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A Search and Discovery of Ultra Compact Dwarf Galaxies

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A Search and Discovery of Ultra Compact Dwarf Galaxies A SEARCH AND DISCOVERY OF ULTRA COMPACT DWARF GALAXIES A Thesis submitted to the faculty of San Francisco State University In partial fulfillment of | the requirements for fyyf the Degree Master of Science In Physics by Russell George Lego San Francisco, California August 2019 Copyright by Russell George Lego 2019 A Search and Discovery of Ultra Compact Dwarf Galaxies Russell George Lego San Francisco, California 2019 A search for an uncommon class of compact stellar systems called Ultra Compact Dwarf Galaxies was carried out. Using data in the visual wavelength band from the Sloan Digital Sky Survey and in the infrared band from UKIRT Infrared Deep Sky Survey, a small subset of potential candidates to spectroscopically confirm was conceived. A proposal for one night of study using the 4-meter Mayall Telescope was submitted and accepted. The observation run was carried out under severe wind conditions that resulted in only enough time for 2 targets to be observed. Spectra were extracted and redshifits were obtained for both targets. The inferred distance associated with each target’s radial velocity confirmed their small physical size as being part of the UCD class. In this paper I present the work involved in the process from the conception of the idea to start the search to the observation run and analysis thereafter. I certify that the Abstract is a correct representation of the content of this thesis. Chair, Thesis Committee PREFACE AND/OR ACKNOWLEDGEMENTS I would like to take this opportunity to thank a certain few people who have helped me immensely during this process. First to Dr. Ron Marzke for taking me under his academic wing and showing me what it means to do professional Astronomy. Second to Dr. Joe Barranco for first inspiring me to switch my major to Physics and his faith that I could actually do it. Next to Dr. Adrienne Cool for motivating me into the field of Astronomy with her wonderful lectures, guidance, and hands-on use of Leuschner Observatory. To Dr. Barbara Neuhauser, for her countless hours spent explaining how the computers we use every day actually work. To Dr. Susan Lea for sharpening my mind in ways and directions I never thought I could go and building in me a fortitude to persevere. v TABLE OF CONTENTS List of Tables..........................................................................................................................viii List of Figures...........................................................................................................................ix List of Appendices........................... x Introduction.................................................................................................................................1 What are Ultra Compact Dwarfs?............................................................................... 1 Why are they important? ................................................................................2 Formation hypothesis...................................................................................................2 Tidal Interaction ..............................................................................................3 Primordial Dwarf Galaxies .............................................................................4 Super Cluster Mergers ....................................................................................6 More Luminous Globular Clusters ................................................................7 Method: Search for Candidates.................................................................................................9 Beginning the Search: Volume, Brightness, and the Low-Z Catalog....................10 Star Galaxy Separation ..............................................................................................13 Data Retrieval .............................................................................................................17 Candidate Selection ................................................................................................... IB Results.......................................................................................................................................22 Observations at Kitt Peak National Observatory....................... 22 Analysis With IRAF...................................................................................................23 Combining Images......................................................................................... 24 Overscan, Bias, and Trimming..................................................................... 25 Flat Fielding................... 27 Extracting and Calibrating Spectra...............................................................28 Obtaining Radial Velocity and Redshifit...................................................... 34 Discussion and Conclusion...................................................................... 36 Reference ..................... 39 Appendices............................................................................................................................... 42 KPNO Proposal........................................... 42 Sample of Data Retrieval Technique........................................................................ 49 Confirming the Source............................... 55 LIST OF TABLES Table Page 1. SDSS Properties of Observed Targets..........................................................36 2. Measured Properties from Observation........................................................37 LIST OF FIGURES Figures Page 1. Number of Objects vs. R-Band Magnitude.......................................................11 2. G-R vs I-Z Color - Color Diagram............................................. 14 3. Star Galaxy Separation with Increasing Wavelength.......................................16 4. Region of Interest for UCD Candidates............................................................ 18 5. Density Contour Plot in Color - Color Space...................................................19 6. UCD candidates found using Hubble Space Telescope.................................. 21 7. Raw Spectra Images for Both Candidates.........................................................24 8. Overscan Region of Flat Field Image................................................................26 9. Final Flat Field Image..................... 27 10. IRAF Aperture Editor and Wavelength Calibrated Spectrum.........................39 11. Raw and Extracted Lamp Spectrum..................... *........................................... 31 12. Wavelength Calibrated Spectra for Both Candidates.......................................32 13. Flux Calibrated Spectrum for M l04 Candidate............................................... 33 14. Radial Velocity Measurement for both Candidates.........................................35 15. SDSS Footprint Around M l04...........................................................................57 ix LIST OF APPENDICES Appendix Page 1. KPNO Proposal....................................................................................................42 2. Sample of Data Retrieval Technique..................................................................49 3. Confirming the M104 Target...............................................................................55 1 1. Introduction a. What are Ultra Compact Dwarfs Ultra Compact dwarfs are stellar systems that contain considerably more stars than globular clusters but have a significantly smaller physical size than a compact elliptical galaxy. They were first discovered neighboring large massive galaxies in the Fornax Cluster (Hilker et al 1999, Drinkwater et al 2000) and are thought to be a new class of objects instead of exceptions to the rule (Phillipps et al 2001). Modern advancements in telescopes, CCD’s, and spectrographs have allowed astronomers to looker deeper and more clearly at the observable universe. The prior constraints that came with imaging the night sky has been shown to preferentially discover objects of certain types while excluding others, especially objects with high surface brightness, low luminosity, and small angular size (Disney and Phillipps 1983). With photometric surveys now utilizing the CCD’s ability to push further down through the background noise of the sky, spectroscopic surveys have been constructed out of this data and new objects are being discovered (Marzke et al 2010.) Among the new discoveries are UCD’s. 2 b. Why Are they So Important? UCD’s make up an important topic for study because they represent a new type of galaxy class and only the second new class to be discovered since 1938 when Harlow Shapley classified the dwarf spheroidal. They also occupy a region in magnitude-size space that is relatively uninhabited by sources of any kind. This gap was originally explained by the assumption that there were just no objects that possessed these types of properties. Under more careful examination it has been shown that there exist objects that do indeed occupy this region but were being missed by large-scale sky surveys because of the algorithms used for spectroscopic targeting. Now that this problem has been addressed, the discoveries of new stellar systems will play an important role in astronomy for years to come. Currently there are under 100 UCD’s found throughout the universe which makes them an extremely rare source of interest, even more so than exo-planets, by orders of magnitude. c. Formation Hypotheses The several
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