node organization network activities and scientific highlights so far
DESCRIPTION
MAGPOP The Italian node (INAF+SISSA). Node organization Network activities and scientific highlights so far. INVOLVED INSTITUTES. Node is scattered both from a geographic ( Padova + Trieste : 180 km) awa from an institutional point of view ( INAF + SISSA ) - PowerPoint PPT PresentationTRANSCRIPT
Node organizationNode organization Network activities and scientific highlights Network activities and scientific highlights
so far so far
MAGPOPMAGPOPThe Italian node (INAF+SISSA)The Italian node (INAF+SISSA)
INVOLVED INSTITUTESINVOLVED INSTITUTES
Node is scattered both from a geographic (Node is scattered both from a geographic (PadovaPadova + Trieste + Trieste: 180 km) awa from an : 180 km) awa from an institutional point of view (institutional point of view (INAF + SISSAINAF + SISSA))
INAF = Istituto Nazionale di Astrofisica (INAF) INAF = Istituto Nazionale di Astrofisica (INAF) gathers 12 ‘Observatories’. Pure research gathers 12 ‘Observatories’. Pure research institute. People from 2 are involved in institute. People from 2 are involved in MAGPOP: Padova and Trieste (MAGPOP: Padova and Trieste (WWW.INAF.ITWWW.INAF.IT). ).
SISSA = Scuola Internazionale di Studi Superiori SISSA = Scuola Internazionale di Studi Superiori Avanzati. Pure PhD university institute in Avanzati. Pure PhD university institute in Trieste, provides PhDs in several scientific Trieste, provides PhDs in several scientific disciplines (disciplines (WWW.SISSA.ITWWW.SISSA.IT). ).
Most team members belongs to INAF. SISSA is Most team members belongs to INAF. SISSA is involved to provide final PhD title to ESR.involved to provide final PhD title to ESR.
INAF-OAPD
INAF-OATS&SISSA
BOX SIZE ' 180 km
Team membersTeam members““Experts in stellar pop. synth, photo ionization codes and models for Experts in stellar pop. synth, photo ionization codes and models for
the effect of dust on SEDsthe effect of dust on SEDs” (ANNEX I) ” (ANNEX I)
NAMENAME INST.INST. Expertises relevant for MAGPOPExpertises relevant for MAGPOPGian Luigi Gian Luigi GranatoGranato
INAFINAFPadovaPadova
AGN and Galaxies SED modelsAGN and Galaxies SED modelsGalaxy formationGalaxy formation
(Ales)Sandro(Ales)SandroBressanBressan
INAFINAFPadovaPadova
Stellar evolutionStellar evolutionPopulation synthesis (SSP)Population synthesis (SSP)
Laura SilvaLaura Silva INAFINAFTriesteTrieste
Galaxies SED models Galaxies SED models Galaxy formationGalaxy formationPopulation synthesis (SSP)Population synthesis (SSP)
Paola AndreaniPaola Andreani INAFINAFTriesteTrieste
IR and sub-mm observationsIR and sub-mm observations
Luigi (Gigi)Luigi (Gigi)DaneseDanese
SISSASISSA Galaxy formationGalaxy formationAGN SED modelsAGN SED models
Pasquale Pasquale PanuzzoPanuzzo
INAFINAFPadovaPadova
Galaxies SED modelsGalaxies SED modelsNebular lines emissionNebular lines emission
Network related activities at INAF nodeNetwork related activities at INAF node Our main role: support for modelling multi-Our main role: support for modelling multi-
wavelength SED of galaxies and AGNs, and wavelength SED of galaxies and AGNs, and the combination of two, in particular the combination of two, in particular the the effects of dust reprocessingeffects of dust reprocessing
• SSPsSSPs• Chemical evolution computationChemical evolution computation• GRASIL (mainly, but not only, SED of dusty GRASIL (mainly, but not only, SED of dusty
galaxies)galaxies)• Radiative models of AGN toriRadiative models of AGN tori
Also models for galaxy formationAlso models for galaxy formation Two PhD students (ESR) are trained on these Two PhD students (ESR) are trained on these
topics. topics.
Research highlights so farResearch highlights so far
GALSYNTH (web interface for GRASIL)GALSYNTH (web interface for GRASIL) Improvement of GRASIL treatment of Improvement of GRASIL treatment of
MIR region (post-ISO PAHs)MIR region (post-ISO PAHs) Early type galaxies in mid IR with our Early type galaxies in mid IR with our
SPIZTER data and our models SPIZTER data and our models Tested against QSO LFs our model for Tested against QSO LFs our model for
the joint evolution of galaxies and QSOsthe joint evolution of galaxies and QSOs
GALSYNTH GALSYNTH a WEB interface to compute GRASIL modelsa WEB interface to compute GRASIL models
http://web.pd.astro.it/galsynthhttp://web.pd.astro.it/galsynth Anyone can register and be a userAnyone can register and be a user Users have their workspacesUsers have their workspaces Interactive editing of parameters, Interactive editing of parameters,
with explanations and bound with explanations and bound checking, including iterationschecking, including iterations
Sets of parameters can be saved, Sets of parameters can be saved, modified, reused. modified, reused.
Batch jobs are executed on a pool Batch jobs are executed on a pool of our computersof our computers
When job completed, user is When job completed, user is notified and downloads modelsnotified and downloads models
Systematic study of Systematic study of ETGs with SpitzerETGs with Spitzer
• IRAC & IRS Blue Peak-Up (16 µm) imaging of fainter Virgo members & brigthest Coma galaxies (80 galaxies)
Cycle 2 P.I. A. Bressan
• IRS LR spectroscopy of Early Type GalaxiesCM relation in Virgo Cluster (17
galaxies) Cycle 1 P.I. A. Bressan
• IRS LR spectroscopy of Field Early type galaxies (20 galaxies)
Cycle 3 P.I. R. Rampazzo
NGC4435: SED of inner SB disk
Spitzer/IRS
Post-ISO PAH - study of ETG with SpitzerPost-ISO PAH - study of ETG with Spitzer
Study of ETG with SpitzerStudy of ETG with Spitzer
Degeneracy in the Optical
Optical QSO LF Optical QSO LF ((ttQQ''4x104x1077 yr) yr)
z=1.5data Croom et al 2004
z=3 data Pei et al 1995
z=4.5 z=6data Fan et al 2004
Lapi et al 2007