SPIDERS: an overview of the largest catalogue of spectroscopically confirmed x-ray galaxy clusters

Kirkpatrick, C. C.; Clerc, N.; Finoguenov, A.; Damsted, S.; Chitham, J. Ider; Kukkola, A.; Gueguen, A.; Furnell, K.; Rykoff, E. S.; Comparat, Johan; Saro, A.; Capasso, R.; Padilla, Nelson; Erfanianfar, G.; Mamon, G. A.; Collins, Chris; Merloni, A.; Brownstein, Joel R.; Schneider, Donald P.

doi:10.1093/mnras/stab127

Cited by 25 publications

(17 citation statements)

References 69 publications

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“…Better constraints on the velocity dispersion are obtained using scaling relations of LX −M200 (Leauthaud et al, 2010) and M200 − σv,VT (Carlberg et al, 1997). The lognormal scatter LX − σv,VT relation is measured to be 0.13 by Kirkpatrick et al (2021). Using the velocity dispersion from scaling relations, the disagreement with simulations consists in a wider tail above 0.7σ extending to 2.5σ.…”

Section: Comparison With Cosmological Simulationsmentioning

confidence: 98%

Radio galaxies in galaxy groups: kinematics, scaling relations, and AGN feedback

Pasini

Finoguenov

Brüggen

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We investigate the kinematic properties of a large (N=998) sample of COSMOS spectroscopic galaxy members distributed among 79 groups. We identify the Brightest Group Galaxies (BGGs) and cross-match our data with the VLA-COSMOS Deep survey at 1.4 GHz, classifying our parent sample into radio/non-radio BGGs and radio/non-radio satellites. The radio luminosity distribution spans from LR ∼ 2 × 1021 W Hz−1 to LR ∼ 3 × 1025 W Hz−1. A phase-space analysis, performed by comparing the velocity ratio (line-of-sight velocity divided by the group velocity dispersion) with the galaxy-group centre offset, reveals that BGGs (radio and non-radio) are mostly (∼80 per cent) ancient infallers. Furthermore, the strongest (LR > 1023 W Hz−1) radio galaxies are always found within 0.2Rvir from the group centre. Comparing our samples with HORIZON-AGN, we find that the velocities and offsets of simulated galaxies are more similar to radio BGGs than to non-radio BGGs, albeit statistical tests still highlight significant differences between simulated and real objects. We find that radio BGGs are more likely to be hosted in high-mass groups. Finally, we observe correlations between the powers of BGG radio galaxies and the X-ray temperatures, Tx, and X-ray luminosities, Lx, of the host groups. This supports the existence of a link between the intragroup medium and the central radio source. The occurrence of powerful radio galaxies at group centres can be explained by Chaotic Cold Accretion, as the AGN can feed from both the galactic and intragroup condensation, leading to the observed positive LR − Tx correlation.

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Section: Comparison With Cosmological Simulationsmentioning

confidence: 98%

Radio galaxies in galaxy groups: kinematics, scaling relations, and AGN feedback

Pasini

Finoguenov

Brüggen

et al. 2021

Monthly Notices of the Royal Astronomical Society

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“…Redshift measurements of the individual galaxies in the cluster field clearly separate the cluster members and interlopers. Previous studies compile spectroscopic redshift measurements of galaxies in clusters identified by other methods (e.g., X-ray, optical, and IR imaging) to refine these cluster catalogs (e.g., Rozo et al 2015;Clerc et al 2016;Sohn et al 2018a,b;Rines et al 2018;Myles et al 2020;Kirkpatrick et al 2021). Other studies identify galaxy overdensities or, equivalently, clusters in redshift space (e.g., Huchra & Geller 1982;Eke et al 2004;Berlind et al 2006;Robotham et al 2011;Tago et al 2010;Tempel et al 2014).…”

Section: Introductionmentioning

confidence: 99%

The HectoMAP Cluster Survey: Spectroscopically Identified Clusters and their Brightest Cluster Galaxies (BCGs)

Sohn,

Geller,

Hwang

et al. 2021

Preprint

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We apply a friends-of-friends (FoF) algorithm to identify galaxy clusters and we use the catalog to explore the evolutionary synergy between BCGs and their host clusters. We base the cluster catalog on the dense HectoMAP redshift survey (2000 redshifts deg −2 ). The HectoMAP FoF catalog includes 346 clusters with 10 or more spectroscopic members. We list these clusters and their members (5992 galaxies with a spectroscopic redshift). We also include central velocity dispersions (σ * ,BCG ) for all of the FoF cluster BCGs, a distinctive feature of the HectoMAP FoF catalog. HectoMAP clusters with higher galaxy number density (80 systems) are all genuine clusters with a strong concentration and a prominent BCG in Subaru/Hyper Suprime-Cam images. The phase-space diagrams show the expected elongation along the line-of-sight. Lower-density systems include some false positives. We establish a connection between BCGs and their host clusters by demonstrating that σ * ,BCG /σ cl decreases as a function of cluster velocity dispersion (σ cl ), in contrast, numerical simulations predict a constant σ * ,BCG /σ cl . Sets of clusters at two different redshifts show that BCG evolution in massive systems is slow over the redshift range z < 0.4. The data strongly suggest that minor mergers may play an important role in BCG evolution in these clusters (σ cl 300 km s −1 ). For systems of lower mass (σ cl < 300 km s −1 ), the data indicate that major mergers may play a significant role. The coordinated evolution of BCGs and their host clusters provides an interesting test of simulations in high density regions of the universe.

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“…The trends in velocity bias discussed in this work are all empirically testable with ongoing spectroscopic campaigns of clusters such as SPIDERS (Kirkpatrick et al 2021) and DESI. The dependence of 𝜎 sat, 1D on 𝑀 ★, sat (or more precisely, the galaxy luminosity) has already been observationally studied for many different modestly-sized samples of clusters (𝑁 ∼ 100) as was noted before, while such observational studies of the redshift and halo mass trends have not yet been well-explored.…”

Section: Discussionmentioning

confidence: 61%

“…For example, Bocquet et al (2015, see Section 3 and Section 5.1) discuss that a 1% prior on the velocity bias improves constraints on both astrophysical and cosmological parameters connected to galaxy clusters by ≈ 30%. Cluster counts as a function of their galaxy velocity dispersion and redshift has also emerged as an alternative approach for cluster cosmology (Caldwell et al 2016;Ntampaka et al 2017Ntampaka et al , 2019Kirkpatrick et al 2021), and the velocity bias is a critical component in forward modelling the relevant observable from cosmological parameters. 4), and the fractional uncertainty on each estimate (right panel).…”

Section: Revised Mass Scale Of Low-𝑍 Sdss Clustersmentioning

confidence: 99%

Galaxy Velocity Bias in Cosmological Simulations: Towards Percent-level Calibration

Anbajagane,

Aung,

Evrard

et al. 2021

Preprint

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Galaxy cluster masses, rich with cosmological information, can be estimated from internal dark matter (DM) velocity dispersions, which in turn can be observationally inferred from satellite galaxy velocities. However, galaxies are biased tracers of the DM, and the bias can vary over host halo and galaxy properties as well as time. We precisely calibrate the velocity bias, 𝑏 𝑣 -defined as the ratio of galaxy and DM velocity dispersions -as a function of redshift, host halo mass, and galaxy stellar mass threshold (𝑀 ★, sat ), for massive halos (𝑀 200c > 10 13.5 M ) from five cosmological simulations: IllustrisTNG, Magneticum, Bahamas + Macsis, The Three Hundred Project, and MultiDark Planck-2. We first compare scaling relations for galaxy and DM velocity dispersion across simulations; the former is estimated using a new ensemble velocity likelihood method that is unbiased for low galaxy counts per halo, while the latter uses a local linear regression. The simulations show consistent trends of 𝑏 𝑣 increasing with 𝑀 200c and decreasing with redshift and 𝑀 ★, sat . The ensemble-estimated theoretical uncertainty in 𝑏 𝑣 is 2-3%, but becomes percent-level when considering only the three highest resolution simulations. We update the mass-richness normalization previously estimated by Farahi et al. (2016) for an SDSS redMaPPer cluster sample. The improved accuracy of our 𝑏 𝑣 estimates reduces the mass normalization uncertainty from 22% to 8%, demonstrating that dynamical estimation techniques can be competitive with weak lensing in calibrating population mean masses. We discuss necessary steps for further improving this precision. Our estimates for 𝑏 𝑣 (𝑀 200c , 𝑀 ★, sat , 𝑧) are made publicly available.

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SPIDERS: an overview of the largest catalogue of spectroscopically confirmed x-ray galaxy clusters

Cited by 25 publications

References 69 publications

Radio galaxies in galaxy groups: kinematics, scaling relations, and AGN feedback

Radio galaxies in galaxy groups: kinematics, scaling relations, and AGN feedback

The HectoMAP Cluster Survey: Spectroscopically Identified Clusters and their Brightest Cluster Galaxies (BCGs)

Galaxy Velocity Bias in Cosmological Simulations: Towards Percent-level Calibration

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