Rules, Standards, and the Internal Point of View

Large scale structure and cosmolog

CODEX weak lensing mass catalogue and implications on the mass-richness relation

The COnstrain Dark Energy with X-ray clusters (CODEX) sample contains the largest flux limited sample of X-ray clusters at 0.35 = alpha mu + beta, with mu = ln (M-200c/M-piv), and M-piv = 10(14.81)M(circle dot). We find a slope alpha = 0.49(-0.15)(+0.20) , normalization exp(beta) = 84.0(-14.8)(+9.2) , and sigma(ln lambda vertical bar mu) = 0.17(-0.09)(+0.13) using CFHT richness estimates. In comparison to other weak lensing richness-mass relations, we find the normalization of the richness statistically agreeing with the normalization of other scaling relations from a broad redshift range (0.0 <z <0.65) and with different cluster selection (X-ray, Sunyaev-Zeldovich, and optical).Peer reviewe

CODEX weak lensing: concentration of galaxy clusters at z ∼ 0.5

We present a stacked weak-lensing analysis of 27 richness selected galaxy clusters at 0.40 <= z <= 0.62 in the COnstrain Dark Energy with X-ray galaxy clusters (CODEX) survey. The fields were observed in five bands with the Canada-France-Hawaii Telescope (CFHT). We measure the stacked surface mass density profile with a 14 sigma significance in the radial range 0.1 < R Mpc h(-1) < 2.5. The profile is well described by the halo model, with the main halo term following a Navarro-Frenk-White profile (NFW) profile and including the off-centring effect. We select the background sample using a conservative colour-magnitude method to reduce the potential systematic errors and contamination by cluster member galaxies. We perform a Bayesian analysis for the stacked profile and constrain the best-fitting NFW parameters M-200c = 6.6(- 0.8)(+1.0) x 10(14) h(-1)M(circle dot) and c(200c) = 3.7(+0.7) (-0.6). The off-centring effect was modelled based on previous observational results found for redMaPPer Sloan Digital Sky Survey clusters. Our constraints on M(200)c and c(200)c allow us to investigate the consistency with numerical predictions and select a concentration-mass relation to describe the high richness CODEX sample. Comparing our best-fitting values forM(200c) and c(200c) with other observational surveys at different redshifts, we find no evidence for evolution in the concentration-mass relation, though it could be mitigated by particular selection functions. Similar to previous studies investigating the X-ray luminosity-mass relation, our data suggest a lower evolution than expected from self-similarity.Brazilian agencies CNPQ; CAPES [2684/2015-2 PDSE, PPVE 23038.008197/2012-45]; Max-Planck-Institute for Extraterrestrial Physics; DFG cluster of excellence `Origin and Structure of the Universe'; FAPESP [2014/137233]; NASA through the Einstein Fellowship program [PF 5-160138]; STFC [ST/N000919/1]; CNPq [312307/2015-2]; [266918]This item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at [email protected]

The SOAR Gravitational ARC Survey

We present the first results of the SOAR Gravitational\ud Arc Survey (SOGRAS). The survey imaged 47\ud clusters in two redshift intervals centered at z = 0.27\ud and z = 0.55, targeting the richest clusters in each\ud interval. Images were obtained in the g′, r′ and i′\ud bands with a median seeing of 0.83, 0.76 and 0.71\ud arcsec, respectively, in these filters. Most of the survey\ud clusters are located within the Sloan Digital Sky\ud Survey (SDSS) Stripe-82 region and all of them are\ud in the SDSS footprint. We present the first results\ud of the survey, including the 6 best strong lensing\ud systems, photometric and morphometric catalogs of\ud the galaxy sample, and cross matches of the clusters\ud and galaxies with complementary samples (spectroscopic\ud redshifts, photometry in several bands, X-ray\ud and Sunyaev Zel’dovich clusters, etc.), exploiting the\ud synergy with other surveys in Stripe-82. We apply\ud several methods to characterize the gravitational arc\ud candidates, including the Mediatrix method (Bom\ud et al. 2012) and ArcFitting (Furlanetto et al. 2012),\ud and for the subtraction of galaxy cluster light. Finally,\ud we apply strong lensing inversion techniques to\ud the best systems, providing constraints on their mass\ud distribution. The analyses of a spectral follow-up with Gemini and the derived dynamical masses are\ud presented in a poster submitted to this same meeting\ud (Cibirka et al.).\ud Deeper follow-up images with Gemini strengthen\ud the case for the strong lensing nature of the candidates\ud found in this survey.Resumo publicado no periódico: Revista Mexicana de Astronomía y Astrofísica. Serie de Conferencias, v. 44, p. 180-181, 2014

RELICS:Strong Lensing Analysis of MACS J0417.5-1154 and Predictions for Observing the Magnified High-Redshift Universe with JWST

Large scale structure and cosmolog

RELICS: Reionization Lensing Cluster Survey

Large surveys of galaxy clusters with the Hubble Space Telescope (HST) and Spitzer, including the Cluster Lensing And Supernova survey with Hubble and the Frontier Fields, have demonstrated the power of strong gravitational lensing to efficiently deliver large samples of high-redshift galaxies. We extend this strategy through a wider, shallower survey named RELICS, the Reionization Lensing Cluster Survey, described here. Our 188-orbit Hubble Treasury Program observed 41 clusters at 0.182 ≤ z ≤ 0.972 with Advanced Camera for Surveys (ACS) and WFC3/IR imaging spanning 0.4-1.7 μm. We selected 21 of the most massive clusters known based on Planck PSZ2 estimates and 20 additional clusters based on observed or inferred lensing strength. RELICS observed 46 WFC3/IR pointings (∼200 arcmin) each with two orbits divided among four filters (F105W, F125W, F140W, and F160W) and ACS imaging as needed to achieve single-orbit depth in each of three filters (F435W, F606W, and F814W). As previously reported by Salmon et al., we discovered over 300 z ∼ 6-10 candidates, including the brightest z ∼ 6 candidates known, and the most distant spatially resolved lensed arc known at z ∼ 10. Spitzer IRAC imaging (945 hr awarded, plus 100 archival, spanning 3.0-5.0 μm) has crucially enabled us to distinguish z ∼ 10 candidates from z ∼ 2 interlopers. For each cluster, two HST observing epochs were staggered by about a month, enabling us to discover 11 supernovae, including 3 lensed supernovae, which we followed up with 20 orbits from our program. Reduced HST images, catalogs, and lens models are available on MAST, and reduced Spitzer images are available on IRSA.© 2019. The American Astronomical Society. All rights reserved.We thank Lindsey Bleem for providing Magellan Megacam LDSS3 images of SPT0254-58 and AS295 prior to RELICS to inform our HST observations of these clusters. We thank Florian Pacaud and Matthias Klein for discussions regarding our AS295 HST pointings. We thank Dale Kocevski for an image of RXC 0142+44 obtained with the University of Hawaii 2.2 m telescope. And we thank Stella Seitz et al. for sharing their HST observations of PLCK G287+32 obtained during the same cycle. We thank the STScI and SSC directors and time allocation committees for enabling these large observing programs. We are grateful to our HST program coordinator William Januszewski for implementing the RELICS HST observations. We thank Jennifer Mack for expert mentoring of our HST image reduction gurus RA and SO. And we thank Gabriel Brammer for providing an updated WFC3/IR hot pixel mask derived from science observations from GO 14114. The RELICS Hubble Treasury Program (GO 14096) consists of observations obtained by the NASA/ESA Hubble Space Telescope (HST). HST is operated by the Association of Universities for Research in Astronomy, Inc. (AURA), under NASA contract NAS5-26555. Data from the NASA/ESA HST presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST), operated by the Space Telescope Science Institute (STScI). STScI is operated by the Association of Universities for Research in Astronomy, Inc..(AURA), under NASA contract NAS 5-26555. The HST Advanced Camera for Surveys (ACS) was developed under NASA contract NAS 5-32864. Spitzer Space Telescope data presented in this paper were obtained from the NASA/IPAC Infrared Science Archive (IRSA), operated by the Jet Propulsion Laboratory, California Institute of Technology. Spitzer and IRSA are operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. We gratefully acknowledge support from JPL for the Spitzer analysis. M.B. and V.S. also acknowledge support by NASA through ADAP grant 80NSSC18K0945, NASA/HST through HST-GO-14096, HST-GO-13666, and two awards issued by Spitzer/JPL/Caltech associated with the SRELICS_DEEP and SRELICS programs. Part of this work by W.D. was performed under the auspices of the U.S..DOE by LLNL under contract DE-AC5207NA27344. K.U. acknowledges support from the Ministry of Science and Technology of Taiwan (grant MOST 106-2628M-001-003-MY3) and from Academia Sinica (grant AS-IA107-M01). O.G. is supported by an NSF Astronomy and Astrophysics Fellowship under award AST-1602595. S.A.R. was supported by NASA grant HST-GO-14208 from STScI, which is operated by Associated Universities for Research in Astronomy, Inc. (AURA), under NASA contract NAS 5-26555. A.M. acknowledges the financial support of the Brazilian funding agency FAPESP (Post-doc fellowshipprocess No. 2014/11806-9). J.H. was supported by a VILLUM FONDEN Investigator grant (project No. 16599)