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Observing CO in Circumstellar Disks Matthew Rt Outman Clemson University, [email protected]

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Observing CO in Circumstellar Disks Matthew Rt Outman Clemson University, Mtroutm@Clemson.Edu Clemson University TigerPrints All Dissertations Dissertations 8-2010 Observing CO in Circumstellar Disks Matthew rT outman Clemson University, [email protected] Follow this and additional works at: https://tigerprints.clemson.edu/all_dissertations Part of the Astrophysics and Astronomy Commons Recommended Citation Troutman, Matthew, "Observing CO in Circumstellar Disks" (2010). All Dissertations. 603. https://tigerprints.clemson.edu/all_dissertations/603 This Dissertation is brought to you for free and open access by the Dissertations at TigerPrints. It has been accepted for inclusion in All Dissertations by an authorized administrator of TigerPrints. For more information, please contact [email protected]. OBSERVING CO IN CIRCUMSTELLAR DISKS A Dissertation Presented to the Graduate School of Clemson University In Partial Fulfillment of the Requirements for the Degree Doctorate of Philosophy Physics by Matthew R. Troutman May 2010 Accepted by: Dr. Sean D. Brittain, Committee Chair Dr. Jeremy King Dr. Mark D. Leising Dr. Bradley Meyer ABSTRACT This dissertation includes high-resolution, near-infrared spectroscopy to study CO in circumstellar disks around Herbig Ae/Be stars. The velocity-resolved spectra was used to measure the distribution of gas in the circumstellar disk and thus determine the evolutionary state of the system. Near-infrared spectra were obtained on over 30 young circumstellar disks around Herbig Ae/Be stars to study the physical processes in the disk. The radial location of the CO emitting gas bears directly on the evolutionary state of the transition objects in the sample. This study included a detailed study of the debris disk star β Pictoris where the disk mass was estimated. The study found that CO is detected in most disks, yet there were no systems showing evidence for the grain growth scenario of planet formation. In addition, by using high-resolution spectra of the fundamental ro-vibrational CO emission lines, one can measure the position centroid of the emission as a function of velocity to provide an independent measurement of M1/2sin(i) and the disk inclination. Knowing the inclination is crucial for determining the radial distribution of gas inferred by other high-resolution spectra using low spatial resolution instruments such as the Heterodyne Instrument for the Far Infrared on Herschel. Perhaps most importantly, by measuring the position centroid of the emission, one can determine where in the disk the CO emitting gas arises independent of assumptions about the disk velocity field, Keplerian or otherwise. This analysis was performed on HD 100546, where asymmetric emission is observed. The results also provide a fundamental test of our fluorescence emission model, which allows our model to infer the CO emission radii in systems that are too distant to spatially resolve the emission. ii ACKNOWLEDGEMENTS I would like to first acknowledge my advisor, Dr. Sean Brittain. Thanks in the help over the years to get here. I also wish to acknowledge the other members of my knowledgeable committee: Dr. Jeremy King, Dr. Mark Leising, and Dr. Bradley Meyer. Thanks for the comments, support, and very helpful questions along the way. I would also like to thank the other faculty members that have helped me through graduate school. I’ve enjoyed the many conversations and extremely appreciate their sup- port. Thank you also to the other students in our group: Joe Liskowksy and Brian Donehew. This work was performed under contract with the Jet Propulsion Laboratory (JPL) funded by NASA through the Michelson Fellowship Program. JPL is managed for NASA by the California Institute of Technology. This dissertation is primarily based on observations obtained at the Gemini Ob- servatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the Particle Physics and Astronomy Research Council (United Kingdom), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), CNPq (Brazil) and CONICET (Argentina). The NIRSPEC data shown were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the Univer- sity of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. The dissertation is also based on observations obtained at the Infrared Telescope Facility, which is operated by the University of Hawaii under Cooperative Agreement no. NCC 5-538 with the National Aeronautics and Space Administration, Science Mission Di- rectorate, Planetary Astronomy Program. iii TABLE OF CONTENTS Page TITLEPAGE ....................................... i ABSTRACT ........................................ ii ACKNOWLEDGMENTS ................................. iii LISTOFTABLES..................................... vi LISTOFFIGURES .................................... vii 1. INTRODUCTION ................................ 1 1.1 ObservingtheGas.............................. 4 1.1.1 COasaTracer ........................... 5 1.2 DisksAroundHerbigAe/BeStars . 6 1.2.1 DebrisDisks............................. 7 1.2.2 TransitionalDisks.......................... 8 1.3 Summary................................... 8 1.3.1 Collisional Excitation . 9 1.3.2 SpectralSynthesis. .. .. .. .. .. .. .. 10 1.3.3 Spectro-astrometry . 10 2. COEXCITATIONANALYSIS. 14 2.1 Collisional Excitation in Disks . 14 2.1.1 LTE/NLTE ............................. 14 2.1.2 Collision Partners and Rates . 15 2.2 The Study of β Pictoris........................... 15 2.2.1 Observations............................. 17 2.2.2 Results................................ 20 2.2.3 Analysis ............................... 24 2.2.4 Discussion .............................. 34 3. HERBIGAE/BESURVEY ........................... 37 3.1 Observations................................. 39 3.2 Results.................................... 39 3.2.1 K-L ................................. 46 3.2.2 MeeusGroups............................ 49 3.2.3 PAHs................................. 49 3.2.4 Br γ ................................. 51 3.2.5 Pf β ................................. 53 3.2.6 Age.................................. 54 3.2.7 HD 97048 and HD 169142 . 54 3.2.8 HD 100453 and HD 158352 . 56 iv Table of Contents (Continued) Page 3.2.9 HD139614.............................. 56 3.2.10 HD142666.............................. 56 3.2.11 PDS144N .............................. 56 3.3 Discussion .................................. 56 3.4 ConclusionofSurvey ............................ 58 3.5 SpectraofSurveySources ......................... 59 3.6 ObjectDataSummaryandReferences . 82 4. SPECTRO-ASTROMETRY .. .. .. .. .. .. .. .. 89 4.1 Spectro-astrometryModel . 89 4.2 Spectro-astrometry of HD 100546 . 89 4.3 Observations................................. 90 4.4 Analysis ................................... 91 4.5 Results.................................... 94 4.5.1 Modeling the Flux and Spectro-astrometry . 100 4.5.2 EffectofaSpiralArm ....................... 101 4.5.3 IntroducingaPlanet . 106 4.5.4 Summary............................... 109 5. SUMMARY .................................... 111 5.1 CollisionalExcitation . 111 5.2 SurveyData ................................. 111 5.3 Spectro-astrometry as a Technique . 112 5.3.1 OtherTracers ............................ 112 5.3.2 Asymmetries............................. 113 APPENDIX......................................... 114 BIBLIOGRAPHY ..................................... 122 v LIST OF TABLES Table Page 2.1 β Pictoris: LogofObservations . 19 2.2 β Pictoris:LineFluxes............................... 23 3.1 Herbig Ae/Be Survey: Log of Observations . ...... 40 3.2 HerbigAe/BeSurvey: DiskSummary . 42 3.3 Herbig Ae/Be Survey: PAH Observations . ..... 45 4.1 HD 100546: Log of Observations . 90 4.2 HD100546: Unblended Lines . 97 vi LIST OF FIGURES Figure Page 1.1 DiskEvolution ................................... 2 1.2 TransitionalDiskScenarios . ..... 9 1.3 DiskVelocityandLineFlux. 11 1.4 Disk Velocity and Spectro-astrometric Signal . .......... 12 1.5 SpectrogramofCOFeature . .. .. .. .. .. .. .. 13 2.1 β Pictoris: AbsorptionSpectrum . 21 2.2 β Pictoris: Non-detection of Emission . 22 2.3 β Pictoris:DiagramofSystem . .. .. .. .. .. .. .. 25 2.4 β Pictoris:ExcitationPlot. 27 2.5 β Pictoris: Chi-squared of H2O.......................... 31 2.6 β Pictoris:Chi-squaredofH. 33 2.7 β Pictoris: ModelComparisons . 34 3.1 Survey:CODetectionRatebyK-L. 47 3.2 Survey:COLuminosityvs.K-L . 48 3.3 Survey: CO Detection Rate by Meeus Group . 50 3.4 Survey: CO Detection Rate by PAH Emission . ..... 51 3.5 Survey: CO Luminosity vs. 3.3 µmPAHLuminosity . 52 3.6 Survey: CO Luminosity vs. 6.2 µmPAHLuminosity . 52 3.7 Survey: CO Luminosity vs. Brγ Luminosity................... 53 3.8 Survey: CO Detection Rate by Pf β ....................... 54 3.9 Survey: CO Detection Rate by Age . 55 3.10 Survey:COOri................................... 59 3.11 Survey:GWOri .................................. 60 3.12 Survey:TOri.................................... 61 3.13 Survey:V380Ori................................. 62 vii List of Figures (Continued) Figure Page 3.14 Survey:HD37357 ................................. 62 3.15 Survey:HD37806 ................................. 63 3.16 Survey:HD38678 ................................. 63 3.17 Survey:HD49662
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