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The Mass - Concentration Relation from Galaxy Kinematics

The Mass - Concentration Relation from Galaxy Kinematics. Doron Lemze (Johns Hopkins University).

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The Mass - Concentration Relation from Galaxy Kinematics

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  1. The Mass - Concentration Relation from Galaxy Kinematics DoronLemze (Johns Hopkins University) A. Biviano, E. Medezinski, P. Rosati, I. Balestra, S. Jouvel, M. Nonino, A. Molino, A. Mercurio, K. Umetsu, M. Postman, H. Ford, D. Kelson, P. Melchior, M. Meneghetti, and the CLASH team CLASH meeting 2013 - London

  2. Motivation A primary science goal of CLASH is to measure the mass profiles in galaxy clusters. Why use galaxy kinematics? There is a drawback in this technique, and it is the assumption of dynamical equilibrium. However, it has also strong advantages. Unlike lensing, galaxy kinematics are not contaminated by line-of-sight structures unrelated to the cluster, and unlike X-ray observation, kinematics can reach beyond the virial radius. Another advantage of this technique vs. lensing is that galaxy kinematics can be applied at lower redshifts where lensing is less sensitive and estimations for single clusters are very challenging. Measuring the profile shapes using different techniques enables a better understanding of the systematics and offers an observational test of the different techniques. CLASH meeting 2013 - London

  3. The uniqueness of our spectroscopic sample We will have the largest relaxed (X-ray selected) cluster sample with cluster members >~ 300 per cluster at 0.2<~ z <~0.6. Not by chance, this redshift range is the ideal one for lensing. We’ll have accurate lensing estimations to compare with the ones derived by galaxy kinematics. This will give us an opportunity to estimate the real uncertainties of this technique. CLASH meeting 2013 - London

  4. Jeans Analysis Jeans eq. Velocity anisotropy Galaxy surface number density Projected velocity dispersion CLASH meeting 2013 - London

  5. Estimating and for the Jeans analysis Diaferio & Geller 1997 Diaferio 1999

  6. Estimating and for the Jeans analysis – no VLT data Diaferio & Geller 1997 Diaferio 1999

  7. Cleaning Subaru galaxies with available photometric redshifts CLASH meeting 2013 - London

  8. Galaxy surface number density CLASH meeting 2013 - London

  9. Galaxy surface number density CLASH meeting 2013 - London

  10. Fitting the data – A611 as an example Data Fit Data Fit

  11. C – M relation using galaxy kinematics vs. the theoretical expectation MACSJ1206 A383 A209 MACSJ1115 MS2137 A2261 A611 RXJ2129 Observed Expected (Duffy et al. 2008)

  12. Summary and future work Summary: We estimated the C-M relation using galaxy kinematics for 8 clusters. Future work: Adding kurtosis (the forth-order velocity moment ) information? More clusters - for how many more in the next few months see Piero’s talk. Different dependencies on the substructure level. Comparing to estimations from lensing and other techniques. CLASH meeting 2013 - London

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