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Query : 2002A&A...386...12D |

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2002A&A...386...12D -
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Astronomy and Astrophysics, volume 386, 12-30 (2002/4-4)
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Lens magnification by CL 0024+1654 in the U and R band.
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DYE S., TAYLOR A.N., GREVE T.R., ROEGNVALDSSON O.E., VAN KAMPEN E., JAKOBSSON P., SIGMUNDSSON V.S., GUDMUNDSSON E.H. and HJORTH J.
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Abstract (from CDS):
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We estimate the total mass distribution of the galaxy cluster CL 0024+1654 from the measured source depletion due to lens magnification in the R band. Within a radius of 0.54h^{–1}.Mpc, a total projected mass of (8.1±3.2)x10^{14}h^{–1}.M_{☉} (EdS) is measured. The 1σ error here includes shot noise, source clustering, uncertainty in background count normalisation and contamination from cluster and foreground galaxies. This corresponds to a mass-to-light ratio of M/L_{B}=470±180. We compute the luminosity function of CL 0024+1654 in order to estimate contamination of the background source counts from cluster galaxies. Three different magnification-based reconstruction methods are employed: 1) an estimator method using a local calculation of lens shear; 2) a non-local, self-consistent method applicable to axi-symmetric mass distributions; 3) a non-local, self-consistent method for derivation of 2D mass maps. We have modified the standard single power-law slope number count theory to incorporate a break and applied this to our observations. Fitting analytical magnification profiles of different cluster models to the observed number counts, we find that CL 0024+1654 is best described either by a NFW model with scale radius r_{s}=334±191h^{–1}kpc and normalisation κ_{s}=0.23±0.08 or a power-law profile with slope ξ=0.61±0.11, central surface mass density κ_{0}=1.52±0.20 and assuming a core radius of r_{core}=35h^{–1}kpc. The NFW model predicts that the cumulative projected mass contained within a radius R scales as M(<R)=2.9x10^{14}(R/1')^1.3-0.5lg (R/1')^{h}-1^M_{☉}. Finally, we have exploited the fact that flux magnification effectively enables us to probe deeper than the physical limiting magnitude of our observations in searching for a change of slope in the U band number counts. We rule out both a total flattening of the counts with a break up to U_{AB}≤26.6 and a change of slope, reported by some studies, from d logN/dm=0.4->0.15 up to U_{AB}≤26.4 with 95% confidence.

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Abstract Copyright:
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Journal keyword(s):
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gravitational lensing - galaxies: clusters: individual: CL 0024+1654 - cosmology: dark matter
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Simbad objects:
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3

Number of rows : 3 |

N | Identifier | Otype |
ICRS (J2000) RA |
ICRS (J2000) DEC |
Mag U | Mag B | Mag V | Mag R | Mag I | Sp type |
#ref
1850 - 2023 |
#notes |
---|---|---|---|---|---|---|---|---|---|---|---|---|

1 | ZwCl 0024+1652 | ClG | 00 26 36.0 | +17 08 36 | 18.35 | ~ | 630 | 1 | ||||

2 | NAME Hubble Deep Field | reg | 12 36 49.5 | +62 12 58 | ~ | 1901 | 1 | |||||

3 | NAME HDF-S | reg | 22 32 56 | -60 33.0 | ~ | 565 | 0 |

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2023.06.04-09:41:38

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