DOCSLIB.ORG

Editor Associate Editors

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text

Load more

VOLUME 30 / NUMBER 1 / 1988 Published by THE AMERICAN JOURNAL OF SCIENCE Editor MINZE STUIVER Associate Editors To serve until January 1, 1989 STEPHEN C PORTER Seattle, Washington To serve until January 1, 1989 W G MOOK Groningen, The Netherlands HANS OESCHGER Bern, Switzerland To serve until January 1, 1990 ANDREW MOORE New Haven, Connecticut To serve until January 1, 1992 CALVIN J HEUSSER Tuxedo, New York Managing Editor RENEE S KRA Kline Geology Laboratory Yale University I New Haven, Connecticut 06511 ISSN: 0033-8222 NOTICE TO READERS AND CONTRIBUTORS Since its inception, the basic purpose of RADIOCARBON has been the publication of compilations of ' 4C dates produced by various laboratories. These lists are extremely useful for the dissemination of basic 14C information. In recent years, RADIOCARBON has also been publishing technical and interpretative articles on all aspects of 14C. We would like to encourage this type of publication on a regular basis. In addition, we will be publishing compilations of published and unpublished dates along with interpretative text for these dates on a regional basis. Authors who would like to compose such an article for his/her area of interest should contact the Managing Editor for infor- mation. Another section is added to our regular issues, "Notes and Comments." Authors are invited to extend discussions or raise pertinent questions to the results of scientific inves- tigations that have appeared on our pages. The section includes short, technical notes to relay information concerning innovative sample preparation procedures. Laboratories may also seek assistance in technical aspects of radiocarbon dating. Book reviews will also be included for special editions. Manuscripts of radiocarbon papers should follow the recommendations in Suggestions to Authors* and RADIOCARBON Style Guide (R, 1984, v 26, p 152-158). Our deadline schedule for submitting manuscripts is: For Date Vol 30, No. 3, 1988 May 1, 1988 Vol 31, No. 1, 1989 Sept 1, 1988 Vol 31, No. 2, 1989 Jan 1, 1989 Half life of 14C. In accordance with the decision of the Fifth Radiocarbon Dating Conference, Cambridge, 1962, all dates published in this volume (as in previous volumes) are based on the Libby value, 5570 ± 30 yr, for the half life. This decision was reaffirmed at the 1 1 th International Radiocarbon Conference in Seattle, Washington, 1982. Because of various uncertainties, when 14C measurements are expressed as dates in years BP the accuracy of the dates is limited, and refinements that take some but not all uncertainties into account may be misleading. The mean of three recent determinations of the half life, 5730 ± 40 yr, (Nature, v 195, no. 4845, p 984, 1962), is regarded as the best value presently available. Published dates in years BP can be converted to this basis by multiplying them by 1.03. AD/BC Dates. In accordance with the decision of the Ninth International Radiocarbon Con- ference, Los Angeles and San Diego, 1976, the designation of AD/BC, obtained by subtracting AD 1950 from conventional BP determinations is discontinued in Radiocarbon. Authors or submitters may include calendar estimates as a comment, and report these estimates as cal AD/BC, citing the specific calibration curve used to obtain the estimate. Calibrated dates will now be reported as "cal BP" or "cal AD/BC" according to the consensus of the Twelfth International Radiocarbon Conference, Trondheim, Norway, 1985. Meaning of b"C. In Volume 3, 1961, we endorsed the notation A (Lamont VIII, 1961) for geochemical measurements of 14C activity, corrected for isotopic fractionation in samples and S14C in the NBS oxalic-acid standard. The value of that entered the calculation of A was defined by reference to Lamont VI, 1959, and was corrected for age. This fact has been lost sight of, by editors as well as by authors, and recent papers have used 514C as the observed deviation from the standard. At the New Zealand Radiocarbon Dating Conference it was recommended to use b14C only for age-corrected samples. Without an age correction, the value should then be reported as percent of modern relative to 0.95 NBS oxalic acid (Pro- ceedings 8th Conference on Radiocarbon Dating, Wellington, New Zealand, 1972). The Ninth International Radiocarbon Conference, Los Angeles and San Diego, 1976, recom- mended that the reference standard, 0.95 times NBS oxalic acid activity, be normalized to 613C = -19°/bo. 14C In several fields, however, age corrections are not possible. 6 and A, uncorrected for age, have been used extensively in oceanography, and are an integral part of models and theories. For the present, therefore, we continue the editorial policy of using A notations for samples not corrected for age. *Suggestions to Authors of the Reports of the United States Geological Survey, 6th ed, 1978, Supt of Documents, U S Govt Printing Office, Washington, DC 20402. Vol 30, No. 1 Radiocarbon 1988. CONTENTS Measurements AA Mozeto, Peter Fritz, M7. Moreira, E Vetter, Ramon Aravena, Eneas Salati, and Rf Drimmie ................................................................. 1 The Relations Between Carbon Isotope Composition and Apparent Age of Freshwater Tufaceous Sediments Anna Pazdur ......................................................................................... 7 Determination of Radon by Liquid Scintillation a/i3 Particle Spectrometry: Towards the Resolution of a 14C Dating Problem Henry Polach and Lauri Kaihola ............................................................. Cultural Evolution and Paleogeography on the Santa Barbara Coast: A 9600-Year 14C Record from Southern California Jon M Erlandson .................................................................................... DATE LISTS DE IC Yang US Geological Survey, Denver, Colorado Radiocarbon Dates V........... Gif Georgette Delibrias and Marie-Therese Guiltier Gif Natural Radiocarbon Measurements XI ......................................... HR Jinadasa Katupotha Hiroshima University Radiocarbon Dates I: West and South Coasts of Sri Lanka ............................................................................................. NOTES AND COMMENTS Letter to the Editor Rene Letolle ........................................................................................... The Second international Symposium on Archaeology and 14C Renee Kra ............................................................................................. 130 Review: Radiocarbon Dating: An Archaeological Perspective, by RE Taylor Frank Hole ............................................................................................ l 31 Preliminary Statement on an Error in British Museum Radiocarbon Dates MS Tile, SGE Bowman, JC Ambers, and KJ Malthews ............................... 132 I [RADIOCARBON, VOL 30, NO 1, 1988, P 1-6] Radiocarbon 1988 GROWTH RATES OF NATURAL AMAZONIAN FOREST TREES BASED ON RADIOCARBON MEASUREMENTS A A MOZETO*, PETER FRITZ**, M Z MOREIRAt, E VETTER*, RAMON ARAVENA**, ENEAS SALATIf and R J DRIMMIE** ABSTRACT. Evergreen trees in the tropical rain forest of the Amazonas Basin can produce growth rings which are not necessarily related to annual events. Therefore, estimation of growth rate cannot be done by dendrochronology. This report presents a technique for deter- mining the growth rate of these trees based on radiocarbon measurements of two segments of equal radial distance from the outer part of the tree trunk. The measured 14C activity is com- pared to local 14C fallout and growth rates are derived from models taking into account bomb 14C effects. Eleven trees from various parts of the Amazon Basin were analyzed. The average growth rates range from ca 5 to > 40 yr per centimeter corresponding to extrapolated ages from ca 60 to > 400 yr. INTRODUCTION Rings of trees growing in temperate climate permit accurate dating of forest stands and determination of growth rates. Such information cannot be obtained on evergreen trees from tropical rain forests. In the Amazonas region annual flooding does, however, cause some cyclicity in tree growth so that trees which defoliate during submersion show annual rings reflect- ing the cambial dormancy induced by lack of oxygen in the root zone. Growth rings of such trees are "often undefined and boundaries frequently run irregularly over the cross section" (Worbes, 1985). In 1980 an international workshop was held to discuss "age and growth rate of tropical trees: new directions for research" (Borman & Berlyn, 1980). It concluded that very few data exist but identified some promising avenues. Among others, Stuiver et al (1980) proposed to use radiocarbon to establish growth rates. The technique would take advantage of the anthropogenic input to the atmospheric radiocarbon reservoir and especially the maximum fallout in the Northern and Southern Hemisphere which followed nuclear testing in 1963/64. This suggestion was applied in modified form in this study. The tree species reported in this study were selected based on the wood specific weight (ratio of dry weight/water saturated weight of the heartwood) and the diameter of tree trunk so as to select both old and young trees. The location and the time of cutting is known and species were * Universidade Federal de Sao Carlos, Departamento de Quimica, Caixa Postal 676, 13560-Sao Carlos, SP, Brazil ** University of Waterloo, Department of Earth Sciences, Waterloo, Ontario, Canada N2L 3G1 t Centro de Energia Nuclear na Agricultura, Universidade de Sao Paulo, Caixa Postal 96, 13400-Piracicaba, SP, Brazil
Recommended publications
  • Imaginative Geographies of Mars: the Science and Significance of the Red Planet, 1877 - 1910

    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.
  • The Evolution of a Heterogeneous Martian Mantle: Clues from K, P, Ti, Cr, and Ni Variations in Gusev Basalts and Shergottite Meteorites

    The Evolution of a Heterogeneous Martian Mantle: Clues from K, P, Ti, Cr, and Ni Variations in Gusev Basalts and Shergottite Meteorites

    Earth and Planetary Science Letters 296 (2010) 67–77 Contents lists available at ScienceDirect Earth and Planetary Science Letters journal homepage: www.elsevier.com/locate/epsl The evolution of a heterogeneous Martian mantle: Clues from K, P, Ti, Cr, and Ni variations in Gusev basalts and shergottite meteorites Mariek E. Schmidt a,⁎, Timothy J. McCoy b a Dept. of Earth Sciences, Brock University, St. Catharines, ON, Canada L2S 3A1 b Dept. of Mineral Sciences, National Museum of Natural History, Smithsonian Institution, Washington, DC 20560-0119, USA article info abstract Article history: Martian basalts represent samples of the interior of the planet, and their composition reflects their source at Received 10 December 2009 the time of extraction as well as later igneous processes that affected them. To better understand the Received in revised form 16 April 2010 composition and evolution of Mars, we compare whole rock compositions of basaltic shergottitic meteorites Accepted 21 April 2010 and basaltic lavas examined by the Spirit Mars Exploration Rover in Gusev Crater. Concentrations range from Available online 2 June 2010 K-poor (as low as 0.02 wt.% K2O) in the shergottites to K-rich (up to 1.2 wt.% K2O) in basalts from the Editor: R.W. Carlson Columbia Hills (CH) of Gusev Crater; the Adirondack basalts from the Gusev Plains have more intermediate concentrations of K2O (0.16 wt.% to below detection limit). The compositional dataset for the Gusev basalts is Keywords: more limited than for the shergottites, but it includes the minor elements K, P, Ti, Cr, and Ni, whose behavior Mars igneous processes during mantle melting varies from very incompatible (prefers melt) to very compatible (remains in the shergottites residuum).
  • Martian Crater Morphology

    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.
  • March 21–25, 2016

    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,
  • Martian Subsurface Properties and Crater Formation Processes Inferred from Fresh Impact Crater Geometries

    Martian Subsurface Properties and Crater Formation Processes Inferred from Fresh Impact Crater Geometries

    Martian Subsurface Properties and Crater Formation Processes Inferred From Fresh Impact Crater Geometries The Harvard community has made this article openly available. Please share how this access benefits you. Your story matters Citation Stewart, Sarah T., and Gregory J. Valiant. 2006. Martian subsurface properties and crater formation processes inferred from fresh impact crater geometries. Meteoritics and Planetary Sciences 41: 1509-1537. Published Version http://meteoritics.org/ Citable link http://nrs.harvard.edu/urn-3:HUL.InstRepos:4727301 Terms of Use This article was downloaded from Harvard University’s DASH repository, and is made available under the terms and conditions applicable to Other Posted Material, as set forth at http:// nrs.harvard.edu/urn-3:HUL.InstRepos:dash.current.terms-of- use#LAA Meteoritics & Planetary Science 41, Nr 10, 1509–1537 (2006) Abstract available online at http://meteoritics.org Martian subsurface properties and crater formation processes inferred from fresh impact crater geometries Sarah T. STEWART* and Gregory J. VALIANT Department of Earth and Planetary Sciences, Harvard University, 20 Oxford Street, Cambridge, Massachusetts 02138, USA *Corresponding author. E-mail: [email protected] (Received 22 October 2005; revision accepted 30 June 2006) Abstract–The geometry of simple impact craters reflects the properties of the target materials, and the diverse range of fluidized morphologies observed in Martian ejecta blankets are controlled by the near-surface composition and the climate at the time of impact. Using the Mars Orbiter Laser Altimeter (MOLA) data set, quantitative information about the strength of the upper crust and the dynamics of Martian ejecta blankets may be derived from crater geometry measurements.
  • Arxiv:2003.06799V2 [Astro-Ph.EP] 6 Feb 2021

    Arxiv:2003.06799V2 [Astro-Ph.EP] 6 Feb 2021

    Thomas Ruedas1,2 Doris Breuer2 Electrical and seismological structure of the martian mantle and the detectability of impact-generated anomalies final version 18 September 2020 published: Icarus 358, 114176 (2021) 1Museum für Naturkunde Berlin, Germany 2Institute of Planetary Research, German Aerospace Center (DLR), Berlin, Germany arXiv:2003.06799v2 [astro-ph.EP] 6 Feb 2021 The version of record is available at http://dx.doi.org/10.1016/j.icarus.2020.114176. This author pre-print version is shared under the Creative Commons Attribution Non-Commercial No Derivatives License (CC BY-NC-ND 4.0). Electrical and seismological structure of the martian mantle and the detectability of impact-generated anomalies Thomas Ruedas∗ Museum für Naturkunde Berlin, Germany Institute of Planetary Research, German Aerospace Center (DLR), Berlin, Germany Doris Breuer Institute of Planetary Research, German Aerospace Center (DLR), Berlin, Germany Highlights • Geophysical subsurface impact signatures are detectable under favorable conditions. • A combination of several methods will be necessary for basin identification. • Electromagnetic methods are most promising for investigating water concentrations. • Signatures hold information about impact melt dynamics. Mars, interior; Impact processes Abstract We derive synthetic electrical conductivity, seismic velocity, and density distributions from the results of martian mantle convection models affected by basin-forming meteorite impacts. The electrical conductivity features an intermediate minimum in the strongly depleted topmost mantle, sandwiched between higher conductivities in the lower crust and a smooth increase toward almost constant high values at depths greater than 400 km. The bulk sound speed increases mostly smoothly throughout the mantle, with only one marked change at the appearance of β-olivine near 1100 km depth.
  • Crater Ice Deposits Near the South Pole of Mars Owen William Westbrook

    Crater Ice Deposits Near the South Pole of Mars Owen William Westbrook

    Crater Ice Deposits Near the South Pole of Mars by Owen William Westbrook Submitted to the Department of Earth, Atmospheric, and Planetary Sciences in partial fulfillment of the requirements for the degree of Master of Science in Earth and Planetary Sciences at the MASSACHUSETTS INSTITUTE OF TECHNOLOGY June 2009 © Massachusetts Institute of Technology 2009. All rights reserved. A uth or ........................................ Department of Earth, Atmospheric, and Planetary Sciences May 22, 2009 Certified by . Maria T. Zuber E. A. Griswold Professor of Geophysics Thesis Supervisor 6- Accepted by.... ...... ..... ........................................... Daniel Rothman Professor of Geophysics Department of Earth, Atmospheric and Planetary Sciences MASSACHUSETTS INSTWITE OF TECHNOLOGY JUL 2 0 2009 ARCHIES LIBRARIES Crater Ice Deposits Near the South Pole of Mars by Owen William Westbrook Submitted to the Department of Earth, Atmospheric, and Planetary Sciences on May 22, 2009, in partial fulfillment of the requirements for the degree of Master of Science in Earth and Planetary Sciences Abstract Layered deposits atop both Martian poles are thought to preserve a record of past climatic conditions in up to three km of water ice and dust. Just beyond the extent of these south polar layered deposits (SPLD), dozens of impact craters contain large mounds of fill material with distinct similarities to the main layered deposits. Previously identified as outliers of the main SPLD, these deposits could offer clues to the climatic history of the Martian south polar region. We extend previous studies of these features by cataloging all crater deposits found near the south pole and quantifying the physical parameters of both the deposits and their host craters.
  • Water on the Moon, III. Volatiles & Activity

    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).
  • Fluid Escape Structures As Possible Indicators of Past Gas Hydrate

    Fluid Escape Structures As Possible Indicators of Past Gas Hydrate

    DOI: 10.1590/2317‑4889201720160090 ARTICLE Fluid escape structures as possible indicators of past gas hydrate dissociation during the deposition of the Barremian sediments in the Recôncavo Basin, NE, Brazil Estruturas de escape de fluidos como possíveis indicadoras de uma paleo‑dissociação de hidratos de gás durante a deposição de sedimentos do Barremiano na Bacia do Recôncavo, NE, Brasil Antonio Fernando Menezes Freire1*, Carlson de Matos Maia Leite2, Flávio Miranda de Oliveira2, Márcio Ferreira Guimarães2, Paulo da Silva Milhomem2, Raphael Pietzsch3, Roberto Salvador Francisco d’Ávila4 ABSTRACT: Empty elliptical vesicles are observed in outcrops RESUMO: Vesículas elípticas ocas são observadas em afloramentos de areni- of Barremian very fine clayey sandstone to siltstone lacustrine tos argilosos muito finos e siltitos lacustrinos do Membro Pitanga da Formação slurry deposits of the Pitanga Member (Maracangalha Forma‑ Maracangalha, expostos na Ilha de Maré, sudeste da Bacia do Recôncavo, Es- tion), exposed in the Maré Island, Southern Recôncavo Basin, tado da Bahia, Brasil. Essas rochas foram depositadas em condições subaquo- Brazil. These sedimentary features have been traditionally in‑ sas e são consideradas depósitos gravitacionais do tipo slurry. Essas feições têm terpreted as water escape structures triggered by the diapirism sido tradicionalmente interpretadas como sendo estruturas de escape de água, of the underlying shales of the Candeias Formation. This work resultado da ação do diapismo de folhelhos sotopostos da Formação Candeias. proposes that vesicles were generated during massive gas hydrate Este trabalho propõe que as vesículas foram geradas durante uma intensa dis- dissociation as a result of tectonic activity in a paleolake system. sociação de hidratos de gás em resposta à atividade tectônica existente naquele Tectonic uplift would have triggered both the reduction of the sistema lacustre.
  • Appendix I Lunar and Martian Nomenclature

    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
  • The Very Forward CASTOR Calorimeter of the CMS Experiment

    The Very Forward CASTOR Calorimeter of the CMS Experiment

    EUROPEAN ORGANIZATION FOR NUCLEAR RESEARCH (CERN) CERN-EP-2020-180 2021/02/11 CMS-PRF-18-002 The very forward CASTOR calorimeter of the CMS experiment The CMS Collaboration* Abstract The physics motivation, detector design, triggers, calibration, alignment, simulation, and overall performance of the very forward CASTOR calorimeter of the CMS exper- iment are reviewed. The CASTOR Cherenkov sampling calorimeter is located very close to the LHC beam line, at a radial distance of about 1 cm from the beam pipe, and at 14.4 m from the CMS interaction point, covering the pseudorapidity range of −6.6 < h < −5.2. It was designed to withstand high ambient radiation and strong magnetic fields. The performance of the detector in measurements of forward energy density, jets, and processes characterized by rapidity gaps, is reviewed using data collected in proton and nuclear collisions at the LHC. ”Published in the Journal of Instrumentation as doi:10.1088/1748-0221/16/02/P02010.” arXiv:2011.01185v2 [physics.ins-det] 10 Feb 2021 © 2021 CERN for the benefit of the CMS Collaboration. CC-BY-4.0 license *See Appendix A for the list of collaboration members Contents 1 Contents 1 Introduction . .1 2 Physics motivation . .3 2.1 Forward physics in proton-proton collisions . .3 2.2 Ultrahigh-energy cosmic ray air showers . .5 2.3 Proton-nucleus and nucleus-nucleus collisions . .5 3 Detector design . .6 4 Triggers and operation . .9 5 Event reconstruction and calibration . 12 5.1 Noise and baseline . 13 5.2 Gain correction factors . 15 5.3 Channel-by-channel intercalibration .
  • Panthera Pardus) Range Countries

    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