SZ Scaling Relations of Galaxy Groups and Clusters Near the North Ecliptic Pole

Pratt, Cameron T.; Bregman, Joel N.

doi:10.3847/1538-4357/ab6e6c

Cited by 12 publications

(9 citation statements)

References 57 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The mass zero point was calibrated with the virial masses of the most spectroscopically wellstudied clusters and groups in ORELSE, which generally had spectral fractions of > 50% and an average of 24 spectroscopic members per structure. The virial masses have been found to be comparable within the error bars of independent X-ray, lensing, and SZ measurements where available (see e.g., Clowe et al 1998;Margoniner et al 2004;Valtchanov et al 2004;Jee et al 2006;Maughan et al 2006;Muchovej et al 2007;Rzepecki et al 2007;Stott et al 2010;Piffaretti et al 2011;Laganá et al 2013;Pratt & Bregman 2020) as well as statistically consistent with the masses we estimate from the overdensity maps directly using the method described in Cucciati et al (2018). We refer the reader to §6.1 of Hung et al (2020) for further discussion of our mass calibration as well as comparisons with other mass estimation methods.…”

Section: Detection and Deblending In Sextractorsupporting

confidence: 75%

An Optical Observational Cluster Mass Function at $z\sim1$ with the ORELSE Survey

Hung,

Lemaux,

Gal

et al. 2021

Preprint

View full text Add to dashboard Cite

We present a new mass function of galaxy clusters and groups using optical/near-infrared wavelength spectroscopic and photometric data from the Observations of Redshift Evolution in Large-Scale Environments (ORELSE) survey. At 𝑧 ∼ 1, cluster mass function studies are rare regardless of wavelength and have never been attempted from an optical/near-infrared perspective. This work serves as a proof of concept that 𝑧 ∼ 1 cluster mass functions are achievable without supplemental X-ray or Sunyaev-Zel'dovich (SZ) data. Measurements of the cluster mass function provide important contraints on cosmological parameters and are complementary to other probes. With ORELSE, a new cluster finding technique based on Voronoi tessellation Monte-Carlo (VMC) mapping, and rigorous purity and completeness testing, we have obtained ∼240 galaxy overdensity candidates in the redshift range 0.55 < 𝑧 < 1.37 at a mass range of 13.6 < log(𝑀/𝑀 ) < 14.8. This mass range is comparable to existing optical cluster mass function studies for the local universe. Our candidate numbers vary based on the choice of multiple input parameters related to detection and characterization in our cluster finding algorithm, which we incorporated into the mass function analysis through a Monte-Carlo scheme. We find cosmological constraints on the matter density, Ω 𝑚 , and the amplitude of fluctuations, 𝜎 8 , of Ω 𝑚 = 0.250 +0.104 −0.099 and 𝜎 8 = 1.150 +0.260 −0.163 . While our Ω 𝑚 value is close to concordance, our 𝜎 8 value is ∼ 2𝜎 higher because of the inflated observed number densities compared to theoretical mass function models owing to how our survey targeted overdense regions. With Euclid and several other large, unbiased optical surveys on the horizon, VMC mapping will enable optical/NIR cluster cosmology at redshifts much higher than what has been possible before.

show abstract

Section: Detection and Deblending In Sextractorsupporting

confidence: 75%

An Optical Observational Cluster Mass Function at $z\sim1$ with the ORELSE Survey

Hung,

Lemaux,

Gal

et al. 2021

Preprint

View full text Add to dashboard Cite

show abstract

“…The virial masses have been found to be comparable within the error bars of independent X-ray, lensing, and SZ measurements where available (see e.g. Clowe et al 1998;Margoniner et al 2004;Valtchanov et al 2004;Jee et al 2006;Maughan et al 2006;Muchovej et al 2007;Rzepecki et al 2007;Stott et al 2010;Piffaretti et al 2011;Laganá et al 2013;Pratt & Bregman 2020) as well as statistically consistent with the masses we estimate from the overdensity maps directly using the method described in Cucciati et al (2018). We refer the reader to section 6.1 of Hung et al (2020) for further discussion of our mass calibration as well as comparisons with other mass estimation methods.…”

Section: Detection and Deblending In Sextractorsupporting

confidence: 75%

An optical observational cluster mass function at z ∼ 1 with the ORELSE survey

Hung

Lemaux

Gal

et al. 2021

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We present a new mass function of galaxy clusters and groups using optical/near-infrared wavelength spectroscopic and photometric data from the Observations of Redshift Evolution in Large-Scale Environments (ORELSE) survey. At z ∼ 1, cluster mass function studies are rare regardless of wavelength and have never been attempted from an optical/near-infrared perspective. This work serves as a proof of concept that z ∼ 1 cluster mass functions are achievable without supplemental X-ray or Sunyaev-Zel’dovich (SZ) data. Measurements of the cluster mass function provide important contraints on cosmological parameters and are complementary to other probes. With ORELSE, a new cluster finding technique based on Voronoi tessellation Monte Carlo (VMC) mapping, and rigorous purity and completeness testing, we have obtained ∼240 galaxy overdensity candidates in the redshift range 0.55 < z < 1.37 at a mass range of 13.6 < log (M/M⊙) < 14.8. This mass range is comparable to existing optical cluster mass function studies for the local universe. Our candidate numbers vary based on the choice of multiple input parameters related to detection and characterization in our cluster finding algorithm, which we incorporated into the mass function analysis through a Monte Carlo scheme. We find cosmological constraints on the matter density, Ωm, and the amplitude of fluctuations, σ8, of $\Omega _{m} = 0.250^{+0.104}_{-0.099}$ and $\sigma _{8} = 1.150^{+0.260}_{-0.163}$. While our Ωm value is close to concordance, our σ8 value is ∼2σ higher because of the inflated observed number densities compared to theoretical mass function models owing to how our survey targeted overdense regions. With Euclid and several other large, unbiased optical surveys on the horizon, VMC mapping will enable optical/NIR cluster cosmology at redshifts much higher than what has been possible before.

show abstract

“…The L X − Y SZ scaling relation has been studied in the past (e.g., Morandi et al 2007;Planck Collaboration et al 2011b,a;De Martino & Atrio-Barandela 2016;Ettori et al 2020;Pratt & Bregman 2020) mostly using Y SZ from Planck and L X from ROSAT data and the MCXC catalog. Both of these quantities are efficient proxies of the total cluster mass, they also scale with each other.…”

Section: The L X − T Relationmentioning

confidence: 99%

Cosmological implications of the anisotropy of ten galaxy cluster scaling relations

Migkas

Pacaud

Schellenberger

et al. 2021

A&A

View full text Add to dashboard Cite

The hypothesis that the late Universe is isotropic and homogeneous is adopted by most cosmological studies, including studies of galaxy clusters. The cosmic expansion rate H0 is thought to be spatially constant, while bulk flows are often presumed to be negligible compared to the Hubble expansion, even at local scales. The effects of bulk flows on the redshift–distance conversion are hence usually ignored. Any deviation from this consensus can strongly bias the results of such studies, and thus the importance of testing these assumptions cannot be understated. Scaling relations of galaxy clusters can be effectively used for this testing. In previous works, we observed strong anisotropies in cluster scaling relations, whose origins remain ambiguous. By measuring many different cluster properties, several scaling relations with different sensitivities can be built. Nearly independent tests of cosmic isotropy and large bulk flows are then feasible. In this work, we make use of up to 570 clusters with measured properties at X-ray, microwave, and infrared wavelengths to construct ten different cluster scaling relations and test the isotropy of the local Universe; to our knowedge, we present five of these scaling relations for the first time. Through rigorous and robust tests, we ensure that our analysis is not prone to generally known systematic biases and X-ray absorption issues. By combining all available information, we detect an apparent 9% spatial variation in the local H0 between (l, b)∼(280°−35°+35°, −15°−20°+20°) and the rest of the sky. The observed anisotropy has a nearly dipole form. Using isotropic Monte Carlo simulations, we assess the statistical significance of the anisotropy to be > 5σ. This result could also be attributed to a ∼900 km s−1 bulk flow, which seems to extend out to at least ∼500 Mpc. These two effects will be indistinguishable until more high-z clusters are observed by future all-sky surveys such as eROSITA.

show abstract

SZ Scaling Relations of Galaxy Groups and Clusters Near the North Ecliptic Pole

Cited by 12 publications

References 57 publications

An Optical Observational Cluster Mass Function at $z\sim1$ with the ORELSE Survey

An Optical Observational Cluster Mass Function at $z\sim1$ with the ORELSE Survey

An optical observational cluster mass function at z ∼ 1 with the ORELSE survey

Cosmological implications of the anisotropy of ten galaxy cluster scaling relations

Contact Info

Product

Resources

About