Spectroscopic Confirmation and Velocity Dispersions for 20 Planck Galaxy Clusters at 0.16 &lt; z &lt; 0.78

Amodeo, Stefania; Mei, S.; Stanford, S. A.; Lawrence, C. R.; Bartlett, J. G.; Stern, Daniel; Chary, R.-R.; Shim, Hyunjin; Marleau, F.; Melin, Jean-Baptiste; Rodríguez‐Gonzálvez, Carmen

doi:10.3847/1538-4357/aa98dd

Cited by 16 publications

(12 citation statements)

References 38 publications

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“…The works by Amodeo et al (2018) and Burenin et al (2018) report precise spectroscopic redshifts for PSZ2 clusters, which are in part also included in our sample. Their spectroscopic information helps us with recalibrating our red-sequence models.…”

Section: Discussionmentioning

confidence: 99%

“…As a result, we obtain photometric redshifts which allow us to estimate the richness and richnessbased mass from our observations. Additionally, we can infer the SZ-based mass and therefore supplement the spectroscopic redshift information from Amodeo et al (2018) and Burenin et al (2018).…”

Section: Discussionmentioning

confidence: 99%

“…Burenin et al (2018) measured spectroscopic redshifts with the BTA 6-m telescope using the instruments SCORPIO and SCORPIO-2 for five of the clusters in our sample, namely PSZ2 G092.69+59.92, PSZ2 G126.28+65.62, PSZ2 G126.57+51.6, PSZ2 G237.68+57.83 and PSZ2 G343.46+52.65. Amodeo et al (2018) provide a spectroscopic redshift for PSZ2 G085.95+25.23 with Keck/LRIS spectroscopy. Streblyanska et al (2018) list spectroscopic redshifts originating from the SDSS DR12 spectroscopic information for PSZ2 G032.31+66.07 and PSZ2 G086.28+74.76.…”

Section: Calibration Of the Redshift Estimatementioning

confidence: 99%

“…It contains SZ-detections down to a significance of signal-to-noise ratio S/N ≥ 4.5. The follow-up and verification process is ongoing (Liu et al 2015;Planck Collaboration et al 2016b;van der Burg et al 2016;Burenin et al 2018;Amodeo et al 2018;Barrena et al 2018;Streblyanska et al 2018;Boada et al 2018), but still incomplete, especially at high redshifts. The primary goal of this work is to help complete the follow-up of cluster candidates in the PSZ2 catalogue at high redshifts z 0.7 with the help of optical data from the William Herschel Telescope.…”

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confidence: 99%

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

Zohren

Schrabback

Burg

et al. 2019

Monthly Notices of the Royal Astronomical Society

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Abstract The Planck satellite has detected cluster candidates via the Sunyaev Zel’dovich (SZ) effect, but the optical follow-up required to confirm these candidates is still incomplete, especially at high redshifts and for SZ detections at low significance. In this work, we present our analysis of optical observations obtained for 32 Planck cluster candidates using ACAM on the 4.2-m William Herschel Telescope. These cluster candidates were pre-selected using SDSS, WISE, and Pan-STARRS images to likely represent distant clusters at redshifts z ≳ 0.7. We obtain photometric redshift and richness estimates for all of the cluster candidates from a red-sequence analysis of r-, i-, and z-band imaging data. In addition, long-slit observations allow us to measure the redshifts of a subset of the clusters spectroscopically. The optical richness is often lower than expected from the inferred SZ mass when compared to scaling relations previously calibrated at low redshifts. This likely indicates the impact of Eddington bias and projection effects or noise-induced detections, especially at low-SZ significance. Thus, optical follow-up not only provides redshift measurements, but also an important independent verification method. We find that 18 (7) of the candidates at redshifts z > 0.5 (z > 0.8) are at least half as rich as expected from scaling relations, thereby clearly confirming these candidates as massive clusters. While the complex selection function of our sample due to our pre-selection hampers its use for cosmological studies, we do provide a validation of massive high-redshift clusters particularly suitable for further astrophysical investigations.

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Section: Discussionmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

Section: Calibration Of the Redshift Estimatementioning

confidence: 99%

mentioning

confidence: 99%

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

Zohren

Schrabback

Burg

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…One of the main aims of this work is to characterize this mass bias for the PSZ2 sample in the case of dynamical masses, in order to obtain unbiased SZ masses which could be used for cosmological studies. The estimation of the mass bias has been studied recently by a large number of groups in the community: Ruel et al (2014), Sifón et al (2016) and Amodeo et al (2018) using SZ and dynamical masses; or von der Linden et al ( 2014), Hoekstra et al (2015), Smith et al (2016), Battaglia et al (2016), Sereno et al (2017), Penna-Lima et al (2017), Medezinski et al (2018) and Miyatake et al (2019) using SZ and weak-lensing masses.…”

Section: Introductionmentioning

confidence: 99%

Velocity dispersion and dynamical masses for 388 Galaxy Clusters and groups. Calibrating the $M_{\rm SZ}$--$M_{\rm dyn}$ scaling relation for the PSZ2 sample

Aguado-Barahona,

Rubino-Martin,

Ferragamo

et al. 2021

Preprint

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The second catalogue of Planck Sunyaev-Zeldovich (SZ) sources, hereafter PSZ2, represents the largest galaxy cluster sample selected by means of their SZ signature in a full-sky survey. Using telescopes at the Canary Island observatories, we conducted the longterm observational program 128-MULTIPLE-16/15B (hereafter LP15), a large and complete optical follow-up campaign of all the unidentified PSZ2 sources in the northern sky, with declinations above −15 • and no correspondence in the first Planck catalogue PSZ1. This paper is the third and last in the series of LP15 results, after Streblyanska et al. ( 2019) and Aguado-Barahona et al. (2019), and presents all the spectroscopic observations of the full program. We complement these LP15 spectroscopic results with Sloan Digital Sky Survey (SDSS) archival data and other observations from a previous program (ITP13-08), and present a catalog of 388 clusters and groups of galaxies including estimates of their velocity dispersion. The majority of them (356) are the optical counterpart of a PSZ2 source. A subset of 297 of those clusters is used to construct the M SZ − M dyn scaling relation, based on the estimated SZ mass from Planck measurements and our dynamical mass estimates. We discuss and correct for different statistical and physical biases in the estimation of the masses, such as the Eddington bias when estimating M S Z and the aperture and the number of galaxies used to calculate M dyn . The SZ-to-dynamical mass ratio for those 297 PSZ2 clusters is (1 − B) = 0.80 ± 0.04 (stat) ±0.05 (sys), with only marginal evidence for a possible mass dependence of this factor. Our value is consistent with previous results in the literature, but presents a significantly smaller uncertainty due to the use of the largest sample size for this type of studies.

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Bayesian recalibration ofPlanckgalaxy cluster scaling relations including relativistic Sunyaev-Zel’dovich corrections

Perrott

2024

Publ. Astron. Soc. Aust.

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We investigate the impact of relativistic SZ corrections on Planck measurements of massive galaxy clusters, finding that they have a significant impact at the $\approx$ 5–15% and up to $\approx$ 3 $\sigma$ level. We investigate the possibility of constraining temperature directly from these SZ measurements but find that only weak constraints are possible for the most significant detections; for most clusters, an external temperature measurement is required to correctly measure integrated Compton-y. We also investigate the impact of profile shape assumptions and find that these have a small but non-negligible impact on measured Compton-y, at the $\approx$ 5% level. Informed by the results of these investigations, we recalibrate the Planck SZ observable-mass scaling relation, using the updated NPIPE data release and a larger sample of X-ray mass estimates. Along with the expected change in the high-mass end of the scaling relation, which does not impact Planck mass estimation, we also find hints of a low-mass deviation, but this requires better understanding of the selection function in order to confirm.

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Spectroscopic Confirmation and Velocity Dispersions for 20 Planck Galaxy Clusters at 0.16 < z < 0.78

Cited by 16 publications

References 38 publications

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

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

Velocity dispersion and dynamical masses for 388 Galaxy Clusters and groups. Calibrating the $M_{\rm SZ}$--$M_{\rm dyn}$ scaling relation for the PSZ2 sample

Bayesian recalibration ofPlanckgalaxy cluster scaling relations including relativistic Sunyaev-Zel’dovich corrections

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