Abstract
We have examined dust emission in galaxy clusters at millimeter wavelengths using the Planck 857 GHz map to constrain the model based on Herschel observations that was used in studies for the Cosmic ORigins Explorer (CORE) mission concept. By stacking the emission from Planck-detected clusters, we estimated the normalization of the infrared luminosity versus mass relation and constrained the spatial profile of the dust emission. We used this newly constrained model to simulate clusters that we inject into Planck frequency maps. The comparison between clusters extracted using these gas+dust simulations and the basic gas-only simulations allows us to assess the impact of cluster dust emission on Planck results. In particular, we determined the impact on cluster parameter recovery (size, flux) and on Planck cluster cosmology results (survey completeness, determination of cosmological parameters). We show that dust emission has a negligible effect on the recovery of individual cluster parameters for the Planck mission, but that it impacts the cluster catalog completeness, reducing the number of detections in the redshift range [0.3–0.8] by up to ∼9%. Correcting for this incompleteness in the cosmological analysis has a negligible effect on cosmological parameter measurements: in particular, it does not ease the tension between Planck cluster and primary cosmic microwave background cosmologies.
Highlights
Quantifying dust emission from galaxy clusters is interesting for both astrophysical and cosmological studies
Dust emission from member galaxies is a tracer of the star formation rate (SFR) in dense environments (Alberts et al 2014, 2016), and the question of intracluster dust embedded in the hot intracluster medium (ICM) concerns stellar feedback and the physical state of the ICM (Montier & Giard 2004)
We investigate the impact of cluster dust emission on the Planck cluster catalog completeness, and on the measurement of cosmological parameters from cluster counts
Summary
Quantifying dust emission from galaxy clusters is interesting for both astrophysical and cosmological studies. The authors of the latter work combined IRAS data with Planck observations to measure dust temperature and determine dust masses in cluster systems. These studies extend the work of Montier & Giard (2005) and Giard et al (2008), who detected dust emission by stacking IRAS maps around clusters. We simulate Planck observations of clusters with both SZ signal and dust emission to quantify the effect of the dust emission on the Planck SZ selection function and photometry (size and SZ flux) in Sect. (7) and (9) of Planck Collaboration XX 2014) This allows us to compute the mass proxy of each object, M5Y0z0 (and the associated cluster size θ5Y0z0, since the redshift is known). We have 1091 objects with position, redshift z, mass M5Y0z0 and size θ5Y0z0
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