Infrared space astronomy, today and tomorrow

Infrared space astronomy, today and tomorrow......Page 1
Preface......Page 2
CONTENTS......Page 5
1......Page 15
2 Energy dissipation in cosmic clouds......Page 17
3 Impurities......Page 18
4 Population of excited states......Page 20
5 Cooling rates......Page 21
6 Grains and ices......Page 24
7 Polycyclic aromatic hydrocarbons......Page 26
8 Grain formation......Page 27
9 Cooling of dense clouds by grain radiation......Page 29
10 The Sunyaev–Zel’dovich e.ect......Page 30
11 The di.use extragalactic background, cosmic metallicity, and star formation......Page 31
12 Background observations......Page 33
13 Contributions from discrete sources......Page 34
14 Star formation rates, metallicity, and energy production......Page 35
15.1 A Single star burst at red shift z......Page 38
15.2 Continuous formation of massive stars......Page 39
15.4 Directly observed star formation......Page 40
References......Page 41
2......Page 43
1 Introduction......Page 45
2.1 Satellite design......Page 46
2.3 Satellite in-orbit performance......Page 49
3.1 Overview of instruments......Page 50
3.2 The ISO camera: ISOCAM......Page 51
3.3 The ISO imaging photopolarimeter: ISOPHOT......Page 53
3.4 The ISO short wavelength spectrometer: SWS......Page 56
3.5 The ISO long wavelength spectrometer: LWS......Page 58
5.1 Operations design......Page 60
5.2 Observing time......Page 62
5.3 Operations performance......Page 63
6 Scientific highlights......Page 64
7.1 ISO data in general......Page 65
7.2 The ISO data archive......Page 66
7.3 Using the ISO data archive......Page 69
7.4 Software tools and overall documentation......Page 73
7.5 Plans until end 2001......Page 74
References......Page 75
3......Page 77
1 Introduction......Page 79
2.1 Cosmic ray impact suppression......Page 81
2.2 Dark subtraction for the LW channel......Page 84
2.3 Flat field correction......Page 85
2.4 Stabilization......Page 86
2.6 Field of view distortion correction......Page 87
3.1 Introduction......Page 90
3.2 Source detection from the wavelet transform......Page 91
3.3.2 Calibration from pattern recognition......Page 93
4.1 Image filtering......Page 95
4.2 Image deconvolution......Page 97
References......Page 101
4......Page 103
1 Introduction......Page 106
2 Mars......Page 109
3 Giant planets......Page 116
3.1 The D/H ratio......Page 120
3.2.1 External source of oxygen in the giant planets......Page 123
3.2.2 Detection of stratospheric hydrocarbons......Page 126
3.3 The tropospheres of the giant planets......Page 129
3.3.1 The 2.7 µm window......Page 131
3.3.3 The far-infrared spectrum of Saturn......Page 133
3.3.4 The 5-µm spectral window......Page 134
4 Pluto......Page 136
5 Titan......Page 137
6 Galilean satellites......Page 140
7 Comet Hale-Bopp (C/1995 O1)......Page 143
8 Short-period comets......Page 147
9 Cometary trails......Page 151
11 Asteroids......Page 153
13 Conclusions and perspectives......Page 157
References......Page 159
5......Page 164
1 The complex objects called stars: Well known and still puzzling......Page 166
2 Red and Brown dwarfs: Stars of very low mass......Page 168
2.1 Calculations of the structure of M-dwarfs and brown giants......Page 169
2.2 How they look like: Spectra of red and brown dwarfs......Page 173
2.3 The search for red and brown dwarfs: Strategies and results......Page 174
3.1 The “Vega-e.ect”......Page 176
3.2 The discovery of planets......Page 179
3.3 Remnant disks as observed by ISO......Page 181
4.1 Basic properties of red giants: RGB and AGB stars and later episodes......Page 183
4.2 Recent calculations of stellar structure and stellar evolution......Page 187
4.4 “Synthetic” models of the evolution of AGB stars taking mass loss into account......Page 188
4.6 The impact of new observations, especially, but not exclusively, by ISO......Page 192
5 AGB stars in our Milky Way and in the Magellanic Clouds......Page 198
6 Concluding remarks......Page 200
References......Page 201
6......Page 205
1 Introduction......Page 208
2.1 Giant molecular clouds and cores......Page 209
2.2 Conditions for collapse......Page 210
2.3.2 Free-fall accretion......Page 213
2.4 Collapse of an isothermal sphere of gas......Page 214
2.5 Collapse of a slowly rotating core......Page 216
3.1 Evidence of infall from molecular line profiles......Page 218
3.2 SEDs of protostars......Page 219
3.3 The line spectrum of a protostar......Page 222
4.2 Pre-main-sequence evolution......Page 224
4.3 The birthline......Page 225
5.1 Accretion disks......Page 227
5.2.1 The velocity .eld......Page 228
5.2.3 Temperature pro.le and luminosity......Page 230
5.2.4 Density structure......Page 231
5.3 Reprocessing disks......Page 232
5.4 Disk-star interaction......Page 233
6.1 Power-law disks......Page 234
6.2 Long-wavelength flux and disk mass......Page 235
6.3.2 Heating by halos......Page 237
6.3.3 Disk atmospheres......Page 239
7.2 Inner radius......Page 241
7.3 Masses......Page 242
8 Disk lifetimes......Page 244
8.2 Mid-infrared ISOCAM surveys......Page 246
8.4 Surveys at millimeter wavelengths......Page 247
9 Disk evolution......Page 249
9.2 Evidence for grain growth......Page 250
9.4 Where is the disk mass?......Page 252
10 Secondary or debris disks......Page 253
References......Page 256
7......Page 261
1 Introduction......Page 263
2 The phases of the interstellar medium......Page 265
3 Abundances......Page 266
4 Extinction curve......Page 268
5.1 Spectral energy distribution......Page 272
5.2 Grain temperatures and infrared emission......Page 273
6.1 Interstellar PAHs......Page 280
6.1.2 Excitation by stellar light......Page 281
6.1.3 Carbon abundance in PAHs......Page 284
6.1.4 Band pro.les......Page 285
6.2 Very small grains......Page 290
7 Dust processing in the interstellar medium......Page 292
7.1.1 Physical processes......Page 293
7.1.2 Observations......Page 297
7.2.1 Physical processes......Page 298
7.2.2 Dust evolution in clouds......Page 302
7.2.3 Dust evolution in photo-dissociation regions......Page 304
8 Dense media around protostars......Page 306
8.1 Absorption spectroscopy of embedded sources......Page 311
8.2 Dust around young stars......Page 318
9 Dustformation......Page 320
9.2 Physical processes......Page 321
9.3.1 Carbon-rich sources......Page 325
9.3.2 Oxygen-rich sources......Page 327
9.3.3 Evolved planetary nebulae......Page 331
9.4 Dust in SNR and hot stars......Page 332
10.1 Sources of dust......Page 333
10.2 Dust processing in the interstellar medium......Page 334
10.3 The crystalline-amorphous-crystalline silicate transition......Page 335
10.4 Interstellar dust in the solar system......Page 336
11 Summary and perspectives......Page 337
References......Page 339
8......Page 346
1 INTRODUCTION......Page 348
2 THE STUDY OF NORMAL GALAXIES......Page 350
3.1.1 Infrared luminosity......Page 352
3.1.2 The infrared-to-blue ratio......Page 354
3.1.3 IRAS colors......Page 355
3.1.4 Other estimators......Page 356
3.2 Correlations......Page 357
3.3 The infrared-radio connection......Page 358
3.4 The “two-component model”......Page 361
4.1 ISO surveys of galaxies......Page 363
4.2 Mid-infrared spectra......Page 365
4.2.1 The aromatic features......Page 366
4.2.2 The mid-infrared continuum......Page 368
4.2.3 High-redshift applications......Page 369
4.2.4 Exceptions......Page 370
4.3 The ISO-IRAS color diagram......Page 371
4.4 A mid-infrared look within galaxies......Page 373
5 A WALK IN THE LINE FOREST......Page 376
5.1 Molecular lines......Page 377
5.2 Fine-structure lines......Page 378
5.3 Interpreting the PDR lines......Page 380
7.1 Challenges and prospects......Page 382
7.2 Suggestions......Page 383
8 CONCLUSION......Page 384
References......Page 385
9......Page 390
1 Introduction......Page 392
2.1 Scales of star formation: From HII regions to starburst galaxies......Page 393
2.2 Observational properties of starburst galaxies......Page 396
2.3 ISO observations of starburst galaxies......Page 398
2.4 The galactic center......Page 402
3.1 A unified model for AGNs......Page 404
3.2 Massive central black holes......Page 407
3.3 Observational properties of AGNs......Page 408
3.4 ISO observations of AGNs......Page 409
4.1 ULIRGs as a class......Page 412
4.2 Arp 220 – the Rosetta stone......Page 417
4.3 The power source of ULIRGs......Page 418
References......Page 420
10......Page 423
1 Introduction......Page 425
2.1 Number counts in the Euclidean case......Page 427
2.2 Faint counts in the Friedman–Lemaˆıtre cosmology......Page 428
2.3 Background radiation......Page 431
3.1 Basic properties of dust absorption and emission......Page 432
3.2 Infrared spectra of extragalactic sources......Page 434
4.1.1 ISOCAM deep surveys of distant galaxies......Page 436
4.2.1 Relevant foreground observations......Page 440
4.1.2 ISOPHOT deep surveys of distant galaxies......Page 437
4.1.3 Deep cosmological surveys with SCUBA......Page 438
4.2 Observations of the Cosmic Background......Page 439
4.2.2 The cosmic infrared background at sub-millimeter wavelengths......Page 441
4.2.3 The cosmic background at all wavelengths......Page 442
4.2.4 ISO observations of the background anisotropies......Page 443
5.1 Where is the nucleosynthesis energy?......Page 444
5.2 Starburst galaxies vs. AGNs......Page 445
5.3 Star formation at high redshift......Page 447
6.1 Spectral energy distributions......Page 450
6.3 Semi–analytic models......Page 451
7 Future cosmological observations in the infrared......Page 452
References......Page 454