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          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents



ID: 661024.0, MPI für Astronomie / Publikationen_mpia
CLASH: Precise new constraints on the mass profile of the galaxy cluster A2261
Authors:Coe, D.; Umetsu, K.; Zitrin, A.; Donahue, M.; Medezinski, E.; Postman, M.; Carrasco, M.; Anguita, T.; Geller, M. J.; Rines, K. J.; Diaferio, A.; Kurtz, M. J.; Bradley, L.; Koekemoer, A.; Zheng, W.; Nonino, M.; Molino, A.; Mahdavi, A.; Lemze, D.; Infante, L.; Ogaz, S.; Melchior, P.; Host, O.; Ford, H.; Grillo, C.; Rosati, P.; Jiménez-Teja, Y.; Moustakas, J.; Broadhurst, T.; Ascaso, B.; Lahav, O.; Bartelmann, M.; Benítez, N.; Bouwens, R.; Graur, O.; Graves, G.; Jha, S.; Jouvel, S.; Kelson, D.; Moustakas, L.; Maoz, D.; Meneghetti, M.; Merten, J.; Riess, A.; Rodney, S.; Seitz, S.
Date of Publication (YYYY-MM-DD):2012
Journal Abbrev.:The Astrophysical Journal
Volume:757
Start Page:id. 22
Audience:Not Specified
Abstract / Description:We precisely constrain the inner mass profile of A2261 (z = 0.225) for the first time and determine that this cluster is not "overconcentrated" as found previously, implying a formation time in agreement with ΛCDM expectations. These results are based on multiple strong-lensing analyses of new 16-band Hubble Space Telescope imaging obtained as part of the Cluster Lensing and Supernova survey with Hubble. Combining this with revised weak-lensing analyses of Subaru wide-field imaging with five-band Subaru + KPNO photometry, we place tight new constraints on the halo virial mass M vir = (2.2 ± 0.2) × 1015 M &sun; h -1 70 (within r vir ≈ 3 Mpc h -1 70) and concentration c vir = 6.2 ± 0.3 when assuming a spherical halo. This agrees broadly with average c(M, z) predictions from recent ΛCDM simulations, which span 5 <~ langcrang <~ 8. Our most significant systematic uncertainty is halo elongation along the line of sight (LOS). To estimate this, we also derive a mass profile based on archival Chandra X-ray observations and find it to be ~35% lower than our lensing-derived profile at r 2500 ~ 600 kpc. Agreement can be achieved by a halo elongated with a ~2:1 axis ratio along our LOS. For this elongated halo model, we find M vir = (1.7 ± 0.2) × 1015 M &sun; h -1 70 and c vir = 4.6 ± 0.2, placing rough lower limits on these values. The need for halo elongation can be partially obviated by non-thermal pressure support and, perhaps entirely, by systematic errors in the X-ray mass measurements. We estimate the effect of background structures based on MMT/Hectospec spectroscopic redshifts and find that these tend to lower M vir further by ~7% and increase c vir by ~5%.
Free Keywords:dark energy; dark matter; galaxies: clusters: individual: Abell 2261; galaxies: evolution; gravitational lensing: strong; gravitational lensing: weak
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astronomie
Identifiers:URL:http://cdsads.u-strasbg.fr/abs/2012ApJ...757...22C
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