The project consists in two data reduction schools on specific VLTI instruments and capabilities and two science schools that put interferometry in context. Please register to receive more details on locations and dates.
Data reduction schools
These hands-on schools will form proficient users of the European ground based facility VLTI. These schools are an evolution of our very successful experience: the winter school � Observing with the VLTI funded through EC FP5. The first school in 2006 will focus on MIDI/AMBER observations, in 2008 thesecond school main topic will be PRIMA and imaging.
Event topics
General lectures: Introduction to interferometry; The VLTI and its instruments; Preparation of observations; Theory of interferometric data processing; Data reduction of MIDI, AMBER and PRIMA data; Image reconstruction from visibilities and closure phases; Model fitting.
Tutorials
How to prepare an observation in interferometry; How to prepare an observation with MIDI, AMBER and PRIMA; The search for calibrator stars principles & tools; Data reduction software of MIDI,AMBER and PRIMA (visibilites); Data reduction software of AMBER (closure and differential phase); Model fitting; Image reconstruction with VLTI. Phase referencing with PRIMA.
Seminars
Stellar diameters measurements; Mira stars and supergiants; The shape of stars; Young Stellar Objects; Active Galactic Nuclei with Keck and VLTI; Molecules around late-type stars; Dust around late-type stars; Exoplanets; Faint objects with PRIMA.
Thematic astrophysical schools
These schools will address key astrophysical challenges where optical interferometry is expected to play an important role and were Europe has a clear standing. Their goal is to complement the data reduction schools by placing optical interferometry in perspective together with other techniques. Synergies between several high angular resolution techniques and facilities (VLTI, VLT, adaptive optics, radio interferometry at mm/cm VLBI/ALMA, HST) with optical interferometry will be addressed within outstanding thematic questions of astrophysics. These schools take place in 2007 and address different astrophysical communities,
Circumstellar disks and planets: Event topics
- Current and future ground & space instrumentation (VLT, VLTI, Spitzer, Hershel, ALMA, VLBI).
- High angular resolution techniques: atmospheric turbulence, adaptive optics, interferometry (optical, thermal, mm and radio); optical synthesis imaging, nulling, astrometry.
- Observations of disks: mm (interferometry) dust & gas observations; optical/IR imaging/AO/polarization; mid-infrared and optical interferometry; spectroscopy, veiling, X-rays.
- Dynamical disk theory: disk hydro and magneto-hydrodynamics, including massive supercomputing simulations; instabilities; disk-jets interaction, star-disk interaction (magnetospheres, stellar breaking, and jets).
- SED models, radiative transfer models (monte-carlo, semi-analytical), coupling radiative transfer codes with hydro-codes, benchmarking.
- Disk chemistry and grain formation.
- Disk evolution, frequency and lifetimes. Disks across the HR diagram.
- Planetesimal growth; disk dispersal, mineralogy, zodiacal light.
- Planetary formation (architectures, theory).
- Overview of extra-solar planet observations; disk/planet interactions,migration; parent star properties.
Active Galactic Nuclei at the highest angular resolutions: Theory and Observations Event topics
- Introduction to Interferometry;
- The VLT Interferometer: the system; AMBER; MIDI; PRIMA;
- ALMA: the system; instrumentation;
- Adaptive optics: concepts; current and future instrumentation;
- Introduction to AGNs: observed types of AGNs; the unified model; luminosity functions and cosmological evolution;
- The Central Black Hole: detecting and measuring BH masses; relation with host galaxy; BH demography and AGN activity; prospects with AO, VLTI and ALMA;
- The accretiondisk: AGN Spectral Energy Distribution; emission mechanisms; theory of accretion disks; jet formation and launch models
- The Broad Line Region: observations; ionization models; elemental abundances; BLRstructure from reverberation mapping; prospects with VLTI
- The obscuring torus: observations; physical models; radiative transfer models; prospects with VLTI, AO and ALMA
- The narrow line region: observations; ionization models (photo- vs shock- ionization); prospects/results with VLTI, AO and ALMA
- Circumnuclear star formation: observations; the starburst-AGN connection from 0 to high redshift; AGN host gala xies; Ultraluminous IRAS galaxies; elemental abundances as tracers of star formation; stellar population synthesis models; prospects with VLTI, AO and ALMA
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