Strong and Weak Lensing

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Conclusions • Strong and weak lensing are extremely powerful techniques • Combining techniques is essential to disentangle luminous and dark matter and establish radial trends • Early-type galaxies live in dark matter halos: – M*/M vir ~2±1% – Dark matter fraction within Re increases with mass – IMF is closer to Salpeter than Chabrier – Total mass profile close to isothermal with scatter • More soon on spiral galaxies from lensing • Clusters of galaxies have different mass profiles: – Total is not isothermal – Dark matter halo can be shallower than NFW
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Page 1 and 2: Strong and Weak Lensing TOMMASO TRE
Page 3 and 4: Introduction
Page 5 and 6: Strong lensing by galaxies Lensed q
Page 7 and 8: Weak lensing: What is it and what c
Page 9 and 10: Why do we need more strong lenses a
Page 12 and 13: Lensing++
Page 14 and 15: Are lensing galaxies special?
Page 16 and 17: The mass structure of early-type ga
Page 18 and 19: …and clumpy • Not covered here:
Page 20 and 21: Galaxies have approximately isother
Page 22 and 23: There are exceptions/caveats HE0435
Page 24 and 25: Enter Stellar Masses New Bayesian s
Page 26 and 27: The IMF of early-type galaxies •
Page 28 and 29: ΔΣ (h M sun/pc 2 ) How about at l
Page 30 and 31: Is there evolution? Lagattuta et al
Page 32 and 33: What about spirals? How “heavy”
Page 34 and 35: New samples: Haggles Marshall et al
Page 36 and 37: Dust is sometimes a problem… but
Page 38 and 39: Clusters are not large ellipticals

Strong and Weak Lensing

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