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Raul Jimenez

Raul Jimenez. The most non-linear phase of LSS. http:// icc.ub.edu /~ jimenez. Extremely successful model. State of the art of data then…. ~14 Gyr (a posteriori information). (DMR)COBE. CMB. 380000 yr (a posteriori information). Avalanche of data. And it still holds!.

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Raul Jimenez

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  1. Raul Jimenez The most non-linear phase of LSS http://icc.ub.edu/~jimenez

  2. Extremely successful model State of the art of data then… ~14 Gyr (a posteriori information) (DMR)COBE CMB 380000 yr (a posteriori information)

  3. Avalanche of data And it still holds!

  4. Credit: Ben Wandelt (IAP)

  5. Credit: Ben Wandelt (IAP)

  6. The Halo Model Linear PS 2h 1h

  7. The Halo Model And provides a formalism to also model the clustering of galaxies: just modify the density profile of the one halo term

  8. Red galaxies are in clusters and Blue galaxies in filaments Gil-Marin et al. 2011 MNRAS

  9. Yet, (present) stellar mass determines where and how the galaxy formed and evolved

  10. SF as a function of environment (Mark Correlations) Sheth, RJ, Panter, Heavens, ApJL, astro-ph/0604581

  11. Credit: Ben Wandelt (IAP)

  12. What we have learned from the most non-linear scales:

  13. Our findings from hydro-simulations are that a similar picture may apply to galaxies Prieto, RJ, Marti, 2011 MNRAS

  14. Prieto, Haiman, RJ 2012/2013 MNRAS

  15. Conclusions and Future Outlook • Smoothing is a very poor way to treat the rich cosmological datasets, i.e. the whole sky • We need to model the DM halos and galaxies • Halo model of such is not god enough to obtain % cosmological parameters • Fully non-linear turbulent flows maybe the clue to exploit scaling laws in non-linearity • We should take advantage of non-linearity

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