SPT-SZ Cluster Likelihood

This is the likelihood code used to produce the results obtained from the SPT-SZ cluster sample with weak-lensing follow-up data from Magellan/Megacam and HST and X-ray follow-up data from Chandra, as presented in Bocquet et al. (2019).

Quickstart

The code is meant to be used within the [CosmoSIS framework] (https://bitbucket.org/joezuntz/cosmosis)

To reproduce the baseline SPTcl results, just run CosmoSIS using the setup file setup_nuLCDM_SPTcl.ini that is provided with this likelihood code.

(A Little) More Details

This package contains three modules (in the CosmoSIS sense):

• compute_HMF computes the halo mass function on a grid of redshifts and masses
• abundance computes the likelihood of the cluster abundance (SPT-SZ SNR and redshifts)
• mass_calibration computes the likelihood using the clusters' follow-up mass calibration data Take a look at the three .yaml files and reach out to me if you have further questions.

References

• Cluster cosmology constraints and analysis pipeline: Bocquet et al. 2019, DOI 10.3847/1538-4357/ab1f10
• SPT-SZ cluster catalog: Bleem et al. 2015, DOI 10.1088/0067-0049/216/2/27
• Weak-lensing dataset from the Hubble Space Telescope (HST-13): Schrabback et al. 2018, DOI 10.1093/mnras/stx2666
• Weak-lensing dataset from the Hubble Space Telescope (HST-30): Schrabback et al. 2021, DOI 10.1093/mnras/stab1386
• Weak-lensing dataset from Magellan/Megacam: Dietrich et al. 2019, DOI 10.1093/mnras/sty3088
• X-ray Chandra dataset: McDonald et al. 2013, DOI 10.1088/0004-637X/774/1/23
• X-ray Chandra z>1.2 dataset: McDonald et al. 2017, DOI 10.3847/1538-4357/aa7740