Mass and galaxy distributions of four massive galaxy clusters from Dark Energy Survey Science Verification data

Melchior, P.; Suchyta, E.; Huff, Eric; Hirsch, Michael; Kacprzak, T.; Rykoff, E. S.; Gruen, D.; Armstrong, R.; Bacon, David; Bechtol, K.; Bernstein, G. M.; Bridle, Sarah; Clampitt, Joseph; Honscheid, K.; Jain, Bhuvnesh; Jouvel, S.; Krause, E.; Lin, Huan; MacCrann, N.; Patton, K.; Plazas, A. A.; Rowe, Barnaby; Vikram, V.; Wilcox, H.; Young, J.; Zuntz, Joe; Abbott, T. M. C.; Abdalla, F. B.; Allam, S.; Banerji, M.; Bernstein, Joseph P.; Bernstein, R. A.; Bertin, E.; Buckley-Geer, E.; Burke, D. L.; Castander, F. J.; Costa, L. N. da; Cunha, C. E.; DePoy, D. L.; Desai, S.; Diehl, H. T.; Doel, P.; Estrada, J.; Evrard, A. E.; Neto, A. Fausti; Fernández, E.; Finley, D. A.; Flaugher, B.; Frieman, Joshua A.; Gaztañaga, E.; Gerdes, D. W.; Gruendl, R. A.; Gutiérrez, G.; Jarvis, M.; Karliner, I.; Kent, Stephen M.; Kuêhn, K.; Kuropatkin, N.; Lahav, O.; Maia, M. A. G.; Makler, M.; Marriner, J.; Marshall, J. L.; Merritt, K. W.; Miller, Christopher J.; Miquel, R.; Mohr, J. J.; Neilsen, Eric H.; Nichol, R. C.; Nord, B.; Reil, K.; Roe, Natalie A.; Roodman, A.; Šako, M.; Sánchez, E.; Santiago, B.; Schindler, R. H.; Schubnell, M.; Sevilla-Noarbe, I.; Sheldon, E.; Smith, Chris; Soares-Santos, M.; Swanson, M. E. C.; Sypniewski, Adam; Tarlè, G.; Thaler, J. J.; Thomas, Daniel; Tucker, D. L.; Walker, A. R.; Wechsler, Risa H.; Weller, J.; Wester, W. C.

doi:10.1093/mnras/stv398

Cited by 67 publications

(76 citation statements)

References 80 publications

(98 reference statements)

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“…They also identified a second galaxy cluster in the field of view at redshift ∼0.6, with an estimated mass of M 200m = 4.0 +3.7 −2.6 × 10 14 M . Melchior et al (2015) studied the weak lensing masses and galaxy distributions of four massive clusters observed during the DES SV period, including RXJ2248. They found M 200c = 17.5 +4.3 −3.7 × 10 14 M , which is in agreement with previous mass estimates.…”

Section: T H E C L U S T E R R X C J 2 2 4 8 7 −4 4mentioning

confidence: 99%

“…We study the galaxy completeness c g , defined as the ratio of the number of true 2 A comparison of weak lensing measurements between DES and CLASH was not performed because they predominantly reveal differences in the shear calibration. The majority of galaxies with shape measurement in both catalogues are very faint for DES, resulting in large and noisy calibration factors (see section 4.2.1 in Melchior et al 2015). In addition, the high density of galaxies in the central region of this cluster creates many more close galaxy pairs or even blends in ground-based DES images than when viewed with HST, rendering shape measurement even more challenging.…”

Section: Star/galaxy Separationmentioning

confidence: 99%

“…In this section we study the stellar mass radial profile of the cluster and relate it to that of dark matter that has been obtained though DES weak lensing studies in Melchior et al (2015). As shown in Section 4.3, stellar mass estimation can be biased if the redshift assumed is biased too: this is a problem if one wants to compute stellar masses with photometric surveys data.…”

Section: Da R K M At T E R a N D S T E L L A R M A S S E Smentioning

confidence: 99%

“…For the blue Figure 8. Cumulative radial distributions of total stellar mass derived in this paper for the DES red (red points), blue (blue points) and all galaxies (purple points) in the cluster, together with the total, non-parametric mass profile reconstructed from DES weak lensing (Melchior et al 2015, green points). The purple solid line is our NFW fit to the DES stellar mass profile, while the blue solid line is the NFW best fit from DES weak lensing.…”

Section: Masking and Background Correctionmentioning

confidence: 99%

“…The comparison of DES and CLASH, in terms of photometric redshifts and star/galaxy separation, is presented in Section 4. Section 5 contains the second part of this paper, where we present the stellar mass results obtained from CLASH and DES, and compare the DES stellar masses to the total mass from the DES weak lensing analysis by Melchior et al (2015). In the following, we assume a concordance cold dark matter ( CDM) cosmological model with m = 0.3, = 0.7 and h = 0.7.…”

Section: Introductionmentioning

confidence: 99%

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Comparing Dark Energy Survey andHST–CLASH observations of the galaxy cluster RXC J2248.7−4431: implications for stellar mass versus dark matter

Palmese

Lahav

Banerji

et al. 2016

Mon. Not. R. Astron. Soc.

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We derive the stellar mass fraction in the galaxy cluster RXC J2248.7−4431 observed with the Dark Energy Survey (DES) during the Science Verification period. We compare the stellar mass results from DES (five filters) with those from the Hubble Space Telescope Cluster Lensing And Supernova Survey (CLASH; 17 filters). When the cluster spectroscopic redshift is assumed, we show that stellar masses from DES can be estimated within 25 per cent of CLASH values. We compute the stellar mass contribution coming from red and blue galaxies, and study the relation between stellar mass and the underlying dark matter using weak lensing studies with DES and CLASH. An analysis of the radial profiles of the DES total and stellar mass yields a stellar-to-total fraction of f = (6.8 ± 1.7) × 10 −3 within a radius of r 200c 2 Mpc. Our analysis also includes a comparison of photometric redshifts and star/galaxy separation efficiency for both data sets. We conclude that space-based small field imaging can be used to calibrate the galaxy properties in DES for the much wider field of view. The technique developed to derive the stellar mass fraction in galaxy clusters can be applied to the ∼100 000 clusters that will be observed within this survey and yield important information about galaxy evolution.

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Section: T H E C L U S T E R R X C J 2 2 4 8 7 −4 4mentioning

confidence: 99%

Section: Star/galaxy Separationmentioning

confidence: 99%

Section: Da R K M At T E R a N D S T E L L A R M A S S E Smentioning

confidence: 99%

Section: Masking and Background Correctionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Comparing Dark Energy Survey andHST–CLASH observations of the galaxy cluster RXC J2248.7−4431: implications for stellar mass versus dark matter

Palmese

Lahav

Banerji

et al. 2016

Mon. Not. R. Astron. Soc.

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Detection of a possible superluminous supernova in the Epoch of Reionization

Mould¹,

Abbott²,

Cooke³

et al. 2017

Science Bulletin

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Short communicationThe Epoch of Reionization (EoR) poses a number of puzzles, including the sufficiency of ionizing radiation, the rapid production of supermassive black holes and the early appearance of abundant metals in larger galaxies. For the first of these, solutions focus on the main sequence evolution of massive stars, but the second and third puzzles involve the terminal phase of stellar evolution, and in particular, core collapse supernovae.Candidates for the ionizing galaxies are seen in deep surveys with the Hubble Space Telescope and wide surveys with large telescopes, such as Subaru. Their supernovae would also be expected to be visible, especially superluminous supernovae (SLSN), such as those seen 1,2 at lower redshifts. Here we present a candidate for the first EoR SLSN, discovered in our deep field survey with the Dark Energy Camera at the Blanco telescope of the Cerro Tololo Interamerican Observatory. The DECamERON survey 3 has accumulated deep near infrared images (0.7-1.05 microns) in three circumpolar fields over the lifetime of the camera, which together provide a solid reference for finding transient objects.One of these fields 4 , New Southern Field-1 (NSF-1) was observed on four nights in 1'' seeing in August 2016. Pipeline processing by NOAO caused individual 5 minute exposures to stacked. After downloading the resultant images from NOAO, we carried out further stacking. The SUDSS program 4 contributed to the reference images. Stellar photometry with a 0.8'' aperture was carried out on the images with DAOPHOT , and cuts were applied to single out objects that had (1) brightened by a magnitude from the reference images and that (2) had a flux deficit of at least a magnitude in the i filter relative to the z filter in the reference image. The second cut is motivated by the dropout concept that a host galaxy with redshift 6 presents its Lyman break to the i filter. Figure 1 shows our top candidate and Figure 2 its spectral energy distribution (sed), using standard calibrations https://cdcvs.fnal.gov/redmine/projects/des-sci-verification/wiki/Photometry.

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CLASH-VLT: A highly precise strong lensing model of the galaxy cluster RXC J2248.7−4431 (Abell S1063) and prospects for cosmography

Caminha

Grillo

Rosati

et al. 2016

A&A

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120

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Aims. We perform a comprehensive study of the total mass distribution of the galaxy cluster RXC J2248.7−4431 (z = 0.348) with a set of highprecision strong lensing models, which take advantage of extensive spectroscopic information on many multiply lensed systems. In the effort to understand and quantify inherent systematics in parametric strong lensing modelling, we explore a collection of 22 models in which we use different samples of multiple image families, different parametrizations of the mass distribution and cosmological parameters. Methods. As input information for the strong lensing models, we use the Cluster Lensing And Supernova survey with Hubble (CLASH) imaging data and spectroscopic follow-up observations, with the VIsible Multi-Object Spectrograph (VIMOS) and Multi Unit Spectroscopic Explorer (MUSE) on the Very Large Telescope (VLT), to identify and characterize bona fide multiple image families and measure their redshifts down to m F814W 26. A total of 16 background sources, over the redshift range 1.0−6.1, are multiply lensed into 47 images, 24 of which are spectroscopically confirmed and belong to ten individual sources. These also include a multiply lensed Lyman-α blob at z = 3.118. The cluster total mass distribution and underlying cosmology in the models are optimized by matching the observed positions of the multiple images on the lens plane. Bayesian Markov chain Monte Carlo techniques are used to quantify errors and covariances of the best-fit parameters. Results. We show that with a careful selection of a large sample of spectroscopically confirmed multiple images, the best-fit model can reproduce their observed positions with a rms scatter of 0. 3 in a fixed flat ΛCDM cosmology, whereas the lack of spectroscopic information or the use of inaccurate photometric redshifts can lead to biases in the values of the model parameters. We find that the best-fit parametrization for the cluster total mass distribution is composed of an elliptical pseudo-isothermal mass distribution with a significant core for the overall cluster halo and truncated pseudo-isothermal mass profiles for the cluster galaxies. We show that by adding bona fide photometric-selected multiple images to the sample of spectroscopic families, one can slightly improve constraints on the model parameters. In particular, we find that the degeneracy between the lens total mass distribution and the underlying geometry of the Universe, which is probed via angular diameter distance ratios between the lens and sources and the observer and sources, can be partially removed. Allowing cosmological parameters to vary together with the cluster parameters, we find (at 68% confidence level) Ω m = 0.25 for a Universe with w = −1 and free curvature. Finally, using toy models mimicking the overall configuration of multiple images and cluster total mass distribution, we estimate the impact of the line-of-sight mass structure on the positional rms to be 0. 3 ± 0. 1. We argue that the apparent sensitivity of our lensing model to cosmograp...

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Mass and galaxy distributions of four massive galaxy clusters from Dark Energy Survey Science Verification data

Cited by 67 publications

References 80 publications

Comparing Dark Energy Survey andHST–CLASH observations of the galaxy cluster RXC J2248.7−4431: implications for stellar mass versus dark matter

Comparing Dark Energy Survey andHST–CLASH observations of the galaxy cluster RXC J2248.7−4431: implications for stellar mass versus dark matter

Detection of a possible superluminous supernova in the Epoch of Reionization

CLASH-VLT: A highly precise strong lensing model of the galaxy cluster RXC J2248.7−4431 (Abell S1063) and prospects for cosmography

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