School/Workshop on parallel computing in astrophysics: 19-23 April, 2010, Santiago, ChileSchool/Workshop on parallel computing in astrophysics: 19-23 April, 2010, Santiago, Chile

Closing remarks

Data: large databases -> mininglarge sets of raw data -> HPC

Simulations: -> HPC-> miningTheoretical model

to understand what´sgoing on

dotheylookthesame?

Galaxies cannot be simulated fully: sub-grid physics

Hydro AMR Semi-analytics

Galaxy and structure formation models:

Cosmology -> DM, DE, Baryons

Evolution of DM -> non-linear, different scales, diff. DM parts. (very large, very small)

-All to some degree including the cosmological large scale effects (some more than others). Example: without this it would be very difficult to obtain a M-Z relation.

-Relative advantages between each method

-Where do the different observed components come from?

SED MC

Comparison between models and observations

On different levels:

-Statistical: systematics, effects of particular features of the evolution of galaxies and structures

-At different epochs (reionization, LBGs, LAEs, SDSS, LSST), or between histories (astroarcheology)

-At the level of individual objects (morphologies at diff. wavelengths including stripping of gas, rotation curves, bars, density profiles, number of satellites, the MW, streams, etc)

-At the level of the parameters used to model the sub-grid physics (efficiency of SF or AGN feedback for example).

Growing Tendency: treat models in the same way as observations

Catch up between models and data (larger volumes, lowermasses, different redshifts, emission lines, gas, stars, etc)

Careful analysis of systematics affecting both, models and observations.

A lot of work to be done!

VC is great but please keep traveling!

School/Workshop on parallel computing in astrophysics: 19-23 April, 2010, Santiago, ChileSchool/Workshop on parallel computing in astrophysics: 19-23 April, 2010, Santiago, Chile

Thank you for comingSpecial thanks: Carlos Oliva

The end