Raman Microspectroscopic Imaging and Multivariate Analysis to Investigate the Chemical Properties of Novel Geological and Planetary Materials
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Imaginative Geographies of Mars: the Science and Significance of the Red Planet, 1877 - 1910
Copyright by Kristina Maria Doyle Lane 2006 The Dissertation Committee for Kristina Maria Doyle Lane Certifies that this is the approved version of the following dissertation: IMAGINATIVE GEOGRAPHIES OF MARS: THE SCIENCE AND SIGNIFICANCE OF THE RED PLANET, 1877 - 1910 Committee: Ian R. Manners, Supervisor Kelley A. Crews-Meyer Diana K. Davis Roger Hart Steven D. Hoelscher Imaginative Geographies of Mars: The Science and Significance of the Red Planet, 1877 - 1910 by Kristina Maria Doyle Lane, B.A.; M.S.C.R.P. Dissertation Presented to the Faculty of the Graduate School of The University of Texas at Austin in Partial Fulfillment of the Requirements for the Degree of Doctor of Philosophy The University of Texas at Austin August 2006 Dedication This dissertation is dedicated to Magdalena Maria Kost, who probably never would have understood why it had to be written and certainly would not have wanted to read it, but who would have been very proud nonetheless. Acknowledgments This dissertation would have been impossible without the assistance of many extremely capable and accommodating professionals. For patiently guiding me in the early research phases and then responding to countless followup email messages, I would like to thank Antoinette Beiser and Marty Hecht of the Lowell Observatory Library and Archives at Flagstaff. For introducing me to the many treasures held deep underground in our nation’s capital, I would like to thank Pam VanEe and Ed Redmond of the Geography and Map Division of the Library of Congress in Washington, D.C. For welcoming me during two brief but productive visits to the most beautiful library I have seen, I thank Brenda Corbin and Gregory Shelton of the U.S. -
General Vertical Files Anderson Reading Room Center for Southwest Research Zimmerman Library
“A” – biographical Abiquiu, NM GUIDE TO THE GENERAL VERTICAL FILES ANDERSON READING ROOM CENTER FOR SOUTHWEST RESEARCH ZIMMERMAN LIBRARY (See UNM Archives Vertical Files http://rmoa.unm.edu/docviewer.php?docId=nmuunmverticalfiles.xml) FOLDER HEADINGS “A” – biographical Alpha folders contain clippings about various misc. individuals, artists, writers, etc, whose names begin with “A.” Alpha folders exist for most letters of the alphabet. Abbey, Edward – author Abeita, Jim – artist – Navajo Abell, Bertha M. – first Anglo born near Albuquerque Abeyta / Abeita – biographical information of people with this surname Abeyta, Tony – painter - Navajo Abiquiu, NM – General – Catholic – Christ in the Desert Monastery – Dam and Reservoir Abo Pass - history. See also Salinas National Monument Abousleman – biographical information of people with this surname Afghanistan War – NM – See also Iraq War Abousleman – biographical information of people with this surname Abrams, Jonathan – art collector Abreu, Margaret Silva – author: Hispanic, folklore, foods Abruzzo, Ben – balloonist. See also Ballooning, Albuquerque Balloon Fiesta Acequias – ditches (canoas, ground wáter, surface wáter, puming, water rights (See also Land Grants; Rio Grande Valley; Water; and Santa Fe - Acequia Madre) Acequias – Albuquerque, map 2005-2006 – ditch system in city Acequias – Colorado (San Luis) Ackerman, Mae N. – Masonic leader Acoma Pueblo - Sky City. See also Indian gaming. See also Pueblos – General; and Onate, Juan de Acuff, Mark – newspaper editor – NM Independent and -
ROSS T. SHINYAMA #8830-0 SUMMER II. Kaiawtr I+9599-O First L-Lawaiian Center 999 Bishop Street, 23Rd Floor
WATANABI] ING I-LP A Limited Liability [,aw Parrnership ":r : , 1 I ' I J. DOUGLAS ING #1538-0 i.,,i l i t I i '.tì ROSS T. SHINYAMA #8830-0 SUMMER II. KAIAWtr I+9599-O First l-lawaiian Center 999 Bishop Street, 23rd Floor Honolulu, Ilawaii 968 1 3 Telephone No.: (808) 544-8300 Facsimile No.: (808) 544-8399 E-mails : [email protected] Attorneys for TMT INTBRNATIONAL OBSBRVATORY, I,LC BOARD OF LAND AND NATURAL RESOURCES FOR THE STATE OF I]AWAI'I IN THE MATTER OF Case No. BLNR-CC -16-002 TMT INTERNATIONAL A Contested Case l{earing Re Conservation OBSBRVATORY, LLC'S PRE-HEARING District Use Permit (CDUP) I{A-3568 for the STATEMENT; EXHIBIT ..1,'; Thirty Meter Telescope at the Mauna Kea CERTIFICATE OF SERVICE Science Reserve, I(a'ohe Mauka, Hãmakua District, Island of Hawai'i, TMK (3) 4-4- 0l 5:009 TABLtr OF CONTBNTS IN'IRODUC]'ION II DI]SCRIPI'ION OF THE PROJECT AND ITS PROCI]DURAL HISTORY A. Description ofthe Project.................. 3 B. Procedulal Llistory 3 l. General Lease and the MI(SR 3 2. T'he Project 5 III. BURDEN OF PROOF I IV. ISSUES TO BE DECIDED AND TIO'S STATEMENT OF POSI'|iON.. A. The Project, Including the Plans Incorporatcd in the Application, is Consistent with Chapter 183C of the Hawai'i Revised Statutes, the Criteria in HAR $ 13-5- 30(c), and Other Applicable Conservation District Rules......... ..........9 i. The Project is consistent with the purpose of the Conservation District.. 10 2. The Project is consistent with the objectives of the sub2one................... -
Martian Crater Morphology
ANALYSIS OF THE DEPTH-DIAMETER RELATIONSHIP OF MARTIAN CRATERS A Capstone Experience Thesis Presented by Jared Howenstine Completion Date: May 2006 Approved By: Professor M. Darby Dyar, Astronomy Professor Christopher Condit, Geology Professor Judith Young, Astronomy Abstract Title: Analysis of the Depth-Diameter Relationship of Martian Craters Author: Jared Howenstine, Astronomy Approved By: Judith Young, Astronomy Approved By: M. Darby Dyar, Astronomy Approved By: Christopher Condit, Geology CE Type: Departmental Honors Project Using a gridded version of maritan topography with the computer program Gridview, this project studied the depth-diameter relationship of martian impact craters. The work encompasses 361 profiles of impacts with diameters larger than 15 kilometers and is a continuation of work that was started at the Lunar and Planetary Institute in Houston, Texas under the guidance of Dr. Walter S. Keifer. Using the most ‘pristine,’ or deepest craters in the data a depth-diameter relationship was determined: d = 0.610D 0.327 , where d is the depth of the crater and D is the diameter of the crater, both in kilometers. This relationship can then be used to estimate the theoretical depth of any impact radius, and therefore can be used to estimate the pristine shape of the crater. With a depth-diameter ratio for a particular crater, the measured depth can then be compared to this theoretical value and an estimate of the amount of material within the crater, or fill, can then be calculated. The data includes 140 named impact craters, 3 basins, and 218 other impacts. The named data encompasses all named impact structures of greater than 100 kilometers in diameter. -
“Mining” Water Ice on Mars an Assessment of ISRU Options in Support of Future Human Missions
National Aeronautics and Space Administration “Mining” Water Ice on Mars An Assessment of ISRU Options in Support of Future Human Missions Stephen Hoffman, Alida Andrews, Kevin Watts July 2016 Agenda • Introduction • What kind of water ice are we talking about • Options for accessing the water ice • Drilling Options • “Mining” Options • EMC scenario and requirements • Recommendations and future work Acknowledgement • The authors of this report learned much during the process of researching the technologies and operations associated with drilling into icy deposits and extract water from those deposits. We would like to acknowledge the support and advice provided by the following individuals and their organizations: – Brian Glass, PhD, NASA Ames Research Center – Robert Haehnel, PhD, U.S. Army Corps of Engineers/Cold Regions Research and Engineering Laboratory – Patrick Haggerty, National Science Foundation/Geosciences/Polar Programs – Jennifer Mercer, PhD, National Science Foundation/Geosciences/Polar Programs – Frank Rack, PhD, University of Nebraska-Lincoln – Jason Weale, U.S. Army Corps of Engineers/Cold Regions Research and Engineering Laboratory Mining Water Ice on Mars INTRODUCTION Background • Addendum to M-WIP study, addressing one of the areas not fully covered in this report: accessing and mining water ice if it is present in certain glacier-like forms – The M-WIP report is available at http://mepag.nasa.gov/reports.cfm • The First Landing Site/Exploration Zone Workshop for Human Missions to Mars (October 2015) set the target -
March 21–25, 2016
FORTY-SEVENTH LUNAR AND PLANETARY SCIENCE CONFERENCE PROGRAM OF TECHNICAL SESSIONS MARCH 21–25, 2016 The Woodlands Waterway Marriott Hotel and Convention Center The Woodlands, Texas INSTITUTIONAL SUPPORT Universities Space Research Association Lunar and Planetary Institute National Aeronautics and Space Administration CONFERENCE CO-CHAIRS Stephen Mackwell, Lunar and Planetary Institute Eileen Stansbery, NASA Johnson Space Center PROGRAM COMMITTEE CHAIRS David Draper, NASA Johnson Space Center Walter Kiefer, Lunar and Planetary Institute PROGRAM COMMITTEE P. Doug Archer, NASA Johnson Space Center Nicolas LeCorvec, Lunar and Planetary Institute Katherine Bermingham, University of Maryland Yo Matsubara, Smithsonian Institute Janice Bishop, SETI and NASA Ames Research Center Francis McCubbin, NASA Johnson Space Center Jeremy Boyce, University of California, Los Angeles Andrew Needham, Carnegie Institution of Washington Lisa Danielson, NASA Johnson Space Center Lan-Anh Nguyen, NASA Johnson Space Center Deepak Dhingra, University of Idaho Paul Niles, NASA Johnson Space Center Stephen Elardo, Carnegie Institution of Washington Dorothy Oehler, NASA Johnson Space Center Marc Fries, NASA Johnson Space Center D. Alex Patthoff, Jet Propulsion Laboratory Cyrena Goodrich, Lunar and Planetary Institute Elizabeth Rampe, Aerodyne Industries, Jacobs JETS at John Gruener, NASA Johnson Space Center NASA Johnson Space Center Justin Hagerty, U.S. Geological Survey Carol Raymond, Jet Propulsion Laboratory Lindsay Hays, Jet Propulsion Laboratory Paul Schenk, -
Chemical and Isotopic Studies of Monogenetic Volcanic Fields: Implications for Petrogenesis and Mantle Source Heterogeneity
MIAMI UNIVERSITY The Graduate School Certificate for Approving the Dissertation We hereby approve the Dissertation of Christine Rasoazanamparany Candidate for the Degree DOCTOR OF PHILOSOPHY ______________________________________ Elisabeth Widom, Director ______________________________________ William K. Hart, Reader ______________________________________ Mike R. Brudzinski, Reader ______________________________________ Marie-Noelle Guilbaud, Reader ______________________________________ Hong Wang, Graduate School Representative ABSTRACT CHEMICAL AND ISOTOPIC STUDIES OF MONOGENETIC VOLCANIC FIELDS: IMPLICATIONS FOR PETROGENESIS AND MANTLE SOURCE HETEROGENEITY by Christine Rasoazanamparany The primary goal of this dissertation was to investigate the petrogenetic processes operating in young, monogenetic volcanic systems in diverse tectonic settings, through detailed field studies, elemental analysis, and Sr-Nd-Pb-Hf-Os-O isotopic compositions. The targeted study areas include the Lunar Crater Volcanic Field, Nevada, an area of relatively recent volcanism within the Basin and Range province; and the Michoacán and Sierra Chichinautzin Volcanic Fields in the Trans-Mexican Volcanic Belt, which are linked to modern subduction. In these studies, key questions include (1) the role of crustal assimilation vs. mantle source enrichment in producing chemical and isotopic heterogeneity in the eruptive products, (2) the origin of the mantle heterogeneity, and (3) the cause of spatial-temporal variability in the sources of magmatism. In all three studies it was shown that there is significant compositional variability within individual volcanoes and/or across the volcanic field that cannot be attributed to assimilation of crust during magmatic differentiation, but instead is attributed to mantle source heterogeneity. In the first study, which focused on the Lunar Crater Volcanic Field, it was further shown that the mantle heterogeneity is formed by ancient crustal recycling plus contribution from hydrous fluid related to subsequent subduction. -
Alluvial Fans As Potential Sites for Preservation of Biosignatures on Mars
Alluvial Fans as Potential Sites for Preservation of Biosignatures on Mars Phylindia Gant August 15, 2016 Candidate, Masters of Environmental Science Committee Chair: Dr. Deborah Lawrence Committee Member: Dr. Manuel Lerdau, Dr. Michael Pace 2 I. Introduction Understanding the origin of life Life on Earth began 3.5 million years ago as the temperatures in the atmosphere were cool enough for molten rocks to solidify (Mojzsis et al 1996). Water was then able to condense and fall to the Earth’s surface from the water vapor that collected in the atmosphere from volcanoes. Additionally, atmospheric gases from the volcanoes supplied Earth with carbon, hydrogen, nitrogen, and oxygen. Even though the oxygen was not free oxygen, it was possible for life to begin from the primordial ooze. The environment was ripe for life to begin, but how would it begin? This question has intrigued humanity since the dawn of civilization. Why search for life on Mars There are several different scientific ways to answer the question of how life began. Some scientists believe that life started out here on Earth, evolving from a single celled organism called Archaea. Archaea are a likely choice because they presently live in harsh environments similar to the early Earth environment such as hot springs, deep sea vents, and saline water (Wachtershauser 2006). Another possibility for the beginning of evolution is that life traveled to Earth on a meteorite from Mars (Whitted 1997). Even though Mars is anaerobic, carbonate-poor and sulfur rich, it was warm and wet when Earth first had organisms evolving (Lui et al. -
ROSS T. SHTNYAMA #8830-0 Li;Ij
s23820 WATANABE ING LLP A Limited Liability Law Partnership li;ij ,ji,,'ì j-1 ir i J. DOUGLAS ING #1.538-0 BRIAN A. KANG #6495.0 ROSS T. SHTNYAMA #8830-0 SUMMER H. KAIAWE #9599-0 First Hawaiian Center 999 Bishop Street, 23rd Floor Honolulu, Hawaii96813 Telephone No.: (808) 544-8300 Facsimile No.: (S08) 544-8399 E-mails: [email protected] Attorneys for TMT I NTERNATIONAL OBSERVATORY, LLC BOARD OF LAND AND NATURAL RESOURCES FOR TI-IE STATE OF HAWAI'I IN THE MATTER OF , Case No. BLNR-CC-16-002 TMT INTERNATIONAL OBSERVATORY, LLC'S A Contested Case Hearing Re Csnservation IFOU'RT|{ AMENDED EXHIBIT LIST and Distríct Use Permit (CDUP) HA-3568 forthe ADDITIONAL EXHIBIT C-40; CERTIFICATE OF Thirty Meter Telescope at the Mauna Kea SERVICE Science Reserve, Kaohe Mauka, Hamaku Distrrict, lsland of Hawaii, TMK (3) 4-4'OL5 PARTY: TMT INTERNATIONAL OBSERVATORY, LLC Received Exhibit No Description lnto Evidence c-1 Testimony of Ed Stone c-2 Testimony of Gary Sanders Received Exhibit No. Description lnto Evidence Graphic showing Mitigation Measures Reduce Size and Visibility of c-3 TMT c-4 Testimony of Mike Bolte New York Times article: From Hawaii's Mauna Kea, A Universe of ' c-5 Discoveries (October 3, 2016) c-6 Testimony of David M. Callies c-7 Testimony of James Hallstrom, including Curriculum Vitae c-8 Testimony of Dr. Heather Kaluna c-9 Testimony of Naea Stevens c-1_0 Direct Testimony of Amber lmai-Hong c-1L Testimony of Robert B. Rechtman Thirty Meter Telescope Archaeological Report, prepared by c-12 Genevieve Glennon and Robert Rechtman (October -
Water on the Moon, III. Volatiles & Activity
Water on The Moon, III. Volatiles & Activity Arlin Crotts (Columbia University) For centuries some scientists have argued that there is activity on the Moon (or water, as recounted in Parts I & II), while others have thought the Moon is simply a dead, inactive world. [1] The question comes in several forms: is there a detectable atmosphere? Does the surface of the Moon change? What causes interior seismic activity? From a more modern viewpoint, we now know that as much carbon monoxide as water was excavated during the LCROSS impact, as detailed in Part I, and a comparable amount of other volatiles were found. At one time the Moon outgassed prodigious amounts of water and hydrogen in volcanic fire fountains, but released similar amounts of volatile sulfur (or SO2), and presumably large amounts of carbon dioxide or monoxide, if theory is to be believed. So water on the Moon is associated with other gases. Astronomers have agreed for centuries that there is no firm evidence for “weather” on the Moon visible from Earth, and little evidence of thick atmosphere. [2] How would one detect the Moon’s atmosphere from Earth? An obvious means is atmospheric refraction. As you watch the Sun set, its image is displaced by Earth’s atmospheric refraction at the horizon from the position it would have if there were no atmosphere, by roughly 0.6 degree (a bit more than the Sun’s angular diameter). On the Moon, any atmosphere would cause an analogous effect for a star passing behind the Moon during an occultation (multiplied by two since the light travels both into and out of the lunar atmosphere). -
Appendix I Lunar and Martian Nomenclature
APPENDIX I LUNAR AND MARTIAN NOMENCLATURE LUNAR AND MARTIAN NOMENCLATURE A large number of names of craters and other features on the Moon and Mars, were accepted by the IAU General Assemblies X (Moscow, 1958), XI (Berkeley, 1961), XII (Hamburg, 1964), XIV (Brighton, 1970), and XV (Sydney, 1973). The names were suggested by the appropriate IAU Commissions (16 and 17). In particular the Lunar names accepted at the XIVth and XVth General Assemblies were recommended by the 'Working Group on Lunar Nomenclature' under the Chairmanship of Dr D. H. Menzel. The Martian names were suggested by the 'Working Group on Martian Nomenclature' under the Chairmanship of Dr G. de Vaucouleurs. At the XVth General Assembly a new 'Working Group on Planetary System Nomenclature' was formed (Chairman: Dr P. M. Millman) comprising various Task Groups, one for each particular subject. For further references see: [AU Trans. X, 259-263, 1960; XIB, 236-238, 1962; Xlffi, 203-204, 1966; xnffi, 99-105, 1968; XIVB, 63, 129, 139, 1971; Space Sci. Rev. 12, 136-186, 1971. Because at the recent General Assemblies some small changes, or corrections, were made, the complete list of Lunar and Martian Topographic Features is published here. Table 1 Lunar Craters Abbe 58S,174E Balboa 19N,83W Abbot 6N,55E Baldet 54S, 151W Abel 34S,85E Balmer 20S,70E Abul Wafa 2N,ll7E Banachiewicz 5N,80E Adams 32S,69E Banting 26N,16E Aitken 17S,173E Barbier 248, 158E AI-Biruni 18N,93E Barnard 30S,86E Alden 24S, lllE Barringer 29S,151W Aldrin I.4N,22.1E Bartels 24N,90W Alekhin 68S,131W Becquerei -
Panthera Pardus) Range Countries
Profiles for Leopard (Panthera pardus) Range Countries Supplemental Document 1 to Jacobson et al. 2016 Profiles for Leopard Range Countries TABLE OF CONTENTS African Leopard (Panthera pardus pardus)...................................................... 4 North Africa .................................................................................................. 5 West Africa ................................................................................................... 6 Central Africa ............................................................................................. 15 East Africa .................................................................................................. 20 Southern Africa ........................................................................................... 26 Arabian Leopard (P. p. nimr) ......................................................................... 36 Persian Leopard (P. p. saxicolor) ................................................................... 42 Indian Leopard (P. p. fusca) ........................................................................... 53 Sri Lankan Leopard (P. p. kotiya) ................................................................... 58 Indochinese Leopard (P. p. delacouri) .......................................................... 60 North Chinese Leopard (P. p. japonensis) ..................................................... 65 Amur Leopard (P. p. orientalis) ..................................................................... 67 Javan Leopard