d survey, and SPTpol Extended Cluster Survey. Here we report the locations (R.A, Dec. and redshift), selected mm-wave properties, and estimated masses for these clusters. The masses are determined using a variety of cluster observables and external datasets; more details are provided below.

Mass-Redshift Distribution of the SPT-SZ, the SPTpol 100d, and the SPT-ECS cluster samples: Here we compare the 2500 deg² SPT-SZ cluster catalog, the SPTpol 100d, and the SPT-ECS cluster sample to other SZ-selected cluster samples. Plotted are the estimated mass versus redshift for the 539 optically-confirmed clusters from the SPT-SZ catalog, 79 clusters from the SPTpol 100d sample, 448 SPT-ECS clusters, 220 clusters from the ACT survey (Marriage et al. 2011; Hasselfield et al. 2013, Hilton et al. 2017), and 1094 SZ-selected clusters from the Planck survey (Planck Collaboration et al. 2013, 2015) with M_500c > 1 x 10¹⁴ M_sun h^-1 . As described in Bleem et al. 2015 and Bocquet et al. 2019, the SPT-masses are determined using the best-fit ξ-Mass scaling relation for a flat LCDM cosmology with Ω_m = 0.3, h=0.7 and σ₈ = 0.8. (This figure is updated from Figure 6 in Bleem et al. 2015.)

Footprints of the SPT-SZ and SPTpol surveys. The footprint of the SPTpol Extended Cluster Survey is in dark blue, SPT-SZ in orange, and the SPTpol 500d survey in light blue.The footprint of the Dark Energy Survey is overplotted in green. (This is Figure 1 in Bleem et al. 2019.)

Redshift histogram of the three reported SPT cluster surveys. The number of clusters in each survey---with each cluster only reported once (so that e.g., clusters in both SPTpol 100d and SPT-SZ are only counted once)---are listed to the right of each survey name. The contribution from the SPTpol 100d survey is plotted on top in green right-diagonal hatch, the contribution from the SPT-ECS survey is plotted in red left-diagonal hatch, and the contribution to the total from the SPT-SZ survey is plotted in black right-diagonal hatch. Combined with these other two samples, the SPT-ECS sample brings the number of SZ-detected clusters reported by the SPT collaboration to over 1,000. (This is part of Figure 5 in Bleem et al. 2019.)

Completeness of the SPT-SZ Cluster Sample: Fractional completeness as a function of mass for the SPT cluster sample in three different redshift bins: 0.25 < z < 0.5 (solid black), 0.5 < z < 0.75 (dot-dashed red), z > 0.75 (dashed blue). This result is based upon the best-fit ξ-Mass scaling relation for a flat LCDM cosmology with Ω_m = 0.3, h=0.7 and σ₈ =0.8. The SPT sample is expected to be nearly 100% complete for M_500c >7×10¹⁴ h^-1 M_sun at z > 0.25. Adopting the best-fit Planck cosmology shifts the mass thresholds up ~17%. (This is Figure 7 in Bleem et al. 2015.)

Completeness of the SPTpol 100d Cluster sample: The estimated completeness as a function of M500c for the SPTpol 100d catalog. Completeness is estimated at four redshifts: 0.25, 0.50, 1.00, and 1.50. (This is Figure 5 in Huang et al. 2019.)

Weak-lensing calibrated cosmology constraints: νΛCDM constraints on Ω_m and σ₈. The SPTcl dataset comprises SPT-SZ+WL+Yx, Planck is TT+lowTEB, KiDS+GAMA and DES Y1 are cosmic shear+galaxy clustering+galaxy-galaxy-lensing. The WtG (X-ray selected clusters) result also contains their f_gas measurement. (This is Figure 6 in Bocquet et al. 2019.)

The evolution of σ₈ as a function of redshift. The red band shows the 1 sigma interval of the prediction obtained from Planck in the νΛCDM cosmology. The blue data points are obtained in a joint SPTcl+Planck analysis, where σ₈(z) is constrained only by the cluster sample. Orange data points are obtained from a similar analysis that allows for more freedom in the SZ scaling relation (see paper). The nearly horizontal error bars on the blue and orange data points indicate the extent of the redshift bins and are shaped to follow the evolution of σ₈ in the νΛCDM model. For comparison, green data points show constraints from the cross-correlation of the galaxy density in the Dark Energy Survey with CMB lensing from SPT (Giannantonio et al. 2016). (This is Figure 14 in Bocquet et al. 2019.)

The mass-lambda relation from the SPT-DES redMaPPer volume-limted sample evaluated for a fixed LCDM cosmology with Ω_m = 0.3, h=0.7, and σ₈ = 0.8. We find the relation to be 28% shallower than that from a weak-lensing analysis of the DES data (McClintock et al. 2019)---a difference significant at the 4 sigma level---with the relations intersecting at lambda = 60 . (This is Figure 11 in Bleem et al. 2019.)

Catalog	Reference	Description
SPTpol Extended Cluster Survey catalog	Bleem et al. (2019)	For each cluster candidate we provide the position, the highest detection significance in filtered SPT maps (and the core radii corresponding to the detection), redshift information and—for each confirmed cluster—a mass estimate. Where available we additionally provide an optical richness from the RM algorithm in "scanning" mode centered at the SPT location, the probability of false association with the RM targeted galaxy overdensity, flag if the estimated radio contamination exceeds 10% of the SZ signal, flag identified strong gravitational lenses, and---if applicable---provide lierature references for the strong lenses and spectroscopic redshifts. Masses are determined using the best-fit ξ-mass scaling relation for a flat LCDM cosmology with Ωm = 0.3, h=0.7 and σ8 = 0.8. The key to the imaging/redshift source is as follows: (1) Pan-STARRS1, (2) PISCO, (3) DES, (4) Magellan/Fourstar, (5) Spitzer/IRAC, (6) WISE, (7) literature photometric redshift, (8) spectroscopic redshift.
SPTpol 100d catalog	Huang et al. (2019)	For each cluster candidate we provide the position, the highest detection significance in filtered SPT maps (and the core radii corresponding to the detection), redshift information and—for each confirmed cluster—a mass estimate. Masses are determined using the best-fit ξ-mass scaling relation for a flat LCDM cosmology with Ωm = 0.3, h=0.7 and σ8 = 0.8.
SPT-SZ 2500d catalog (updated redshifts)	Bocquet et al. (2019)	Updated calibration of the photometric redshifts and additional spectroscopic redshifts. We provide updated mass estimates using the best-fit ξ-mass scaling relation for a flat LCDM cosmology with Ωm = 0.3, h=0.7 and σ8 = 0.8, and mass estimates marginalized over all scaling relation and cosmology parameters from the weak-lensing calibrated cosmology analysis.
Fiducial SPT-SZ 2500d catalog	Bleem et al. (2015)	For each cluster candidate we provide the position, the highest detection significance in filtered SPT maps (and the core radii corresponding to the detection), the integrated YSZ within a 0.75 arcmin aperture, redshift information and—for each confirmed cluster—a mass estimate. Masses are determined using the best-fit ξ-mass scaling relation for a flat LCDM cosmology with Ωm = 0.3, h=0.7 and σ8 = 0.8.

If you have any questions regarding these datasets or their use, please contact Lindsey Bleem (lbleem_at_anl.gov), Sebastian Bocquet (sebastian.bocquet_at_physik.lmu.de), or Nicholas Huang (ndhuang_at_berkeley.edu).

nuLCDM MCMC chain for the SPTcl dataset Cluster Cosmology Constraints from the 2500 deg2 SPT-SZ Survey: Inclusion of Weak Gravitational Lensing Data from Magellan and the Hubble Space Telescope Details of this chain can be found in Bocquet et. al 2019

SPT-SZ Likelihood Release from Cluster Cosmology Constraints from the 2500 deg2 SPT-SZ Survey: Inclusion of Weak Gravitational Lensing Data from Magellan and the Hubble Space Telescope. See also this Github repository and report issues here.

Data Release from NOAO Survey Program SPT-GMOS: A Gemini/GMOS-South Spectroscopic Survey of Galaxy Clusters in the SPT-SZ Survey Details of this program can be found in Bayliss et. al 2016

First SPT Spectroscopic Data Release Spectroscopy of Galaxies in Massive Clusters: Galaxy Properties and Dynamical Cluster Mass Calibration
Details of this program can be found in Ruel et. al 2014

Papers

Bleem et al. 2019 The SPTpol Extended Cluster Survey here

Huang et al. 2019 Galaxy Clusters Selected via the Sunyaev-Zel'dovich Effect in the SPTpol 100-Square-Degree Survey here

Bocquet et al. 2019 Cluster Cosmology Constraints from the South Pole Telescope 2500 deg2SZ Survey:Inclusion of Weak Gravitational Lensing Data from Magellan and the Hubble Space Telescope here

Bayliss et al. 2016 SPT-GMOS: A Gemini/GMOS-South Spectroscopic Survey of Galaxy Clusters in the SPT-SZ Survey here

de Haan et al. 2016 Cosmological Constraints from Galaxy Clusters in the 2500 square-degree SPT-SZ Survey here

Bleem et al. 2015 Galaxy Clusters Discovered via the Sunyaev-Zel'dovich Effect in the 2500-square-degree SPT-SZ survey here

Bocquet et al. 2015 Mass Calibration and Cosmological Analysis of the SPT-SZ Galaxy Cluster Sample Using Velocity Dispersion, σ_v, and X-ray Y_X Measurements here

Ruel et al. 2014. Optical Spectroscopy and Velocity Dispersions of Galaxy Clusters from the SPT-SZ Survey here