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NSF, National Science Foundation

KICP, Kavli Institute for Cosmological Physics

USAP, United States Antarctic Program

Antarctic Support Contract (ASC)

DOE Office of Science High Energy Physics



Related Websites

CBI, Cosmic Background Imager

DASI, Degree Angular Scale Interferometer

WMAP, Wilkinson Microwave Anisotropy Probe

Planck



 
Overview
Figures
Catalog and Cosmology Products
Additional Resources
Quick Links
 

Overview

 

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. This sample is presented in Bleem et al. 2015 (ApJS, 216, 27; arXiv:1409.0850). 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.

If you have any questions regarding this data set or its use, please contact Lindsey Bleem (bleeml_at_uchicago_edu).

 
 

Figures

 

Mass-Redshift Distribution of the SPT-SZ cluster sample: Here we compare the 2500 deg2 SPT-SZ cluster catalog to other X-ray and SZ-selected cluster samples. Plotted are the estimated mass versus redshift for the 516 optically-confirmed clusters from the SPT catalog, 91 clusters from the ACT survey (Marriage et al. 2011; Hasselfield et al. 2013), 809 SZ-selected clusters from the Planck survey (Planck Collaboration et al. 2013) and 740 X-ray clusters selected from the ROSAT all-sky survey (Piffaretti et al. 2011) with M500c > 1 × 1014 Msun h-1 . We mark as lower limits the redshifts of the three high-redshift SPT systems for which the Spitzer redshift-model is poorly constrained (black triangles). We plot clusters in common between the datasets multiple times, using the masses and redshifts reported for each catalog. As described in Bleem et al. 2015, the SPT-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. (This is Figure 6 in Bleem et al. 2015.)

 



Completeness of the 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 Ωm = 0.3, h=0.7 and σ8 =0.8. The SPT sample is expected to be nearly 100% complete for M500c >7×1014 h-1 Msun 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.)

 
 
 

Catalog and Cosmology Products

 

The 2500d SPT-SZ Cluster Sample
The cluster sample, as reported in Bleem et al. 2015, can be found here. 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. We also provide masses for the best-fit Planck cosmology here.

If you have any questions regarding this data set or its use, please contact Lindsey Bleem (bleeml_at_uchicago.edu)

Velocity Dispersion-Based Mass Estimates
Using the metholodogy presented in Bocquet et al. 2015 (ApJ, 799, 214; astro-ph/1407.2942 ) we provide masses derived from a velocity dispersion-based mass calibration for the confirmed clusters in the 2500d SPT-SZ cluster sample. These mass estimates are marginalized over both cosmological and scaling relation parameters; the best fit values of these parameters can be found in Table 1 in Bocquet et al. 2014. In particular publish here masses derived using the 720d SPT cluster sample (Reichardt et al. 2013 ApJ 763), the BBN, H0 priors and 63 SPT clusters with velocity dispersion measurements. The cluster table with dispersion-based masses is found here.

If you have any questions regarding this data set or its use, please contact Sebastian Bocquet (bocquet_at_usm.lmu.de)

Coming Soon:

X-ray- & Weak-Lensing- Based Mass Estimates
In addition to velocity dispersion measurements, the SPT collaboration has undertaken a multi-wavelength campaign to obtain X-ray and weak lensing measurements for ~50-100 clusters per technique. Estimates of cluster masses marginalized over both cosmological and scaling relation parameters and incorporating follow-up X-ray data from a large Chandra X-ray Visionary Project will be posted in conjunction with de Haan et al (in preparation), and weak-lensing based mass calibrations will also be provided in future updates.


 
 

Additional Resources

 

Data Release from NOAO Survey Program: "Spectroscopy of Galaxies in Massive Clusters: Galaxy Properties and Dynamical Cluster Mass Calibration" link
Details of this program can be found in Ruel et. al 2014; here

 
 

Quick Links

 

Papers

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, σv, and X-ray YX Measurements here
Ruel et al. 2014. Optical Spectroscopy and Velocity Dispersions of Galaxy Clusters from the SPT-SZ Survey here


Data Products

The SPT-SZ 2500d cluster sample as presented in Bleem et al. 2015 here.
The SPT-SZ 2500d cluster sample with masses derived using the best-fit Planck cosmology here.
Velocity-dispersion based mass estimates for the sample derived using the metholodgy of Bocquet et al. 2015 here.


 
 
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Contact:

   

jchyde.uchicago.edu

Webmaster:

   

egaltsevakicp.uchicago.edu

Last update:

   

September 7, 2011