Optical follow-up study of 32 high-redshift galaxy cluster candidates from Planck with the William Herschel Telescope

Zohren, H.; Schrabback, T.; Burg, R. F. J. van der; Arnaud, M.; Melin, Jean-Baptiste; Busch, Jan Luca van den; Hoekstra, Henk; Klein, Matthias

doi:10.1093/mnras/stz1838

“…In the PSZ2 catalog, 63 entries out of 309 are without redshift and mass estimates, meaning that they were not confirmed detections at the time of their publication. However, in follow-up optical studies by Buddendiek et al (2015), Burenin (2017), Burenin et al (2018), Barrena et al (2018), Streblyanska et al (2018), Streblyanska et al (2019), Aguado-Barahona et al (2019), Boada et al (2019), and Zohren et al (2019), redshifts have been obtained for 35 of these 63 Planck detections. From these redshifts we computed M 500 by interpolating the M 500 versus z curves provided in the PSZ2 individual algorithm catalogs for each detection (see Appendix D in Planck Collaboration XXVII 2016).…”

Section: Cluster Samplementioning

confidence: 99%

The Planck clusters in the LOFAR sky. I. LoTSS-DR2: new detections and sample overview

Botteon,

Shimwell,

Cassano

et al. 2022

Preprint

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Context. Relativistic electrons and magnetic fields permeate the intra-cluster medium (ICM) and manifest themselves as diffuse sources of synchrotron emission observable at radio wavelengths, namely radio halos and radio relics. Although there is broad consensus that the formation of these sources is connected to turbulence and shocks in the ICM, the details of the required particle acceleration, the strength and morphology of the magnetic field in the cluster volume, and the influence of other sources of high-energy particles are poorly known. Aims. Sufficiently large samples of radio halos and relics, which would allow us to examine the variation among the source population and pinpoint their commonalities and differences, are still missing. At present, due to the physical properties of the sources and the capabilities of existing facilities, large numbers of these sources are easiest to detect at low radio frequencies, where they shine brightly. Methods. We examined the low-frequency radio emission from all 309 clusters in the second catalog of Planck Sunyaev Zel'dovich detected sources that lie within the 5634 deg 2 covered by the Second Data Release of the LOFAR Two-meter Sky Survey (LoTSS-DR2). We produced LOFAR images at different resolutions, with and without discrete sources subtracted, and created overlays with optical and X-ray images before classifying the diffuse sources in the ICM, guided by a decision tree. Results. Overall, we found 83 clusters that host a radio halo and 26 that host one or more radio relics (including candidates). About half of them are new discoveries. The detection rate of clusters that host a radio halo and one or more relics in our sample is 30 ± 11% and 10 ± 6%, respectively. Extrapolating these numbers, we anticipate that once LoTSS covers the entire northern sky it will provide the detection of 251 ± 92 clusters that host a halo and 83 ± 50 clusters that host at least one relic from Planck clusters alone. All images and results produced in this work are publicly available via the project website.

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“…[49]) and are still been continuously refined (e.g. [50,51]). Therefore, the redshifts of some of these clusters have further been updated after the publication of the Planck SZ2 catalog.…”

Section: For Planck Esz Samplementioning

confidence: 99%

A model-independent test of the evolution of gas depletion factor for SPT-SZ and Planck ESZ clusters

Bora

¹

,

Desai

²

2021

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The gas mass fraction in galaxy clusters has been widely used to determine cosmological parameters. This method assumes that the ratio of the cluster gas mass fraction to the cosmic baryon fraction ($$\gamma (z)$$ γ ( z ) ) is constant as a function of redshift. In this work, we look for a time evolution of $$\gamma (z)$$ γ ( z ) at $$R_{500}$$ R 500 by using both the SPT-SZ and Planck Early SZ (ESZ) cluster data, in a model-independent fashion without any explicit dependence on the underlying cosmology. For this calculation, we use a non-parametric functional form for the Hubble parameter obtained from Gaussian Process regression using cosmic chronometers. We parameterize $$\gamma (z)$$ γ ( z ) as: $$\gamma (z)= \gamma _0(1+\gamma _1 z)$$ γ ( z ) = γ 0 ( 1 + γ 1 z ) to constrain the redshift evolution. We find contradictory results between both the samples. For SPT-SZ, $$\gamma (z)$$ γ ( z ) decreases as a function of redshift (at more than 5$$\sigma $$ σ ), whereas a positive trend with redshift is found for Planck ESZ data (at more than 4$$\sigma $$ σ ). We however find that the $$\gamma _1$$ γ 1 values for a subset of SPT-SZ and Planck ESZ clusters between the same redshift interval agree to within $$1\sigma $$ 1 σ . When we allow for a dependence on the halo mass in the evolution of the gas depletion factor, the $$4-5\sigma $$ 4 - 5 σ discrepancy reduces to $$2\sigma $$ 2 σ .

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“…At higher redshifts (z 1), optical weak lensing becomes increasingly difficult due to a dearth of background galaxies and difficulties in measuring their shape with blending and lower signal to noise. High-redshift mass information is important as there are suggestions that scaling relations calibrated at lower redshifts may mis-estimate the masses at higher redshifts (Zohren et al 2019;Salvati et al 2018Salvati et al , 2019.…”

Section: Introductionmentioning

confidence: 99%

Improving cosmological constraints from galaxy cluster number counts with CMB-cluster-lensing data: Results from the SPT-SZ survey and forecasts for the future

Chaubal,

Reichardt,

Gupta

et al. 2021

Preprint

0

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We show the improvement to cosmological constraints from galaxy cluster surveys with the addition of CMB-cluster lensing data. We explore the cosmological implications of adding mass information from the 3.1 σ detection of gravitational lensing of the cosmic microwave background (CMB) by galaxy clusters to the Sunyaev-Zel'dovich (SZ) selected galaxy cluster sample from the 2500 deg 2 SPT-SZ survey and targeted optical and X-ray followup data. In the ΛCDM model, the combination of the cluster sample with the Planck power spectrum measurements prefers σ 8 (Ω m /0.3) 0.5 = 0.831 ± 0.020. Adding the cluster data reduces the uncertainty on this quantity by a factor of 1.4, which is unchanged whether or not the 3.1 σ CMB-cluster lensing measurement is included. We then forecast the impact of CMBcluster lensing measurements with future cluster catalogs. Adding CMB-cluster lensing measurements to the SZ cluster catalog of the on-going SPT-3G survey is expected to improve the expected constraint on the dark energy equation of state w by a factor of 1.3 to σ(w) = 0.19. We find the largest improvements from CMB-cluster lensing measurements to be for σ 8 , where adding CMB-cluster lensing data to the cluster number counts reduces the expected uncertainty on σ 8 by factors of 2.4 and 3.6 for SPT-3G and CMB-S4 respectively.

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Optical follow-up study of 32 high-redshift galaxy cluster candidates from Planck with the William Herschel Telescope

Cited by 12 publications

References 60 publications

The Planck clusters in the LOFAR sky. I. LoTSS-DR2: new detections and sample overview

The Planck clusters in the LOFAR sky. I. LoTSS-DR2: new detections and sample overview

A model-independent test of the evolution of gas depletion factor for SPT-SZ and Planck ESZ clusters

Improving cosmological constraints from galaxy cluster number counts with CMB-cluster-lensing data: Results from the SPT-SZ survey and forecasts for the future

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