Lecturers |
Participants |
Préface |
Preface |
Contents |
Some Quantitative Aspects of Galactic and Extragalactic Infrared Astronomy / M. HarwitCourse 1: |
Introduction / 1: |
Energy dissipation in cosmic clouds / 2: |
Impurities / 3: |
Population of excited states / 4: |
Cooling rates / 5: |
Grains and ices / 6: |
Polycyclic aromatic hydrocarbons / 7: |
Grain formation / 8: |
Cooling of dense clouds by grain radiation / 9: |
The Sunyaev-Zel'dovich effect / 10: |
The diffuse extragalactic background, cosmic metallicity, and star formation / 11: |
Background observations / 12: |
Contributions from discrete sources / 13: |
Star formation rates, metallicity, and energy production / 14: |
Must most of the energy production have occurred at low red shifts z? / 15: |
A Single star burnt at red shift z / 15.1: |
Continuous formation of massive stars / 15.2: |
Low-mass stars / 15.3: |
Directly observed star formation / 15.4: |
The epoch from which the bulk of the integrated background radiation reaches us / 16: |
Overviewof the ISO Mission / M.F. KesslerCourse 2: |
ISO satellite |
Satellite design / 2.1: |
Satellite observing modes / 2.2: |
Satellite in-orbit performance / 2.3: |
Instrument payload |
Overview of instruments / 3.1: |
The ISO camera: ISOCAM / 3.2: |
The ISO imaging photopolarimeter: ISOPHOT / 3.3: |
The ISO short wavelength spectrometer: SWS / 3.4: |
The ISO long wavelength spectrometer: LWS / 3.5: |
Orbit |
Operations |
Operations design / 5.1: |
Observing time / 5.2: |
Operations performance / 5.3: |
Scientific highlights |
The ISO legacy |
ISO data in general / 7.1: |
The ISO data archive / 7.2: |
Using the ISO data archive / 7.3: |
Software tools and overall documentation / 7.4: |
Plans until end 2001 / 7.5: |
Conclusions |
Data Analysis with ISOCAM / J.L. StarkCourse 3: |
ISOCAM data calibration |
Cosmic ray impact suppression |
Dark subtraction for the LW channel |
Flat field correction |
Stabilization / 2.4: |
Jitter / 2.5: |
Field of view distortion correction / 2.6: |
Source detection in ISOCAM images |
Source detection from the wavelet transform |
ISOCAM faint source detection: The PRETI method |
Calibration from pattern recognition / 3.3.1: |
Example / 3.3.3: |
Image restoration using the wavelet transform |
Image filtering / 4.1: |
Image deconvolution / 4.2: |
Conclusion |
ISO Observations of Solar-System Objects / T. EncrenazCourse 4: |
Mars |
Giant planets |
The D/H ratio |
The stratospheres of the giant planets |
External source of oxygen in the giant planets / 3.2.1: |
Detection of stratospheric hydrocarbons / 3.2.2: |
Fluorescence emissions in the stratospheres of Jupiter and Saturn / 3.2.3: |
The tropospheres of the giant planets |
The 2.7 ?m window |
The 7-11 ?m spectrum of Jupiter and Saturn |
The far-infrared spectrum of Saturn |
The 5-?m spectral window / 3.3.4: |
Pluto |
Titan |
Galilean satellites |
Comet Hale-Bopp (C/1995 O1) |
Short-period comets |
Cometary trails |
Distant comets and Kuiper-Belt objects |
Asteroids |
Zodiacal light |
Conclusions and perspectives |
Stars and Galactic Structure / H. HabingCourse 5: |
The complex objects called stars: Well known and still puzzling |
Outline of these notes / 1.1: |
Red and Brown dwarfs: Stars of very low mass |
Calculations of the structure of M-dwarfs and brown giants |
How they look like: Spectra of red and brown dwarfs |
The search for red and brown dwarfs: Strategies and results |
Luminosity function |
Main-sequence stars: Debris disks and planets |
The "Vega-effect" |
The discovery of planets |
Remnant disks as observed by ISO |
Red giants |
Basic properties of red giants: RGB and AGB stars and later episodes |
Recent calculations of stellar structure and stellar evolution |
Ab-initio models of the evolution of AGB stars taking mass loss intoaccount / 4.3: |
"Synthetic" models of the evolution of AGB stars taking mass lossintoaccount / 4.4: |
And what about double stars? / 4.5: |
The impact of new observations, especially, but not exclusively, by ISO / 4.6: |
AGB stars in our Milky Way and in the Magellanic Clouds |
Concluding remarks |
Star Formation / A. NattaCourse 6: |
Collapse of molecular cores |
Giant molecular clouds and cores |
Conditions for collapse |
Free-fall collapse |
Cloud collapse / 2.3.1: |
Free-fall accretion / 2.3.2: |
Collapse of an isothermal sphere of gas |
Collapse of a slowly rotating core |
Observable properties of protostars |
Evidence of infall from molecular line profiles |
SEDs of protostars |
The line spectrum of a protostar |
Protostellar and pre-main-sequence evolution |
The protostellar phase |
Pre-main-sequence evolution |
The birthline |
Circumstellar disks |
Accretion disks |
Properties of steady accretion disks |
The velocity field / 5.2.1: |
Timescales / 5.2.2: |
Temperature profile and luminosity / 5.2.3: |
Density structure / 5.2.4: |
Reprocessing disks |
Disk-star interaction / 5.4: |
SEDs of disks |
Power-law disks / 6.1: |
Long-wavelength flux and disk mass / 6.2: |
Comparison with TTS observations: Heating mechanism / 6.3: |
Flared disks / 6.3.1: |
Heating by halos / 6.3.2: |
Disk atmospheres / 6.3.3: |
Disk properties from observations |
Mass accretion rate |
Inner radius |
Masses |
Sizes |
Disk lifetimes |
Ground-based near and mid-infrared surveys / 8.1: |
Mid-infrared ISOCAM surveys / 8.2: |
ISOPHOT 60 ?m survey / 8.3: |
Surveys at millimeter wavelengths / 8.4: |
Disk evolution |
Can we observe the early planet formation phase? / 9.1: |
Evidence for grain growth / 9.2: |
Evidence of planetesimals / 9.3: |
Where is the disk mass? / 9.4: |
Secondary or debris disks |
Summary |
Dust in the Interstellar Medium / by F. Boulanger ; P. Cox ; A.P. JonesCourse 7: |
The phases of the interstellar medium |
Abundances |
Extinction curve |
Infrared emission from dust |
Spectral energy distribution |
Grain temperatures and infrared emission |
Dust composition as a function of size |
Interstellar PAHs |
Small aromatic hydrocarbons in cirrus / 6.1.1: |
Excitation by stellar light / 6.1.2: |
Carbon abundance in PAHs / 6.1.3: |
Band profiles / 6.1.4: |
Very small grains |
Large grains |
Dust processing in the interstellar medium |
Grain sputtering and shattering in shock waves |
Physical processes / 7.1.1: |
Observations / 7.1.2: |
Grain growth in molecular clouds |
Dust evolution in clouds / 7.2.1: |
Dust evolution in photo-dissociation regions / 7.2.3: |
Dense media around protostars |
Absorption spectroscopy of embedded sources |
Dust around young stars |
Dust formation |
AGB stars |
Infrared spectroscopy of AGB and post-AGB stars |
Carbon-rich sources / 9.3.1: |
Oxygen-rich sources / 9.3.2: |
Evolved planetary nebulae / 9.3.3: |
Dust in SNR and hot stars |
The life cycle of dust |
Sources of dust / 10.1: |
The crystalline-amorphous-crystalline silicate transition / 10.2: |
Interstellar dust in the solar system / 10.4: |
Summary and perspectives |
Normal Galaxies in the Infrared / by G. HelouCourse 8: |
The study of normal galaxies |
Galaxies in the infrared: The IRAS ERA |
Basic parameters and statitics |
Infrared luminosity / 3.1.1: |
The infrared-to-blue ratio / 3.1.2: |
IRAS colors / 3.1.3: |
Other estimators / 3.1.4: |
Correlations |
The infrared-radio connection |
The "two-component model" |
ISO reshapes the dust continuum |
ISO surveys of galaxies |
Mid-infrared spectra |
The aromatic features / 4.2.1: |
The mid-infrared continuum / 4.2.2: |
High-redshift applications / 4.2.3: |
Exceptions / 4.2.4: |
The ISO-IRAS color diagram |
The global infrared spectrum / 4.3.1: |
A mid-infrared look within galaxies |
A walk in the line forest |
Molecular lines |
Fine-structure lines |
Interpreting the PDR lines |
More studies |
Tomorrow's infrared galaxies |
Challenges and prospects |
Suggestions |
Active Galaxies / by D. KunzeCourse 9: |
Starburst galaxies |
Scales of star formation: From H II regions to starburst galaxies |
Observational properties of starburst galaxies |
ISO observations of starburst galaxies |
The galactic center |
Active galactic nuclei |
A unified model for AGNs |
Massive central black holes |