期刊
ASTROPHYSICAL JOURNAL
卷 757, 期 1, 页码 -出版社
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/757/1/22
关键词
dark energy; dark matter; galaxies: clusters: individual (Abell 2261); galaxies: evolution; gravitational lensing: strong; gravitational lensing: weak
资金
- NASA [NAS 5-26555, NAS 5-32864, HST-GO-12065.01-A]
- National Science Council of Taiwan [NSC100-2112-M-001-008-MY3]
- Israel Science Foundation
- German Science Foundation [Transregio TR 33]
- Spanish MICINN [YA2010-22111-C03-00]
- Junta de Andalucia Proyecto de Excelencia [NBL2003]
- INAF Contracts [ASI-INAF I/009/10/0, ASI-INAF I/023/05/0, ASI-INAF I/088/06/0, PRIN INAF 2009, PRIN INAF 2010]
- NSF [AST-0847157]
- UK's STFC
- Royal Society
- Wolfson Foundation
- Academia Sinica Career Development Award
- Internationale Spitzenforschung II-1 of the Baden-Wurttemberg Stiftung
- Smithsonian Institution
- Cottrell College Science Award from Research Corporation
- INFN [PD51]
- PRIN-MIUR [2008NR3EBK_003]
- Conicyt FONDAP/BASAL grant
- DFG
- STFC [ST/J001511/1] Funding Source: UKRI
- Science and Technology Facilities Council [ST/J001511/1] Funding Source: researchfish
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 Lambda CDM 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) x 10(15) M-circle dot h(70)(-1) (within r(vir) approximate to 3 Mpc h(70)(-1)) and concentration c(vir) = 6.2 +/- 0.3 when assuming a spherical halo. This agrees broadly with average c(M, z) predictions from recent Lambda CDM simulations, which span 5 less than or similar to < c > less than or similar to 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 similar to 35% lower than our lensing-derived profile at r(2500) similar to 600 kpc. Agreement can be achieved by a halo elongated with a similar to 2:1 axis ratio along our LOS. For this elongated halo model, we find M-vir = (1.7 +/- 0.2) x 10(15) M-circle dot h(70)(-1) 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 similar to 7% and increase c(vir) by similar to 5%.
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