Showing papers by "David Bacon published in 2019"
ASTRON1, Leiden University2, University of Paris3, Rhodes University4, University of Hertfordshire5, University of Edinburgh6, University of Hamburg7, INAF8, Open University9, Rutherford Appleton Laboratory10, Paris Diderot University11, Jagiellonian University12, Chalmers University of Technology13, Radboud University Nijmegen14, Commonwealth Scientific and Industrial Research Organisation15, University of Manchester16, University of the Western Cape17, University of Oxford18, Kapteyn Astronomical Institute19, University of Amsterdam20, Institute of Cosmology and Gravitation, University of Portsmouth21, Joint Institute for VLBI in Europe22, University of Bologna23, University of Nottingham24, Ruhr University Bochum25, Mbarara University of Science and Technology26, Max Planck Society27, Centre national de la recherche scientifique28, Spanish National Research Council29, University of La Laguna30, University College Dublin31, Bielefeld University32
TL;DR: The LOFAR Two-metre Sky Survey (LoTSS) is an ongoing sensitive, high-resolution 120-168 MHz survey of the entire northern sky for which observations are now 20% complete as discussed by the authors.
Abstract: The LOFAR Two-metre Sky Survey (LoTSS) is an ongoing sensitive, high-resolution 120–168 MHz survey of the entire northern sky for which observations are now 20% complete. We present our first full-quality public data release. For this data release 424 square degrees, or 2% of the eventual coverage, in the region of the HETDEX Spring Field (right ascension 10h45m00s to 15h30m00s and declination 45°00′00″ to 57°00′00″) were mapped using a fully automated direction-dependent calibration and imaging pipeline that we developed. A total of 325 694 sources are detected with a signal of at least five times the noise, and the source density is a factor of ∼10 higher than the most sensitive existing very wide-area radio-continuum surveys. The median sensitivity is S 144 MHz = 71 μ Jy beam−1 and the point-source completeness is 90% at an integrated flux density of 0.45 mJy. The resolution of the images is 6″ and the positional accuracy is within 0.2″. This data release consists of a catalogue containing location, flux, and shape estimates together with 58 mosaic images that cover the catalogued area. In this paper we provide an overview of the data release with a focus on the processing of the LOFAR data and the characteristics of the resulting images. In two accompanying papers we provide the radio source associations and deblending and, where possible, the optical identifications of the radio sources together with the photometric redshifts and properties of the host galaxies. These data release papers are published together with a further ∼20 articles that highlight the scientific potential of LoTSS.
277 citations
University of Portsmouth1, University of Pennsylvania2, University of Queensland3, Australian National University4, African Institute for Mathematical Sciences5, University of Chicago6, Lawrence Berkeley National Laboratory7, University of Southampton8, Fermilab9, Korea Astronomy and Space Science Institute10, University College London11, Texas A&M University12, Stanford University13, University of Illinois at Urbana–Champaign14, Spanish National Research Council15, California Institute of Technology16, University of Arizona17, University of Michigan18, University of California, Berkeley19, University of California, Santa Cruz20, University of Pittsburgh21, Autonomous University of Madrid22, Swinburne University of Technology23, University of Lisbon24, ETH Zurich25, Ohio State University26, Max Planck Society27, Ludwig Maximilian University of Munich28, Harvard University29, University of Namibia30, Macquarie University31, University of Sydney32, University of São Paulo33, National Institutes of Natural Sciences, Japan34, Academia Sinica35, University of Sussex36, Brandeis University37, State University of Campinas38, Oak Ridge National Laboratory39, Carnegie Institution for Science40, Argonne National Laboratory41
TL;DR: In this paper, the authors presented an improved measurement of the Hubble constant using the inverse distance ladder method, which added the information from 207 Type Ia supernovae (SNe Ia) from the DES at redshift 0.018
Abstract: We present an improved measurement of the Hubble constant (H0) using the 'inverse distance ladder' method, which adds the information from 207 Type Ia supernovae (SNe Ia) from the Dark Energy Survey (DES) at redshift 0.018
199 citations
TL;DR: Combined results from these probes derive constraints on the equation of state, w, of dark energy and its energy density in the Universe, demonstrating the potential power of large multiprobe photometric surveys and paving the way for order of magnitude advances in constraints on properties ofdark energy and cosmology over the next decade.
Abstract: The combination of multiple observational probes has long been advocated as a powerful technique to constrain cosmological parameters, in particular dark energy. The Dark Energy Survey has measured 207 spectroscopically confirmed type Ia supernova light curves, the baryon acoustic oscillation feature, weak gravitational lensing, and galaxy clustering. Here we present combined results from these probes, deriving constraints on the equation of state, w, of dark energy and its energy density in the Universe. Independently of other experiments, such as those that measure the cosmic microwave background, the probes from this single photometric survey rule out a Universe with no dark energy, finding w=-0.80_{-0.11}^{+0.09}. The geometry is shown to be consistent with a spatially flat Universe, and we obtain a constraint on the baryon density of Ω_{b}=0.069_{-0.012}^{+0.009} that is independent of early Universe measurements. These results demonstrate the potential power of large multiprobe photometric surveys and pave the way for order of magnitude advances in our constraints on properties of dark energy and cosmology over the next decade.
107 citations
TL;DR: In this article, the authors investigated the impact of 21cm foreground clean on the cross-correlations with spectroscopic optical surveys with well-constrained redshifts and found that a redshift uncertainty σ_z ≥ 0.04 causes significant degradation in the cross power spectrum signal.
Abstract: The future of precision cosmology could benefit from cross-correlations between intensity maps of unresolved neutral hydrogen (H i) and more conventional optical galaxy surveys. A major challenge that needs to be overcome is removing the 21cm foreground emission that contaminates the cosmological H i signal. Using N-body simulations, we simulate H i intensity maps and optical catalogues that share the same underlying cosmology. Adding simulated foreground contamination and using state-of-the-art reconstruction techniques, we investigate the impacts that 21cm foregrounds and other systematics have on these cross-correlations. We find that the impact a Fast Independent Component Analysis 21cm foreground clean has on the cross-correlations with spectroscopic optical surveys with well-constrained redshifts is minimal. However, problems arise when photometric surveys are considered: We find that a redshift uncertainty σ_z ≥ 0.04 causes significant degradation in the cross-power spectrum signal. We diagnose the main root of these problems, which relates to arbitrary amplitude changes along the line of sight in the intensity maps caused by the foreground clean and suggest solutions that should be applicable to real data. These solutions involve a reconstruction of the line-of-sight temperature means using the available overlapping optical data along with an artificial extension to the H i data through redshift to address edge effects. We then put these solutions through a further test in a mock experiment that uses a clustering-based redshift estimation technique to constrain the photometric redshifts of the optical sample. We find that with our suggested reconstruction, cross-correlations can be utilized to make an accurate prediction of the optical redshift distribution.
33 citations
Carnegie Mellon University1, University of Cambridge2, Fermilab3, University of Chicago4, University of Wisconsin-Madison5, Texas A&M University6, Institute of Cosmology and Gravitation, University of Portsmouth7, Institut d'Astrophysique de Paris8, University College London9, Stanford University10, SLAC National Accelerator Laboratory11, University of Illinois at Urbana–Champaign12, National Center for Supercomputing Applications13, IFAE14, Indian Institute of Technology, Hyderabad15, Spanish National Research Council16, Autonomous University of Madrid17, University of Michigan18, Santa Cruz Institute for Particle Physics19, Ohio State University20, Max Planck Society21, Ludwig Maximilian University of Munich22, Harvard University23, Macquarie University24, Catalan Institution for Research and Advanced Studies25, Princeton University26, Universidade Federal do Rio Grande do Sul27, University of Southampton28, State University of Campinas29, Oak Ridge National Laboratory30
TL;DR: Fornax 6 is a star cluster with a peculiarly low surface brightness and irregular shape, which may indicate a strong tidal influence from its host galaxy as discussed by the authors, but it is still likely more metal-rich than most of the globular clusters in the system.
Abstract: Since first noticed by Shapley in 1939, a faint object coincident with the Fornax dwarf spheroidal has long been discussed as a possible sixth globular cluster system. However, debate has continued over whether this overdensity is a statistical artifact or a blended galaxy group. In this Letter we demonstrate, using deep DECam imaging data, that this object is well resolved into stars and is a bona fide star cluster. The stellar overdensity of this cluster is statistically significant at the level of ~ 6 - 6.7 sigma in several different photometric catalogs including Gaia. Therefore, it is highly unlikely to be caused by random fluctuation. We show that Fornax 6 is a star cluster with a peculiarly low surface brightness and irregular shape, which may indicate a strong tidal influence from its host galaxy. The Hess diagram of Fornax 6 is largely consistent with that of Fornax field stars, but it appears to be slightly bluer. However, it is still likely more metal-rich than most of the globular clusters in the system. Faint clusters like Fornax 6 that orbit and potentially get disrupted in the centers of dwarf galaxies can prove crucial for constraining the dark matter distribution in Milky Way satellites.
22 citations
TL;DR: In this article, the authors developed a methodology to remove modes from a galaxy survey power spectrum that are associated with systematic errors, which can then be used to remove these systematic contaminants at least as well as applying corrective weighting to the observed galaxies, but benefits from giving an unbiased power.
Abstract: We develop a practical methodology to remove modes from a galaxy survey power spectrum that are associated with systematic errors. We apply this to the BOSS CMASS sample, to see if it removes the excess power previously observed beyond the best-fit $\Lambda$CDM model on very large scales. We consider several possible sources of data contamination, and check whether they affect the number of targets that can be observed and the power spectrum measurements. We describe a general framework for how such knowledge can be transformed into template fields. Mode subtraction can then be used to remove these systematic contaminants at least as well as applying corrective weighting to the observed galaxies, but benefits from giving an unbiased power. Even after applying templates for all known systematics, we find a large-scale power excess, but this is reduced compared with that observed using the weights provided by the BOSS team. This excess is at much larger scales than the BAO scale and does not affect the main results of BOSS. However, it will be important for the measurement of a scale-dependent bias due to primordial non-Gaussianity. The excess is beyond that allowed by any simple model of non-Gaussianity matching Planck data, and is not matched in other surveys. We show that this power excess can further be reduced but is still present using "phenomenological" templates, designed to consider further potentially unknown sources of systematic contamination. As all discrepant angular modes can be removed using "phenomenological" templates, the potentially remaining contaminant acts radially.
22 citations
TL;DR: In this article, the authors used the X-ray surface brightness measurements of the Coma cluster and from 58 stacked galaxy clusters along with the weak lensing data to test the theory of emergent gravity.
Abstract: Verlinde's theory of Emergent Gravity (EG) describes gravity as an emergent phenomenon rather than a fundamental force. Applying this reasoning in de Sitter space leads to gravity behaving differently on galaxy and galaxy cluster scales; this excess gravity might offer an alternative to dark matter. Here we test these ideas using the data from the Coma cluster and from 58 stacked galaxy clusters. The X-ray surface brightness measurements of the clusters at 0.1 < z < 1.2 along with the weak lensing data are used to test the theory. We find that the simultaneous EG fits of the X-ray and weak lensing datasets are significantly worse than those provided by General Relativity (with cold dark matter). For the Coma cluster, the predictions from emergent gravity and general relativity agree in the range of 250 – 700 kpc, while at around 1 Mpc scales, EG total mass predictions are larger by a factor of 2. For the cluster stack the predictions are only in good agreement at around the 1 – 2 Mpc scales, while for r 10 Mpc EG is in strong tension with the data. According to the Bayesian information criterion analysis, GR is preferred in all tested datasets; however, we also discuss possible modifications of EG that greatly relax the tension with the data.
20 citations
TL;DR: In this paper, the S3-SAX catalogue of unresolved HI (21cm) spectral line emission is used to construct a redshift distribution estimator, which is tested using simulations.
Abstract: Precision cosmology requires accurate galaxy redshifts, but next generation optical surveys will observe unprecedented numbers of resolved galaxies, placing strain on the amount of spectroscopic follow-up required. We show how useful information can be gained on the redshift distributions of optical galaxy samples from spatial cross-correlations with intensity maps of unresolved HI (21cm) spectral line emission. We construct a redshift distribution estimator, which we test using simulations. We utilise the S3-SAX catalogue which includes HI emission information for each galaxy, which we use to construct HI intensity maps. We also make use of simulated LSST and Euclid-like photometry enabling us to apply the HI clustering calibration to realistic simulated photometric redshifts. While taking into account important limitations to HI intensity mapping such as lost k-modes from foreground cleaning and poor angular resolution due to large receiver beams, we show that excellent constraints on redshift distributions can be provided for an optical photometric sample.
18 citations
TL;DR: In this article, a measurement of lensing ratios using galaxy position and lensing data from the Dark Energy Survey, and CMB lensing from the South Pole Telescope and Planck was presented, obtaining the highest precision lensing ratio measurements.
Abstract: Correlations between tracers of the matter density field and gravitational lensing are sensitive to the evolution of the matter power spectrum and the expansion rate across cosmic time. Appropriately defined ratios of such correlation functions, on the other hand, depend only on the angular diameter distances to the tracer objects and to the gravitational lensing source planes. Because of their simple cosmological dependence, such ratios can exploit available signal-to-noise ratio down to small angular scales, even where directly modelling the correlation functions is difficult. We present a measurement of lensing ratios using galaxy position and lensing data from the Dark Energy Survey, and CMB lensing data from the South Pole Telescope and Planck, obtaining the highest precision lensing ratio measurements to date. Relative to the concordance ΛCDM model, we find a best-fitting lensing ratio amplitude of A = 1.1 ± 0.1. We use the ratio measurements to generate cosmological constraints, focusing on the curvature parameter. We demonstrate that photometrically selected galaxies can be used to measure lensing ratios, and argue that future lensing ratio measurements with data from a combination of LSST and Stage-4 CMB experiments can be used to place interesting cosmological constraints, even after considering the systematic uncertainties associated with photometric redshift and galaxy shear estimation.
14 citations
University of California, Los Angeles1, University of Melbourne2, University of Pennsylvania3, University of Chicago4, Fermilab5, Argonne National Laboratory6, Canadian Institute for Advanced Research7, University of Illinois at Urbana–Champaign8, University of Arizona9, Max Planck Society10, Ludwig Maximilian University of Munich11, Cardiff University12, National Institute of Standards and Technology13, Autonomous University of Madrid14, University of California, Berkeley15, University of Portsmouth16, University College London17, Stanford University18, IFAE19, Spanish National Research Council20, University of KwaZulu-Natal21, California Institute of Technology22, Indian Institute of Technology, Hyderabad23, McGill University24, University of California, Santa Cruz25, University of Michigan26, Harvey Mudd College27, European Southern Observatory28, University of Cambridge29, Lawrence Berkeley National Laboratory30, University of Colorado Boulder31, Ohio State University32, University of California, Davis33, University of São Paulo34, Texas A&M University35, Princeton University36, University of Toronto37, University of Minnesota38, Ames Research Center39, University of Sussex40, Case Western Reserve University41, Yale University42, School of the Art Institute of Chicago43, University of Southampton44, Brandeis University45, Harvard University46, Oak Ridge National Laboratory47, University of Maryland, College Park48
TL;DR: This detection of gravitational lensing due to galaxy clusters using only the polarization of the cosmic microwave background (CMB) is reported, a key first step for cluster cosmology with future low-noise CMB surveys, like CMB-S4, for which CMB polarization will be the primary channel for cluster lensing measurements.
Abstract: We report the first detection of gravitational lensing due to galaxy clusters using only the polarization of the cosmic microwave background (CMB). The lensing signal is obtained using a new estimator that extracts the lensing dipole signature from stacked images formed by rotating the cluster-centered Stokes QU map cutouts along the direction of the locally measured background CMB polarization gradient. Using data from the SPTpol 500 deg^{2} survey at the locations of roughly 18 000 clusters with richness λ≥10 from the Dark Energy Survey (DES) Year-3 full galaxy cluster catalog, we detect lensing at 4.8σ. The mean stacked mass of the selected sample is found to be (1.43±0.40)×10^{14}M_{⊙} which is in good agreement with optical weak lensing based estimates using DES data and CMB-lensing based estimates using SPTpol temperature data. This measurement is a key first step for cluster cosmology with future low-noise CMB surveys, like CMB-S4, for which CMB polarization will be the primary channel for cluster lensing measurements.
14 citations
TL;DR: In this article, the angular two-point correlation of the LoFAR Two-metre Sky Survey (LoTSS) data has been studied and a suite of quality cuts have been defined.
Abstract: The LOFAR Two-metre Sky Survey (LoTSS) will map the complete Northern sky and provide an excellent opportunity to study the distribution and evolution of the large-scale structure of the Universe. We study the completeness of the LoTSS first data release (DR1) and find a point-source completeness of 99 % above flux densities of 0.8 mJy and define a suite of quality cuts. We determine the count-in-cell statistics and differential source counts statistic and measure the angular two-point correlation function of the LoTSS radio sources. The counts-in-cell statistic reveals that the distribution of radio sources cannot be described by a spatial Poisson process. Instead, a good fit is provided by a compound Poisson distribution. The differential source counts are in good agreement with previous findings in deep fields at low radio frequencies and with simulated catalogues from the SKA design study sky and the Tiered Radio Extragalactic Continuum Simulation. The angular two-point correlation is $ 1$ deg. Restricting the value added source catalogue to low-noise regions and a flux density threshold of 2 mJy provides our most reliable estimate of the angular two-point correlation. For smaller flux density thresholds systematic issues are identified, most likely related to the flux density calibration of the individual pointings. Based on the distribution of photometric redshifts of LoTSS sources and the Planck 2018 best-fit cosmological model, the theoretically predicted angular two-point correlation between 0.1 deg and 6 deg agrees with the measured clustering for a subsample of radio sources with redshift information. We find agreement with the expectation of large-scale statistical isotropy of the radio sky at the per cent level. The angular two-point correlation agrees well with the expectation of the cosmological standard model. (abbreviated)
TL;DR: In this paper, the authors show that the next generation of spectroscopic galaxy redshift surveys will be able to measure the Doppler magnification effect with sufficient signal-to-noise to test GR on large scales.
Abstract: The apparent sizes and brightnesses of galaxies are correlated in a dipolar pattern around matter overdensities in redshift space, appearing larger on their near side and smaller on their far side. The opposite effect occurs for galaxies around an underdense region. These patterns of apparent magnification induce dipole and higher multipole terms in the cross-correlation of galaxy number density fluctuations with galaxy size/brightness (which is sensitive to the convergence field). This provides a means of directly measuring peculiar velocity statistics at low and intermediate redshift, with several advantages for performing cosmological tests of GR. In particular, it does not depend on empirically-calibrated scaling relations like the Tully-Fisher and Fundamental Plane methods. We show that the next generation of spectroscopic galaxy redshift surveys will be able to measure the Doppler magnification effect with sufficient signal-to-noise to test GR on large scales. We illustrate this with forecasts for the constraints that can be achieved on parametrised deviations from GR for forthcoming low-redshift galaxy surveys with DESI and SKA2. Although the cross-correlation statistic considered has a lower signal to noise than RSD, it will be a useful probe of GR since it is sensitive to different systematics.
TL;DR: In this paper, a full-sky derivation of weak lensing observables in the Post-Friedmann (PF) formalism is presented, accounting for scalar, vector and tensor perturbations, as well as galaxies' peculiar velocities.
Abstract: We present a full-sky derivation of weak lensing observables in the Post-Friedmann (PF) formalism. Weak lensing has the characteristic of mixing small scales and large scales since it is affected by inhomogeneities integrated along the photon trajectory. With the PF formalism, we develop a modelling of lensing observables which encompasses both leading order relativistic effects and effects that are due to the fully non-linear matter distribution at small scales. We derive the reduced shear, convergence and rotation up to order $1/c^4$ in the PF approximation, accounting for scalar, vector and tensor perturbations, as well as galaxies' peculiar velocities. We discuss the various contributions that break the Kaiser-Squires relation between the shear and the convergence at different orders. We pay particular attention to the impact of the frame-dragging vector potential on lensing observables and we discuss potential ways to measure this effect in future lensing surveys.
Fermilab1, University of Michigan2, University of Sussex3, Stanford University4, Ludwig Maximilian University of Munich5, University of Portsmouth6, University of Manchester7, Liverpool John Moores University8, University of Nottingham9, University of KwaZulu-Natal10, University of Edinburgh11, Texas A&M University12, Uppsala University13, Lancaster University14, University of Porto15, University College London16, Rhodes University17, Institut d'Astrophysique de Paris18, University of Illinois at Urbana–Champaign19, IFAE20, Spanish National Research Council21, University of Pennsylvania22, California Institute of Technology23, Autonomous University of Madrid24, Ohio State University25, University of Washington26, University of California, Santa Cruz27, Australian Astronomical Observatory28, University of São Paulo29, Princeton University30, Catalan Institution for Research and Advanced Studies31, University of Southampton32, State University of Campinas33, Oak Ridge National Laboratory34
TL;DR: The authors constrain the luminosity function (LF) of cluster red-sequence galaxies as a function of the red-shift of the X-ray selected clusters in the Dark Energy Survey Science Verification data.
Abstract: Using similar to 100 X-ray selected clusters in the Dark Energy Survey Science Verification data, we constrain the luminosity function ( LF) of cluster red-sequence galaxies as a function of redshi ...
TL;DR: In this article, the dependence of the interactions of intermediate-size ½ self-interstitial atom (SIA) loops with an edge dislocation was investigated by molecular dynamics simulations for the interatomic potential derived by Ackland et al. (A97).
Abstract: The dependence of the interactions of intermediate-size ½ self-interstitial atom (SIA) loops with an edge dislocation on strain rate and temperature was investigated by molecular dynamics (MD) simulations for the interatomic potential derived by Ackland et al. (A97). For low temperatures (T = 1 K), the mechanisms of the interactions were in agreement with recent literature. It was shown that a second passing of the dislocation through the loop led to a different mechanism than the one that occurred upon first passing. Since these mechanisms are associated with different SIA loop sizes, and since the loop lost a number of SIAs upon first interaction, it was deduced that the dividing threshold between large and small loops (rendering them strong or weak obstacles, respectively) is at the vicinity of the loop size studied (169 SIAs). For higher temperatures (T = 300 K), the strain rate dependence proved strong: for low strain rates, the dislocation absorbed the loop as a double super-jog almost ...
TL;DR: In this article, a full-sky derivation of weak lensing observables in the Post-Friedmann (PF) formalism is presented, accounting for scalar, vector and tensor perturbations, as well as galaxies' peculiar velocities.
Abstract: We present a full-sky derivation of weak lensing observables in the Post-Friedmann (PF) formalism. Weak lensing has the characteristic of mixing small scales and large scales since it is affected by inhomogeneities integrated along the photon trajectory. With the PF formalism, we develop a modelling of lensing observables which encompasses both leading order relativistic effects and effects that are due to the fully non-linear matter distribution at small scales. We derive the reduced shear, convergence and rotation up to order $1/c^4$ in the PF approximation, accounting for scalar, vector and tensor perturbations, as well as galaxies' peculiar velocities. We discuss the various contributions that break the Kaiser-Squires relation between the shear and the convergence at different orders. We pay particular attention to the impact of the frame-dragging vector potential on lensing observables and we discuss potential ways to measure this effect in future lensing surveys.
22 Oct 2019
TL;DR: The results show, that the machine learning approach is appropriate to benchmark national innovation profiles, to identify key determinants on a cluster as well as on a national level whilst considering correlating features and long term effects.
Abstract: National innovation performance is essential for being economically competitive. The key determinants for its increase or decrease and the impact of governmental decisions or policy instruments are still not clear. Recent approaches are either limited due to qualitatively selected features or due to a small database with few observations. The aim of this paper is to propose a suitable machine learning approach for national innovation performance data analysis. We use clustering and correlation analysis, Bayesian Neural Network with Local Interpretable Model-Agnostic Explanations and BreakDown for decomposing innovation output prediction. Our results show, that the machine learning approach is appropriate to benchmark national innovation profiles, to identify key determinants on a cluster as well as on a national level whilst considering correlating features and long term effects and the impact of changes in innovation input (e.g. by governmental decision or innovation policy) on innovation output can be predicted and herewith the increase or decrease of national innovation performance.
TL;DR: In this paper, the authors used the X-ray surface brightness measurements of the Coma cluster and from 58 stacked galaxy clusters along with the weak lensing data to test the theory of emergent gravity.
Abstract: Verlinde's theory of Emergent Gravity (EG) describes gravity as an emergent phenomenon rather than a fundamental force. Applying this reasoning in de Sitter space leads to gravity behaving differently on galaxy and galaxy cluster scales; this excess gravity might offer an alternative to dark matter. Here we test these ideas using the data from the Coma cluster and from 58 stacked galaxy clusters. The X-ray surface brightness measurements of the clusters at $0.1 < z < 1.2$ along with the weak lensing data are used to test the theory. We find that the simultaneous EG fits of the X-ray and weak lensing datasets are significantly worse than those provided by General Relativity (with cold dark matter). For the Coma cluster, the predictions from Emergent Gravity and General Relativity agree in the range of 250 - 700 kpc, while at around 1 Mpc scales, EG total mass predictions are larger by a factor of 2. For the cluster stack the predictions are only in good agreement at around the 1 - 2 Mpc scales, while for $r \gtrsim 10$ Mpc EG is in strong tension with the data. According to the Bayesian information criterion analysis, GR is preferred in all tested datasets; however, we also discuss possible modifications of EG that greatly relax the tension with the data.