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  • 1
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    OSIRIS‐REx Visible and Near‐Infrared Observations of the Moon (2019)
    Wiley
    Details
    Publication Date: 2019
    Description: Abstract The Origins, Spectral Interpretation, Resource Identification, and Security‐Regolith Explorer (OSIRIS‐REx) mission observed the Moon during the spacecraft's Earth gravity assist in 2017. From the spacecraft view, the lunar phase was 42°, and the in‐view hemisphere was dominated by anorthositic highlands terrain. Lunar spectra obtained by the OSIRIS‐REx Visible and InfraRed Spectrometer show evidence of several candidate absorption features. We observe the 2.8‐μm hydration band, confirming the spectral results from other missions, but detected in full‐disk spectra. We also tentatively identify weak spectral features near 0.9 and 1.3 μm, consistent with lunar regolith containing a mixture of plagioclase and orthopyroxene minerals, as expected for highlands terrain.
    Print ISSN: 0094-8276
    Electronic ISSN: 1944-8007
    Topics: Geosciences , Physics
    Published by Wiley on behalf of American Geophysical Union (AGU).
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  • 2
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    Molecular recognition and metal ion template synthesis (1989)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1989-05-26
    Description: Methods for the design and synthesis of ligands intended to be specific for a metal ion have been a recent chemical development. This article describes how this process can be inverted so that the specifics of the coordination environment around the metal ion can be used as a template in large-scale ligand synthesis. The synthesis of macrobicyclic ligands for ferric ion has been accomplished by using active esters of catechol ligands in which catecholate coordination to iron is a prelude to the organic chemical reactions that link the coordination subunits together into one ligand system surrounding a central metal ion coordination site. The lanthanide(III) ions, which are among the most labile metal ions known, have coordination numbers of 8 or higher, and thus their encapsulation into a macrobicyclic structure is a challenging problem. Lanthanide amine complexes have been used as metal templates in the synthesis of such macrobicyclic lanthanide complexes. There is evidence that such a complex is inert to exchange in aqueous solution.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉McMurry, T J -- Raymond, K N -- Smith, P H -- New York, N.Y. -- Science. 1989 May 26;244(4907):938-43.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Radiation Oncology Branch, National Cancer Institute, Bethesda, MD 20892.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/2658057" target="_blank"〉PubMed〈/a〉
    Keywords: Cations ; Chemical Phenomena ; Chemistry ; Iron/metabolism ; *Ligands ; Macromolecular Substances ; Metals/*metabolism ; Metals, Rare Earth/metabolism ; Molecular Structure ; Templates, Genetic
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
    Published by American Association for the Advancement of Science (AAAS)
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  • 3
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    Detection of perchlorate and the soluble chemistry of martian soil at the Phoenix lander site (2009)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2009-07-04
    Description: The Wet Chemistry Laboratory on the Phoenix Mars Lander performed aqueous chemical analyses of martian soil from the polygon-patterned northern plains of the Vastitas Borealis. The solutions contained approximately 10 mM of dissolved salts with 0.4 to 0.6% perchlorate (ClO4) by mass leached from each sample. The remaining anions included small concentrations of chloride, bicarbonate, and possibly sulfate. Cations were dominated by Mg2+ and Na+, with small contributions from K+ and Ca2+. A moderately alkaline pH of 7.7 +/- 0.5 was measured, consistent with a carbonate-buffered solution. Samples analyzed from the surface and the excavated boundary of the approximately 5-centimeter-deep ice table showed no significant difference in soluble chemistry.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Hecht, M H -- Kounaves, S P -- Quinn, R C -- West, S J -- Young, S M M -- Ming, D W -- Catling, D C -- Clark, B C -- Boynton, W V -- Hoffman, J -- Deflores, L P -- Gospodinova, K -- Kapit, J -- Smith, P H -- New York, N.Y. -- Science. 2009 Jul 3;325(5936):64-7. doi: 10.1126/science.1172466.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA. michael.h.hecht@jpl.nasa.gov〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/19574385" target="_blank"〉PubMed〈/a〉
    Keywords: *Anions ; *Cations ; Chemical Phenomena ; Extraterrestrial Environment ; Hydrogen-Ion Concentration ; *Mars ; Oxidation-Reduction ; *Perchlorates ; Solubility ; Spacecraft ; Temperature ; Water
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
    Published by American Association for the Advancement of Science (AAAS)
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  • 4
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    Mars water-ice clouds and precipitation (2009)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2009-07-04
    Description: The light detection and ranging instrument on the Phoenix mission observed water-ice clouds in the atmosphere of Mars that were similar to cirrus clouds on Earth. Fall streaks in the cloud structure traced the precipitation of ice crystals toward the ground. Measurements of atmospheric dust indicated that the planetary boundary layer (PBL) on Mars was well mixed, up to heights of around 4 kilometers, by the summer daytime turbulence and convection. The water-ice clouds were detected at the top of the PBL and near the ground each night in late summer after the air temperature started decreasing. The interpretation is that water vapor mixed upward by daytime turbulence and convection forms ice crystal clouds at night that precipitate back toward the surface.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Whiteway, J A -- Komguem, L -- Dickinson, C -- Cook, C -- Illnicki, M -- Seabrook, J -- Popovici, V -- Duck, T J -- Davy, R -- Taylor, P A -- Pathak, J -- Fisher, D -- Carswell, A I -- Daly, M -- Hipkin, V -- Zent, A P -- Hecht, M H -- Wood, S E -- Tamppari, L K -- Renno, N -- Moores, J E -- Lemmon, M T -- Daerden, F -- Smith, P H -- New York, N.Y. -- Science. 2009 Jul 3;325(5936):68-70. doi: 10.1126/science.1172344.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Earth and Space Science and Engineering, York University, Toronto, Ontario, Canada. whiteway@yorku.ca〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/19574386" target="_blank"〉PubMed〈/a〉
    Keywords: Atmosphere ; Extraterrestrial Environment ; *Ice ; *Mars ; Spacecraft ; *Steam ; Temperature ; Time Factors
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
    Published by American Association for the Advancement of Science (AAAS)
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  • 5
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    Results from the Mars Pathfinder camera (1997)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1997
    Description: Images of the martian surface returned by the Imager for Mars Pathfinder (IMP) show a complex surface of ridges and troughs covered by rocks that have been transported and modified by fluvial, aeolian, and impact processes. Analysis of the spectral signatures in the scene (at 440- to 1000-nanometer wavelength) reveal three types of rock and four classes of soil. Upward-looking IMP images of the predawn sky show thin, bluish clouds that probably represent water ice forming on local atmospheric haze (opacity approximately 0.5). Haze particles are about 1 micrometer in radius and the water vapor column abundance is about 10 precipitable micrometers.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Smith, P H -- Bell, J F 3rd -- Bridges, N T -- Britt, D T -- Gaddis, L -- Greeley, R -- Keller, H U -- Herkenhoff, K E -- Jaumann, R -- Johnson, J R -- Kirk, R L -- Lemmon, M -- Maki, J N -- Malin, M C -- Murchie, S L -- Oberst, J -- Parker, T J -- Reid, R J -- Sablotny, R -- Soderblom, L A -- Stoker, C -- Sullivan, R -- Thomas, N -- Tomasko, M G -- Wegryn, E -- New York, N.Y. -- Science. 1997 Dec 5;278(5344):1758-65.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA. psmith@lpl.arizona.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/9388170" target="_blank"〉PubMed〈/a〉
    Keywords: Atmosphere ; *Extraterrestrial Environment ; Ice ; *Mars ; Minerals ; *Water ; Wind
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
    Published by American Association for the Advancement of Science (AAAS)
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  • 6
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    Overview of the Mars Pathfinder mission and assessment of landing site predictions (1997)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1997-12-31
    Description: Chemical analyses returned by Mars Pathfinder indicate that some rocks may be high in silica, implying differentiated parent materials. Rounded pebbles and cobbles and a possible conglomerate suggest fluvial processes that imply liquid water in equilibrium with the atmosphere and thus a warmer and wetter past. The moment of inertia indicates a central metallic core of 1300 to 2000 kilometers in radius. Composite airborne dust particles appear magnetized by freeze-dried maghemite stain or cement that may have been leached from crustal materials by an active hydrologic cycle. Remote-sensing data at a scale of generally greater than approximately 1 kilometer and an Earth analog correctly predicted a rocky plain safe for landing and roving with a variety of rocks deposited by catastrophic floods that are relatively dust-free.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Golombek, M P -- Cook, R A -- Economou, T -- Folkner, W M -- Haldemann, A F -- Kallemeyn, P H -- Knudsen, J M -- Manning, R M -- Moore, H J -- Parker, T J -- Rieder, R -- Schofield, J T -- Smith, P H -- Vaughan, R M -- New York, N.Y. -- Science. 1997 Dec 5;278(5344):1743-8.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/9388167" target="_blank"〉PubMed〈/a〉
    Keywords: Atmosphere ; *Extraterrestrial Environment ; Geologic Sediments ; Magnetics ; *Mars ; Water
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
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  • 7
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    Atmospheric imaging results from the Mars exploration rovers: Spirit and Opportunity (2004)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2004-12-04
    Description: A visible atmospheric optical depth of 0.9 was measured by the Spirit rover at Gusev crater and by the Opportunity rover at Meridiani Planum. Optical depth decreased by about 0.6 to 0.7% per sol through both 90-sol primary missions. The vertical distribution of atmospheric dust at Gusev crater was consistent with uniform mixing, with a measured scale height of 11.56 +/- 0.62 kilometers. The dust's cross section weighted mean radius was 1.47 +/- 0.21 micrometers (mm) at Gusev and 1.52 +/- 0.18 mm at Meridiani. Comparison of visible optical depths with 9-mm optical depths shows a visible-to-infrared optical depth ratio of 2.0 +/- 0.2 for comparison with previous monitoring of infrared optical depths.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Lemmon, M T -- Wolff, M J -- Smith, M D -- Clancy, R T -- Banfield, D -- Landis, G A -- Ghosh, A -- Smith, P H -- Spanovich, N -- Whitney, B -- Whelley, P -- Greeley, R -- Thompson, S -- Bell, J F 3rd -- Squyres, S W -- New York, N.Y. -- Science. 2004 Dec 3;306(5702):1753-6.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Texas A&M University, College Station, TX 77843, USA. lemmon@tamu.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/15576613" target="_blank"〉PubMed〈/a〉
    Keywords: Algorithms ; Atmosphere ; Carbon Dioxide ; Extraterrestrial Environment ; *Mars ; Solar System ; Spacecraft ; Temperature
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
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  • 8
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    Textures of the soils and rocks at Gusev Crater from Spirit's Microscopic Imager (2004)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2004-08-07
    Description: The Microscopic Imager on the Spirit rover analyzed the textures of the soil and rocks at Gusev crater on Mars at a resolution of 100 micrometers. Weakly bound agglomerates of dust are present in the soil near the Columbia Memorial Station. Some of the brushed or abraded rock surfaces show igneous textures and evidence for alteration rinds, coatings, and veins consistent with secondary mineralization. The rock textures are consistent with a volcanic origin and subsequent alteration and/or weathering by impact events, wind, and possibly water.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Herkenhoff, K E -- Squyres, S W -- Arvidson, R -- Bass, D S -- Bell, J F 3rd -- Bertelsen, P -- Cabrol, N A -- Gaddis, L -- Hayes, A G -- Hviid, S F -- Johnson, J R -- Kinch, K M -- Madsen, M B -- Maki, J N -- McLennan, S M -- McSween, H Y -- Rice, J W Jr -- Sims, M -- Smith, P H -- Soderblom, L A -- Spanovich, N -- Sullivan, R -- Wang, A -- New York, N.Y. -- Science. 2004 Aug 6;305(5685):824-6.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉U.S. Geological Survey Astrogeology Team, Flagstaff, AZ 86001, USA. kherkenhoff@usgs.gov〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/15297663" target="_blank"〉PubMed〈/a〉
    Keywords: Extraterrestrial Environment ; Geologic Sediments ; *Mars ; Volcanic Eruptions ; Water ; Wind
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
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  • 9
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    Evidence from Opportunity's Microscopic Imager for water on Meridiani Planum (2004)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2004-12-04
    Description: The Microscopic Imager on the Opportunity rover analyzed textures of soils and rocks at Meridiani Planum at a scale of 31 micrometers per pixel. The uppermost millimeter of some soils is weakly cemented, whereas other soils show little evidence of cohesion. Rock outcrops are laminated on a millimeter scale; image mosaics of cross-stratification suggest that some sediments were deposited by flowing water. Vugs in some outcrop faces are probably molds formed by dissolution of relatively soluble minerals during diagenesis. Microscopic images support the hypothesis that hematite-rich spherules observed in outcrops and soils also formed diagenetically as concretions.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Herkenhoff, K E -- Squyres, S W -- Arvidson, R -- Bass, D S -- Bell, J F 3rd -- Bertelsen, P -- Ehlmann, B L -- Farrand, W -- Gaddis, L -- Greeley, R -- Grotzinger, J -- Hayes, A G -- Hviid, S F -- Johnson, J R -- Jolliff, B -- Kinch, K M -- Knoll, A H -- Madsen, M B -- Maki, J N -- McLennan, S M -- McSween, H Y -- Ming, D W -- Rice, J W Jr -- Richter, L -- Sims, M -- Smith, P H -- Soderblom, L A -- Spanovich, N -- Sullivan, R -- Thompson, S -- Wdowiak, T -- Weitz, C -- Whelley, P -- New York, N.Y. -- Science. 2004 Dec 3;306(5702):1727-30.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉U.S. Geological Survey Astrogeology Team, Flagstaff, AZ 86001, USA. kherkenhoff@usgs.gov〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/15576607" target="_blank"〉PubMed〈/a〉
    Keywords: Extraterrestrial Environment ; Ferric Compounds ; Geologic Sediments ; *Mars ; Minerals ; Silicates ; Spacecraft ; *Water
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
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  • 10
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    H2O at the Phoenix landing site (2009)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2009-07-04
    Description: The Phoenix mission investigated patterned ground and weather in the northern arctic region of Mars for 5 months starting 25 May 2008 (solar longitude between 76.5 degrees and 148 degrees ). A shallow ice table was uncovered by the robotic arm in the center and edge of a nearby polygon at depths of 5 to 18 centimeters. In late summer, snowfall and frost blanketed the surface at night; H(2)O ice and vapor constantly interacted with the soil. The soil was alkaline (pH = 7.7) and contained CaCO(3), aqueous minerals, and salts up to several weight percent in the indurated surface soil. Their formation likely required the presence of water.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Smith, P H -- Tamppari, L K -- Arvidson, R E -- Bass, D -- Blaney, D -- Boynton, W V -- Carswell, A -- Catling, D C -- Clark, B C -- Duck, T -- Dejong, E -- Fisher, D -- Goetz, W -- Gunnlaugsson, H P -- Hecht, M H -- Hipkin, V -- Hoffman, J -- Hviid, S F -- Keller, H U -- Kounaves, S P -- Lange, C F -- Lemmon, M T -- Madsen, M B -- Markiewicz, W J -- Marshall, J -- McKay, C P -- Mellon, M T -- Ming, D W -- Morris, R V -- Pike, W T -- Renno, N -- Staufer, U -- Stoker, C -- Taylor, P -- Whiteway, J A -- Zent, A P -- New York, N.Y. -- Science. 2009 Jul 3;325(5936):58-61. doi: 10.1126/science.1172339.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA. psmith@lpl.arizona.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/19574383" target="_blank"〉PubMed〈/a〉
    Keywords: Calcium Carbonate ; Extraterrestrial Environment ; Hydrogen-Ion Concentration ; *Ice ; *Mars ; Robotics ; Spacecraft ; Temperature ; *Water
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
    Published by American Association for the Advancement of Science (AAAS)
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