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37 results on '"G. Weigle"'

1. Color, Composition, and Thermal Environment of Kuiper Belt Object (486958) Arrokoth

Author: W. M. Grundy, M. K. Bird, D. T. Britt, J. C. Cook, D P Cruikshank, C. J. A. Howett, S Krijt, I R. Linscott, C. B. Olkin, A. H. Parker, S Protopapa, M Ruaud, O M Umurhan, L. A. Young, C M D Ore, J. J. Kavelaars, J T Keane, Y J Pendleton, S. B. Porter, F Scipioni, J R. Spencer, S. A. Stern, A J. Verbiscer, Harold Anthony Weaver, R P. Binzel, M W. Buie, B J Buratti, A Cheng, A. M. Earle, H A Elliott, L Gabasova, G R Gladstone, Matthew E. Hill, M Horanyi, D. E. Jennings, A W Lunsford, D J Mccomas, W B. McKinnon, R L. McNutt, Jr, J. M. Moore, J W Parker, E Quirico, D C Reuter, P M Schenk, B Schmitt, M R Showalter, K N. Singer, G Weigle, and A. M. Zangari
Subjects: Astrophysics
Abstract: The New Horizons spacecraft flew past the Kuiper Belt object (486958) Arrokoth (also known as 2014 MU69) in January 2019. Because of the great distance to the outer Solar System and limited bandwidth, it will take until late 2020 to downlink all the spacecraft's observations back to Earth. Three papers in this issue analyze recently downlinked data, including the highest-resolution images taken during the encounter (see the Perspective by Jewitt). Spencer et al. examined Arrokoth's geology and geophysics using stereo imaging, dated the surface using impact craters, and produced a geomorphological map. Grundy et al. investigated the composition of the surface using color imaging and spectroscopic data and assessed Arrokoth's thermal emission using microwave radiometry. McKinnon et al. used simulations to determine how Arrokoth formed: Two gravitationally bound objects gently spiraled together during the formation of the Solar System. Together, these papers determine the age, composition, and formation process of the most pristine object yet visited by a spacecraft.
Published: 2020
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2. Color, Composition, and Thermal Environment of Kuiper Belt Object (486958) Arrokoth

Author: Catherine B. Olkin, Dale P. Cruikshank, Simon B. Porter, Orkan M. Umurhan, Allen Lunsford, Silvia Protopapa, M. Ruaud, James Tuttle Keane, A. F. Cheng, Alex Parker, Mihaly Horanyi, Eric Quirico, Mark R. Showalter, Jeffrey M. Moore, D. E. Jennings, G. R. Gladstone, Francesca Scipioni, Bernard Schmitt, Amanda M. Zangari, Matthew E. Hill, Carly Howett, Ralph L. McNutt, S. A. Stern, John R. Spencer, William B. McKinnon, Marc W. Buie, L. Gabasova, Paul M. Schenk, D. C. Reuter, Kelsi N. Singer, G. Weigle, Anne J. Verbiscer, Joel Wm. Parker, Daniel T. Britt, Michael K. Bird, David J. McComas, H. A. Weaver, Leslie A. Young, H. A. Elliott, A. M. Earle, Yvonne J. Pendleton, Richard P. Binzel, Jason C. Cook, Ivan Linscott, William M. Grundy, Sebastiaan Krijt, C. M. Dalle Ore, Bonnie J. Buratti, Jj Kavelaars, Lowell Observatory [Flagstaff], NASA Ames Research Center (ARC), Southwest Research Institute [Boulder] (SwRI), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), French Centre National d'Etudes Spatiales (CNES), and Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences
Subjects: Solar System, Materials science, 010504 meteorology & atmospheric sciences, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Mineralogy, chemistry.chemical_element, FOS: Physical sciences, Radiation, 01 natural sciences, Spectral line, Methane, Kuiper belt, chemistry.chemical_compound, ices, Arrokoth, 0103 physical sciences, Thermal, 010303 astronomy & astrophysics, Physics::Atmospheric and Oceanic Physics, 0105 earth and related environmental sciences, 2014 MU69, methanol, Earth and Planetary Astrophysics (astro-ph.EP), CH3OH, Multidisciplinary, surface composition, New Horizons spacecraft, color, chemistry, 13. Climate action, Brightness temperature, Astrophysics::Earth and Planetary Astrophysics, Carbon, Microwave, Astrophysics - Earth and Planetary Astrophysics
Abstract: The outer Solar System object (486958) Arrokoth (provisional designation 2014 MU69) has been largely undisturbed since its formation. We studied its surface composition using data collected by the New Horizons spacecraft. Methanol ice is present along with organic material, which may have formed through irradiation of simple molecules. Water ice was not detected. This composition indicates hydrogenation of carbon monoxide-rich ice and/or energetic processing of methane condensed on water ice grains in the cold, outer edge of the early Solar System. There are only small regional variations in color and spectra across the surface, which suggests that Arrokoth formed from a homogeneous or well-mixed reservoir of solids. Microwave thermal emission from the winter night side is consistent with a mean brightness temperature of 29 ± 5 kelvin. ©2020, NASA (contract no. NASW-02008), NASA (grant no. NAS5-97271 / TaskOrder30)
Published: 2020
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3. Detecting Upward Directed Charged Particle Fluxes in the Mars Science Laboratory Radiation Assessment Detector

Author: Arik Posner, Robert F. Wimmer-Schweingruber, Cesar Martin, Bent Ehresmann, Cary Zeitlin, J. K. Appel, Sönke Burmeister, David E. Brinza, Günther Reitz, J. Peterson, Jingnan Guo, Donald M. Hassler, E. Böhm, Stephan Böttcher, Henning Lohf, S. C. R. Rafkin, G. Weigle, Daniel Matthiä, and Jan Koehler
Subjects: Physics, 010504 meteorology & atmospheric sciences, Cosmic ray, Geophysics, Atmosphere of Mars, Mars Exploration Program, Martian soil, Environmental Science (miscellaneous), Radiation, Radiation assessment detector, 01 natural sciences, Charged particle, Martian surface, 0103 physical sciences, General Earth and Planetary Sciences, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Remote sensing
Abstract: The Mars Science Laboratory rover Curiosity, operating on the surface of Mars, is exposed to radiation fluxes from above and below. Galactic Cosmic Rays travel through the Martian atmosphere, producing a modified spectrum consisting of both primary and secondary particles at ground level. These particles produce an upward directed secondary particle spectrum as they interact with the Martian soil. Here we develop a method to distinguish the upward and downward directed particle fluxes in the Radiation Assessment Detector (RAD) instrument, verify it using data taken during the cruise to Mars, and apply it to data taken on the Martian surface. We use a combination of Geant4 and Planetocosmics modeling to find discrimination criteria for the flux directions. After developing models of the cruise phase and surface shielding conditions, we compare model-predicted values for the ratio of upward to downward flux with those found in RAD observation data. Given the quality of available information on Mars Science Laboratory spacecraft and rover composition, we find generally reasonable agreement between our models and RAD observation data. This demonstrates the feasibility of the method developed and tested here. We additionally note that the method can also be used to extend the measurement range and capabilities of the RAD instrument to higher energies.
Published: 2018

4. Initial results from the New Horizons exploration of 2014 MU 69 , a small Kuiper Belt object

Author: J. Fischetti, S. Bhaskaran, Matthias Hahn, Karl Whittenburg, Derek S. Nelson, G. A. Griffith, Amanda M. Zangari, B. J. Buratti, James T. Keane, E. J. Lessac-Chenen, Ralph L. McNutt, Tiffany J. Finley, J. Scherrer, M. A. Ritterbush, M. M. Saina, G. Dunn, T. A. Hill, J. Van Eck, T. Stryk, J. M. Albers, D. C. Reuter, C. M. Dalle Ore, H. A. Elliott, D. J. Schultz, J. Andrews, Douglas P. Hamilton, M. H. Versteeg, Orkan M. Umurhan, Matthew E. Hill, Hai Nguyen, M. Simon, L. Gabasova, D. E. Jennings, D. J. Katz, J. E. Riedel, N. Behrooz, M. N. Fosbury, Henry B. Throop, A. J. Verbiscer, E. Bernardoni, Ross A. Beyer, C. Engelbrecht, Francesca Scipioni, H. L. Winters, Thomas H. Zurbuchen, Carey M. Lisse, Veronica J. Bray, M. G. Ryschkewitsch, Stuart J. Robbins, S. E. Jaskulek, M. C. Kochte, Thomas Mehoke, M. S. Lahr, M. J. Salinas, V. A. Mallder, S. P. Williams, B. H. May, D. M. Mages, C. C. Deboy, Simon B. Porter, Gerhard Kruizinga, Marc W. Buie, Jorge I. Nunez, John Hayes, Peter Kollmann, P. Dharmavaram, J. M. Moore, Darrell F. Strobel, John Stansberry, R. P. Binzel, H. M. Hart, Jillian Redfern, E. W. Stahlheber, H. K. Kang, James L. Green, Anthony F. Egan, Carly Howett, Fran Bagenal, Dale Stanbridge, Chris B. Hersman, C. L. Chavez, Debi Rose, J. Y. Pelgrift, Maria E. Banks, D. C. Schurr, Matthew R. Buckley, L. S. Turner, Ivan Linscott, Kaj E. Williams, J. Eisig, Mihaly Horanyi, Matthew Jones, Mark R. Showalter, William B. McKinnon, Leslie A. Young, E. J. Colwell, Daniel T. Britt, Kirby Runyon, David J. McComas, G. Weigle, Bernard Schmitt, Susan D. Benecchi, Alissa M. Earle, M. J. Kinczyk, Tod R. Lauer, M. R. Piquette, Lori S. Glaze, Carver J. Bierson, L. M. Burke, Brian Carcich, O. S. Custodio, A. Harch, Harold A. Weaver, Dale P. Cruikshank, Oliver L. White, L. E. Brown, William M. Grundy, G. K. Oxton, Chelsea L. Ferrell, David E. Kaufmann, Mohamed Ramy El-Maarry, K. A. Harmon, W. R. Schlei, Eric Quirico, Derek C. Richardson, J. M. Freeze, Jennifer Hanley, R. G. Shelton, Andrew J. Steffl, Mike Bird, H. W. Taylor, Harold J. Reitsema, Stamatios M. Krimigis, D. R. Boone, E. D. Fattig, A. L. Regiec, D. J. Rodgers, Jason D. Hofgartner, D. Velez, Catherine B. Olkin, Kelsi N. Singer, Brian Bauer, Carl J. Ercol, Martin Pätzold, Nicole Martin, Stewart Bushman, J. Firer, Allen W. Lunsford, R. W. Webbert, A. L. Chaikin, Alex Parker, C. A. Conrad, M. P. Conner, S. B. Cooper, Chloe B. Beddingfield, William M. Folkner, J. E. Lee, M. B. Tapley, G. R. Gladstone, D. A. Aguilar, Glen H. Fountain, Emma Birath, Rebecca Sepan, Jeremy Bauman, J. Wm. Parker, S. Weidner, J. R. Jensen, Jason C. Cook, Alan D. Howard, William M. Owen, Andrew F. Cheng, B. L. Enke, Sarah A. Hamilton, Tom Andert, K. B. Beisser, K. E. Bechtold, J. R. Wendel, Rajani D. Dhingra, Paul M. Schenk, Michael E. Summers, J. R. Spencer, D. W. Hals, Silvia Protopapa, A. C. Ocampo, Mark E. Holdridge, S. A. Stern, A. Taylor, R. M. Tedford, G. P. Keleher, Gabe Rogers, Frederic Pelletier, Jj Kavelaars, Yanping Guo, Jon Pineau, Steven J. Conard, Alice Bowman, A. Hosadurga, B. G. Williams, Michael Vincent, David Y. Kusnierkiewicz, Paul E. Rosendall, G. B. Lawrence, J. R. Stuart, M. M. Stothoff, Jr. D. S. Mehoke, Southwest Research Institute [Boulder] (SwRI), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Lowell Observatory [Flagstaff], Space Physics Research Laboratory [Ann Arbor] (SPRL), University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, SwRI Planetary Science Directorate [Boulder], Universitat de Lleida, Institut für Raumfahrttechnik, Universität der Bundeswehr München [Neubiberg], Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], Department of Space Studies [Boulder], Rheinische Friedrich-Wilhelms-Universität Bonn, Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Institute of Hydrology, NASA Goddard Space Flight Center (GSFC), Department of Physics, Chemistry and Biology [Linköping] (IFM), Linköping University (LIU), Africa Rice Center [Bénin] (AfricaRice), Africa Rice Center [Côte d'Ivoire] (AfricaRice), Consultative Group on International Agricultural Research [CGIAR] (CGIAR)-Consultative Group on International Agricultural Research [CGIAR] (CGIAR), Yonsei University, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Centre International de Hautes Etudes Agronomiques Méditerranéennes - Institut Agronomique Méditerranéen de Montpellier (CIHEAM-IAMM), Centre International de Hautes Études Agronomiques Méditerranéennes (CIHEAM), Princeton University, Reed College, Hanoi National University of Education (HNUE), Rhenish Institute for Environmental Research (RIU), University of Cologne, School of Earth, Atmospheric and Environmental Sciences [Manchester] (SEAES), University of Manchester [Manchester], ESA, Southwest Research Institute [San Antonio] (SwRI), NASA Ames Research Center (ARC), Laboratoire pour l'utilisation du rayonnement électromagnétique (LURE), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-MENRT-Centre National de la Recherche Scientifique (CNRS), Lunar and Planetary Laboratory [Tucson] (LPL), University of Arizona, Johns Hopkins University (JHU), Institute of Physics of the Czech Academy of Sciences (FZU / CAS), Czech Academy of Sciences [Prague] (CAS), Laboratoire de Chimie Analytique Bio-Inorganique et Environnement (LCABIE), Université de Pau et des Pays de l'Adour (UPPA)-Centre National de la Recherche Scientifique (CNRS), Department of Biochemistry, Faculty of Biology, University of Warmia and Mazury [Olsztyn], California Institute of Technology (CALTECH)-NASA, Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), University of Warmia and Mazury, Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), inconnu temporaire UPEMLV, Inconnu, INGENIERIE (INGENIERIE), Institut de recherches sur la catalyse et l'environnement de Lyon (IRCELYON), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Génie des Procédés Plasmas et Traitement de Surface (ENSCP), PARIS, Africa Rice Center, Africa Rice Center (AfricaRice), Institut de pharmacologie moléculaire et cellulaire (IPMC), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Centre National de la Recherche Scientifique (CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Institute of Physics of Academy of Sciences of Czech Republic, and Czech Academy of Sciences [Prague] (ASCR)
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Solar System, Multidisciplinary, 010504 meteorology & atmospheric sciences, Spacecraft, business.industry, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], FOS: Physical sciences, Astronomy, Coma (optics), Contact binary, Albedo, 01 natural sciences, Object (philosophy), Solar wind, 13. Climate action, 0103 physical sciences, Pebble, business, 010303 astronomy & astrophysics, Geology, ComputingMilieux_MISCELLANEOUS, Astrophysics - Earth and Planetary Astrophysics, 0105 earth and related environmental sciences
Abstract: The Kuiper Belt is a distant region of the Solar System. On 1 January 2019, the New Horizons spacecraft flew close to (486958) 2014 MU69, a Cold Classical Kuiper Belt Object, a class of objects that have never been heated by the Sun and are therefore well preserved since their formation. Here we describe initial results from these encounter observations. MU69 is a bi-lobed contact binary with a flattened shape, discrete geological units, and noticeable albedo heterogeneity. However, there is little surface color and compositional heterogeneity. No evidence for satellites, ring or dust structures, gas coma, or solar wind interactions was detected. By origin MU69 appears consistent with pebble cloud collapse followed by a low velocity merger of its two lobes., 43 pages, 8 figure
Published: 2019

5. Excesses in the low-mass Higgs-boson search and the $$\varvec{W}$$ W -boson mass measurement

Author: T. Biekötter, S. Heinemeyer, and G. Weiglein
Subjects: Astrophysics, QB460-466, Nuclear and particle physics. Atomic energy. Radioactivity, QC770-798
Abstract: Abstract The CDF collaboration recently reported a measurement of the W-boson mass $$M_W$$ M W whose value shows a large upward deviation from the Standard Model (SM) prediction. The question arises whether such large values of $$M_W$$ M W could be accommodated in extensions of the SM without violating other constraints and which phenomenological consequences this would have. A different type of deviation from the SM has been observed experimentally in the searches for light Higgs bosons. CMS has observed two excesses with a local significance of about $$3\,\sigma $$ 3 σ in the $$\gamma \gamma $$ γ γ and $$\tau ^+\tau ^-$$ τ + τ - final states for a hypothetical Higgs-boson mass of approximately 95 GeV. These two excesses are compatible with the corresponding ATLAS limits. Earlier an excess was also observed in the Higgs-boson searches at LEP in the $$b {\bar{b}}$$ b b ¯ final state at the local $$2\,\sigma $$ 2 σ confidence level at about the same mass. It was shown recently that the three excesses can be accommodated in a Two-Higgs-Doublet Model that is extended with a real singlet (N2HDM) of Yukawa type IV, while being in agreement with all other theoretical and experimental constraints. We demonstrate here that the region of the parameter space that describes the three excesses can also give rise to a large contribution to $$M_W$$ M W in agreement with the recent CDF measurement. We discuss further phenomenological consequences of this scenario.
Published: 2023
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6. Imaging and spectral performance of the New Horizons Ralph instrument during the 2015 Pluto encounter (Conference Presentation)

Author: Dennis C. Reuter, Tony B. Hull, Pascal Hallibert, Dae Wook Kim, S. Alan Stern, G. Weigle, Catherine B. Olkin, Allen W. Lunsford, and Donald E. Jennings
Subjects: Telescope, Pluto, Geography, New horizons, law, Visible imaging, High spatial resolution, Astronomy, Astrophysics, law.invention
Abstract: The Ralph instrument on the New Horizons mission consists of a telescope that feeds two focal planes: the Multi-spectral Visible Imaging Camera (MVIC), a visible, near-IR imager and the Linear Etalon Imaging Spectral Array (LEISA), a short-wavelength IR spectral imager. During the encounter with the Pluto system in 2015, Ralph operated as expected collecting numerous high spatial resolution images of the main components of the system, Pluto and Charon, as well as the four much smaller objects Hydra, Kerberos, Nix and Styx. New Horizons, launched on January 19, 2006, is the first mission to explore Kuiper Belt Objects (KBOs).
Published: 2017

7. New Horizons DataTrack Tool for Playback Planning and Sequencing

Author: B. Enke, Catherine B. Olkin, Emma Birath, Tiffany J. Finley, Kendall Kaufmann, Kimberly Ennico, Zach Dischner, Leslie A. Young, Brian T. Carcich, A. Harch, G. Weigle, and Stephen P. Williams
Subjects: New horizons, Computer science, Computer graphics (images)
Published: 2016

8. Surface compositions across Pluto and Charon

Author: Dale P. Cruikshank, Marc W. Buie, William M. Grundy, John R. Spencer, C. M. Dalle Ore, Bonnie J. Buratti, J. Wm. Parker, Silvia Protopapa, Henry B. Throop, Andrew F. Cheng, Bernard Schmitt, C. C. C. Tsang, A. J. Verbiscer, Catherine B. Olkin, Allen W. Lunsford, Jason C. Cook, Leslie A. Young, Paul M. Schenk, John Stansberry, Harold A. Weaver, Ivan Linscott, Eric Quirico, Kimberly Ennico, S. Philippe, Kelsi N. Singer, D. E. Jennings, G. Weigle, Alissa M. Earle, Alex Parker, Ross A. Beyer, Carly Howett, D. C. Reuter, Richard P. Binzel, S. A. Stern, Lowell Observatory [Flagstaff], Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), NASA Ames Research Center (ARC), Southwest Research Institute [Boulder] (SwRI), University of Victoria [Canada] (UVIC), Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University-Smithsonian Institution, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), NASA Goddard Space Flight Center (GSFC), and SwRI Planetary Science Directorate [Boulder]
Subjects: 010504 meteorology & atmospheric sciences, Outcrop, FOS: Physical sciences, 01 natural sciences, Charon, Astrobiology, Latitude, Impact crater, 0103 physical sciences, Glacial period, Ejecta, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Pluton, geography, Multidisciplinary, geography.geographical_feature_category, Bedrock, Pluto, Surface, New Horizons mission, composition, [SDU]Sciences of the Universe [physics], Protoplanet, Astrophysics - Earth and Planetary Astrophysics
Abstract: The New Horizons spacecraft mapped colors and infrared spectra across the encounter hemispheres of Pluto and Charon. The volatile ices CH$_4$, CO, and N$_2$, that dominate Pluto's surface, have complicated spatial distributions resulting from sublimation, condensation, and glacial flow acting over seasonal and geological timescales. Pluto's H$_2$O ice "bedrock" is also mapped, with isolated outcrops occurring in a variety of settings. Pluto's surface exhibits complex regional color diversity associated with its distinct provinces. Charon's color pattern is simpler, dominated by neutral low latitudes and a reddish northern polar region. Charon near infrared spectra reveal highly localized areas with strong NH$_3$ absorption tied to small craters with relatively fresh-appearing impact ejecta., Comment: in Science 351, aad9189 (2016)
Published: 2016

9. Calibration and Characterization of the Radiation Assessment Detector (RAD) on Curiosity

Author: Yoshiyuki Iwata, T. Murakami, Donald M. Hassler, E. Böhm, Thomas Berger, Sönke Burmeister, Cary Zeitlin, Hisashi Kitamura, David E. Brinza, G. Weigle, S. Rafkin, Daniel Matthiä, Jingnan Guo, Y. Tyler, Bent Ehresmann, Günther Reitz, Henning Lohf, A. Posner, Stephan Böttcher, Robert F. Wimmer-Schweingruber, Jan Köhler, M. Vincent, Cesar Martin, and J. K. Appel
Subjects: Physics, Solar particle events, 010504 meteorology & atmospheric sciences, Payload, Space radiation dosimetry, Curiosity rover, Astrophysics::Instrumentation and Methods for Astrophysics, Mars, Astronomy and Astrophysics, Cosmic ray, Mars Exploration Program, Scintillator, Radiation assessment detector, Galactic cosmic rays, 01 natural sciences, Particle detector, Energetic particle radiation, Space and Planetary Science, Physics::Space Physics, 0103 physical sciences, Calibration, Dosimetry, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Remote sensing
Abstract: The Radiation Assessment Detector, RAD, is one of the ten instruments that make up the science payload of the Mars Science Laboratory Curiosity rover. RAD is an energetic particle detector, capable of measuring the charged and neutral particles that make significant contributions to the radiation dose that will be received by future human explorers when they visit Mars. Prior to the launch of MSL in November 2011, RAD and its near-identical twin flight spare unit were calibrated using laboratory sources, charged particle beams, and neutron fields. The initial calibration parameters obtained in these tests were used for real-time data analysis by the instrument’s onboard software. These parameters have subsequently been refined using data obtained during the cruise to Mars and during Curiosity’s mission on the surface of Mars. The most critical use of calibration is in the dosimetry analysis performed onboard. Calibration is also used in onboard analysis to determine which events should be stored for telemetry to Earth. Accelerator data obtained with the flight spare unit after Curiosity was launched provide detailed information about the response of the organic and inorganic scintillators to ion beams over a wide range of charge and energy. Here we report on the methods used to determine calibration parameters, the results obtained, as well as providing an overview of the modifications to the instrument’s software and configuration that have been made over the course of the mission.
Published: 2016

10. Inflight Radiometric Calibration of New Horizons' Multispectral Visible Imaging Camera (MVIC)

Author: Ross A. Beyer, Bonnie J. Buratti, Carly Howett, R. P. Binzel, Silvia Protopapa, Joel Wm. Parker, Dale P. Cruikshank, G. Weigle, Harold A. Weaver, A.L. Graps, S. A. Stern, Paul M. Schenk, Alissa M. Earle, Marc W. Buie, Bernard Schmitt, S. Phillippe, Constantine Tsang, Alex Parker, Kelsi N. Singer, D. C. Reuter, C. M. Dalle Ore, Catherine B. Olkin, Andrew F. Cheng, Allen W. Lunsford, D. E. Jennings, Eric Quirico, K.P. Harrison, Simon B. Porter, John R. Spencer, Kimberly Ennico, Leslie A. Young, Jason C. Cook, William M. Grundy, Ivan Linscott, Henry B. Throop, J. R. Lovering, A. J. Verbiscer, and John Stansberry
Subjects: 010504 meteorology & atmospheric sciences, Multispectral image, FOS: Physical sciences, Field of view, 01 natural sciences, Optics, 0103 physical sciences, Calibration, 010303 astronomy & astrophysics, Radiometric calibration, Instrumentation and Methods for Astrophysics (astro-ph.IM), 0105 earth and related environmental sciences, Remote sensing, Earth and Planetary Astrophysics (astro-ph.EP), Pixel, business.industry, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Planetary Data System, Panchromatic film, Space and Planetary Science, Environmental science, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, business, Astrophysics - Earth and Planetary Astrophysics
Abstract: © 2016 Elsevier Inc. We discuss two semi-independent calibration techniques used to determine the inflight radiometric calibration for the New Horizons’ Multi-spectral Visible Imaging Camera (MVIC). The first calibration technique compares the measured number of counts (DN) observed from a number of well calibrated stars to those predicted using the component-level calibration. The ratio of these values provides a multiplicative factor that allows a conversation between the preflight calibration to the more accurate inflight one, for each detector. The second calibration technique is a channel-wise relative radiometric calibration for MVIC's blue, near-infrared and methane color channels using Hubble and New Horizons observations of Charon and scaling from the red channel stellar calibration. Both calibration techniques produce very similar results (better than 7% agreement), providing strong validation for the techniques used. Since the stellar calibration described here can be performed without a color target in the field of view and covers all of MVIC's detectors, this calibration was used to provide the radiometric keyword values delivered by the New Horizons project to the Planetary Data System (PDS). These keyword values allow each observation to be converted from counts to physical units; a description of how these keyword values were generated is included. Finally, mitigation techniques adopted for the gain drift observed in the near-infrared detector and one of the panchromatic framing cameras are also discussed.
Published: 2016
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11. Mounting evidence for a 95 GeV Higgs boson

Author: T. Biekötter, S. Heinemeyer, and G. Weiglein
Subjects: Multi-Higgs Models, Specific BSM Phenomenology, Nuclear and particle physics. Atomic energy. Radioactivity, QC770-798
Abstract: Abstract In 2018 CMS reported an excess in the light Higgs-boson search in the diphoton decay mode at about 95 GeV based on Run 1 and first year Run 2 data. The combined local significance of the excess was 2.8 σ. The excess is compatible with the limits obtained in the ATLAS searches from the diphoton search channel. Recently, CMS reported another local excess with a significance of 3.1 σ in the light Higgs-boson search in the di-tau final state, which is compatible with the interpretation of a Higgs boson with a mass of about 95 GeV. We show that the observed results can be interpreted as manifestations of a Higgs boson in the Two-Higgs Doublet Model with an additional real singlet (N2HDM). We find that the lightest Higgs boson of the N2HDM can fit both excesses simultaneously, while the second-lightest state is such that it satisfies the Higgs-boson measurements at 125 GeV, and the full Higgs-boson sector is compatible with all Higgs exclusion bounds from the searches at LEP, the Tevatron and the LHC as well as with other theoretical and experimental constraints. Finally, we demonstrate that it is furthermore possible to accommodate the excesses observed by CMS in the two search channels together with a local 2.3 σ excess in the b b ¯ $$ b\overline{b} $$ final state observed at LEP in the same mass range.
Published: 2022
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12. The Pluto system: Initial results from its exploration by New Horizons

Author: Darrell F. Strobel, James L. Green, Mark R. Showalter, Francis Nimmo, C. Bryan, Richard P. Binzel, M. J. Freeze, Matthew R. Buckley, Matthew E. Hill, Stewart Bushman, Chris B. Hersman, Brian Carcich, Kirby Runyon, Leslie A. Young, Douglas S. Mehoke, Jeremy Bauman, S. Weidner, Nickalaus Pinkine, William M. Grundy, Robert A. Jacobson, V. A. Mallder, Thomas K. Greathouse, H. K. Kang, Ralph L. McNutt, S. Bhaskaran, Dale P. Cruikshank, Marc W. Buie, D. C. Reuter, William M. Owen, Andrew F. Cheng, Peter D. Bedini, C. M. Dalle Ore, Mihaly Horanyi, Alice Bowman, Tiffany J. Finley, David P. Hinson, Harold A. Weaver, David J. McComas, Max Mutchler, Yanping Guo, Oliver L. White, R. W. Webbert, D. E. Jennings, Olivier S. Barnouin, Jennifer Hanley, Harold J. Reitsema, B. Page, K. L. Lindstrom, Catherine B. Olkin, Jorge I. Nunez, M. E. Banks, Carey M. Lisse, A. Hill, John R. Spencer, Coralie D. Jackman, G. R. Gladstone, E. D. Melin, Allen W. Lunsford, M. H. Versteeg, Eric J. Zirnstein, Emma Birath, Thomas Mehoke, Joel Wm. Parker, H. M. Hart, Jane M. Andrews, Zach Dischner, Derek S. Nelson, Amanda M. Zangari, Kurt D. Retherford, Veronica J. Bray, Andrew J. Steffl, M. Piquette, Douglas P. Hamilton, Mike Bird, Stamatios M. Krimigis, Kaj E. Williams, Matthias Hahn, Karl Whittenburg, C. A. Conrad, Kelsi N. Singer, Steven J. Conard, J. E. Lee, Silvia Protopapa, B. G. Williams, Constantine Tsang, Orkan M. Umurhan, Kimberly Ennico, Glen H. Fountain, J. M. Moore, Carolyn M. Ernst, J. Peterson, J. Ercol, Jason C. Cook, Alan D. Howard, H. A. Elliott, Michael Vincent, David Y. Kusnierkiewicz, O. S. Custodio, M. G. Ryschkewitsch, Sarah A. Hamilton, D. J. Bogan, Eric Schindhelm, M. Brozovic, K. B. Beisser, Mark E. Holdridge, James H. Roberts, S. A. Stern, M. B. Tapley, Simon B. Porter, A. Harch, W. W. Woods, B. Bauer, Debi Rose, S. P. Williams, Alex Parker, Philip J. Dumont, Sarah H. Flanigan, Gabe Rogers, Dale Stanbridge, Ivan Linscott, Frederic Pelletier, B. Sepan, Andrew B. Calloway, Jamey Szalay, Tod R. Lauer, Jillian Redfern, Martin Paetzold, Tom Andert, A. J. Verbiscer, Paul M. Schenk, Nicole Martin, Michael E. Summers, Stuart J. Robbins, H. W. Taylor, A. C. Ocampo, Bonnie J. Buratti, A. Taylor, William B. McKinnon, G. Weigle, Alissa M. Earle, David E. Kaufmann, M. Soluri, T. Stryk, Henry B. Throop, Fran Bagenal, G. L. Tyler, Ross A. Beyer, C. C. Deboy, Peter Kollmann, Carly Howett, and Joshua A. Kammer
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), geography, Multidisciplinary, geography.geographical_feature_category, Haze, Landform, FOS: Physical sciences, Terrain, Crust, Astrobiology, Atmosphere, Pluto, Tectonics, Planet, Geology, Astrophysics - Earth and Planetary Astrophysics
Abstract: The Pluto system was recently explored by NASA's New Horizons spacecraft, making closest approach on 14 July 2015. Pluto's surface displays diverse landforms, terrain ages, albedos, colors, and composition gradients. Evidence is found for a water-ice crust, geologically young surface units, surface ice convection, wind streaks, volatile transport, and glacial flow. Pluto's atmosphere is highly extended, with trace hydrocarbons, a global haze layer, and a surface pressure near 10 microbars. Pluto's diverse surface geology and long-term activity raise fundamental questions about how small planets remain active many billions of years after formation. Pluto's large moon Charon displays tectonics and evidence for a heterogeneous crustal composition, its north pole displays puzzling dark terrain. Small satellites Hydra and Nix have higher albedos than expected., 8 pages - Initial Science paper from NASA's New Horizons Pluto Encounter
Published: 2015

13. Possible indications for new Higgs bosons in the reach of the LHC: N2HDM and NMSSM interpretations

Author: T. Biekötter, A. Grohsjean, S. Heinemeyer, C. Schwanenberger, and G. Weiglein
Subjects: Astrophysics, QB460-466, Nuclear and particle physics. Atomic energy. Radioactivity, QC770-798
Abstract: Abstract In several searches for additional Higgs bosons at the LHC, in particular in a CMS search exploring decays to pairs of top quarks, $$t\bar{t}$$ t t ¯ , and in an ATLAS search studying tau leptons, $$\tau ^+\tau ^-$$ τ + τ - , local excesses of about $$3\,\sigma $$ 3 σ standard deviations or above have been observed at a mass scale of approximately $$ 400 \,\text {GeV}$$ 400 GeV . We investigate to what extent a possible signal in these channels could be accommodated in the Next-to-Two-Higgs-Doublet Model (N2HDM) or the Next-to Minimal Supersymmetric Standard Model (NMSSM). In a second step we analyze whether such a model could be compatible with both a signal at around $$400\,\text {GeV}$$ 400 GeV and $$96\,\text {GeV}$$ 96 GeV , where the latter possibility is motivated by observed excesses in searches for the $$b \bar{b}$$ b b ¯ final state at LEP and the di-photon final state at CMS. The analysis for the N2HDM reveals that the observed excesses at $$400 \,\text {GeV}$$ 400 GeV in the $$t\bar{t}$$ t t ¯ and $$\tau ^+\tau ^-$$ τ + τ - channels point towards different regions of the parameter space, while one such excess and an additional Higgs boson at around $$96\,\text {GeV}$$ 96 GeV could simultaneously be accommodated. In the context of the NMSSM an experimental confirmation of a signal in the $$t\bar{t}$$ t t ¯ final state would favour the alignment-without-decoupling limit of the model, where the Higgs boson at $$125\,\text {GeV}$$ 125 GeV could be essentially indistinguishable from the Higgs boson of the standard model. In contrast, a signal in the $$\tau ^+\tau ^-$$ τ + τ - channel can only be accommodated outside of this limit, and parts of the investigated parameter space could be probed with Higgs signal-rate measurements at the (HL-)LHC.
Published: 2022
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14. Measurements of the neutron spectrum on the Martian surface with MSL/RAD

Author: Günther Reitz, Sönke Burmeister, Jan Köhler, Cesar Martin, S. Rafkin, Jingnan Guo, Stephan Böttcher, G. Weigle, Robert F. Wimmer-Schweingruber, J. K. Appel, Cary Zeitlin, David E. Brinza, O. Kortmann, Bent Ehresmann, Arik Posner, E. Böhm, and Donald M. Hassler
Subjects: Martian, Physics, Equivalent dose, business.industry, Gamma ray, Mars, Mars Exploration Program, Radiation, Radiation assessment detector, Computational physics, Geophysics, Optics, neutron, Space and Planetary Science, Geochemistry and Petrology, Martian surface, dose rate, Earth and Planetary Sciences (miscellaneous), Neutron, gamma, business
Abstract: The Radiation Assessment Detector (RAD), onboard the Mars Science Laboratory (MSL) rover Curiosity, measures the energetic charged and neutral particles and the radiation dose rate on the surface of Mars. An important factor for determining the biological impact of the Martian surface radiation is the specific contribution of neutrons, with their deeper penetration depth and ensuing high biological effectiveness. This is very difficult to measure quantitatively, resulting in considerable uncertainties in the total radiation dose. In contrast to charged particles, neutral particles (neutrons and gamma rays) are generally only measured indirectly. Measured spectra are a complex convolution of the incident particle spectrum with the detector response function and must be unfolded. We apply an inversion method (based on a maximum likelihood estimation) to calculate the neutron and gamma spectra from the RAD neutral particle measurements. Here we show the first spectra on the surface of Mars and compare them to theoretical predictions. The measured neutron spectrum (ranging from 8 to 740 MeV) translates into a radiation dose rate of 14±4μGy/d and a dose equivalent rate of 61±15μSv/d. This corresponds to 7% of the measured total surface dose rate and 10% of the biologically relevant surface dose equivalent rate on Mars. Measuring the Martian neutron and gamma spectra is an essential step for determining the mutagenic influences to past or present life at or beneath the Martian surface as well as the radiation hazard for future human exploration, including the shielding design of a potential habitat.
Published: 2014

15. Volatile and Organic Compositions of Sedimentary Rocks in Yellowknife Bay, Gale Crater, Mars

Author: M. A. Meyer, Mark I. Richardson, Robert C. Anderson, Marisa C. Palucis, Sara Navarro Lopez, Rodney C. Ewing, Sanjeev Gupta, Caroline Freissinet, Edward M. Stolper, James F. Bell, M. A. Ravine, I. G. Mitrofanov, Thomas F. Bristow, Dawn Y. Sumner, Joel A. Hurowitz, Robert M. Haberle, Claire E. Newman, Andrew Steele, Muriel Saccoccio, Leslie Keely, E. Pallier, Jason P. Dworkin, Claude Geffroy, Mary A. Voytek, Michael Caplinger, Fred Goesmann, Yann Parot, Maria-Paz Zorzano Mier, A. B. Sanin, S. W. Squyres, Javier Caride Rodriguez, J. L. Griffes, Julio José Romeral-Planello, Jason Feldman, Katherine L. French, V. Sautter, Nicolas Mangold, David L. Bish, Vivian Lafaille, Michael D. Smith, François Raulin, V. Prokhorov, Gilles Berger, S. Slavney, Heather B. Franz, S. Johnstone, Susanne P. Schwenzer, Felipe Gómez, Harri Haukka, Francis A. Cucinotta, J. Hudgins, T. Cleghorn, Pascaline Francois, Alain Lepinette Malvitte, Shuai Li, Paul R. Mahaffy, K. M. Robertson, Bruce M. Jakosky, J. Guo, Juergen Schieber, Rafael Navarro-González, G. J. Flesch, Scott M. McLennan, Jennifer G. Blank, M. Carmosino, Kenneth A. Farley, Yves Langevin, P. D. Archer, A. E. Brunner, M. D. Dyar, S. Le Mouélic, V. Hipkin, Sara Alejandra Sans Fuentes, Kenneth S. Edgett, Sabrina Feldman, Gale Paulsen, Paul Herrera, Alberto G. Fairén, Kirsten L. Siebach, Jan-Peter Muller, M. J. Schoppers, Eldar Noe Dobrea, Nina Lanza, Marc Gailhanou, Genevieve Marchand, Sönke Burmeister, Craig Hardgrove, Justin N. Maki, Ari-Matti Harri, Michael C. Malin, M. J. Wolff, Roger E. Summons, H. Blau, Jacqueline Cameron, Jeff A. Berger, Didier Keymeulen, Agnes Cousin, Guillermo M. Muñoz Caro, Eric Lyness, Cedric Pilorget, Michael B. Baker, Christopher S. Edwards, M. L. Litvak, Brian M. Duston, Rebecca M. E. Williams, T. Nolan, Robert T. Downs, V. E. Hamilton, Walter Goetz, Pamela G. Conrad, J. Baroukh, Nathan T. Bridges, Meenakshi Wadhwa, Roger C. Wiens, Samuel M. Clegg, Philippe Sarrazin, L. Bleacher, Eric Lorigny, Mike Toplis, Michael H. Wong, Timothy H. McConnochie, Ian Mcewan, Kiran Patel, Mary Beth Wilhelm, John P. Grotzinger, Jeffrey E. Moersch, Michael A. Wilson, Mark Paton, I. Plante, Eric Lewin, Franck Poitrasson, Tori M. Hoehler, P. Guillemot, Mackenzie Day, David F. Blake, José Antonio Rodríguez Manfredi, G. W. Lugmair, Robert F. Wimmer-Schweingruber, Dorothy Z. Oehler, Samuel Teinturier, Bent Ehresmann, Jérémie Lasue, K. E. Herkenhoff, Daniel C. Berman, Scott VanBommel, Jeffrey R. Johnson, Emily M. McCullough, A. A. Fraeman, Ezat Heydari, Penelope L. King, K. M. Stack, Diana L. Blaney, A. Salamon, John G. Spray, L. Posiolova, Jeff Hollingsworth, David Choi, Kevin W. Lewis, B. D. Prats, Tonci Balic-Zunic, Mehdi Benna, H. M. Elliott, Jesús Martínez-Frías, R. Mueller-Mellin, William V. Boynton, Lance E. Christensen, Richard Leveille, John A. Grant, David E. Harker, J. M. Morookian, Caleb I. Fassett, S. Jacob, Donald Fay, R. Perez, Horton E. Newsom, Morten Madsen, M. G. Trainer, G. Israel, B. E. Nixon, Claude d’Uston, John E. Moores, Olivier Gasnault, Daniel J. Krysak, Vladislav Tretyakov, G. M. Perrett, Andrew D. Aubrey, L. E. Kirkland, F. Stalport, B. L. Barraclough, Alain Cros, Stephan Böttcher, Michel Cabane, William B. Brinckerhoff, Jack D. Farmer, James J. Wray, P. Y. Meslin, Arnaud Buch, Allan H. Treiman, S. C. R. Rafkin, B. C. Clark, Noureddine Melikechi, R. Jackson, Luther W. Beegle, Angela Lundberg, Bethany L. Ehlmann, William E. Dietrich, Karl Iagnemma, K. Supulver, Radu Popa, R. Zimdar, Melissa Floyd, Wesley T. Huntress, Paul B. Niles, D. M. Delapp, C. N.. Achilles, Darrell Drake, T. Nelson, Alain Gaboriaud, Verónica Peinado-Gonzalez, Edward P. Vicenzi, T. Boucher, Jennifer L. Eigenbrode, C. Tate, David J. Des Marais, F. Javier Martin-Torres, Antoine Charpentier, Chris Webster, Mildred P. Martin, Robert M. Sucharski, Lucy M. Thompson, Cyril Szopa, D. Halleaux, Antonio Molina Jurado, Richard V. Morris, Andrey Vostrukhin, Peter C. Thomas, Ara V. Nefian, Pablo Sobron Sanchez, Manuel de la Torre Juárez, B. Elliott, Hannu Savijärvi, J. Bentz, Sergey Nikiforov, S. Gordon, Shaunna M. Morrison, Jean-Luc Lacour, Günter Reitz, M. E. Newcombe, David E. Brinza, C. Yana, Gary Kocurek, L. J. Lipkaman, C. M. Garcia, Maria Genzer, Fred Calef, A. Godber, Stubbe F. Hviid, C. Donny, T. Van Beek, Ruslan O. Kuzmin, Alexander Hayes, T. S. Olson, George D. Cody, J. Martín-Soler, N. Karpushkina, John Bridges, Mercedes Jiménez, M. Lefavor, Sylvestre Maurice, H. L. K. Manning, Ralph E. Milliken, Susanne Schröder, N. Spanovich, L. J. Edwards, A. Koefoed, Roser Urqui-O'Callaghan, Eduardo Sebastian Martinez, Cary Zeitlin, Noël Stewart, David T. Vaniman, E. A. Breves, Laurent Favot, A. Varenikov, Gérard Manhès, R. B. Williams, David Martin, Steven J. Rowland, E. Boehm, Adrian P. Jones, Alexis Paillet, R. Francis, Sushil K. Atreya, Mariek E. Schmidt, David Baratoux, N. I. Boyd, Qiu-Mei Lee, I. L. ten Kate, Bernard Hallet, K. Stoiber, Vivian Z. Sun, M. R. Kennedy, Gillian M. Krezoski, Mark A. Bullock, T. Stein, Michelle E. Minitti, I. Pradler, Susan L. S. Stipp, Scott Davis, Robert O. Pepin, B. L. Ehlmann, Janne Kauhanen, Dmitry Golovin, Steve J. Chipera, Raymond E. Arvidson, Javier Gómez-Elvira, L. C. Kah, Melissa S. Rice, Isaias Carrasco Blazquez, Cécile Fabre, John J. Simmonds, Joy A. Crisp, Jens Frydenvang, Florence Tan, Julia DeMarines, S. P. Gorevan, Elizabeth B. Rampe, E. McCartney, Lauren DeFlores, K. Harshman, D. N. Harpold, J. Van Beek, Luis Mora-Sotomayor, Douglas W. Ming, Kristen E. Miller, John Campbell, Amy McAdam, L. Saper, Robert Sullivan, Lorenzo Fluckiger, Kjartan M. Kinch, Arik Posner, H. Bower, A. A. Pavlov, D. Scholes, Insoo Jun, Brigitte Gondet, Patrice Coll, Burt Baker, Donald M. Hassler, Ralf Gellert, Laurie A. Leshin, T. Siili, Gilles Dromart, Lauren A. Edgar, Ryan B. Anderson, Robert Dingler, Leon Radziemski, Jean-Baptiste Sirven, G. Weigle, Cynthia K. Little, A. Mezzacappa, Olivier Forni, A. S. Kozyrev, Edward A. Cloutis, Ashwin Vasavada, A. Behar, François Robert, D. M. Rubin, Alexey Malakhov, E. Jensen, T. C. Owen, Sebastien Hettrich, Miguel Ramos, B. Sutter, Melinda A. Kahre, Patrick Pinet, John H. Jones, Claude Brunet, B. Pavri, Nilton O. Renno, Evgeny Atlaskin, Laurent Peret, Maxim Mokrousov, David Lees, J. J. B. Avalos, Jennifer C. Stern, Ann Ollila, Josefina Torres Redondo, Miles J. Johnson, M. A. D. P. Hernandez, Daniel P. Glavin, Albert S. Yen, Christophe Agard, Jouni Polkko, Christopher P. McKay, J. Peterson, Oliver Botta, Mark T. Lemmon, Marion Nachon, K. M. Bean, Bruce A. Cantor, Jan Köhler, M. Fitzgibbon, Carlos Armiens-Aparicio, Jorge Pla-Garcia, Henrik Kahanpää, Frances Westall, Walter Schmidt, M.-H. Kim, Kenneth G. Miller, Sharon A. Wilson, S. McNair, O. Kortmann, David Grinspoon, E. M. Lee, S. Indyk, Osku Kemppinen, E. Raaen, Michael Mischna, R. S. Sletten, James B. Garvin, John M. Ward, R. L. Tokar, Paulo M. Vasconcelos, Charles Malespin, T. J. Parker, Aaron J. Sengstacken, S. Bender, Jean-Pierre Williams, F. Fedosov, Patrick Mauchien, Audrey Dupont, R. A. Yingst, David Coscia, David A. Cremers, Danika Wellington, Kenneth H. Nealson, J. K. Jensen, Martin R. Fisk, J. Joseph, Amy J. Williams, W. Brunner, NASA Johnson Space Center (JSC), NASA, NASA Goddard Space Flight Center (GSFC), Center for Research and Exploration in Space Science and Technology [GSFC] (CRESST), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Interuniversitaire des Systèmes Atmosphériques (LISA (UMR_7583)), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12)-Centre National de la Recherche Scientifique (CNRS), Department of Physics [Guelph], University of Guelph, Department of Atmospheric, Oceanic, and Space Sciences [Ann Arbor] (AOSS), University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, ASU School of Earth and Space Exploration (SESE), Arizona State University [Tempe] (ASU), Laboratoire de Génie des Procédés et Matériaux - EA 4038 (LGPM), CentraleSupélec, Space Science and Astrobiology Division at Ames, NASA Ames Research Center (ARC), Division of Geological and Planetary Sciences [Pasadena], California Institute of Technology (CALTECH), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Department of Astronomy [Ithaca], Cornell University [New York], Center for Earth and Planetary Studies [Washington] (CEPS), Smithsonian National Air and Space Museum, Smithsonian Institution-Smithsonian Institution, Department of Earth Science and Technology [Imperial College London], Imperial College London, United States Geological Survey [Reston] (USGS), Department of Geosciences [Stony Brook], Stony Brook University [SUNY] (SBU), State University of New York (SUNY)-State University of New York (SUNY), Rensselaer Polytechnic Institute (RPI), Princeton University, State University of New York (SUNY), Department of Earth, Atmospheric and Planetary Sciences [MIT, Cambridge] (EAPS), Massachusetts Institute of Technology (MIT), Department of Earth and Planetary Sciences [Knoxville], The University of Tennessee [Knoxville], Instituto de Ciencias Nucleares [Mexico], Universidad Nacional Autónoma de México = National Autonomous University of Mexico (UNAM), Geophysical Laboratory [Carnegie Institution], Carnegie Institution for Science, Department of Earth and Planetary Science [UC Berkeley] (EPS), University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), NOAA Earth System Research Laboratory (ESRL), National Oceanic and Atmospheric Administration (NOAA), Lunar and Planetary Institute [Houston] (LPI), Planetary Science Institute [Tucson] (PSI), School of Earth and Atmospheric Sciences [Atlanta], Georgia Institute of Technology [Atlanta], Aalto University, Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Applied Research Associates, Inc. (ARA), Center for Meteorite Studies [Tempe], Ashima Research, ATOS Origin, Australian National University (ANU), Bay Area Environmental Research Institute (BAER), Big Head Endian LLC, Brock University [Canada], Brown University, Canadian Space Agency (CSA), Capgemini Consulting [Paris], Carnegie Mellon University [Pittsburgh] (CMU), Catholic University of America, Institut des Matériaux, de Microélectronique et des Nanosciences de Provence (IM2NP), Aix Marseille Université (AMU)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), Centre de biophysique moléculaire (CBM), Université d'Orléans (UO)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS), Centre National d'Études Spatiales [Toulouse] (CNES), Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Chesapeake Energy Corporation, Service de la Corrosion et du Comportement des Matériaux dans leur Environnement (SCCME), Département de Physico-Chimie (DPC), CEA-Direction des Energies (ex-Direction de l'Energie Nucléaire) (CEA-DES (ex-DEN)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-CEA-Direction des Energies (ex-Direction de l'Energie Nucléaire) (CEA-DES (ex-DEN)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire d'Interaction Laser Matière (LILM), Concordia College, Moorhead, CS-Systèmes d'Information [Toulouse] (CS-SI), Delaware State University (DSU), Denver Museum of Nature and Science, Deutsches Zentrum für Luft- und Raumfahrt (DLR), Finnish Meteorological Institute (FMI), GeoRessources, Institut national des sciences de l'Univers (INSU - CNRS)-Centre de recherches sur la géologie des matières premières minérales et énergétiques (CREGU)-Université de Lorraine (UL)-Centre National de la Recherche Scientifique (CNRS), Géosciences Environnement Toulouse (GET), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Global Science and Technology, Inc., Honeybee Robotics Ltd, Indiana University [Bloomington], Indiana University System, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut de Chimie des Milieux et Matériaux de Poitiers (IC2MP), Université de Poitiers-Institut national des sciences de l'Univers (INSU - CNRS)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Institut des Sciences de la Terre (ISTerre), Université Joseph Fourier - Grenoble 1 (UJF)-Institut Français des Sciences et Technologies des Transports, de l'Aménagement et des Réseaux (IFSTTAR)-Institut national des sciences de l'Univers (INSU - CNRS)-Institut de recherche pour le développement [IRD] : UR219-PRES Université de Grenoble-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Jackson State University (JSU), Jacobs Technology ESCG, Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement [Lyon] (LGL-TPE), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Minéralogie et Cosmochimie du Muséum (LMCM), Muséum national d'Histoire naturelle (MNHN)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Los Alamos National Laboratory (LANL), Space Remote Sensing Group (ISR-2), Malin Space Science Systems (MSSS), Depertment of Polymer Chemistry, Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, DLR Institute of Planetary Research, German Aerospace Center (DLR), NASA Headquarters, Oregon State University (OSU), Search for Extraterrestrial Intelligence Institute (SETI), Smithsonian Institution, Department of Space Studies [Boulder], Southwest Research Institute [Boulder] (SwRI), Space Research Institute of the Russian Academy of Sciences (IKI), Russian Academy of Sciences [Moscow] (RAS), TechSource Inc., Texas A&M University [College Station], The Open University [Milton Keynes] (OU), University of Arizona, Met Office Hadley Centre for Climate Change (MOHC), United Kingdom Met Office [Exeter], Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], Niels Bohr Institute [Copenhagen] (NBI), Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH), Institute for Astronomy [Honolulu], University of Hawai‘i [Mānoa] (UHM), California Institute of Technology (CALTECH)-NASA, Universidad Nacional Autónoma de México (UNAM), Carnegie Institution for Science [Washington], University of California [Berkeley], University of California-University of California, Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS)-Aix Marseille Université (AMU), Université d'Orléans (UO)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-Institut de Chimie du CNRS (INC), Centre National de la Recherche Scientifique (CNRS)-Université de Lorraine (UL)-Centre de recherches sur la géologie des matières premières minérales et énergétiques (CREGU)-Institut national des sciences de l'Univers (INSU - CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-PRES Université de Grenoble-Université Joseph Fourier - Grenoble 1 (UJF)-Institut Français des Sciences et Technologies des Transports, de l'Aménagement et des Réseaux (IFSTTAR)-Institut national des sciences de l'Univers (INSU - CNRS)-Institut de recherche pour le développement [IRD] : UR219-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry]), University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement (LGL-TPE), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Université Jean Monnet - Saint-Étienne (UJM)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), NWO-NSO: The role of perchlorates in the preservation of organic compounds on Mars, Petrology, Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon), Centre National de la Recherche Scientifique (CNRS)-Muséum national d'Histoire naturelle (MNHN), and Kruch, Catherine
Subjects: Geologic Sediments, 010504 meteorology & atmospheric sciences, Extraterrestrial Environment, Curiosity rover, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Mineralogy, [SDU.ASTR.EP] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Mars, Sulfides, 01 natural sciences, organic compositions, Bassanite, 0103 physical sciences, Exobiology, [SDU.ASTR.SR] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Hydrocarbons, Chlorinated, MSL, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Total organic carbon, Martian, mudstone samples, Volatile Organic Compounds, Multidisciplinary, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Water, Mars Exploration Program, Carbon Dioxide, Oxygen, Bays, 13. Climate action, Rocknest, Sample Analysis at Mars, Sedimentary rock, Pyrolysis
Abstract: H 2 O, CO 2 , SO 2 , O 2 , H 2 , H 2 S, HCl, chlorinated hydrocarbons, NO, and other trace gases were evolved during pyrolysis of two mudstone samples acquired by the Curiosity rover at Yellowknife Bay within Gale crater, Mars. H 2 O/OH-bearing phases included 2:1 phyllosilicate(s), bassanite, akaganeite, and amorphous materials. Thermal decomposition of carbonates and combustion of organic materials are candidate sources for the CO 2 . Concurrent evolution of O 2 and chlorinated hydrocarbons suggests the presence of oxychlorine phase(s). Sulfides are likely sources for sulfur-bearing species. Higher abundances of chlorinated hydrocarbons in the mudstone compared with Rocknest windblown materials previously analyzed by Curiosity suggest that indigenous martian or meteoritic organic carbon sources may be preserved in the mudstone; however, the carbon source for the chlorinated hydrocarbons is not definitively of martian origin.
Published: 2014

16. Measurements of energetic particle radiation in transit to Mars on the Mars Science Laboratory

Author: Robert F. Wimmer-Schweingruber, S. Kang, Sönke Burmeister, Francis A. Cucinotta, Jingnan Guo, S. Rafkin, Donald M. Hassler, Cary Zeitlin, David E. Brinza, E. Böhm, Arik Posner, G. Weigle, Jan Köhler, Cesar Martin, Bent Ehresmann, Günther Reitz, and Stephan Böttcher
Subjects: Multidisciplinary, Spacecraft, business.industry, Equivalent dose, Mars, Mars Science Laboratory, Cosmic ray, Mars Exploration Program, Energetic Particle Radiation, Space Flight, Radiation assessment detector, Radiation Dosage, Sievert, Astrobiology, Radiation Assessment Detector, Humans, Transit (astronomy), Particle radiation, business, Cosmic Radiation
Abstract: Going to Mars The Mars Science Laboratory spacecraft containing the Curiosity rover, was launched from Earth in November 2011 and arrived at Gale crater on Mars in August 2012. Zeitlin et al. (p. 1080 ) report measurements of the energetic particle radiation environment inside the spacecraft during its cruise to Mars, confirming the hazard likely to be posed by this radiation to astronauts on a future potential trip to Mars. Williams et al. (p. 1068 , see the Perspective by Jerolmack ) report the detection of sedimentary conglomerates (pebbles mixed with sand and turned to rock) at Gale crater. The rounding of the rocks suggests abrasion of the pebbles as they were transported by flowing water several kilometers or more from their source.
Published: 2013

17. MSL-RAD Cruise Operations Concept

Author: Stephan Boettcher, Cary Zeitlin, David E. Brinza, G. Weigle, Cesar Martin, Robert Wimmer-Schweingrubber, and Donald M. Hassler
Subjects: Physics, Spacecraft, Network packet, business.industry, Duty cycle, Payload, Detector, Volume (computing), business, Radiation assessment detector, Computer hardware, Simulation, Mass storage
Abstract: The Mars Science Laboratory (MSL) payload includes the Radiation Assessment Detector (RAD) instrument, intended to fully characterize the radiation environment for the MSL mission. The RAD instrument operations concept is intended to reduce impact to spacecraft resources and effort for the MSL operations team. By design, RAD autonomously performs regular science observations without the need for frequent commanding from the Rover Compute Element (RCE). RAD operates with pre-defined "sleep" and "observe" periods, with an adjustable duty cycle for meeting power and data volume constraints during the mission. At the start of a new science observation, RAD performs a pre-observation activity to assess count rates for selected RAD detector elements. Based on this assessment, RAD can enter "solar event" mode, in which instrument parameters (including observation duration) are selected to more effectively characterize the environment. At the end of each observation period, RAD stores a time-tagged, fixed length science data packet in its non-volatile mass memory storage. The operating cadence is defined by adjustable parameters, also stored in non-volatile memory within the instrument. Periodically, the RCE executes an on-board sequence to transfer RAD science data packets from the instrument mass storage to the MSL downlink buffer. Infrequently, the RAD instrument operating configuration is modified by updating internal parameter tables and configuration entries.
Published: 2012

18. The Radiation Assessment Detector (RAD) Investigation

Author: Sönke Burmeister, Robert F. Wimmer-Schweingruber, Cary Zeitlin, David E. Brinza, Francis A. Cucinotta, Arik Posner, E. Böhm, Y. Tyler, K. Neal, Stephan Böttcher, J. Andrews, Mark A. Bullock, Kerrington D. Smith, S. Rafkin, Donald M. Hassler, Bent Ehresmann, Günther Reitz, G. Weigle, J. Peterson, L. Seimetz, M. Epperly, O. Kortmann, David Grinspoon, Jan Köhler, and Cesar Martin
Subjects: Physics, Mars radiation environment, Radiation, Physics::Instrumentation and Detectors, business.industry, Detector, Mars, Mars Science Laboratory, Astronomy and Astrophysics, Cosmic ray, Mars Exploration Program, Radiation assessment detector, Particle detector, Optics, Space and Planetary Science, Health threat from cosmic rays, Neutron detection, MSL, Particle radiation, business, Human exploration detectors in space, Remote sensing
Abstract: The Radiation Assessment Detector (RAD) on the Mars Science Laboratory (MSL) is an energetic particle detector designed to measure a broad spectrum of energetic particle radiation. It will make the first-ever direct radiation measurements on the surface of Mars, detecting galactic cosmic rays, solar energetic particles, secondary neutrons, and other secondary particles created both in the atmosphere and in the Martian regolith. The radiation environment on Mars, both past and present, may have implications for habitability and the ability to sustain life. Radiation exposure is also a major concern for future human missions. The RAD instrument combines charged- and neutral-particle detection capability over a wide dynamic range in a compact, low-mass, low-power instrument. These capabilities are required in order to measure all the important components of the radiation environment. RAD consists of the RAD Sensor Head (RSH) and the RAD Electronics Box (REB) integrated together in a small, compact volume. The RSH contains a solid-state detector telescope with three silicon PIN diodes for charged particle detection, a thallium doped Cesium Iodide scintillator, plastic scintillators for neutron detection and anti-coincidence shielding, and the front-end electronics. The REB contains three circuit boards, one with a novel mixed-signal ASIC for processing analog signals and an associated control FPGA, another with a second FPGA to communicate with the rover and perform onboard analysis of science data, and a third board with power supplies and power cycling or “sleep”-control electronics. The latter enables autonomous operation, independent of commands from the rover. RAD is a highly capable and highly configurable instrument that paves the way for future compact energetic particle detectors in space.
Published: 2012

19. Ralph: A Visible/Infrared Imager for the New Horizons Pluto/Kuiper Belt Mission

Author: Stuart McMuldroch, Dennis C. Reuter, Leslie A. Young, Donald E. Jennings, John Stone, Allen Lunsford, John J. Hanley, Lisa Hardaway, Derek Sabatke, Harold Reitsma, Robert Parizek, Catherine B. Olkin, James W. Baer, Jeffrey M. Moore, G. Weigle, Jeffrey E. Van Cleve, John Scherrer, John R. Spencer, Henry B. Throop, and S. Alan Stern
Subjects: Physics, New horizons, Infrared, Astrophysics (astro-ph), Near-infrared spectroscopy, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Panchromatic film, Pluto, Imaging spectroscopy, Primary (astronomy), Space and Planetary Science, Visible infrared, Color imaging, Remote sensing
Abstract: The New Horizons instrument named Ralph is a visible/near infrared multi-spectral imager and a short wavelength infrared spectral imager. It is one of the core instruments on New Horizons, NASA's first mission to the Pluto/Charon system and the Kuiper Belt. Ralph combines panchromatic and color imaging capabilities with IR imaging spectroscopy. Its primary purpose is to map the surface geology and composition of these objects, but it will also be used for atmospheric studies and to map the surface temperature. It is a compact, low-mass (10.5 kg), power efficient (7.1 W peak), and robust instrument with good sensitivity and excellent imaging characteristics. Other than a door opened once in flight, it has no moving parts. These characteristics and its high degree of redundancy make Ralph ideally suited to this long-duration flyby reconnaissance mission., 18 pages, 15 figures, 4 tables; To appear in a special volume of Space Science Reviews on the New Horizons mission
Published: 2009

20. Higgs-mass predictions in the MSSM and beyond

Author: P. Slavich, S. Heinemeyer, E. Bagnaschi, H. Bahl, M. Goodsell, H. E. Haber, T. Hahn, R. Harlander, W. Hollik, G. Lee, M. Mühlleitner, S. Paßehr, H. Rzehak, D. Stöckinger, A. Voigt, C. E. M. Wagner, G. Weiglein, B. C. Allanach, T. Biekötter, S. Borowka, J. Braathen, M. Carena, T. N. Dao, G. Degrassi, F. Domingo, P. Drechsel, U. Ellwanger, M. Gabelmann, R. Gröber, J. Klappert, T. Kwasnitza, D. Meuser, L. Mihaila, N. Murphy, K. Nickel, W. Porod, E. A. Reyes Rojas, I. Sobolev, and F. Staub
Subjects: Astrophysics, QB460-466, Nuclear and particle physics. Atomic energy. Radioactivity, QC770-798
Abstract: Abstract Predictions for the Higgs masses are a distinctive feature of supersymmetric extensions of the Standard Model, where they play a crucial role in constraining the parameter space. The discovery of a Higgs boson and the remarkably precise measurement of its mass at the LHC have spurred new efforts aimed at improving the accuracy of the theoretical predictions for the Higgs masses in supersymmetric models. The “Precision SUSY Higgs Mass Calculation Initiative” (KUTS) was launched in 2014 to provide a forum for discussions between the different groups involved in these efforts. This report aims to present a comprehensive overview of the current status of Higgs-mass calculations in supersymmetric models, to document the many advances that were achieved in recent years and were discussed during the KUTS meetings, and to outline the prospects for future improvements in these calculations.
Published: 2021
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21. Prospects for direct searches for light Higgs bosons at the ILC with 250 GeV

Author: P. Drechsel, G. Moortgat-Pick, and G. Weiglein
Subjects: Astrophysics, QB460-466, Nuclear and particle physics. Atomic energy. Radioactivity, QC770-798
Abstract: Abstract The particle discovered in the Higgs boson searches at the LHC with a mass of about 125 GeV is compatible within the present uncertainties with the Higgs boson predicted in the Standard Model (SM), but it could also be identified with one of the neutral Higgs bosons in a variety of beyond the SM (BSM) theories with an extended Higgs sector. The possibility that an additional Higgs boson (or even more than one) could be lighter than the state that has been detected at 125 GeV occurs generically in many BSM models and has some support from slight excesses that were observed above the background expectations in Higgs searches at LEP and at the LHC. The couplings between additional Higgs fields and the electroweak gauge bosons in BSM theories could be probed by model-independent Higgs searches at lepton colliders. We present a generator-level extrapolation of the limits obtained at LEP to the case of a future $$e^+e^-$$ e + e - collider, both for the search where the light Higgs boson decays into a pair of bottom quarks and for the decay-mode-independent search utilising the recoil method. We find that at the ILC with a centre-of-mass energy of 250 GeV, an integrated luminosity of 500 fb $$^{-1}$$ - 1 and polarised beams, the sensitivity to a light Higgs boson with reduced couplings to gauge bosons is improved by more than an order of magnitude compared to the LEP limits and goes much beyond the projected indirect sensitivity of the HL-LHC with 3000 fb $$^{-1}$$ - 1 from the rate measurements of the detected state at 125 GeV.
Published: 2020
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22. Noise analysis of three newborn infant isolettes

Author: R J, Berens and C G, Weigle
Subjects: Incubators, Infant, Evaluation Studies as Topic, Infant, Newborn, Humans, Prospective Studies, Noise
Abstract: The purpose of this study was to evaluate the noise of three newborn infant isolettes.An observational, prospective study evaluated noise in three isolettes (Ohmeda, Air Shields, and Drager). The study measured interior isolette noise production during quiet noise situations and isolette noise attenuation of added low- and high-frequency noise. Noise was measured on the decibel A scale and in the 125 Hz and 1000 Hz bands.During quiet conditions the Ohmeda and Drager isolettes had the least noise production on the basis of decibel A levels (p0.001). Low-frequency noise on the decibel A scale was attenuated the most by the Drager isolette (p0.001), although the overall difference may be clinically insignificant. The Ohmeda isolette attenuated high-frequency noise by 28.4 dB as measured on the decibel A scale, which was greater than values for the Drager (22.8 dB) and Air Shields (14 dB) isolettes (p0.001).High-frequency noise attenuation by the Ohmeda and Drager isolettes is clinically and statistically greater than high-frequency noise attenuation by the Air Shields isolette.
Published: 1997

23. Cost analysis of ceiling tile replacement for noise abatement

Author: R J, Berens and C G, Weigle
Subjects: Analysis of Variance, Evaluation Studies as Topic, Intensive Care Units, Neonatal, Costs and Cost Analysis, Infant, Newborn, Noise, Occupational, Humans, Hospital Design and Construction, Prospective Studies
Abstract: Our purpose was to evaluate the cost and benefit of noise reduction after replacement of acoustic ceiling tile in an open ward neonatal intensive care unit (NICU).An observational, prospective study evaluated noise in an open ward NICU before and after suspended ceiling tiles were replaced. Noise was rated by a 10-point visual analog scale and measured with a decibel meter.The mean decibel level was 55 before and 53 after renovation (p0.05). The median visual analog score was 5 before and 4 after renovation (p = 0.09). The cost of ceiling tile replacement was $2400.The renovation resulted in a small decrease in the decibel level in the NICU, although this measured decrease was not perceived by observers. With a formal prerenovation noise evaluation, a more efficient ceiling tile might have been selected or the project may have been aborted or modified because of the low levels of noise already present.
Published: 1996

24. Global analysis of dark matter simplified models with leptophobic spin-one mediators using MasterCode

Author: E. Bagnaschi, J. C. Costa, K. Sakurai, M. Borsato, O. Buchmueller, A. De Roeck, M. J. Dolan, J. R. Ellis, H. Flächer, K. Hahn, S. Heinemeyer, M. Lucio, D. Martínez Santos, K. A. Olive, S. Trifa, and G. Weiglein
Subjects: Astrophysics, QB460-466, Nuclear and particle physics. Atomic energy. Radioactivity, QC770-798
Abstract: Abstract We report the results of a global analysis of dark matter simplified models (DMSMs) with leptophobic mediator particles of spin one, considering the cases of both vector and axial-vector interactions with dark matter (DM) particles and quarks. We require the DMSMs to provide all the cosmological DM density indicated by Planck and other observations, and we impose the upper limits on spin-independent and -dependent scattering from direct DM search experiments. We also impose all relevant LHC constraints from searches for monojet events and measurements of the dijet mass spectrum. We model the likelihood functions for all the constraints and combine them within the MasterCode framework, and probe the full DMSM parameter spaces by scanning over the mediator and DM masses and couplings, not fixing any of the model parameters. We find, in general, two allowed regions of the parameter spaces: one in which the mediator couplings to Standard Model (SM) and DM particles may be comparable to those in the SM and the cosmological DM density is reached via resonant annihilation, and one in which the mediator couplings to quarks are $$\lesssim \, 10^{-3}$$ ≲10-3 and DM annihilation is non-resonant. We find that the DM and mediator masses may well lie within the ranges accessible to LHC experiments. We also present predictions for spin-independent and -dependent DM scattering, and present specific results for ranges of the DM couplings that may be favoured in ultraviolet completions of the DMSMs.
Published: 2019
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25. Supersymmetric models in light of improved Higgs mass calculations

Author: E. Bagnaschi, H. Bahl, J. Ellis, J. L. Evans, T. Hahn, S. Heinemeyer, W. Hollik, K. A. Olive, S. Paßehr, H. Rzehak, I. V. Sobolev, G. Weiglein, and J. Zheng
Subjects: Astrophysics, QB460-466, Nuclear and particle physics. Atomic energy. Radioactivity, QC770-798
Abstract: Abstract We discuss the parameter spaces of supersymmetry (SUSY) scenarios taking into account the improved Higgs-mass prediction provided by FeynHiggs 2.14.1. Among other improvements, this prediction incorporates three-loop renormalization-group effects and two-loop threshold corrections, and can accommodate three separate mass scales: $$m_{{{\tilde{q}}}}$$ mq~ (for squarks), $$m_{\tilde{g\,}\!}$$ mg~ (for gluinos) and $$m_{{{\tilde{\chi }}}}$$ mχ~ (for electroweakinos). Furthermore, it contains an improved treatment of the $$\overline{\mathrm {DR}}$$ DR¯ scalar top parameters avoiding problems with the conversion to on-shell parameters, that yields more accurate results for large SUSY-breaking scales. We first consider the CMSSM, in which the soft SUSY-breaking parameters $$m_0$$ m0 and $$m_{1/2}$$ m1/2 are universal at the GUT scale, and then sub-GUT models in which universality is imposed at some lower scale. In both cases, we consider the constraints from the Higgs-boson mass $$M_h$$ Mh in the bulk of the $$(m_0, m_{1/2})$$ (m0,m1/2) plane and also along stop coannihilation strips where sparticle masses may extend into the multi-TeV range. We then consider the minimal anomaly-mediated SUSY-breaking scenario, in which large sparticle masses are generic. In all these scenarios the substantial improvements between the calculations of $$M_h$$ Mh in FeynHiggs 2.14.1 and FeynHiggs 2.10.0, which was used in an earlier study, change significantly the preferred portions of the models’ parameter spaces. Finally, we consider the pMSSM11, in which sparticle masses may be significantly smaller and we find only small changes in the preferred regions of parameter space.
Published: 2019
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26. Likelihood analysis of the pMSSM11 in light of LHC 13-TeV data

Author: E. Bagnaschi, K. Sakurai, M. Borsato, O. Buchmueller, M. Citron, J. C. Costa, A. De Roeck, M. J. Dolan, J. R. Ellis, H. Flächer, S. Heinemeyer, M. Lucio, D. Martínez Santos, K. A. Olive, A. Richards, V. C. Spanos, I. Suárez Fernández, and G. Weiglein
Subjects: Astrophysics, QB460-466, Nuclear and particle physics. Atomic energy. Radioactivity, QC770-798
Abstract: Abstract We use MasterCode to perform a frequentist analysis of the constraints on a phenomenological MSSM model with 11 parameters, the pMSSM11, including constraints from $$\sim 36$$ ∼36 /fb of LHC data at 13 TeV and PICO, XENON1T and PandaX-II searches for dark matter scattering, as well as previous accelerator and astrophysical measurements, presenting fits both with and without the $$(g-2)_\mu $$ (g-2)μ constraint. The pMSSM11 is specified by the following parameters: 3 gaugino masses $$M_{1,2,3}$$ M1,2,3 , a common mass for the first-and second-generation squarks $$m_{\tilde{q}}$$ mq~ and a distinct third-generation squark mass $$m_{\tilde{q}_3}$$ mq~3 , a common mass for the first-and second-generation sleptons $$m_{\tilde{\ell }}$$ mℓ~ and a distinct third-generation slepton mass $$m_{\tilde{\tau }}$$ mτ~ , a common trilinear mixing parameter A, the Higgs mixing parameter $$\mu $$ μ , the pseudoscalar Higgs mass $$M_A$$ MA and $$\tan \beta $$ tanβ . In the fit including $$(g-2)_\mu $$ (g-2)μ , a Bino-like $$\tilde{\chi }^0_{1}$$ χ~10 is preferred, whereas a Higgsino-like $$\tilde{\chi }^0_{1}$$ χ~10 is mildly favoured when the $$(g-2)_\mu $$ (g-2)μ constraint is dropped. We identify the mechanisms that operate in different regions of the pMSSM11 parameter space to bring the relic density of the lightest neutralino, $$\tilde{\chi }^0_{1}$$ χ~10 , into the range indicated by cosmological data. In the fit including $$(g-2)_\mu $$ (g-2)μ , coannihilations with $$\tilde{\chi }^0_{2}$$ χ~20 and the Wino-like $$\tilde{\chi }^\pm _{1}$$ χ~1± or with nearly-degenerate first- and second-generation sleptons are active, whereas coannihilations with the $$\tilde{\chi }^0_{2}$$ χ~20 and the Higgsino-like $$\tilde{\chi }^\pm _{1}$$ χ~1± or with first- and second-generation squarks may be important when the $$(g-2)_\mu $$ (g-2)μ constraint is dropped. In the two cases, we present $$\chi ^2$$ χ2 functions in two-dimensional mass planes as well as their one-dimensional profile projections and best-fit spectra. Prospects remain for discovering strongly-interacting sparticles at the LHC, in both the scenarios with and without the $$(g-2)_\mu $$ (g-2)μ constraint, as well as for discovering electroweakly-interacting sparticles at a future linear $$e^+ e^-$$ e+e- collider such as the ILC or CLIC.
Published: 2018
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27. Likelihood analysis of the sub-GUT MSSM in light of LHC 13-TeV data

Author: J. C. Costa, E. Bagnaschi, K. Sakurai, M. Borsato, O. Buchmueller, M. Citron, A. De Roeck, M. J. Dolan, J. R. Ellis, H. Flächer, S. Heinemeyer, M. Lucio, D. Martínez Santos, K. A. Olive, A. Richards, and G. Weiglein
Subjects: Astrophysics, QB460-466, Nuclear and particle physics. Atomic energy. Radioactivity, QC770-798
Abstract: Abstract We describe a likelihood analysis using MasterCode of variants of the MSSM in which the soft supersymmetry-breaking parameters are assumed to have universal values at some scale $$M_\mathrm{in}$$ Min below the supersymmetric grand unification scale $$M_\mathrm{GUT}$$ MGUT , as can occur in mirage mediation and other models. In addition to $$M_\mathrm{in}$$ Min , such ‘sub-GUT’ models have the 4 parameters of the CMSSM, namely a common gaugino mass $$m_{1/2}$$ m1/2 , a common soft supersymmetry-breaking scalar mass $$m_0$$ m0 , a common trilinear mixing parameter A and the ratio of MSSM Higgs vevs $$\tan \beta $$ tanβ , assuming that the Higgs mixing parameter $$\mu > 0$$ μ>0 . We take into account constraints on strongly- and electroweakly-interacting sparticles from $$\sim 36$$ ∼36 /fb of LHC data at 13 TeV and the LUX and 2017 PICO, XENON1T and PandaX-II searches for dark matter scattering, in addition to the previous LHC and dark matter constraints as well as full sets of flavour and electroweak constraints. We find a preference for $$M_\mathrm{in}\sim 10^5$$ Min∼105 to $$10^9 \,\, \mathrm {GeV}$$ 109GeV , with $$M_\mathrm{in}\sim M_\mathrm{GUT}$$ Min∼MGUT disfavoured by $$\Delta \chi ^2 \sim 3$$ Δχ2∼3 due to the $$\mathrm{BR}(B_{s, d} \rightarrow \mu ^+\mu ^-)$$ BR(Bs,d→μ+μ-) constraint. The lower limits on strongly-interacting sparticles are largely determined by LHC searches, and similar to those in the CMSSM. We find a preference for the LSP to be a Bino or Higgsino with $$m_{\tilde{\chi }^0_{1}} \sim 1 \,\, \mathrm {TeV}$$ mχ~10∼1TeV , with annihilation via heavy Higgs bosons H / A and stop coannihilation, or chargino coannihilation, bringing the cold dark matter density into the cosmological range. We find that spin-independent dark matter scattering is likely to be within reach of the planned LUX-Zeplin and XENONnT experiments. We probe the impact of the $$(g-2)_\mu $$ (g-2)μ constraint, finding similar results whether or not it is included.
Published: 2018
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28. Higgs-boson masses and mixing matrices in the NMSSM: analysis of on-shell calculations

Author: P. Drechsel, R. Gröber, S. Heinemeyer, M. Mühlleitner, H. Rzehak, and G. Weiglein
Subjects: Astrophysics, QB460-466, Nuclear and particle physics. Atomic energy. Radioactivity, QC770-798
Abstract: Abstract We analyze the Higgs-boson masses and mixing matrices in the NMSSM based on an on-shell (OS) renormalization of the gauge-boson and Higgs-boson masses and the parameters of the top/scalar top sector. We compare the implementation of the OS calculations in the codes NMSSMCALC and NMSSM-FeynHiggs up to $${\mathcal {O}}(\alpha _t\alpha _s)$$ O ( α t α s ) . We identify the sources of discrepancies at the one- and at the two-loop level. Finally we compare the OS and $$\overline{\mathrm {DR}}$$ DR ¯ evaluation as implemented in NMSSMCALC. The results are important ingredients for an estimate of the theoretical precision of Higgs-boson mass calculations in the NMSSM.
Published: 2017
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29. Likelihood analysis of the minimal AMSB model

Author: E. Bagnaschi, M. Borsato, K. Sakurai, O. Buchmueller, R. Cavanaugh, V. Chobanova, M. Citron, J. C. Costa, A. De Roeck, M. J. Dolan, J. R. Ellis, H. Flächer, S. Heinemeyer, G. Isidori, M. Lucio, F. Luo, D. Martínez Santos, K. A. Olive, A. Richards, and G. Weiglein
Subjects: Astrophysics, QB460-466, Nuclear and particle physics. Atomic energy. Radioactivity, QC770-798
Abstract: Abstract We perform a likelihood analysis of the minimal anomaly-mediated supersymmetry-breaking (mAMSB) model using constraints from cosmology and accelerator experiments. We find that either a wino-like or a Higgsino-like neutralino LSP, $$\tilde{\chi }^0_{1}$$ χ ~ 1 0 , may provide the cold dark matter (DM), both with similar likelihoods. The upper limit on the DM density from Planck and other experiments enforces $$m_{\tilde{\chi }^0_{1}} \lesssim 3 \,\, \mathrm {TeV}$$ m χ ~ 1 0 ≲ 3 TeV after the inclusion of Sommerfeld enhancement in its annihilations. If most of the cold DM density is provided by the $$\tilde{\chi }^0_{1}$$ χ ~ 1 0 , the measured value of the Higgs mass favours a limited range of $$\tan \beta \sim 5$$ tan β ∼ 5 (and also for $$\tan \beta \sim 45$$ tan β ∼ 45 if $$\mu > 0$$ μ > 0 ) but the scalar mass $$m_0$$ m 0 is poorly constrained. In the wino-LSP case, $$m_{3/2}$$ m 3 / 2 is constrained to about $$900\,\, \mathrm {TeV}$$ 900 TeV and $$m_{\tilde{\chi }^0_{1}}$$ m χ ~ 1 0 to $$2.9\pm 0.1\,\, \mathrm {TeV}$$ 2.9 ± 0.1 TeV , whereas in the Higgsino-LSP case $$m_{3/2}$$ m 3 / 2 has just a lower limit $$\gtrsim 650\,\, \mathrm {TeV}$$ ≳ 650 TeV ( $$\gtrsim 480\,\, \mathrm {TeV}$$ ≳ 480 TeV ) and $$m_{\tilde{\chi }^0_{1}}$$ m χ ~ 1 0 is constrained to $$1.12 ~(1.13) \pm 0.02\,\, \mathrm {TeV}$$ 1.12 ( 1.13 ) ± 0.02 TeV in the $$\mu >0$$ μ > 0 ( $$\mu 0$$ μ > 0 .
Published: 2017
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30. WIND-SPEED AND WIND-DIRECTION DISTRIBUTIONS AT ARGUS ISLAND OFF BERMUDA

Author: Francis G. Weigle, John M. Gorman, and Anthony J. Perrone
Subjects: Argus, Geography, integumentary system, Meteorology, Anemometer, Cumulative distribution function, Maximum sustained wind, Wind direction, Atmospheric sciences, computer, Standard deviation, Wind speed, computer.programming_language
Abstract: Argus Island wind information was systematically recorded and processed over a three-year period. The recording, processing, and analysis procedures used are described. Monthly mean wind speeds with standard deviations are compared with monthly median wind speeds and quartiles. Monthly distributions of wind speed are given, as well as yearly distributions. Cumulative distribution plots compare wind-speed occurrences over the three-year period. A time plot of daily mean and maximum wind speeds is given, and diurnal variations are discussed. The distributions of wind direction for each month are also shown.
Published: 1965

31. The Aspens: Their Growth and Management

Author: W. G. Weigle, E. H. Frothingham and W. G. Weigle, E. H. Frothingham
Published: 1911

32. Time Variability of Ambient‐Noise Directionality

Author: A. J. Perrone, E. M. Arase, F. G. Weigle, and T. Arase
Subjects: Acoustics and Ultrasonics, Arts and Humanities (miscellaneous), Meteorology, Ambient noise level, Range (statistics), Elevation, Columbia university, Geodesy, Naval research, Deep sea, Noise (radio), Geology
Abstract: Measurements of the time variation of ambient noise of the deep ocean at fixed elevation angles have been made in 13‐octave bands in the frequency range 200–1500 cps. This is the same frequency range used by Fox [J. Acoust. Soc. Am. 35, 811 (1963)]. The fixed angles are the up‐ and down‐going refraction‐surface‐reflection (RSR) angles at this depth and result in observations of noise typical of the deep ocean at this depth. The measurements of the level of ambient noise are correlated with simultaneous weather observations. The noise distributions are shown to be peaked at the RSR angles at low sea states and at other angles at high sea states. [Hudson Laboratories, Columbia University Informal Documentation No. 45. Work supported by the U. S. Office of Naval Research.]
Published: 1964

33. Project Bold Venture: Lake Tanganyika Sound Attenuation Experiment

Author: David G. Browning, William H. Thorp, Everett N. Jones, J. M. Gorman, F. G. Weigle, and Robert H. Mellen
Subjects: Water depth, Absorption (acoustics), Oceanography, Acoustics and Ultrasonics, Arts and Humanities (miscellaneous), Sound transmission class, Anomaly (natural sciences), Attenuation, Seawater, Low frequency, Acoustic attenuation, Seismology, Geology
Abstract: In order to determine the cause of the low‐frequency sound attenuation anomaly in seawater, comparative measurements are being made in freshwater. The Lake Tanganyika experiment (23°C) was conducted to determine the temperature dependency of the anomaly and to overcome the depth limitations of the previous Lake Superior experiment. The sound propagation run was conducted along a 130‐mile track with an average water depth of 2000 ft. Attenuation coefficients were obtained for center frequencies of 315–10000 Hz in 13‐oct bands. The results show an anomalous behavior, but the relaxation frequency is poorly defined. Comparison is made with the absorption predicted from chemical analysis of the water.
Published: 1972

34. Characteristics of Ambient Noise off Bermuda

Author: F. G. Weigle
Subjects: Acoustics and Ultrasonics, Meteorology, Ambient noise level, Mean value, Magnetic tape, Geodesy, Wind speed, Radio spectrum, Standard deviation, law.invention, Noise, Arts and Humanities (miscellaneous), law, Wave height, Environmental science
Abstract: The data resulting from a 23‐month ambient‐noise measurement program are reviewed. 2‐min‐long broad‐band magnetic tape recordings were made every 2 h, from omnidirectional hydrophones at fixed locations. Ten noise‐level readings were made in each of ten logit frequency bands between 100 and 1000 cps from each recording. The mean value obtained from each set of ten readings was taken as the representative level of that 2‐min sample in subsequent data processing. The data clearly show the dependence of ambient‐noise level upon wind‐speed and a lesser dependence upon wave height. The spectrum is seen to change markedly with wind speed and to suggest the presence of both wind‐dependent and non wind‐dependent mechanisms. Level‐distribution histograms show dependence upon both frequency and season. The standard deviation is shown to be a function of both frequency and wind speed. Power‐spectrum analyses indicate the occurrence of cyclical noise variations with periods up to 55 h.
Published: 1966

35. A contact binary satellite of the asteroid (152830) Dinkinesh.

Author: Levison HF, Marchi S, Noll KS, Spencer JR, Statler TS, Bell JF 3rd, Bierhaus EB, Binzel R, Bottke WF, Britt D, Brown ME, Buie MW, Christensen PR, Dello Russo N, Emery JP, Grundy WM, Hahn M, Hamilton VE, Howett C, Kaplan H, Kretke K, Lauer TR, Manzoni C, Marschall R, Martin AC, May BH, Mottola S, Olkin CB, Pätzold M, Parker JW, Porter S, Preusker F, Protopapa S, Reuter DC, Robbins SJ, Salmon J, Simon AA, Stern SA, Sunshine JM, Wong I, Weaver HA, Adam C, Ancheta S, Andrews J, Anwar S, Barnouin OS, Beasley M, Berry KE, Birath E, Bolin B, Booco M, Burns R, Campbell P, Carpenter R, Crombie K, Effertz M, Eifert E, Ellis C, Faiks P, Fischetti J, Fleming P, Francis K, Franco R, Freund S, Gallagher C, Geeraert J, Gobat C, Gorgas D, Granat C, Gray S, Haas P, Harch A, Hegedus K, Isabelle C, Jackson B, Jacob T, Jennings S, Kaufmann D, Keeney BA, Kennedy T, Lauffer K, Lessac-Chenen E, Leonard R, Levine A, Lunsford A, Martin T, McAdams J, Mehall G, Merkley T, Miller G, Montanaro M, Montgomery A, Murphy G, Myers M, Nelson DS, Ocampo A, Olds R, Pelgrift JY, Perkins T, Pineau J, Poland D, Ramanan V, Rose D, Sahr E, Short O, Solanki I, Stanbridge D, Sutter B, Talpas Z, Taylor H, Treiu B, Vermeer N, Vincent M, Wallace M, Weigle G, Wibben DR, Wiens Z, Wilson JP, and Zhao Y
Abstract: Asteroids with diameters less than about 5 km have complex histories because they are small enough for radiative torques (that is, YORP, short for the Yarkovsky-O'Keefe-Radzievskii-Paddack effect) 1 to be a notable factor in their evolution 2 . (152830) Dinkinesh is a small asteroid orbiting the Sun near the inner edge of the main asteroid belt with a heliocentric semimajor axis of 2.19 AU; its S-type spectrum 3,4 is typical of bodies in this part of the main belt 5 . Here we report observations by the Lucy spacecraft 6,7 as it passed within 431 km of Dinkinesh. Lucy revealed Dinkinesh, which has an effective diameter of only 720 m, to be unexpectedly complex. Of particular note is the presence of a prominent longitudinal trough overlain by a substantial equatorial ridge and the discovery of the first confirmed contact binary satellite, now named (152830) Dinkinesh I Selam. Selam consists of two near-equal-sized lobes with diameters of 210 m and 230 m. It orbits Dinkinesh at a distance of 3.1 km with an orbital period of about 52.7 h and is tidally locked. The dynamical state, angular momentum and geomorphologic observations of the system lead us to infer that the ridge and trough of Dinkinesh are probably the result of mass failure resulting from spin-up by YORP followed by the partial reaccretion of the shed material. Selam probably accreted from material shed by this event., (© 2024. The Author(s).)
Published: 2024
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36. Mars' surface radiation environment measured with the Mars Science Laboratory's Curiosity rover.

Author: Hassler DM, Zeitlin C, Wimmer-Schweingruber RF, Ehresmann B, Rafkin S, Eigenbrode JL, Brinza DE, Weigle G, Böttcher S, Böhm E, Burmeister S, Guo J, Köhler J, Martin C, Reitz G, Cucinotta FA, Kim MH, Grinspoon D, Bullock MA, Posner A, Gómez-Elvira J, Vasavada A, and Grotzinger JP
Subjects: Deinococcus physiology, Deinococcus radiation effects, Humans, Organic Chemicals analysis, Radiation Dosage, Space Flight, Surface Properties radiation effects, Cosmic Radiation, Exobiology, Extraterrestrial Environment, Mars
Abstract: The Radiation Assessment Detector (RAD) on the Mars Science Laboratory's Curiosity rover began making detailed measurements of the cosmic ray and energetic particle radiation environment on the surface of Mars on 7 August 2012. We report and discuss measurements of the absorbed dose and dose equivalent from galactic cosmic rays and solar energetic particles on the martian surface for ~300 days of observations during the current solar maximum. These measurements provide insight into the radiation hazards associated with a human mission to the surface of Mars and provide an anchor point with which to model the subsurface radiation environment, with implications for microbial survival times of any possible extant or past life, as well as for the preservation of potential organic biosignatures of the ancient martian environment.
Published: 2014
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37. Measurements of energetic particle radiation in transit to Mars on the Mars Science Laboratory.

Author: Zeitlin C, Hassler DM, Cucinotta FA, Ehresmann B, Wimmer-Schweingruber RF, Brinza DE, Kang S, Weigle G, Böttcher S, Böhm E, Burmeister S, Guo J, Köhler J, Martin C, Posner A, Rafkin S, and Reitz G
Subjects: Humans, Cosmic Radiation, Mars, Radiation Dosage, Space Flight
Abstract: The Mars Science Laboratory spacecraft, containing the Curiosity rover, was launched to Mars on 26 November 2011, and for most of the 253-day, 560-million-kilometer cruise to Mars, the Radiation Assessment Detector made detailed measurements of the energetic particle radiation environment inside the spacecraft. These data provide insights into the radiation hazards that would be associated with a human mission to Mars. We report measurements of the radiation dose, dose equivalent, and linear energy transfer spectra. The dose equivalent for even the shortest round-trip with current propulsion systems and comparable shielding is found to be 0.66 ± 0.12 sievert.
Published: 2013
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