DOCSLIB.ORG

Characteristics of the Pathfinder APXS Sites

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Characteristics of the Pathfinder APXS Sites JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 106, NO. E7, PAGES 14,621-14,665,JULY 25, 2001 Characteristicsof the Pathfinder APXS sites:Implications for the compositionof Martian rocks and soils NathanT. Bridgesand Joy A. Crisp JetPropulsion Laboratory, Pasadena, California James F. Bell III Centerfor Radiophysicsand Space Research, Cornell University, Ithaca, New York Abstract. An integratedstudy of spectral,elemental abundance, and image data from the Pathfinderalpha proton X-ray spectrometer(APXS) measurementsites has led to a better understandingof the natureof Martiansurface matehals. This rigorousanalysis provides a new level of detailthat forms the basisfor the resultsreported here and that can be usedby future scientiststrying to understandrocks and soilson Mars. EachAPXS sitehas been precisely locatedby analyzingstereo Imager for Mars Pathfinder(IMP) androver camera images to determine the positionof the APXS duringdeployment. Rover and IMP imagesare usedto assesslocal geology,namely, the presence of pebbles,clods, and aeolian features in soilsand surface textures anddust concentrations on rocks. IMP spectrausing the latestcalibrations for radianceand reflectanceare analyzedat a numberof differentillumination geometries for eachAPXS site. The three-dimensionalorientation of the siteshas been determined and then used to computethe true sunlight(incidence) and viewing (emission) angles. Where suitable photometric coverage is available,reflectances are fit to the Hapke-Irvinefunction. This is thenused to adjustspectral reflectancesto a normalizedillumination geometry common to all rocksand soils. Comparingall the datasets shows a positivecorrelation among red/blue reflectance ratio, SO3content, and dust abundanceon rocks,indicating that rocks are coatedwith varyingamounts of sulfur-rich,red dust. Otherelements, such as siliconand iron, are poortracers for dustbecause their abundances within soil are similarto thosewithin rock. Rock APXS targetsthat are bluer,poorer in sulfur,and have minimaldust coverage face toward the northeast,the directionin whichwinds may be capableof efficientlyremoving loose material under current Martian conditions. The IMP spectralproperties of the soilsshow poor correlations with APXS elementalabundances. On the basisof currently releasedAPXS data,bulk soilsat the Pathfinderlanding site are richerin silicaand sulfurthan the Viking landingsites, suggesting a differentcomposition. The APXS soilswith the mostapparent pebblesare the poorestin SiO2,indicating that either the pebblesare moremafic thanthe APXS rocksor thepebble-free soil componentis inherentlyenriched in SiO2compared to Viking soils. The mixtureof materialsat the APXS sitesis a reflectionof the overall complexityof Martian surfacematerials, a detailedunderstanding of whichshould drive the choice of futureinstruments and missions. 1. Introduction abundances(from here on, APXS "ite" refers to the region within the actual 5-cm APXS analysis spot or an area that The alpha proton X-my spectrometer(APXS) on Mars likely containsthe spot, as describedbelow). IMP furnishes Pathfinder's Sojourner rover provided the first in situ similar information, generally at a lower spatial resolution, measurements of Martian surface materials and the first andprovides visible andnear-IR spectrathat are relatedto the analyses of unequivocalMartian rocks. It acquired 16 oxidation state, mineralogy, and physical nature of the measurementsof geologic materials, of which 11 were of surface.As wasrecognized before landing, the complementary sufficient quality that they have been converted to oxide information providedby these instrumentscould serve as a abundances [Rieder et al., 1997a]. These 11 measurement very useful tool for constraining the elemental chemistry, targetsconsist of :5 rocks and 6 soils. Supportingthe APXS mineralogy,and physical makeup of the materials[Golombek, measurementswere the rover camerasand the lander'sImager 1997; Smith et al., 1997b]. for Mars Pathfinder(IMP). The images from the rover show The Pathfinder APXS and supporting data collectively the detailedmorphology of APXS sites, giving clues to the provide previously unavailable information regarding the components contributing to the measuredbulk elemental Martian surface. The only other successfulMars landers, Viking 1 and 2, had well-calibratedX-my fluorescence spectrometers(XRFS) and comparableresolution cameras. Copyright2001 by theAmerican Geophysical Union. However,the XRFS did not measurerocks [e.g., Clark et al., Papernumber 2000JE001393. 1982] and the camerassampled fewer wavelengthsthan IMP 0148-0227/01/2000JE001393509.00 and could be calibrated only to within 10% uncertainty 14,621 14,622 BRIDGES ET AL.' PATHFINDER APXS SITES [Guinnesset al., 1987]. The availability of an imaging rover iron-bearingminerals and their weatheredproducts [Smith et on Pathfinder provided greater spatial resolution for some al., 1997b]. The band centersof the 12 "geology" filters areasthan achievablewith the fixed camerasof Viking. Initial rangein wavelengthfrom 440 to 1000 nm [seeSmith et al., studiesusing complementary APXS data, rover imaging, and 1997b, Figure6]. IMP data are 12-bit encoded,providing a IMP spectra/imaging have proven very useful for 64-fold improvementin dataprecision over the 6-bit Viking understandingthe geology of the landing site [Bridgeset al., Landercameras. Spectral features of two main mineral groups 19.97, 1998, 2000; Basilevskyet al., 1999; Bell and Bustani, expectedon the Martian surfacespan the IMP wavelength 1999; Bridgesand Crisp, 1999; McSweenet al., 1999; Bell et range. Crystallineferric (Fe 3*) oxides,oxyhydroxides, and al., 2000]. poorlycrystalline and nanophase ferric oxides have diagnostic This paperdocuments and exploresthe relationshipamong spectralsignatures from 440 to 860 nm, a region sampledby APXS, IMP imaging/spectra, and rover imaging data for the eight IMP geology filters [Morris et al., 1985, 1989, 1990; APXS sites. This is done in order to better understand and Smithet al., 1997b]. Ferrous(Fe 2*) silicates,principally characterize the rocks and soils at the Pathfinder site and Mars pyroxene and olivine, have absorption bands near 1 /•m in general,namely, their mixing relationships,physical state, [Cloutisand Gaffey, 1991; Gaffeyet al., 1993]. Thesebands spectralproperties, and geochemistry. In addition, the new were well sampled by the five filters spread over the level of detail reported herein should benefit future wavelengthrange of 860 to 1000 nm [Smithet al., 1997b]. investigationsof Martian surfacematerials, which will require Onceon the Martian surface,IMP acquiredmultispectral data progressively more sophisticated measurementsand data of the entire Pathfinderlanding site. Seven imaging sequences analysis techniques. First, a brief review of the IMP, rover can be ttsedfor spectralanalyses (Table 1). Except for the camera,and APXS instrumentsis presented.This is followed Multispectral Spots, each of these covers almost the entire by an overview of earlier related studies. The methods landingsite scene. The Superpanand Multispectral Spots are employedto analyze the data are then presented. This is of mostrelevance because they wereacquired in all 12 geology followed by a discussionof the location, geology, surface filters with losslessor minimal (2:1) compression. orientation, and spectralproperties of each APXS site. The IMP images also provided important information on illumination geometry of each measurementspot, combined geology and geomorphology. The Insuranceand Superpan, with simple photometricmodeling and assumptions,is then with losslessor 2:1 compression,acquired images of rocksand usedto normalize the reflectancesand spectral ratios to a soils with a resolutionof 1 mrad/pixel, comparableto the 0.7 commongeometry. The paper goes on to comparethe APXS, mrad/pixelfor the Viking Landercameras. Finally, several imaging, and normalized spectral data. The Pathfinder soil IMP sequenceswere devotedto determining the position, compositionsare then comparedto Viking analyses. Finally, orientation,and location of the rover. Thesedata were usedby inferences on the overall characteristics of rocks and soils on engineersto updateposition and orientationinformation in Mars are explored. the rover software,plan traverses,and assessthe successof previoustraverses and have beenttsed here to help determine 2. Background APXS site positions. 2.1. IMP Data 2.2. Rover Imaging Data The Imagerfor Mars Pathfindercamera provided visible-near The PathfinderSojourner rover camed one color and two IR multispectral,stereo imaging at the Pathfinderlanding site monochrome cameras [Rover Team, 1997a]. The color camera at a resolutionof 1 mrad/pixel [Smith et al., 1997a]. The IMP was located on the rear of the rover. It had pixels for red, filter set wasdesigned to searchfor the spectralsignatures of green,and infrared and a crosstrack by along track resolution Table 1. PathfinderImage Sequences Relevant to GeologySpectral Studies , ,, , Imaee Seauence Compressiona Fi![ers, gm Stereo Sol(s) PredeployPan (SOO01) 6:1 (965)' 12:1 (670) 670, 965 no 1 (stowed position) Mission SuccessPan (S0002,8) 12:1,2x2 pix. ave.b (440, 670);24:1 (530) 440, 530, 670 yes (stowedposition) Insurance Pan (S0030-33) lossless 440, 530, 600, 750 yes (stowedposition) Monster Pan (S0069,70,73,74) 6:1, 2x2 pix. ave.b(all,except 670)' 6:1 (670) 440, 530, 670, 750, 965 yes (deployedposition) Gallery Pan (S0164-167) 6:1 440, 530, 670 no 8-19 (deployed position) MultispectralSpots (S0171-2)
Load more

Recommended publications
  • Copyrighted Material
    Index Abulfeda crater chain (Moon), 97 Aphrodite Terra (Venus), 142, 143, 144, 145, 146 Acheron Fossae (Mars), 165 Apohele asteroids, 353–354 Achilles asteroids, 351 Apollinaris Patera (Mars), 168 achondrite meteorites, 360 Apollo asteroids, 346, 353, 354, 361, 371 Acidalia Planitia (Mars), 164 Apollo program, 86, 96, 97, 101, 102, 108–109, 110, 361 Adams, John Couch, 298 Apollo 8, 96 Adonis, 371 Apollo 11, 94, 110 Adrastea, 238, 241 Apollo 12, 96, 110 Aegaeon, 263 Apollo 14, 93, 110 Africa, 63, 73, 143 Apollo 15, 100, 103, 104, 110 Akatsuki spacecraft (see Venus Climate Orbiter) Apollo 16, 59, 96, 102, 103, 110 Akna Montes (Venus), 142 Apollo 17, 95, 99, 100, 102, 103, 110 Alabama, 62 Apollodorus crater (Mercury), 127 Alba Patera (Mars), 167 Apollo Lunar Surface Experiments Package (ALSEP), 110 Aldrin, Edwin (Buzz), 94 Apophis, 354, 355 Alexandria, 69 Appalachian mountains (Earth), 74, 270 Alfvén, Hannes, 35 Aqua, 56 Alfvén waves, 35–36, 43, 49 Arabia Terra (Mars), 177, 191, 200 Algeria, 358 arachnoids (see Venus) ALH 84001, 201, 204–205 Archimedes crater (Moon), 93, 106 Allan Hills, 109, 201 Arctic, 62, 67, 84, 186, 229 Allende meteorite, 359, 360 Arden Corona (Miranda), 291 Allen Telescope Array, 409 Arecibo Observatory, 114, 144, 341, 379, 380, 408, 409 Alpha Regio (Venus), 144, 148, 149 Ares Vallis (Mars), 179, 180, 199 Alphonsus crater (Moon), 99, 102 Argentina, 408 Alps (Moon), 93 Argyre Basin (Mars), 161, 162, 163, 166, 186 Amalthea, 236–237, 238, 239, 241 Ariadaeus Rille (Moon), 100, 102 Amazonis Planitia (Mars), 161 COPYRIGHTED
    [Show full text]
  • Pueblo County Taxsale Advertising
    Pueblo County Taxsale Advertising Date 10/04/2021 Page 1 1 420406001 313.66 * # LOT 17 SUNSET MEADOWS PUEBLO HOME DEV CO LLC COMM FROM THE NW COR OF 17 331004012 444.96 * C/O BARBARA O CONNELL THE INTERSECTION OF MARTINEZ BRIAN S S2 7-20-64 48.36A S2 OF SEC 7-20- WALKING STICK BLVD AND EI RIVERA ALAN J/RIVERA LANCE -64 E OF D+RGW RR + W2SE4 N PRINCIPIO DRIVE, SAID PT ALSO 35 DICK TREFZ ST OF 47TH ST + W OF UNIVERSITY BEING THE ELY COR OF PAR K LOT 3 BLK 40 BELMONT 26TH 31891 ALDRED RD PARK 18TH FILING ALSO LESS ACCORDING TO THE RECORDED 2 420406001 1,015.45 * E 155.1 FT OF S 112.25 FT LOT 12 NW4NW4SW4 10A (296.40A) LESS PLAT OF NORTH VISTA CAULIFLOWER GARDENS 13.5A ABANDONED RR + RD HIGHLANDS, FLING NO. 1 FILED AMENDED CONTG .40A LESS 5A #599466 LESS 5A #396406 NOVEMBER 15, 2019 AT RIVERA ALAN J/RIVERA LANCE 18 331004016 509.99 * LESS 1.5A #411120 LESS 1.5A RECEPTION NO. 2159276; TH N. 35 DICK TREFZ ST #398118 LESS .01A #553603 TO 75°32'15" W., A DIST OF 2,074.11 LOT 3 BLK 40 BELMONT 26TH CITY LESS 30.29A #559536 TO FT TO THE PT OF BEG; TH S. 3 420406001 1,268.55 * BOTTS CLINTON S OTERO 6TH FILING LESS 10.112A 48°32'22" E, A DIST OF 698.55 FT; 31932 ALDRED RD #577004 TO OTERO 7TH FILING TH SELY ALONG THE ARC OF A E 110 FT OF N 100 FT + W 110 FT E LESS 15.515A #579206 TO OTERO CURVE TO THE RIGHT WHOSE RIVERA ALAN J/RIVERA LANCE 130 FT OF S 100 FT OF N 200 FT 8TH FILING LESS 1.75A #577214 RADIUS IS 720.00 FT,.
    [Show full text]
  • High Resolution Habitat Suitability Modeling for a Narrow-Range Endemic Alpine Hawaiian Species
    HIGH RESOLUTION HABITAT SUITABILITY MODELING FOR A NARROW-RANGE ENDEMIC ALPINE HAWAIIAN SPECIES A THESIS SUBMITTED TO THE GRADUATE DIVISION OF THE UNIVERSITY OF HAWAI‘I AT HILO IN PARTIAL FULFILLMENT OF THE REQUIREMENTS FOR THE DEGREE OF MASTER OF SCIENCE IN TROPICAL CONSERVATION BIOLOGY AND ENVIRONMENTAL SCIENCE MAY 2016 By: Nathan Michael Stephenson Thesis Committee: Ryan Perroy, Chairperson Jesse Eiben Frederick Klasner Keywords: Microhabitat, Structure from Motion, Lidar, MaxEnt, Habitat Suitability ii ACKNOWLEDGMENTS I would like to thank the Office of Maunakea Management for funding this project and also providing vehicles and equipment when necessary. The Office of Maunakea Management has been instrumental in the completion of this project and is a great resource for the community, with knowledgeable staff and access to information. I would also like to thank UNAVCO for facilitating the collection of high resolution lidar data and providing us with an excellent analyst, Marianne Okal. I would like to thank the Pacific Internship Programs for Exploring Science (PIPES) which provided a brilliant summer intern, Sean Kirkpatrick, who was a pleasure to work with. I would like to give a special thanks to my graduate committee Ryan, Frederick, and Jesse. Ryan has been an incredible teacher and mentor for my undergraduate and graduate careers and the completion of this project would not have been possible without his continued guidance and support. Frederick, Fritz, has facilitated and participated in many field collections and directed me to the resources and information necessary to finish this thesis. Jesse has been an invaluable resource with a wealth of knowledge about the Maunakea summit and our species of interest.
    [Show full text]
  • Modern Astronomy: Voyage to the Planets Lecture 4 the Red Planet
    Modern Astronomy: Voyage to the Planets Lecture 4 Mars the Red Planet University of Sydney Centre for Continuing Education Autumn 2005 first spacecraft to reach Mariner 4 flyby 1965 Mars Mariner 6 flyby 1969 Mariner 7 flyby 1969 Mariner 9 orbiter There have been many Mars 5 USSR orbiter 1973 spacecraft sent to orbiter/lander Viking 1 Landed Chryse Planitia Mars over the past 1976-1982 orbiter/lander Viking 2 Landed Utopia Planitia few decades. Here are 1976-1980 the successful ones, Mars Global orbiter Laser altimeter with a description of Surveyor 1997-present the highlights of each Mars Pathfinder lander & rover 1997 Landed Ares Vallis mission. 2001 Mars orbiter Studying composition Odyssey 2001-present Mars Express/ ESA orbiter + lander Geology + atmosphere Beagle 2003–present Spirit & rovers Landed Gusev Crater & Opportunity 2003–present Meridiani The Face of Mars Basic facts Mars Mars/Earth Mass 0.64185 x 1024 kg 0.107 Radius 3397 km 0.532 Mean density 3.92 g/cm3 0.713 Gravity (equatorial) 3.71 m/s2 0.379 Semi-major axis 227.92 x 106 km 1.524 Period 686.98 d 1.881 Orbital inclination 1.85o - Orbital eccentricity 0.0935 5.59 Axial tilt 25.2o 1.074 Rotation period 24.6229 h 1.029 Length of day 24.6597 h 1.027 Mars is quite small relative to Earth, but in other ways is extremely similar. The radius is only half that of Earth, though the total surface area is comparable to the land area of Earth. It take nearly twice as long to orbit the Sun, but the length of its day and its axial tilt are very close to Earth’s.
    [Show full text]
  • The Color of Mars: Spectrophotometric Measurements at the Pathfinder
    I The Color of Mars: Spectrophotometric Measurements at the Pathfinder bnding Site J. N. Makil, J. J. Lorrel, P. H, Smith2, R. D. 13randt1,D. J. Steinwancl’ ‘ Jet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena,CA91109 2Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721 Submitted to Journal of Geophysical Research, Planets, 30 January 1998. Revised 14 May 1998 . ABSTRACT We calculate the color of the Martian sky and surface directly using the absolute calibration of the Pathfinder lander camera, which was observed to be stable during the mission. The measured colors of the Martian sky and surface at the Pathfinder site are identical to the Viking sites, i.e., a predominantly yellowish brown color with only subtle variations. These colors are distributed continuously and fall into 5 overlapping groups with distinct average colors and unique spatial characteristics: shadowed soil, soil, soilhock mixtures, rock, and sky. We report that the primary difference between the sky color and the color of the rocks is due to a difference.. in brightness. Measurements of the sky color show that the sky reddens away from the sun and towards the horizon, and that the sky color varies with time of day and is re(idest at local noon. Wc present a true color picture of the Martian surface and color enhancement techniques that increase image saturation, maximize color discriminability while preserving hue, and eliminate brightness variations while preserving the chromaticity of the scene. Although Mars has long been called the “red” planet, quantitative measurements of the surface color from telescopic and surface observations indicate a light to moderate yellowlsh brown color.
    [Show full text]
  • Free Astronomy Magazine March-April 2021
    cover EN.qxp_l'astrofilo 25/02/2021 16:35 Page 1 THE FREE MULTIMEDIA MAGAZINE THAT KEEPS YOU UPDATED ON WHAT IS HAPPENING IN SPACE Bi-monthly magazine of scientific and technical information ✶ March-April 2021 S P E C I A L I S S U E Mars Rovers from Sojourner to Perseverance www.astropublishing.com ✶✶www.facebook.com/astropublishing [email protected] colophon EN_l'astrofilo 25/02/2021 16:33 Page 2 www.northek.it www.facebook.com/northek.it [email protected] phone +39 01599521 Ritchey-Chrétien ➤ SCHOTT Supremax 33 optics ➤ optical diameter 355 mm ➤ useful diameter 350 mm ➤ focal length 2800 mm Dall-Kirkham ➤ focal ratio f/8 ➤ SCHOTT Supremax 33 optics ➤ 18-point floating cell ➤ optical diameter 355 mm ➤ customized focuser ➤ useful diameter 350 mm ➤ focal length 7000 mm ➤ focal ratio f/20 Cassegrain ➤ 18-point floating cell ➤ SCHOTT Supremax 33 optics ➤ Feather Touch 2.5” focuser ➤ optical diameter 355 mm ➤ useful diameter 350 mm ➤ focal length 5250 mm ➤ focal ratio f/15 ➤ 18-point floating cell ➤ Feather Touch 2.5” focuser colophon EN_l'astrofilo 25/02/2021 16:33 Page 3 Mars Rovers BI-MONTHLY MAGAZINE OF SCIENTIFIC AND TECHNICAL INFORMATION 4 from Sojourner to Perseverance FREELY AVAILABLE THROUGH THE INTERNET March-April 2021 Sojourner 6 Spirit & Opportunity English edition of the magazine lA’ STROFILO 14 Editor in chief Michele Ferrara Scientific advisor Prof. Enrico Maria Corsini Publisher Astro Publishing di Pirlo L. Via Bonomelli, 106 25049 Iseo - BS - ITALY Curiosity email [email protected] Internet Service Provider Aruba S.p.A. Via San Clemente, 53 24036 Ponte San Pietro - BG - ITALY 26 Copyright All material in this magazine is, unless otherwise stated, property of Astro Publishing di Pirlo L.
    [Show full text]
  • Planets Solar System Paper Contents
    Planets Solar system paper Contents 1 Jupiter 1 1.1 Structure ............................................... 1 1.1.1 Composition ......................................... 1 1.1.2 Mass and size ......................................... 2 1.1.3 Internal structure ....................................... 2 1.2 Atmosphere .............................................. 3 1.2.1 Cloud layers ......................................... 3 1.2.2 Great Red Spot and other vortices .............................. 4 1.3 Planetary rings ............................................ 4 1.4 Magnetosphere ............................................ 5 1.5 Orbit and rotation ........................................... 5 1.6 Observation .............................................. 6 1.7 Research and exploration ....................................... 6 1.7.1 Pre-telescopic research .................................... 6 1.7.2 Ground-based telescope research ............................... 7 1.7.3 Radiotelescope research ................................... 8 1.7.4 Exploration with space probes ................................ 8 1.8 Moons ................................................. 9 1.8.1 Galilean moons ........................................ 10 1.8.2 Classification of moons .................................... 10 1.9 Interaction with the Solar System ................................... 10 1.9.1 Impacts ............................................ 11 1.10 Possibility of life ........................................... 12 1.11 Mythology .............................................
    [Show full text]
  • 6 X 10 Long.P65
    Cambridge University Press 978-0-521-80393-9 - Worlds on Fire: Volcanoes on the Earth, the Moon, Mars, Venus and Io Charles Frankel Index More information Index aa flow, 53, 55, 195, 250–51 anorthosite, 75, 101, 107 Acala (lava field, Io), 289 Apennine Bench Formation, Moon, 75, 84, accretion (planetary), 5–7, 64 93, 100–101 Aci Castello (Etna), 50 Apennine Mountains, Moon, 72–73, 73, Acidalia (plains, Mars), 192–93 99–100 Adirondack (rock, Mars), 154 Aphrodite Terra (Venus), 208, 213, 215, Aidne Corona (volcano, Venus), 208, 224, 217–18, 248–49, 249, Plate XVII Alba Patera (volcano, Mars), 127, 128, 134, Apollinaris Patera (volcano, Mars), 128, 146, 136, 139, 167, 169–70, 190–96, 190, 154, Plate XVI 192–93, 195, Plate XI Apollo landing sites (map), 65 Albor Tholus (volcano, Mars), 128, 136–37, Apollo 11, 67–71 137, 197, Plates XIV, XV Apollo 12, 70–72, 244 Alcott (impact crater, Venus), 237 Apollo 13, 72 Aldrin, Buzz, 68–69 Apollo 14, 72, 84 ALH 79001 (meteorite, Mars), 156 Apollo 15, 72–77, 81, 82–83, 84–85, 93, ALH 84001 (meteorite, Mars), 129, 156–58, 97–99, 98–101, 102–103, 111 161–63, 162 Apollo 16, 76, 95 alkali Apollo 17, 76–83, 77, 79, 85, 87, 91, on Earth, 18, 55, 57, 294 104–108, 104, 106–107, 109, 111, on Mars, 144 Plates IX, X on the Moon, 67 arachnoid (Venus), 217, 219, 224–25, 226 on Venus, 210, 212 Aram Chaos (Mars), 151 alkaline basalt, 41, 50–51, 60, 212–13, 245, archebacteria, 31 Plate XIX Arenal (volcano, Earth), 8 alkaline suite, 18, 41, 47–48 Ares Vallis (Mars), 148–49 Alpha Regio (Venus), 208, 215, 260–61, 262 Aristarchus
    [Show full text]
  • Phonology and Dictionary of Yavapai
    UC Berkeley Dissertations, Department of Linguistics Title Phonology and Dictionary of Yavapai Permalink https://escholarship.org/uc/item/9671j4f8 Author Shaterian, Alan Publication Date 1983 eScholarship.org Powered by the California Digital Library University of California Phonology and Dictionary of Yavapai By Alan William Shaterian A.B. (Syracuse University) 1963 C.Phil. (University of California) 1973 DISSERTATION Submitted in partial satisfaction of the requirements for the degree of DOCTOR OF PHILOSOPHY in Linguistics in the GRADUATE DIVISION OF THE UNIVERSITY OF CALIFORNIA, BERKELEY Approved: Chairmai Reproduced with permission of the copyright owner. Further reproduction prohibited without permission. YAVAPAI PHONOLOGY AND DICTIONARY Copyright @ 1983 by Alan Shaterian Reproduced with permission of the copyright owner. Further reproduction prohibited without permission. DEDICATION For Jeanie Reproduced with permission of the copyright owner. Further reproduction prohibited without permission. YAVAPAI PHONOLOGY AND DICTIONARY by Alan Shaterian ABSTRACT This work will preserve the fundamental facts about the Yavapai language, the most evanescent of the Pai group of Yuman languages, a linguistic family which in its vari­ ety of members and geographic distribution is analagous to the Germanic family as of five centuries ago. The dis­ sertation explores the relationship between the pattern of speech sounds and the shape of words in Yavapai. It de­ scribes the phonology, morphology, and a part of the lex­ icon in a format which is accessible to linguists of varied theoretical backgrounds. It is the speech of Chief Grace Jimulla Mitchell (1903-1976), a speaker of the Prescott subdialect of North­ eastern Yavapai, that forms the basis of the description. The research necessary for this undertaking was spon­ sored in part by the Survey of California and Other Indian Languages at the University of California at Berkeley.
    [Show full text]
  • On Boy Scouts and Anti-Discrimination Law: the Associational Rights of Quasi-Religious Organizations
    NOTES ON BOY SCOUTS AND ANTI-DISCRIMINATION LAW: THE ASSOCIATIONAL RIGHTS OF QUASI-RELIGIOUS ORGANIZATIONS Erez Reuveni∗ INTRODUCTION ............................................................................................... 109 I. THE BSA CASES SINCE DALE .............................................................. 114 A. Boy Scouts of America v. Dale ................................................... 114 B. Access to Public Facilities........................................................... 116 C. Access to Public Benefits, Programs, and Contracts .................. 117 D. Summary...................................................................................... 120 II. APPLYING EXISTING LAW TO PRIVATE ASSOCIATION......................... 120 A. The Religion Clauses................................................................... 121 1. Free Exercise ......................................................................... 121 2. Establishment ........................................................................ 126 B. Expressive Association ................................................................ 130 C. Speech and Unconstitutional Conditions..................................... 134 1. Free Speech ........................................................................... 135 2. Unconstitutional Conditions.................................................. 139 III. A TRIPARTITE APPROACH TO EXPRESSIVE ASSOCIATIONS ................. 144 A. Religious, Secular, and Quasi-Religious Associations................ 145
    [Show full text]
  • Transcript of Tax Delinquent Land Available for Sale Date: 9/24/2021
    2753 Jefferson Bess STATE OF ALABAMA-DEPARTMENT OF REVENUE-PROPERTY TAX DIVISION PAGE NO: 1 TRANSCRIPT OF TAX DELINQUENT LAND AVAILABLE FOR SALE DATE: 9/24/2021 Name CO. YR. C/S# CLASS CODE PARCEL ID DESCRIPTION AV Amt Bid at Tax Sale BARHAM SAM 68 00 0070 2 68 6838000230380010000000 LOTS D BL 27 BESS 200 45.19 BURNS CLAUDE TERRELL 68 00 0212 3 68 6829003020250050000000 LOT 6 BL 4 DONALDS ADD TO GRASSELLI 1850 158.68 BURTON J 68 00 0218 2 68 6821001930000250030000 COM NW COR OF SE4 OF SW4 SEC 19 TP 17S R 4W TH E 740 94.96 124.7 FT S 112.7 FT TO POB CONT S 96.1 FT W 454.4 CARLTON ARTHUR WILLIE ESTATE OF 68 00 0267 2 65 6830003520180130000000 LOT 17 BL 3 HUDSON GROVE 1100 114.42 CARPENTER JANET BETHEL 68 00 0275 2 68 6830002230250120000000 LOT 10 BL C WEST FAIRFIELD 500 69.31 CASCONE JEANETTE L 68 00 0301 2 51 6820002440100160000000 LOTS 31 32 & 33 BL 7 BOOKER HGTS BENNETT REALTY C 300 52.33 OS 3RD ADD CHRISTON BARBARA 68 00 0319 2 68 6838001710010220010000 LOT 10 BLK 373-A BESS C I & LD CO 4TH ADD TO WEST 760 85.39 LAKE HGLDS5/96 COLLINS JIMMY 68 00 0342 2 51 6821002740150120000000 W 1/2 OF LOT 1 BL 2 W M CAPPS 440 130.94 DAVIS LELA B 68 00 0433 2 68 6837003620000210010000 COM NW COR NW 1/4 NW 1/4 TH S 230 FT TO POB TH CO 400 64.79 NT S 280 FTTO NW LINE I-59 TH NE 152 FT TH NW 140 DAVIS PETTIE 68 00 0436 2 68 6837002640000460000000 POB SW COR OF SE 1/4 SEC 26 TSP 19S R 5W TH N 655 880 92.04 .3 FT TO SWR/W OF MCWAINE DR TH SE ALG R/W 40 FT T DENNIS SEMPLE 68 00 0467 2 68 6838000210040210000000 LOT 1 BL 5 PAULS HILL 1480 126.51 DIGGINS C LEON 68 00 0477 2 68 6838000230020090000000 LOT 13 14 & 15 BL 3 TILLMANS ADD 1480 128.11 ELLIS RAIFORD 68 00 0567 2 68 6830002720220030000000 LOTS 6-7 BLK 9 DONALDS 1ST ADD TO OAKDALE 460 52.99 ELLIS RAIFORD 68 00 0568 2 53 6830002720210090000000 LOT 19+20 BLK 8 DONALDS FIRST ADD TO OAKDALE 200 36.69 2753 Jefferson Bess STATE OF ALABAMA-DEPARTMENT OF REVENUE-PROPERTY TAX DIVISION PAGE NO: 2 TRANSCRIPT OF TAX DELINQUENT LAND AVAILABLE FOR SALE DATE: 9/24/2021 Name CO.
    [Show full text]
  • ASX and Media Release
    ASX and Media Release Tuesday, 20 July 2021 Tenement Expansion Over New VMS Prospects with Evidence of High Grade Massive Sulphide Mineralisation at Red Mountain, Alaska ASX Code: WRM HIGHLIGHTS Issued Securities • White Rock has secured additional tenements over historic VMS prospects and Shares: 89.5 million an emerging trend of new VMS targets at its 100% owned Red Mountain Options: 3.0 million Project, Alaska. Cash on hand (31 Mar 2021) • Surface reconnaissance has identified multiple prospect areas, some with high $10.9M grade massive sulphide rock float that is dominantly sphalerite (zinc sulphide), galena (lead sulphide), chalcopyrite (copper sulphide) and pyrite (iron sulphide). Market Cap (19 July 2021) $43.4M at $0.485 per share Directors & Management Peter Lester Non-Executive Chairman Matthew Gill Managing Director & Chief Executive Officer Jeremy Gray Non-Executive Director Shane Turner Company Secretary Photos 1 and 2:- Samples of massive sulphide float from the emerging Keevy VMS Trend. Rohan Worland • Field work is progressing with detailed mapping, surface geochemical Exploration Manager sampling and ground geophysics underway to assist in targeting drill holes For further information, contact: that will test a number of these new prospects in the coming weeks. Matthew Gill or Shane Turner Phone: 03 5331 4644 White Rock Minerals (“White Rock” or “the Company”) is pleased to announce the expansion of its district-scale tenement package at its 100% owned Red Mountain Project [email protected] www.whiterockminerals.com.au (Figure 1). The Company has moved to secure additional contiguous tenements to the north that cover the Galleon Prospect that was previously held by competitors and additional contiguous tenements to the south that cover the newly identified Keevy VMS Trend.
    [Show full text]