A HIGH-RESOLUTION MASS MAP OF GALAXY CLUSTER SUBSTRUCTURE: LensPerfect ANALYSIS OF A1689
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, MS 169-327, Pasadena, CA 91109 (United States)
- Instituto de Astrofisica de AndalucIa (CSIC), Camino Bajo de Huetor 50, Granada 18008 (Spain)
- Department of Theoretical Physics, University of Basque Country UPV/EHU, Leioa (Spain)
We present a strong lensing (SL) mass model of A1689 which resolves substructures an estimated 25 kpc across within the central {approx}400 kpc diameter. We achieve this resolution by perfectly reproducing the observed (strongly lensed) input positions of 168 multiple images of 55 knots residing within 135 images of 42 galaxies. Our model makes no assumptions about light tracing mass, yet we reproduce the brightest visible structures with some slight deviations. A1689 remains one of the strongest known lenses on the sky, with an Einstein radius of R{sub E} = 47.''0 {+-} 1.''2 (143{sup +3}{sub -4} kpc) for a lensed source at z{sub s} = 2. We find that a single Navarro-Frenk-White (NFW) or Sersic profile yields a good fit simultaneously (with only slight tension) to both our SL mass model and published weak lensing (WL) measurements at larger radius (out to the virial radius). According to this NFW fit, A1689 has a mass of M{sub vir} = 2.0{sup +0.5}{sub -0.3} x 10{sup 15} M{sub sun} h {sup -1}{sub 70} (M{sub 200} = 1.8{sup +0.4}{sub -0.3} x 10{sup 15} M{sub sun} h {sup -1}{sub 70}) within the virial radius r{sub vir} = 3.0 {+-} 0.2 Mpc h {sup -1}{sub 70} (r{sub 200} = 2.4{sup +0.1}{sub -0.2} Mpc h {sup -1}{sub 70}), and a central concentration c{sub vir} = 11.5{sup +1.5}{sub -1.4} (c{sub 200} = 9.2 {+-} 1.2). Our SL model prefers slightly higher concentrations than previous SL models, bringing our SL + WL constraints in line with other recent derivations. Our results support those of previous studies which find A1689 has either an anomalously large concentration or significant extra mass along the line of sight (perhaps in part due to triaxiality). If clusters are generally found to have higher concentrations than realized in simulations, this could indicate that they formed earlier, perhaps as a result of early dark energy.
- OSTI ID:
- 21471228
- Journal Information:
- Astrophysical Journal, Vol. 723, Issue 2; Other Information: DOI: 10.1088/0004-637X/723/2/1678; ISSN 0004-637X
- Country of Publication:
- United States
- Language:
- English
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