Santos / Pasquini / Correia Precision Spectroscopy in Astrophysics

Proceedings of the ESO/Lisbon/Aveiro Conference held in Aveiro, Portugal, 11-15 September 2006
2008
ISBN: 978-3-540-75485-5
Verlag: Springer Berlin Heidelberg
Format: PDF
Kopierschutz: 1 - PDF Watermark

E-Book, Englisch, 328 Seiten

Reihe: ESO Astrophysics Symposia

Since the use of high-precision/resolution spectroscopy is closely connected to the ability to collect a large number of photons, the scientific domains using this technique benefit tremendously from the use of 8-meter class telescopes and will fully exploit the tremendous gain provided by future Extremely Large Telescopes (ELTs). This volume comprehensively covers the astrophysical and technical aspects of high-precision spectroscopy with an outlook to future developments.

Autoren/Hrsg.

Santos, Nuno C.

Pasquini, Luca

Correia, Alexandre C. M.

Romaniello, Martino

Inhaltsverzeichnis

1;Preface;5
2;Contents;7
3;List of Participants;16
4;I Abundances and Isotopes;21
4.1;Lithium Isotopic Abundances in Stars;22
4.1.1;1 Determination of the Li Isotope Ratio;22
4.1.2;2 Lithium in Metal-poor Halo Stars;25
4.1.3;3 Search for;26
4.1.4;in Planet-hosting Stars;26
4.1.5;4 The Need for New Instrumentation;27
4.1.6;References;27
4.2;Lithium Isotopic Abundances in Old Stars;28
4.2.1;1 Introduction;28
4.2.2;2 Data and Analysis;29
4.2.3;3 Isotopic Abundance Ratios and Our Best Guess Fit;30
4.2.4;References;31
4.3;Accurate Quantitative Spectroscopy of OB Stars: the H, He and C Spectrum;33
4.3.1;1 Introduction;33
4.3.2;2 Model Calculations;34
4.3.3;3 Observations and Analysis;34
4.3.4;4 Results for the Programme Stars;34
4.3.5;5 Conclusions;36
4.3.6;References;36
4.4;High Resolution Spectroscopy of HgMn stars: A Time of Surprises;37
4.4.1;References;38
4.5;High-resolution Spectroscopy of Faint Stars with Transiting Planets;39
4.5.1;1 Introduction;39
4.5.2;2 Results;40
4.5.3;References;42
4.6;First Resolved Narrow Line Pro.les in Ultracool Dwarfs;43
4.6.1;1 Introduction;43
4.6.2;2 Zeeman Splitting;44
4.6.3;3 Very Slow Rotation – The Rising Part of the Rotation Activity Connection in M- dwarfs;44
4.6.4;References;46
4.7;Physical Parameters of Evolved Stars in Clusters and in the Field from Line- depth Ratios;47
4.7.1;1 Introduction;47
4.7.2;2 Star Samples;48
4.7.3;3 E.ective Temperature Determination;48
4.7.4;4 Color Excess of IC 4651;49
4.7.5;5 Conclusion;50
4.7.6;References;50
4.8;UVES and CRIRES Spectroscopy of AGB Stars: Technetium and the Third Dredge- up;52
4.8.1;1 Introduction;52
4.8.2;2 UVES Observations;53
4.8.3;3 CRIRES Observations;54
4.8.4;References;55
4.9;Characterisation of the Ursa Major Group;56
4.9.1;1 Introduction;56
4.9.2;2 Observations, Data Reduction and Analysis;56
4.9.3;3 Results and Discussion;57
4.9.4;4 Requests;58
4.9.5;5 Acknowledgements and Remarks;59
4.9.6;References;59
4.10;[C/O] Observations in Low-[Fe/H] Halo Stars;62
4.10.1;References;63
4.11;Oxygen Abundances in Metal-poor Stars, from [ OI], OI and IR OH Lines;64
4.11.1;1 Introduction;64
4.11.2;2 Observations;64
4.11.3;3 Analysis;64
4.11.4;4 Conclusions;65
4.11.5;References;67
4.12;Sulphur Abundances in Metal-poor Stars;68
4.12.1;1 Introduction;68
4.12.2;2 Observations of Sulphur Lines;68
4.12.3;3 Sulphur Abundances from UVES Spectra;69
4.12.4;4 Conclusions;70
4.12.5;References;71
4.13;Isotopic Abundances of Eu, Ba, and Sm in Metal- Poor Stars;72
4.13.1;1 Introduction;72
4.13.2;2 Observations and Analysis;72
4.13.3;3 Results;73
4.13.4;4 Conclusions;75
4.13.5;References;75
5;II QSO Absorption Lines;77
5.1;Gas-phase Deuterium Abundances, Near and Far;78
5.1.1;1 The Importance of Deuterium Abundances;78
5.1.2;2 Methods of Observing Atomic Deuterium;80
5.1.3;3 Lyman Series Absorptions;80
5.1.4;4 The Value of New Advances in Spectroscopy;83
5.1.5;References;83
5.2;Comprehensive Abundance Measurements in Damped Lya Systems;84
5.2.1;1 Introduction;84
5.2.2;2 Chemical Variations;85
5.2.3;3 Star Formation Histories;86
5.2.4;4 Future Prospects for DLAs with ELTs;87
5.2.5;References;87
5.3;Molecular Hydrogen at High Redshift and the Variation with Time of the Electron- to- proton Mass Ratio, µ = me/ mp;88
5.3.1;1 Introduction;88
5.3.2;2 High Metallicities and H2 Molecules;89
5.3.3;3 The Variation of µ;90
5.3.4;References;91
5.4;Spectroscopy of QSO Pairs;92
5.4.1;1 Introduction and Motivation;92
5.4.2;2 Absorber Sizes and Coherence Scales;93
5.4.3;3 The Properties of QSOs and Their Environments;96
5.4.4;References;97
5.5;Small-scale Structure of High-redshift OVI Absorption Systems;98
5.5.1;1 Outline and Results;98
5.5.2;References;99
5.6;Hot Halos around High-Redshift Galaxies;100
5.6.1;1 Introduction and Methods;100
5.6.2;2 Results and Conclusions;100
5.6.3;References;101
6;III Fundamental Constants;102
6.1;Astrophysical Probes of Fundamental Physics;103
6.1.1;1 Theoretical Expectations;103
6.1.2;2 From a and µ to w(z);104
6.1.3;3 Conclusions;106
6.1.4;Acknowledgments;108
6.1.5;References;108
6.2;Revisiting VLT/UVES Constraints on a Varying Fine- structure Constant;109
6.2.1;1 Introduction;109
6.2.2;2 A Simple Measure of the Limiting Precision on . a/ a;109
6.2.3;3 Application to Existing Constraints on . a/ a;111
6.2.4;4 Conclusion;112
6.2.5;References;113
6.3;On the Variation of the Fine-structure Constant, and Precision Spectroscopy;114
6.3.1;1 Limits on the Variation of a using UVES/VLT Data;114
6.3.2;2 . a/ a Measurement and Precise Spectroscopy;115
6.3.3;References;117
6.4;High-Precision Measurements of . a/ a from QSO Absorption Spectra;118
6.4.1;1 Introduction;118
6.4.2;2 Results;119
6.4.3;References;121
6.5;Probing Fundamental Constant Evolution with Redshifted OH Lines;122
6.5.1;1 Introduction;122
6.5.2;2 Radio OH Lines;122
6.5.3;3 Conjugate Behaviour of the Satellite OH Lines;123
6.5.4;4 NewWSRT Results;124
6.5.5;References;125
6.6;A Molecular Probe of Dark Energy;126
6.6.1;1 Introduction;126
6.6.2;2 The Concept;126
6.6.3;3 Major Advances;127
6.6.4;4 Improvements in the Present Analysis;128
6.6.5;5 Future Prospects;129
6.6.6;References;129
7;IV Beyond Photon Noise;130
7.1;Establishing Wavelength Standards in the near Infra- red: Th- Ar;131
7.1.1;1 Wavelength Calibration in the Near Infra-Red and the Th- Ar hollow cathode l131
7.1.2;2 Laboratory Work and Results;132
7.1.3;3 Additional Measurements;133
7.1.4;4 Summary;134
7.1.5;References;134
7.2;Atomic Data for Astrophysics - Parameters, Precision, Priorities;135
7.2.1;1 Introduction;135
7.2.2;2 Parameters;135
7.2.3;3 Energy Levels;136
7.2.4;4 Wavelengths;136
7.2.5;5 Oscillator Strengths;137
7.2.6;References;140
7.3;Optimal Extraction of Echelle Spectra;141
7.3.1;1 Introduction;141
7.3.2;2 Main Assumptions;141
7.3.3;3 Equations;141
7.3.4;4 Limitations, Generalization and Free Parameters;144
7.3.5;Reference;144
7.4;Hydrodynamical Model Atmospheres and 3D Spectral Synthesis;145
7.4.1;1 Radiation-hydrodynamics Modeling – Overview;145
7.4.2;2 High Precision Line Shifts from 3D Models?;146
7.4.3;3 3D Radiative Transfer in Metal-poor Atmospheres;148
7.4.4;4 3D Models and the Solar Oxygen Abundance;149
7.4.5;5 Remarks on Precision Spectroscopy and 3D Models;150
7.4.6;References;150
7.5;Intrinsic Lineshifts in Astronomical Spectra;151
7.5.1;1 Wavelength Shift vs. Radial Velocity;151
7.5.2;2 Convective Lineshifts in Stellar Photospheres;151
7.5.3;3 ‘Ultimate’ Information Content of Stellar Spectra;152
7.5.4;4 Wavelength Shifts from Intergalactic Convection;154
7.5.5;References;154
7.6;Study of Line Bisectors and its Relation with Precise Radial Velocities in the Search for Extrasolar Planets;155
7.6.1;1 Introduction;155
7.6.2;2 Analysis;155
7.6.3;3 Results;156
7.6.4;References;156
7.7;A Pan-Spectral Method of Abundance Determination;157
7.7.1;1 Description of the Method;157
7.7.2;2 Testing the Method;158
7.7.3;References;160
7.8;Spectroscopic Binary Mass Determination Using Relativity;161
7.8.1;1 Introduction;161
7.8.2;2 Single-Lined Spectroscopic Binary;161
7.8.3;3 Double-Lined Spectroscopic Binary;162
7.8.4;4 Discussion;163
7.8.5;References;164
7.9;Asteroseismology/Oscillations;165
7.10;Asteroseismology Across the HR Diagram;166
7.10.1;1 Introduction;166
7.10.2;2 Uncertainties in Stellar Structure and Evolution;168
7.10.3;3 Asteroseismic Constraints;169
7.10.4;4 Final Remarks;170
7.10.5;References;171
7.11;High-Precision Spectroscopy of Pulsating Stars;172
7.11.1;1 Line-Pro.le Variations due to Pulsations;172
7.11.2;2 Methodology for Line-Pro.le Analysis;173
7.11.3;3 Towards Lower Amplitudes;175
7.11.4;References;175
7.12;Mapping Atmospheric Motions in Classical and Type II Cepheids;176
7.12.1;1 Introduction;176
7.12.2;2 Observation and Data Reduction;176
7.12.3;3 Results;177
7.12.4;4 Simple Model Computation;178
7.12.5;5 Conclusions;179
7.12.6;References;179
7.13;Iron Abundances of Southern Double-mode Cepheids from High- resolution Echelle Spectroscopy;180
7.13.1;1 Introduction;180
7.13.2;2 Observations and Data Reduction;180
7.13.3;3 Results;181
7.13.4;References;183
8;V Planets;184
8.1;Radial Velocity Planet Detection using a Gas Absorption Cell;185
8.1.1;1 Introduction;185
8.1.2;2 Gas Absorption Cells as the Velocity Metric;186
8.1.3;3 Details of the Gas Cell Technique;186
8.1.4;4 Conclusions;190
8.1.5;References;190
8.2;Pushing Down the Limits of the Radial Velocity Technique;191
8.2.1;1 On the RV Precision of HARPS;191
8.2.2;2 Error Budget;193
8.2.3;3 A New ThAr Reference Atlas for Wavelength Calibration;193
8.2.4;4 Future Developments;194
8.2.5;References;194
8.3;Transiting Planets: Follow the FLAMES...;195
8.3.1;1 Introduction;195
8.3.2;2 Why a Spectroscopic Follow-up is Needed?;196
8.3.3;3 Main Results;197
8.3.4;4 Beyond the Follow-up;198
8.3.5;References;198
8.4;Planet Detection Around M Dwarfs: New Constraints on Planet Formation Models;200
8.4.1;1 Introduction;200
8.4.2;2 Planets Around M Dwarfs;201
8.4.3;3 Our HARPS and SOPHIE Programs;202
8.4.4;4 Habitability and Transits;203
8.4.5;References;204
8.5;Planets Around Giant Stars;206
8.5.1;1 Introduction;206
8.5.2;2 Properties of Planets Around Giant Stars;208
8.5.3;References;209
8.6;Planets Around Active Stars;210
8.6.1;1 Introduction;210
8.6.2;2 Observations;211
8.6.3;3 Stellar Activity;212
8.6.4;4 Planetary Companions and Future Works;212
8.6.5;References;213
8.7;A Catalogue of Nearby Exoplanets;214
8.7.1;1 Introduction;214
8.7.2;2 Data Reduction;215
8.7.3;References;215
8.8;Determination of the Orbital Parameters of a System with N + 1 Bodies using a Simple Fourier Analysis of the Data;216
8.8.1;1 Radial Velocity;216
8.8.2;2 Fourier Analysis;217
8.8.3;3 Conclusion;219
8.8.4;References;219
8.9;Extrasolar Comets;220
8.9.1;1 The Existence of Comets Around ß Pictoris;220
8.9.2;2 Solving the Stability of the Gaseous Disk;221
8.9.3;3 Two Families of Comets?;221
8.9.4;4 Conclusion;223
8.9.5;References;223
8.10;Measuring Winds in Titan’s Atmosphere with High- precision Doppler Velocimetry;224
8.10.1;1 Background;224
8.10.2;2 Observations;224
8.10.3;3 Analysis and Interpretation;225
8.10.4;References;227
9;VI Future Developments;228
9.1;The European Large Telescope and its Spectroscopic Instrumentation;229
9.1.1;1 The E-ELT Programme;229
9.1.2;2 Advantages of an ELT;230
9.1.3;3 Status of E-ELT Programme;231
9.1.4;4 Acknowledgements;234
9.1.5;References;234
9.2;CRIRES: A High Resolution Infrared Spectrograph for ESO’s VLT;235
9.2.1;1 Introduction;235
9.2.2;2 Main Characteristics of CRIRES;235
9.2.3;3 Example Spectra from Commissioning;237
9.2.4;4 Conclusions and Outlook;238
9.2.5;References;238
9.3;Stellar Oscillations Network Group: Asteroseismology and Planet Hunting;239
9.3.1;1 Introduction;239
9.3.2;2 Asteroseismology and Planets;239
9.3.3;3 Outline of SONG;240
9.3.4;4 Implementation;242
9.3.5;References;242
9.4;Interferometric Spectroscopy;243
9.4.1;1 Introduction;243
9.4.2;2 Astrophysics with Interferometric Spectroscopy;243
9.4.3;3 Implementation of Interferometric Spectroscopy;244
9.4.4;4 Conclusions;246
9.4.5;References;246
9.5;A Global Network of 2 m-class spectroscopic telescopes;247
9.5.1;1 Introduction;247
9.5.2;2 Network’s Sites;247
9.5.3;3 First Results;249
9.5.4;4 Conclusion;250
9.5.5;References;250
9.6;Possibility of Heterodyne Correlation Interferometry with a Tunable Laser and Absolute Frequency Measurements;251
9.6.1;1 Introduction;251
9.6.2;2 Astrophysical Lasers;251
9.6.3;3 Acknowledgements;253
9.6.4;References;253
9.7;CODEX;256
9.7.1;1 Why an Accurate H-R Spectrograph at ELT?;256
9.7.2;2 The CODEX Design;259
9.7.3;References;260
10;VII Posters;261
10.1;Precision Laboratory UV and IR Wavelengths for Cosmological and Astrophysical Applications;262
10.1.1;1 Introduction;262
10.1.2;2 Resonance UV Wavelengths for Cosmology;262
10.1.3;3 Parity Forbidden IR Wavelengths for Astrophysics;263
10.1.4;References;263
10.2;Abundance Analysis of a Centauri A;264
10.2.1;1 Introduction;264
10.2.2;2 The RHD Models, New [Fe/H] and Asteroseismology;264
10.2.3;References;265
10.3;The SB3 Star 74 Aqr: Abundances and Magnetic Field;266
10.3.1;1 The System;266
10.3.2;2 Magnetic Field;267
10.3.3;References;267
10.4;Nitrogen Isotope Ratios in Comets;268
10.4.1;References;269
10.5;Finding Stable Fits for Extrasolar Planetary Systems;271
10.5.1;References;271
10.6;Heavy Calcium in CP Stars: A New Isotopic Anomaly;273
10.6.1;1 Introduction;273
10.6.2;2 Details;273
10.6.3;References;274
10.7;The Li Abundance and the Age of AB Dor Association;275
10.7.1;1 Introduction;275
10.7.2;References;276
10.8;Si and Ca Abundances of a Selected Sample of Evolved Stars;277
10.8.1;1 Introduction;277
10.8.2;References;278
10.9;Abundance Trends with Condensation Temperature in Planet- harbouring Stars: Hints of Pollution?;279
10.9.1;1 Introduction;279
10.9.2;2 Results and Conclusions;280
10.10;Using the HeII Lya Forest to Constrain the Temperature of the IGM;281
10.10.1;1 Idea;281
10.10.2;2 Application to Data;282
10.10.3;References;282
10.11;Production of H+ 3 and D+ 3 from (CH3)2CO and (CD3)2CO in PDR’S;283
10.11.1;1 Introduction;283
10.11.2;2 Experimental Setup;283
10.11.3;3 Results and Discussion;284
10.11.4;References;285
10.12;Bisectors as Distance Estimators for Microquasars?;287
10.12.1;1 Scienti.c Context;287
10.12.2;2 New Exploratory Method to Obtain Distance Estimate;287
10.12.3;3 Known Caveats and Prospects;288
10.12.4;References;288
10.13;Metallicity of Pleiades Dwarf;289
10.13.1;1 Introduction;289
10.13.2;2 Observation and Results;290
10.13.3;References;290
10.14;Precision of Radial Velocity Surveys using Multiobject Spectrographs – Experiences with Hectochelle;291
10.14.1;1 The Hectochelle Instrument;291
10.14.2;2 The Multiobject Advantage — and Drawback;291
10.14.3;3 Key: Continuous Calibration and Optimal Extraction;292
10.14.4;References;293
10.15;High Resolution Study of the Young Quadruple System AOVel with an Eclipsing BpSi Primary;295
10.15.1;1 Introduction;295
10.15.2;2 Observations and Spectral Analysis;295
10.15.3;3 Results;295
10.15.4;References;296
10.16;A Survey for Extrasolar Planets Around A–F Type Stars;297
10.16.1;1 Introduction;297
10.16.2;2 Monitored Sample and Observations;297
10.16.3;3 The New Planet;298
10.16.4;4 Conclusions;298
10.16.5;References;298
10.17;A Study of the Magnetic Helium Variable Emission- line Star HD125823.;299
10.17.1;References;300
10.18;bHROS: The High-Resolution Optical Spectrograph at Gemini South;301
10.19;Stellar Wobble Caused by a Binary System: Investigation in the Framework of the General Three Body Problem;303
10.19.1;1 The Problem;303
10.19.2;2 Our Work - Some Results;303
10.19.3;3 Conclusion;304
10.19.4;References;304
10.20;The Chemical Composition of B-type Pulsators: Some Unexpected Results;305
10.20.1;1 B-type Pulsators and the Rationale of the Project;305
10.20.2;2 Nitrogen Excess in Slowly-rotating;306
10.20.3;Cephei Stars:;306
10.20.4;Deep Mixing or Di.usion?;306
10.20.5;3 Future Developments;306
10.20.6;References;306
10.21;Radial Velocity Precision in the Near-Infrared with T- EDI;307
10.21.1;1 The T-EDI Instrument;307
10.21.2;2 Photon-limited Radial Velocity Precision;308
10.21.3;References;308
10.22;HD154708 - The Challenging Abundance Analysis of an Extremely Magnetic Star;309
10.22.1;1 Observations;309
10.22.2;2 Abundance analysis;309
10.22.3;References;310
10.23;A Search for Disk-Locking in the Chamaeleon I Star Forming Region;311
10.23.1;1 Introduction;311
10.23.2;2 Observations and Analysis;311
10.23.3;References;312
10.24;A Precision Radial Velocity Survey of Red Giants;313
10.24.1;1 Motivation and Observations;313
10.24.2;2 The Survey;314
10.24.3;Acknowledgements;314
10.24.4;References;314
10.25;Chromospheric Lines as Diagnostics of Stellar Oscillations;315
10.25.1;1 Background;315
10.25.2;2 Observations;315
10.25.3;3 Conclusions;316
10.25.4;References;316
10.26;Comparing 3D Solar Model Atmospheres with Observations: Hydrogen Lines and Centre- to- limb Variations;317
10.26.1;References;318
10.27;Towards the Detection of Re.ected Light from Exo- planets: a Comparison of Two Methods;319
10.27.1;1 Introduction;319
10.27.2;2 Simulation and Conclusion;319
10.27.3;References;320
10.28;A Correlation Between the Activity Level and the Radial- velocity for Solar- type Stars?*;321
10.28.1;1 Introduction;321
10.28.2;2 Observations and Preliminary Results;321
10.28.3;References;322
10.29;Spectroscopic Parameters for a Sample of Metal- rich Solar- type Stars;323
10.29.1;1 Motivation;323
10.29.2;2 A New Sample of Metal-rich Stars;323
10.29.3;References;324
10.30;Radial Velocity Search for Extrasolar Planets in Binary Systems;325
10.30.1;1 Introduction;325
10.30.2;2 Observation and Our Target Stars;325
10.30.3;References;326
10.31;Inferring Photospheric Velocities from P Cygni Lines in Type IIP Supernova Atmospheres;327
10.31.1;1 Introduction;327
10.31.2;2 Model Computations;327
10.31.3;3 Results;328
10.31.4;References;328
10.32;High-resolution Spectroscopic Characterization of Young Stars;329
10.32.1;References;330
10.33;TIRAVEL – Template Independent RAdial VELocity Measurement;331
10.33.1;1 Introduction;331
10.33.2;2 TIRAVEL;331
10.33.3;3 Real Test Cases;332
10.33.4;4 Summary;332
10.33.5;References;332