FESR Consorzio COMETA - Progetto PI2S2 Supernova Remnants and Grid Computing at INAF-OAPa Marco Miceli Consorzio COMETA, INAF-OAPa Grid Open Days all’Università di Palermo Palermo, F. Bocchino, INAF-OAPa, Consorzio COMETA S. Orlando, INAF-OAPa, Consorzio COMETA F. Reale, Università di Palermo, INAF-OAPa, Consorzio COMETA E. Troja, Università di Palermo, INAF-IASF Pa

Palermo, Grid Open Days all’Università di Palermo, Outline Introduction: Supernova Remnants Studying SNRs by using GRID Hydrodynamic Modeling Analysis of X-ray observations Conclusions

Palermo, Grid Open Days all’Università di Palermo, Supernova Remnants (SNRs) Supernova explosion Total energy released:  erg “Visible” energy:  erg Mass ejected: several solar masses Formation of blast wave shocks Heating of the ambient medium Compression Interaction with interstellar clouds Propagation of the ejecta Chemical enrichment of the galaxy Propagation of supersonic “bullets” Crab nebula hard X-rays soft X-rays Infrared

Palermo, Grid Open Days all’Università di Palermo, Supernova Remnants (SNRs) Physical processes involved: Purely Hydrodynamic effects Thermal conduction Radiative cooling (thermal emission) Synchrotron losses (non-thermal emission) Non-equilibrium of ionization Therefore an accurate diagnostics of the physical properties of the plasma and a detailed modeling of the system are required

Palermo, Grid Open Days all’Università di Palermo, Studying SNRs by using GRID Modeling: hydrodynamic simulations performed on the HPC system of the COMETA GRID. Data Analysis: extensive spectral analysis performed with multiple GRID tasks High Performance Computing is required to solve numerically the HD equations describing the evolution of the system. See Orlando’s talk for details Spatially resolved analysis of X-ray spectra observed with the CCD cameras of the XMM-Newton X-ray telescope

Palermo, Grid Open Days all’Università di Palermo, Hydrodynamic Modeling The Vela SNR Distance: ~250 pc Age: ~11000 yr In middle-aged SNR the bulk of the X-ray emission is commonly associated with shocked ISM, but: Vela SNR: 6 X-ray emitting shrapnels, probably associated with ejecta (outside the border of the shell). Recent discovery of new shrapnels inside the shell (Miceli et al. 2007, submitted) keV Rosat All Sky Survey

Palermo, Grid Open Days all’Università di Palermo, Hydrodynamic Modeling  : mass density v : bulk velocity P : pressure E : tot. energy per unit mass q :  (T)  T (Spitzer & saturated) n : density  ( T ): radiative losses function  : internal energy per unit mass Numerical solution through the FLASH code, an advanced HD code made parallel with MPI (see Orlando’s talk for details) P= Aims: evolution of supersonic fragments of ejecta (interaction with the shock waves and with the ambient medium) Equations of the model:

Palermo, Grid Open Days all’Università di Palermo, Initial conditions: exploding sphere of ejecta with a density inhomogeneity (i.e the shrapnel) M ej = 12 M ⊙ E = erg R 0 = 4.5 x cm V ej (R 0 ) = 6 x cm/s (v(R)  r)  (R) following Wang & Chevalier 2002 M shrapnel = 1/20 M ej  shrapnel =  ej 2-D simulations in cylindrical coordinates (axial symmetry). We follow the evolution of the system for ~ yr (the Vela age is ~ yr) Hydrodynamic Modeling r (cm) z (cm)

Palermo, Grid Open Days all’Università di Palermo, Hydrodynamic Modeling Parameter space exploration: We investigate how the evolution of the system depends on the density contrast (between the shrapnel and the surrounding ejecta) and on the initial position of the shrapnel. R shrapnel /R 0  (*) The COMETA HPC system is expected to be more efficient than the CINECA CLX by about a factor of 1.5 (see Orlando’s talk) “Complete” run executed on the CINECA CLX cluster (total CPU time~9000 h) “Complete” runs to be done on the COMETA HPC system (*) Pure HD run (no thermal cond. no rad. losses) executed on the HPC system COMETA (total CPU time~250 h, memory~7 Mb, output size~3 Gb).

Palermo, Grid Open Days all’Università di Palermo, flash.jdl Type = "Job"; JobType = "MVAPICH2"; NodeNumber = 32; Executable = "flash2"; StdOutput = "mpi.out"; StdError = "mpi.err"; InputSandbox = {"watchdog.sh","mpi.pre.sh","mpi.post.sh","flash.par","flash2"}; OutputSandbox = {"mpi.err","mpi.out","watchdog.out",“shrapnel.log","amr_log"}; Requirements = (other.GlueCEUniqueId == "unipa-ce- 01.pa.pi2s2.it:2119/jobmanager-lcglsf-hpc"); MyProxyServer = "grid001.ct.infn.it"; RetryCount = 3;

Palermo, Grid Open Days all’Università di Palermo, Hydrodynamic Modeling log  (g/cm 3 ) T (K) spatial res x 2048 point The Vela SNR keV ROSAT All SKy Survey ( keV) The COMETA HD run:  = 30, R shr = 1/3 R 0 )

Palermo, Grid Open Days all’Università di Palermo, Analysis of X-ray observations Equivalent width eV Spatially resolved spectral analysis of XMM-Newton observations IC 443SN keV cnt/s

Palermo, Grid Open Days all’Università di Palermo, Analysis of X-ray observations Define Model Calculate Model Folding by detector response Compare to data Change model parameters Forward-fitting algorithm For each spectral region Local/absolute  2 minimum?

Palermo, Grid Open Days all’Università di Palermo, Analysis of X-ray observations Finding a new  2 minimum

Palermo, Grid Open Days all’Università di Palermo, Analysis of X-ray observations A12N B1B1 12P F1F1 Off- line B2B2 12P F2F2

Palermo, Grid Open Days all’Università di Palermo, Conclusions Using the GRID for HPC Preliminary simulations already performed Complete parameter space exploration scheduled Need for more efficiency (see Orlando’s talk) Using the GRID for data analysis Huge speed-up in the spectral analysis process (Troja et al A&A, submitted) Large program of spatially resolved spectral analysis of SN 1006

Palermo, Grid Open Days all’Università di Palermo, Any Questions ? Thank you very much for your kind attention!