The Emission-Line Universe

Cover......Page 1
Half-title......Page 3
Title......Page 7
Copyright......Page 8
Contents......Page 9
Contributors......Page 10
Participants......Page 11
Preface......Page 13
Acknowledgements......Page 14
1.1. Introduction......Page 15
1.2.1.2 Collisional excitation......Page 16
1.2.1.4 Some hints......Page 17
1.2.2.2 The transfer of the ionizing photons produced by the nebula......Page 18
1.3.2 Ionic and elemental abundances......Page 20
1.3.2.1 Direct methods......Page 21
1.3.2.2 Statistical methods......Page 22
1.3.3 Estimation of the effective temperature of the ionizing stars......Page 24
1.3.4 Determining the star-formation rate......Page 26
1.3.5 How can one distinguish normal galaxies from AGN hosts?......Page 27
1.4.2 Why do we construct photoionization models?......Page 29
1.4.4 Abundance derivation by tailored model fitting......Page 30
1.4.5 Abundance derivation using grids of models......Page 32
1.4.8 The interpretation of data from integral field spectroscopy......Page 33
1.5.1 Correction for reddening, underlying stellar absorption and aperture effects......Page 34
1.5.3 The importance of the stellar energy distribution......Page 35
1.5.5 Temperature fluctuations and the ORL/CEL discrepancy......Page 37
1.5.6 Shocks and related issues......Page 39
Appendix: Lists of useful lines and how to deal with them......Page 40
REFERENCES......Page 50
2.2.1 Redshift......Page 55
2.2.2 Narrow-band filters and dispersers......Page 56
2.2.3 The signal-to-noise ratio......Page 57
2.2.5 Line width......Page 58
2.2.6 Equivalent width......Page 59
2.3.1 Narrow-band imaging......Page 60
2.3.2 Spectroscopic surveys......Page 63
2.3.3 The sky background......Page 65
2.3.4 Planning for a survey......Page 68
2.4.1 The search for galaxies at very high redshifts......Page 69
2.4.2 Clusters and clustering from line-emission surveys......Page 71
2.4.3 Lyman-α surveys as probes of the cosmic reionization......Page 72
2.4.4 Serendipitous discoveries......Page 73
2.5. Surveys for other emission lines......Page 74
REFERENCES......Page 75
3.1. Preamble......Page 80
3.2.1 Cosmological preliminaries......Page 82
3.2.2 Physics of recombination......Page 83
3.2.3 Coupling of gas and radiation......Page 85
3.2.4 Hydrogen molecules in the early Universe......Page 88
3.3.1 Linear theory......Page 89
3.3.2 Statistics of density fields......Page 91
3.3.3 Spherical collapse......Page 92
3.3.4 Dark-halo mergers......Page 96
3.3.5 Assembly history of a Milky Way halo......Page 98
3.3.6 Smallest SUSY–CDM microhalos......Page 101
3.4.1 Uncertainties in the power spectrum......Page 104
3.4.2 First baryonic objects......Page 106
3.4.3 21-cm signatures of the neutral IGM......Page 109
3.4.4 Concluding remarks......Page 113
REFERENCES......Page 116
4.1. Introduction......Page 120
4.2.1 Primordial star formation......Page 121
4.2.2 Primordial stars: properties......Page 122
4.2.3 Primordial stars and galaxies: observable properties......Page 123
4.2.5 Nucleosynthesis and abundance pattern......Page 125
4.3.1 ISM emission and “escape”......Page 126
4.3.2 Lyα: the observational problem......Page 127
4.3.3 Lessons from local starbursts......Page 128
4.3.4.1 Basic line-formation processes and examples......Page 129
4.3.4.3 Lyα transfer: geometrical effects......Page 131
4.3.5 Lessons from Lyman-break galaxies......Page 132
4.3.6 Lyα through the intergalactic medium......Page 133
4.3.7 Lyα from sources prior to reionization......Page 134
4.3.8 The Lyα luminosity function and reionization......Page 136
4.4.1 Search methods......Page 137
4.4.2 Distant Lyα emitters......Page 138
4.4.2.1 Population III signatures in LAEs?......Page 139
4.4.2.2 Dust properties of high-z LAEs......Page 140
4.4.3.1 i-dropout(z～6)samples......Page 142
4.4.3.2 Optical-dropout samples…......Page 143
4.4.3.2 Optical-dropo…......Page 144
4.4.4 What next?......Page 146
REFERENCES......Page 147
5.2. The discovery and nature of active galaxies......Page 152
5.3. Identifying active galaxies......Page 154
5.4. A diverse taxonomy......Page 156
5.5.1 An overview......Page 157
5.5.2.1 Physical considerations......Page 158
5.5.3.1 Physical considerations......Page 160
5.5.3.2 Observational evidence......Page 161
5.5.4 The broad-line region......Page 162
5.5.5 The narrow-line region......Page 165
5.5.6 The “obscuring torus”......Page 167
5.6. Distinguishing AGNs from other emission-line galaxies......Page 168
5.7. The theory of reverberation mapping......Page 169
5.7.1 The nature of continuum variability......Page 170
5.7.2 Reverberation-mapping assumptions......Page 171
5.7.4 Velocity–delay maps......Page 172
5.7.5 Recovering velocity–delay maps from real data......Page 175
5.8.1 The size of the broad-line region......Page 177
5.8.3 The BLR radius–luminosity relationship......Page 178
5.8.4 Black-hole masses......Page 180
5.9.1 The BLR gas: discrete clouds or a continuous flow?......Page 183
5.9.2 Physical conditions in the BLR......Page 184
5.9.4 The kinematics of the BLR......Page 186
5.10.1 The geometry of the obscuring torus......Page 187
5.11. Cosmological implications......Page 188
5.11.1 The space density of AGNs......Page 189
5.11.2 The luminosity function......Page 190
5.11.3 Masses of distant quasars......Page 191
REFERENCES......Page 193
6.1.2 The star-formation rate......Page 197
6.1.4 The infall rate......Page 198
6.1.6 Stellar evolution and nucleosynthesis: the stellar yields......Page 199
6.1.7 Type Ia SN progenitors......Page 200
6.1.9 Analytical models......Page 201
6.2. The Milky Way and other spirals......Page 203
6.2.2 The two-infall model......Page 204
6.2.3 Common conclusions from Milky Way models......Page 209
6.2.5 Abundance gradients in external galaxies......Page 210
6.2.6 How to model the Hubble sequence......Page 212
6.2.7 Type Ia SN rates in various types of galaxy......Page 214
6.3.1 Properties of dwarf irregular galaxies......Page 215
6.3.2 Galactic winds......Page 219
6.3.3 Results on DIGs and BCGs from purely chemical models......Page 220
6.3.4 Results from chemo-dynamical models: IZw18......Page 222
6.4.2 Chemical properties......Page 225
6.4.4 The ellipticals–quasars connection......Page 226
6.4.5 The chemical evolution of QSOs......Page 227
6.4.6 The chemical enrichment of the ICM......Page 229
REFERENCES......Page 231
7.2.1 Why infrared emission lines?......Page 236
7.2.2.1 Infrared observing technology......Page 237
7.2.3 Important infrared emission lines......Page 239
7.2.3.1 Hydrogen emission in the infrared......Page 240
7.2.3.2 Metal lines......Page 241
7.3.1 H II regions......Page 242
7.3.2.2 Morphology and outflow kinematics......Page 244
7.3.3 Supernova remnants......Page 246
7.4.1.1 T Tauri stars......Page 253
7.4.1.2 Herbig–Haro Objects......Page 254
7.4.1.3 Young massive stars......Page 258
7.4.2 Massive stars......Page 259
7.4.2.2 Luminous blue variables......Page 262
7.4.2.3 Wolf–Rayet stars......Page 265
7.4.3 Magnetospherically active stars......Page 268
7.4.4.2 X-ray binaries......Page 270
REFERENCES......Page 275
8.1. Introduction......Page 276
8.2. Extended-source imaging......Page 278
8.2.2 Flux calibration......Page 279
8.2.3 Equations for calibration......Page 280
8.3. Imaging in the airglow-windows range......Page 282
8.3.2 Fringing removal using the package mscred......Page 283
8.4. Selection of candidates and line flux......Page 285
REFERENCES......Page 286
9.2. Long-slit spectra......Page 288
9.2.1 Signal-to-noise calculations......Page 290
9.3.2 Flat-field and illumination corrections......Page 291
9.3.3 Wavelength calibration......Page 292
9.3.4 Flux calibration......Page 293
9.4.3 Illumination correction......Page 294
9.4.6 Flux calibration......Page 295
REFERENCES......Page 296
10.3. Optical principles......Page 297
10.4. From theory to practical design......Page 299
10.4.2 Piezoelectric transducers......Page 300
10.5. The tunable filter......Page 301
10.5.1 History......Page 302
10.6.2 Ghosts......Page 304
10.7.3 Operation modes of tunable filters......Page 305
10.9. Definitions......Page 306
10.10. Procedure......Page 307
10.10.1 Preliminary steps......Page 308
10.10.3 Flux calibration......Page 309
REFERENCES......Page 310