Projection effects in galaxy cluster samples: insights from X-ray redshifts

Ramos-Ceja, M. E.; Pacaud, F.; Reiprich, T. H.; Migkas, K.; Lovisari, Lorenzo; Schellenberger, G.

doi:10.1051/0004-6361/201935111

Cited by 18 publications

(13 citation statements)

References 61 publications

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“…Utilizing the FWC data, the Quiescent Particle Background (QPB) ) is modelled and then subtracted from the observation. We follow the procedure described in Ramos-Ceja et al (2019). First, the cleaned observation data is matched with the suitable FWC data and then this FWC template is re-projected to the sky position.…”

Section: Xmm-newtonmentioning

confidence: 99%

“…Therefore, it is required to detect and excise the point sources, for example in the calculation of surface brightness profiles and spectral analysis. To detect the point sources in the observation, we implement the procedure described in Pacaud et al (2006) and Ramos-Ceja et al (2019). Firstly, wavelet filtering is applied on the combined detector image in the soft energy band (0.5 − 2.0 keV).…”

Section: Xmm-newtonmentioning

confidence: 99%

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The eROSITA view of the Abell 3391/95 field: The Northern Clump

Veronica

Biffi

et al. 2022

A&A

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Context. Galaxy clusters grow through mergers and accretion of substructures along large-scale filaments. Many of the missing baryons in the local Universe may reside in such filaments as the Warm-Hot Intergalactic Medium (WHIM). Aims. SRG/eROSITA Performance Verification (PV) observations revealed the binary cluster Abell 3391/3395 and the Northern Clump (the MCXC J0621.7-5242 galaxy cluster) are aligning along a cosmic filament in soft X-rays, similarly to what has been seen in simulations before. We aim to understand the dynamical state of the Northern Clump as it enters the atmosphere (3 × R 200 ) of Abell 3391. Methods. We analyzed joint eROSITA, XMM-Newton, and Chandra observations to probe the morphological, thermal, and chemical properties of the Northern Clump from its center out to a radius of 1077 kpc (1.1 × R 200 ). We utilized the ASKAP/EMU radio data, DECam optical image, and Planck y-map to study the influence of the Wide Angle Tail (WAT) radio source on the Northern Clump central Intra-Cluster Medium (ICM). From the Magneticum simulation, we identified an analog of the A3391/95 system along with an infalling group resembling the Northern Clump. Results. The Northern Clump is a Weak Cool-Core cluster centered on a WAT radio galaxy. The gas temperature over 0.2 − 0.5R 500 is k B T 500 = 1.99 ± 0.04 keV. We employed the mass-temperature (M − T ) scaling relation and obtained a mass estimate of M 500 = (7.68 ± 0.43) × 10 13 M and R 500 = (636 ± 12) kpc. Its X-ray atmosphere has a boxy shape and deviates from spherical symmetry. We identify a southern surface brightness edge, likely caused by subsonic motion relative to the filament gas in the southern direction. At ∼ R 500 , the southern atmosphere (infalling head) appears to be 42% hotter than its northern atmosphere. We detect a downstream tail pointing towards north with a projected length of ∼ 318 kpc, plausibly the result of ram pressure stripping. The analog group in the Magneticum simulation is experiencing changes in its gas properties and a shift between the position of the halo center and that of the bound gas, while approaching the main cluster pair. Conclusions. The Northern Clump is a dynamically active system and far from being relaxed. Its atmosphere is affected by interaction with the WAT and by gas sloshing or its infall towards Abell 3391 along the filament, consistent with the analog group-size halo in the Magneticum simulation.

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Section: Xmm-newtonmentioning

confidence: 99%

Section: Xmm-newtonmentioning

confidence: 99%

The eROSITA view of the Abell 3391/95 field: The Northern Clump

Veronica

Biffi

et al. 2022

A&A

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“…to compare the profiles from eROSITA with XMM-Newton, the eventfiles were obtained from the archive to perform analysis on. The analysis carried out in this work closely follows that described in Ramos-Ceja et al (2019). To summarise, flare filtering was carried out in order to identify and remove any soft proton flares that were present in the observation, CCDs that were in an anomalous state during the observation were removed, and the instrumental background and exposure were corrected for.…”

Section: Xmm-newtonmentioning

confidence: 99%

X-Ray Studies of the Abell 3158 Galaxy Cluster with eROSITA

Whelan,

Veronica,

Pacaud

et al. 2021

Preprint

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Context. The most nearby clusters are the best places to study physical and enrichment effects in the faint cluster outskirts. The Abell 3158 cluster (A3158), located at z = 0.059 is quite extended with a characteristic radius r 200 = 23.95 arcmin. The metal distribution in the outskirts of this cluster has previously been studied with XMM-Newton. In 2019, A3158 was observed as a calibration target in a pointed observation with the eROSITA telescope onboard the Spektrum-Roentgen-Gamma (SRG) mission. Bright large clusters, like A3158, are ideal for studying the metal distribution in the cluster outskirts, along with the temperature profile and morphology. With the deeper observation time of the eROSITA telescope, these properties can be studied in greater detail and at larger radii now. Furthermore, bright nearby clusters are ideal X-ray instrumental cross-calibration targets as they cover a large fraction of the detector and do not vary in time.Aims. We first aim to compare the temperature, metal abundance and normalisation profiles of the cluster from eROSITA with previous XMM-Newton and Chandra data. Following this calibration work, we aim to investigate the temperature and metallicity of the cluster out to close to r 200 , measure the galaxy velocity dispersion, and determine the cluster mass. Furthermore, we aim to search for infalling clumps and background clusters in the field. Methods. We determined 1d temperature, abundance and normalisation profiles from both eROSITA and XMM-Newton data as well as 2d maps of temperature and metal abundance distribution from eROSITA data. The velocity dispersion was determined and the cluster mass was calculated from the mass -velocity dispersion (M 200 -σ v ) relation. Galaxy density maps were created to get a better understanding of the structure of the cluster and the outskirts. Results. The overall (i.e., in the range 0.2 − 0.5r 500 ) temperature was measured to be 4.725 ± 0.035 keV. The temperature, abundance and normalisation profiles of eROSITA all agree on a 10% level with those we determined using XMM-Newton and Chandra data; and they are also consistent with the profiles published previously by the X-COP project. The Abell 3158 cluster morphology and surface brightness profile look regular at a first glance. Clusters that have such profiles typically are relaxed and host cool cores. However, from the temperature profile and map we see that the cluster lacks a cool core, as was noted before. Instead, the presence of an off-centre cool clump to the west of the central cluster region, which has been previously detected, is observed. These are indications that the cluster may be undergoing some sloshing and merger activity. Furthermore there is a bow shaped edge near the location of the cool gas clump West of the cluster centre. Further out in the West of the X-ray images of A3158 an extension of gas is detected; the larger scale extension described here for the first time. The velocity dispersion of the cluster member galaxies was measured to be 1058 ± 41km s −1 ba...

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“…Second, cluster catalogues are hardly affected by projection effects (e.g. Ramos-Ceja et al 2019), namely the inclusion of spurious sources resulting from the projection of unrelated systems along the line of sight, because the centrally concentrated X-ray emission clearly indicates the presence of gas trapped in the potential well of a cluster (e.g. Frenk et al 1990;Reblinsky & Bartelmann 1999).…”

Section: Introductionmentioning

confidence: 99%

The X-CLASS survey: A catalogue of 1646 X-ray-selected galaxy clusters up to z ∼ 1.5

Koulouridis

Clerc

Sadibekova

et al. 2021

A&A

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Context. Cosmological probes based on galaxy clusters rely on cluster number counts and large-scale structure information. X-ray cluster surveys are well suited for this purpose because they are far less affected by projection effects than optical surveys, and cluster properties can be predicted with good accuracy. Aims. The XMM Cluster Archive Super Survey, X-CLASS, is a serendipitous search of X-ray-detected galaxy clusters in 4176 XMM-Newton archival observations until August 2015. All observations are clipped to exposure times of 10 and 20 ks to obtain uniformity, and they span ∼269 deg 2 across the high-Galactic latitude sky (|b| > 20 o ). The main goal of the survey is the compilation of a wellselected cluster sample suitable for cosmological analyses. Methods. We describe the detection algorithm, the visual inspection, the verification process, and the redshift validation of the cluster sample, as well as the cluster selection function computed by simulations. We also present the various metadata that are released with the catalogue, along with two different count-rate measurements, an automatic one provided by the pipeline, and a more detailed and accurate interactive measurement. Furthermore, we provide the redshifts of 124 clusters obtained with a dedicated multi-object spectroscopic follow-up programme. Results. With this publication, we release the new X-CLASS catalogue of 1646 well-selected X-ray-detected clusters over a wide sky area, along with their selection function. The sample spans a wide redshift range, from the local Universe up to z ∼ 1.5, with 982 spectroscopically confirmed clusters, and over 70 clusters above z = 0.8. The redshift distribution peaks at z∼ 0.1, while if we remove the pointed observations it peaks at z ∼ 0.3. Because of its homogeneous selection and thorough verification, the cluster sample can be used for cosmological analyses, but also as a test-bed for the upcoming eROSITA observations and other current and future large-area cluster surveys. It is the first time that such a catalogue is made available to the community via an interactive database which gives access to a wealth of supplementary information, images, and data.

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Projection effects in galaxy cluster samples: insights from X-ray redshifts

Cited by 18 publications

References 61 publications

The eROSITA view of the Abell 3391/95 field: The Northern Clump

The eROSITA view of the Abell 3391/95 field: The Northern Clump

X-Ray Studies of the Abell 3158 Galaxy Cluster with eROSITA

The X-CLASS survey: A catalogue of 1646 X-ray-selected galaxy clusters up to z ∼ 1.5

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