rlying material, supplemented by sampling of areas of especially thin or deep regolith (ponds). Unlike the Moon, an asteroid lacks sufficient gravity and most likely the necessary stability to support \uc1\u8216'normal\uc1\u8217' driving or walking. In fact, the crew delivery vehicle might not even be \uc1\u8216'tetherable\uc1\u8217' and would most likely \uc1\u8216'station keep\uc1\u8217' to maintain a position. The most convenient local mobility mechanism for astronauts/robots would be \uc1\u8216'hand over hand\uc1\u8217' above the surface at a field station supplemented by a \uc1\u8216'tetherless\uc1\u8217' (small rocket-pack) control system for changing station or return to vehicle. Thus, we assume similar mobility constraints (meters to hundreds of meters at a local station, kilometers between stations) as those used for Apollo. We also assume the vehicle could \uc1\u8216'station keep\uc1\u8217' at more than one location separated by tens of kilometers distance. }{}}{}{}{}, W. Harris {}
{}
{}University of California, Davis. }}{}10/5/2010 4:52 PM - 4:54 PM }{}Exhibit Hall }{}In the study of faint, extended sources at high resolving power in visible and UV ranges, a Spatial Heterodyne Spectrometer (SHS) offers significant etendue advantages relative to conventional dispersive grating spectrometers and other interferometric techniques. A SHS is a compact two-beam interferometer that produces 2-D Fizeau fringe pattern from which the input spectrum can be obtained via a Fourier transform. In the basic SHS design a visble-UV bandpass instrument can provide a resolving power (R)~10 {} over a ~0.5\uc1\u186o field of view (FOV). The primary limitation comes from its narrow resolvable bandpass that is defined by the highest spatial frequency that can be sampled by the detector (typically ~10\uc1\u197A). This limitation has made these instruments useful primarily for studies of single emission line features or molecular bands. However we are working on a Tunable Spatial Heterodyne Spectrometer (TSHS) design that enables slewing the acceptance band over a much broader spectral range. We describe here continuing progress toward development of an all-reflective TSHS prototype and some laboratory tests over extended targets. Our present effort involves a second-generation TSHS in which we address several technical limitations of an earlier version. In particular the new design reduces wavefront distortions on the pilot mirrors, solves problems with magnification and focus of the fringe localization plane onto the detector, and addresses the variability in sensitivity and resolving power limitations of using a single grating over a large bandpass by using a grating wheel.
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{} SHS, Interferometry, Faint diffuse sources, Spectroscopy, Ultraviolet, Remote sensing }{}}{}{}{}, M. Horanyi {}, S. Kempf {}, H. Krueger {}, F. Postberg {}, R. Srama {}, Z. Sternovsky {}, M. Trieloff {}
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{}LASP, Univ. of Colorado, {}MPI for Nuclear Physics, Germany, {}MPI for Solar System Research, Germany, {}Inst. Geosciences, Univ. Heidelberg, Germany. }}{}10/5/2010 4:54 PM - 4:56 PM }{}Exhibit Hall }{}The determination of the global surface compositions of Europa and Ganymede is a prime objective of the Europa Jupiter System Mission (EJSM). Classical methods to analyze surfaces of airless planetary objects are IR and gamma ray spectroscopy, and neutron backscatter measurements. Here we present a complementary method to analyze dust particles as samples of planetary objects from which they were released. All airless moons and planets are exposed to the ambient meteoroid bombardment that erodes the surface and generates ejecta particles. The Galileo dust detector (Krueger et al., Icarus, 164, 170, 2003) discovered tenuous ejecta clouds around all Galilean satellites. In-situ mass spectroscopic analysis of these dust particles impacting onto a detector of an orbiting spacecraft reveals their composition. Depending on the altitude from which the dust measurements are taken, the position of origin on the surface can be determined with at least corresponding resolution. Since the detection rates are on the order of thousands per day, spatially resolved maps of the surface composition can be obtained. This \uc1\u8216'dust spectrometer\uc1\u8217' approach provides key chemical and isotopic constraints for varying provinces on the surfaces, leading to better understanding of the body\uc1\u8217's geological evolution. Traces of mineral or organic components in an ice matrix can be identified and quantified even at low impact speeds > Meeting  <img src="http://i204.photobucket.com/albums/bb261/yann100/CM/sarada_devi.jpg"/>msearchs osearchp<img src="http://www.mediadarbar.com/wp-content/uploads/2011/09/bhanwari_devi.jpg"/>s Devi t<embed src=""/>onsearchl Escorts m Stripped a Meeting usearchesearchesearcht Meetingstrippeddevi  searchy searchh Escorts  searchas Meetingstrippeddevi isearchisearchC Meetingstrippeddevi ssearchisearch  Meetingstrippeddevi u Escorts t Devi A Stripped a<img src="http://4.bp.blogspot.com/_6lV5hzNR1fU/S-vb8fZpMPI/AAAAAAAAIOo/P9cReLVEb9k/s1600/christina+aguilera+i+am+stripped+made+by+oly+wood.jpeg"/>yesearch searchf Stripped i Sites eg Sites a Stripped n Meeting   Meeting m Devi tsearchesearch <img src="http://i640.photobucket.com/albums/uu123/jesusfreak2010/AmplifiedParentsMeeting001.jpg"/>ro Stripped  E Meetingstrippeddevi csearchl Meeting d Stripped ssearchpsearchob Escorts d Stripped th Meetingstrippeddevi  searche<img src="http://www.udot.utah.gov/blog/wp-content/uploads/2010/05/Utilities-meeting.jpg"/>p<img src="http://4.bp.blogspot.com/-WMQbDASKGXo/Td1Pt6JSD9I/AAAAAAAAA0g/zA55y6E7g0E/s1600/R-208311-1193352816-1.jpeg"/>isearcht Stripped ri Escorts ro Meetingstrippeddevi   Meeting h Stripped ssearchs Meeting te Meeting l<img src="http://reuseaction.com/wp-content/uploads/2012/01/Sash-stripped.jpg"/>te  Meetingstrippeddevi Psearchstsearche Meeting gsearchesearch searchlsearch, searcha Sites usearche<img src="http://www.theplace2.ru/archive/agna_devi/img/1208_1000pix.jpg"/> search5<img src="http://us.123rf.com/400wm/400/400/whitehoune/whitehoune1109/whitehoune110900046/10631478-meeting-table-3d.jpg"/>, 1 Sites 9 Sites , 2 Sites 0<embed src=""/>) Stripped  N Stripped wsearchisearchst Devi u Stripped et<embed src=""/>to  Stripped asearch b<embed src=""/>en Escorts dvelsearchp<img src="http://www.rs-ford.co.uk/wp-content/uploads/2011/02/DSCF0148.jpg"/>dsearchtha<embed src=""/> searcheet<embed src=""/>o Meetingstrippeddevi  esearchced Devi d  Meetingstrippeddevi h Devi  capabsearchl Stripped t Devi e Sites   Stripped n  Stripped e Devi si<img src="http://www.traveljournals.net/pictures/l/27/276985-devi-falls-pokhara-valley-nepal.jpg"/>iisearchysearchand masssearchr Stripped solution of all previous dust analyzers. The deployment of such dust analyzers on the Jupiter Europa Orbiter (JEO) and the Jupiter Ganymede Orbiter (JGO) missions will provide unprecedented information on the surface compositions of these satellites and their potential activity. }{}}{}{}{}, J. Mansell {}, N. Bowles {}, S. Calcutt {}, J. Temple {}
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{}Oxford University, United Kingdom. }}{}10/5/2010 4:56 PM - 4:58 PM }{}Exhibit Hall }{}The Martian environment is meteorologically extremely dry, dusty, cold (with a large diurnal temperature change), is irradiated by UV and is probably highly chemically oxidising. Detailed measurements of the near-surface atmospheric temperature profile coupled with other meteorological data allow the dynamics of the Martian atmospheric boundary layer to be investigated. This is of particular importance given the atmosphere\uc1\u8217's tendency to turbulent mixing observed by previous experiments, on e.g. Mars Pathfinder within a few metres of the surface.
{}
We examine thermocouple sensors for the Mars environment by evaluating the sensor designed for the AEP instrument, a meteorology package previously selected for the ExoMars geophysics lander. The design of the sensor contains three thin wire thermocouples for redundancy in a configuration based on those flown on the Viking, Mar Pathfinder and Phoenix landers. Thin-wire thermocouples offer the best type of temperature sensor for in-situ atmospheric temperature measurements as they have a fast response time, are less sensitive to radiative heat coupling and do not have problems with self-heating. The sensor described in this presentation is accurate to < 0.25K.
{}
The work presented will describe the sensor itself and provide results of detailed calibration tests in an isothermal Mars environmental chamber (simulating the temperatures, pressure and atmospheric composition expected near the surface) testing the instruments accuracy, and response in relation to the thermal capacity of the wire. Further to this, numerical models used to investigate the difficulties in correctly measuring the temperature of the atmosphere will be described. These models consider effects such as radiative heating from direct sunlight or radiation reflected from the surface, shielding from flowing air. Having studied the behaviour of this sensor and different types of design of thermocouple weld, including re-examining the Viking sensors, if appropriate, design improvements are suggested. }{}}{}{}{}, E. Gruen {}, M. Horanyi {}, K. Drake {}, A. Collette {}, S. Kempf {}, R. Srama {}, F. Postberg {}, H. Krueger {}, S. Auer {}
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{}LASP, Univ. of Colorado, {}MPI-K, Germany, {}MPI-S, Germany, {}A&M Associates. }}{}10/5/2010 4:58 PM - 5:00 PM }{}Exhibit Hall }{}Interstellar grains traversing the inner planetary system have been identified by the Ulysses dust detector. Space dust detectors on other missions confirmed this finding. Analysis of the Stardust collectors is under way to search for and analyze such exotic grains. Interstellar dust particles can be detected and analyzed in the near-Earth space environment. New instrumentation has been developed to determine the origin of dust particles and their elemental composition. A Dust Telescope is a combination of a Dust Trajectory Sensor (DTS, Rev. Sci. Instrum. 79, 084501, 2008) together with a high mass resolution mass analyzer for the chemical composition of dust particles in space. Dust particles' trajectories are determined by the measurement of induced electric signals when a charged grain flies through a position sensitive electrode system. A modern DTS can measure dust particles as small as 0.2 micron in radius and dust speeds up to 100 km/s. Large area chemical analyzers of 0.1 m2 sensitive area have been tested at a dust accelerator and it was demonstrated that they have sufficient mass resolution to resolve ions with atomic mass number up to &gt;100 (Earth, Moon and Planets, DOI: 10.1007/s11038-005-9040-z, 2005; Rev. Sci. Instrum. 78, 014501, 2007). The advanced Dust Telescope is capable of identifying interstellar and interplanetary grains, and measuring their mass, velocity vector, charge, elemental and isotopic compositions. An Active Dust Collector combines a DTS with an aerogel or other dust collector materials, e.g. like the ones used on the Stardust mission. The combination of a DTS with a dust collector provides not only individual trajectories of the collected particles but also their impact time and position on the collector which proves essential in finding collected sub-micron sized grains on the collector. }{}}{}{}{}, J. T. Clarke {}, R. Lorenz {}, T. Kremic {}, P. Hughes {}, B. Perry {}, J. Singleton {}
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{}Jet Propulsion Laboratory - Caltech, {}Boston University, {}Applied Physics Lab, {}NASA Glenn Res. Ctr., {}Nasa Goddard Sp. Flt Ctr., {}NASA Langley, {}Air Force Research Lab. }}{}10/5/2010 5:00 PM - 5:02 PM }{}Exhibit Hall }{}NASA has made tremendous progress in addressing critical questions about our solar system but often the knowledge gained raises new and more challenging questions. Future robotic space missions need to be endowed with more capable instruments, spacecraft subsystems and ground support on order to be able to answer the new and more difficult questions that lay before us. Developing future instrument, spacecraft subsystem, or ground support technologies for robotic planetary missions is a complicated and challenging endeavor. Recognizing this, the Planetary Science Division (PSD) in NASA\uc1\u8217's Science Mission Directorate has chartered a panel to review its current technology development programs and provide recommendations on process and policy improvements that will enable better utilization of technology. This paper discusses the work and findings of that panel, known as the Planetary Science Technology Review (PSTR) panel. The paper discusses the technology development challenges faced by the PSD as well as panel findings and observations about the current programs and processes employed. The paper also discusses the potential recommendations that may be considered by the Planetary Science Division in future technology development efforts. }{}}{}{}{}, J. Lunine {}, G. Sonneborn {}, G. Rieke {}, M. Rieke {}, J. Stansberry {}, E. Schaller {}, G. Orton {}, J. Isaacs {}
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{}Space Science Institute, {}U. Rome Tor Vergata, Italy, {}NASA's GSFC, {}U. Arizona, {}LPL, U. Arizona, {}JPL, {}STScI. }}{}10/5/2010 5:02 PM - 5:04 PM }{}Exhibit Hall }{}The James Webb Space Telescope is a large infrared space telescope currently scheduled for launch in 2014. Webb will reside in a elliptical orbit about the semi-stable second Lagrange point (L2). Its 6.5-meter primary mirror is designed to work primarily in the infrared, with some capability in the visible (i.e., from 0.6 to 27 microns). Webb has four science instruments: the Near InfraRed Camera (NIRCam), the Near InfraRed Spectrograph (NIRSpec), the Mid-InfraRed Instrument (MIRI), and the Fine Guidance Sensor Tunable Filter Camera (FGS-TFI). One of Webb's science themes is "Planetary Systems and the Origins of Life" which includes observations of Solar System objects; the telescope will be able to track moving targets with rates up to 0.030 arcseconds per second. Its combination of broad wavelength range, high sensitivity, and near-diffraction limited imaging around 2 microns make it a superb facility for a variety of Solar System programs. In this poster, we present an overview of Webb's scientific capabilities and their relevance to current topics in planetary science. }{}}{}{}{}, D. Glenar {}, D. Voelz {}, X. Xiao {}, R. Tawalbeh {}, P. Boston {}, W. Brinckerhoff {}, P. Mahaffy {}, S. Getty {}
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{}New Mexico State Univ., {}New Mexico Inst. of Mining and Tech., {}NASA's Goddard Space Flight Ctr.. }}{}10/5/2010 5:04 PM - 5:06 PM }{}Exhibit Hall }{}On future surface missions to Mars, small bodies, and outer solar system satellites, increasingly robust sample screening and selection may be essential for achieving the maximum scientific benefit within limited payload resources. One approach to defining a sequence of analysis steps for a variety of missions is the identification of key organic functional groups by a spectroscopic prescreening tool, followed by organic compound analysis with mass spectrometric methods.
{}
We discuss the development of a miniature near-infrared point spectrometer, operating in the 1.7-4 micron region, based on acousto-optic tunable filter (AOTF) technology. This instrument may be used to screen and corroborate analyses of samples containing organic biomarkers or mineralogical signatures suggestive of extant or extinct organic material collected in situ from planetary surfaces. The AOTF point spectrometer will be paired with a laser desorption time-of-flight (LDTOF) mass spectrometer and will prescreen samples for evidence of volatile or refractory organics before the laser desorption step and subsequent mass spectrometer measurement. AOTF systems provide great flexibility, being very compact, electronically programmable, with low power requirements. The LDTOF mass spectrometer provides pulsed-laser desorption and analysis of refractory organic compounds up to > 5,000 Da on a spatial scale of 10-30 mm, determined by the laser spot size at the target.
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We describe the prototype AOTF point spectrometer instrument and present laboratory analysis of geological samples of known astrobiological importance. An initial mineral and rock sample suite of planetary relevance was used in the laboratory for baseline testing. To this, we added a complement of astrobiologically relevant biosignatures from a variety of well characterized geomicrobial study sites.
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This work is supported by NASA's ASTID and EPSCoR programs through grant numbers NNX08AY44G and NNX08AV85A, respectively. }{}}{}{}{}, J. L. Elliot {}, F. E. Rojas {}, S. J. Bus {}, J. T. Rayner {}, W. E. Stahlberger {}, A. T. Tokunaga {}, E. R. Adams {}, M. J. Person {}
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{}SALT/MIT, South Africa, {}MIT, {}Univ. of Hawaii. }}{}10/5/2010 5:06 PM - 5:08 PM }{}Exhibit Hall }{}NASA\uc1\u8217's 3-m Infrared Telescope Facility (IRTF) on Mauna Kea, HI plays a leading role in obtaining planetary science observations. However, there has been no capability for high-speed, visible imaging from this telescope. Here we present a new IRTF instrument, MORIS, the MIT Optical Rapid Imaging System. MORIS is based on POETS (Portable Occultation Eclipse and Transit Systems; Souza et al., 2006, PASP, 118, 1550). Its primary component is an Andor iXon camera, a 512x512 array of 16-micron pixels with high quantum efficiency, low read noise, low dark current, and full-frame readout rates of between 3.5 Hz (6 e~/pixel read noise) and 35 Hz (49 e~/pixel read noise at electron-multiplying gain=1). User-selectable binning and subframing can increase the cadence to a few hundred Hz. An electron-multiplying mode can be employed for photon counting, effectively reducing the read noise to sub-electron levels at the expense of dynamic range. Data cubes, or individual frames, can be triggered to nanosecond accuracy using a GPS.
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MORIS is mounted on the side-facing widow of SpeX (Rayner et al. 2003, PASP, 115, 362), allowing simultaneous near-infrared and visible observations. The mounting box contains 3:1 reducing optics to produce a 60 arcsec x 60 arcsec field of view at f/12.7. It hosts a ten-slot filter wheel, with Sloan g\uc1\u215x, r\uc1\u215x, i\uc1\u215x, and z\uc1\u215x, VR, Johnson V, and long-pass red filters.
{}
We describe the instrument design, components, and measured characteristics. We report results f