Instituto de Astrofisica de Canarias
La Laguna, Tenerife, Canary Islands (Spain)
December 2nd - 13th, 1996
Organizing Committee: 

F. Sánchez, A. Aparicio, A. Herrero


-Observations of the most Luminous Stars.
        Prof. Dr. Philip Massey.Kitt Peak National Observatory
-Quantitative Spectroscopy of the most Luminous Blue Stars in Galaxies.
        Prof. Dr. Rolf Kudritzki. Universität-Sternwarte München
-Massive Stars and the Interaction with the ISM.
        Prof. Dr. Claus Leitherer. Space Telescope Science Institute
-The Extragalactic distance scale.
Prof. Dr. Barry Madore. NASA / IPAC. Extragalactic Database Infrared Processing and Analisys Center
-Resolved Stellar Populations in Luminous Galaxies.
        Prof. Dr. Mario Mateo.University of Michigan.
-Neutral and Ionized Gas in Nearby Galaxies.
        Prof. Dr. Evan Skillman.University of Minnesota.
-Dwarf Galaxies.
        Prof. Dr. Gary Da Costa. Mt Stromlo & Siding Spring Observatory
-Stellar Evolution.
        Prof. Dr. Cesare Chiosi. Universita di Padova.


Prof. Dr. Philip Massey
Kitt Peak National Observatory

1. Introducing the Unevolved Luminous Stars
1.1.- Stellar parameters, ages, main-sequence evolution: Luminous EQ Massive
1.2.- Colors of hot stars
1.3.- Color-Magnitude Diagrams
1.4.- Effects of reddening
1.5.- Bolometric Corrections
1.6.- Spectral Classification
1.7.- HR Diagrams: The Difference Betwen "Luminous and Bright"
2. Finding Main-sequence Luminous Stars in the Local Group Methodology: 
2.1.- UBV Photometry with CCDs
2.2.- Reddening-free indices
2.3.- Spectroscopy
---doing it one star at a time
---doing a bunch of stars at once
2.4.- HRDs for OB associations in the Local Group
3. Finding the Evolved Descendants of Massive Stars: LBVs, WRs, and RSGs
3.1.- Motivation: Observational Constraints on Stellar Evolution
3.2.- How to find them: Not as Easy as You Might Think
Wolf-Rayets---bias towards WCs
RSGs---telling foreground dwarfs from RSGs
LBVs---the "tip of the iceberg" effect
4. Secrets of Star Formation as Revealed by Luminous Stars
4.1.- UBV Photometry + Classification ---> HRDs
4.2.- Initial Mass Functions and Upper Mass Limits in the
Field and Associations of the Milky Way and Magellanic Clouds (MC)
4.3.- What's Next: Extention to Galaxies beyond the MCs
5. Secrets of Stellar Evolution Revealed by Luminous Stars
5.1.- Global Properties: RSG/BSG Ratios, O/WR Ratios, WC/WN Ratios
5.2.- Individual OB Associations: coeveal tests of stellar evolution.

Prof. Dr. Rolf Kudritzki
Universität-Sternwarte München

1. The physics of hot star atmospheres
1.1.- Stellar winds and hydrodynamic atmosphere models
1.2.- NLTE-effects and spectrum synthesis
1.3.- Ionizing fluxes
1.4.- X-ray emission
1.5.- IR-excess 
2. Spectral diagnostics of luminous blue supergiants
2.1.- Effective temperatures and gravities
2.2.- Stellar wind properties
2.3.- Masses, radii and luminosities
2.4.- Abundances
3. The stellar cluster in the Galactic Center
3.1.- IR-spectroscopy and the HeI emission line stars
3.2.- Hydrodynamic model atmospheres and IR line emission
3.3.- The physical properties of the young cluster of massive stars in the Galactic Center
4. Radiation driven winds and the wind momentume-luminosity relation as a tool for extragalactic distances
4.1.- Wind momentum and stellar luminosity: theory
4.2.- The observed wind momentum luminosity relation of galactic supergiants
5. O,B,A-supergiants in Local Group galaxies
5.1.- The most massive stars in the Galaxy and the Magellanic Clouds
5.2.- Element abundances from HST and optical spectroscopy
5.3.- Supergiants in M31 and M33
5.4.- Wind momentum in Local Group galaxies
6. The step beyond the Local Group
6.1.- The new 8m class telescopes and quantitativ spectroscopy beyond the Local Group: an outlook
6.2.- Preparative work and first results
6.3.- Stellar element abundances in HST Cepheid-fields
6.4.- Wind momentum and distances up to the Virgo cluster


Prof. Dr. Claus Leitherer
Space Telescope Science Institute

1. Introduction
2. Regions of high-mass star formation
2.1.- High-mass SF in the Galaxy
2.2.- 30 Doradus: the Rosetta Stone
2.3.- Nearby galaxies: cluster vs. field population
2.4.- Implications for more distant galaxies
3. Techniques to constrain the stellar content
3.1.- Spectroscopy and photometry of individual stars
3.2.- CM diagrams of resolved populations
3.3.- Evolutionary synthesis of unresolved populations
3.4.- Nebular diagnostics as stellar tracers
3.5.- IMF and SF history in nearby galaxies
4. Release of mass and energy by massive stars
4.1.- Wind properties of individual stars
4.2.- Wind-blown bubbles around massive stars
4.3.- Mass and energy release by stellar populations
4.4.- Stars versus supernovae
4.5.- Dynamics of GEHRs
5. Massive stars and galaxy evolution
5.1.- Modes of SF in galaxies
5.2.- Massive stars and the global properties of the ISM
5.3.- Galactic superwinds
5.4.- Chemical evolution of dwarf galaxies
6. Epilogue


Prof. Dr. Barry Madore
Extragalactic Database Infrared Processing and Analisys Center

1. Historical Introduction to the Extragalactic Distance Scale
1.1.- Hubble's program
1.2.- Decades of revision
1.3.- Decades of divergence
1.4.- Fundamental problems and issues before HST
2. Cepheid Period-Luminosity Relation: Empirical Calibration
2.1.- An observer's view of the Cepheid instability strip
2.2.- Reddening corrections and intrinsic colors
2.3.- Metallicity effects
2.4.- Zero points and the distance to the LMC
2.5.- Infrared photometry
2.6.- Multi-wavelength solutions
3. Tip of the Red Giant Branch Distances
3.1.- Historical perspective (Shapley, etc.)
3.2.- Theory of the core Helium flash
3.3.- Calibration of the first ascent red giant branch peak luminosity
3.4.- Local Group galaxies
3.5.- Comparison with Cepheid distance scale
3.6.-Applications with HST
4. Secondary Distance Indicators: Description and New Calibrations
4.1.- Tully-Fisher
4.2.- Planetary Nebula Luminosity Functions
4.3.- Surface Brightness Fluctuations
4.4.- Type Ia Supernovae
4.5.- Type II Supernovae
5. The Hubble Space Telescope Key Project: Latest Results on Ho
5.1.- Philosphy and strategy of the Key Project
5.2.- Make-up of the Team
5.3.- Calibrators (plan, sampleand status report)
5.4.- HST optimized search procedure
5.5.- Local calibrators: Virgocentric flow 
5.6.- Cepheid distances to Virgo: Ho out to 1,000 km/sec
5.7.- Cepheid distance to Fornax:
Interim recalibration of all secondary calibrators
Ho out to beyond 10,000 km/sec
5.8.- Remaining issues
5.9.- Cosmological Implications


Prof. Dr. Mario Mateo 
University of Michigan

1. Introduction: Current range of ground/space based studies of resolved galaxies
2. Methods:
2.1.- Crowded field photometry
2.2.- Photometry in fields with complex backgrounds
3. The Magellanic Clouds:Probing regions of high stellar density
3.1.- In clusters
3.2.- The field
4. M31, M33 and outliers of the Local Group
5. Stellar populations in nearby groups
5.1.- The M81 group
5.2.- Sculptor group
5.3.- Cen A group
6. Stellar populations in nearby galaxy clusters: Pushing techniques and analyses to the limit.


Prof. Dr. Evan Skillman
University of Minnesota

1. The ISM distributions in Local Group Galaxies (1 hour)
1.1.- HI distributions
1.2.- Molecular distributions
1.3.- H-alpha distributions
1.4.-What we don't know
2. Star Formation in Local Group Galaxies (1 hour)
2.1.- H-alpha observations and star formation rates
2.2.- Associations between young stars, H-alpha, and atomic/molecular gas
2.3.- Star formation laws and thresholds
3. H II Regions in Local Group Galaxies and Chemical Abundance Determinations (1 hour)
3.1.- Converting HII emission line spectra into chemical abundances
3.2.- Abundance trends in spiral and irregular galaxies
3.3.- Current problems with emission line abundances
4. Self-Consistent Chemical Evolution in Local Group Galaxies and Implications for the Evolution of Galaxies (2 hours)
4.1.- Simple theories of chemical evolution
4.2.- The comparison of gas mass fractions with abundances
4.3.- Relative abundances as constraints
4.4.- Comparison with recent star formation histories 
4.5.- Making sense of it all


Prof. Dr. Gary Da Costa
Mt Stromlo & Siding Spring Observatory

1. Introduction.
1.1.- What is an "old stellar population" and how do we recognize it?
1.2.- Indicators of age and their applicability to resolved stellar populations
1.3.- Case study: the Old Populations of the LMC and SMC - implications from both the cluster and field populations.
2. The dSph and dE galaxies of the Local Group.
2.1.- Properties and Star Formation Histories of:
Galactic dSph companions
M31 dE and dSph companions
Tucana - isolated Local Group dSph
3. What can be inferred about the formation and evolution of this class of galaxies?
4. The dIrrs of the Local Group (excluding the SMC).
4.1.- Properties and Characteristics
4.2.- The role of dwarfs such as Phoenix and LGS3 in linking dIrr and dSph/dE galaxies
5. Dwarf Galaxies beyond the Local Group.
5.1.- Properties and Characteristics of dwarf members of nearby groups.
5.2.- Case study: dSph galaxies in the M81 Group.


Prof. Dr. Cesare Chiosi
Universita di Padova

1. Introduction
2. Stellar Evolution at different Metallicities
3. Advances Phases of Stellar Evolution
3.1.- Low and Intermediate Mass Stars
3.2.- Massive Stars
4. Cepheids
4.1.- Structure
4.2.- The Period-Luminosity relation