### Abstract

The combined resolution and sensitivity of the Advanced Camera for Surveys deep imaging provides the capability of high-accuracy lens modeling of Abell 1689. Originally based on the technique of Broadhurst and coworkers, our software is designed to provide a precise and efficient method of modeling cluster lenses without assumptions relating the large-scale cluster dark matter to the light. Abell 1689 is robustly modeled using a freely varying cluster halo component consisting of an NFW profile, shapelets (Refregier), and a mass sheet, as well as a galaxy component based on the light. Another improvement over previous modeling techniques is the application of magnification-corrected image magnitude constraints. The mass within the ∼50″ Einstein radius was found to be 2.04_{-0.11}^{+0.03} × 10^{14}M _{⊙}-and was reliably fitted by an NFW with c = r _{200}/r_{s} = 5.70_{-0.50}^{+0.34} and r _{s} = 239_{-24}^{-28}(727_{-73} ^{+85}kpc), which gives d ln ρ/d ln r = -1.34 at r = 150 kpc. The overall B-band mass-to-light ratio within the Einstein radius is 215 _{-2}^{+13} M_{⊙} L_{⊙}g^{-1} versus only 32_{-1}^{-3} M_{⊙} L _{⊙}^{-1} for the galaxy component. For the overall surface mass density distribution, there are two regimes where the slope, d log Σ/d log R, is nearly constant. The intermediate slope from 6 to 30 kpc is -0.41_{-0.05}^{+0.01}, while the outer slope from 80 to 120 kpc is -0.57_{-0.12}^{+0.02} In addition, our final model is consistent with the results from Broadhurst and coworkers. Monte Carlo simulations are also performed to explore the modeling systematics related to the image positional errors, the dependence on multiple image systems, and the WMAP predictions.

Original language | English |
---|---|

Pages (from-to) | 639-661 |

Number of pages | 23 |

Journal | Astrophysical Journal |

Volume | 640 |

Issue number | 2 I |

DOIs | |

Publication status | Published - 2006 Apr 1 |

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### All Science Journal Classification (ASJC) codes

- Astronomy and Astrophysics
- Space and Planetary Science

### Cite this

*Astrophysical Journal*,

*640*(2 I), 639-661. https://doi.org/10.1086/500285

}

*Astrophysical Journal*, vol. 640, no. 2 I, pp. 639-661. https://doi.org/10.1086/500285

**Mass modeling of abell 1689 advanced camera for surveys observations with a perturbed navarro-frenk-white model.** / Zekser, K. C.; White, R. L.; Broadhurst, T. J.; Benítez, N.; Ford, H. C.; Illingworth, G. D.; Blakeslee, J. P.; Postman, M.; Jee, Myung Kook; Coe, D. A.

Research output: Contribution to journal › Article

TY - JOUR

T1 - Mass modeling of abell 1689 advanced camera for surveys observations with a perturbed navarro-frenk-white model

AU - Zekser, K. C.

AU - White, R. L.

AU - Broadhurst, T. J.

AU - Benítez, N.

AU - Ford, H. C.

AU - Illingworth, G. D.

AU - Blakeslee, J. P.

AU - Postman, M.

AU - Jee, Myung Kook

AU - Coe, D. A.

PY - 2006/4/1

Y1 - 2006/4/1

N2 - The combined resolution and sensitivity of the Advanced Camera for Surveys deep imaging provides the capability of high-accuracy lens modeling of Abell 1689. Originally based on the technique of Broadhurst and coworkers, our software is designed to provide a precise and efficient method of modeling cluster lenses without assumptions relating the large-scale cluster dark matter to the light. Abell 1689 is robustly modeled using a freely varying cluster halo component consisting of an NFW profile, shapelets (Refregier), and a mass sheet, as well as a galaxy component based on the light. Another improvement over previous modeling techniques is the application of magnification-corrected image magnitude constraints. The mass within the ∼50″ Einstein radius was found to be 2.04-0.11+0.03 × 1014M ⊙-and was reliably fitted by an NFW with c = r 200/rs = 5.70-0.50+0.34 and r s = 239-24-28(727-73 +85kpc), which gives d ln ρ/d ln r = -1.34 at r = 150 kpc. The overall B-band mass-to-light ratio within the Einstein radius is 215 -2+13 M⊙ L⊙g-1 versus only 32-1-3 M⊙ L ⊙-1 for the galaxy component. For the overall surface mass density distribution, there are two regimes where the slope, d log Σ/d log R, is nearly constant. The intermediate slope from 6 to 30 kpc is -0.41-0.05+0.01, while the outer slope from 80 to 120 kpc is -0.57-0.12+0.02 In addition, our final model is consistent with the results from Broadhurst and coworkers. Monte Carlo simulations are also performed to explore the modeling systematics related to the image positional errors, the dependence on multiple image systems, and the WMAP predictions.

AB - The combined resolution and sensitivity of the Advanced Camera for Surveys deep imaging provides the capability of high-accuracy lens modeling of Abell 1689. Originally based on the technique of Broadhurst and coworkers, our software is designed to provide a precise and efficient method of modeling cluster lenses without assumptions relating the large-scale cluster dark matter to the light. Abell 1689 is robustly modeled using a freely varying cluster halo component consisting of an NFW profile, shapelets (Refregier), and a mass sheet, as well as a galaxy component based on the light. Another improvement over previous modeling techniques is the application of magnification-corrected image magnitude constraints. The mass within the ∼50″ Einstein radius was found to be 2.04-0.11+0.03 × 1014M ⊙-and was reliably fitted by an NFW with c = r 200/rs = 5.70-0.50+0.34 and r s = 239-24-28(727-73 +85kpc), which gives d ln ρ/d ln r = -1.34 at r = 150 kpc. The overall B-band mass-to-light ratio within the Einstein radius is 215 -2+13 M⊙ L⊙g-1 versus only 32-1-3 M⊙ L ⊙-1 for the galaxy component. For the overall surface mass density distribution, there are two regimes where the slope, d log Σ/d log R, is nearly constant. The intermediate slope from 6 to 30 kpc is -0.41-0.05+0.01, while the outer slope from 80 to 120 kpc is -0.57-0.12+0.02 In addition, our final model is consistent with the results from Broadhurst and coworkers. Monte Carlo simulations are also performed to explore the modeling systematics related to the image positional errors, the dependence on multiple image systems, and the WMAP predictions.

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U2 - 10.1086/500285

DO - 10.1086/500285

M3 - Article

AN - SCOPUS:33645802800

VL - 640

SP - 639

EP - 661

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

IS - 2 I

ER -