13 results on '"Grillo, Claudio"'
Search Results
2. Early Results from GLASS-JWST. XIX. A High Density of Bright Galaxies at z ≈ 10 in the A2744 Region.
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Castellano, Marco, Fontana, Adriano, Treu, Tommaso, Merlin, Emiliano, Santini, Paola, Bergamini, Pietro, Grillo, Claudio, Rosati, Piero, Acebron, Ana, Leethochawalit, Nicha, Paris, Diego, Bonchi, Andrea, Belfiori, Davide, Calabrò, Antonello, Correnti, Matteo, Nonino, Mario, Polenta, Gianluca, Trenti, Michele, Boyett, Kristan, and Brammer, G.
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- 2023
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3. Early Results from GLASS-JWST. XIII. A Faint, Distant, and Cold Brown Dwarf.
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Nonino, Mario, Glazebrook, Karl, Burgasser, Adam J., Polenta, Gianluca, Morishita, Takahiro, Lepinzan, Marius, Castellano, Marco, Fontana, Adriano, Merlin, Emiliano, Bonchi, Andrea, Paris, Diego, Treu, Tommaso, Vulcani, Benedetta, Wang, Xin, Santini, Paola, Vanzella, Eros, Nanayakkara, Themiya, Mercurio, Amata, Rosati, Piero, and Grillo, Claudio
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- 2023
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4. Early Results from GLASS-JWST. IX. First Spectroscopic Confirmation of Low-mass Quiescent Galaxies at z > 2 with NIRISS.
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Marchesini, Danilo, Brammer, Gabriel, Morishita, Takahiro, Bergamini, Pietro, Wang, Xin, Bradac, Marusa, Roberts-Borsani, Guido, Strait, Victoria, Treu, Tommaso, Fontana, Adriano, Jones, Tucker, Santini, Paola, Vulcani, Benedetta, Acebron, Ana, Calabrò, Antonello, Castellano, Marco, Glazebrook, Karl, Grillo, Claudio, Mercurio, Amata, and Nanayakkara, Themiya
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- 2023
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5. Unveiling the Dynamical State of Massive Clusters through the ICL Fraction
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Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (Brasil), Conselho Nacional de Desenvolvimento Científico e Tecnológico (Brasil), Consejo Superior de Investigaciones Científicas (España), Ministerio de Economía y Competitividad (España), European Commission, Academia Sinica (Taiwan), Ministry of Science and Technology (Taiwan), Ministero degli Affari Esteri e della Cooperazione Internazionale, Jiménez-Teja, Y., Dupke, Renato A., Benítez, Narciso, Koekemoer, Anton M., Zitrin, Adi, Umetsu, Keiichi, Ziegler, Bodo L., Frye, Brenda L., Ford, Holland, Bouwens, Rychard J., Bradley, Larry D., Broadhurst, Thomas, Coe, Dan, Donahue, Megan, Graves, Genevieve J., Grillo, Claudio, Infante, Leopoldo, Jouvel, Stephanie, Kelson, Daniel D., Lahav, Ofer, Lazkoz, Ruth, Lemze, Dorom, Maoz, Dan, Medezinski, Elinor, Melchior, Peter, Meneghetti, Massimo, Mercurio, Amata, Merten, Julian, Molino, Alberto, Moustakas, Leonidas A., Nonino, Mario, Ogaz, Sara, Riess, Adam G., Rosati, Piero, Sayers, Jack, Seitz, Stella, Zheng, Wei, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (Brasil), Conselho Nacional de Desenvolvimento Científico e Tecnológico (Brasil), Consejo Superior de Investigaciones Científicas (España), Ministerio de Economía y Competitividad (España), European Commission, Academia Sinica (Taiwan), Ministry of Science and Technology (Taiwan), Ministero degli Affari Esteri e della Cooperazione Internazionale, Jiménez-Teja, Y., Dupke, Renato A., Benítez, Narciso, Koekemoer, Anton M., Zitrin, Adi, Umetsu, Keiichi, Ziegler, Bodo L., Frye, Brenda L., Ford, Holland, Bouwens, Rychard J., Bradley, Larry D., Broadhurst, Thomas, Coe, Dan, Donahue, Megan, Graves, Genevieve J., Grillo, Claudio, Infante, Leopoldo, Jouvel, Stephanie, Kelson, Daniel D., Lahav, Ofer, Lazkoz, Ruth, Lemze, Dorom, Maoz, Dan, Medezinski, Elinor, Melchior, Peter, Meneghetti, Massimo, Mercurio, Amata, Merten, Julian, Molino, Alberto, Moustakas, Leonidas A., Nonino, Mario, Ogaz, Sara, Riess, Adam G., Rosati, Piero, Sayers, Jack, Seitz, Stella, and Zheng, Wei
- Abstract
We have selected a sample of 11 massive clusters of galaxies observed by the Hubble Space Telescope in order to study the impact of the dynamical state on the intracluster light (ICL) fraction, the ratio of total integrated ICL to the total galaxy member light. With the exception of the Bullet cluster, the sample is drawn from the Cluster Lensing and Supernova Survey and the Frontier Fields program, containing five relaxed and six merging clusters. The ICL fraction is calculated in three optical filters using the CHEFs ICL estimator, a robust and accurate algorithm free of a priori assumptions. We find that the ICL fraction in the three bands is, on average, higher for the merging clusters, ranging between ∼7% and 23%, compared with the ∼2%-11% found for the relaxed systems. We observe a nearly constant value (within the error bars) in the ICL fraction of the regular clusters at the three wavelengths considered, which would indicate that the colors of the ICL and the cluster galaxies are, on average, coincident and, thus, so are their stellar populations. However, we find a higher ICL fraction in the F606W filter for the merging clusters, consistent with an excess of lower-metallicity/younger stars in the ICL, which could have migrated violently from the outskirts of the infalling galaxies during the merger event. © 2018. The American Astronomical Society. All rights reserved.
- Published
- 2018
6. CLASH: COMPLETE LENSING ANALYSIS OF THE LARGEST COSMIC LENS MACS J0717.5+3745 AND SURROUNDING STRUCTURES.
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Medezinski, Elinor, Umetsu, Keiichi, Nonino, Mario, Merten, Julian, Zitrin, Adi, Broadhurst, Tom, Donahue, Megan, Sayers, Jack, Waizmann, Jean-Claude, Koekemoer, Anton, Coe, Dan, Molino, Alberto, Melchior, Peter, Mroczkowski, Tony, Czakon, Nicole, Postman, Marc, Meneghetti, Massimo, Lemze, Doron, Ford, Holland, and Grillo, Claudio
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GALAXY clusters ,GRAVITATIONAL lenses ,ACCRETION (Astrophysics) ,SUPERNOVAE ,ASTROPHYSICS research - Abstract
The galaxy cluster MACS J0717.5+3745 (z = 0.55) is the largest known cosmic lens, with complex internal structures seen in deep X-ray, Sunyaev-Zel'dovich effect, and dynamical observations. We perform a combined weak- and strong-lensing analysis with wide-field BVR
c i′z′ Subaru/Suprime-Cam observations and 16-band Hubble Space Telescope observations taken as part of the Cluster Lensing And Supernova survey with Hubble. We find consistent weak distortion and magnification measurements of background galaxies and combine these signals to construct an optimally estimated radial mass profile of the cluster and its surrounding large-scale structure out to 5 Mpc h–1 . We find consistency between strong-lensing and weak-lensing in the region where these independent data overlap, <500 kpc h–1 . The two-dimensional weak-lensing map reveals a clear filamentary structure traced by distinct mass halos. We model the lensing shear field with nine halos, including the main cluster, corresponding to mass peaks detected above 2.5σκ . The total mass of the cluster as determined by the different methods is Mvir ≈ (2.8 ± 0.4) × 1015 M☼ . Although this is the most massive cluster known at z > 0.5, in terms of extreme value statistics, we conclude that the mass of MACS J0717.5+3745 by itself is not in serious tension with ΛCDM, representing only a ∼2σ departure above the maximum simulated halo mass at this redshift. [ABSTRACT FROM AUTHOR]- Published
- 2013
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7. GALAXY HALO TRUNCATION AND GIANT ARC SURFACE BRIGHTNESS RECONSTRUCTION IN THE CLUSTER MACSJ1206.2-0847.
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EICHNER, THOMAS, SEITZ, STELLA, SUYU, SHERRY H., HALKOLA, ALEKSI, UMETSU, KEIICHI, ZITRIN, ADI, COE, DAN, MONNA, ANNA, ROSATI, PIERO, GRILLO, CLAUDIO, BALESTRA, ITALO, POSTMAN, MARC, KOEKEMOER, ANTON, WEI ZHENG, HØST, OLE, LEMZE, DORON, BROADHURST, TOM, MOUSTAKAS, LEONIDAS, BRADLEY, LARRY, and MOLINO, ALBERTO
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GALAXIES ,X-ray emission spectroscopy ,STAR clusters ,SURFACE brightness (Astronomy) ,GRAVITATIONAL lenses - Abstract
In this work, we analyze the mass distribution of MACSJ1206.2-0847, particularly focusing on the halo properties of its cluster members. The cluster appears relaxed in its X-ray emission, but has a significant amount of intracluster light that is not centrally concentrated, suggesting that galaxy-scale interactions are still ongoing despite the overall relaxed state. The cluster lenses 12 background galaxies into multiple images and one galaxy at z = 1.033 into a giant arc and its counterimage. The multiple image positions and the surface brightness (SFB) distribution of the arc, which is bent around several cluster members, are sensitive to the cluster galaxy halo properties. We model the cluster mass distribution with a Navarro-Frenk-White profile and the galaxy halos with two parameters for the mass normalization and the extent of a reference halo assuming scalings with their observed near-infrared light. We match the multiple image positions at an rms level of 0. ''85 and can reconstruct the SFB distribution of the arc in several filters to a remarkable accuracy based on this cluster model. The length scale where the enclosed galaxy halo mass is best constrained is about 5 effective radii-a scale in between those accessible to dynamical and field strong-lensing mass estimates on the one hand and galaxy-galaxy weak-lensing results on the other hand. The velocity dispersion and halo size of a galaxy with m160W,AB = 19.2 and M
B,Vega = -20.7 are σ = 150 km s-1 and r ≈ 26±6 kpc, respectively, indicating that the halos of the cluster galaxies are tidally stripped.We also reconstruct the unlensed source, which is smaller by a factor of ~5.8 in area, demonstrating the increase in morphological information due to lensing. We conclude that this galaxy likely has star-forming spiral arms with a red (older) central component. [ABSTRACT FROM AUTHOR]- Published
- 2013
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8. HUBBLE SPACE TELESCOPE COMBINED STRONG AND WEAK LENSING ANALYSIS OF THE CLASH SAMPLE: MASS AND MAGNIFICATION MODELS AND SYSTEMATIC UNCERTAINTIES.
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Zitrin, Adi, Fabris, Agnese, Merten, Julian, Melchior, Peter, Meneghetti, Massimo, Koekemoer, Anton, Coe, Dan, Maturi, Matteo, Bartelmann, Matthias, Postman, Marc, Umetsu, Keiichi, Seidel, Gregor, Sendra, Irene, Broadhurst, Tom, Balestra, Italo, Biviano, Andrea, Grillo, Claudio, Mercurio, Amata, Nonino, Mario, and Rosati, Piero
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GALAXY clusters ,GRAVITATIONAL lenses ,DARK matter ,REDSHIFT - Abstract
We present results from a comprehensive lensing analysis in Hubble Space Telescope (HST) data of the complete Cluster Lensing And Supernova survey with Hubble cluster sample. We identify previously undiscovered multiple images, allowing improved or first constraints on the cluster inner mass distributions and profiles. We combine these strong lensing constraints with weak lensing shape measurements within the HST field of view (FOV) to jointly constrain the mass distributions. The analysis is performed in two different common parameterizations (one adopts light-traces-mass for both galaxies and dark matter while the other adopts an analytical, elliptical Navarro-Frenk-White form for the dark matter) to provide a better assessment of the underlying systematics—which is most important for deep, cluster-lensing surveys, especially when studying magnified high-redshift objects. We find that the typical (median), relative systematic differences throughout the central FOV are ∼40% in the (dimensionless) mass density, κ, and ∼20% in the magnification, μ. We show maps of these differences for each cluster, as well as the mass distributions, critical curves, and two-dimensional (2D)-integrated mass profiles. For the Einstein radii (z
s = 2) we find that all typically agree within 10% between the two models, and Einstein masses agree, typically, within ∼15%. At larger radii, the total projected, 2D-integrated mass profiles of the two models, within r ∼ 2′, differ by ∼30%. Stacking the surface-density profiles of the sample from the two methods together, we obtain an average slope of dlog (Σ)/dlog (r) ∼ –0.64 ± 0.1, in the radial range [5350] kpc. Last, we also characterize the behavior of the average magnification, surface density, and shear differences between the two models as a function of both the radius from the center and the best-fit values of these quantities. All mass models and magnification maps are made publicly available for the community. [ABSTRACT FROM AUTHOR]- Published
- 2015
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9. CLASH: WEAK-LENSING SHEAR-AND-MAGNIFICATION ANALYSIS OF 20 GALAXY CLUSTERS.
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Umetsu, Keiichi, Medezinski, Elinor, Nonino, Mario, Merten, Julian, Postman, Marc, Meneghetti, Massimo, Donahue, Megan, Czakon, Nicole, Molino, Alberto, Seitz, Stella, Gruen, Daniel, Lemze, Doron, Balestra, Italo, Benítez, Narciso, Biviano, Andrea, Broadhurst, Tom, Ford, Holland, Grillo, Claudio, Koekemoer, Anton, and Melchior, Peter
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DARK matter ,OPEN clusters of stars ,METAPHYSICAL cosmology ,STAR clusters ,GRAVITATIONAL lenses - Abstract
We present a joint shear-and-magnification weak-lensing analysis of a sample of 16 X-ray-regular and 4 high-magnification galaxy clusters at 0.19 ≲ z ≲ 0.69 selected from the Cluster Lensing And Supernova survey with Hubble (CLASH). Our analysis uses wide-field multi-color imaging, taken primarily with Suprime-Cam on the Subaru Telescope. From a stacked-shear-only analysis of the X-ray-selected subsample, we detect the ensemble-averaged lensing signal with a total signal-to-noise ratio of ≃ 25 in the radial range of 200-3500 kpc h
–1 , providing integrated constraints on the halo profile shape and concentration-mass relation. The stacked tangential-shear signal is well described by a family of standard density profiles predicted for dark-matter-dominated halos in gravitational equilibrium, namely, the Navarro-Frenk-White (NFW), truncated variants of NFW, and Einasto models. For the NFW model, we measure a mean concentration of at an effective halo mass of . We show that this is in excellent agreement with Λ cold dark matter (ΛCDM) predictions when the CLASH X-ray selection function and projection effects are taken into account. The best-fit Einasto shape parameter is , which is consistent with the NFW-equivalent Einasto parameter of ∼0.18. We reconstruct projected mass density profiles of all CLASH clusters from a joint likelihood analysis of shear-and-magnification data and measure cluster masses at several characteristic radii assuming an NFW density profile. We also derive an ensemble-averaged total projected mass profile of the X-ray-selected subsample by stacking their individual mass profiles. The stacked total mass profile, constrained by the shear+magnification data, is shown to be consistent with our shear-based halo-model predictions, including the effects of surrounding large-scale structure as a two-halo term, establishing further consistency in the context of the ΛCDM model. [ABSTRACT FROM AUTHOR]- Published
- 2014
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10. CLASH-X: A COMPARISON OF LENSING AND X-RAY TECHNIQUES FOR MEASURING THE MASS PROFILES OF GALAXY CLUSTERS.
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Donahue, Megan, Voit, G. Mark, Mahdavi, Andisheh, Umetsu, Keiichi, Ettori, Stefano, Merten, Julian, Postman, Marc, Hoffer, Aaron, Baldi, Alessandro, Coe, Dan, Czakon, Nicole, Bartelmann, Mattias, Benitez, Narciso, Bouwens, Rychard, Bradley, Larry, Broadhurst, Tom, Ford, Holland, Gastaldello, Fabio, Grillo, Claudio, and Infante, Leopoldo
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GALAXY clusters ,X-ray spectra ,DARK matter ,GRAVITATIONAL lenses - Abstract
We present profiles of temperature, gas mass, and hydrostatic mass estimated from new and archival X-ray observations of CLASH clusters. We compare measurements derived from XMM and Chandra observations with one another and compare both to gravitational lensing mass profiles derived with CLASH Hubble Space Telescope and Subaru Telescope lensing data. Radial profiles of Chandra and XMM measurements of electron density and enclosed gas mass are nearly identical, indicating that differences in hydrostatic masses inferred from X-ray observations arise from differences in gas-temperature measurements. Encouragingly, gas temperatures measured in clusters by XMM and Chandra are consistent with one another at ∼100-200 kpc radii, but XMM temperatures systematically decline relative to Chandra temperatures at larger radii. The angular dependence of the discrepancy suggests that additional investigation on systematics such as the XMM point-spread function correction, vignetting, and off-axis responses is yet required. We present the CLASH-X mass-profile comparisons in the form of cosmology-independent and redshift-independent circular-velocity profiles. We argue that comparisons of circular-velocity profiles are the most robust way to assess mass bias. Ratios of Chandra hydrostatic equilibrium (HSE) mass profiles to CLASH lensing profiles show no obvious radial dependence in the 0.3-0.8 Mpc range. However, the mean mass biases inferred from the weak-lensing (WL) and SaWLens data are different. As an example, the weighted-mean value at 0.5 Mpc is 〈 b〉 = 0.12 for the WL comparison and 〈 b〉 = –0.11 for the SaWLens comparison. The ratios of XMM HSE mass profiles to CLASH lensing profiles show a pronounced radial dependence in the 0.3-1.0 Mpc range, with a weighted mean mass bias value rising to 〈 b〉 ≳ 0.3 at ∼1 Mpc for the WL comparison and 〈 b〉 ≈ 0.25 for the SaWLens comparison. The enclosed gas mass profiles from both Chandra and XMM rise to a value ≈1/8 times the total-mass profiles inferred from lensing at ≈0.5 Mpc and remain constant outside of that radius, suggesting that M
gas × 8 profiles may be an excellent proxy for total-mass profiles at ≳ 0.5 Mpc in massive galaxy clusters. [ABSTRACT FROM AUTHOR]- Published
- 2014
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11. CLASH-VLT: CONSTRAINTS ON THE DARK MATTER EQUATION OF STATE FROM ACCURATE MEASUREMENTS OF GALAXY CLUSTER MASS PROFILES.
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Sartoris, Barbara, Biviano, Andrea, Rosati, Piero, Borgani, Stefano, Umetsu, Keiichi, Bartelmann, Matthias, Girardi, Marisa, Grillo, Claudio, Lemze, Doron, Zitrin, Adi, Balestra, Italo, Mercurio, Amata, Nonino, Mario, Postman, Marc, Czakon, Nicole, Bradley, Larry, Broadhurst, Tom, Coe, Dan, Medezinski, Elinor, and Melchior, Peter
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- 2014
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12. A BRIGHTEST CLUSTER GALAXY WITH AN EXTREMELY LARGE FLAT CORE.
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Postman, Marc, Lauer, Tod R., Donahue, Megan, Graves, Genevieve, Coe, Dan, Moustakas, John, Koekemoer, Anton, Bradley, Larry, Ford, Holland C., Grillo, Claudio, Zitrin, Adi, Lemze, Doron, Broadhurst, Tom, Moustakas, Leonidas, Ascaso, Begoña, Medezinski, Elinor, and Kelson, Daniel
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GALAXY clusters ,SUPERNOVAE spectra ,PHOTOMETRY ,STELLAR luminosity function - Abstract
Hubble Space Telescope images of the galaxy cluster A2261, obtained as part of the Cluster Lensing And Supernova survey with Hubble, show that the brightest galaxy in the cluster, A2261-BCG, has the largest core yet detected in any galaxy. The cusp radius of A2261-BCG is 3.2 kpc, twice as big as the next largest core known, and ∼3 × bigger than those typically seen in the most luminous brightest cluster galaxies. The morphology of the core in A2261-BCG is also unusual, having a completely flat interior surface brightness profile, rather than the typical shallow cusp rising into the center. This implies that the galaxy has a core with constant or even centrally decreasing stellar density. Interpretation of the core as an end product of the “scouring” action of a binary supermassive black hole implies a total black hole mass ∼10
10 M☼ from the extrapolation of most relationships between core structure and black hole mass. The core falls 1σ above the cusp radius versus galaxy luminosity relation. Its large size in real terms, and the extremely large black hole mass required to generate it, raises the possibility that the core has been enlarged by additional processes, such as the ejection of the black holes that originally generated the core. The flat central stellar density profile is consistent with this hypothesis. The core is also displaced by 0.7 kpc from the center of the surrounding envelope, consistent with a local dynamical perturbation of the core. [ABSTRACT FROM AUTHOR]- Published
- 2012
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13. CLASH: MASS DISTRIBUTION IN AND AROUND MACS J1206.2-0847 FROM A FULL CLUSTER LENSING ANALYSIS.
- Author
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Umetsu, Keiichi, Medezinski, Elinor, Nonino, Mario, Merten, Julian, Zitrin, Adi, Molino, Alberto, Grillo, Claudio, Carrasco, Mauricio, Donahue, Megan, Mahdavi, Andisheh, Coe, Dan, Postman, Marc, Koekemoer, Anton, Czakon, Nicole, Sayers, Jack, Mroczkowski, Tony, Golwala, Sunil, Koch, Patrick M., Lin, Kai-Yang, and Molnar, Sandor M.
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GALAXY clusters ,GRAVITATIONAL lenses ,METAPHYSICAL cosmology ,DARK matter - Abstract
We derive an accurate mass distribution of the galaxy cluster MACS J1206.2-0847 (z = 0.439) from a combined weak-lensing distortion, magnification, and strong-lensing analysis of wide-field Subaru BVR
c Ic z′ imaging and our recent 16-band Hubble Space Telescope observations taken as part of the Cluster Lensing And Supernova survey with Hubble program. We find good agreement in the regions of overlap between several weak- and strong-lensing mass reconstructions using a wide variety of modeling methods, ensuring consistency. The Subaru data reveal the presence of a surrounding large-scale structure with the major axis running approximately northwest-southeast (NW-SE), aligned with the cluster and its brightest galaxy shapes, showing elongation with a ∼2: 1 axis ratio in the plane of the sky. Our full-lensing mass profile exhibits a shallow profile slope dln Σ/dln R ∼ –1 at cluster outskirts (R ≳ 1 Mpc h–1 ), whereas the mass distribution excluding the NW-SE excess regions steepens farther out, well described by the Navarro-Frenk-White form. Assuming a spherical halo, we obtain a virial mass Mvir = (1.1 ± 0.2 ± 0.1) × 1015 M☼ h–1 and a halo concentration cvir = 6.9 ± 1.0 ± 1.2 (cvir ∼ 5.7 when the central 50 kpc h–1 is excluded), which falls in the range 4 ≲ 〈 c〉 ≲ 7 of average c(M, z) predictions for relaxed clusters from recent Λ cold dark matter simulations. Our full-lensing results are found to be in agreement with X-ray mass measurements where the data overlap, and when combined with Chandra gas mass measurements, they yield a cumulative gas mass fraction of 13.7+4.5 – 3.0 % at 0.7 Mpc h–1 (≈ 1.7 r2500 ), a typical value observed for high-mass clusters. [ABSTRACT FROM AUTHOR]- Published
- 2012
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