SL applications I

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The dark and luminous matter density profiles of galaxies and clusters of galaxies

lecture 1

  • Why? What are we trying to learn? [15m; RT 15m]
  • Strong Lensing Constraints [10m; RT 25m]
    • Results for simple models (SIS, SIE, and NFW)
      • Show pictures of classic configurations for clusters and galaxies (double; quads; central images; 1004; CL0024; A1689)
      • Physical differences between clusters and galaxies (Rein/Rvir)
  • What about real life? [5m; RT 30m]
  • Challenges with galaxies and clusters - Departures from simple theoretical pictures
    • Presence of satellites/perturbers (e.g.)
    • Detectability: resolution, sensitivity, dust (ground vs space; SWELLS)
    • For clusters: which images are lensed? (A1689 Limousin vs Broadhurst)

BREAK #1: SHOW THEM PICTURES OF CLUSTER AND GALAXY LENSES AND ASK THEM TO INTERPRET THEM [10m; RT 40m]

  • Measuring Redshifts (spec and photo-z) [10m; RT 50]
    • Emission lines
    • Absorption lines
    • Spectral Breaks/Dropout technique
  • Degeneracies [5m; RT 55m]
    • What does lensing measure well? Total mass, slope, and orientation/elongation (Kochanek 2006)
    • Dark vs luminous matter? (rotation curves example; plot from Dutton et al. 2011)
  • Adding more constraints to break degeneracies
    • Stellar kinematics: Jeans Modelling and stellar velocity dispersion measurements [10 m; RT 65m]
    • Stellar population synthesis models: basic principles [5m; RT 70m]

BREAK #2: WRITE DOWN A QUESTION FOR ME AND LET”S DISCUSS IT [10m; RT 80m]

  • Critical Review of the Literature and Open Problems [10m; RT 90m]

Inner profiles as test of CDM? MS2137, A1703; A 383 C-M relation, high concentration clusters. What about the effects of baryons?


HW: plot kappa and shear vs radius as a function of f* for two component models using typical values for clusters and galaxies (SIS+NFW).


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