Clash-Vlt: Dissecting the Frontier Fields Galaxy Cluster Macs J0416.1-2403 With ∼800 Spectra of Member Galaxies

Balestra, I.; Mercurio, A.; Sartoris, B.; Girardi, M.; Grillo, C.; Nonino, M.; Rosati, P.; Biviano, A.; Ettori, S.; Forman, W.; Jones, C.; Koekemoer, Anton M.; Medezinski, Elinor; Merten, Julian; Ogrean, G. A.; Tozzi, P.; Umetsu, Keiichi; Vanzella, E.; Weeren, R. J. van; Zitrin, Adi; Annunziatella, Marianna; Caminha, G. B.; Broadhurst, Tom; Coe, Dan; Donahue, M.; Fritz, A.; Frye, Brenda; Kelson, Daniel D.; Lombardi, Marco; Maier, C.; Meneghetti, M.; Monna, A.; Postman, Marc; Scodeggio, M.; Seitz, S.; Ziegler, B.

doi:10.3847/0067-0049/224/2/33

Cited by 111 publications

(158 citation statements)

References 90 publications

(141 reference statements)

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“…CLASH-VLT collected a large sample of spectra for galaxies in the field of view of this cluster, leading to the spectroscopic confirmation of ∼ 800 cluster members and to the discovery of multiply-imaged background sources. More details on VIMOS spectroscopic data can be found in Balestra et al (2016). These data have been used to obtain a precise total reconstruction of the cluster via gravitational strong lensing modeling (Grillo et al 2015).…”

Section: Data Samplementioning

confidence: 99%

Mass Profile Decomposition of the Frontier Fields Cluster MACS J0416-2403: Insights on the Dark-matter Inner Profile

Annunziatella

Bonamigo

Grillo

et al. 2017

ApJ

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We present a high resolution dissection of the two-dimensional total mass distribution in the core of the Hubble Frontier Fields galaxy cluster MACS J0416.1−2403, at z = 0.396. We exploit HST/WFC3 near-IR (F160W) imaging, VLT/MUSE spectroscopy, and Chandra data to separate the stellar, hot gas, and dark-matter mass components in the inner 300 kpc of the cluster. We combine the recent results of our refined strong lensing analysis, which includes the contribution of the intracluster gas, with the modeling of the surface brightness and stellar mass distributions of 193 cluster members, of which 144 are spectroscopically confirmed. We find that moving from 10 to 300 kpc from the cluster center the stellar to total mass fraction decreases from 12% to 1% and the hot gas to total mass fraction increases from 3% to 9%, resulting in a baryon fraction of approximatively 10% at the outermost radius. We measure that the stellar component represents ∼ 30%, near the cluster center, and 15%, at larger clustercentric distances, of the total mass in the cluster substructures. We subtract the baryonic mass component from the total mass distribution and conclude that within 30 kpc (∼ 3 times the effective radius of the BCG) from the cluster center the surface mass density profile of the total mass and global (cluster plus substructures) dark-matter are steeper and that of the diffuse (cluster) dark-matter is shallower than a NFW profile. Our current analysis does not point to a significant offset between the cluster stellar and dark-matter components. This detailed and robust reconstruction of the inner dark matter distribution in a larger sample of galaxy clusters will set a new benchmark for different structure formation scenarios.

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Section: Data Samplementioning

confidence: 99%

Mass Profile Decomposition of the Frontier Fields Cluster MACS J0416-2403: Insights on the Dark-matter Inner Profile

Annunziatella

Bonamigo

Grillo

et al. 2017

ApJ

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“…MAMPOSSt performs a maximum likelihood analysis of the distribution of cluster galaxies in projected phase-space, comparing it with theoretical distributions predicted by the Jeans equation (Binney & Tremaine 1987) for given models of the mass and velocity anisotropy profiles. It has been tested on cluster-size halos extracted from cosmological simulations (Mamon et al 2013) and applied to several galaxy clusters already Guennou et al 2014;Munari et al 2014;Durret et al 2015;Balestra et al 2016;Pizzuti et al 2016).…”

Section: The Mass Profilementioning

confidence: 99%

The dynamics ofz~ 1 clusters of galaxies from the GCLASS survey

Biviano

Burg

Muzzin

et al. 2016

A&A

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Context. The dynamics of clusters of galaxies and its evolution provide information on their formation and growth, on the nature of dark matter and on the evolution of the baryonic components. Poor observational constraints exist so far on the dynamics of clusters at redshift z > 0.8. Aims. We aim to constrain the internal dynamics of clusters of galaxies at redshift z ∼ 1, namely their mass profile M(r), velocity anisotropy profile β(r), and pseudo-phase-space density profiles Q(r) and Q r (r), obtained from the ratio between the mass density profile and the third power of the (total and, respectively, radial) velocity dispersion profiles of cluster galaxies. Methods. We used the spectroscopic and photometric data-set of 10 clusters at 0.87 < z < 1.34 from the Gemini Cluster Astrophysics Spectroscopic Survey (GCLASS). We determined the individual cluster masses from their velocity dispersions, then stack the clusters in projected phase-space. We investigated the internal dynamics of this stack cluster, using the spatial and velocity distribution of its member galaxies. We determined the stack cluster M(r) using the MAMPOSSt method, and its β(r) by direct inversion of the Jeans equation. The procedures used to determine the two aforementioned profiles also allowed us to determine Q(r) and Q r (r). Results. Several M(r) models are statistically acceptable for the stack cluster (Burkert, Einasto, Hernquist, NFW). The stack cluster total mass concentration, c ≡ r 200 /r −2 = 4.0 +1.0 −0.6 , is in agreement with theoretical expectations. The total mass distribution is less concentrated than both the cluster stellar-mass and the cluster galaxies distributions. The stack cluster β(r) indicates that galaxy orbits are isotropic near the cluster center and become increasingly radially elongated with increasing cluster-centric distance. Passive and star-forming galaxies have similar β(r). The observed β(r) is similar to that of dark matter particles in simulated cosmological halos. Q(r) and Q r (r) are almost power-law relations with slopes similar to those predicted from numerical simulations of dark matter halos. Conclusions. Comparing our results with those obtained for lower-redshift clusters, we conclude that the evolution of the concentration-total mass relation and pseudo-phase-space density profiles agree with the expectations from ΛCDM cosmological simulations. The fact that Q(r) and Q r (r) already follow the theoretical expectations in z ∼ 1 clusters suggest these profiles are the result of rapid dynamical relaxation processes, such as violent relaxation. The different concentrations of the total and stellar mass distribution, and their subsequent evolution, can be explained by merging processes of central galaxies leading to the formation of the brightest cluster galaxy. The orbits of passive cluster galaxies appear to become more isotropic with time, while those of starforming galaxies do not evolve, presumably because star-formation is quenched on a shorter timescale than that required for orbital is...

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“…Only two 4h-pointings were performed, one using the low-resolution blue grism (covering the spectral range of 3700-6700 Å with a resolution of 180) and one using the medium-resolution (MR) red grism (which covers the 4800-10 000 Å with a resolution of 580). The spectra were reduced with the VIMOS Interactive Pipeline and Graphical Interface (VIPGI; Scodeggio et al 2005) and redshifts were measured following the procedure described in Balestra et al (2016). A quality flag (QF) is assigned to each spectroscopic redshift depending on if it is 'secure' (QF = 3), 'likely' (QF = 2), 'insecure' (QF = 1) or if it is based on a strong emission line (QF = 9).…”

Section: Vlt Spectroscopymentioning

confidence: 99%

“…The combination of different independent techniques [stellar kinematics in the brightest cluster galaxy (BCG), X-ray, weak and strong lensing (SL), stellar kinematics, etc.] allows one to robustly constrain the DM density profile of galaxy clusters from the inner region up to large radial distances (∼5 Mpc; see Sand, Treu & Ellis 2002;Sand et al 2004;Newman et al 2009Newman et al , 2011Umetsu et al 2012Umetsu et al , 2016Biviano et al 2013;Balestra et al 2016). Gravitational lensing offers a unique technique to investigate the mass distribution of galaxy clusters, since it is generated by the total mass of the lens, i.e.…”

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confidence: 99%

Precise strong lensing mass profile of the CLASH galaxy cluster MACS 2129

Monna

Seitz

Balestra

et al. 2017

Mon. Not. R. Astron. Soc.

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We present a detailed strong lensing (SL) mass reconstruction of the core of the galaxy cluster MACS J2129.4−0741 (z cl = 0.589) obtained by combining high-resolution Hubble Space Telescope photometry from the CLASH (Cluster Lensing And Supernovae survey with Hubble) survey with new spectroscopic observations from the CLASH-VLT (Very Large Telescope) survey. A background bright red passive galaxy at z sp = 1.36, sextuply lensed in the cluster core, has four radial lensed images located over the three central cluster members. Further 19 background lensed galaxies are spectroscopically confirmed by our VLT survey, including 3 additional multiple systems. A total of 31 multiple images are used in the lensing analysis. This allows us to trace with high precision the total mass profile of the cluster in its very inner region (R < 100 kpc). Our final lensing mass model reproduces the multiple images systems identified in the cluster core with high accuracy of 0.4 arcsec. This translates to a high-precision mass reconstruction of MACS 2129, which is constrained at a level of 2 per cent. The cluster has Einstein parameter E = (29 ± 4) arcsec and a projected total mass of M tot (< E ) = (1.35 ± 0.03) × 10 14 M within such radius. Together with the cluster mass profile, we provide here also the complete spectroscopic data set for the cluster members and lensed images measured with VLT/Visible Multi-Object Spectrograph within the CLASH-VLT survey.

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Clash-Vlt: Dissecting the Frontier Fields Galaxy Cluster Macs J0416.1-2403 With ∼800 Spectra of Member Galaxies

Cited by 111 publications

References 90 publications

Mass Profile Decomposition of the Frontier Fields Cluster MACS J0416-2403: Insights on the Dark-matter Inner Profile

Mass Profile Decomposition of the Frontier Fields Cluster MACS J0416-2403: Insights on the Dark-matter Inner Profile

The dynamics ofz~ 1 clusters of galaxies from the GCLASS survey

Precise strong lensing mass profile of the CLASH galaxy cluster MACS 2129

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