EGEE-II INFSO-RI Enabling Grids for E-sciencE EGEE and gLite are registered trademarks Maurizio Salaris & Santi Cassisi & Fabio Pasian ARI – Liverpool John Moores University, UK INAF – Collurania Astronomical Observatory, I INAF – Trieste Astronomical Observatory, I & GRID a B ag of S tellar T racks & I sochrones …and… much more! In collaboration with: A.Pietrinferni F. Castelli D. Cordier M. Castellani P. Manzato R. Smareglia G. Taffoni C. Vuerli S. Percival

Enabling Grids for E-sciencE EGEE-II INFSO-RI Why…, ? Stellar evolution model and isochrone archives are a fondamental working tool in modern astrophysics. Their use ranges from the study of single stellar objects, to Galactic and extragalactic stellar systems, in the near universe and at high redshift. Improvements in the physical inputs Homogeneity Coverage of the parameter space User friendly

Enabling Grids for E-sciencE EGEE-II INFSO-RI Equation of State: FreeEos by A. Irwin (2005) Radiative opacity: high-T  OPAL (Rogers et al. 2000) - low-T  Alexander & Ferguson (1994) + Ferguson et al. (2005) Conductive opacity: Potekhin (1999) Nuclear cross sections: NACRE (Angulo et al. 1999) + updates (Kunz et al. 2000, Formicola et al …) The most updated library of stellar evolution models currently available!!! Input physics

Enabling Grids for E-sciencE EGEE-II INFSO-RI The coverage 11 metallicities: from Very Metal-poor Stars to Very metal-rich ones Heavy elements mixture: scaled solar & α -enhanced Helium abundance: Y pr =  Y/  Z~1.4 Core convection: canonical & overshooting Mass loss: Reimers’ law with  =0.2 and 0.4 Extremely fine mass grid for all evolutionary stages From the Pre-Main Sequence to the end of the Asymptotic Giant Branch or C-ignition Updated Color – T eff transformations + BC scale

Enabling Grids for E-sciencE EGEE-II INFSO-RI Why, What,.... ? Evolutionary tracks Isochrones Luminosity Functions Synthetic Colour – Magnitude Diagrams Tables with relevant data

Enabling Grids for E-sciencE EGEE-II INFSO-RI Evolutionary tracks & isochrones: some examples

Enabling Grids for E-sciencE EGEE-II INFSO-RI Horizontal Branch stellar models: some examples RR Lyrae instability strip Accurate sampling of the different evolutionary phases A reliable tool for population synthesis analysis A fundamental ingredient for investigating the properties of different types of pulsating stars

Enabling Grids for E-sciencE EGEE-II INFSO-RI Synthetic Colour-Magnitude diagrams ~90,000 objects SFR typical of the solar neighbourhood Salpeter IMF 1  photometric error of 0.03 mag 20% unresolved binaries a n e x a m p l e ! we can account for a spread in the AMR, photometric errors, depth effects, interstellar extinction and unresolved binaries It provides information about the number and period distribution of various types of radially pulsating stars

Enabling Grids for E-sciencE EGEE-II INFSO-RI Theory  Observations: some scientific cases NGC2420: (m  M) 0 =11.90 mag E(B  V)=0.06 [Fe/H]=  0.44 solid – overshooting 3.2Gyr dashed – canonical 2Gyr

Enabling Grids for E-sciencE EGEE-II INFSO-RI Determination of Star Formation Histories

Enabling Grids for E-sciencE EGEE-II INFSO-RI The Horizontal Branch: The R parameter N HB – number of HB stars N RGB – number of RGB stars brighter than the HB The mean GC He abundance is Y=0.250±0.006 Fully consistent with the primordial He abundance obtained by CMB observations coupled to primordial nucleosynthesis calculations

Enabling Grids for E-sciencE EGEE-II INFSO-RI Initial-Final mass relation

Enabling Grids for E-sciencE EGEE-II INFSO-RI Future developments more models… more chemical compositions… more photometric filters… integrated colours, mass-to-light-ratios theoretical high resolution Spectral Energy Distributions…

Enabling Grids for E-sciencE EGEE-II INFSO-RI Integrated spectra We are at present working intensively (large part of the work is completed) on computing theoretical integrated spectra (at both low- and high resolution), integrated colours, mass-to- light ratios, for studies of extragalactic stellar populations Low resolution theoretical spectra of a typical Galactic globular cluster and an old open cluster

Enabling Grids for E-sciencE EGEE-II INFSO-RI Integrated properties of extragalactic Stellar Systems

Enabling Grids for E-sciencE EGEE-II INFSO-RI Why, What, Where ? A Bag of Stellar Tracks and Isochrones

Enabling Grids for E-sciencE EGEE-II INFSO-RI

Enabling Grids for E-sciencE EGEE-II INFSO-RI A WEB interface allows the user to compute Evolutionary Tracks/Isochrones/Luminosity Functions/Synthetic CMDs

Enabling Grids for E-sciencE EGEE-II INFSO-RI

Enabling Grids for E-sciencE EGEE-II INFSO-RI Some numbers related to the BaSTI “traffic” (last update 8 May 2007) Visits (since Feb. 2004): Total – about 6000 Average per day – 9 Average visit length – 5 min Page views (since Feb. 2004): Total – about Average per day – 19 Average per visit – 2.1 The refereed papers introducing BaSTI have collected 138 citations in 19 months Summary of last year’s visits and page views

Enabling Grids for E-sciencE EGEE-II INFSO-RI The BaSTI To make the archive VO compliant Standards… Query language Data access layer Semantics Data models A pilot project for stellar astrophysics Re-building the database to allow ADQL access

Enabling Grids for E-sciencE EGEE-II INFSO-RI The BaSTI The state-of-the-art: Connection with three WPs WP3 – integration of DBs WP4 – theory within VO WP5 – connection with grids Part of the EU/FP6 funded VO-DCA project Will participate in definition of VO Data Model for theory Will test integration of VO-compliant DB with EGEE

Enabling Grids for E-sciencE EGEE-II INFSO-RI Basti & GRID Finalising the ‘gridification’ of the code to allow the calculation of new models using the Grid infrastructure State-of-the-art: Our evolutionary code is now efficiently running within LINUX platform and we start the preliminary tests needed before a massive use of the Grid infrastructure. Mid-term projects: We plan to compute in the next few months an extended set of stellar models for chemical compositions and masses not yet included in the BaSTI archive. We’ll also compute a large set of integrated spectra for stellar populations with complex Star Formation Histories Long-term project: We wish to allow an “on-line” access to our evolutionary code so that users can compute their own evolutionary models: the computational work should be performed within a Grid infrastructure

Enabling Grids for E-sciencE EGEE-II INFSO-RI EGEE Added Values CPU power: –E-computing lab –Production burst –Efficient CPU usage/sharing Data storing/sharing: –Distributed data for distributed users –Replica and security –Common interface to software and data FRANEC simulations are highly computing demanding and produce a huge amount of data.

Enabling Grids for E-sciencE EGEE-II INFSO-RI Proposed Activity Run simulations of the FRANEC code on the Grid Manage Job submission from portal; Store data on Grid environment; Share data to Virtual Observatory Community –Interoperability use case(?)

Enabling Grids for E-sciencE EGEE-II INFSO-RI Proposed Activity To allow users to run FRANEC simulation SW we need to create some specific services on EGEE common environment; They must be used to run both one or more stellar population runs; They are modular and easy to integrate with new code implementations: when some upgrade is needed.

Enabling Grids for E-sciencE EGEE-II INFSO-RI Expected implementation

Enabling Grids for E-sciencE EGEE-II INFSO-RI Why EGEE EGEE infrastructure is stable and efficent; Need to use job management + data management + metadata management services Services are not too complicated to integrate;