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2017 ANNUAL REPORT 2017 Annual Report Table of Contents the Michael J
Roadmaps for Progress 2017 ANNUAL REPORT 2017 Annual Report Table of Contents The Michael J. Fox Foundation is dedicated to finding a cure for 2 A Note from Michael Parkinson’s disease through an 4 Annual Letter from the CEO and the Co-Founder aggressively funded research agenda 6 Roadmaps for Progress and to ensuring the development of 8 2017 in Photos improved therapies for those living 10 2017 Donor Listing 16 Legacy Circle with Parkinson’s today. 18 Industry Partners 26 Corporate Gifts 32 Tributees 36 Recurring Gifts 39 Team Fox 40 Team Fox Lifetime MVPs 46 The MJFF Signature Series 47 Team Fox in Photos 48 Financial Highlights 54 Credits 55 Boards and Councils Milestone Markers Throughout the book, look for stories of some of the dedicated Michael J. Fox Foundation community members whose generosity and collaboration are moving us forward. 1 The Michael J. Fox Foundation 2017 Annual Report “What matters most isn’t getting diagnosed with Parkinson’s, it’s A Note from what you do next. Michael J. Fox The choices we make after we’re diagnosed Dear Friend, can open doors to One of the great gifts of my life is that I've been in a position to take my experience with Parkinson's and combine it with the perspectives and expertise of others to accelerate possibilities you’d improved treatments and a cure. never imagine.’’ In 2017, thanks to your generosity and fierce belief in our shared mission, we moved closer to this goal than ever before. For helping us put breakthroughs within reach — thank you. -
Tubular Symplectic Inclusions in Olivine from the Fukang Pallasite
Meteoritics & Planetary Science 45, Nr 5, 899–910 (2010) doi: 10.1111/j.1945-5100.2010.01054.x Tubular symplectic inclusions in olivine from the Fukang pallasite Michael R. STEVENS1, David R. BELL1,2, and Peter R. BUSECK1,2* 1School of Earth and Space Exploration, Arizona State University, Tempe, Arizona 85287, USA 2Department of Chemistry and Biochemistry, Arizona State University, Tempe, Arizona 85287, USA *Corresponding author. E-mail: [email protected] (Received 11 June 2009; revision accepted 27 March 2010) Abstract–Olivine from the Fukang meteorite, like that from many other pallasites, contains distinctive arrays of parallel, straight, tubular inclusions. They differ in their extension and linearity from those in terrestrial olivines. They comprise approximately 1% of the total volume. Most have lens-shaped cross-sections, but some are rounded. The major axis of the lens-shaped inclusions is rigorously oriented along olivine [001], and the rounded ones lie along olivine [010] and a few along [100]. The linear nature and orientations of the inclusions suggest that they nucleated on screw dislocations, perhaps formed through shock triggering. High-resolution transmission electron microscopy (TEM) and energy-dispersive x-ray spectroscopy show that the inclusions consist of symplectic intergrowths of chromite, diopside, and silica that appear to have formed by exsolution from the host olivine. The symplectites consist of chromite lamellae with approximately 35-nm spacings that grew outward from a central plane, with interstitial diopside and silica. Contrast modulations having an average spacing of 4.4 nm occur within the chromite lamellae. Using a reaction- front model, we estimate that exsolution occurred over a period of 30 to 100 min, suggesting rapid cooling at high temperature. -
18Th EANA Conference European Astrobiology Network Association
18th EANA Conference European Astrobiology Network Association Abstract book 24-28 September 2018 Freie Universität Berlin, Germany Sponsors: Detectability of biosignatures in martian sedimentary systems A. H. Stevens1, A. McDonald2, and C. S. Cockell1 (1) UK Centre for Astrobiology, University of Edinburgh, UK ([email protected]) (2) Bioimaging Facility, School of Engineering, University of Edinburgh, UK Presentation: Tuesday 12:45-13:00 Session: Traces of life, biosignatures, life detection Abstract: Some of the most promising potential sampling sites for astrobiology are the numerous sedimentary areas on Mars such as those explored by MSL. As sedimentary systems have a high relative likelihood to have been habitable in the past and are known on Earth to preserve biosignatures well, the remains of martian sedimentary systems are an attractive target for exploration, for example by sample return caching rovers [1]. To learn how best to look for evidence of life in these environments, we must carefully understand their context. While recent measurements have raised the upper limit for organic carbon measured in martian sediments [2], our exploration to date shows no evidence for a terrestrial-like biosphere on Mars. We used an analogue of a martian mudstone (Y-Mars[3]) to investigate how best to look for biosignatures in martian sedimentary environments. The mudstone was inoculated with a relevant microbial community and cultured over several months under martian conditions to select for the most Mars-relevant microbes. We sequenced the microbial community over a number of transfers to try and understand what types microbes might be expected to exist in these environments and assess whether they might leave behind any specific biosignatures. -
Geologic Map of the Victoria Quadrangle (H02), Mercury
H01 - Borealis Geologic Map of the Victoria Quadrangle (H02), Mercury 60° Geologic Units Borea 65° Smooth plains material 1 1 2 3 4 1,5 sp H05 - Hokusai H04 - Raditladi H03 - Shakespeare H02 - Victoria Smooth and sparsely cratered planar surfaces confined to pools found within crater materials. Galluzzi V. , Guzzetta L. , Ferranti L. , Di Achille G. , Rothery D. A. , Palumbo P. 30° Apollonia Liguria Caduceata Aurora Smooth plains material–northern spn Smooth and sparsely cratered planar surfaces confined to the high-northern latitudes. 1 INAF, Istituto di Astrofisica e Planetologia Spaziali, Rome, Italy; 22.5° Intermediate plains material 2 H10 - Derain H09 - Eminescu H08 - Tolstoj H07 - Beethoven H06 - Kuiper imp DiSTAR, Università degli Studi di Napoli "Federico II", Naples, Italy; 0° Pieria Solitudo Criophori Phoethontas Solitudo Lycaonis Tricrena Smooth undulating to planar surfaces, more densely cratered than the smooth plains. 3 INAF, Osservatorio Astronomico di Teramo, Teramo, Italy; -22.5° Intercrater plains material 4 72° 144° 216° 288° icp 2 Department of Physical Sciences, The Open University, Milton Keynes, UK; ° Rough or gently rolling, densely cratered surfaces, encompassing also distal crater materials. 70 60 H14 - Debussy H13 - Neruda H12 - Michelangelo H11 - Discovery ° 5 3 270° 300° 330° 0° 30° spn Dipartimento di Scienze e Tecnologie, Università degli Studi di Napoli "Parthenope", Naples, Italy. Cyllene Solitudo Persephones Solitudo Promethei Solitudo Hermae -30° Trismegisti -65° 90° 270° Crater Materials icp H15 - Bach Australia Crater material–well preserved cfs -60° c3 180° Fresh craters with a sharp rim, textured ejecta blanket and pristine or sparsely cratered floor. 2 1:3,000,000 ° c2 80° 350 Crater material–degraded c2 spn M c3 Degraded craters with a subdued rim and a moderately cratered smooth to hummocky floor. -
Thirty-Six Dramatic Situations
G o zzi m a int a ine d th a t th ere ca n b e but thirty- six tra gic s a o s . e oo ea a s t o find o e h e was itu ti n Schill r t k gr t p in " m r , but e e . un abl e t o find eve n so m any as G ozzi . G o th Th e Thirty - Six Dram atic Situ ations GE ORGES POLTI Transl a ted by Lucil e R ay a o Fr nklin , Ohi J A M ES K NAPP H E R V E 1 9 2 4 PY H 1 9 1 6 1 9 1 7 CO RI G T , , T H E E D ITO R CO M PAN Y P H 1 92 1 CO YRI G T , JAM E S KN APP R E E VE 2 839 6 T H E T H I R TY - SI X D R AMAT I C SITUAT I ONS I NTR OD U CTI ON G o zzi m a int a in ed th a t th ere can b e but thirty - six tra gic s a o s . e o o ea a s t o fin o e h e itu ti n Schill r t k gr t p in d m r , but was a e s s un bl t o find even o m a ny a G o zzi . - Th irty six situations only ! There is , to me , some a thing t ntalizing about the assertion , unaccompanied as it is by any explanation either from Gozzi , or from Goethe or Schiller , and presenting a problem which it does not solve . -
Calcium Isotopes in Natural and Experimental Carbonated Silicate Melts
Western University Scholarship@Western Electronic Thesis and Dissertation Repository 2-27-2018 2:30 PM Calcium Isotopes in Natural and Experimental Carbonated Silicate Melts Matthew Maloney The University of Western Ontario Supervisor Bouvier, Audrey The University of Western Ontario Co-Supervisor Withers, Tony The University of Western Ontario Graduate Program in Geology A thesis submitted in partial fulfillment of the equirr ements for the degree in Master of Science © Matthew Maloney 2018 Follow this and additional works at: https://ir.lib.uwo.ca/etd Part of the Geochemistry Commons Recommended Citation Maloney, Matthew, "Calcium Isotopes in Natural and Experimental Carbonated Silicate Melts" (2018). Electronic Thesis and Dissertation Repository. 5256. https://ir.lib.uwo.ca/etd/5256 This Dissertation/Thesis is brought to you for free and open access by Scholarship@Western. It has been accepted for inclusion in Electronic Thesis and Dissertation Repository by an authorized administrator of Scholarship@Western. For more information, please contact [email protected]. Abstract The calcium stable isotopic compositions of mantle-sourced rocks and minerals were investigated to better understand the carbon cycle in the Earth’s mantle. Bulk carbonatites and kimberlites were analyzed to identify a geochemical signature of carbonatite magmatism, while inter-mineral fractionation was measured in co-existing Ca-bearing carbonate and silicate minerals. Bulk samples show a range of composition deviating from the bulk silicate Earth δ44/40Ca composition indicating signatures of magmatic processes or marine carbonate addition 44/40 to source materials. Δ Cacarbonate-silicate values range from -0.55‰ to +1.82‰ and positively correlate with Ca/Mg ratios in pyroxenes. -
N Arieuican%Mllsellm
n ARieuican%Mllsellm PUBLISHED BY THE AMERICAN MUSEUM OF NATURAL HISTORY CENTRAL PARK WEST AT 79TH STREET, NEW YORK 24, N.Y. NUMBER 2I63 DECEMBER I9, I963 The Pallasites BY BRIAN MASON' INTRODUCTION The pallasites are a comparatively rare type of meteorite, but are remarkable in several respects. Historically, it was a pallasite for which an extraterrestrial origin was first postulated because of its unique compositional and structural features. The Krasnoyarsk pallasite was discovered in 1749 about 150 miles south of Krasnoyarsk, and seen by P. S. Pallas in 1772, who recognized these unique features and arranged for its removal to the Academy of Sciences in St. Petersburg. Chladni (1794) examined it and concluded it must have come from beyond the earth, at a time when the scientific community did not accept the reality of stones falling from the sky. Compositionally, the combination of olivine and nickel-iron in subequal amounts clearly distinguishes the pallasites from all other groups of meteorites, and the remarkable juxtaposition of a comparatively light silicate mineral and heavy metal poses a nice problem of origin. Several theories of the internal structure of the earth have postulated the presence of a pallasitic layer to account for the geophysical data. No apology is therefore required for an attempt to provide a comprehensive account of this remarkable group of meteorites. Some 40 pallasites are known, of which only two, Marjalahti and Zaisho, were seen to fall (table 1). Of these, some may be portions of a single meteorite. It has been suggested that the pallasite found in Indian mounds at Anderson, Ohio, may be fragments of the Brenham meteorite, I Chairman, Department of Mineralogy, the American Museum of Natural History. -
Large Impact Basins on Mercury: Global Distribution, Characteristics, and Modification History from MESSENGER Orbital Data Caleb I
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 117, E00L08, doi:10.1029/2012JE004154, 2012 Large impact basins on Mercury: Global distribution, characteristics, and modification history from MESSENGER orbital data Caleb I. Fassett,1 James W. Head,2 David M. H. Baker,2 Maria T. Zuber,3 David E. Smith,3,4 Gregory A. Neumann,4 Sean C. Solomon,5,6 Christian Klimczak,5 Robert G. Strom,7 Clark R. Chapman,8 Louise M. Prockter,9 Roger J. Phillips,8 Jürgen Oberst,10 and Frank Preusker10 Received 6 June 2012; revised 31 August 2012; accepted 5 September 2012; published 27 October 2012. [1] The formation of large impact basins (diameter D ≥ 300 km) was an important process in the early geological evolution of Mercury and influenced the planet’s topography, stratigraphy, and crustal structure. We catalog and characterize this basin population on Mercury from global observations by the MESSENGER spacecraft, and we use the new data to evaluate basins suggested on the basis of the Mariner 10 flybys. Forty-six certain or probable impact basins are recognized; a few additional basins that may have been degraded to the point of ambiguity are plausible on the basis of new data but are classified as uncertain. The spatial density of large basins (D ≥ 500 km) on Mercury is lower than that on the Moon. Morphological characteristics of basins on Mercury suggest that on average they are more degraded than lunar basins. These observations are consistent with more efficient modification, degradation, and obliteration of the largest basins on Mercury than on the Moon. This distinction may be a result of differences in the basin formation process (producing fewer rings), relaxation of topography after basin formation (subduing relief), or rates of volcanism (burying basin rings and interiors) during the period of heavy bombardment on Mercury from those on the Moon. -
Voided Certificate of Employee Information Reports
Public Contracts Equal Employment Opportunity Compliance Monitoring Program Voided Certificate of Employee Information Report Report run on: June 6, 2017 3:22 PM Name of Company Cert Street City State Zip (PC) 2 HD 37407 245 EAST 30TH NEW YORK CITY NY 10016 1515 BOARDWALK, INC 18317 121 WASHINGTON ST TOMS RIVER NJ 08753 174 NEWARK AVENUE ASSOCIATES, LP 34742 103 EISENHOWER PARKWAY ROSELAND NJ 07068 1993-N2 PROPERTIES, NO. 3 LIMITED PARTNERSHI 19621 12100 WILSHIRE BLVD LOS ANGELES CA 90025 1ST CALL PAINTING CONTRACTORS, LLC 37000 980-B DEHART PLACE ELIZABETH NJ 07202 3-2-1 QUALITY PRINTING 21779 100 JERSEY AVENUE NEW BRUNSWICK NJ 08901 3-D MFG.-DBA- AMERICAN LA-FRANCE 2831 500 S. AIRPORT ROAD SHAWANO WI 54166 4 FRONT VIDEO DESIGN INC. 22299 1500 BROADWAY #509 NEW YORK NY 10036 55 WASHINGTON STREET LLC 28132 P.O. BOX 66 CLOSTER NJ 07624 9-15 SOUTH MAIN STREET CORP. 20587 1125 ATLANTIC AVE., SUITE 617 ATLANTIC CITY NJ 08401 A & A ENGINEERING 9780 300 CORPORATE CENTER DRIVE MANALAPAN NJ 07726 A & B WIPER SUPPLY, INC. 6848 116 FOUNTAIN ST. PHILADELPHIA PA 19127 A & E CARPENTRY, INC. 8048 584 STUDIO RD. RIDGEFIELD NJ 07657 A & L UNIFORMS, L L C 37818 2605 SOUTH BROAD STREET TRENTON NJ 08610 A & P TUTORING, LLC 34701 4201 CHURCH ROAD #242 MT. LAUREL NJ 08054 A & R AUTO SUPPLY, INC. 7169 300 ATLANTIC CITY BLVD. TOMS RIVER NJ 08757 A & S FUEL OIL CO. INC. 25667 95 CALAIS ROAD PO BOX 22 IRONIA NJ 07845 A & W TECHNICAL SALES, INC. 33404 420 COMMERCE LANE, SUITE 3 WEST BERLIN NJ 08091 A AND C LABORATORIES, INC 17387 168 W. -
Mysterious Mercury Bepicolumbo Heads for the World of Ice and Fire
A Digital Supplement to Astronomy Insights Astronomy Magazine © 2018 Kalmbach Media Mysterious Mercury BepiColumbo Heads for the World of Ice and Fire Dcember 2018 • Astronomy.com Voyage to a world Color explodes from Mercury’s surface in this enhanced-color mosaic taken through several filters. The yellow and orange hues signify relatively young plains likely formed when fluid lavas erupted from volcanoes. Medium- and dark-blue regions are older terrain, while the light-blue and white streaks represent fresh material excavated from relatively recent impacts. ALL IMAGES, UNLESS OTHERWISE NOTED: NASA/JHUAPL/CIW 2 ASTRONOMY INSIGHTS • DECEMBER 2018 A world of both fire and ice, Mercury excites and confounds scientists. The BepiColombo probe aims to make sense of this mysterious world. by Ben Evans of extremesWWW.ASTRONOMY.COM 3 Mercury is a land of contrasts. The solar system’s smallest planet boasts the largest core relative to its size. Temperatures at noon can soar as high as 800 degrees Fahrenheit (425 degrees Celsius) — hot enough to melt lead — but dip as low as –290 F (–180 C) before dawn. Mercury resides nearest the Sun, and it has the most eccentric orbit. At its closest, the planet lies only 29 mil- lion miles (46 million kilometers) from the Sun — less than one-third Earth’s distance — but swings out as far as 43 million miles (70 million km). Its rapid movement across our sky earned it a reputation among ancient skywatchers as the fleet-footed messenger of the gods: Italian scientist Giuseppe “Bepi” Colombo helped develop a technique for sending a space Hermes to the Greeks and Mercury to the Romans. -
Melania G. Mazzucco
Mamoli Zorzi and Manthorne (eds.) FROM DARKNESS TO LIGHT WRITERS IN MUSEUMS 1798-1898 Edited by Rosella Mamoli Zorzi and Katherine Manthorne From Darkness to Light explores from a variety of angles the subject of museum ligh� ng in exhibi� on spaces in America, Japan, and Western Europe throughout the nineteenth and twen� eth centuries. Wri� en by an array of interna� onal experts, these collected essays gather perspec� ves from a diverse range of cultural sensibili� es. From sensi� ve discussions of Tintore� o’s unique approach to the play of light and darkness as exhibited in the Scuola Grande di San Rocco in Venice, to the development of museum ligh� ng as part of Japanese ar� s� c self-fashioning, via the story of an epic American pain� ng on tour, museum illumina� on in the work of Henry James, and ligh� ng altera� ons at Chatsworth, this book is a treasure trove of illumina� ng contribu� ons. FROM DARKNESS TO LIGHT FROM DARKNESS TO LIGHT The collec� on is at once a refreshing insight for the enthusias� c museum-goer, who is brought to an awareness of the exhibit in its immediate environment, and a wide-ranging scholarly compendium for the professional who seeks to WRITERS IN MUSEUMS 1798-1898 proceed in their academic or curatorial work with a more enlightened sense of the lighted space. As with all Open Book publica� ons, this en� re book is available to read for free on the publisher’s website. Printed and digital edi� ons, together with supplementary digital material, can also be found at www.openbookpublishers.com Cover image: -
Rock Art of Latin America & the Caribbean
World Heritage Convention ROCK ART OF LATIN AMERICA & THE CARIBBEAN Thematic study June 2006 49-51 rue de la Fédération – 75015 Paris Tel +33 (0)1 45 67 67 70 – Fax +33 (0)1 45 66 06 22 www.icomos.org – [email protected] THEMATIC STUDY OF ROCK ART: LATIN AMERICA & THE CARIBBEAN ÉTUDE THÉMATIQUE DE L’ART RUPESTRE : AMÉRIQUE LATINE ET LES CARAÏBES Foreword Avant-propos ICOMOS Regional Thematic Studies on Études thématiques régionales de l’art Rock Art rupestre par l’ICOMOS ICOMOS is preparing a series of Regional L’ICOMOS prépare une série d’études Thematic Studies on Rock Art of which Latin thématiques régionales de l’art rupestre, dont America and the Caribbean is the first. These la première porte sur la région Amérique latine will amass data on regional characteristics in et Caraïbes. Ces études accumuleront des order to begin to link more strongly rock art données sur les caractéristiques régionales de images to social and economic circumstances, manière à préciser les liens qui existent entre and strong regional or local traits, particularly les images de l’art rupestre, les conditions religious or cultural traditions and beliefs. sociales et économiques et les caractéristiques régionales ou locales marquées, en particulier Rock art needs to be anchored as far as les croyances et les traditions religieuses et possible in a geo-cultural context. Its images culturelles. may be outstanding from an aesthetic point of view: more often their full significance is L’art rupestre doit être replacé autant que related to their links with the societies that possible dans son contexte géoculturel.