2002/02/28 by Tommaso Treu, L. V. E. Koopmans, Leon Koopmans · 9 citations
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysics #Dark matter #Dark matter halo #Einstein radius #Einstein ring #Galaxies: Formation, Evolution, Phenomena #Galaxy #Gravitational lens #Halo #Mass distribution #Physics #Redshift #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.1086/341216
8 pages, 4 figures, ApJ, in press, minor changes
arxiv created 2002/04/10 · openalex publication_date 2002/08/10 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/06
We combine our recent measurements of the velocity dispersion and the surface brightness profile of the lens galaxy D in the system MG 2016+112 ( z = 1.004) with constraints from gravitational lensing to study its internal mass distribution. We find the following: (1) dark matter accounts for more than 50% of the total mass within the Einstein radius (99% confidence limit [CL]), whereas ~75% is the more likely contribution. In particular, we can exclude at the 8 σ level that mass follows light inside the Einstein radius with a constant mass-to-light ratio ( M / L ). (2) The total mass distribution inside the Einstein radius is well described by a density profile ∝ r , with an effective slope γ' = 2.0 ± 0.1 ± 0.1, including random and systematic uncertainties. (3) The offset of galaxy D from the local fundamental plane independently constrains the stellar M / L and matches the range derived from our models, leading to a more stringent lower limit of more than 60% on the fraction of dark matter within the Einstein radius (99% CL). Under the assumption of adiabatic contraction, we show that the inner slope of the dark matter halo before the baryons collapsed to form the lens galaxy is γ i < 1.4 (68% CL), only marginally consistent with the highest resolution cold dark matter simulations that indicate γ i ~ 1.5. This might indicate either that adiabatic contraction is a poor description of early-type galaxy formation or that additional processes play a role as well. Indeed, the apparently isothermal density distribution inside the Einstein radius is not a natural outcome of adiabatic contraction models, where it appears to be a mere coincidence. By contrast, we argue that isothermality might be the result of a stronger coupling between luminous and dark matter, possibly the result of (incomplete) violent relaxation processes during the formation of the innermost regions of the galaxy. Hence, we conclude that galaxy D appears already relaxed ~8 Gyr ago. We briefly discuss the importance of our results for lens statistics and the determination of the Hubble constant from gravitational lens time delays.