ISBN: 3-540-67386-5
TITLE: Astronomie spatiale infrarouge, aujourd'hui et demain Infrared space astronomy, today and tomorrow
AUTHOR: Casoli, F.; Lequeux, J.; David, F. (Eds.)
TOC:

Lecturers xi
Participants xiii
Prface xvii
Preface xxi
Contents xxv
Course 1. Some Quantitative Aspects of Galactic and Extragalactic Infrared Astronomy
by M. Harwit 1
1 Introduction 3
2 Energy dissipation in cosmic clouds 3
3 Impurities 4
4 Population of excited states 6
5 Cooling rates 7
6 Grains and ices 10
7 Polycyclic aromatic hydrocarbons 12
8 Grain formation 13
9 Cooling of dense clouds by grain radiation 15
10 The Sunyaev-Zel'dovich effect 16
11 The diffuse extragalactic background, cosmic metallicity, and star formation 17
12 Background observations 19
13 Contributions from discrete sources 20
14 Star formation rates, metallicity, and energy production 21
15 Must most of the energy production have occurred at low red shifts z? 24
15.1 A Single star burnt at red shift z 24
15.2 Continuous formation of massive stars 25
15.3 Low-mass stars 26
15.4 Directly observed star formation 26
16 The epoch from which the bulk of the integrated background
radiation reaches us 27
Course 2. Overviewof the ISO Mission
by M.F. Kessler 29
1 Introduction 31
2 ISO satellite 32
2.1 Satellite design 32
2.2 Satellite observing modes 35
2.3 Satellite in-orbit performance 35
3 Instrument payload 36
3.1 Overview of instruments 36
3.2 The ISO camera: ISOCAM 37
3.3 The ISO imaging photopolarimeter: ISOPHOT 39
3.4 The ISO short wavelength spectrometer: SWS 42
3.5 The ISO long wavelength spectrometer: LWS 44
4 Orbit 46
5 Operations 46
5.1 Operations design 46
5.2 Observing time 48
5.3 Operations performance 49
6 Scientific highlights 50
7 The ISO legacy 51
7.1 ISO data in general 51
7.2 The ISO data archive 52
7.3 Using the ISO data archive 55
7.4 Software tools and overall documentation 59
7.5 Plans until end 2001 60
8 Conclusions 61
Course 3. Data Analysis with ISOCAM
by J.L. Stark 63
1 Introduction 65
2 ISOCAM data calibration 67
2.1 Cosmic ray impact suppression 67
2.2 Dark subtraction for the LW channel 70
2.3 Flat field correction 71
2.4 Stabilization 72
2.5 Jitter 73
2.6 Field of view distortion correction 73
3 Source detection in ISOCAM images 76
3.1 Introduction 76
3.2 Source detection from the wavelet transform 77
3.3 ISOCAM faint source detection: The PRETI method 79
3.3.1 Introduction 79
3.3.2 Calibration from pattern recognition 79
3.3.3 Example 81
4 Image restoration using the wavelet transform 81
4.1 Image filtering 81
4.2 Image deconvolution 83
5 Conclusion 87
Course 4. ISO Observations of Solar-System Objects
by T. Encrenaz 89
1 Introduction 92
2 Mars 95
3 Giant planets 102
3.1 The D/H ratio 106
3.2 The stratospheres of the giant planets 109
3.2.1 External source of oxygen in the giant planets 109
3.2.2 Detection of stratospheric hydrocarbons 112
3.2.3 Fluorescence emissions in the stratospheres of Jupiter and Saturn 115
3.3 The tropospheres of the giant planets 115
3.3.1 The 2.7 m window 117
3.3.2 The 711 m spectrum of Jupiter and Saturn 119
3.3.3 The far-infrared spectrum of Saturn 119
3.3.4 The 5-m spectral window 120
4 Pluto 122
5 Titan 123
6 Galilean satellites 126
7 Comet Hale-Bopp (C/1995 O1) 129
8 Short-period comets 133
9 Cometary trails 137
10 Distant comets and Kuiper-Belt objects 139
11 Asteroids 139
12 Zodiacal light 143
13 Conclusions and perspectives 143
Course 5. Stars and Galactic Structure
by H. Habing 151
1 The complex objects called stars: Well known and still puzzling 153
1.1 Outline of these notes 155
2 Red and Brown dwarfs: Stars of very low mass 155
2.1 Calculations of the structure of M-dwarfs and brown giants 156
2.2 How they look like: Spectra of red and brown dwarfs 160
2.3 The search for red and brown dwarfs: Strategies and results 161
2.4 Luminosity function 163
3 Main-sequence stars: Debris disks and planets 163
3.1 The "Vega-effect" 163
3.2 The discovery of planets 166
3.3 Remnant disks as observed by ISO 168
4 Red giants 170
4.1 Basic properties of red giants: RGB and AGB stars and later episodes 171
4.2 Recent calculations of stellar structure and stellar evolution 171
4.3 Ab-initio models of the evolution of AGB stars taking mass loss into account 175
4.4 "Synthetic" models of the evolution of AGB stars taking mass loss into account 175
4.5 And what about double stars? 179
4.6 The impact of new observations, especially, but not exclusively, by ISO 179
5 AGB stars in our Milky Way and in the Magellanic Clouds 185
6 Concluding remarks 187
Course 6. Star Formation
by A. Natta 193
1 Introduction 197
2 Collapse of molecular cores 198
2.1 Giant molecular clouds and cores 198
2.2 Conditions for collapse 199
2.3 Free-fall collapse 202
2.3.1 Cloud collapse 202
2.3.2 Free-fall accretion 202
2.4 Collapse of an isothermal sphere of gas 203
2.5 Collapse of a slowly rotating core 205
3 Observable properties of protostars 207
3.1 Evidence of infall from molecular line profiles 207
3.2 SEDs of protostars 208
3.3 The line spectrum of a protostar 211
4 Protostellar and pre-main-sequence evolution 213
4.1 The protostellar phase 213
4.2 Pre-main-sequence evolution 213
4.3 The birthline 214
5 Circumstellar disks 216
5.1 Accretion disks 216
5.2 Properties of steady accretion disks 217
5.2.1 The velocity field 217
5.2.2 Timescales 219
5.2.3 Temperature profile and luminosity 219
5.2.4 Density structure 220
5.3 Reprocessing disks 221
5.4 Disk-star interaction 222
6 SEDs of disks 223
6.1 Power-law disks 223
6.2 Long-wavelength flux and disk mass 224
6.3 Comparison with TTS observations: Heating mechanism 226
6.3.1 Flared disks 226
6.3.2 Heating by halos 226
6.3.3 Disk atmospheres 228
7 Disk properties from observations 230
7.1 Mass accretion rate 230
7.2 Inner radius 230
7.3 Masses 231
7.4 Sizes 231
8 Disk lifetimes 233
8.1 Ground-based near and mid-infrared surveys 235
8.2 Mid-infrared ISOCAM surveys 235
8.3 ISOPHOT 60 m survey 236
8.4 Surveys at millimeter wavelengths 236
9 Disk evolution 238
9.1 Can we observe the early planet formation phase? 239
9.2 Evidence for grain growth 239
9.3 Evidence of planetesimals 241
9.4 Where is the disk mass? 241
10 Secondary or debris disks 242
11 Summary 245
Course 7. Dust in the Interstellar Medium
by F. Boulanger, P. Cox and A.P. Jones 251
1 Introduction 253
2 The phases of the interstellar medium 255
3 Abundances 256
4 Extinction curve 258
5 Infrared emission from dust 262
5.1 Spectral energy distribution 262
5.2 Grain temperatures and infrared emission 263
6 Dust composition as a function of size 270
6.1 Interstellar PAHs 270
6.1.1 Small aromatic hydrocarbons in cirrus 271
6.1.2 Excitation by stellar light 271
6.1.3 Carbon abundance in PAHs 271
6.1.4 Band profiles 275
6.2 Very small grains 280
6.3 Large grains 281
7 Dust processing in the interstellar medium 282
7.1 Grain sputtering and shattering in shock waves 283
7.1.1 Physical processes 283
7.1.2 Observations 287
7.2 Grain growth in molecular clouds 288
7.2.1 Physical processes 288
7.2.2 Dust evolution in clouds 292
7.2.3 Dust evolution in photo-dissociation regions 294
8 Dense media around protostars 296
8.1 Absorption spectroscopy of embedded sources 301
8.2 Dust around young stars 308
9 Dust formation 310
9.1 AGB stars 311
9.2 Physical processes 311
9.3 Infrared spectroscopy of AGB and post-AGB stars 315
9.3.1 Carbon-rich sources 315
9.3.2 Oxygen-rich sources 317
9.3.3 Evolved planetary nebulae 321
9.4 Dust in SNR and hot stars 322
10 The life cycle of dust 323
10.1 Sources of dust 323
10.2 Dust processing in the interstellar medium 324
10.3 The crystalline-amorphous-crystalline silicate transition 325
10.4 Interstellar dust in the solar system 326
11 Summary and perspectives 327
Course 8. Normal Galaxies in the Infrared
by G. Helou 337
1 Introduction 339
2 The study of normal galaxies 341
3 Galaxies in the infrared: The IRAS ERA 343
3.1 Basic parameters and statitics 343
3.1.1 Infrared luminosity 343
3.1.2 The infrared-to-blue ratio 345
3.1.3 IRAS colors 346
3.1.4 Other estimators 347
3.2 Correlations 348
3.3 The infrared-radio connection 349
3.4 The "two-component model" 352
4 ISO reshapes the dust continuum 354
4.1 ISO surveys of galaxies 354
4.2 Mid-infrared spectra 356
4.2.1 The aromatic features 357
4.2.2 The mid-infrared continuum 359
4.2.3 High-redshift applications 360
4.2.4 Exceptions 361
4.3 The ISO-IRAS color diagram 362
4.3.1 The global infrared spectrum 364
4.4 A mid-infrared look within galaxies 364
5 A walk in the line forest 367
5.1 Molecular lines 368
5.2 Fine-structure lines 369
5.3 Interpreting the PDR lines 371
6 More studies 373
7 Tomorrow's infrared galaxies 373
7.1 Challenges and prospects 373
7.2 Suggestions 374
8 Conclusion 375
Course 9. Active Galaxies
by D. Kunze 381
1 Introduction 383
2 Starburst galaxies 384
2.1 Scales of star formation: From H II regions to starburst galaxies 384
2.2 Observational properties of starburst galaxies 387
2.3 ISO observations of starburst galaxies 389
2.4 The galactic center 393
3 Active galactic nuclei 395
3.1 A unified model for AGNs 395
3.2 Massive central black holes 398
3.3 Observational properties of AGNs 399
3.4 ISO observations of AGNs 400
4 Ultraluminous infrared galaxies 403
4.1 ULIRGs as a class 403
4.2 Arp 220  the Rosetta stone 408
4.3 The power source of ULIRGs 409
Course 10. Cosmology with ISO
by J.-L. Puget 415
1 Introduction 417
2 Relevant quantities and notations for number counts 419
2.1 Number counts in the Euclidean case 419
2.2 Faint counts in the FriedmanLema itre cosmology 420
2.3 Background radiation 423
3 Spectra in the IR/SUBMM range 424
3.1 Basic properties of dust absorption and emission 424
3.2 Infrared spectra of extragalactic sources 426
4 Observations 428
4.1 Deep surveys of weak sources 428
4.1.1 ISOCAM deep surveys of distant galaxies 428
4.1.2 ISOPHOT deep surveys of distant galaxies 429
4.1.3 Deep cosmological surveys with SCUBA 430
4.2 Observations of the Cosmic Background 431
4.2.1 Relevant foreground observations 432
4.2.2 The cosmic infrared background at sub-millimeter wavelengths 433
4.2.3 The cosmic background at all wavelengths 434
4.2.4 ISO observations of the background anisotropies 435
5 Cosmological implications 436
5.1 Where is the nucleosynthesis energy? 436
5.2 Starburst galaxies vs. AGNs 437
5.3 Star formation at high redshift 439
6 Models of galaxy in the infrared 442
6.1 Spectral energy distributions 442
6.2 Phenomenological models 443
6.3 Semi-analytic models 443
7 Future cosmological observations in the infrared 444
8 Conclusions 446
Seminars by participants 451
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