The Double Galaxy Cluster A2465. III. X-Ray and Weak-lensing Observations

ABSTRACT If properly calibrated, the shapes of galaxy clusters can be used to investigate many physical processes: from feedback and quenching of star formation, to the nature of dark matter. Theorists frequently measure shapes using moments of inertia of simulated particles’. We instead create mock (optical, X-ray, strong-, and weak-lensing) observations of the 22 most massive ($\sim 10^{14.7}\, \mathrm{ M}_\odot$) relaxed clusters in the BAHAMAS simulations. We find that observable measures of shape are rounder. Even when moments of inertia are projected into 2D and evaluated at matched radius, they overestimate ellipticity by 56 per cent (compared to observable strong lensing) and 430 per cent (compared to observable weak lensing). Therefore, we propose matchable quantities and test them using observations of eight relaxed clusters from the Hubble Space Telescope (HST) and Chandra X-Ray Observatory. We also release our HST data reduction and lensing analysis software to the community. In real clusters, the ellipticity and orientation angle at all radii are strongly correlated. In simulated clusters, the ellipticity of inner (<rvir/20) regions becomes decoupled: for example, with greater misalignment of the central cluster galaxy. This may indicate overly efficient implementation of feedback from active galactic nuclei. Future exploitation of cluster shapes as a function of radii will require better understanding of core baryonic processes. Exploitation of shapes on any scale will require calibration on simulations extended all the way to mock observations.

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Weak lensing calibration of mass bias in the REFLEX+BCS X-ray galaxy cluster catalogue

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/stw3322 ◽

2016 ◽

Vol 466 (3) ◽

pp. 3663-3673 ◽

Cited By ~ 12

Author(s):

Melanie Simet ◽

Nicholas Battaglia ◽

Rachel Mandelbaum ◽

Uroš Seljak

Keyword(s):

Galaxy Cluster ◽

Weak Lensing ◽

X Ray ◽

Mass Bias

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Impact of Weak Lensing Mass Calibration on eROSITA Galaxy Cluster Cosmological Studies – a Forecast

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/stz1778 ◽

2019 ◽

Cited By ~ 4

Author(s):

S Grandis ◽

J J Mohr ◽

J P Dietrich ◽

S Bocquet ◽

A Saro ◽

...

Keyword(s):

Count Rate ◽

Galaxy Cluster ◽

Effective Area ◽

Mass Scale ◽

Weak Lensing ◽

Parameter Uncertainties ◽

X Ray ◽

Mass Scaling ◽

Mass Calibration ◽

The Impact

Abstract We forecast the impact of weak lensing (WL) cluster mass calibration on the cosmological constraints from the X-ray selected galaxy cluster counts in the upcoming eROSITA survey. We employ a prototype cosmology pipeline to analyze mock cluster catalogs. Each cluster is sampled from the mass function in a fiducial cosmology and given an eROSITA count rate and redshift, where count rates are modeled using the eROSITA effective area, a typical exposure time, Poisson noise and the scatter and form of the observed X-ray luminosity– and temperature–mass–redshift relations. A subset of clusters have mock shear profiles to mimic either those from DES and HSC or from the future Euclid and LSST surveys. Using a count rate selection, we generate a baseline cluster cosmology catalog that contains 13k clusters over 14,892 deg2 of extragalactic sky. Low mass groups are excluded using raised count rate thresholds at low redshift. Forecast parameter uncertainties for ΩM, σ8 and w are 0.023 (0.016; 0.014), 0.017 (0.012; 0.010), and 0.085 (0.074; 0.071), respectively, when adopting DES+HSC WL (Euclid; LSST), while marginalizing over the sum of the neutrino masses. A degeneracy between the distance–redshift relation and the parameters of the observable–mass scaling relation limits the impact of the WL calibration on the w constraints, but with BAO measurements from DESI an improved determination of w to 0.043 becomes possible. With Planck CMB priors, ΩM (σ8) can be determined to 0.005 (0.007), and the summed neutrino mass limited to ∑mν < 0.241 eV (at 95%). If systematics on the group mass scale can be controlled, the eROSITA group and cluster sample with 43k objects and LSST WL could constrain ΩM and σ8 to 0.007 and w to 0.050.

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The massive galaxy cluster XMMU J1230.3+1339 at z ∼ 1: colour-magnitude relation, Butcher-Oemler effect, X-ray and weak lensing mass estimates★

Monthly Notices of the Royal Astronomical Society ◽

10.1111/j.1365-2966.2010.17874.x ◽

2011 ◽

Vol 411 (4) ◽

pp. 2667-2694 ◽

Cited By ~ 26

Author(s):

M. Lerchster ◽

S. Seitz ◽

F. Brimioulle ◽

R. Fassbender ◽

M. Rovilos ◽

...

Keyword(s):

Galaxy Cluster ◽

Weak Lensing ◽

X Ray ◽

Massive Galaxy

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Investigating the Relationship Between the Hot Gas and the Dark Matter Components of Galaxy Clusters.

Proceedings of the International Astronomical Union ◽

10.1017/s1743921307014342 ◽

2007 ◽

Vol 3 (S244) ◽

pp. 374-375

Author(s):

Leila C. Powell ◽

Scott T. Kay ◽

Arif Babul ◽

Andisheh Mahdavi

Keyword(s):

Dark Matter ◽

Total Mass ◽

Surface Brightness ◽

Galaxy Cluster ◽

Weak Lensing ◽

X Ray ◽

Hot Gas ◽

Cluster Properties ◽

The Impact ◽

The Relationship

AbstractVarious differences in galaxy cluster properties derived from X-ray and weak lensing observations have been highlighted in the literature. One such difference is the observation of mass concentrations in lensing maps which have no X-ray counterparts (e.g. Jee, White, Ford et al. 2005). We investigate this issue by identifying substructures in maps of projected total mass (analogous to weak lensing mass reconstructions) and maps of projected X-ray surface brightness for three simulated clusters. We then compare the 2D mass substructures with both 3D subhalo data and the 2D X-ray substructures. Here we present preliminary results from the first comparison, where we have assessed the impact of projecting the data on subhalo identification.

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XMM-Newton X-ray and HST weak gravitational lensing study of the extremely X-ray luminous galaxy cluster Cl J120958.9+495352 (z = 0.902)

Astronomy and Astrophysics ◽

10.1051/0004-6361/201730913 ◽

2018 ◽

Vol 610 ◽

pp. A71 ◽

Cited By ~ 1

Author(s):

Sophia Thölken ◽

Tim Schrabback ◽

Thomas H. Reiprich ◽

Lorenzo Lovisari ◽

Steven W. Allen ◽

...

Keyword(s):

Temperature Profile ◽

Gravitational Lensing ◽

Mass Fraction ◽

High Redshift ◽

Galaxy Cluster ◽

Cooling Time ◽

Weak Lensing ◽

Imaging Data ◽

Weak Gravitational Lensing ◽

X Ray

Context. Observations of relaxed, massive, and distant clusters can provide important tests of standard cosmological models, for example by using the gas mass fraction. To perform this test, the dynamical state of the cluster and its gas properties have to be investigated. X-ray analyses provide one of the best opportunities to access this information and to determine important properties such as temperature profiles, gas mass, and the total X-ray hydrostatic mass. For the last of these, weak gravitational lensing analyses are complementary independent probes that are essential in order to test whether X-ray masses could be biased. Aims. We study the very luminous, high redshift (z = 0.902) galaxy cluster Cl J120958.9+495352 using XMM-Newton data. We measure global cluster properties and study the temperature profile and the cooling time to investigate the dynamical status with respect to the presence of a cool core. We use Hubble Space Telescope (HST) weak lensing data to estimate its total mass and determine the gas mass fraction. Methods. We perform a spectral analysis using an XMM-Newton observation of 15 ks cleaned exposure time. As the treatment of the background is crucial, we use two different approaches to account for the background emission to verify our results. We account for point spread function effects and deproject our results to estimate the gas mass fraction of the cluster. We measure weak lensing galaxy shapes from mosaic HST imaging and select background galaxies photometrically in combination with imaging data from the William Herschel Telescope. Results. The X-ray luminosity of Cl J120958.9+495352 in the 0.1–2.4 keV band estimated from our XMM-Newton data is LX = (13.4−1.0+1.2) × 1044 erg/s and thus it is one of the most X-ray luminous clusters known at similarly high redshift. We find clear indications for the presence of a cool core from the temperature profile and the central cooling time, which is very rare at such high redshifts. Based on the weak lensing analysis, we estimate a cluster mass of M500 / 1014 M⊙ = 4.4−2.0+2.2(star.) ± 0.6(sys.) and a gas mass fraction of fgas,2500 = 0.11−0.03+0.06 in good agreement with previous findings for high redshift and local clusters.

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Deprojection of Galaxy Cluster X‐Ray, Sunyaev‐Zeldovich Temperature Decrement, and Weak‐Lensing Mass Maps

The Astrophysical Journal ◽

10.1086/323359 ◽

2001 ◽

Vol 561 (2) ◽

pp. 600-620 ◽

Cited By ~ 30

Author(s):

S. Zaroubi ◽

G. Squires ◽

G. de Gasperis ◽

A. E. Evrard ◽

Y. Hoffman ◽

...

Keyword(s):

Galaxy Cluster ◽

Weak Lensing ◽

X Ray

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Dark Energy Surveyed Year 1 results: calibration of cluster mis-centring in the redMaPPer catalogues

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/stz1361 ◽

2019 ◽

Vol 487 (2) ◽

pp. 2578-2593 ◽

Cited By ~ 13

Author(s):

Y Zhang ◽

T Jeltema ◽

D L Hollowood ◽

S Everett ◽

E Rozo ◽

...

Keyword(s):

Dark Energy ◽

Gamma Distribution ◽

Galaxy Cluster ◽

Weak Lensing ◽

Descriptive Model ◽

X Ray ◽

Projected Distance

Abstract The centre determination of a galaxy cluster from an optical cluster finding algorithm can be offset from theoretical prescriptions or N-body definitions of its host halo centre. These offsets impact the recovered cluster statistics, affecting both richness measurements and the weak lensing shear profile around the clusters. This paper models the centring performance of the redMaPPer cluster finding algorithm using archival X-ray observations of redMaPPer-selected clusters. Assuming the X-ray emission peaks as the fiducial halo centres, and through analysing their offsets to the redMaPPer centres, we find that ${\sim } 75\pm 8 {{\ \rm per\ cent}}$ of the redMaPPer clusters are well centred and the mis-centred offset follows a Gamma distribution in normalized, projected distance. These mis-centring offsets cause a systematic underestimation of cluster richness relative to the well-centred clusters, for which we propose a descriptive model. Our results enable the DES Y1 cluster cosmology analysis by characterizing the necessary corrections to both the weak lensing and richness abundance functions of the DES Y1 redMaPPer cluster catalogue.

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An X-Ray–Selected Galaxy Cluster at [CLC][ITAL]z[/ITAL][/CLC] = 1.26

The Astronomical Journal ◽

10.1086/300934 ◽

1999 ◽

Vol 118 (1) ◽

pp. 76-85 ◽

Cited By ~ 126

Author(s):

Piero Rosati ◽

S. A. Stanford ◽

Peter R. Eisenhardt ◽

Richard Elston ◽

Hyron Spinrad ◽

...

Keyword(s):

Galaxy Cluster ◽

X Ray

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The role of AGN activity in the building up of the BCG at z ∼ 1.6

Proceedings of the International Astronomical Union ◽

10.1017/s1743921320003105 ◽

2019 ◽

Vol 15 (S356) ◽

pp. 280-284

Author(s):

Angela Bongiorno ◽

Andrea Travascio

Keyword(s):

Galaxy Cluster ◽

Cluster Galaxy ◽

X Ray ◽

Groups Of Galaxies ◽

Star Forming ◽

The Core ◽

The Galaxy ◽

Multi Wavelength

AbstractXDCPJ0044.0-2033 is one of the most massive galaxy cluster at z ∼1.6, for which a wealth of multi-wavelength photometric and spectroscopic data have been collected during the last years. I have reported on the properties of the galaxy members in the very central region (∼ 70kpc × 70kpc) of the cluster, derived through deep HST photometry, SINFONI and KMOS IFU spectroscopy, together with Chandra X-ray, ALMA and JVLA radio data.In the core of the cluster, we have identified two groups of galaxies (Complex A and Complex B), seven of them confirmed to be cluster members, with signatures of ongoing merging. These galaxies show perturbed morphologies and, three of them show signs of AGN activity. In particular, two of them, located at the center of each complex, have been found to host luminous, obscured and highly accreting AGN (λ = 0.4−0.6) exhibiting broad Hα line. Moreover, a third optically obscured type-2 AGN, has been discovered through BPT diagram in Complex A. The AGN at the center of Complex B is detected in X-ray while the other two, and their companions, are spatially related to radio emission. The three AGN provide one of the closest AGN triple at z > 1 revealed so far with a minimum (maximum) projected distance of 10 kpc (40 kpc). The discovery of multiple AGN activity in a highly star-forming region associated to the crowded core of a galaxy cluster at z ∼ 1.6, suggests that these processes have a key role in shaping the nascent Brightest Cluster Galaxy, observed at the center of local clusters. According to our data, all galaxies in the core of XDCPJ0044.0-2033 could form a BCG of M* ∼ 1012Mȯ hosting a BH of 2 × 108−109Mȯ, in a time scale of the order of 2.5 Gyrs.

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