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Sample records for phoenix landins site

  1. Phoenix Site Panorama

    NASA Technical Reports Server (NTRS)

    2008-01-01

    [figure removed for brevity, see original site] Click on image for animation

    This movie is compiled of images from Phoenix's Stereo Surface Imager (SSI) camera that were taken on sols 1 and 3. The top images, highlighted in yellow at the beginning of the movie, have been stretched eight times to show details of features in the background. Phoenix's parachute, backshell, heatshield, and impact site can also be seen.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  2. Phoenix Site Panorama

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This view is compiled of images from Phoenix's Stereo Surface Imager (SSI) camera that were taken on sols 1 and 3. The top portion has been stretched eight fold to show details of features in the background. Phoenix's parachute, backshell, heatshield, and impact site can also be seen.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  3. Phoenix Test Sample Site

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This image, acquired by NASA's Phoenix Mars Lander's Surface Stereo Imager on Sol 7, the seventh day of the mission (June 1, 2008), shows the so-called 'Knave of Hearts' first-dig test area to the north of the lander. The Robotic Arm's scraping blade left a small horizontal depression above where the sample was taken.

    Scientists speculate that white material in the depression left by the dig could represent ice or salts that precipitated into the soil. This material is likely the same white material observed in the sample in the Robotic Arm's scoop.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  4. Phoenix Test Sample Site

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This image, acquired by NASA's Phoenix Mars Lander's Surface Stereo Imager on Sol 7, the seventh day of the mission (June 1, 2008), shows the so-called 'Knave of Hearts' first-dig test area to the north of the lander. The Robotic Arm's scraping blade left a small horizontal depression above where the sample was taken.

    Scientists speculate that white material in the depression left by the dig could represent ice or salts that precipitated into the soil. This material is likely the same white material observed in the sample in the Robotic Arm's scoop.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  5. Earth Site Corresponding to Phoenix Mars Lander Targeted Site

    NASA Image and Video Library

    2008-05-22

    The targeted landing site for NASA Phoenix Mars Lander is at about 68 degrees north latitude, 233 degrees east longitude in the Martian arctic. The Phoenix lander, which landed May 25, 2008 ceased its operations about six months later.

  6. Chlorine Salts at the Phoenix Landing Site

    NASA Astrophysics Data System (ADS)

    Hanley, J.; Horgan, B.

    2016-09-01

    Although chlorine salts (perchlorates, chlorides) are known to exist at the Phoenix landing site, their distribution and type have not been positively identified yet. We look for these salts through a novel NIR remote sensing technique.

  7. Phoenix Landing Site Indicated on Global View

    NASA Technical Reports Server (NTRS)

    2008-01-01

    NASA's Phoenix Mars Mission landed at 68.2 degrees north latitude, 234.2 degrees east longitude. The far-northern location of the site is indicated on this global view from the Mars Orbiter Camera on NASA's Mars Global Surveyor.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by JPL, Pasadena, Calif. Spacecraft development was by Lockheed Martin Space Systems, Denver.

  8. Earth Site Corresponding to Phoenix Mars Lander's Targeted Site

    NASA Technical Reports Server (NTRS)

    2008-01-01

    The targeted landing site for NASA's Phoenix Mars Lander is at about 68 degrees north latitude, 233 degrees east longitude in the Martian arctic.

    On Earth, those coordinates specify a location in northwestern Canada.

    Canada supplied the Phoenix spacecraft's Meteorological Station.

    The Phoenix Mission is led by the University of Arizona on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory. Spacecraft development is by Lockheed Martin Space Systems.

  9. Sulfur Mineralogy at the Mars Phoenix Landing Site

    NASA Technical Reports Server (NTRS)

    Ming, Douglas W.; Morris, R.V.; Golden, D.C.; Sutter, B.; Clark, B.C.; Boynton, W.V.; Hecht, M.H.; Kounaves, S.P.

    2009-01-01

    The Mars Phoenix Scout mission landed at the northernmost location (approx.68deg N) of any lander or rover on the martian surface. This paper compares the S mineralogy at the Phoenix landing site with S mineralogy of soils studied by previous Mars landers. S-bearing phases were not directly detected by the payload onboard the Phoenix spacecraft. Our objective is to derive the possible mineralogy of S-bearing phases at the Phoenix landing site based upon Phoenix measurements in combination with orbital measurements, terrestrial analog and Martian meteorite studies, and telescopic observations.

  10. Stereo View of Phoenix Test Sample Site

    NASA Image and Video Library

    2008-06-02

    This anaglyph image, acquired by NASA’s Phoenix Lander’s Surface Stereo Imager on June 1, 2008, shows a stereoscopic 3D view of the so-called Knave of Hearts first-dig test area to the north of the lander. 3D glasses are necessary to view this image.

  11. Stereo View of Phoenix Test Sample Site

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This anaglyph image, acquired by NASA's Phoenix Lander's Surface Stereo Imager on Sol 7, the seventh day of the mission (June 1, 2008), shows a stereoscopic 3D view of the so-called 'Knave of Hearts' first-dig test area to the north of the lander. The Robotic Arm's scraping blade left a small horizontal depression above where the sample was taken.

    Scientists speculate that white material in the depression left by the dig could represent ice or salts that precipitated into the soil. This material is likely the same white material observed in the sample in the Robotic Arm's scoop.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  12. Phoenix Test Sample Site in Color

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This color image, acquired by NASA's Phoenix Mars Lander's Surface Stereo Imager on Sol 7, the seventh day of the mission (June 1, 2008), shows the so-called 'Knave of Hearts' first-dig test area to the north of the lander. The Robotic Arm's scraping blade left a small horizontal depression above where the sample was taken.

    Scientists speculate that white material in the depression left by the dig could represent ice or salts that precipitated into the soil. This material is likely the same white material observed in the sample in the Robotic Arm's scoop.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  13. Phoenix Test Sample Site in Color

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This color image, acquired by NASA's Phoenix Mars Lander's Surface Stereo Imager on Sol 7, the seventh day of the mission (June 1, 2008), shows the so-called 'Knave of Hearts' first-dig test area to the north of the lander. The Robotic Arm's scraping blade left a small horizontal depression above where the sample was taken.

    Scientists speculate that white material in the depression left by the dig could represent ice or salts that precipitated into the soil. This material is likely the same white material observed in the sample in the Robotic Arm's scoop.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  14. Stereo View of Phoenix Test Sample Site

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This anaglyph image, acquired by NASA's Phoenix Lander's Surface Stereo Imager on Sol 7, the seventh day of the mission (June 1, 2008), shows a stereoscopic 3D view of the so-called 'Knave of Hearts' first-dig test area to the north of the lander. The Robotic Arm's scraping blade left a small horizontal depression above where the sample was taken.

    Scientists speculate that white material in the depression left by the dig could represent ice or salts that precipitated into the soil. This material is likely the same white material observed in the sample in the Robotic Arm's scoop.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  15. Water at the Phoenix landing site

    NASA Astrophysics Data System (ADS)

    Smith, Peter Hollingsworth

    The Phoenix mission investigated patterned ground and climate in the northern arctic region of Mars for 5 months starting May 25, 2008. A shallow ice table was uncovered by the robotic arm in a nearby polygon's edge and center at depths of 5-15 cm. In late summer snowfall and frost blanket the surface at night; water ice and vapor constantly interact with the soil. Analysis reveals an alkaline Ph with CaCO 3 , aqueous minerals, and salts making up several wt% of the soil; liquid water is implicated as having been important in creating these components. In combination with the oxidant perchlorate (~1 wt%), an energy source for terrestrial microbes, and a prior epoch of higher temperatures and humidity, this region may have been a habitable zone.

  16. The Phoenix Mission and its Current Landing Site options

    NASA Astrophysics Data System (ADS)

    Tamppari, LK; Smith, P.; Arvidson, RE; Phoenix Team

    2005-08-01

    Phoenix is the 2007 Mars Scout program mission that will send a lander and suite of instruments to study the north polar region on Mars. Central goals for the Phoenix mission are to study the recent history of water as written into the high latitude soils and to search for habitable zones. In order to do this, Phoenix carries a comprehensive suite of seven instruments. This suite includes 3 cameras, an optical microscope and an atomic-force microscope, allowing imaging at spatial scales ranging from kms, for large scale geomorphological studies, to microns, for examining single grain sizes and shapes. Phoenix also has a meteorology suite, which includes atmospheric temperature measurements at 3 levels, atmospheric pressure, and an upward-looking lidar, for dust and water-ice cloud detection. A robotic arm will dig a trench into the surface near the lander to collect and deliver samples to on-board chemistry and mineralogy experiments. These experiments will allow the detection of the mineral makeup of the soil as well as its water content, pH, salt content, and organic content. An important aspect of this exciting mission is the selection of the landing site, within the 65-72 deg N latitude band. Both science and safety concerns will play into this selection. Work is ongoing to determine the most favorable location, with consideration focusing on the best ice/soil ratio, the shallowest slopes and fewest large rocks. Current sites under consideration will be discussed. Selected in 2003, Phoenix was recently confirmed to proceed into Phase C/D of spacecraft development. This research was funded by a NASA Grant and carried out by the Jet Propulsion Laboratory, California Institute of Technology.

  17. Initial CRISM Observations of the Candidate 2007 Phoenix Landing Sites

    NASA Astrophysics Data System (ADS)

    Seelos, K. D.; Murchie, S.; Arvidson, R. E.; Seelos, F. P.

    2006-12-01

    The Mars Reconnaissance Orbiter (MRO) Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) will acquire multispectral and targeted hyperspectral visible and near infrared data of the candidate Phoenix landing sites during the first few months of primary mission operations (beginning early November). Three 150 x 75 km candidate Phoenix landing sites are located in the high northern plains of Mars within a region from 65-72° N and 120-140° E. Geomorphologic characterization of this region indicates a relatively homogeneous terrain primarily composed of multiple kilometer-scale polygonal plains with superposed degraded craters. At decameter spatial scales, the area is ubiquitously covered by patterned ground in the form of basketball terrain, stripes, and small polygons. Spectral variation of these different types of landforms and materials that are detected by CRISM at 100- or 200-meter scales (multispectral) or ~20-meter scales (targeted hyperspectral) will be analyzed and initial results presented. Implications for Phoenix landing site selection and in situ measurements will also be discussed. CRISM observations along with other MRO data will be critical to the selection of the final landing site prior to launch in August of 2007.

  18. Solar Panel Buffeted by Wind at Phoenix Site

    NASA Technical Reports Server (NTRS)

    2008-01-01

    Winds were strong enough to cause about a half a centimeter (.19 inch) of motion of a solar panel on NASA's Phoenix Mars lander when the lander's Surface Stereo Imager took this picture on Aug. 31, 2008, during the 96th Martian day since landing.

    The lander's telltale wind gauge has been indicating wind speeds of about 4 meters per second (9 miles per hour) during late mornings at the site.

    These conditions were anticipated and the wind is not expected to do any harm to the lander.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  19. Solar Panel Buffeted by Wind at Phoenix Site

    NASA Technical Reports Server (NTRS)

    2008-01-01

    Winds were strong enough to cause about a half a centimeter (.19 inch) of motion of a solar panel on NASA's Phoenix Mars lander when the lander's Surface Stereo Imager took this picture on Aug. 31, 2008, during the 96th Martian day since landing.

    The lander's telltale wind gauge has been indicating wind speeds of about 4 meters per second (9 miles per hour) during late mornings at the site.

    These conditions were anticipated and the wind is not expected to do any harm to the lander.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  20. Evidence for calcium carbonate at the Mars Phoenix landing site.

    PubMed

    Boynton, W V; Ming, D W; Kounaves, S P; Young, S M M; Arvidson, R E; Hecht, M H; Hoffman, J; Niles, P B; Hamara, D K; Quinn, R C; Smith, P H; Sutter, B; Catling, D C; Morris, R V

    2009-07-03

    Carbonates are generally products of aqueous processes and may hold important clues about the history of liquid water on the surface of Mars. Calcium carbonate (approximately 3 to 5 weight percent) has been identified in the soils around the Phoenix landing site by scanning calorimetry showing an endothermic transition beginning around 725 degrees C accompanied by evolution of carbon dioxide and by the ability of the soil to buffer pH against acid addition. Based on empirical kinetics, the amount of calcium carbonate is most consistent with formation in the past by the interaction of atmospheric carbon dioxide with liquid water films on particle surfaces.

  1. Martian Sunrise at Phoenix Landing Site, Sol 101

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This sequence of nine images taken by the Surface Stereo Imager on NASA's Phoenix Mars Lander shows the sun rising on the morning of the lander's 101st Martian day after landing.

    The images were taken on Sept. 5, 2008. The local solar times at the landing site for the nine images were between 1:23 a.m. and 1:41 a.m.

    The landing site is on far-northern Mars, and the mission started in late northern spring. For nearly the entire first 90 Martian days of the mission, the sun never set below the horizon. As the amount of sunshine each day declined steadily after that, so has the amount of electricity available for the solar-powered spacecraft.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by JPL, Pasadena, Calif. Spacecraft development was by Lockheed Martin Space Systems, Denver.

  2. Martian Sunrise at Phoenix Landing Site, Sol 101

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This sequence of nine images taken by the Surface Stereo Imager on NASA's Phoenix Mars Lander shows the sun rising on the morning of the lander's 101st Martian day after landing.

    The images were taken on Sept. 5, 2008. The local solar times at the landing site for the nine images were between 1:23 a.m. and 1:41 a.m.

    The landing site is on far-northern Mars, and the mission started in late northern spring. For nearly the entire first 90 Martian days of the mission, the sun never set below the horizon. As the amount of sunshine each day declined steadily after that, so has the amount of electricity available for the solar-powered spacecraft.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by JPL, Pasadena, Calif. Spacecraft development was by Lockheed Martin Space Systems, Denver.

  3. 78 FR 52759 - Expansion of Foreign-Trade Zone 75 Under Alternative Site Framework; Phoenix, Arizona

    Federal Register 2010, 2011, 2012, 2013, 2014

    2013-08-26

    ... ASF to include an additional magnet site, proposed Site 9, within the Phoenix, Arizona U.S. Customs...,000-acre activation limit for the zone, and to a five-year ASF sunset provision for magnet sites...

  4. Determining Size Distribution at the Phoenix Landing Site

    NASA Astrophysics Data System (ADS)

    Mason, E. L.; Lemmon, M. T.

    2016-12-01

    Dust aerosols play a crucial role in determining atmospheric radiative heating on Mars through absorption and scattering of sunlight. How dust scatters and absorbs light is dependent on size, shape, composition, and quantity. Optical properties of the dust have been well constrained in the visible and near infrared wavelengths using various methods [Wolff et al. 2009, Lemmon et al. 2004]. In addition, the dust is nonspherical, and irregular shapes have shown to work well in determining effective particle size [Pollack et al. 1977]. Variance of the size distribution is less constrained but constitutes an important parameter in fully describing the dust. The Phoenix Lander's Surface Stereo Imager performed several cross-sky brightness surveys to determine the size distribution and scattering properties of dust in the wavelength range of 400 to 1000 nm. In combination with a single-layer radiative transfer model, these surveys can be used to help constrain variance of the size distribution. We will present a discussion of seasonal size distribution as it pertains to the Phoenix landing site.

  5. The water cycle at the Phoenix landing site, Mars

    NASA Astrophysics Data System (ADS)

    Cull, Selby

    2010-01-01

    The water cycle is critically important to understanding Mars system science, especially interactions between water and surface minerals or possible biological systems. In this thesis, the water cycle is examined at the Mars Phoenix landing site (68.22°N, 125.70°W), using data from the Compact Reconnaissance Imaging Spectrometer for Mars (CRISM), High-Resolution Imaging Science Experiment (HiRISE), the Phoenix Lander Surface Stereo Imager (SSI), and employing non-linear spectral mixing models. The landing site is covered for part of the year by the seasonal ice cap, a layer of CO2 and H2O ice that is deposited in mid-fall and sublimates in mid-spring. During the mid-summer, H2O ice is deposited on the surface at the Phoenix landing site. CO2 ice forms at the site during fall. The onset date of seasonal ices varies annually, perhaps due to variable levels of atmospheric dust. During fall and winter, the CO2 ice layer thickens and sinters into a slab of ice, ˜30 cm thick. After the spring equinox, the CO2 slab breaks into smaller grains as it sublimates. Long before all of the CO2 ice is gone, H2O ice dominates the near-infrared spectra of the surface. Additional H2O ice is cold-trapped onto the surface of the CO2 ice deposit during this time. Sublimation during the spring is not uniform, and depends on the thermal inertia properties of the surface, including depth of ground ice. All of the seasonal ices have sublimated by mid-spring; however, a few permanent ice deposits remain throughout the summer. These are small water ice deposits on the north-facing slopes of Heimdal Crater and adjacent plateaus, and a small patch of mobile water ices that chases shadows in a small crater near the landing site. During the late spring and early summer, the site is free of surface ice. During this time, the water cycle is dominated by vapor exchange between the subsurface water ice deposits and the atmosphere. Two types of subsurface ice were found at the Phoenix landing site

  6. 77 FR 74457 - Foreign-Trade Zone 75-Phoenix, Arizona Application for Expansion (New Magnet Site) Under...

    Federal Register 2010, 2011, 2012, 2013, 2014

    2012-12-14

    ... Foreign-Trade Zones Board Foreign-Trade Zone 75--Phoenix, Arizona Application for Expansion (New Magnet...)) to include a new magnet site in Phoenix, Arizona. The application was submitted pursuant to the... following magnet sites: Site 1 (338 acres)--within the 550-acre Phoenix Sky Harbor Center and adjacent...

  7. Ground Ice at the Phoenix Landing Site: A Preflight Assessment

    NASA Technical Reports Server (NTRS)

    Mellon, M. T.; Arvidson, R. E.; Seelos, F.; Tamppari, L. K.; Boynton, W. V.; Smith, P.

    2004-01-01

    One of the objectives of the Mars Scout mission, Phoenix, is to characterize the present state of water in the martian environment, in a location where water may play a significant role in the present and past habitability of Mars. Given the generally dry and cold climate of Mars today any substantial amount of water is expected to occur in the form of ground ice (subsurface ice) within the regolith. The Mars Odyssey Gamma Ray Spectrometer has indicated abundant subsurface hydrogen and inferred ground ice at high latitudes. Therefore, the Phoenix mission will be targeted to land in the northern high latitudes (approximately 65 degrees N - 75 degrees N) where ground ice is expected to be abundantly available for analysis. The lander will be capable of excavating, sampling, and analyzing, dry and water-rich/icy soils. The location and depth of excavation necessary to achieve the goals of sampling and analysis of icy material become important parameters to assess. In the present work we ask two key questions: 1) At what depth within the regolith do we expect to find ice? 2) How might this depth vary over the region of potential landing sites? Numerous lines of evidence can be employed to provide an indication of the presence or absence of shallow ground ice at the potential landing sites. For example geomorphology, neutrons, gamma rays, and theory each contribute clues to an overall understanding of the distribution of ice. Orbital observations provide information on a variety of spatial scales, typically 10 s of meters (patterned ground) to 100 s of kilometers (gamma rays). While information on all of these scales are important, of particular interest is how the presence and depth of ground ice might vary on spatial scales comparable to the lander and its work area. While ground ice may be stable (and present) on a regional scale, local-scale slopes and changes in the physical characteristics of soils can result in significant variations in the distribution of ice.

  8. Mars Exploration Program 2007 Phoenix landing site selection and characteristics

    USGS Publications Warehouse

    Arvidson, R.; Adams, D.; Bonfiglio, G.; Christensen, P.; Cull, S.; Golombek, M.; Guinn, J.; Guinness, E.; Heet, T.; Kirk, R.; Knudson, A.; Malin, M.; Mellon, M.; McEwen, A.; Mushkin, A.; Parker, T.; Seelos, F.; Seelos, K.; Smith, P.; Spencer, D.; Stein, T.; Tamppari, L.

    2009-01-01

    To ensure a successful touchdown and subsequent surface operations, the Mars Exploration Program 2007 Phoenix Lander must land within 65?? to 72?? north latitude, at an elevation less than -3.5 km. The landing site must have relatively low wind velocities and rock and slope distributions similar to or more benign than those found at the Viking Lander 2 site. Also, the site must have a soil cover of at least several centimeters over ice or icy soil to meet science objectives of evaluating the environmental and habitability implications of past and current near-polar environments. The most challenging aspects of site selection were the extensive rock fields associated with crater rims and ejecta deposits and the centers of polygons associated with patterned ground. An extensive acquisition campaign of Odyssey Thermal Emission Imaging Spectrometer predawn thermal IR images, together with ???0.31 m/pixel Mars Reconnaissance Orbiter High Resolution Imaging Science Experiment images was implemented to find regions with acceptable rock populations and to support Monte Carlo landing simulations. The chosen site is located at 68.16?? north latitude, 233.35?? east longitude (areocentric), within a ???50 km wide (N-S) by ???300 km long (E-W) valley of relatively rock-free plains. Surfaces within the eastern portion of the valley are differentially eroded ejecta deposits from the relatively recent ???10-km-wide Heimdall crater and have fewer rocks than plains on the western portion of the valley. All surfaces exhibit polygonal ground, which is associated with fracture of icy soils, and are predicted to have only several centimeters of poorly sorted basaltic sand and dust over icy soil deposits. Copyright 2008 by the American Geophysical Union.

  9. Subsurface Materials Exposed at the Phoenix Landing Site

    NASA Astrophysics Data System (ADS)

    Blaney, D.; Archer, D.; Arvidson, R.; Cull, S.; Ellehoj, M.; Fisher, D.; Hecht, M.; Lemmon, M.; Mellon, M.; Morris, R.; Pike, T.; Stoker, C.

    2008-12-01

    The Phoenix Mission excavated materials at the Phoenix Landing site using the Robotic Arm (RA) while materials in the trenches and in the talus piles were documented with the Surface Stereo Imager (SSI) using 15 filters with bands from 485-1005 nm. Two polygons (Humpty Dumpty and Wonderland) are in the workspace and have frozen ice/soils mixtures that were exposed and monitored. Samples collected from the trenches were also delivered by the MECA Optical Microscope (OM) providing information on the optical properties and grain size/texture of these materials at microscopic scales. Excavations in Humpty Dumpty (Dodo-Goldilocks and Upper Cupboard trenches) revealed a high albedo deposit consistent with a relatively pure ice spectrally. Dodo-Goldilocks was first exposed on Sol 9 with digging stopping on Sol 21. The ice in Dodo-Goldilocks was left undisturbed till Sol 99. The sublimation process monitored using 15 filter observations. Over time the ice signature decreased in the deposit and became consistent with the surface soils seen at the landing site. Sublimation was not uniform with some high albedo patches prominent on Sol 102. On Sol 99 the robotic arm scraped the sublimation lag from Dodo-Goldilocks and delivered the sample to the MECA OM. Collection of the sample exposed fresh high albedo ice. High albedo materials at the Dodo-Goldilocks and Upper Cupboard trenches were generally hard based on interactions with the Robotic Arm. During the initial excavation, clods of ice/soil mixtures were produced that sublimated away over within 4 sols. These ice clods could have been formed by brittle fracture of very cold pure ice or be a small deposit of weaker ice soil/layer on top of the Dodo-Goldilocks deposit. Excavation in Wonderland (Snow White trench) revealed an ice/soil mixture with significantly more soil than at Dodo-Goldilocks based on spectral characteristics. After exposing a harder, spectrally different layer with the RA secondary blade, sublimation of

  10. Dark Skies and Clouds Move in at Phoenix site

    NASA Technical Reports Server (NTRS)

    2008-01-01

    Clouds of dust and ice swirl past the Surface Stereo Imager (SSI) camera on NASA's Phoenix Mars Lander in a series of images taken on the 132nd Martian day of the mission (Oct. 7, 2008). The images show the increase in storm activity and potential for snowfall.

    The solar powered spacecraft was disabled by decreased light from heavy dust storms in the area a few weeks later. The last communication heard from the lander occurred on Nov. 2, 2008.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  11. Dark Skies and Clouds Move in at Phoenix site

    NASA Technical Reports Server (NTRS)

    2008-01-01

    Clouds of dust and ice swirl past the Surface Stereo Imager (SSI) camera on NASA's Phoenix Mars Lander in a series of images taken on the 132nd Martian day of the mission (Oct. 7, 2008). The images show the increase in storm activity and potential for snowfall.

    The solar powered spacecraft was disabled by decreased light from heavy dust storms in the area a few weeks later. The last communication heard from the lander occurred on Nov. 2, 2008.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  12. Size-Frequency Distribution of Rock Clasts at the Phoenix Landing Site

    NASA Astrophysics Data System (ADS)

    Heet, T. L.; Arvidson, R. E.; Mellon, M. T.; Golombek, M. P.; Marshall, J.

    2008-12-01

    Rock populations on the plains surrounding the Phoenix landing site were analyzed using a combination of ground-based and orbital data. We determined the size-frequency distribution of rocks larger than 1.5 meters in diameter using images from the Mars Reconnaissance Orbiter High Resolution Imaging Science Experiment (HiRISE). Surface images taken by the Phoenix Lander Surface Stereo Imager camera were used to characterize the size-frequency distribution of rocks as small as 2 centimeters. Comparison of the size-frequency distribution of rocks for the Phoenix landing site with model curves shows that the rock population is characterized by significantly more pebble-sized rocks (>10 centimeters) than simple crushing models predict. Additionally, comparison with rock counts from Mars Exploration Rover Spirit rover images show that the Phoenix landing site is depleted in rocks relative to the Gusev plains. The depletion of rocks of all sizes at the Phoenix landing site is consistent with the proposed hypothesis that rocks were removed from the surface during fluidized ejecta emplacement by nearby Heimdall crater. We also characterized rock populations on a detailed scale within eight meters of the Phoenix Lander. Results indicate that more rocks are located in polygon troughs than in polygon interiors, although the biggest rocks are found within polygon interiors. Nearest neighbor statistics show that rocks with diameters between 2cm and 30cm on polygon interiors are clumped or less uniformly dispersed, whereas rocks in polygon troughs are uniformly spaced. The differences observed between rock distributions within the polygon interior and polygon trough units suggest that polygons are actively redistributing rocks in a manner consistent with thermal-contraction-based cryoturbation.

  13. Mars 101: Linking Educational Content to Mission Purpose on the Phoenix Mars Lander Mission Web Site

    NASA Astrophysics Data System (ADS)

    Schmidt, L. J.; Smith, P. H.; Lombardi, D.

    2006-12-01

    The Phoenix Mars Lander, scheduled to launch in August 2007, is the first mission in NASA's Scout Program. Phoenix has been specifically designed to measure volatiles (especially water) in the northern arctic plains of Mars, where the Mars Odyssey detected evidence of ice-rich soil near the surface. A fundamental part of the mission's goal-driven education and public outreach program is the Phoenix Mars Lander 2007 web site. Content for the site was designed not only to further the casual user's understanding of the Phoenix mission and its objectives, but also to meet the needs of the more science-attentive user who desires in-depth information. To this end, the web site's "Mars 101" module includes five distinct themes, all of which are directly connected to the mission's purpose: Mars Intro includes basic facts about Mars and how the planet differs from Earth; Polar Regions discusses the history of polar exploration on Earth and the similarities between these regions on Mars and Earth; Climate covers the effects that Earth's polar regions have on climate and how these same effects may occur on Mars; Water on Mars introduces the reader to the idea of liquid water and water ice on Mars; and Biology includes a discussion of the requirements of life and life in the universe to facilitate reader understanding of what Phoenix might find. Each of the five themes is described in simple language accompanied by relevant images and graphics, with hypertext links connecting the science-attentive user to more in-depth content. By presenting the "Mars 101" content in a manner that relates each subheading to a specific component of the mission's purpose, the Phoenix web site nurtures understanding of the mission and its relevance to NASA's Mars Exploration goals by the general lay public as well as the science-attentive user.

  14. Evidence for Calcium Carbonate at the Phoenix Landing Site

    NASA Technical Reports Server (NTRS)

    Boynton, W. V.; Ming, D. W.; Sutter, B.; Arvidson, R. E.; Hoffman, J.; Niles, P. B.; Smith, P.

    2009-01-01

    The Phoenix mission has recently finished its study of the north polar environment of Mars with the aim to help understand both the current climate and to put constraints on past climate. An important part of understanding the past climate is the study of secondary minerals, those formed by reaction with volatile compounds such as H2O and CO2. This work describes observations made by the Thermal and Evolved-Gas Analyzer (TEGA) on the Phoenix Lander related to carbonate minerals. Carbonates are generally considered to be products of aqueous processes. A wet and warmer climate during the early history of Mars coupled with a much denser CO2 atmosphere are ideal conditions for the aqueous alteration of basaltic materials and the subsequent formation of carbonates. Carbonates (Mg- and Ca-rich) are predicted to be thermodynamically stable minerals in the present martian environment, however, there have been only a few indications of carbonates on the surface by a host of orbiting and landed missions to Mars. Carbonates (Mg-rich) have been suggested to be a component (2-5 wt %) of the martian global dust based upon orbital thermal emission spectroscopy. The identifications, based on the presence of a 1480 cm-1 absorption feature, are consistent with Mgcarbonates. A similar feature is observed in brighter, undisturbed soils by Mini-TES on the Gusev plains. Recently, Mg-rich carbonates have been identified in the Nili Fossae region by the CRISM instrument onboard the Mars Reconnaissance Orbiter. Carbonates have also been confirmed as aqueous alteration phases in martian meteorites so it is puzzling why there have not been more discoveries of carbonates by landers, rovers, and orbiters. Carbonates may hold important clues about the history of liquid water and aqueous processes on the surface of Mars.

  15. Discovery of Perchlorate at the Phoenix Landing Site

    NASA Astrophysics Data System (ADS)

    Hecht, M. H.; Kounaves, S. P.; Quinn, R. C.; West, S. J.; Young, S. M.; Clark, B. C.; Deflores, L. P.; Kapit, J. A.; Gospodinova, K.; Smith, P. H.; Team, T. P.

    2008-12-01

    One of several payload components on the Phoenix Lander, the Microscopy, Electrochemistry, and Conductivity Analyzer (MECA) is a suite of instruments that includes a microscopy station (optical and atomic force), four wet chemistry laboratories (WCL), and a soil probe. After the addition of up to 1 cm3 of martian soil into 25 ml of an aqueous calibration solution, the WCL measures solution cation and anion concentration, including pH, as well as total conductivity and cyclic voltammetry. With the exception of a redundant coulombic titration of halides, all cation and anion measurements are made with ion selective electrodes (ISE). Among the species not directly measured are sulfate and carbonate, which can be inferred indirectly by the response to acid and Ba additions, and soluble Fe, which can sometimes be detected with cyclic voltammetry. Responses from several cation and anion sensors were observed almost immediately upon addition of soil to the solution. Most striking was a three order-of-magnitude increase of the Hofmeister series sensor, which could only be explained by a large concentration of the perchlorate ion, ClO4-. Perchlorates are highly water soluble oxidants, often deliquescent, and some are powerful freezing-point depressors that can form aqueous brines at mean Martian temperatures appropriate to this region, as low as -70 deg C. This combination of properties has implications that span the disciplines of geochemistry, atmospheric sciences, astrobiology, and the potential for future human exploration. An important qualification of any such discussion, however, is uncertainty about how widespread the distribution of perchlorate may be. Other WCL findings, including alkaline pH and buffered response to purposeful addition of acid consistent with the presence of carbonates, will also be summarized.

  16. 75 FR 17692 - Foreign-Trade Zone 75 -- Phoenix, Arizona, Application for Reorganization under Alternative Site...

    Federal Register 2010, 2011, 2012, 2013, 2014

    2010-04-07

    ...-acre Phoenix Sky Harbor Center and adjacent air cargo terminal at the Phoenix Sky Harbor International...) - the jet fuel storage and distribution system at and adjacent to the Phoenix Sky Harbor International...

  17. Microscopic Investigation of Martian Soil Samples at the Phoenix Site

    NASA Astrophysics Data System (ADS)

    Pike, W. T.; Staufer, U.; Hecht, M. H.; Marshall, J.; Team, M. M.

    2008-12-01

    We have used the optical and atomic force microscopes (OM and AFM) of the MECA microscopy station on Phoenix (M. Hecht et al., Microscopy Capabilities of the Microscopy, Electrochemistry, and Conductivity Analyzer , JGR accepted for publication) to image samples within reach of the robot arm and delivered to sets of substrates mounted in a sample wheel. For loading the sample, the wheel was pushed out of the MECA enclosure, exposing only one set of substrates: strong and weak magnets, micro-buckets, silicone and silicon featuring grids of micromachined small holes and posts to capture particles. A thickness of up to 200 micrometers of material can be brought into the microscopy station under a leveling blade before the samples are rotated into the field of view of the microscopes as the substrates are tilted from horizontal to vertical. This tilt can cause the loss of a portion of the material depending on the relative strength of the adhesion forces compared to Martian gravity. The time constraints of sample delivery have so far ensured that any ice would have sublimed prior to delivery. From OM images of fully loaded substrates the particles found so far can be very coarsely grouped into three different categories: 1. subrounded strongly magnetic grains, of both a rough and glassy appearance with different shades of yellow, red, brown and black color in a size range of 50 to 100 micrometers, comprising about 10% of the sample volume; 2. small white flecks of a few micrometers in size, about 0.5% of the sample volume; 3. a majority component of a fine, uniformly coloured orange-reddish dust forming agglomerations from a few tens of microns in diameter to below the resolution of the OM with less magnetic attraction than the larger grains. Using populations on more sparsely populated substrates a size distribution could be estimated. The particle size distribution increases with decreasing size until cut off by the 4-micrometer resolution limit of the OM. The AFM

  18. Convective vortices and dust devils at the Phoenix Mars mission landing site

    NASA Astrophysics Data System (ADS)

    Ellehoj, M. D.; Gunnlaugsson, H. P.; Taylor, P. A.; Kahanpää, H.; Bean, K. M.; Cantor, B. A.; Gheynani, B. T.; Drube, L.; Fisher, D.; Harri, A.-M.; Holstein-Rathlou, C.; Lemmon, M. T.; Madsen, M. B.; Malin, M. C.; Polkko, J.; Smith, P. H.; Tamppari, L. K.; Weng, W.; Whiteway, J.

    2010-04-01

    The Phoenix Mars Lander detected a larger number of short (˜20 s) pressure drops that probably indicate the passage of convective vortices or dust devils. Near-continuous pressure measurements have allowed for monitoring the frequency of these events, and data from other instruments and orbiting spacecraft give information on how these pressure events relate to the seasons and weather phenomena at the Phoenix landing site. Here 502 vortices were identified with a pressure drop larger than 0.3 Pa occurring in the 151 sol mission (Ls 76 to 148). The diurnal distributions show a peak in convective vortices around noon, agreeing with current theory and previous observations. The few events detected at night might have been mechanically forced by turbulent eddies caused by the nearby Heimdal crater. A general increase with major peaks in the convective vortex activity occurs during the mission, around Ls = 111. This correlates with changes in midsol surface heat flux, increasing wind speeds at the landing site, and increases in vortex density. Comparisons with orbiter imaging show that in contrast to the lower latitudes on Mars, the dust devil activity at the Phoenix landing site is influenced more by active weather events passing by the area than by local forcing.

  19. Phoenix landing site and sample context images from the Surface Stereo Imager

    NASA Astrophysics Data System (ADS)

    Lemmon, M. T.; Arvidson, R.; Blaney, D.; Dejong, E.; Madsen, M. B.; Malin, M.; Mellon, M.; Morris, R.; Pike, W. T.; Smith, P. H.; Stoker, C.; Team, P. S.

    2008-12-01

    Phoenix landed in the northern plains of Mars in an area with low rock abundance dominated by few-meter- scale polygonal patterned ground with decimeter scale troughs. The Phoenix Surface Stereo Imager (SSI) provides geomorphic and spectral information about the Phoenix landing site for scales that range from site- wide to context for samples analyzed by other Phoenix instruments. The SSI is a multispectral stereo camera with properties that are comparable to the Mars Exploration Rover Pancam. It has MER-heritage 1024x1024 pixel detectors, a 14-degree field of view for individual images, and resolution as high as 1-2 mm for near- field terrain (0.24 mrad/pixel). Images are taken through one of 24 filters, including 13 unique spectral bandpasses, 2 stereo bandpasses, 2 filters paired with lenses for best focus on the lander deck, 6 solar filters for atmospheric dust and water vapor and ice measurements, and 1 polarizer. The stereo separation of the eyes is 15 cm, and the focus and toe-in are optimized at 3 to 3.5 m to support Robotic Arm (RA) operations. SSI can image from the camera bar at -72 degrees to the zenith, and through 360 degrees of azimuth. As with Pancam, panoramic images are built on the ground from a number of individual frames. SSI provided geomorphic information through a set of campaigns. Three major site panoramas were acquired: on sols 1 and 3, a low-resolution monochromatic site panorama provided context for higher- resolution images in the RA workspace; a color-stereo panorama was completed on sol 43; a multispectral high-resolution panorama is currently underway. High resolution detail observations were conducted throughout the mission for high priority targets in and beyond the workspace. These campaigns show a landscape dominated by polygons with typical diameters of 2 to 4 meters. Troughs between the polygons have depths of typically 5-20 cm relative to the polygon centers. Phoenix landed with access to a trough and parts of two polygons

  20. An Application Using Triaxial Ellipsoids to Model Martian Dust at the Phoenix Landing Site

    NASA Astrophysics Data System (ADS)

    Mason, E. L.; Lemmon, M. T.

    2014-12-01

    Martian atmospheric dust is not spherical and contains irregular shaped particles. This irregularity adds complexity to models determining radiative heating of the atmosphere. Particle size has been studied extensively with remote sensing, but particle shape is still poorly understood. Bi et al. show that an assortment of triaxial ellipsoids provides a good analog for the scattering properties of terrestrial dust aerosols. In addition Z. Meng et al. (2010) have developed a database containing single-scattering properties of irregularly shaped dust particles with pre-defined microphysical and optical parameters. The tabulation allows quick and efficient use of the results from time-consuming models and can be applied to the Martian atmosphere. The landing site for Phoenix was in a region that fell within the northern seasonal ice cap and was active during a period of large dust upwelling. The lander's Surface Stereo Imager performed several cross-sky brightness surveys to constrain the size distribution and scattering and absorption properties of the airborne dust in the Martian northern polar environment. Using the database, single scattering properties adapted to the Martian atmosphere can be used to determine bulk scattering properties of the medium at the Phoenix landing site. We will present a comparison of triaxial ellipsoids with spheroidal models using Phoenix spectrophotometric data and show that triaxial ellipsoid properties can produce a good fit to the observed data. In addition we will provide initial results of polarization to test the triaxial ellipsoid hypothesis.

  1. Full-Circle Color Panorama of Phoenix Lander Deck and Landing Site on Northern Mars, Animation

    NASA Technical Reports Server (NTRS)

    2008-01-01

    [figure removed for brevity, see original site] Click on image to view the animation

    This view combines more than 500 images taken after NASA's Phoenix Mars Lander arrived on an arctic plain at 68.22 degrees north latitude, 234.25 degrees east longitude on Mars.

    This movie makes a slow tour around highlights of the image including the landscape and the spacecraft's science deck.

    The full-circle panorama in approximately true color shows the polygonal patterning of ground at the landing area, similar to patterns in permafrost areas on Earth. The center of the image is the westward part of the scene. Trenches where Phoenix's robotic arm has been exposing subsurface material are visible in the right half of the image. The spacecraft's meteorology mast, topped by the telltale wind gauge, extends into the sky portion of the panorama.

    This view comprises more than 100 different Stereo Surface Imager camera pointings, with images taken through three different filters at each pointing. It is presented here as a cylindrical projection.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  2. Full-Circle Color Panorama of Phoenix Lander Deck and Landing Site on Northern Mars, Animation

    NASA Technical Reports Server (NTRS)

    2008-01-01

    [figure removed for brevity, see original site] Click on image to view the animation

    This view combines more than 500 images taken after NASA's Phoenix Mars Lander arrived on an arctic plain at 68.22 degrees north latitude, 234.25 degrees east longitude on Mars.

    This movie makes a slow tour around highlights of the image including the landscape and the spacecraft's science deck.

    The full-circle panorama in approximately true color shows the polygonal patterning of ground at the landing area, similar to patterns in permafrost areas on Earth. The center of the image is the westward part of the scene. Trenches where Phoenix's robotic arm has been exposing subsurface material are visible in the right half of the image. The spacecraft's meteorology mast, topped by the telltale wind gauge, extends into the sky portion of the panorama.

    This view comprises more than 100 different Stereo Surface Imager camera pointings, with images taken through three different filters at each pointing. It is presented here as a cylindrical projection.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  3. Full-Circle Color Panorama of Phoenix Landing Site on Northern Mars

    NASA Technical Reports Server (NTRS)

    2008-01-01

    [figure removed for brevity, see original site] Click on image for animation

    This view combines more than 400 images taken during the first several weeks after NASA's Phoenix Mars Lander arrived on an arctic plain at 68.22 degrees north latitude, 234.25 degrees east longitude on Mars.

    The full-circle panorama in approximately true color shows the polygonal patterning of ground at the landing area, similar to patterns in permafrost areas on Earth. The center of the image is the westward part of the scene. Trenches where Phoenix's robotic arm has been exposing subsurface material are visible in the right half of the image. The spacecraft's meteorology mast, topped by the telltale wind gauge, extends into the sky portion of the panorama.

    This view comprises more than 100 different camera pointings, with images taken through three different filters at each pointing. It is presented here as a cylindrical projection.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  4. Full-Circle Color Panorama of Phoenix Landing Site on Northern Mars

    NASA Technical Reports Server (NTRS)

    2008-01-01

    [figure removed for brevity, see original site] Mission Success Pan Click on image to view the movie

    This view combines more than 400 images taken during the first several weeks after NASA's Phoenix Mars Lander arrived on an arctic plain at 68.22 degrees north latitude, 234.25 degrees east longitude on Mars.

    The movie makes a slow tour around highlights of the image.

    The full-circle panorama in approximately true color shows the polygonal patterning of ground at the landing area, similar to patterns in permafrost areas on Earth. The center of the image is the westward part of the scene. Trenches where Phoenix's robotic arm has been exposing subsurface material are visible in the right half of the image. The spacecraft's meteorology mast, topped by the telltale wind gauge, extends into the sky portion of the panorama.

    This view comprises more than 100 different camera pointings, with images taken through three different filters at each pointing. It is presented here as a cylindrical projection.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  5. Full-Circle Color Panorama of Phoenix Landing Site on Northern Mars

    NASA Technical Reports Server (NTRS)

    2008-01-01

    [figure removed for brevity, see original site] Mission Success Pan Click on image to view the movie

    This view combines more than 400 images taken during the first several weeks after NASA's Phoenix Mars Lander arrived on an arctic plain at 68.22 degrees north latitude, 234.25 degrees east longitude on Mars.

    The movie makes a slow tour around highlights of the image.

    The full-circle panorama in approximately true color shows the polygonal patterning of ground at the landing area, similar to patterns in permafrost areas on Earth. The center of the image is the westward part of the scene. Trenches where Phoenix's robotic arm has been exposing subsurface material are visible in the right half of the image. The spacecraft's meteorology mast, topped by the telltale wind gauge, extends into the sky portion of the panorama.

    This view comprises more than 100 different camera pointings, with images taken through three different filters at each pointing. It is presented here as a cylindrical projection.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  6. Phoenix Mars Lander: Vortices and Dust Devils at the Landing Site

    NASA Astrophysics Data System (ADS)

    Ellehoj, M. D.; Taylor, P. A.; Gunnlaugsson, H. P.; Gheynani, B. T.; Drube, L.; von Holstein-Rathlou, C.; Whiteway, J.; Lemmon, M.; Madsen, M. B.; Fisher, D.; Volpe, R.; Smith, P.

    2008-12-01

    Near continuous measurements of temperatures and pressure on the Phoenix Mars Lander are used to identify the passage of vertically oriented vortex structures at the Phoenix landing site (126W, 68N) on Mars. Observations: During the Phoenix mission the pressure and temperature sensors frequently detected features passing over or close to the lander. Short duration (order 20 s) pressure drops of order 1-2 Pa, and often less, were observed relatively frequently, accompanied by increases in temperature. Similar features were observed from the Pathfinder mission, although in that case the reported pressure drops were often larger [1]. Statistics of the pressure drop features over the first 102 sols of the Phoenix mission shows that most of the events occur between noon and 15:00 LMST - the hottest part of the sol. Dust Raising: By assuming the concept of a vortex in cyclostrophic flow as well as various assumptions about the atmosphere, we obtain a pressure drop of 1.9 - 3.2 Pa if dust is to be raised. We only saw few pressure drops this large in Sols 0-102. However, the features do not need to pass directly over the lander and the pressures could be lower than the minima we measure. Furthermore, the response time of the pressure sensor is of order 3-5 s so it may not capture peak pressure perturbations. Thus, more dust devils may have occurred near the Phoenix site, but most of our detected vortices would be ghostly, dustless devils. Modelling: Using a Large Eddy Simulation model, we can simulate highly convective boundary layers on Mars [2]. The typical vortex has a diameter of 150 m, and extends up to 1 km. Further calculations give an incidence of 11 vortex events per day that could be compatible with the LES simulations. Deeper investigation of this is planned -but the numbers are roughly compatible. If the significant pressure signatures are limited to the center of the vortex then 5 per sol might be appropriate. The Phoenix mission has collected a unique set of

  7. Periglacial landforms at the Phoenix landing site and the northern plains of Mars

    NASA Astrophysics Data System (ADS)

    Mellon, Michael T.; Arvidson, Raymond E.; Marlow, Jeffrey J.; Phillips, Roger J.; Asphaug, Erik

    2008-11-01

    We examine potentially periglacial landforms in Mars Orbiter Camera (MOC) and High Resolution Imaging Science Experiment (HiRISE) images at the Phoenix landing site and compare them with numerical models of permafrost processes to better understand the origin, nature, and history of the permafrost and the surface of the northern plains of Mars. Small-scale (3-6 m) polygonal-patterned ground is ubiquitous throughout the Phoenix landing site and northern plains. Larger-scale (20-25 m) polygonal patterns and regularly spaced (20-35 m) rubble piles (localized collections of rocks and boulders) are also common. Rubble piles were previously identified as ``basketball terrain'' in MOC images. The small polygon networks exhibit well-developed and relatively undegraded morphology, and they overlay all other landforms. Comparison of the small polygons with a numerical model shows that their size is consistent with a thermal contraction origin on current-day Mars and are likely active. In addition, the observed polygon size is consistent with a subsurface rheology of ice-cemented soil on depth scales of about 10 m. The size and morphology of the larger polygonal patterns and rubble piles indicate a past episode of polygon formation and rock sorting in thermal contraction polygons, while the ice table was about twice as deep as it is presently. The pervasive nature of small and large polygons, and the extensive sorting of surface rocks, indicates that widespread overturning of the surface layer to depths of many meters has occurred in the recent geologic past. This periglacial reworking has had a significant influence on the landscape at the Phoenix landing site and over the Martian northern plains.

  8. A Physical Taxonomy of Martian Sand and Dust Grainsat the Phoenix Landing Site

    NASA Astrophysics Data System (ADS)

    Marshall, John; Stoker, Carol

    2014-11-01

    A quantitative taxonomy of martian sand and dust grains for soil samples at the Phoenix lander site has been developed from the mission’s optical microscope data with a resolution of 4 μm per pixel. Approx. 3-4000 grains were analyzed for color, hue, size, shape, surface texture, aspect ratio, and optical properties. At least 26 types of sand and dust grains have been identified. Grain colors include black, brown, orange, red, white, and clear. Most grains are opaque, but many are translucent or transparent. Grain shapes range from botryoidal, blackberry-like, bead-like and rounded, to subrounded, elongate, angular, and highly irregular forms. Surface textures range from knobbly, rough, and multifaceted to smooth and polished. Surface reflectivity varied from dull to shiny to specularly reflective. Materials may include augite, pyroxenes, olivine, volcanic glass, hematite, other iron oxides, and salts. Grain size of the sand has a modal value of ~90 μm, but there is no gradation into dust sizes, indicating a bimodal distribution of the samples. The dust was probably imported into the region from aeolian dust storms. This accords with a mineralogical dissimilarity between the sand and dust grain populations. The sand is dominated by black and brown grains; the dust is dominated by orange grains. The Phoenix site also has centimeter and larger stones in abundance that again have no apparent gradation into the sand size material. Thus, the Phoenix landing site soil appears multimodal. The soil appears to be magnetically susceptible, but it is unclear what the source of magnetism might be. Specific magnetic minerals were not identified in the samples with the possible exception of paramagnetic microbotryoidal hematite. The soil was nevertheless adhesive to the substrates and internally cohesive (forming spherical aggregates) owing to van der Waals forces and possibly salt/moisture bonding.

  9. Subsurface ices at the Mars Phoenix Landing Site: Assessing emplacement mechanisms

    NASA Astrophysics Data System (ADS)

    Cull, S.; Arvidson, R. E.; Mellon, M. T.; Skemer, P. A.; Shaw, A.; Morris, R. V.

    2010-12-01

    Several mechanisms have been proposed to explain the emplacement of subsurface ices on Mars: vapor diffusion from the atmosphere, freezing of bodies of surface water (e.g., lakes or oceans), buried glaciers, or accumulation and burial of packed snow. These formation mechanisms predict different physical properties for the subsurface ices: vapor diffusion should produce pore ice, whereas other mechanisms should produce massive, relatively pure ice. NASA's Phoenix Lander uncovered two types of ice at its 2008 landing site on the northern plains of Mars: a light-toned ice (Dodo-Goldilocks) that broke into pieces during backhoe operations; and a hard, darker icy surface that had to be scraped to provide particulate materials for sampling (Snow White). Here, we use spectra from Phoenix's Surface Stereo Imager (SSI) and a non-linear mixing model with ice and soil components to determine the ice to soil ratio of the ices exposed at the Phoenix landing site. We find Dodo-Goldilocks consists of almost pure water ice. The darker icy material contains ~30 wt% ice (~55 vol%), indicating that it probably formed as pore ice between grains of soil. We conclude that these two types of ice represent two different emplacement mechanisms and periods of deposition. Snow White ice was probably deposited via vapor diffusion from the atmosphere. Dodo-Goldilocks ice was probably deposited through an ice-lens or needle ice mechanism. Buried snow or glacial ice is unlikely for Dodo-Goldilocks, given its restricted spatial extent and the fact that the site is covered by large rocks.

  10. Geologic Setting and Soil Physical Properties of the Mars Phoenix Landing Site

    NASA Astrophysics Data System (ADS)

    Arvidson, R. E.; Mellon, M. T.

    2008-12-01

    The Phoenix Lander touched down ~30 km to the southwest (68.22 N, 234.25 E) of the Amazonian aged, 10 km wide, bowl-shaped Heimdall impact crater. The lander is sitting on ejecta deposits from the Heimdall event that were emplaced as a ground hugging, volatile rich flow, interpreted to be a consequence of impact into icy soil and bedrock. The ejecta deposits have been differentially eroded by aeolian activity and reworked by permafrost-related processes into polygonal ground. Rock abundances are low relative to most of Mars and rocks are concentrated in troughs in between polygons and tend to be evenly spaced, implying an on-going process of polygon formation. Rocks range from tabular to rounded in shape and massive to vesicular in texture. Very few aeolian features (e.g., ripples or ventifacted rock surfaces) are evident, in contrast to the other Mars landing sites. Based on analyses of Mars Reconnaissance Orbiter CRISM hyperspectral data (~0.4 to 4 micrometers) and Phoenix observations, the surface cover is dominated by basaltic soils (sandy silts) and ferric-rich dust, with only contribution from minerals formed under aqueous conditions. The soil is cloddy and adheres to spacecraft surfaces, probably because of electrostatic charging. Densely-cemented icy soil is found within a few centimeters of the surface and once exposed and allowed to warm in the sunlight the ice eventually sublimates into the atmosphere, leaving behind soil lag deposits. The Phoenix landing site is unique relative to the other five sites (two Viking Landers, Pathfinder, Spirit and Opportunity rovers) because of the high latitude, location on relatively young ejecta emplaced as a volatile-rich flow, and because the ice table depth is predicted to have varied from centimeters to as much as a meter beneath the surface during orbital shifts associated with Martian Milankovitch cycles and consequent insolation over the northern latitudes.

  11. Revegetation Study of Adobe Dam, Phoenix, Arizona. Task 4. Revision. Site Characteristics.

    DTIC Science & Technology

    1983-08-18

    r GOVT ACCESSION NO 3. RECIPIENT’S CATALOG NUMER 4. TITLE (and SubefI.) S. TYPE OF REPORT & PERIOD COVERED Phoenix Ari na...PAGE (When Dae Entored) , r " ’:i’ ’ ’l "’%wW’ l; " r1,41’ :: "::. :" ".. :" "" ’ " - r • .., . lr.:,TI of.. 10,.P . . . mo m SECURITY CLASSIFICATION OF...Arizona Department of Transportation, minning companies in the Phoeniz area, and the Desert Botarial Gardon . Task No. 4 "Site Characteristics."

  12. (Ca,Mg)-Carbonate and Mg-Carbonate at the Phoenix Landing Site: Evaluation of the Phoenix Lander's Thermal Evolved Gas Analyzer (TEGA) Data Using Laboratory Simulations

    NASA Technical Reports Server (NTRS)

    Sutter, B.; Ming, D. W.; Boynton, W. V.; Niles, P. B.; Morris, R. V.

    2011-01-01

    Calcium carbonate (4.5 wt. %) was detected in the soil at the Phoenix Landing site by the Phoenix Lander s The Thermal and Evolved Gas Analyzer [1]. TEGA operated at 12 mbar pressure, yet the detection of calcium carbonate is based on interpretations derived from thermal analysis literature of carbonates measured under ambient (1000 mbar) and vacuum (10(exp -3) mbar) conditions [2,3] as well as at 100 and 30 mbar [4,5] and one analysis at 12 mbar by the TEGA engineering qualification model (TEGA-EQM). Thermodynamics (Te = H/ S) dictate that pressure affects entropy ( S) which causes the temperature (Te) of mineral decomposition at one pressure to differ from Te obtained at another pressure. Thermal decomposition analyses of Fe-, Mg-, and Ca-bearing carbonates at 12 mbar is required to enhance the understanding of the TEGA results at TEGA operating pressures. The objectives of this work are to (1) evaluate the thermal and evolved gas behavior of a suite of Fe-, Mg-, Ca-carbonate minerals at 1000 and 12 mbar and (2) discuss possible emplacement mechanisms for the Phoenix carbonate.

  13. Martian Boundary Layer Water Ice Clouds At The Proposed NASA Phoenix Lander Site

    NASA Astrophysics Data System (ADS)

    Michelangeli, Diane; Pathak, J.

    2006-12-01

    Results from the one-dimensional University of Helsinki atmospheric boundary layer (ABL) model are applied to a one-dimensional Mars microphysics model (MMM) to study the diurnal variation of ground fogs and ice cloud formation at the proposed NASA Phoenix landing site. Phoenix is scheduled to reach Mars in 2008 and land in the northern plains (65°-72°N). A Meteorology station (MET), consisting of a pressure sensor, 3 mast-mounted temperature sensors and an upward-looking LIDAR, will enable weather and boundary layer observations. The LIDAR (Light Detection and Ranging) instrument will be capable of monitoring dust and ice clouds, including fog and dust plumes, in the Martian boundary layer. Understanding these future LIDAR observations is the motivation for the modeling studies conducted for this paper. Observations from the MGS TES for the proposed landing site and season Ls 76 125 have been used for the model initialization, both in the ABL and MMM. The diurnal variations of temperature and eddy diffusion coefficients produced by the ABL are then applied to the MMM. Sensitivity to water ice cloud simulation is studied by varying the vertical resolution of the MMM and by inclusion of surface fluxes of dust and water vapor. The results from these studies will be presented at the conference. Acknowledgements: This work is supported by the Canadian Space Agency and Natural Sciences and Engineering Research Council of Canada.

  14. Soluble sulfate in the martian soil at the Phoenix landing site

    NASA Astrophysics Data System (ADS)

    Kounaves, Samuel P.; Hecht, Michael H.; Kapit, Jason; Quinn, Richard C.; Catling, David C.; Clark, Benton C.; Ming, Douglas W.; Gospodinova, Kalina; Hredzak, Patricia; McElhoney, Kyle; Shusterman, Jennifer

    2010-05-01

    Sulfur has been detected by X-ray spectroscopy in martian soils at the Viking, Pathfinder, Opportunity and Spirit landing sites. Sulfates have been identified by OMEGA and CRISM in Valles Marineris and by the spectrometers on the MER rovers at Meridiani and Gusev. The ubiquitous presence of sulfur has been interpreted as a widely distributed sulfate mineralogy. One goal of the Wet Chemistry Laboratory (WCL) on NASA's Phoenix Mars Lander was to determine soluble sulfate in the martian soil. We report here the first in-situ measurement of soluble sulfate equivalent to ˜1.3(±0.5) wt% as SO4 in the soil. The results and models reveal SO42- predominately as MgSO4 with some CaSO4. If the soil had been wet in the past, epsomite and gypsum would be formed from evaporation. The WCL-derived salt composition indicates that if the soil at the Phoenix site were to form an aqueous solution by natural means, the water activity for a dilution of greater than ˜0.015 g H2O/g soil would be in the habitable range of known terrestrial halophilic microbes.

  15. Ice Lens Formation and Frost Heave at the Phoenix Landing Site

    NASA Technical Reports Server (NTRS)

    Zent, A. P.; Sizemore, H. G.; Remple, A. W.

    2011-01-01

    Several lines of evidence indicate that the volume of shallow ground ice in the martian high latitudes exceeds the pore volume of the host regolith. Boynton et al. found an optimal fit to the Mars Odyssey Gamma Ray Spectrometer (GRS) data at the Phoenix landing site by modeling a buried layer of 50-75% ice by mass (up to 90% ice by volume). Thermal and optical observations of recent impact craters in the northern hemisphere have revealed nearly pure ice. Ice deposits containing only 1-2% soil by volume were excavated by Phoenix. The leading hypothesis for the origin of this excess ice is that it developed in situ by a mechanism analogous to the formation of terrestrial ice lenses and needle ice. Problematically, terrestrial soil-ice segregation is driven by freeze/thaw cycling and the movement of bulk water, neither of which are expected to have occurred in the geologically recent past on Mars. If however ice lens formation is possible at temperatures less than 273 K, there are possible implications for the habitability of Mars permafrost, since the same thin films of unfrozen water that lead to ice segregation are used by terrestrial psychrophiles to metabolize and grow down to temperatures of at least 258 K.

  16. Soil moisture detection from radar imagery of the Phoenix, Arizona test site

    NASA Technical Reports Server (NTRS)

    Cihlar, J.; Ulaby, F. T.; Mueller, R.

    1975-01-01

    The Environmental Research Institute of Michigan (ERIM) dual-polarization X and L band radar was flown to acquire radar imagery over the Phoenix (Arizona) test site. The site was covered by a north-south pass and an east-west pass. Radar response to soil moisture was investigated. Since the ERIM radar does not have accurately measured antenna patterns, analysis of the L band data was performed separately for each of several strips along the flight line, each corresponding to a narrow angle of incidence. For the NS pass, good correlation between the radar return and mositure content was observed for each of the two nearest (to nadir) angular ranges. At higher angular ranges, no correlation was observed. The above procedure was not applied to the EW pass due to flight path misalignments. The results obtained stress the importance of radar calibration, the digitization process, and the angle of incidence.

  17. Geomorphic and geologic settings of the Phoenix Lander mission landing site

    NASA Astrophysics Data System (ADS)

    Heet, T. L.; Arvidson, R. E.; Cull, S. C.; Mellon, M. T.; Seelos, K. D.

    2009-11-01

    The Phoenix Lander touched down on the northern distal flank of the shield volcano Alba Patera in a ˜150 km wide valley underlain by the Scandia region unit. The geomorphology and geology of the landing site is dominated by the ˜0.6 Ga, 11.5 km wide, bowl-shaped impact crater, Heimdal, and its areally extensive ejecta deposits. The Lander is located ˜20 km to the west of the crater and is sitting on a plains surface underlain by partially eroded Heimdal ejecta deposits. Heimdal was produced by a hypervelocity impact into fine-grained, ice-rich material and is inferred to have produced high velocity winds and a ground-hugging ejecta emplacement mode that destroyed or buried preexisting surfaces and rock fields out to ˜10 crater radii. Patterned ground is ubiquitous, with complex polygon patterns and rock rubble piles located on older plains (˜3.3 Ga) to the west of the ejecta deposits. Crater size frequency distributions are complex and represent equilibria between crater production and destruction processes (e.g., aeolian infill, cryoturbation, relaxation of icy substrate). Rock abundances increase near craters for the older plains and rocks with their dark shadows explain the reason for the few percent lower albedo for these plains as opposed to the Heimdal ejecta deposits. Many rocks at the landing site have been reworked by cryoturbation and moved to polygon troughs. The evidence for cryoturbation and the lack of aeolian features imply that the soils sampled by Phoenix are locally derived and mixed with a subordinate amount of windblown dust.

  18. Phoenix Trenches

    NASA Technical Reports Server (NTRS)

    2008-01-01

    [figure removed for brevity, see original site] Annotated Version

    [figure removed for brevity, see original site] Left-eye view of a stereo pair [figure removed for brevity, see original site] Right-eye view of a stereo pair

    This image is a stereo, panoramic view of various trenches dug by NASA's Phoenix Mars Lander. The images that make up this panorama were taken by Phoenix's Surface Stereo Imager at about 4 p.m., local solar time at the landing site, on the 131st, Martian day, or sol, of the mission (Oct. 7, 2008).

    In figure 1, the trenches are labeled in orange and other features are labeled in blue. Figures 2 and 3 are the left- and right-eye members of a stereo pair.

    For scale, the 'Pet Donkey' trench just to the right of center is approximately 38 centimeters (15 inches) long and 31 to 34 centimeters (12 to 13 inches) wide. In addition, the rock in front of it, 'Headless,' is about 11.5 by 8.5 centimeters (4.5 by 3.3 inches), and about 5 centimeters (2 inches) tall.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  19. Phoenix Trenches

    NASA Technical Reports Server (NTRS)

    2008-01-01

    [figure removed for brevity, see original site] Annotated Version

    [figure removed for brevity, see original site] Left-eye view of a stereo pair [figure removed for brevity, see original site] Right-eye view of a stereo pair

    This image is a stereo, panoramic view of various trenches dug by NASA's Phoenix Mars Lander. The images that make up this panorama were taken by Phoenix's Surface Stereo Imager at about 4 p.m., local solar time at the landing site, on the 131st, Martian day, or sol, of the mission (Oct. 7, 2008).

    In figure 1, the trenches are labeled in orange and other features are labeled in blue. Figures 2 and 3 are the left- and right-eye members of a stereo pair.

    For scale, the 'Pet Donkey' trench just to the right of center is approximately 38 centimeters (15 inches) long and 31 to 34 centimeters (12 to 13 inches) wide. In addition, the rock in front of it, 'Headless,' is about 11.5 by 8.5 centimeters (4.5 by 3.3 inches), and about 5 centimeters (2 inches) tall.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  20. A revised Pitzer model for low-temperature soluble salt assemblages at the Phoenix site, Mars

    NASA Astrophysics Data System (ADS)

    Toner, J. D.; Catling, D. C.; Light, B.

    2015-10-01

    The Wet Chemistry Laboratory (WCL) on the Mars Phoenix Lander measured ions in a soil-water extraction and found Na+, K+, H+ (pH), Ca2+, Mg2+, SO42-, ClO4-, and Cl-. Equilibrium models offer insights into salt phases that were originally present in the Phoenix soil, which dissolved to form the measured WCL solution; however, there are few experimental datasets for single cation perchlorates (ClO4-), and none for mixed perchlorates, at low temperatures, which are needed to build models. In this study, we measure ice and salt solubilities in binary and ternary solutions in the Na-Ca-Mg-ClO4 system, and then use this data, along with existing data, to construct a low-temperature Pitzer model for perchlorate brines. We then apply our model to a nominal WCL solution. Previous studies have modeled either freezing of a WCL solution or evaporation at a single temperature. For the first time, we model evaporation at subzero temperatures, which is relevant for dehydration conditions that might occur at the Phoenix site. Our model indicates that a freezing WCL solution will form ice, KClO4, hydromagnesite (3MgCO3·Mg(OH)2·3H2O), calcite (CaCO3), meridianiite (MgSO4·11H2O), MgCl2·12H2O, NaClO4·2H2O, and Mg(ClO4)2·6H2O at the eutectic (209 K). The total water held in hydrated salt phases at the eutectic is ∼1.2 wt.%, which is much greater than hydrated water contents when evaporation is modeled at 298.15 K (∼0.3 wt.%). Evaporation of WCL solutions at lower temperatures (down to 210 K) results in lower water activities and the formation of more dehydrated minerals, e.g. kieserite (MgSO4·H2O) instead of meridianiite. Potentially habitable brines, with water activity aw > 0.6, can occur when soil temperatures are above 220 K and when the soil liquid water content is greater than 0.4 wt.% (100 ×gH2O gsoil-1). In general, modeling indicates that mineral assemblages derived from WCL-type solutions are characteristic of the soil temperature, water content, and water

  1. Ice Lens Formation and Frost Heave at the Phoenix Landing Site

    NASA Astrophysics Data System (ADS)

    Zent, A.; Sizemore, H. G.; Rempel, A. W.

    2010-12-01

    Several lines of evidence indicate that the volume of shallow ground ice in the Martian high latitudes exceeds the pore volume of the host regolith. Boynton et al. (2002) found an optimal fit to the Mars Odyssey Gamma Ray Spectrometer (GRS) data at the Phoenix landing site by modeling a buried layer of 50-75% ice by mass (up to 90% by volume). Thermal and optical observations of recent impact craters in the northern hemisphere have revealed nearly pure ice. Ice deposits containing only 1-2% soil by volume were excavated by Phoenix. The leading hypothesis for the origin of this excess, or segregated, ice is that it developed in situ by a mechanism analogous to the formation of terrestrial ice lenses and needle ice. Problematically, terrestrial soil-ice segregation is driven by freeze/thaw cycling and the movement of bulk water, which are not expected to have occurred in the geologically recent past on Mars. We have developed a numerical model that applies the physics of pre-melting to track phase partitioning in soil pore spaces and test for conditions under which ice lenses could initiate. Our results indicate that diurnal cycling in the ice-cemented regolith and resultant pressure gradients in thin films at grain-ice interfaces can cause interparticle forces to unload, initiating an ice lens at temperatures as low as 245 K. These results indicate that in situ ice segregation may have occurred on Mars in the recent past, and that geologically young ice lenses may account for much of observed excess ice.

  2. 75 FR 64708 - Reorganization of Foreign-Trade Zone 75 under Alternative Site Framework; Phoenix, AZ

    Federal Register 2010, 2011, 2012, 2013, 2014

    2010-10-20

    ...; Phoenix, AZ Pursuant to its authority under the Foreign-Trade Zones Act of June 18, 1934, as amended (19 U...; Whereas, the City of Phoenix, grantee of Foreign-Trade Zone 75, submitted an application to the Board (FTZ... Maricopa County and portions of Pinal and Yavapai Counties, Arizona, within and adjacent to the...

  3. Full-Circle Color Panorama of Phoenix Landing Site on Northern Mars

    NASA Image and Video Library

    2008-12-21

    This view combines more than 400 images taken during the first several weeks after NASA Phoenix Mars Lander arrived on an arctic plain at 68.22 degrees north latitude, 234.25 degrees east longitude on Mars.

  4. Landing Site Dispersion Analysis and Statistical Assessment for the Mars Phoenix Lander

    NASA Technical Reports Server (NTRS)

    Bonfiglio, Eugene P.; Adams, Douglas; Craig, Lynn; Spencer, David A.; Strauss, William; Seelos, Frank P.; Seelos, Kimberly D.; Arvidson, Ray; Heet, Tabatha

    2008-01-01

    The Mars Phoenix Lander launched on August 4, 2007 and successfully landed on Mars 10 months later on May 25, 2008. Landing ellipse predicts and hazard maps were key in selecting safe surface targets for Phoenix. Hazard maps were based on terrain slopes, geomorphology maps and automated rock counts of MRO's High Resolution Imaging Science Experiment (HiRISE) images. The expected landing dispersion which led to the selection of Phoenix's surface target is discussed as well as the actual landing dispersion predicts determined during operations in the weeks, days, and hours before landing. A statistical assessment of these dispersions is performed, comparing the actual landing-safety probabilities to criteria levied by the project. Also discussed are applications for this statistical analysis which were used by the Phoenix project. These include using the statistical analysis used to verify the effectiveness of a pre-planned maneuver menu and calculating the probability of future maneuvers.

  5. Physical Properties of the Icy Soil at the Phoenix Landing Site

    NASA Astrophysics Data System (ADS)

    Keller, H.; Markiewicz, W. J.; Hviid, S. F.; Goetz, W.; Mellon, M. T.; El Maarry, M.; Madsen, M. B.; Smith, P.; Pike, W.; Zent, A.; Hecht, M. H.; Ming, D.; Staufer, U.

    2008-12-01

    The geomorphological setting of the subpolar terrain at the landing site is characterized by polygonal structures. These structures are generated by long term and periodic cycles of contraction and expansion of the subsurface icy soil. The physical properties of the covering soil layer effectively control the details of this process that has its counterpart on earth in (sub) polar regions including the Siberian tundra and in Antartica. One of the prime science goals of the Phoenix mission is to investigate the physical properties of the icy soil, how these processes are influenced by water vapour diffusion in the regolith and exchange of the water vapour with the atmosphere. It is important to understand these processes on diurnal, seasonal, and climatic time scales. Phoenix landed in the middle of one of the polygons. Its retro rockets cleared the ice table of the polygon underneath the jet assemblies from ca. 5 to 10 cm of loose cloddy regolith. Soil was piled up in the centre. The fact that the soil looked still cloddy similar to that in undisturbed areas suggests strong cohesiveness of the matrix material. The clumps were not destroyed by the blast. Excavated regolith material imaged in the scoop was made up of agglomerates of grains smaller than the best resolution of the Robotic Arm Camera (20 micron). Higher resolution images (4 micron) of the microscope corroborate that the soil is predominantly composed of agglomerates of very small particles with a mean size comparable to those observed in the Martian atmosphere. The Atomic Force Microscope reveals micron sized particles and smaller, partly of plate-like shape, indicating clay like particles. The matrix material of the soil is of reddish colour probably due to iron oxideadmixture. Only about 10% by volume of the soil are most often rounded grains between 40 to 100 micrometers of diameter. Some are glassy resembling micro tektites, and most of these are magnetic. The cohesiveness of the clumps and clods of

  6. Atmospheric dynamics at the Phoenix landing site as seen by the Surface Stereo Imager

    NASA Astrophysics Data System (ADS)

    Moores, John E.; Lemmon, Mark T.; Smith, Peter H.; Komguem, Leonce; Whiteway, James A.

    2010-01-01

    The Surface Stereo Imager has made observations of dust blowing aloft and clouds near the horizon at the Phoenix landing site. These subtle features are apparent because of the high signal-to-noise ratio of the camera which allows for the removal of a mean frame from multiple images captured in rapid succession and the ability to conduct simultaneous capture through different filters in each camera eye. By examining the ratios between two filters, it was possible to determine in a relative sense how the water ice content of the atmosphere changed over the mission and on a diurnal time scale. The direction of travel and speed of features aloft near the zenith has been inferred and agree well with the diurnal pattern of near-surface wind direction from the Telltale. Direct observation of cumulus-like cloud near the surface suggests convection of water vapor-rich air, but only until midday, requiring a mechanism to inhibit cloud formation in the early afternoon. The spectral ratios agree well with the observation of cloud and indicate a general increase in water ice toward the end of the mission as well as a strong diurnal pattern. However, even in periods of high water ice content, there is still a great deal of variability and days when dense clouds are absent. Also, different cloud layers are occasionally observed moving in different directions, indicating occasional wind shear aloft. Features observed had estimated minimum optical depths up to 0.11.

  7. An Historical Search for Unfrozen Water at the Phoenix Landing Site

    NASA Technical Reports Server (NTRS)

    Zent, Aaron

    2004-01-01

    The goal of this work is to explore the history of the high-latitude subsurface in the latitude range of the Phoenix landing site (65-75 deg. N). The approach is to use time-marching climate models to search for times, locations, and depths where thick films of unfrozen water might periodically occur. Thick films of unfrozen water (as distinct from ubiquitous monolayer water) are interesting for two reasons. First, multi-layer films of water may be bio-available. Second, patterned ground may require the occurrence of thick films of unfrozen water to facilitate the migration of particles and the development of excess pore ice, as reported by the Odyssey Gamma Ray Spectrometer (GRS) results. For the purposes of this work, we define conditions adequate to establish thick films of unfrozen water to be T greater than 268 K, and RH greater than 0.5. We start with the need to understand the atmospheric pressure. Because of the fact that we're looking at high latitudes, the seasonal cap buffers surface temperature for some part of the year. That directly affects the subsurface thermal regime, at least in the uppermost meter where we will be

  8. An Historical Search for Unfrozen Water at the Phoenix Landing Site

    NASA Technical Reports Server (NTRS)

    Zent, Aaron

    2004-01-01

    The goal of this work is to explore the history of the high-latitude subsurface in the latitude range of the Phoenix landing site (65-75 deg. N). The approach is to use time-marching climate models to search for times, locations, and depths where thick films of unfrozen water might periodically occur. Thick films of unfrozen water (as distinct from ubiquitous monolayer water) are interesting for two reasons. First, multi-layer films of water may be bio-available. Second, patterned ground may require the occurrence of thick films of unfrozen water to facilitate the migration of particles and the development of excess pore ice, as reported by the Odyssey Gamma Ray Spectrometer (GRS) results. For the purposes of this work, we define conditions adequate to establish thick films of unfrozen water to be T greater than 268 K, and RH greater than 0.5. We start with the need to understand the atmospheric pressure. Because of the fact that we're looking at high latitudes, the seasonal cap buffers surface temperature for some part of the year. That directly affects the subsurface thermal regime, at least in the uppermost meter where we will be

  9. Full-Circle Color Panorama of Phoenix Landing Site on Northern Mars, Vertical Projection

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This view combines more than 400 images taken during the first several weeks after NASA's Phoenix Mars Lander arrived on an arctic plain at 68.22 degrees north latitude, 234.25 degrees east longitude on Mars.

    The full-circle panorama in approximately true color shows the polygonal patterning of ground in the landing area, similar to patterns in permafrost areas on Earth. North is toward the top. Trenches where Phoenix's robotic arm has been exposing subsurface material are visible just north of the lander.

    This view comprises more than 100 different camera pointings, with images taken through three different filters at each pointing. It is presented here as a vertical projection.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  10. Phoenix rising

    SciTech Connect

    Buchsbaum, L.

    2008-08-15

    Phoenix Coal currently operates 3 surface coal mines in Western Kentucky and have recently obtained the permits to construct their first underground mine. The expansion of the Phoenix Coal company since its formation in July 2004 is described. 4 photos.

  11. The Aqueous Chemistry of the Soils at the Phoenix Landing Site

    NASA Astrophysics Data System (ADS)

    Kounaves, S. P.; Hecht, M. H.; Quinn, R.; West, S. J.; Young, S. M.; Clark, B. C.; Ming, D. W.; Boynton, W. V.; Gospodinova, K.; Kapit, J.; Deflores, L. P.; Smith, P. H.; Team, A

    2008-12-01

    The MECA Wet Chemistry Laboratory (WCL) analyses on the Phoenix Mars Lander have provided the first direct evidence of the soluble ionic components of the Martian soil. The analyses were performed on samples acquired from the surface (Rosy Red) and at the soil/ice interface approximately 4-5 cm under the surface (Sorceress). Even though the samples are from a rather unique site because of the high polar latitude and the polygon-patterned ground, they present a picture of a geochemical environment different from some previously hypothesized. Addition of 25mL of a water/calibrant solution to approximately 1cc of each of the soil samples resulted in the detection of a variety of ionic species, increased solution conductivity, and a slightly alkaline pH. The major constituent cations identified and quantified to date include Na+, K+, Mg2+, and Ca2+, while the anions included Cl- and ClO4-. Sulfate analysis was performed using a Ba2+ titration method. Even though carbonate and bicarbonate were not directly measured, their presence and quantification is supported by the alkaline pH of the solution, its buffering capacity after the addition of an acid, common ion effects, conductivity, and the modeled equilibrium species distribution of the system. The species distribution resulting from the modeling and consideration of additional interactions; dissolution, precipitation, ion exchange, ads/desorption, charge balance, the behavior over the several hours of monitoring, provided constraints for carbonate speciation and concentration and was used to formulate and test soil simulants. Results from the Thermal and Evolved Gas Analyzer (TEGA) also support the presence of a significant amount of calcite in the soil.

  12. Atmospheric Dynamics at the Phoenix Landing site as seen by the Surface Stereo Imager

    NASA Astrophysics Data System (ADS)

    Moores, J.; Lemmon, M.; Smith, P.

    2008-12-01

    The Surface Stereo Imager has been used to observe the sky at the Phoenix Landing Site in Green Valley, Mars over the course of the primary and extended mission. Over this time period blowing dust aloft and clouds near the horizon have been observed. These subtle features are apparent due to the high signal to noise ratio of the camera which allows for the removal of a mean frame from multiple images captured in rapid succession and the ability to conduct simultaneous capture through different filters in each camera eye. The velocity of the features observed near the zenith is not directly inferred by this method due to a lack of information about the height of the features (other then that they are far beyond the camera cross-over point). However, the direction can typically be extracted, except in cases where features do not track from frame to frame due to high winds aloft. This direction varies mainly by time of day and is consistent with the near surface winds as measured by the Wind Telltale, located on the meteorological mast. As for the horizon data set, features remain subtle until trains of cloud-like features become visible between sols 65 and 75 and remain a daily feature. However, these are not the only features revealed as structure within the blowing dust is visible in nearly all data sets processed to date. Examples of both types of features will be presented and discussed. In addition to these data sets aloft, the rate of accumulation of air-fall dust over the course of the mission can also be determined based on observations of the Wind Telltale mirror. To date, nearly 3000 observations of this reflective surface have been taken in many lighting conditions throughout the day, as well as in shadow. These show varying degrees of dust and frost accumulation. As such, we will report on a high-temporal resolution data set derived from photometric calculations of the mirror.

  13. Geomorphology of the 2007 Phoenix Mission Landing Sites in the Northern Plains of Mars

    NASA Astrophysics Data System (ADS)

    Seelos, K. D.; Arvidson, R. E.; Golombek, M.; Parker, T.; Tamppari, L.; Smith, P.

    2005-12-01

    In 2008, the Phoenix lander will touch down in the northern plains of Mars to sample and characterize near surface and underlying ice-rich soils, gather meteorological data, and provide insight into the evolution of the surrounding landscape. Three regions from 65 to 72 N and (A) 250-270E, (B) 120-140E, and (C) 65-85E that meet both engineering and scientific constraints were chosen for concentrated acquisition of remote data to support landing site selection. Smaller areas (150x75 km) within these regions devoid of large craters or other hazards were selected as potential landing sites; center coordinates for these targeted areas are (A) 68N, 260E, (B) 67.5N, 130E, and (C) 70N, 80E. MOLA topographic data along with MOC imagery and THEMIS 36m/pixel visible, 18m/pixel visible, and ~100m/pixel infrared data are utilized to produce geomorphologic maps at 36m/pixel for the larger regions and 18m/pixel for the targeted sites. All regions are dominated by intercrater plains units, with the plains in regions B and C comprised of slightly elevated, multiple kilometer-scale polygonal blocks surrounded or infilled by finer-grained material. The plains unit of region A lacks large polygons, instead exhibiting a smooth to mottled appearance. Patterned ground is ubiquitous throughout all regions. The characteristic dimpled texture of "basketball" terrain is most common, being superposed on the large polygons in regions B and C, and often organized into stripes with orientations partially controlled by local slopes. Small-scale polygonal ground is also observed usually in association with crater ejecta. Craters throughout all regions appear highly degraded, with most small craters (< 1km) remarkably worn with little or no rim definition and ejecta present only as a faint dark halo. Larger craters frequently exhibit pedestal-style ejecta. The style and state of landform degradation and the consistent presence of patterned ground throughout all regions suggests the long

  14. An Historical Search for Unfrozen Water at the Phoenix Landing Site

    NASA Astrophysics Data System (ADS)

    Zent, A. P.

    2004-11-01

    The 2007 Phoenix mission will land near 70 N latitude, and excavate the regolith to sample ground ice. Chemical analyses will search for dissolved species, chemical sediments, and organic compounds that may indicate the chemical and environmental history of the ground ice. Mars periodically experiences high obliquities, leading to warming of the polar latitudes. This raises the possibility that thin films of unfrozen water could serve as habitats for microbial communities in a manner analogous to terrestrial permafrost communities. However, Phoenix can only access the uppermost millimeters of the ground ice. We model the likely history of the ground ice that Phoenix will access. The model tracks surface energy balance, including cap latent heat. The upper boundary condition is the annual average H2O vapor density, which is a sensitive function of H2O ice albedo and conductivity, as well as the albedo, emissivity, and thermal conductivity of the seasonal CO2 cap. Relatively small variations in these properties can introduce considerable uncertainties in the actual depth of the ground ice. We bracket these uncertainties by assuming either that: a) the annual average H2O vapor density is invariant with time, or b) the annual average H2O vapor density is proportional to the column abundance determined by radiative balance. For most thermophysical properties, the model predicts that ground ice has become more shallow over the past 25 ka, corresponding with migration of perihelion from northern summer to northern winter. The ice Phoenix will access has probably been recently deposited from the atmosphere, and has not experienced heating at high obliquities. Therefore, it is unlikely to have constituted a viable habitat. Nonetheless, Phoenix may encounter materials relict of earlier periods of high obliquity when thin unfrozen films were possible.

  15. Full-Circle Color Panorama of Phoenix Landing Site on Northern Mars, Polar Projection

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This view combines more than 400 images taken during the first several weeks after NASA's Phoenix Mars Lander arrived on an arctic plain at 68.22 degrees north latitude, 234.25 degrees east longitude on Mars.

    The full-circle panorama in approximately true color shows the polygonal patterning of ground at the landing area, similar to patterns in permafrost areas on Earth. South is toward the top. Trenches where Phoenix's robotic arm has been exposing subsurface material are visible in the lower half of the image. The spacecraft's meteorology mast, topped by the telltale wind gauge, extends into the sky portion of the panorama.

    This view comprises more than 100 different camera pointings, with images taken through three different filters at each pointing. It is presented here as a polar projection.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  16. Chemistry Lab for Phoenix Mars Lander

    NASA Image and Video Library

    2007-08-02

    The targeted landing site for NASA Phoenix Mars Lander is at about 68 degrees north latitude, 233 degrees east longitude in the Martian arctic. The Phoenix lander, which landed May 25, 2008 ceased its operations about six months later.

  17. Time-Dependent SSI Multispectral Properties for Rock, Soil, Ice, and Sublimation Lags at the Phoenix Landing Site on Mars

    NASA Astrophysics Data System (ADS)

    Morris, R. V.; Lemmon, M. T.; Arvidson, R. E.; Blaney, D. L.; Ellehoj, M. D.; Mellon, M. T.; Phoenix, S. T.

    2008-12-01

    The Surface Stereo Imager (SSI) on the Phoenix Lander is a 15 band multispectral imager covering the spectral range from 0.45 to 1.00 micrometers. More than 250 15-filter spectral image cubes have been obtained for surface targets at the Phoenix landing site in the north polar region of Mars. The spectra of surface soils and rocks are dominated by a ferric absorption edge from nanophase ferric oxide, and they are broadly similar to most multispectral data obtained during the Pathfinder and MER missions. Negative spectral slopes between about 0.70 and 1.00 micrometers, indicative of high concentrations of olivine in the El Dorado sand sheet at Gusev crater, were not detected. The albedo (cos(i) corrected) of Phoenix surface spectra is highly dependent on the time of sol (albedo at 0.80 micrometers varies by a factor of 2), consistent with opposition and phase function effects. Subsurface layers bearing water ice were exposed at a depth of about 4 cm by digging with the robotic arm scoop. The SSI spectra of icy materials are highly variable, ranging from typical ice (spectrally neutral and high albedo near 0.7) at the Dodo-Goldilocks trench to low albedo spectra (about 0.3 at 0.80 micrometers) with a ferric absorption edge at the Snow White trench. The differences are attributed, respectively, to low and high concentrations of fine-grained and ferric-rich material dispersed throughout the ice. The spectra of the icy surfaces are dependent on time as the ice sublimes. At Snow White, an optically thick (about 300 micrometers) sublimate lag develops within two sols. At Dodo- Goldilocks, the time scale for development of an optically thick sublimate lag is 5 to greater than 60 sols, depending on location within the trench. The spectra of sublimate lag are equivalent to those for fine-grained soil.

  18. A prelanding assessment of the ice table depth and ground ice characteristics in Martian permafrost at the Phoenix landing site

    NASA Astrophysics Data System (ADS)

    Mellon, Michael T.; Boynton, William V.; Feldman, William C.; Arvidson, Raymond E.; Titus, Timothy N.; Bandfield, Joshua L.; Putzig, Nathaniel E.; Sizemore, Hanna G.

    2008-11-01

    We review multiple estimates of the ice table depth at potential Phoenix landing sites and consider the possible state and distribution of subsurface ice. A two-layer model of ice-rich material overlain by ice-free material is consistent with both the observational and theoretical lines of evidence. Results indicate ground ice to be shallow and ubiquitous, 2-6 cm below the surface. Undulations in the ice table depth are expected because of the thermodynamic effects of rocks, slopes, and soil variations on the scale of the Phoenix Lander and within the digging area, which can be advantageous for analysis of both dry surficial soils and buried ice-rich materials. The ground ice at the ice table to be sampled by the Phoenix Lander is expected to be geologically young because of recent climate oscillations. However, estimates of the ratio of soil to ice in the ice-rich subsurface layer suggest that that the ice content exceeds the available pore space, which is difficult to reconcile with existing ground ice stability and dynamics models. These high concentrations of ice may be the result of either the burial of surface snow during times of higher obliquity, initially high-porosity soils, or the migration of water along thin films. Measurement of the D/H ratio within the ice at the ice table and of the soil-to-ice ratio, as well as imaging ice-soil textures, will help determine if the ice is indeed young and if the models of the effects of climate change on the ground ice are reasonable.

  19. A prelanding assessment of the ice table depth and ground ice characteristics in Martian permafrost at the Phoenix landing site

    USGS Publications Warehouse

    Mellon, M.T.; Boynton, W.V.; Feldman, W.C.; Arvidson, R. E.; Titus, Joshua T.N.; Bandfield, L.; Putzig, N.E.; Sizemore, H.G.

    2009-01-01

    We review multiple estimates of the ice table depth at potential Phoenix landing sites and consider the possible state and distribution of subsurface ice. A two-layer model of ice-rich material overlain by ice-free material is consistent with both the observational and theoretical lines of evidence. Results indicate ground ice to be shallow and ubiquitous, 2-6 cm below the surface. Undulations in the ice table depth are expected because of the thermodynamic effects of rocks, slopes, and soil variations on the scale of the Phoenix Lander and within the digging area, which can be advantageous for analysis of both dry surficial soils and buried ice-rich materials. The ground ice at the ice table to be sampled by the Phoenix Lander is expected to be geologically young because of recent climate oscillations. However, estimates of the ratio of soil to ice in the ice-rich subsurface layer suggest that that the ice content exceeds the available pore space, which is difficult to reconcile with existing ground ice stability and dynamics models. These high concentrations of ice may be the result of either the burial of surface snow during times of higher obliquity, initially high-porosity soils, or the migration of water along thin films. Measurement of the D/H ratio within the ice at the ice table and of the soil-to-ice ratio, as well as imaging ice-soil textures, will help determine if the ice is indeed young and if the models of the effects of climate change on the ground ice are reasonable. Copyright 2008 by the American Geophysical Union.

  20. Introduction to special section on the Phoenix Mission: Landing Site Characterization Experiments, Mission Overviews, and Expected Science

    NASA Astrophysics Data System (ADS)

    Smith, P. H.; Tamppari, L.; Arvidson, R. E.; Bass, D.; Blaney, D.; Boynton, W.; Carswell, A.; Catling, D.; Clark, B.; Duck, T.; DeJong, E.; Fisher, D.; Goetz, W.; Gunnlaugsson, P.; Hecht, M.; Hipkin, V.; Hoffman, J.; Hviid, S.; Keller, H.; Kounaves, S.; Lange, C. F.; Lemmon, M.; Madsen, M.; Malin, M.; Markiewicz, W.; Marshall, J.; McKay, C.; Mellon, M.; Michelangeli, D.; Ming, D.; Morris, R.; Renno, N.; Pike, W. T.; Staufer, U.; Stoker, C.; Taylor, P.; Whiteway, J.; Young, S.; Zent, A.

    2008-10-01

    Phoenix, the first Mars Scout mission, capitalizes on the large NASA investments in the Mars Polar Lander and the Mars Surveyor 2001 missions. On 4 August 2007, Phoenix was launched to Mars from Cape Canaveral, Florida, on a Delta 2 launch vehicle. The heritage derived from the canceled 2001 lander with a science payload inherited from MPL and 2001 instruments gives significant advantages. To manage, build, and test the spacecraft and its instruments, a partnership has been forged between the Jet Propulsion Laboratory, the University of Arizona (home institution of principal investigator P. H. Smith), and Lockheed Martin in Denver; instrument and scientific contributions from Canada and Europe have augmented the mission. The science mission focuses on providing the ground truth for the 2002 Odyssey discovery of massive ice deposits hidden under surface soils in the circumpolar regions. The science objectives, the instrument suite, and the measurements needed to meet the objectives are briefly described here with reference made to more complete instrument papers included in this special section. The choice of a landing site in the vicinity of 68°N and 233°E balances scientific value and landing safety. Phoenix will land on 25 May 2008 during a complex entry, descent, and landing sequence using pulsed thrusters as the final braking strategy. After a safe landing, twin fan-like solar panels are unfurled and provide the energy needed for the mission. Throughout the 90-sol primary mission, activities are planned on a tactical basis by the science team; their requests are passed to an uplink team of sequencing engineers for translation to spacecraft commands. Commands are transmitted each Martian morning through the Deep Space Network by way of a Mars orbiter to the spacecraft. Data are returned at the end of the Martian day by the same path. Satisfying the mission's goals requires digging and providing samples of interesting layers to three on-deck instruments. By

  1. Possible Segregated Ice at the Phoenix Landing Site: Was Liquid Water Involved?

    NASA Astrophysics Data System (ADS)

    Stoker, C.; Blaney, D.; Hecht, M.; Catling, D.; Pike, W. T.; Mellon, M.; Kounaves, S.; Lemmon, M.

    2008-12-01

    Lander cameras on the Phoenix mission revealed polygonal terrain at the landing site. Areas identified by topography within the work area of the arm included a polygon and a surrounding trough. Two trenches were dug, the first (Goldilocks) on the shoulder of a trough area exposed a bright, hard material and the second (Snow white) in the center of the polygon exposed hard material, but with multispectral properties indistinguishable from soil. Visibile-NIR spectra of the Goldilocks bright material are consistent with slightly dusty ice. When first exposed, a 2 cm chunk of material broke off and was observed to completely disappear in 3 sols, an implied sublmation rate of 100 micrometers per hour. We hypothesize that the Goldilocks bright material is segregated ice. The material is hard, localized, has distinct edges, and was initially covered with only 3 cm of soil, thus was 2cm shallower than the hard layer in the Snow white trench in spite of a more south-facing exposure. A trench dug 40 cm further south of Goldilocks, with similar orientation, reached 18 cm depth without encountering hard material. Plausible mechanisms for emplacement of segregated ice include liquid water pooled into a thermally-produced crack analogous to terrestrial ice wedge polygon formation, snowparticles depositing preferentially in the troughs, and vapor deposition preferentially into cracks (D. Fisher, Icarus 179, 387, 2005). Mission observations were performed relevant to evaluating these formation mechanisms. Wet chemistry analyses of soils suggest they contain Mg(ClO4)2, a soluble hygroscopic salt with a eutectic freezing point of /- 68C. If liquid water moved though the soil and formed the bright deposit in Goldilocks trench, a higher concentration of perchlorate would be expected in the area of the ice. Mg(ClO4)2. 6 H2O would crystallize when the salty water froze, forming white rhombohedral crystals. After scraping away the surface soil, approximately 500 cm2of bright material was

  2. Thermal and Evolved Gas Analysis of Magnesium Perchlorate: Implications for Perchlorates in Soils at the Mars Phoenix Landing Site

    NASA Technical Reports Server (NTRS)

    Ming, Douglas W.; Morris, R.V.; Lauer, H. V.; Sutter, B.; Golden, D.C.; Boynton, W.V.

    2009-01-01

    Perchlorate salts were discovered in the soils around the Phoenix landing site on the northern plains of Mars [1]. Perchlorate was detected by an ion selective electrode that is part of the MECA Wet Chemistry Laboratory (WCL). The discovery of a mass 32 fragment (likely 02) by the Thermal and Evolved-Gas Analyzer (TEGA) provided additional confirmation of a strong oxidizer in the soils around the landing site. The purpose of this paper is to evaluate the thermal and evolved gas behavior of perchlorate salts using TEGA-like laboratory testbed instruments. TEGA ovens were fabricated from high purity Ni. Hence, an additional objective of this paper is to determine the effects that Ni might have on the evolved gas behavior of perchlorate salts.

  3. Phoenix's Position on Mars

    NASA Technical Reports Server (NTRS)

    2008-01-01

    [figure removed for brevity, see original site] Click on the image for the animation

    This animation shows an orbital view sweeping upward from Olympus Mons, the tallest volcano in the solar system, to the location of NASA's Phoenix Mars Lander in the northern polar reaches of Mars. The animation then zooms in on the flat terrain where Phoenix touched down May 25, 2008.

    Phoenix eased down to the surface of Mars at approximately 68 degrees north latitude, 234 degrees east longitude, landing in the center of the red circle at the end of the animation. Before Phoenix landed, engineers had predicted it would land within the blue ellipse.

    Phoenix touched down on the Red Planet at 4:53 p.m. Pacific Time (7:53 p.m. Eastern Time), May 25, 2008, in an arctic region called Vastitas Borealis.

    The shaded relief map is based on data from the Mars Orbiter Laser Altimeter on NASA's Mars Global Surveyor orbiter.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  4. Detection of perchlorate and the soluble chemistry of martian soil at the Phoenix lander site.

    PubMed

    Hecht, M H; Kounaves, S P; Quinn, R C; West, S J; Young, S M M; Ming, D W; Catling, D C; Clark, B C; Boynton, W V; Hoffman, J; Deflores, L P; Gospodinova, K; Kapit, J; Smith, P H

    2009-07-03

    The Wet Chemistry Laboratory on the Phoenix Mars Lander performed aqueous chemical analyses of martian soil from the polygon-patterned northern plains of the Vastitas Borealis. The solutions contained approximately 10 mM of dissolved salts with 0.4 to 0.6% perchlorate (ClO4) by mass leached from each sample. The remaining anions included small concentrations of chloride, bicarbonate, and possibly sulfate. Cations were dominated by Mg2+ and Na+, with small contributions from K+ and Ca2+. A moderately alkaline pH of 7.7 +/- 0.5 was measured, consistent with a carbonate-buffered solution. Samples analyzed from the surface and the excavated boundary of the approximately 5-centimeter-deep ice table showed no significant difference in soluble chemistry.

  5. Confirmation of Soluble Sulfate at the Phoenix Landing Site: Implications for Martian Geochemistry and Habitability

    NASA Technical Reports Server (NTRS)

    Kounaves, S. P.; Hecht, M. H.; Kapit, J.; Quinn, R. C.; Catling, D. C.; Clark, B. C.; Ming, D. W.; Gospodinova, K.; Hredzak, P.; McElhoney, K.; hide

    2010-01-01

    Over the past several decades, elemental sulfur in martian soils and rocks has been detected by a number of missions using X-ray spectroscopy [1-3]. Optical spectroscopy has also provided evidence for widespread sulfates on Mars [4,5]. The ubiquitous presence of sulfur in soils has been interpreted as a widely distributed sulfate mineralogy [6]. However, direct confirmation as to the identity and solubility of the sulfur species in martian soil has never been obtained. One goal of the Wet Chemistry Laboratory (WCL) [7] on board the 2007 Phoenix Mars Lander [8] was to determine soluble sulfate in the martian soil. The WCL received three primary samples. Each sample was added to 25 mL of leaching solution and analysed for solvated ionic species, pH, and conductivity [9,10]. The analysis also showed a discrepancy between charge balance, ionic strength, and conductivity, suggesting unidentified anionic species.

  6. Modeling water ice clouds on Mars at the proposed Phoenix Lander site using a one-dimensional aerosol model.

    NASA Astrophysics Data System (ADS)

    Pathak, J.; Michelangeli, D. V.; Tamppari, L. K.

    2004-11-01

    The Phoenix lander which will land on Mars in 2008 and be there from about Ls=76-140 as a NASA Scout mission will carry a MDRobotics/Optech lidar system supported by the Canadian Space Agency, to investigate various aspects of the atmosphere at the landing site. Clouds are an important element of the Martian climate system because of their ability to redistribute water vapor [Michelangeli et al., 1993; Clancy et al., 1996], and their impact on the radiation field. Since the condensation of ice particles is occurring most likely on suspended dust within the atmosphere, cloud formation will also modify the amount and location of dust in the Martian atmosphere, thus having an impact on radiation and dynamics. In order to effectively model clouds and dust in the Martian environment, we have modified the Community Aerosol and Radiation Model for Atmospheres (CARMA, developed by NASA/Ames Research Center) which is capable of simulating microphysics, transport and radiation. The one dimensional model results simulated at the proposed Phoenix lander site will be compared with the MGS TES cloud and dust opacity results. Acknowledgements. This work is supported by the Canadian Space Agency and Natural Sciences and Engineering Council of Canada. References: Clancy,R.T., A.W.Grossman, M.J. Wolff, P.B. James, D.J.Ruddy, Y.N. Billawala, B.J. Sandor, S.W. Lee and D.O. Muhleman, Water vapor saturation at low altitudes around Mars aphelion: A key to Mars climate?, Icarus, 122, 36-62, 1996. Michelangeli, D.V., O.B. Toon, R.M. Haberle, and J.B. Pollack, Numerical simulation of the formation and evolution of water ice clouds in the Martian atmosphere, Icarus, 100, 261 -285, 1993.

  7. Phoenix Lander on Mars

    NASA Technical Reports Server (NTRS)

    2007-01-01

    NASA's Phoenix Mars Lander monitors the atmosphere overhead and reaches out to the soil below in this artist's depiction of the spacecraft fully deployed on the surface of Mars.

    Phoenix has been assembled and tested for launch in August 2007 from Cape Canaveral Air Force Station, Fla., and for landing in May or June 2008 on an arctic plain of far-northern Mars. The mission responds to evidence returned from NASA's Mars Odyssey orbiter in 2002 indicating that most high-latitude areas on Mars have frozen water mixed with soil within arm's reach of the surface.

    Phoenix will use a robotic arm to dig down to the expected icy layer. It will analyze scooped-up samples of the soil and ice for factors that will help scientists evaluate whether the subsurface environment at the site ever was, or may still be, a favorable habitat for microbial life. The instruments on Phoenix will also gather information to advance understanding about the history of the water in the icy layer. A weather station on the lander will conduct the first study Martian arctic weather from ground level.

    The vertical green line in this illustration shows how the weather station on Phoenix will use a laser beam from a lidar instrument to monitor dust and clouds in the atmosphere. The dark 'wings' to either side of the lander's main body are solar panels for providing electric power.

    The Phoenix mission is led by Principal Investigator Peter H. Smith of the University of Arizona, Tucson, with project management at NASA's Jet Propulsion Laboratory and development partnership with Lockheed Martin Space Systems, Denver. International contributions for Phoenix are provided by the Canadian Space Agency, the University of Neuchatel (Switzerland), the University of Copenhagen (Denmark), the Max Planck Institute (Germany) and the Finnish Meteorological institute. JPL is a division of the California Institute of Technology in Pasadena.

  8. Phoenix Lander on Mars

    NASA Technical Reports Server (NTRS)

    2007-01-01

    NASA's Phoenix Mars Lander monitors the atmosphere overhead and reaches out to the soil below in this artist's depiction of the spacecraft fully deployed on the surface of Mars.

    Phoenix has been assembled and tested for launch in August 2007 from Cape Canaveral Air Force Station, Fla., and for landing in May or June 2008 on an arctic plain of far-northern Mars. The mission responds to evidence returned from NASA's Mars Odyssey orbiter in 2002 indicating that most high-latitude areas on Mars have frozen water mixed with soil within arm's reach of the surface.

    Phoenix will use a robotic arm to dig down to the expected icy layer. It will analyze scooped-up samples of the soil and ice for factors that will help scientists evaluate whether the subsurface environment at the site ever was, or may still be, a favorable habitat for microbial life. The instruments on Phoenix will also gather information to advance understanding about the history of the water in the icy layer. A weather station on the lander will conduct the first study Martian arctic weather from ground level.

    The vertical green line in this illustration shows how the weather station on Phoenix will use a laser beam from a lidar instrument to monitor dust and clouds in the atmosphere. The dark 'wings' to either side of the lander's main body are solar panels for providing electric power.

    The Phoenix mission is led by Principal Investigator Peter H. Smith of the University of Arizona, Tucson, with project management at NASA's Jet Propulsion Laboratory and development partnership with Lockheed Martin Space Systems, Denver. International contributions for Phoenix are provided by the Canadian Space Agency, the University of Neuchatel (Switzerland), the University of Copenhagen (Denmark), the Max Planck Institute (Germany) and the Finnish Meteorological institute. JPL is a division of the California Institute of Technology in Pasadena.

  9. The effect of cangrelor and access site on ischaemic and bleeding events: insights from CHAMPION PHOENIX.

    PubMed

    Gutierrez, J Antonio; Harrington, Robert A; Blankenship, James C; Stone, Gregg W; Steg, Ph Gabriel; Gibson, C Michael; Hamm, Christian W; Price, Matthew J; Généreux, Philippe; Prats, Jayne; Deliargyris, Efthymios N; Mahaffey, Kenneth W; White, Harvey D; Bhatt, Deepak L

    2016-04-07

    To assess whether the use of the femoral or radial approach for percutaneous coronary intervention (PCI) interacted with the efficacy and safety of cangrelor, an intravenous P2Y12 inhibitor, in CHAMPION PHOENIX. A total of 11 145 patients were randomly assigned in a double-dummy, double-blind manner either to a cangrelor bolus and 2-h infusion or to clopidogrel at the time of PCI. The primary endpoint, a composite of death, myocardial infarction, ischaemia-driven revascularization, or stent thrombosis, and the primary safety endpoint, Global Use of Strategies to Open Occluded Coronary Arteries (GUSTO) defined severe bleeding, were evaluated at 48 h. Of the patients undergoing PCI and receiving study drug treatment, a total of 8064 (74%) and 2855 (26%) patients underwent femoral or radial PCI, respectively. Among the femoral cohort, the primary endpoint rate was 4.8% with cangrelor vs. 6.0% with clopidogrel (odds ratio, OR [95% confidence interval, CI] = 0.79 [0.65-0.96]); among the radial cohort, the primary endpoint was 4.4% with cangrelor vs. 5.7% with clopidogrel (OR [95% CI] = 0.76 [0.54-1.06]), P-interaction 0.83. The rate of GUSTO severe bleeding in the femoral cohort was 0.2% with cangrelor vs. 0.1% with clopidogrel (OR [95% CI] = 1.73 [0.51-5.93]). Among the radial cohort, the rate of GUSTO severe bleeding was 0.1% with cangrelor vs. 0.1% with clopidogrel (OR [95% CI] = 1.02 [0.14-7.28]), P-interaction 0.65. The evaluation of safety endpoints with the more sensitive ACUITY-defined bleeding found major bleeding in the femoral cohort to be 5.2% with cangrelor vs. 3.1% with clopidogrel (OR [95% CI] = 1.69 [1.35-2.12]); among the radial cohort the rate of ACUITY major bleeding was 1.5% with cangrelor vs. 0.7% with clopidogrel (OR [95% CI] = 2.17 [1.02-4.62], P-interaction 0.54). In CHAMPION PHOENIX, cangrelor reduced ischaemic events with no significant increase in GUSTO-defined severe bleeding. The absolute rates of bleeding, regardless of the definition

  10. The effect of cangrelor and access site on ischaemic and bleeding events: insights from CHAMPION PHOENIX

    PubMed Central

    Gutierrez, J. Antonio; Harrington, Robert A.; Blankenship, James C.; Stone, Gregg W.; Steg, Ph. Gabriel; Gibson, C. Michael; Hamm, Christian W.; Price, Matthew J.; Généreux, Philippe; Prats, Jayne; Deliargyris, Efthymios N.; Mahaffey, Kenneth W.; White, Harvey D.; Bhatt, Deepak L.

    2016-01-01

    Aims To assess whether the use of the femoral or radial approach for percutaneous coronary intervention (PCI) interacted with the efficacy and safety of cangrelor, an intravenous P2Y12 inhibitor, in CHAMPION PHOENIX. Methods and results A total of 11 145 patients were randomly assigned in a double-dummy, double-blind manner either to a cangrelor bolus and 2-h infusion or to clopidogrel at the time of PCI. The primary endpoint, a composite of death, myocardial infarction, ischaemia-driven revascularization, or stent thrombosis, and the primary safety endpoint, Global Use of Strategies to Open Occluded Coronary Arteries (GUSTO) defined severe bleeding, were evaluated at 48 h. Of the patients undergoing PCI and receiving study drug treatment, a total of 8064 (74%) and 2855 (26%) patients underwent femoral or radial PCI, respectively. Among the femoral cohort, the primary endpoint rate was 4.8% with cangrelor vs. 6.0% with clopidogrel (odds ratio, OR [95% confidence interval, CI] = 0.79 [0.65–0.96]); among the radial cohort, the primary endpoint was 4.4% with cangrelor vs. 5.7% with clopidogrel (OR [95% CI] = 0.76 [0.54–1.06]), P-interaction 0.83. The rate of GUSTO severe bleeding in the femoral cohort was 0.2% with cangrelor vs. 0.1% with clopidogrel (OR [95% CI] = 1.73 [0.51–5.93]). Among the radial cohort, the rate of GUSTO severe bleeding was 0.1% with cangrelor vs. 0.1% with clopidogrel (OR [95% CI] = 1.02 [0.14–7.28]), P-interaction 0.65. The evaluation of safety endpoints with the more sensitive ACUITY-defined bleeding found major bleeding in the femoral cohort to be 5.2% with cangrelor vs. 3.1% with clopidogrel (OR [95% CI] = 1.69 [1.35–2.12]); among the radial cohort the rate of ACUITY major bleeding was 1.5% with cangrelor vs. 0.7% with clopidogrel (OR [95% CI] = 2.17 [1.02–4.62], P-interaction 0.54). Conclusion In CHAMPION PHOENIX, cangrelor reduced ischaemic events with no significant increase in GUSTO-defined severe bleeding. The absolute rates

  11. Airborne dust and soil particles at the Phoenix landing site, Mars

    NASA Astrophysics Data System (ADS)

    Madsen, M. B.; Drube, L.; Goetz, W.; Leer, K.; Falkenberg, T. V.; Gunnlaugsson, H. P.; Haspang, M. P.; Hviid, S. F.; Ellehøj, M. D.; Lemmon, M. T.

    2009-04-01

    The three iSweep targets on the Phoenix lander instrument deck utilize permanent magnets and 6 different background colors for studies of airborne dust [1]. The name iSweep is short for Improved Sweep Magnet experiments and derives from MER heritage [2, 3] as the rovers carried a sweep magnet, which is a very strong ring magnet built into an aluminum structure. Airborne dust is attracted and held by the magnet and the pattern formed depends on magnetic properties of the dust. The visible/near-infrared spectra acquired of the iSweep are rather similar to typical Martian dust and soil spectra. Because of the multiple background colors of the iSweeps the effect of the translucence of thin dust layers can be studied. This is used to estimate the rate of dust accumulation and will be used to evaluate light scattering properties of the particles. Some particles raised by the retro-rockets during the final descent came to rest on the lander deck and spectra of these particles are studied and compared with those of airborne dust and with spectra obtained from other missions. High resolution images acquired by the Optical Microscope (OM) [4] showed subtle differences between different Phoenix soil samples in terms of particle size and color. Most samples contain orange dust (particles smaller than 10 micrometer) as their major component and silt-sized (50-80 micrometer large) subrounded particles. Both particle types are substantially magnetic. Based on results from the Mars Exploration Rovers, the magnetization of the silt-sized particles is believed to be caused by magnetite. Morphology, texture and color of these particles (ranging from colorless, red-brown to almost black) suggest a multiple origin: The darkest particles probably represent lithic fragments, while the brighter ones could be impact or volcanic glasses. [1] Leer K. et al. (2008) JGR, 113, E00A16. [2] Madsen M.B. et al. (2003) JGR, 108, 8069. [3] Madsen M.B. et al. (2008) JGR (in print). [4] Hecht M.H. et

  12. Stable isotope measurements of martian atmospheric CO2 at the Phoenix landing site.

    PubMed

    Niles, Paul B; Boynton, William V; Hoffman, John H; Ming, Douglas W; Hamara, Dave

    2010-09-10

    Carbon dioxide is a primary component of the martian atmosphere and reacts readily with water and silicate rocks. Thus, the stable isotopic composition of CO2 can reveal much about the history of volatiles on the planet. The Mars Phoenix spacecraft measurements of carbon isotopes [referenced to the Vienna Pee Dee belemnite (VPDB)] [delta13C(VPDB) = -2.5 +/- 4.3 per mil (per thousand)] and oxygen isotopes [referenced to the Vienna standard mean ocean water (VSMOW)] (delta18O(VSMOW) = 31.0 +/- 5.7 per thousand), reported here, indicate that CO2 is heavily influenced by modern volcanic degassing and equilibration with liquid water. When combined with data from the martian meteorites, a general model can be constructed that constrains the history of water, volcanism, atmospheric evolution, and weathering on Mars. This suggests that low-temperature water-rock interaction has been dominant throughout martian history, carbonate formation is active and ongoing, and recent volcanic degassing has played a substantial role in the composition of the modern atmosphere.

  13. Stable Isotope Measurements of Martian Atmospheric CO2 at the Phoenix Landing Site

    NASA Astrophysics Data System (ADS)

    Niles, Paul B.; Boynton, William V.; Hoffman, John H.; Ming, Douglas W.; Hamara, Dave

    2010-09-01

    Carbon dioxide is a primary component of the martian atmosphere and reacts readily with water and silicate rocks. Thus, the stable isotopic composition of CO2 can reveal much about the history of volatiles on the planet. The Mars Phoenix spacecraft measurements of carbon isotopes [referenced to the Vienna Pee Dee belemnite (VPDB)] [δ13CVPDB = -2.5 ± 4.3 per mil (‰)] and oxygen isotopes [referenced to the Vienna standard mean ocean water (VSMOW)] (δ18OVSMOW = 31.0 ± 5.7‰), reported here, indicate that CO2 is heavily influenced by modern volcanic degassing and equilibration with liquid water. When combined with data from the martian meteorites, a general model can be constructed that constrains the history of water, volcanism, atmospheric evolution, and weathering on Mars. This suggests that low-temperature water-rock interaction has been dominant throughout martian history, carbonate formation is active and ongoing, and recent volcanic degassing has played a substantial role in the composition of the modern atmosphere.

  14. Observations of near-surface fog at the Phoenix Mars landing site

    NASA Astrophysics Data System (ADS)

    Moores, John E.; Komguem, Léonce; Whiteway, James A.; Lemmon, Mark T.; Dickinson, Cameron; Daerden, Frank

    2011-02-01

    The Surface Stereo Imager (SSI) on the Phoenix Mars Lander was able to complement the operations of the LIDAR on four occasions during the mission by observing the laser beam while the LIDAR laser was transmitting. These SSI observations permitted measurement of the scatter from atmospheric aerosols below 200 m where the LIDAR emitter and receiver do not overlap fully. The observed laser scattering was used to estimate the ice-water content (IWC) of near surface fog. Values of IWC up to 1.7 ± 1.0 mg m-3 were observed. Compared to air aloft, fog formation was inhibited near the surface which had accumulated at least 30 ± 24 mg m-2 (0.030 pr-μm) on sol 113. Microphysical modeling shows that when precipitation is included, up to 0.48 pr-μm of water may be present on the surface at the time of measurement. Integrated over the entire night, this represents up to 2.5 pr-μm of water taken up diurnally by the surface, or 6% of the total water column.

  15. Phoenix's Snow White Trench

    NASA Technical Reports Server (NTRS)

    2008-01-01

    A soil sample taken from the informally named 'Snow White' trench at NASA's Phoenix Mars Lander work site produced minerals that indicate evidence of past interaction between the minerals and liquid water.

    This image was taken by the Surface Stereo Imager on Sol 103, the 103rd day since landing (Sept. 8, 2008).

    The trench is approximately 23 centimeters (9 inches) long.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by JPL, Pasadena, Calif. Spacecraft development was by Lockheed Martin Space Systems, Denver.

  16. Phoenix Work Area Animation

    NASA Technical Reports Server (NTRS)

    2008-01-01

    [figure removed for brevity, see original site] Click on image for animation

    This animation from Sol 1 shows a mosaic of the Phoenix digging area in the Martian terrain. Phoenix scientists are very pleased with this view as the terrain features few rocks an optimal place for digging. The mast of the camera looks disjointed because the photos that comprise this mosaic were taken at different times of day. This video also show some of the lander's instrumentation.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  17. Phoenix Animation Looking North

    NASA Technical Reports Server (NTRS)

    2008-01-01

    [figure removed for brevity, see original site] Click on image for animation

    This animation is a series of images, taken by NASA's Phoenix Mars Lander's Surface Stereo Imager, combined into a panoramic view looking north from the lander. The area depicted is beyond the immediate workspace of the lander and shows a system of polygons and troughs that connect with the ones Phoenix will be investigating in depth.

    The images were taken on sol 14 (June 8, 2008) or the 14th Martian day after landing.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  18. Effect of evaporation and freezing on the salt paragenesis and habitability of brines at the Phoenix landing site

    NASA Astrophysics Data System (ADS)

    Elsenousy, Amira; Hanley, Jennifer; Chevrier, Vincent F.

    2015-07-01

    The WCL (Wet Chemistry Lab) instrument on board the Phoenix Lander identified the soluble ionic composition of the soil at the landing site. However, few studies have been conducted to understand the parent salts of these soluble ions. Here we studied the possible salt assemblages at the Phoenix landing site using two different thermodynamic models: FREZCHEM and Geochemist's Workbench (GWB). Two precipitation pathways were used: evaporation (T > 0 °C using both FREZCHEM and GWB) and freezing (T < 0 °C using only FREZCHEM). Through applying three different models of initial ionic concentrations (from sulfate to chlorate/perchlorate dominated), we calculated the resulting precipitated minerals. The results-through both freezing and evaporation-showed some common minerals that precipitated regardless of the ionic initial concentration. These ubiquitous minerals are magnesium chlorate hexahydrate Mg(ClO3)2ṡ6H2O, potassium perchlorate (KClO4) and gypsum (CaSO4ṡ2H2O). Other minerals evidence specific precipitation pathway. Precipitation of highly hydrated salts such as meridianiite (MgSO4ṡ11H2O) and MgCl2ṡ12H2O indicate freezing pathway, while precipitation of the low hydrated salts (anhydrite, kieserite and epsomite) indicate evaporation. The present hydration states of the precipitated hydrated minerals probably reflect the ongoing thermal processing and recent seasonally varying humidity conditions at the landing site, but these hydration states might not reflect the original depositional conditions. The simulations also showed the absence of Ca-perchlorate in all models, mainly because of the formation of two main salts: KClO4 and gypsum which are major sinks for ClO-4 and Ca2+ respectively. Finally, in consideration to the Martian life, it might survive at the very low temperatures and low water activities of the liquids formed. However, besides the big and widely recognized challenges to life posed by those extreme environmental parameters (especially low

  19. Possible Landing Ellipses for Phoenix

    NASA Image and Video Library

    2007-08-02

    Launch date makes a difference in the orientation of ellipses marking where NASA Phoenix Mars Lander would have a high probability of landing, given the planned targeting for the spring 2008 landing site.

  20. 20. This adobe building, housing the Phoenix Herald in 1879, ...

    Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

    20. This adobe building, housing the Phoenix Herald in 1879, stood on the site later occupied by the Stroud Building. The Salt River Herald, Phoenix's first newspaper, was founded in 1878; in 1879, it became the Phoenix Herald. Prior to 1879, the adobe building served as the office for a stagecoach line operating between Maricopa and Prescott via Phoenix. Credit PPL. - Stroud Building, 31-33 North Central Avenue, Phoenix, Maricopa County, AZ

  1. Combustion of Organic Molecules by the Thermal Decomposition of Perchlorate Salts: Implications for Organics at the Mars Phoenix Scout Landing Site

    NASA Technical Reports Server (NTRS)

    Ming, D.W.; Morris, R.V.; Niles, B.; Lauer, H.V.; Archer, P.D.; Sutter, B.; Boynton, W.V.; Golden, D.C.

    2009-01-01

    The Mars 2007 Phoenix Scout Mission successfully landed on May 25, 2008 and operated on the northern plains of Mars for 150 sols. The primary mission objective was to study the history of water and evaluate the potential for past and present habitability in Martian arctic ice-rich soil [1]. Phoenix landed near 68 N latitude on polygonal terrain created by ice layers that are a few centimeters under loose soil materials. The Phoenix Mission is assessing the potential for habitability by searching for organic molecules in the ice or icy soils at the landing site. Organic molecules are necessary building blocks for life, although their presence in the ice or soil does not indicate life itself. Phoenix searched for organic molecules by heating soil/ice samples in the Thermal and Evolved-Gas Analyzer (TEGA, [2]). TEGA consists of 8 differential scanning calorimeter (DSC) ovens integrated with a magnetic-sector mass spectrometer with a mass range of 2-140 daltons [2]. Endothermic and exothermic reactions are recorded by the TEGA DSC as samples are heated from ambient to 1000 C. Evolved gases, including any organic molecules and their fragments, are simultaneously measured by the mass spectrometer during heating. Phoenix TEGA data are still under analysis; however, no organic fragments have been identified to date in the evolved gas analysis (EGA). The MECA Wet Chemistry Lab (WCL) discovered a perchlorate salt in the Phoenix soils and a mass 32 peak evolved between 325 and 625 C for one surface sample dubbed Baby Bear [3]. The mass 32 peak is attributed to evolved O2 generated during the thermal decomposition of the perchlorate salt. Perchlorates are very strong oxidizers when heated, so it is possible that organic fragments evolved in the temperature range of 300-600 C were combusted by the O2 released during the thermal decomposition of the perchlorate salt. The byproduct of the combustion of organic molecules is CO2. There is a prominent release of CO2 between 200

  2. Soluble salts at the Phoenix Lander site, Mars: A reanalysis of the Wet Chemistry Laboratory data

    NASA Astrophysics Data System (ADS)

    Toner, J. D.; Catling, D. C.; Light, B.

    2014-07-01

    The Wet Chemistry Laboratory (WCL) on the Phoenix Mars Scout Lander analyzed soils for soluble ions and found Ca2+, Mg2+, Na+, K+, Cl-, SO42-, and ClO4-. The salts that gave rise to these ions can be inferred using aqueous equilibrium models; however, model predictions are sensitive to the initial solution composition. This is problematic because the WCL data is noisy and many different ion compositions are possible within error bounds. To better characterize ion concentrations, we reanalyzed WCL data using improvements to original analyses, including Kalman optimal smoothing and ion-pair corrections. Our results for Rosy Red are generally consistent with previous analyses, except that Ca2+ and Cl- concentrations are lower. In contrast, ion concentrations in Sorceress 1 and Sorceress 2 are significantly different from previous analyses. Using the more robust Rosy Red WCL analysis, we applied equilibrium models to determine salt compositions within the error bounds of the reduced data. Modeling with FREZCHEM predicts that WCL solutions evolve Ca-Mg-ClO4-rich compositions at low temperatures. These unusual compositions are likely influenced by limitations in the experimental data used to parameterize FREZCHEM. As an alternative method to evaluate salt assemblages, we employed a chemical divide model based on the eutectic temperatures of salts. Our chemical divide model predicts that the most probable salts in order of mass abundance are MgSO4·11H2O (meridianiite), MgCO3·nH2O, Mg(ClO4)2·6H2O, NaClO4·2H2O, KClO4, NaCl·2H2O (hydrohalite), and CaCO3 (calcite). If ClO3- is included in the chemical divide model, then NaClO3 precipitates instead of NaClO4·2H2O and Mg(ClO3)2·6H2O precipitates in addition to Mg(ClO4)2·6H2O. These salt assemblages imply that at least 1.3 wt.% H2O is bound in the soil, noting that we cannot account for water in hydrated insoluble salts or deliquescent brines. All WCL solutions within error bounds precipitate Mg(ClO4)2·6H2O and/or Mg

  3. Spectral Modeling of Ground Ices Exposed by Trenching at the Phoenix Mars Landing Site

    NASA Astrophysics Data System (ADS)

    Cull, S.; Arvidson, R. E.; Blaney, D.; Morris, R. V.

    2008-12-01

    The Phoenix Lander, which landed on the northern plains of Mars on 25 May 2008, used its Robotic Arm (RA) to dig six trenches during its nominal 90-sol mission: Dodo-Goldilocks, Snow White, Cupboard, Neverland, Burn Alive, and Stone Soup. During excavation of the first five of these, the RA encountered hard material interpreted to be the ice table, and the Stereo Surface Imager (SSI) imaged the exposed materials using 15 filters spanning a wavelength range from 445 to 1001 nm. Materials exposed in the Dodo- Goldilocks and Snow White trenches are spectroscopically dissimilar: Dodo-Goldilocks hard material is brighter relative to the surrounding soil, and has a distinct downturn around 800 nm resulting from a dusty ice with low soil-to-ice ratio. Snow White hard stuff varies in brightness and spectral shape depending on the phase angle, with low-phase angle images showing dark material and higher phase angles showing more soil-like material. The Snow White material does not have the strong 800-nm downturn seen in Dodo- Goldilocks, because the soil-to-ice ratio is high as inferred by the rapid development of a sublimation lag; however, the albedo variation with phase angle could be due to strong forward-scattering at low phase angles, consistent with icy material. A modified Hapke model is used to estimate the relative abundances of water ice and dust in the Dodo- Goldilocks and Snow White materials, with dehydrated palagonite as an analogue for dust . The ice exposed at Dodo-Goldilocks must be relatively dust-free, since only a small amount of dust is needed to obscure water ice absorptions. In our modeling, we find that as little as 5 wt% 20-um dust is enough to completely mask the 1001 nm absorption in 1-mm grain size water ice. Dodo-Goldilocks spectra can have up to a 20% drop in reflectance from 800 nm to 1001 nm, which is best-matched in our Hapke model by water ice with path lengths on the order of 2-3 mm. The Snow White dark materials typically have a small

  4. Phoenix's Workplace Map

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This image from NASA's Phoenix Mars Lander shows the spacecraft's recent activity site as of the 23rd Martian day of the mission, or Sol 22 (June 16, 2008), after the spacecraft touched down on the Red Planet's northern polar plains. The mosaic was taken by the lander's Surface Stereo Imager (SSI). Phoenix's solar panels are seen in the foreground.

    The trench informally called 'Snow White' was dug by Phoenix's Robotic Arm in a patch of Martian soil near the center of a polygonal surface feature, nicknamed 'Cheshire Cat.' The 'dump pile' is located at the top of the trench, and has been dubbed 'Croquet Ground.' The digging site has been nicknamed 'Wonderland.'

    Snow White, seen here in an SSI image from Sol 22 (June 16, 2008) is about 2 centimeters (.8 inches) deep and 30 centimeters (12 inches) long. As of Sol 24 (June 18, 2008), the trench is 5 centimeters (2 inches deep) and the trench has been renamed 'Snow White 1,' as a second trench has been dug to its right and nicknamed 'Snow White 2.'

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  5. Formation and Persistence of Brine on Mars: Experimental Simulations throughout the Diurnal Cycle at the Phoenix Landing Site

    NASA Astrophysics Data System (ADS)

    Fischer, E.; Martínez, G. M.; Rennó, N. O.

    2016-12-01

    In the last few years, water ice and salts capable of melting this ice and producing liquid saline water (brine) have been detected on Mars. Moreover, indirect evidence for brine has been found in multiple areas of the planet. Here, we simulate full diurnal cycles of temperature and atmospheric water vapor content at the Phoenix landing site for the first time and show experimentally that, in spite of the low Mars-like chamber temperature, brine forms minutes after the ground temperature exceeds the eutectic temperature of salts in contact with water ice. Moreover, we show that the brine stays liquid for most of the diurnal cycle when enough water ice is available to compensate for evaporation. This is predicted to occur seasonally in areas of the polar region where the temperature exceeds the eutectic value and frost or snow is deposited on saline soils, or where water ice and salts coexist in the shallow subsurface. This is important because the existence of liquid water is a key requirement for habitability.

  6. Formation and Persistence of Brine on Mars: Experimental Simulations throughout the Diurnal Cycle at the Phoenix Landing Site.

    PubMed

    Fischer, E; Martínez, G M; Rennó, N O

    2016-12-01

    In the last few years, water ice and salts capable of melting this ice and producing liquid saline water (brine) have been detected on Mars. Moreover, indirect evidence for brine has been found in multiple areas of the planet. Here, we simulate full diurnal cycles of temperature and atmospheric water vapor content at the Phoenix landing site for the first time and show experimentally that, in spite of the low Mars-like chamber temperature, brine forms minutes after the ground temperature exceeds the eutectic temperature of salts in contact with water ice. Moreover, we show that the brine stays liquid for most of the diurnal cycle when enough water ice is available to compensate for evaporation. This is predicted to occur seasonally in areas of the polar region where the temperature exceeds the eutectic value and frost or snow is deposited on saline soils, or where water ice and salts coexist in the shallow subsurface. This is important because the existence of liquid water is a key requirement for habitability. Key Words: Mars-Ice-Perchlorates-Brine-Water-Raman spectroscopy. Astrobiology 16, 937-948.

  7. Formation and Persistence of Brine on Mars: Experimental Simulations throughout the Diurnal Cycle at the Phoenix Landing Site

    PubMed Central

    Martínez, G.M.; Rennó, N.O.

    2016-01-01

    Abstract In the last few years, water ice and salts capable of melting this ice and producing liquid saline water (brine) have been detected on Mars. Moreover, indirect evidence for brine has been found in multiple areas of the planet. Here, we simulate full diurnal cycles of temperature and atmospheric water vapor content at the Phoenix landing site for the first time and show experimentally that, in spite of the low Mars-like chamber temperature, brine forms minutes after the ground temperature exceeds the eutectic temperature of salts in contact with water ice. Moreover, we show that the brine stays liquid for most of the diurnal cycle when enough water ice is available to compensate for evaporation. This is predicted to occur seasonally in areas of the polar region where the temperature exceeds the eutectic value and frost or snow is deposited on saline soils, or where water ice and salts coexist in the shallow subsurface. This is important because the existence of liquid water is a key requirement for habitability. Key Words: Mars—Ice—Perchlorates—Brine—Water—Raman spectroscopy. Astrobiology 16, 937–948. PMID:27912028

  8. Phoenix Sol 2 Northwestern Panorama

    NASA Technical Reports Server (NTRS)

    2008-01-01

    [figure removed for brevity, see original site] Click on image for animation

    This is an animation of a camera going through the Surface Stereo Imager (SSI) on the Phoenix lander. At the end of the animation is an approximate color mosaic taken by Phoenix's SSI camera. The view is toward the northwest, showing polygonal terrain near the lander and out to the horizon.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  9. Constraints on water vapor vertical distribution at the Phoenix landing site during summer from MGS TES day and night observations

    NASA Astrophysics Data System (ADS)

    Pankine, Alexey A.; Tamppari, Leslie K.

    2015-05-01

    We present a new method to retrieve column abundances and vertical extent of the water vapor from the Mars Global Surveyor (MGS) Thermal Emission Spectrometer (TES) spectra. The new method enables retrievals from the nighttime TES spectra. The retrieval algorithm employs a new model of the vertical distribution of water vapor in the martian atmosphere. In this model water vapor is confined to a layer of finite height in the lower atmosphere. The atmosphere is dry above this 'wet' layer. Within the 'wet' layer the water vapor has a constant mixing ratio below the water ice cloud condensation height and is saturated above that height. The new retrieval method simultaneously fits the daytime and nighttime TES spectra for a given location using a single mixing ratio profile. We apply this new method to the TES spectra collected over the site of the Phoenix spacecraft landing during late northern spring and summer. Retrieved daytime column abundances are ∼1-5 pr-μm higher than in the previous TES retrieval. Nighttime column abundances are lower than the daytime abundances by ∼5-10 pr-μm due to assumed exchange with soil and predicted water ice cloud formation. The height of the 'wet' layer varies with season, reaching ∼18 km around Ls = 80-100° and decreasing to 7-10 km by Ls = 140°. Changes in the vertical extent of vapor are consistent with seasonal changes in the intensity of the turbulent mixing in the lower atmosphere and in the water ice cloud condensation height. Water vapor extends by several kilometers above the top of the boundary layer at ∼4 km, suggesting that vertical transport of vapor is not limited to the boundary layer.

  10. How Phoenix Looks Under Itself

    NASA Technical Reports Server (NTRS)

    2008-01-01

    [figure removed for brevity, see original site] Click on image for animation

    This is an animation of NASA's Phoenix Mars Lander reaching with its Robotic Arm and taking a picture of the surface underneath the lander. The image at the conclusion of the animation was taken by Phoenix's Robotic Arm Camera (RAC) on the eighth Martian day of the mission, or Sol 8 (June 2, 2008). The light feature in the middle of the image below the leg is informally called 'Holy Cow.' The dust, shown in the dark foreground, has been blown off of 'Holy Cow' by Phoenix's thruster engines.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  11. How Phoenix Looks Under Itself

    NASA Technical Reports Server (NTRS)

    2008-01-01

    [figure removed for brevity, see original site] Click on image for animation

    This is an animation of NASA's Phoenix Mars Lander reaching with its Robotic Arm and taking a picture of the surface underneath the lander. The image at the conclusion of the animation was taken by Phoenix's Robotic Arm Camera (RAC) on the eighth Martian day of the mission, or Sol 8 (June 2, 2008). The light feature in the middle of the image below the leg is informally called 'Holy Cow.' The dust, shown in the dark foreground, has been blown off of 'Holy Cow' by Phoenix's thruster engines.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  12. How Phoenix Talks to Earth

    NASA Technical Reports Server (NTRS)

    2008-01-01

    [figure removed for brevity, see original site] Click on the image for the animation

    This animation shows how NASA's Phoenix Mars Lander stays in contact with Earth. As NASA's Mars Odyssey orbiter passes overhead approximately every two hours, Phoenix transmits images and scientific data from the surface to the orbiter, which then relays the data to NASA's Deep Space Network of antennas on Earth. Similarly, NASA's Deep Space Network transmits instructions from Earth to Odyssey, which then relays the information to Phoenix.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  13. Phoenix Telltale Movement

    NASA Technical Reports Server (NTRS)

    2008-01-01

    [figure removed for brevity, see original site] Click on image for animation

    This is an animation of a camera pushing through NASA's Phoenix Mars Lander's Stereo Surface Imager (SSI). At the conclusion of the animation is a set of SSI images of the telltale taken on the first, second, and third days of the mission, or sols 1, 2, and 3 (May 26, 27, and 28, 2008). The last set of images were taken one minute apart and shows the telltale moving in the wind.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  14. Microscopy analysis of soils at the Phoenix landing site, Mars: Classification of soil particles and description of their optical and magnetic properties

    NASA Astrophysics Data System (ADS)

    Goetz, W.; Pike, W. T.; Hviid, S. F.; Madsen, M. B.; Morris, R. V.; Hecht, M. H.; Staufer, U.; Leer, K.; Sykulska, H.; Hemmig, E.; Marshall, J.; Morookian, J. M.; Parrat, D.; Vijendran, S.; Bos, B. J.; El Maarry, M. R.; Keller, H. U.; Kramm, R.; Markiewicz, W. J.; Drube, L.; Blaney, D.; Arvidson, R. E.; Bell, J. F.; Reynolds, R.; Smith, P. H.; Woida, P.; Woida, R.; Tanner, R.

    2010-08-01

    The optical microscope onboard the Phoenix spacecraft has returned color images (4 μm pixel-1) of soils that were delivered to and held on various substrates. A preliminary taxonomy of Phoenix soil particles, based on color, size, and shape, identifies the following particle types [generic names in brackets]: (1) reddish fines, mostly unresolved, that are spectrally similar to (though slightly darker than) global airborne dust [red fines], (2) silt- to sand-sized brownish grains [brown sand], (3) silt- to sand-sized black grains [black sand], and (4) small amounts of whitish fines, possibly salts [white fines]. Most particles have a saturation magnetization in the range 0.5-2 Am2 kg-1 as inferred from their interaction with magnetic substrates. The particle size distribution has two distinct peaks below 10 μm (fines) and in the range 20-100 μm (grains), respectively, and is different from that of ripple soils in Gusev crater. In particular medium to large sand grains appear to be absent in Phoenix soils. Most sand grains have subrounded shape with variable texture. A fractured grain (observed on sol 112) reveals evidence of micrometer-sized crystal facets. The brown sand category displays a large diversity in color including shiny, almost colorless particles. Potential source regions for these grains may be the Tharsis volcanoes or Heimdal crater (20 km east of the landing site). The black grains are suggested to belong to a more widespread population of particles with mafic mineralogy. The absence of black/brown composite grains is consistent with different formation pathways and source regions for each grain type.

  15. Phoenix Lander on Mars (Stereo)

    NASA Technical Reports Server (NTRS)

    2007-01-01

    NASA's Phoenix Mars Lander monitors the atmosphere overhead and reaches out to the soil below in this stereo illustration of the spacecraft fully deployed on the surface of Mars. The image appears three-dimensional when viewed through red-green stereo glasses.

    Phoenix has been assembled and tested for launch in August 2007 from Cape Canaveral Air Force Station, Fla., and for landing in May or June 2008 on an arctic plain of far-northern Mars. The mission responds to evidence returned from NASA's Mars Odyssey orbiter in 2002 indicating that most high-latitude areas on Mars have frozen water mixed with soil within arm's reach of the surface.

    Phoenix will use a robotic arm to dig down to the expected icy layer. It will analyze scooped-up samples of the soil and ice for factors that will help scientists evaluate whether the subsurface environment at the site ever was, or may still be, a favorable habitat for microbial life. The instruments on Phoenix will also gather information to advance understanding about the history of the water in the icy layer. A weather station on the lander will conduct the first study Martian arctic weather from ground level.

    The vertical green line in this illustration shows how the weather station on Phoenix will use a laser beam from a lidar instrument to monitor dust and clouds in the atmosphere. The dark 'wings' to either side of the lander's main body are solar panels for providing electric power.

    The Phoenix mission is led by Principal Investigator Peter H. Smith of the University of Arizona, Tucson, with project management at NASA's Jet Propulsion Laboratory and development partnership with Lockheed Martin Space Systems, Denver. International contributions for Phoenix are provided by the Canadian Space Agency, the University of Neuchatel (Switzerland), the University of Copenhagen (Denmark), the Max Planck Institute (Germany) and the Finnish Meteorological institute. JPL is a division of the California

  16. Phoenix Lander on Mars (Stereo)

    NASA Technical Reports Server (NTRS)

    2007-01-01

    NASA's Phoenix Mars Lander monitors the atmosphere overhead and reaches out to the soil below in this stereo illustration of the spacecraft fully deployed on the surface of Mars. The image appears three-dimensional when viewed through red-green stereo glasses.

    Phoenix has been assembled and tested for launch in August 2007 from Cape Canaveral Air Force Station, Fla., and for landing in May or June 2008 on an arctic plain of far-northern Mars. The mission responds to evidence returned from NASA's Mars Odyssey orbiter in 2002 indicating that most high-latitude areas on Mars have frozen water mixed with soil within arm's reach of the surface.

    Phoenix will use a robotic arm to dig down to the expected icy layer. It will analyze scooped-up samples of the soil and ice for factors that will help scientists evaluate whether the subsurface environment at the site ever was, or may still be, a favorable habitat for microbial life. The instruments on Phoenix will also gather information to advance understanding about the history of the water in the icy layer. A weather station on the lander will conduct the first study Martian arctic weather from ground level.

    The vertical green line in this illustration shows how the weather station on Phoenix will use a laser beam from a lidar instrument to monitor dust and clouds in the atmosphere. The dark 'wings' to either side of the lander's main body are solar panels for providing electric power.

    The Phoenix mission is led by Principal Investigator Peter H. Smith of the University of Arizona, Tucson, with project management at NASA's Jet Propulsion Laboratory and development partnership with Lockheed Martin Space Systems, Denver. International contributions for Phoenix are provided by the Canadian Space Agency, the University of Neuchatel (Switzerland), the University of Copenhagen (Denmark), the Max Planck Institute (Germany) and the Finnish Meteorological institute. JPL is a division of the California

  17. Phoenix Mars Lander Spacecraft Processing

    NASA Image and Video Library

    2007-05-10

    In the Payload Hazardous Servicing Facility, technicians attach a crane to the Phoenix Mars Lander spacecraft. The crane will be used to remove the heat shield from around the Phoenix. The Phoenix mission is the first project in NASA's first openly competed program of Mars Scout missions. Phoenix will land in icy soils near the north polar permanent ice cap of Mars and explore the history of the water in these soils and any associated rocks, while monitoring polar climate. Landing is planned in May 2008 on arctic ground where a mission currently in orbit, Mars Odyssey, has detected high concentrations of ice just beneath the top layer of soil. It will serve as NASA's first exploration of a potential modern habitat on Mars and open the door to a renewed search for carbon-bearing compounds, last attempted with NASA’s Viking missions in the 1970s. A stereo color camera and a weather station will study the surrounding environment while the other instruments check excavated soil samples for water, organic chemicals and conditions that could indicate whether the site was ever hospitable to life. Microscopes can reveal features as small as one one-thousandth the width of a human hair. Launch of Phoenix aboard a Delta II rocket is targeted for Aug. 3 from Cape Canaveral Air Force Station in Florida.

  18. Phoenix Mars Lander Spacecraft Processing

    NASA Image and Video Library

    2007-05-10

    In the Payload Hazardous Servicing Facility, the Phoenix Mars Lander (foreground) can be seen inside the backshell. In the background, workers are helping place the heat shield, just removed from the Phoenix, onto a platform. The Phoenix mission is the first project in NASA's first openly competed program of Mars Scout missions. Phoenix will land in icy soils near the north polar permanent ice cap of Mars and explore the history of the water in these soils and any associated rocks, while monitoring polar climate. Landing is planned in May 2008 on arctic ground where a mission currently in orbit, Mars Odyssey, has detected high concentrations of ice just beneath the top layer of soil. It will serve as NASA's first exploration of a potential modern habitat on Mars and open the door to a renewed search for carbon-bearing compounds, last attempted with NASA’s Viking missions in the 1970s. A stereo color camera and a weather station will study the surrounding environment while the other instruments check excavated soil samples for water, organic chemicals and conditions that could indicate whether the site was ever hospitable to life. Microscopes can reveal features as small as one one-thousandth the width of a human hair. Launch of Phoenix aboard a Delta II rocket is targeted for Aug. 3 from Cape Canaveral Air Force Station in Florida.

  19. Phoenix Mars Lander Spacecraft Processing

    NASA Image and Video Library

    2007-05-10

    In the Payload Hazardous Servicing Facility, technicians lower a crane over the Phoenix Mars Lander spacecraft. The crane will be used to remove the heat shield from around the Phoenix. The Phoenix mission is the first project in NASA's first openly competed program of Mars Scout missions. Phoenix will land in icy soils near the north polar permanent ice cap of Mars and explore the history of the water in these soils and any associated rocks, while monitoring polar climate. Landing is planned in May 2008 on arctic ground where a mission currently in orbit, Mars Odyssey, has detected high concentrations of ice just beneath the top layer of soil. It will serve as NASA's first exploration of a potential modern habitat on Mars and open the door to a renewed search for carbon-bearing compounds, last attempted with NASA’s Viking missions in the 1970s. A stereo color camera and a weather station will study the surrounding environment while the other instruments check excavated soil samples for water, organic chemicals and conditions that could indicate whether the site was ever hospitable to life. Microscopes can reveal features as small as one one-thousandth the width of a human hair. Launch of Phoenix aboard a Delta II rocket is targeted for Aug. 3 from Cape Canaveral Air Force Station in Florida.

  20. Ultrahigh resolution topographic mapping of Mars with MRO HiRISE stereo images: Meter-scale slopes of candidate Phoenix landing sites

    USGS Publications Warehouse

    Kirk, R.L.; Howington-Kraus, E.; Rosiek, M.R.; Anderson, J.A.; Archinal, B.A.; Becker, K.J.; Cook, D.A.; Galuszka, D.M.; Geissler, P.E.; Hare, T.M.; Holmberg, I.M.; Keszthelyi, L.P.; Redding, B.L.; Delamere, W.A.; Gallagher, D.; Chapel, J.D.; Eliason, E.M.; King, R.; McEwen, A.S.

    2009-01-01

    The objectives of this paper are twofold: first, to report our estimates of the meter-to-decameter-scale topography and slopes of candidate landing sites for the Phoenix mission, based on analysis of Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) images with a typical pixel scale of 3 m and Mars Reconnaissance Orbiter (MRO) High Resolution Imaging Science Experiment (HiRISE) images at 0.3 m pixel-1 and, second, to document in detail the geometric calibration, software, and procedures on which the photogrammetric analysis of HiRISE data is based. A combination of optical design modeling, laboratory observations, star images, and Mars images form the basis for software in the U.S. Geological Survey Integrated Software for Imagers and Spectrometers (ISIS) 3 system that corrects the images for a variety of distortions with single-pixel or subpixel accuracy. Corrected images are analyzed in the commercial photogrammetric software SOCET SET (??BAE Systems), yielding digital topographic models (DTMs) with a grid spacing of 1 m (3-4 pixels) that require minimal interactive editing. Photoclinometry yields DTMs with single-pixel grid spacing. Slopes from MOC and HiRISE are comparable throughout the latitude zone of interest and compare favorably with those where past missions have landed successfully; only the Mars Exploration Rover (MER) B site in Meridiani Planum is smoother. MOC results at multiple locations have root-mean-square (RMS) bidirectional slopes of 0.8-4.5?? at baselines of 3-10 m. HiRISE stereopairs (one per final candidate site and one in the former site) yield 1.8-2.8?? slopes at 1-m baseline. Slopes at 1 m from photoclinometry are also in the range 2-3?? after correction for image blur. Slopes exceeding the 16?? Phoenix safety limit are extremely rare. Copyright 2008 by the American Geophysical Union.

  1. Flyover Animation of Phoenix Workspace

    NASA Technical Reports Server (NTRS)

    2008-01-01

    [figure removed for brevity, see original site] Click on image for animation

    This animated 'flyover' of the workspace of NASA's Phoenix Mars Lander's was created from images taken by the Surface Stereo Imager on Sol 14 (June 8, 2008), or the 14th Martian day after landing.

    The visualization uses both of the camera's 'eyes' to provide depth perception and ranging. The camera is looking north over the workspace.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  2. Phoenix Eases Down to Mars

    NASA Technical Reports Server (NTRS)

    2008-01-01

    [figure removed for brevity, see original site] Click on the image for the animation

    This artist's conception depicts NASA's Phoenix Mars Lander a moment before its touchdown on the arctic plains of Mars. Pulsed rocket engines control the spacecraft's speed during the final seconds of descent.

    This illustration is part of the animation featured above.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  3. Flyover Animation of Phoenix Workspace

    NASA Technical Reports Server (NTRS)

    2008-01-01

    [figure removed for brevity, see original site] Click on image for animation

    This animated 'flyover' of the workspace of NASA's Phoenix Mars Lander's was created from images taken by the Surface Stereo Imager on Sol 14 (June 8, 2008), or the 14th Martian day after landing.

    The visualization uses both of the camera's 'eyes' to provide depth perception and ranging. The camera is looking north over the workspace.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  4. The Ground Beneath Phoenix's Feet

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This view of a portion of the spacecraft deck and one of the footpads of NASA's three-legged Phoenix Mars Lander shows a solid surface at the spacecraft's landing site. As the legs touched down on the surface of Mars, they kicked up some loose material on top of the footpad, but overall, the surface is unperturbed.

    Each footpad is about the size of a large dinner plate, measuring 11.5 inches from rim to rim. The base of the footpad is shaped like the bottom of a shallow bowl to provide stability.

    This image was taken by the Phoenix spacecraft's Surface Stereo Imager shortly after landing on Mars.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  5. Terrain Type for Phoenix Landing

    NASA Image and Video Library

    2007-07-09

    This view shows the texture of the ground in the area that was favored as a landing site for NASA Phoenix Mars Lander mission. The pattern resembles permafrost terrain on Earth, where cycles of thawing and freezing cause cracking into polygon shapes.

  6. Phoenix Work Area Animation

    NASA Image and Video Library

    2008-05-28

    This image from Sol 1 shows a mosaic of NASA Mars Phoenix digging area in the Martian terrain. Phoenix scientists were very pleased with this view as the terrain features few rocks -- an optimal place for digging.

  7. Topographical Context of Phoenix Landing Region

    NASA Image and Video Library

    2007-08-02

    This area was designated Region D in the process of evaluating potential landing sites for NASA Phoenix Mars Lander. The topographical information is from the Mars Orbiter Laser Altimeter on NASA Mars Global Surveyor orbiter.

  8. Identity of the Perchlorate Parent Salt(s) at the Phoenix Mars Landing Site Based on Reanalysis of the Calcium Sensor Response

    NASA Astrophysics Data System (ADS)

    Kounaves, S. P.; Folds, K. E.; Hansen, V. M.; Weber, A. W.; Carrier, B. L.; Chaniotakis, N. A.

    2012-12-01

    analyses further constrain and provide a clear indication that the dominate parent salt in the soil at the Phoenix landing site is Ca(ClO4)2, with little or no contribution by Mg or Na-perchlorate salts. [1] Kounaves et al. (2010) J. Geophys. Res., 114, E00A19. [2] Hecht et al. (2009) Science, 325, 64-67. [3] Kounaves et al. (2010) Geophys. Res. Let., 37, L09201 [4] Quinn et al. (2011) Geophys. Res. Lett., 38, L14202. [5] Gellert et al. (2004) Science, 305, 829-32.

  9. Phoenix Telltale Movie with Clouds, Sol 103

    NASA Technical Reports Server (NTRS)

    2008-01-01

    NASA's Phoenix Mars Lander's telltale catches a breeze as clouds move over the landing site on Sol 103 (Sept. 7, 2008), the 103rd Martian day since landing.

    Phoenix's Surface Stereo Imager took this series of images during daily telltale monitoring around 3 p.m. local solar time and captured the clouds moving over the landing site.

    Phoenix can measure wind speed and direction by imaging the telltale, which is about about 10 centimeters (4 inches) tall. The telltale was built by the University of Aarhus, Denmark.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  10. Phoenix Mars Lander Spacecraft Processing

    NASA Image and Video Library

    2007-05-10

    An overhead crane lowers the backshell with the Phoenix Mars Lander inside toward a spin table for spin testing in the Payload Hazardous Servicing Facility. The Phoenix mission is the first project in NASA's first openly competed program of Mars Scout missions. Phoenix will land in icy soils near the north polar permanent ice cap of Mars and explore the history of the water in these soils and any associated rocks, while monitoring polar climate. Landing is planned in May 2008 on arctic ground where a mission currently in orbit, Mars Odyssey, has detected high concentrations of ice just beneath the top layer of soil. It will serve as NASA's first exploration of a potential modern habitat on Mars and open the door to a renewed search for carbon-bearing compounds, last attempted with NASA’s Viking missions in the 1970s. A stereo color camera and a weather station will study the surrounding environment while the other instruments check excavated soil samples for water, organic chemicals and conditions that could indicate whether the site was ever hospitable to life. Microscopes can reveal features as small as one one-thousandth the width of a human hair. Launch of Phoenix aboard a Delta II rocket is targeted for Aug. 3 from Cape Canaveral Air Force Station in Florida.

  11. Phoenix Mars Lander Spacecraft Processing

    NASA Image and Video Library

    2007-05-10

    This closeup shows the spin test of the Phoenix Mars Lander in the Payload Hazardous Servicing Facility. The Phoenix mission is the first project in NASA's first openly competed program of Mars Scout missions. Phoenix will land in icy soils near the north polar permanent ice cap of Mars and explore the history of the water in these soils and any associated rocks, while monitoring polar climate. Landing is planned in May 2008 on arctic ground where a mission currently in orbit, Mars Odyssey, has detected high concentrations of ice just beneath the top layer of soil. It will serve as NASA's first exploration of a potential modern habitat on Mars and open the door to a renewed search for carbon-bearing compounds, last attempted with NASA’s Viking missions in the 1970s. A stereo color camera and a weather station will study the surrounding environment while the other instruments check excavated soil samples for water, organic chemicals and conditions that could indicate whether the site was ever hospitable to life. Microscopes can reveal features as small as one one-thousandth the width of a human hair. Launch of Phoenix aboard a Delta II rocket is targeted for Aug. 3 from Cape Canaveral Air Force Station in Florida.

  12. Phoenix Mars Lander Spacecraft Processing

    NASA Image and Video Library

    2007-05-10

    In the Payload Hazardous Servicing Facility, an overhead crane lifts the heat shield from the Phoenix Mars Lander spacecraft. The Phoenix mission is the first project in NASA's first openly competed program of Mars Scout missions. Phoenix will land in icy soils near the north polar permanent ice cap of Mars and explore the history of the water in these soils and any associated rocks, while monitoring polar climate. Landing is planned in May 2008 on arctic ground where a mission currently in orbit, Mars Odyssey, has detected high concentrations of ice just beneath the top layer of soil. It will serve as NASA's first exploration of a potential modern habitat on Mars and open the door to a renewed search for carbon-bearing compounds, last attempted with NASA’s Viking missions in the 1970s. A stereo color camera and a weather station will study the surrounding environment while the other instruments check excavated soil samples for water, organic chemicals and conditions that could indicate whether the site was ever hospitable to life. Microscopes can reveal features as small as one one-thousandth the width of a human hair. Launch of Phoenix aboard a Delta II rocket is targeted for Aug. 3 from Cape Canaveral Air Force Station in Florida.

  13. Phoenix Mars Lander Spacecraft Processing

    NASA Image and Video Library

    2007-05-10

    In the Payload Hazardous Servicing Facility, an overhead crane moves the heat shield toward a platform at left. The heat shield was removed from the Phoenix Mars Lander spacecraft at right. The Phoenix mission is the first project in NASA's first openly competed program of Mars Scout missions. Phoenix will land in icy soils near the north polar permanent ice cap of Mars and explore the history of the water in these soils and any associated rocks, while monitoring polar climate. Landing is planned in May 2008 on arctic ground where a mission currently in orbit, Mars Odyssey, has detected high concentrations of ice just beneath the top layer of soil. It will serve as NASA's first exploration of a potential modern habitat on Mars and open the door to a renewed search for carbon-bearing compounds, last attempted with NASA’s Viking missions in the 1970s. A stereo color camera and a weather station will study the surrounding environment while the other instruments check excavated soil samples for water, organic chemicals and conditions that could indicate whether the site was ever hospitable to life. Microscopes can reveal features as small as one one-thousandth the width of a human hair. Launch of Phoenix aboard a Delta II rocket is targeted for Aug. 3 from Cape Canaveral Air Force Station in Florida.

  14. Phoenix Mars Lander Spacecraft Processing

    NASA Image and Video Library

    2007-05-10

    An overhead crane lifts the backshell with the Phoenix Mars Lander inside off its work stand in the Payload Hazardous Servicing Facility. The spacecraft is being moved to a spin table (back left) for spin testing. The Phoenix mission is the first project in NASA's first openly competed program of Mars Scout missions. Phoenix will land in icy soils near the north polar permanent ice cap of Mars and explore the history of the water in these soils and any associated rocks, while monitoring polar climate. Landing is planned in May 2008 on arctic ground where a mission currently in orbit, Mars Odyssey, has detected high concentrations of ice just beneath the top layer of soil. It will serve as NASA's first exploration of a potential modern habitat on Mars and open the door to a renewed search for carbon-bearing compounds, last attempted with NASA’s Viking missions in the 1970s. A stereo color camera and a weather station will study the surrounding environment while the other instruments check excavated soil samples for water, organic chemicals and conditions that could indicate whether the site was ever hospitable to life. Microscopes can reveal features as small as one one-thousandth the width of a human hair. Launch of Phoenix aboard a Delta II rocket is targeted for Aug. 3 from Cape Canaveral Air Force Station in Florida.

  15. Phoenix Mars Lander Spacecraft Processing

    NASA Image and Video Library

    2007-05-10

    This closeup shows the Phoenix Mars Lander spacecraft nestled inside the backshell. The spacecraft is ready for spin testing on the spin table to which it is attached in the Payload Hazardous Servicing Facility. The Phoenix mission is the first project in NASA's first openly competed program of Mars Scout missions. Phoenix will land in icy soils near the north polar permanent ice cap of Mars and explore the history of the water in these soils and any associated rocks, while monitoring polar climate. Landing is planned in May 2008 on arctic ground where a mission currently in orbit, Mars Odyssey, has detected high concentrations of ice just beneath the top layer of soil. It will serve as NASA's first exploration of a potential modern habitat on Mars and open the door to a renewed search for carbon-bearing compounds, last attempted with NASA’s Viking missions in the 1970s. A stereo color camera and a weather station will study the surrounding environment while the other instruments check excavated soil samples for water, organic chemicals and conditions that could indicate whether the site was ever hospitable to life. Microscopes can reveal features as small as one one-thousandth the width of a human hair. Launch of Phoenix aboard a Delta II rocket is targeted for Aug. 3 from Cape Canaveral Air Force Station in Florida.

  16. Phoenix Mars Lander Spacecraft Processing

    NASA Image and Video Library

    2007-05-10

    This closeup shows the Phoenix Mars Lander spacecraft nestled inside the backshell. The spacecraft will undergo spin testing on the spin table to which it is attached in the Payload Hazardous Servicing Facility. The Phoenix mission is the first project in NASA's first openly competed program of Mars Scout missions. Phoenix will land in icy soils near the north polar permanent ice cap of Mars and explore the history of the water in these soils and any associated rocks, while monitoring polar climate. Landing is planned in May 2008 on arctic ground where a mission currently in orbit, Mars Odyssey, has detected high concentrations of ice just beneath the top layer of soil. It will serve as NASA's first exploration of a potential modern habitat on Mars and open the door to a renewed search for carbon-bearing compounds, last attempted with NASA’s Viking missions in the 1970s. A stereo color camera and a weather station will study the surrounding environment while the other instruments check excavated soil samples for water, organic chemicals and conditions that could indicate whether the site was ever hospitable to life. Microscopes can reveal features as small as one one-thousandth the width of a human hair. Launch of Phoenix aboard a Delta II rocket is targeted for Aug. 3 from Cape Canaveral Air Force Station in Florida.

  17. Phoenix Mars Lander Spacecraft Processing

    NASA Image and Video Library

    2007-05-10

    In the Payload Hazardous Servicing Facility, workers help guide the heat shield onto a platform. The heat shield was removed from the Phoenix Mars Lander spacecraft.. The Phoenix mission is the first project in NASA's first openly competed program of Mars Scout missions. Phoenix will land in icy soils near the north polar permanent ice cap of Mars and explore the history of the water in these soils and any associated rocks, while monitoring polar climate. Landing is planned in May 2008 on arctic ground where a mission currently in orbit, Mars Odyssey, has detected high concentrations of ice just beneath the top layer of soil. It will serve as NASA's first exploration of a potential modern habitat on Mars and open the door to a renewed search for carbon-bearing compounds, last attempted with NASA’s Viking missions in the 1970s. A stereo color camera and a weather station will study the surrounding environment while the other instruments check excavated soil samples for water, organic chemicals and conditions that could indicate whether the site was ever hospitable to life. Microscopes can reveal features as small as one one-thousandth the width of a human hair. Launch of Phoenix aboard a Delta II rocket is targeted for Aug. 3 from Cape Canaveral Air Force Station in Florida.

  18. Phoenix Mars Lander Spacecraft Processing

    NASA Image and Video Library

    2007-05-10

    In the Payload Hazardous Servicing Facility, workers watch as an overhead crane lowers the heat shield toward a platform. The heat shield was removed from the Phoenix Mars Lander spacecraft. The Phoenix mission is the first project in NASA's first openly competed program of Mars Scout missions. Phoenix will land in icy soils near the north polar permanent ice cap of Mars and explore the history of the water in these soils and any associated rocks, while monitoring polar climate. Landing is planned in May 2008 on arctic ground where a mission currently in orbit, Mars Odyssey, has detected high concentrations of ice just beneath the top layer of soil. It will serve as NASA's first exploration of a potential modern habitat on Mars and open the door to a renewed search for carbon-bearing compounds, last attempted with NASA’s Viking missions in the 1970s. A stereo color camera and a weather station will study the surrounding environment while the other instruments check excavated soil samples for water, organic chemicals and conditions that could indicate whether the site was ever hospitable to life. Microscopes can reveal features as small as one one-thousandth the width of a human hair. Launch of Phoenix aboard a Delta II rocket is targeted for Aug. 3 from Cape Canaveral Air Force Station in Florida.

  19. Phoenix Mars Lander Spacecraft Processing

    NASA Image and Video Library

    2007-05-10

    In the Payload Hazardous Servicing Facility, technicians secure the backshell with the Phoenix Mars Lander inside onto a spin table for spin testing. The Phoenix mission is the first project in NASA's first openly competed program of Mars Scout missions. Phoenix will land in icy soils near the north polar permanent ice cap of Mars and explore the history of the water in these soils and any associated rocks, while monitoring polar climate. Landing is planned in May 2008 on arctic ground where a mission currently in orbit, Mars Odyssey, has detected high concentrations of ice just beneath the top layer of soil. It will serve as NASA's first exploration of a potential modern habitat on Mars and open the door to a renewed search for carbon-bearing compounds, last attempted with NASA’s Viking missions in the 1970s. A stereo color camera and a weather station will study the surrounding environment while the other instruments check excavated soil samples for water, organic chemicals and conditions that could indicate whether the site was ever hospitable to life. Microscopes can reveal features as small as one one-thousandth the width of a human hair. Launch of Phoenix aboard a Delta II rocket is targeted for Aug. 3 from Cape Canaveral Air Force Station in Florida.

  20. How Phoenix Measures Wind Speed and Direction

    NASA Technical Reports Server (NTRS)

    2008-01-01

    [figure removed for brevity, see original site] Click on image for animation

    This animation shows how NASA's Phoenix Mars Lander can measure wind speed and direction by imaging the Telltale with the Stereo Surface Imager (SSI).

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  1. Flyover Video of Phoenix Work Area

    NASA Technical Reports Server (NTRS)

    2008-01-01

    [figure removed for brevity, see original site] Click on image for animation

    This video shows an overhead view of NASA's Phoenix Mars Lander and the work area of the Robotic Arm.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  2. Flyover Video of Phoenix Work Area

    NASA Technical Reports Server (NTRS)

    2008-01-01

    [figure removed for brevity, see original site] Click on image for animation

    This video shows an overhead view of NASA's Phoenix Mars Lander and the work area of the Robotic Arm.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  3. Phoenix's Lay of the Land

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This image from NASA's Phoenix Mars Lander shows the spacecraft's recent activity site as of the 23rd Martian day of the mission, or Sol 22 (June 16, 2008), after the spacecraft touched down on the Red Planet's northern polar plains. The mosaic was taken by the lander's Surface Stereo Imager (SSI). Parts of Phoenix can be seen in the foreground.

    The first two trenches dug by the lander's Robotic Arm, called 'Dodo' and 'Goldilocks,' were enlarged on the 19th Martian day of the mission, or Sol 18 (June 12, 2008), to form one trench, dubbed 'Dodo-Goldilocks.' Scoops of material taken from those trenches are informally called 'Baby Bear' and 'Mama Bear.' Baby Bear was carried to Phoenix's Thermal and Evolved-Gas Analyzer, or TEGA, instrument for analysis, while Mama Bear was delivered to Phoenix's Microscopy, Electrochemistry and Conductivity Analyzer instrument suite, or MECA, for a closer look.

    The color inset picture of the Dodo-Goldilocks trench, also taken with Phoenix's SSI, reveals white material thought to be ice.

    More recently, on Sol 22 (June 16, 2008), Phoenix's Robotic Arm began digging a trench, dubbed 'Snow White,' in a patch of Martian soil near the center of a polygonal surface feature, nicknamed 'Cheshire Cat.' The 'dump pile' is located at the top of the trench, and has been dubbed 'Croquet Ground.' The digging site has been nicknamed 'Wonderland.'

    The Snow White trench, seen here in an SSI image from Sol 22 (June 16, 2008) is about 2 centimeters (.8 inches) deep and 30 centimeters (12 inches) long. As of Sol 25 (June 19, 2008), the trench is 5 centimeters (2 inches deep) and the trench has been renamed 'Snow White 1,' as a second trench has been dug to its right and nicknamed 'Snow White 2.'

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems

  4. Phoenix's Lay of the Land

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This image from NASA's Phoenix Mars Lander shows the spacecraft's recent activity site as of the 23rd Martian day of the mission, or Sol 22 (June 16, 2008), after the spacecraft touched down on the Red Planet's northern polar plains. The mosaic was taken by the lander's Surface Stereo Imager (SSI). Parts of Phoenix can be seen in the foreground.

    The first two trenches dug by the lander's Robotic Arm, called 'Dodo' and 'Goldilocks,' were enlarged on the 19th Martian day of the mission, or Sol 18 (June 12, 2008), to form one trench, dubbed 'Dodo-Goldilocks.' Scoops of material taken from those trenches are informally called 'Baby Bear' and 'Mama Bear.' Baby Bear was carried to Phoenix's Thermal and Evolved-Gas Analyzer, or TEGA, instrument for analysis, while Mama Bear was delivered to Phoenix's Microscopy, Electrochemistry and Conductivity Analyzer instrument suite, or MECA, for a closer look.

    The color inset picture of the Dodo-Goldilocks trench, also taken with Phoenix's SSI, reveals white material thought to be ice.

    More recently, on Sol 22 (June 16, 2008), Phoenix's Robotic Arm began digging a trench, dubbed 'Snow White,' in a patch of Martian soil near the center of a polygonal surface feature, nicknamed 'Cheshire Cat.' The 'dump pile' is located at the top of the trench, and has been dubbed 'Croquet Ground.' The digging site has been nicknamed 'Wonderland.'

    The Snow White trench, seen here in an SSI image from Sol 22 (June 16, 2008) is about 2 centimeters (.8 inches) deep and 30 centimeters (12 inches) long. As of Sol 25 (June 19, 2008), the trench is 5 centimeters (2 inches deep) and the trench has been renamed 'Snow White 1,' as a second trench has been dug to its right and nicknamed 'Snow White 2.'

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems

  5. Phoenix Deploying its Wrist

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This animated gif shows a series of images taken by Phoenix's Stereo Surface Imager (SSI) on Sol 3. It illustrates the actions that Phoenix's Robotic Arm took to deploy its wrist.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  6. Phoenix Lidar Operation Animation

    NASA Technical Reports Server (NTRS)

    2008-01-01

    [figure removed for brevity, see original site] Click on image for animation

    This is an animation of the Canadian-built meteorological station's lidar, which was successfully activated on Sol 2. The animation shows how the lidar is activated by first opening its dust cover, then emitting rapid pulses of light (resembling a brilliant green laser) into the Martian atmosphere. Some of the light then bounces off particles in the atmosphere, and is reflected back down to the lidar's telescope. This allows the lidar to detect dust, clouds and fog.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  7. Martian Surface Beneath Phoenix

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This is an image of the Martian surface beneath NASA's Phoenix Mars Lander. The image was taken by Phoenix's Robotic Arm Camera (RAC) on the eighth Martian day of the mission, or Sol 8 (June 2, 2008). The light feature in the middle of the image below the leg is informally called 'Holy Cow.' The dust, shown in the dark foreground, has been blown off of 'Holy Cow' by Phoenix's thruster engines.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  8. Martian Surface Beneath Phoenix

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This is an image of the Martian surface beneath NASA's Phoenix Mars Lander. The image was taken by Phoenix's Robotic Arm Camera (RAC) on the eighth Martian day of the mission, or Sol 8 (June 2, 2008). The light feature in the middle of the image below the leg is informally called 'Holy Cow.' The dust, shown in the dark foreground, has been blown off of 'Holy Cow' by Phoenix's thruster engines.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  9. Maps of the Martian Landing Sites and Rover Traverses: Viking 1 and 2, Mars Pathfinder, and Phoenix Landers, and the Mars Exploration Rovers.

    NASA Astrophysics Data System (ADS)

    Parker, T. J.; Calef, F. J., III; Deen, R. G.; Gengl, H.

    2016-12-01

    The traverse maps produced tactically for the MER and MSL rover missions are the first step in placing the observations made by each vehicle into a local and regional geologic context. For the MER, Phoenix and MSL missions, 25cm/pixel HiRISE data is available for accurately localizing the vehicles. Viking and Mars Pathfinder, however, relied on Viking Orbiter images of several tens of m/pixel to triangulate to horizon features visible both from the ground and from orbit. After Pathfinder, MGS MOC images became available for these landing sites, enabling much better correlations to horizon features and localization predictions to be made, that were then corroborated with HiRISE images beginning 9 years ago. By combining topography data from MGS, Mars Express, and stereo processing of MRO CTX and HiRISE images into orthomosaics (ORRs) and digital elevation models (DEMs), it is possible to localize all the landers and rover positions to an accuracy of a few tens of meters with respect to the Mars global control net, and to better than half a meter with respect to other features within a HiRISE orthomosaic. JPL's MIPL produces point clouds of the MER Navcam stereo images that can be processed into 1cm/pixel ORR/DEMs that are then georeferenced to a HiRISE/CTX base map and DEM. This allows compilation of seamless mosaics of the lander and rover camera-based ORR/DEMs with the HiRISE ORR/DEM that can be viewed in 3 dimensions with GIS programs with that capability. We are re-processing the Viking Lander, Mars Pathfinder, and Phoenix lander data to allow similar ORR/DEM products to be made for those missions. For the fixed landers and Spirit, we will compile merged surface/CTX/HiRISE ORR/DEMs, that will enable accurate local and regional mapping of these landing sites, and allow comparisons of the results from these missions to be made with current and future surface missions.

  10. Declining Sunshine for Phoenix Lander

    NASA Technical Reports Server (NTRS)

    2008-01-01

    The yellow line on this graphic indicates the number of hours of sunlight each sol, or Martian day, at the Phoenix landing site's far-northern latitude, beginning with the entire Martian day (about 24 hours and 40 minutes) for the first 90 sols, then declining to no sunlight by about sol 300. The blue tick mark indicates that on Sol 124 (Sept. 29, 2008), the sun is above the horizon for about 20 hours.

    The brown vertical bar represents the period from Nov. 18 to Dec. 24, 2008, around the 'solar conjunction,' when the sun is close to the line between Mars and Earth, affecting communications.

    The green vertical rectangle represents the period from February to November 2009 when the Phoenix lander is expected to be encased in carbon-dioxide ice.

  11. Declining Sunshine for Phoenix Lander

    NASA Technical Reports Server (NTRS)

    2008-01-01

    The yellow line on this graphic indicates the number of hours of sunlight each sol, or Martian day, at the Phoenix landing site's far-northern latitude, beginning with the entire Martian day (about 24 hours and 40 minutes) for the first 90 sols, then declining to no sunlight by about sol 300. The blue tick mark indicates that on Sol 124 (Sept. 29, 2008), the sun is above the horizon for about 20 hours.

    The brown vertical bar represents the period from Nov. 18 to Dec. 24, 2008, around the 'solar conjunction,' when the sun is close to the line between Mars and Earth, affecting communications.

    The green vertical rectangle represents the period from February to November 2009 when the Phoenix lander is expected to be encased in carbon-dioxide ice.

  12. Dust Devil Tracks and Wind Streaks in the North Polar Region of Mars: A Study of the 2007 Phoenix Mars Lander Sites

    NASA Technical Reports Server (NTRS)

    Drake, Nathan B.; Tamppari, Leslie K.; Baker, R. David; Cantor, Bruce A.; Hale, Amy S.

    2006-01-01

    The 65-72 latitude band of the North Polar Region of Mars, where the 2007 Phoenix Mars Lander will land, was studied using satellite images from the Mars Global Surveyor (MGS) Mars Orbiter Camera Narrow-Angle (MOC-NA) camera. Dust devil tracks (DDT) and wind streaks (WS) were observed and recorded as surface evidence for winds. No active dust devils (DDs) were observed. 162 MOC-NA images, 10.3% of total images, contained DDT/WS. Phoenix landing Region C (295-315W) had the highest concentration of images containing DDT/WS per number of available images (20.9%); Region D (130-150W) had the lowest (3.5%). DDT and WS direction were recorded for Phoenix landing regions A (110-130W), B (240-260W), and C to infer local wind direction. Region A showed dominant northwest-southeast DDT/WS, Region B showed dominant north-south, east-west and northeast-southwest DDT/WS, and region C showed dominant west/northwest - east/southeast DDT/ WS. Results indicate the 2007 Phoenix Lander has the highest probability of landing near DDT/WS in landing Region C. Based on DDT/WS linearity, we infer Phoenix would likely encounter directionally consistent background wind in any of the three regions.

  13. Dust Devil Tracks and Wind Streaks in the North Polar Region of Mars: A Study of the 2007 Phoenix Mars Lander Sites

    NASA Technical Reports Server (NTRS)

    Drake, Nathan B.; Tamppari, Leslie K.; Baker, R. David; Cantor, Bruce A.; Hale, Amy S.

    2006-01-01

    The 65-72 latitude band of the North Polar Region of Mars, where the 2007 Phoenix Mars Lander will land, was studied using satellite images from the Mars Global Surveyor (MGS) Mars Orbiter Camera Narrow-Angle (MOC-NA) camera. Dust devil tracks (DDT) and wind streaks (WS) were observed and recorded as surface evidence for winds. No active dust devils (DDs) were observed. 162 MOC-NA images, 10.3% of total images, contained DDT/WS. Phoenix landing Region C (295-315W) had the highest concentration of images containing DDT/WS per number of available images (20.9%); Region D (130-150W) had the lowest (3.5%). DDT and WS direction were recorded for Phoenix landing regions A (110-130W), B (240-260W), and C to infer local wind direction. Region A showed dominant northwest-southeast DDT/WS, Region B showed dominant north-south, east-west and northeast-southwest DDT/WS, and region C showed dominant west/northwest - east/southeast DDT/ WS. Results indicate the 2007 Phoenix Lander has the highest probability of landing near DDT/WS in landing Region C. Based on DDT/WS linearity, we infer Phoenix would likely encounter directionally consistent background wind in any of the three regions.

  14. Phoenix Lidar Operation Animation

    NASA Image and Video Library

    2008-05-29

    This image from NASA Phoenix Mars Lander of the Canadian-built meteorological station lidar, which was successfully activated on Sol 2 by first opening its dust cover, then emitting rapid pulses of light.

  15. Phoenix Color Targets

    NASA Technical Reports Server (NTRS)

    2008-01-01

    These images of three Phoenix color targets were taken on sols 1 and 2 by the Surface Stereo Imager (SSI) on board the Phoenix lander. The bottom target was imaged in approximate color (SSI's red, green, and blue filters: 600, 530, and 480 nanometers), while the others were imaged with an infrared filter (750 nanometers). All of them will be imaged many times over the mission to monitor the color calibration of the camera. The two at the top show grains 2 to 3 millimeters in size that were likely lifted to the Phoenix deck during landing. Each of the large color chips on each target contains a strong magnet to protect the interior material from Mars' magnetic dust.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  16. Phoenix Robotic Arm Rasp

    NASA Image and Video Library

    2008-07-15

    This photograph shows the rasp protruding from the back of the scoop on NASA Phoenix Mars Lander Robotic Arm engineering model in the Payload Interoperability Testbed at the University of Arizona, Tucson.

  17. Phoenix Color Targets

    NASA Technical Reports Server (NTRS)

    2008-01-01

    These images of three Phoenix color targets were taken on sols 1 and 2 by the Surface Stereo Imager (SSI) on board the Phoenix lander. The bottom target was imaged in approximate color (SSI's red, green, and blue filters: 600, 530, and 480 nanometers), while the others were imaged with an infrared filter (750 nanometers). All of them will be imaged many times over the mission to monitor the color calibration of the camera. The two at the top show grains 2 to 3 millimeters in size that were likely lifted to the Phoenix deck during landing. Each of the large color chips on each target contains a strong magnet to protect the interior material from Mars' magnetic dust.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  18. City of Phoenix - Energize Phoenix Program

    SciTech Connect

    Laloudakis, Dimitrios J.

    2014-09-29

    Energize Phoenix (EPHX) was designed as an ambitious, large-scale, three-year pilot program to provide energy efficiency upgrades in buildings, along Phoenix’s new Light Rail Corridor – part of a federal effort to reduce energy consumption and stimulate job growth, while simultaneously reducing the country’s carbon footprint and promoting a shift towards a green economy. The program was created through a 2010 competitive grant awarded to the City of Phoenix who managed the program in partnership with Arizona State University (ASU), the state’s largest university, and Arizona Public Service (APS), the state’s largest electricity provider. The U.S. Department of Energy (DOE) Better Buildings Neighborhood Program (BBNP) and the American Recovery and Reinvestment Act (ARRA) of 2009 provided $25M in funding for the EPHX program. The Light Rail Corridor runs through the heart of downtown Phoenix, making most high-rise and smaller commercial buildings eligible to participate in the EPHX program, along with a diverse mix of single and multi-family residential buildings. To ensure maximum impact and deeper market penetration, Energize Phoenix was subdivided into three unique parts: i. commercial rebate program, ii. commercial financing program, and iii. residential program Each component was managed by the City of Phoenix in partnership with APS. Phoenix was fortunate to partner with APS, which already operated robust commercial and residential rebate programs within its service territory. Phoenix tapped into the existing utility contractor network, provided specific training to over 100 contracting firms, and leveraged the APS rebate program structure (energy efficiency funding) to launch the EPHX commercial and residential rebate programs. The commercial finance program was coordinated and managed through a contract with National Bank of Arizona, NBAZ, which also provided project capital leveraging EPHX finance funds. Working in unison, approved contractors

  19. Phoenix Society for Burn Survivors

    MedlinePlus

    ... Community Blog Taking Care of Yourself at Phoenix World Burn Congress 3 Oct 2017 Imagine this: a ... Menu Get Support Find Resources Our Programs Phoenix World Burn Congress Get Involved Ways to Give Who ...

  20. Phoenix Wet Chemistry Laboratory Units

    NASA Image and Video Library

    2008-06-26

    This image shows four Wet Chemistry Laboratory units, part of the Microscopy, Electrochemistry, and Conductivity Analyzer MECA instrument on board NASA Phoenix Mars Lander. This image was taken before Phoenix launch on August 4, 2007.

  1. Composite View from Phoenix Lander

    NASA Image and Video Library

    2009-07-02

    This mosaic of images from the Surface Stereo Imager camera on NASA Phoenix Mars Lander shows several trenches dug by Phoenix, plus a corner of the spacecraft deck and the Martian arctic plain stretching to the horizon.

  2. Soil on Phoenix's MECA

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This image shows soil delivery to NASA's Phoenix Mars Lander's Microscopy, Electrochemistry and Conductivity Analyzer (MECA). The image was taken by the lander's Surface Stereo Imager on the 131st Martian day, or sol, of the mission (Oct. 7, 2008).

    At the bottom of the image is the chute for delivering samples to MECA's microscopes. It is relatively clean due to the Phoenix team using methods such as sprinkling to minimize cross-contamination of samples. However, the cumulative effect of several sample deliveries can be seen in the soil piles on either side of the chute.

    On the right side are the four chemistry cells with soil residue piled up on exposed surfaces. The farthest cell has a large pile of material from an area of the Phoenix workspace called 'Stone Soup.' This area is deep in the trough at a polygon boundary, and its soil was so sticky it wouldn't even go through the funnel.

    One of Phoenix's solar panels is shown in the background of this image.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  3. Soil on Phoenix's MECA

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This image shows soil delivery to NASA's Phoenix Mars Lander's Microscopy, Electrochemistry and Conductivity Analyzer (MECA). The image was taken by the lander's Surface Stereo Imager on the 131st Martian day, or sol, of the mission (Oct. 7, 2008).

    At the bottom of the image is the chute for delivering samples to MECA's microscopes. It is relatively clean due to the Phoenix team using methods such as sprinkling to minimize cross-contamination of samples. However, the cumulative effect of several sample deliveries can be seen in the soil piles on either side of the chute.

    On the right side are the four chemistry cells with soil residue piled up on exposed surfaces. The farthest cell has a large pile of material from an area of the Phoenix workspace called 'Stone Soup.' This area is deep in the trough at a polygon boundary, and its soil was so sticky it wouldn't even go through the funnel.

    One of Phoenix's solar panels is shown in the background of this image.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  4. Aqueous extracts of a Mars analogue regolith that mimics the Phoenix landing site do not inhibit spore germination or growth of model spacecraft contaminants Bacillus subtilis 168 and Bacillus pumilus SAFR-032

    NASA Astrophysics Data System (ADS)

    Nicholson, Wayne L.; McCoy, Lashelle E.; Kerney, Krystal R.; Ming, Douglas W.; Golden, D. C.; Schuerger, Andrew C.

    2012-08-01

    Because Mars is a primary target for life detection and habitability assessment missions, its exploration is also by necessity a Planetary Protection issue. The recent finding of significant levels of perchlorate (ClO4-) in regolith sampled from the Phoenix landing site raises the question of its potential biotoxicity to putative indigenous martian life, microbial forward contaminants from Earth, or future human visitors. To address this issue, an analogue regolith was constructed based on regolith chemistry data from the Phoenix landing site. A Mars Aqueous Regolith Extract (MARE) was prepared from the Phoenix analogue regolith and analyzed by ion chromatography. The MARE contained (mg/L) the cations Na+ (1411 ± 181), Mg2+ (1051 ± 160), Ca2+ (832 ± 125), and K+ (261 ± 29), and the anions SO42-(5911±993), ClO4-(5316±1767), Cl(171±25) and F- (2.0 ± 0.4). Nitrogen-containing species NO3-(773±113) and NO2-(6.9±2.3) were also present as a result of regolith preparation procedures, but their relevance to Mars is at present unknown. The MARE was tested for potential toxic effects on two model spacecraft contaminants, the spore-forming bacteria Bacillus subtilis strain 168 and Bacillus pumilus strain SAFR-032. In B. subtilis, spore germination and initial vegetative growth (up to ˜5 h) was not inhibited in a rich complex medium prepared with the MARE, but growth after 5 h was significantly suppressed in medium prepared using the MARE. Both B. subtilis and B. pumilus exhibited significantly higher rates of spore germination and growth in the MARE vs. DW with no additions (likely due to endogenous spore nutrients), but germination and growth was further stimulated by addition of glucose and a combination of buffered inorganic salts (K2HPO4, KH2PO4, (NH4)2SO4, and MgSO4). The data indicate that the aqueous environment in the regolith from the Phoenix landing site containing high levels of perchlorate does not pose a significant barrier to growth of putative

  5. Soil on Phoenix Deck

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This image, taken by the Surface Stereo Imager (SSI) of NASA's Phoenix Lander, shows Martian soil piled on top of the spacecraft's deck and some of its instruments. Visible in the upper-left portion of the image are several wet chemistry cells of the lander's Microscopy, Electrochemistry, and Conductivity Analyzer (MECA). The instrument on the lower right of the image is the Thermal and Evolved-Gas Analyzer. The excess sample delivered to the MECA's sample stage can be seen on the deck in the lower left portion of the image.

    This image was taken on Martian day, or sol, 142, on Saturday, Oct. 19, 2008. Phoenix landed on Mars' northern plains on May 25, 2008.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  6. Soil on Phoenix Deck

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This image, taken by the Surface Stereo Imager (SSI) of NASA's Phoenix Lander, shows Martian soil piled on top of the spacecraft's deck and some of its instruments. Visible in the upper-left portion of the image are several wet chemistry cells of the lander's Microscopy, Electrochemistry, and Conductivity Analyzer (MECA). The instrument on the lower right of the image is the Thermal and Evolved-Gas Analyzer. The excess sample delivered to the MECA's sample stage can be seen on the deck in the lower left portion of the image.

    This image was taken on Martian day, or sol, 142, on Saturday, Oct. 19, 2008. Phoenix landed on Mars' northern plains on May 25, 2008.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  7. Phoenix's Wet Chemistry Lab

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This is an illustration of soil analysis on NASA's Phoenix Mars Lander's Wet Chemistry Lab (WCL) on board the Microscopy, Electrochemistry, and Conductivity Analyzer (MECA) instrument. By dissolving small amounts of soil in water, WCL will attempt to determine the pH, the abundance of minerals such as magnesium and sodium cations or chloride, bromide and sulfate anions, as well as the conductivity and redox potential.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  8. Phoenix's Wet Chemistry Lab

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This is an illustration of the analytical procedure of NASA's Phoenix Mars Lander's Wet Chemistry Lab (WCL) on board the Microscopy, Electrochemistry, and Conductivity Analyzer (MECA) instrument. By dissolving small amounts of soil in water, WCL can determine the pH, the abundance of minerals such as magnesium and sodium cations or chloride, bromide and sulfate anions, as well as the conductivity and redox potential.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  9. Clumps in Phoenix Scoop

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This sample of Martian soil was collected by the NASA's Phoenix Mars Lander during the 14th Martian day after landing (June 8, 2008) for later delivery to the lander's Optical Microscope. The Robotic Arm Camera took the picture of the contents of the arm's scoop, about 9 centimeters (3.5 inches) wide.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  10. Phoenix Robotic Arm Rasp

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This photograph shows the rasp protruding from the back of the scoop on NASA's Phoenix Mars Lander's Robotic Arm engineering model in the Payload Interoperability Testbed at the University of Arizona, Tucson.

    This is the position the rasp will assume when it drills into the Martian soil to acquire an icy soil sample for analysis.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is led by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  11. Clumps in Phoenix Scoop

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This sample of Martian soil was collected by the NASA's Phoenix Mars Lander during the 14th Martian day after landing (June 8, 2008) for later delivery to the lander's Optical Microscope. The Robotic Arm Camera took the picture of the contents of the arm's scoop, about 9 centimeters (3.5 inches) wide.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  12. Phoenix's Wet Chemistry Lab

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This is an illustration of soil analysis on NASA's Phoenix Mars Lander's Wet Chemistry Lab (WCL) on board the Microscopy, Electrochemistry, and Conductivity Analyzer (MECA) instrument. By dissolving small amounts of soil in water, WCL will attempt to determine the pH, the abundance of minerals such as magnesium and sodium cations or chloride, bromide and sulfate anions, as well as the conductivity and redox potential.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  13. Phoenix's Wet Chemistry Lab

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This is an illustration of the analytical procedure of NASA's Phoenix Mars Lander's Wet Chemistry Lab (WCL) on board the Microscopy, Electrochemistry, and Conductivity Analyzer (MECA) instrument. By dissolving small amounts of soil in water, WCL can determine the pH, the abundance of minerals such as magnesium and sodium cations or chloride, bromide and sulfate anions, as well as the conductivity and redox potential.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  14. Phoenix Lander Work Area

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This image shows NASA's Phoenix Mars Lander Robotic Arm work area with an overlay. The pink area is available for digging, the green area is reserved for placing the Thermal and Electrical Conductivity Probe (TECP) instrument. Soil can be dumped in the violet area.

    Images were displayed using NASA Ames 'Viz' visualization software.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  15. Soil on Phoenix's TEGA

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This image shows soil on the doors of the Thermal and Evolved Gas Analyzer (TEGA) onboard NASA's Phoenix Mars Lander. The image was taken by the lander's Robotic Arm Camera on the 131st Martian day, or sol, of the mission (Oct. 7, 2008). This sample delivered to TEGA was named 'Rosy Red.'

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  16. Phoenix Robotic Arm Rasp

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This photograph shows the rasp protruding from the back of the scoop on NASA's Phoenix Mars Lander's Robotic Arm engineering model in the Payload Interoperability Testbed at the University of Arizona, Tucson.

    This is the position the rasp will assume when it drills into the Martian soil to acquire an icy soil sample for analysis.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is led by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  17. Animation of Panorama of Phoenix Landing Area Looking Southeast

    NASA Technical Reports Server (NTRS)

    2008-01-01

    [figure removed for brevity, see original site] Click on image for animation

    This is an animation of panoramic images taken by NASA's Phoenix Mars Lander's Surface Stereo Imager on Sol 15 (June 9, 2008), the 15th Martian day after landing. The panorama looks to the southeast and shows rocks casting shadows, polygons on the surface and as the image looks to the horizon, Phoenix's backshell gleams in the distance.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  18. PHOENIX. Higher Wage Careers.

    ERIC Educational Resources Information Center

    Bismarck State Coll., ND.

    This document outlines the curriculum plan for the one-semester vocational-technical training component of PHOENIX: A Model Program for Higher-Wage Potential Careers offered by Bismarck State College (North Dakota) which prepares and/or retrains individuals for higher-wage technical careers. The comprehensive model for the program is organized…

  19. Phoenix Robotic Arm

    NASA Technical Reports Server (NTRS)

    2007-01-01

    A vital instrument on NASA's Phoenix Mars Lander is the robotic arm, which will dig into the icy soil and bring samples back to the science deck of the spacecraft for analysis. In September 2006 at a Lockheed Martin Space Systems clean room facility near Denver, spacecraft technician Billy Jones inspects the arm during the assembly phase of the mission.

    Using the robotic arm -- built by the Jet Propulsion Laboratory, Pasadena -- the Phoenix mission will study the history of water and search for complex organic molecules in the ice-rich soil.

    The Phoenix mission is led by Principal Investigator Peter H. Smith of the University of Arizona, Tucson, with project management at NASA's Jet Propulsion Laboratory and development partnership with Lockheed Martin Space Systems. International contributions for Phoenix are provided by the Canadian Space Agency, the University of Neuchatel (Switzerland), the University of Copenhagen, and the Max Planck Institute in Germany. JPL is a division of the California Institute of Technology in Pasadena.

  20. The Phoenix Mars Mission

    NASA Technical Reports Server (NTRS)

    Tamppari, Leslie K.; Smith, Peter H.

    2008-01-01

    This slide presentation details the Phoenix Mission which was designed to enhance our understanding of water and the potential for habitability on the north polar regions of Mars. The slides show the instruments and the robotics designed to scrape Martian surface material, and analyze it in hopes of identifying water in the form of ice, and other chemicals.

  1. Phoenix Robotic Arm

    NASA Technical Reports Server (NTRS)

    2007-01-01

    A vital instrument on NASA's Phoenix Mars Lander is the robotic arm, which will dig into the icy soil and bring samples back to the science deck of the spacecraft for analysis. In September 2006 at a Lockheed Martin Space Systems clean room facility near Denver, spacecraft technician Billy Jones inspects the arm during the assembly phase of the mission.

    Using the robotic arm -- built by the Jet Propulsion Laboratory, Pasadena -- the Phoenix mission will study the history of water and search for complex organic molecules in the ice-rich soil.

    The Phoenix mission is led by Principal Investigator Peter H. Smith of the University of Arizona, Tucson, with project management at NASA's Jet Propulsion Laboratory and development partnership with Lockheed Martin Space Systems. International contributions for Phoenix are provided by the Canadian Space Agency, the University of Neuchatel (Switzerland), the University of Copenhagen, and the Max Planck Institute in Germany. JPL is a division of the California Institute of Technology in Pasadena.

  2. Phoenix Violence Prevention Initiative.

    ERIC Educational Resources Information Center

    Waits, Mary Jo; Johnson, Ryan; Silverstein, Rustin

    This report describes seven categories of violent crime in Phoenix, Arizona, and provides causes, facts, preventative programs, and lessons learned pertaining to each category of violence. The categories are: (1) prenatal and early childhood; (2) families; (3) individual youth; (4) schools; (5) neighborhood and community; (6) workplace; and (7)…

  3. The Phoenix Mars Mission

    NASA Technical Reports Server (NTRS)

    Tamppari, Leslie K.; Smith, Peter H.

    2008-01-01

    This slide presentation details the Phoenix Mission which was designed to enhance our understanding of water and the potential for habitability on the north polar regions of Mars. The slides show the instruments and the robotics designed to scrape Martian surface material, and analyze it in hopes of identifying water in the form of ice, and other chemicals.

  4. Trace gas measurements in Phoenix, Arizona (1998)

    SciTech Connect

    Nunnermacker, L.J.

    2000-01-09

    The DOE Atmospheric Chemistry Program, and the Arizona Department of Environmentel Quality (DEQ) conducted a field program in the Phoenix Metropolitan area in the late spring of 1998. The experiment was composed of a linked set of aircraft and surface measurements designed to characterize the chemical and meteorological processes leading to ozone episodes. The existing network of Arizona DEQ sites in Phoenix was utilized to document ground level concentrations of ozone and its precursors. West of the downtown area, a site (Usery Pass) was set up for the detailed characterization of the mature Phoenix urban plume. Detailed measurements in the source region were made at several sites in downtown Phoenix. The DOE G-1 aircraft, equipped wih a comprehensive array of instruments to characterize atmospheric trace gas and aerosol composition, flew over the region at various times during the day. All times in the following discussion are local standard time (LST). Morning flights were typically made between 08:00 and 12:00 upwind, to measure background concentrations, and over the Phoenix source region, to characterize the sources of ozone precursors. Afternoon flights over the Phoenix source region and downwind between 15:00 and 18:00 were made to examine the chemical properties and physical distribution of the photochemically aged urban plume. The aircraft flights typically included an atmospheric sounding to circa 3 km upwind and over Phoenix in the morning, and downwind in the afternoon. A total of 22 flights were made on 14 different days during the one month program. The motivation for conducting the program was to examine ozone formation rates and efficiencies in an environment where the pollutant mix is dominated by vehicle emissions, where the contribution of biogenic hydocarbons to ozone formation is thought to be low, and where processing conditions are different than they are in the Eastern US. The latter includes significant differences in atmospheric humidity

  5. TRACE GAS MEASUREMENTS IN PHOENIX, ARIZONA (1998).

    SciTech Connect

    NUNNERMACKER,L.J.

    2000-01-09

    The DOE Atmospheric Chemistry Program, and the Arizona Department of Environmental Quality (DEQ) conducted a field program in the Phoenix Metropolitan area in the late spring of 1998. The experiment was composed of a linked set of aircraft and surface measurements designed to characterize the chemical and meteorological processes leading to ozone episodes. The existing network of Arizona DEQ sites in Phoenix was utilized to document ground level concentrations of ozone and its precursors. West of the downtown area, a site (Usery Pass) was set up for the detailed characterization of the mature Phoenix urban plume. Detailed measurements in the source region were made at several sites in downtown Phoenix. The DOE G-1 aircraft, equipped with a comprehensive array of instruments to characterize atmospheric trace gas and aerosol composition, flew over the region at various times during the day. All times in the following discussion are local standard time (LST). Morning flights were typically made between 08:00 and 12:00 upwind, to measure background concentrations, and over the Phoenix source region, to characterize the sources of ozone precursors. Afternoon flights over the Phoenix source region and downwind between 15:00 and 18:00 were made to examine the chemical properties and physical distribution of the photochemically aged urban plume. The aircraft flights typically included an atmospheric sounding to circa 3 km upwind and over Phoenix in the morning, and downwind in the afternoon. A total of 22 flights were made on 14 different days during the one month program. The motivation for conducting the program was to examine ozone formation rates and efficiencies in an environment where the pollutant mix is dominated by vehicle emissions, where the contribution of biogenic hydrocarbons to ozone formation is thought to be low, and where processing conditions are different than they are in the Eastern US. The latter includes significant differences in atmospheric

  6. Atmospheric movies acquired at the Mars Science Laboratory landing site: Cloud morphology, frequency and significance to the Gale Crater water cycle and Phoenix mission results

    NASA Astrophysics Data System (ADS)

    Moores, John E.; Lemmon, Mark T.; Rafkin, Scot C. R.; Francis, Raymond; Pla-Garcia, Jorge; de la Torre Juárez, Manuel; Bean, Keri; Kass, David; Haberle, Robert; Newman, Claire; Mischna, Michael; Vasavada, Ashwin; Rennó, Nilton; Bell, Jim; Calef, Fred; Cantor, Bruce; Mcconnochie, Timothy H.; Harri, Ari-Matti; Genzer, Maria; Wong, Michael; Smith, Michael D.; Javier Martín-Torres, F.; Zorzano, María-Paz; Kemppinen, Osku; McCullough, Emily

    2015-05-01

    We report on the first 360 sols (LS 150° to 5°), representing just over half a Martian year, of atmospheric monitoring movies acquired using the NavCam imager from the Mars Science Laboratory (MSL) Rover Curiosity. Such movies reveal faint clouds that are difficult to discern in single images. The data set acquired was divided into two different classifications depending upon the orientation and intent of the observation. Up to sol 360, 73 Zenith movies and 79 Supra-Horizon movies have been acquired and time-variable features could be discerned in 25 of each. The data set from MSL is compared to similar observations made by the Surface Stereo Imager (SSI) onboard the Phoenix Lander and suggests a much drier environment at Gale Crater (4.6°S) during this season than was observed in Green Valley (68.2°N) as would be expected based on latitude and the global water cycle. The optical depth of the variable component of clouds seen in images with features are up to 0.047 ± 0.009 with a granularity to the features observed which averages 3.8°. MCS also observes clouds during the same period of comparable optical depth at 30 and 50 km that would suggest a cloud spacing of 2.0 to 3.3 km. Multiple motions visible in atmospheric movies support the presence of two distinct layers of clouds. At Gale Crater, these clouds are likely caused by atmospheric waves given the regular spacing of features observed in many Zenith movies and decreased spacing towards the horizon in sunset movies consistent with clouds forming at a constant elevation. Reanalysis of Phoenix data in the light of the NavCam equatorial dataset suggests that clouds may have been more frequent in the earlier portion of the Phoenix mission than was previously thought.

  7. Phoenix Mars Lander Spacecraft Heat Shield Installation

    NASA Image and Video Library

    2007-05-11

    In the Payload Hazardous Servicing Facility, the Phoenix Mars Lander spacecraft undergoes spin testing. The Phoenix mission is the first project in NASA's first openly competed program of Mars Scout missions. Phoenix will land in icy soils near the north polar permanent ice cap of Mars and explore the history of the water in these soils and any associated rocks, while monitoring polar climate. Landing is planned in May 2008 on arctic ground where a mission currently in orbit, Mars Odyssey, has detected high concentrations of ice just beneath the top layer of soil. It will serve as NASA's first exploration of a potential modern habitat on Mars and open the door to a renewed search for carbon-bearing compounds, last attempted with NASA's Viking missions in the 1970s. A stereo color camera and a weather station will study the surrounding environment while the other instruments check excavated soil samples for water, organic chemicals and conditions that could indicate whether the site was ever hospitable to life. Microscopes can reveal features as small as one one-thousandth the width of a human hair. Launch of Phoenix aboard a Delta II rocket is targeted for Aug. 3 from Cape Canaveral Air Force Station in Florida.

  8. Phoenix Mars Lander Spacecraft Heat Shield Installation

    NASA Image and Video Library

    2007-05-11

    In the Payload Hazardous Servicing Facility, technicians prepare to install the heat shield on the Phoenix Mars Lander spacecraft. The Phoenix mission is the first project in NASA's first openly competed program of Mars Scout missions. Phoenix will land in icy soils near the north polar permanent ice cap of Mars and explore the history of the water in these soils and any associated rocks, while monitoring polar climate. Landing is planned in May 2008 on arctic ground where a mission currently in orbit, Mars Odyssey, has detected high concentrations of ice just beneath the top layer of soil. It will serve as NASA's first exploration of a potential modern habitat on Mars and open the door to a renewed search for carbon-bearing compounds, last attempted with NASA's Viking missions in the 1970s. A stereo color camera and a weather station will study the surrounding environment while the other instruments check excavated soil samples for water, organic chemicals and conditions that could indicate whether the site was ever hospitable to life. Microscopes can reveal features as small as one one-thousandth the width of a human hair. Launch of Phoenix aboard a Delta II rocket is targeted for Aug. 3 from Cape Canaveral Air Force Station in Florida.

  9. Phoenix Mars Lander Spacecraft Heat Shield Installation

    NASA Image and Video Library

    2007-05-11

    In the Payload Hazardous Servicing Facility, technicians complete the installation of the heat shield on the Phoenix Mars Lander spacecraft. The Phoenix mission is the first project in NASA's first openly competed program of Mars Scout missions. Phoenix will land in icy soils near the north polar permanent ice cap of Mars and explore the history of the water in these soils and any associated rocks, while monitoring polar climate. Landing is planned in May 2008 on arctic ground where a mission currently in orbit, Mars Odyssey, has detected high concentrations of ice just beneath the top layer of soil. It will serve as NASA's first exploration of a potential modern habitat on Mars and open the door to a renewed search for carbon-bearing compounds, last attempted with NASA's Viking missions in the 1970s. A stereo color camera and a weather station will study the surrounding environment while the other instruments check excavated soil samples for water, organic chemicals and conditions that could indicate whether the site was ever hospitable to life. Microscopes can reveal features as small as one one-thousandth the width of a human hair. Launch of Phoenix aboard a Delta II rocket is targeted for Aug. 3 from Cape Canaveral Air Force Station in Florida.

  10. Phoenix Mars Lander Spacecraft Heat Shield Installation

    NASA Image and Video Library

    2007-05-11

    In the Payload Hazardous Servicing Facility, technicians install the heat shield on the Phoenix Mars Lander spacecraft. The Phoenix mission is the first project in NASA's first openly competed program of Mars Scout missions. Phoenix will land in icy soils near the north polar permanent ice cap of Mars and explore the history of the water in these soils and any associated rocks, while monitoring polar climate. Landing is planned in May 2008 on arctic ground where a mission currently in orbit, Mars Odyssey, has detected high concentrations of ice just beneath the top layer of soil. It will serve as NASA's first exploration of a potential modern habitat on Mars and open the door to a renewed search for carbon-bearing compounds, last attempted with NASA's Viking missions in the 1970s. A stereo color camera and a weather station will study the surrounding environment while the other instruments check excavated soil samples for water, organic chemicals and conditions that could indicate whether the site was ever hospitable to life. Microscopes can reveal features as small as one one-thousandth the width of a human hair. Launch of Phoenix aboard a Delta II rocket is targeted for Aug. 3 from Cape Canaveral Air Force Station in Florida.

  11. Phoenix Mars Lander Spacecraft Heat Shield Installation

    NASA Image and Video Library

    2007-05-11

    In the Payload Hazardous Servicing Facility, the heat shield for the Phoenix Mars Lander is moved into position for installation on the spacecraft. The Phoenix mission is the first project in NASA's first openly competed program of Mars Scout missions. Phoenix will land in icy soils near the north polar permanent ice cap of Mars and explore the history of the water in these soils and any associated rocks, while monitoring polar climate. Landing is planned in May 2008 on arctic ground where a mission currently in orbit, Mars Odyssey, has detected high concentrations of ice just beneath the top layer of soil. It will serve as NASA's first exploration of a potential modern habitat on Mars and open the door to a renewed search for carbon-bearing compounds, last attempted with NASA's Viking missions in the 1970s. A stereo color camera and a weather station will study the surrounding environment while the other instruments check excavated soil samples for water, organic chemicals and conditions that could indicate whether the site was ever hospitable to life. Microscopes can reveal features as small as one one-thousandth the width of a human hair. Launch of Phoenix aboard a Delta II rocket is targeted for Aug. 3 from Cape Canaveral Air Force Station in Florida.

  12. Phoenix's 'Dodo' Trench

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This image was taken by NASA's Phoenix Mars Lander's Robotic Arm Camera (RAC) on the ninth Martian day of the mission, or Sol 9 (June 3, 2008). The center of the image shows a trench informally called 'Dodo' after the second dig. 'Dodo' is located within the previously determined digging area, informally called 'Knave of Hearts.' The light square to the right of the trench is the Robotic Arm's Thermal and Electrical Conductivity Probe (TECP). The Robotic Arm has scraped to a bright surface which indicated the Arm has reached a solid structure underneath the surface, which has been seen in other images as well.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  13. Phoenix's La Mancha Trench

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This false color image, taken by NASA's Phoenix Mars Lander's Surface Stereo Imager, was taken on the 131st Martian day, or sol, of the mission (Oct. 7, 2008). The image shows color variations of the trench, informally named 'La Mancha,' and reveals the ice layer beneath the soil surface. The trench's depth is about 5 centimeters deep.

    The color outline of the shadow at the bottom of the image is a result of sun movement with the combined use of infrared, green, and blue filters.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  14. Underneath the Phoenix Lander

    NASA Technical Reports Server (NTRS)

    2008-01-01

    The Robotic Arm Camera on NASA's Phoenix Mars Lander took this image on Oct. 18, 2008, during the 142nd Martian day, or sol, since landing. The flat patch in the center of the image has the informal name 'Holy Cow,' based on researchers' reaction when they saw the initial image of it only a few days after the May 25, 2008 landing. Researchers first saw this flat patch in an image taken by the Robotic Arm Camera on May 30, the fifth Martian day of the mission.

    The Phoenix mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  15. Underneath the Phoenix Lander

    NASA Technical Reports Server (NTRS)

    2008-01-01

    The Robotic Arm Camera on NASA's Phoenix Mars Lander took this image on Oct. 18, 2008, during the 142nd Martian day, or sol, since landing. The flat patch in the center of the image has the informal name 'Holy Cow,' based on researchers' reaction when they saw the initial image of it only a few days after the May 25, 2008 landing. Researchers first saw this flat patch in an image taken by the Robotic Arm Camera on May 30, the fifth Martian day of the mission.

    The Phoenix mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  16. Phoenix's Wet Chemistry Laboratory Units

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This image shows four Wet Chemistry Laboratory units, part of the Microscopy, Electrochemistry, and Conductivity Analyzer (MECA) instrument on board NASA's Phoenix Mars Lander. This image was taken before Phoenix's launch on August 4, 2007.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  17. Phoenix's Wet Chemistry Laboratory Units

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This image shows four Wet Chemistry Laboratory units, part of the Microscopy, Electrochemistry, and Conductivity Analyzer (MECA) instrument on board NASA's Phoenix Mars Lander. This image was taken before Phoenix's launch on August 4, 2007.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  18. Phoenix, AZ, USA

    NASA Image and Video Library

    1973-06-22

    SL2-03-200 (22 June 1973) --- The city of Phoenix, AZ (33.5N, 112.0W) can be seen in good detail in this color infrared scene. Situated among truck crop agriculture fields, the color infrared photo depicts the vegetated fields as shades of red making the agriculture stand out in this desert environment. To the east, Lake Theodore Roosevelt and dam can be easily seen. Photo credit: NASA

  19. Phoenix Opens its Eyes

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This image, one of the first captured by NASA's Phoenix Mars Lander, shows the vast plains of the northern polar region of Mars. The flat landscape is strewn with tiny pebbles and shows polygonal cracking, a pattern seen widely in Martian high latitudes and also observed in permafrost terrains on Earth. The polygonal cracking is believed to have resulted from seasonal contraction and expansion of surface ice.

    Phoenix touched down on the Red Planet at 4:53 p.m. Pacific Time (7:53 p.m. Eastern Time), May 25, 2008, in an arctic region called Vastitas Borealis, at 68 degrees north latitude, 234 degrees east longitude.

    This is an approximate-color image taken shortly after landing by the spacecraft's Surface Stereo Imager, inferred from two color filters, a violet, 450-nanometer filter and an infrared, 750-nanometer filter.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  20. Phoenix Opens its Eyes

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This image, one of the first captured by NASA's Phoenix Mars Lander, shows the vast plains of the northern polar region of Mars. The flat landscape is strewn with tiny pebbles and shows polygonal cracking, a pattern seen widely in Martian high latitudes and also observed in permafrost terrains on Earth. The polygonal cracking is believed to have resulted from seasonal contraction and expansion of surface ice.

    Phoenix touched down on the Red Planet at 4:53 p.m. Pacific Time (7:53 p.m. Eastern Time), May 25, 2008, in an arctic region called Vastitas Borealis, at 68 degrees north latitude, 234 degrees east longitude.

    This is an approximate-color image taken shortly after landing by the spacecraft's Surface Stereo Imager, inferred from two color filters, a violet, 450-nanometer filter and an infrared, 750-nanometer filter.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  1. Telecommunications Relay Support of the Mars Phoenix Lander Mission

    NASA Technical Reports Server (NTRS)

    Edwards, Charles D., Jr.; Erickson, James K.; Gladden, Roy E.; Guinn, Joseph R.; Ilott, Peter A.; Jai, Benhan; Johnston, Martin D.; Kornfeld, Richard P.; Martin-Mur, Tomas J.; McSmith, Gaylon W.; hide

    2010-01-01

    The Phoenix Lander, first of NASA's Mars Scout missions, arrived at the Red Planet on May 25, 2008. From the moment the lander separated from its interplanetary cruise stage shortly before entry, the spacecraft could no longer communicate directly with Earth, and was instead entirely dependent on UHF relay communications via an international network of orbiting Mars spacecraft, including NASA's 2001 Mars Odyssey (ODY) and Mars Reconnaissance Orbiter (MRO) spacecraft, as well as ESA's Mars Express (MEX) spacecraft. All three orbiters captured critical event telemetry and/or tracking data during Phoenix Entry, Descent and Landing. During the Phoenix surface mission, ODY and MRO provided command and telemetry services, far surpassing the original data return requirements. The availability of MEX as a backup relay asset enhanced the robustness of the surface relay plan. In addition to telecommunications services, Doppler tracking observables acquired on the UHF link yielded an accurate position for the Phoenix landing site.

  2. Telecommunications Relay Support of the Mars Phoenix Lander Mission

    NASA Technical Reports Server (NTRS)

    Edwards, Charles D., Jr.; Erickson, James K.; Gladden, Roy E.; Guinn, Joseph R.; Ilott, Peter A.; Jai, Benhan; Johnston, Martin D.; Kornfeld, Richard P.; Martin-Mur, Tomas J.; McSmith, Gaylon W.; Thomas, Reid C.; Varghese, Phil; Signori, Gina; Schmitz, Peter

    2010-01-01

    The Phoenix Lander, first of NASA's Mars Scout missions, arrived at the Red Planet on May 25, 2008. From the moment the lander separated from its interplanetary cruise stage shortly before entry, the spacecraft could no longer communicate directly with Earth, and was instead entirely dependent on UHF relay communications via an international network of orbiting Mars spacecraft, including NASA's 2001 Mars Odyssey (ODY) and Mars Reconnaissance Orbiter (MRO) spacecraft, as well as ESA's Mars Express (MEX) spacecraft. All three orbiters captured critical event telemetry and/or tracking data during Phoenix Entry, Descent and Landing. During the Phoenix surface mission, ODY and MRO provided command and telemetry services, far surpassing the original data return requirements. The availability of MEX as a backup relay asset enhanced the robustness of the surface relay plan. In addition to telecommunications services, Doppler tracking observables acquired on the UHF link yielded an accurate position for the Phoenix landing site.

  3. Assessing Habitability: Lessons from the Phoenix Mission

    NASA Technical Reports Server (NTRS)

    Stoker, Carol R.

    2013-01-01

    The Phoenix mission's key objective was to search for a habitable zone. The Phoenix lander carried a robotic arm with digging scoop to collect soil and icy material for analysis with an instrument payload that included volatile mineral and organic analysis(3) and soil ionic chemistry analysis (4). Results from Phoenix along with theoretical modeling and other previous mission results were used to evaluate the habitability of the landing site by considering four factors that characterize the environments ability to support life as we know it: the presence of liquid water, the presence of an energy source to support metabolism, the presence of nutrients containing the fundamental building blocks of life, and the absence of environmental conditions that are toxic to or preclude life. Phoenix observational evidence for the presence of liquid water (past or present) includes clean segregated ice, chemical etching of soil grains, calcite minerals in the soil and variable concentrations of soluble salts5. The maximum surface temperature measured was 260K so unfrozen water can form only in adsorbed films or saline brines but warmer climates occur cyclically on geologically short time scales due to variations in orbital parameters. During high obliquity periods, temperatures allowing metabolism extend nearly a meter into the subsurface. Phoenix discovered 1%w/w perchlorate salt in the soil, a chemical energy source utilized by a wide range of microbes. Nutrient sources including C, H, N, O, P and S compounds are supplied by known atmospheric sources or global dust. Environmental conditions are within growth tolerance for terrestrial microbes. Summer daytime temperatures are sufficient for metabolic activity, the pH is 7.8 and is well buffered and the projected water activity of a wet soil will allow growth. In summary, martian permafrost in the north polar region is a viable location for modern life. Stoker et al. presented a formalism for comparing the habitability of

  4. Soil Fills Phoenix Laboratory Cell

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This image shows four of the eight cells in the Thermal and Evolved-Gas Analyzer, or TEGA, on NASA's Phoenix Mars Lander. TEGA's ovens, located underneath the cells, heat soil samples so the released gases can be analyzed.

    Left to right, the cells are numbered 7, 6, 5 and 4. Phoenix's Robotic Arm delivered soil most recently to cell 6 on the 137th Martian day, or sol, of the mission (Oct. 13, 2008).

    Phoenix's Robotic Arm Camera took this image at 3:03 p.m. local solar time on Sol 138 (Oct. 14, 2008).

    Phoenix landed on Mars' northern plains on May 25, 2008.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  5. How Phoenix Creates Color Images (Animation)

    NASA Technical Reports Server (NTRS)

    2008-01-01

    [figure removed for brevity, see original site] Click on image for animation

    This simple animation shows how a color image is made from images taken by Phoenix.

    The Surface Stereo Imager captures the same scene with three different filters. The images are sent to Earth in black and white and the color is added by mission scientists.

    By contrast, consumer digital cameras and cell phones have filters built in and do all of the color processing within the camera itself.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASAaE(TM)s Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  6. How Phoenix Creates Color Images (Animation)

    NASA Technical Reports Server (NTRS)

    2008-01-01

    [figure removed for brevity, see original site] Click on image for animation

    This simple animation shows how a color image is made from images taken by Phoenix.

    The Surface Stereo Imager captures the same scene with three different filters. The images are sent to Earth in black and white and the color is added by mission scientists.

    By contrast, consumer digital cameras and cell phones have filters built in and do all of the color processing within the camera itself.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASAaE(TM)s Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  7. Phoenix's Laser Beam in Action on Mars

    NASA Technical Reports Server (NTRS)

    2008-01-01

    [figure removed for brevity, see original site] Click on image to view the animation

    The Surface Stereo Imager camera aboard NASA's Phoenix Mars Lander acquired a series of images of the laser beam in the Martian night sky. Bright spots in the beam are reflections from ice crystals in the low level ice-fog. The brighter area at the top of the beam is due to enhanced scattering of the laser light in a cloud. The Canadian-built lidar instrument emits pulses of laser light and records what is scattered back.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  8. Wind-Related Topography in Phoenix's Region of Mars (Animation)

    NASA Technical Reports Server (NTRS)

    2008-01-01

    [figure removed for brevity, see original site] Click on image for animation

    This movie shifts from a global zoom indicating the Phoenix landing area on Mars to a topographical map indicating relative elevations in the landing region. The elevations could affect wind patterns at the site.

    In particular, Phoenix is in a broad, shallow valley. The edge of the valley, about 150 meters (500 feet) above the floor, may provide enough of a slope to the east of Phoenix to explain winds coming from the east during nights at the site. Cooler, denser air could be sinking down the slope and toward the lander.

    Atmospheric scientists on the Phoenix team are analyzing wind patterns to distiguish effects of nearby topography from larger-scale movement of the atmosphere in the polar region.

    The elevation information for this topographical mapping comes from the Mars Orbiter Laser Altimeter on NASA's Mars Global Surveyor orbiter. The blue-coded area is the valley floor. Orange and yellow indicate relatively higher elevations.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver. JPL managed the Mars Global Surveyor mission for the NASA Science Mission Directorate.

  9. Wind-Related Topography in Phoenix's Region of Mars (Animation)

    NASA Technical Reports Server (NTRS)

    2008-01-01

    [figure removed for brevity, see original site] Click on image for animation

    This movie shifts from a global zoom indicating the Phoenix landing area on Mars to a topographical map indicating relative elevations in the landing region. The elevations could affect wind patterns at the site.

    In particular, Phoenix is in a broad, shallow valley. The edge of the valley, about 150 meters (500 feet) above the floor, may provide enough of a slope to the east of Phoenix to explain winds coming from the east during nights at the site. Cooler, denser air could be sinking down the slope and toward the lander.

    Atmospheric scientists on the Phoenix team are analyzing wind patterns to distiguish effects of nearby topography from larger-scale movement of the atmosphere in the polar region.

    The elevation information for this topographical mapping comes from the Mars Orbiter Laser Altimeter on NASA's Mars Global Surveyor orbiter. The blue-coded area is the valley floor. Orange and yellow indicate relatively higher elevations.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver. JPL managed the Mars Global Surveyor mission for the NASA Science Mission Directorate.

  10. Phoenix Checks out its Work Area

    NASA Technical Reports Server (NTRS)

    2008-01-01

    [figure removed for brevity, see original site] Click on image for animation

    This animation shows a mosaic of images of the workspace reachable by the scoop on the robotic arm of NASA's Phoenix Mars Lander, along with some measurements of rock sizes.

    Phoenix was able to determine the size of the rocks based on three-dimensional views from stereoscopic images taken by the lander's 7-foot mast camera, called the Surface Stereo Imager. The stereo pair of images enable depth perception, much the way a pair of human eyes enable people to gauge the distance to nearby objects.

    The rock measurements were made by a visualization tool known as Viz, developed at NASA's Ames Research Laboratory. The shadow cast by the camera on the Martian surface appears somewhat disjointed because the camera took the images in the mosaic at different times of day.

    Scientists do not yet know the origin or composition of the flat, light-colored rocks on the surface in front of the lander.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  11. 'Dodo-Goldilocks' Trench Dug by Phoenix

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This color image was acquired by NASA's Phoenix Mars Lander's Surface Stereo Imager on the 19th day of the mission, or Sol 19 (June 13, 2008), after the May 25, 2008, landing. This image shows one trench informally called 'Dodo-Goldilocks' after two digs (dug on Sol 18, or June 12, 2008) by Phoenix's Robotic Arm. The trench is 22 centimeters (8.7 inches) wide and 35 centimeters (13.8 inches) long. At its deepest point, the trench is 7 to 8 centimeters (2.7 to 3 inches) deep.

    White material, possibly ice, is located only at the upper portion of the trench, indicating that it is not continuous throughout the excavated site. According to scientists, the trench might be exposing a ledge, or only a portion of a slab, of the white material.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  12. Zenith Movie showing Phoenix's Lidar Beam (Animation)

    NASA Technical Reports Server (NTRS)

    2008-01-01

    [figure removed for brevity, see original site] Click on image for animation

    A laser beam from the Canadian-built lidar instrument on NASA's Phoenix Mars Lander can be seen in this contrast-enhanced sequence of 10 images taken by Phoenix's Surface Stereo Imager on July 26, 2008, during early Martian morning hours of the mission's 61st Martian day after landing.

    The view is almost straight up and includes about 1.5 kilometer (about 1 mile) of the length of the beam. The camera, from its position close to the lidar on the lander deck, took the images through a green filter centered on light with wavelength 532 nanometers, the same wavelength of the laser beam. The movie has been artificially colored to to approximately match the color that would be seen looking through this filter on Mars. Contrast is enhanced to make the beam more visible.

    The lidar beam can be seen extending from the lower right to the upper right, near the zenith, as it reflects off particles suspended in the atmosphere. Particles that scatter the beam directly into the camera can be seen to produce brief sparkles of light. In the background, dust can be seen drifting across the sky pushed by winds aloft.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  13. Zenith Movie showing Phoenix's Lidar Beam (Animation)

    NASA Technical Reports Server (NTRS)

    2008-01-01

    [figure removed for brevity, see original site] Click on image for animation

    A laser beam from the Canadian-built lidar instrument on NASA's Phoenix Mars Lander can be seen in this contrast-enhanced sequence of 10 images taken by Phoenix's Surface Stereo Imager on July 26, 2008, during early Martian morning hours of the mission's 61st Martian day after landing.

    The view is almost straight up and includes about 1.5 kilometer (about 1 mile) of the length of the beam. The camera, from its position close to the lidar on the lander deck, took the images through a green filter centered on light with wavelength 532 nanometers, the same wavelength of the laser beam. The movie has been artificially colored to to approximately match the color that would be seen looking through this filter on Mars. Contrast is enhanced to make the beam more visible.

    The lidar beam can be seen extending from the lower right to the upper right, near the zenith, as it reflects off particles suspended in the atmosphere. Particles that scatter the beam directly into the camera can be seen to produce brief sparkles of light. In the background, dust can be seen drifting across the sky pushed by winds aloft.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  14. Phoenix `07 MET Pressure sensor: Instrument

    NASA Astrophysics Data System (ADS)

    Polkko, J.; Kahanpää, H.; Harri, A.-M.; Schmidt, W.; Genzer, M.; Mäkelä, M.; Savijarvi, H.; Kauhanen, J.

    2008-09-01

    Abstract The Phoenix '07 Lander landed successfully on the Martian northern polar region 25.5.2008. The mission is part of the National Aeronautics and Space Administration's (NASA's) Scout program. The seminal questions for the Phoenix mission are: (1) can the Martian arctic support life, (2) what is the history of water at the landing site, and (3) how is the Martian climate affected by polar dynamics. These translate into practical science goals and tasks of characterizing the surface, analyzing samples of the soil and ice, and to observing and monitoring the atmospheric conditions and phenomena. Meteorology experiment (MET) onboard the Phoenix '07 lander will provide the first surface based observations of atmospheric pressure, temperature and wind in the Martian polar region above the polar circle. The MET instrument also includes a lidar for detecting dust and ice particles in the air column above the lander. Pressure observations are crucial for the success of the MET experiment. The Martian atmosphere goes through a large scale atmospheric pressure cycle due to the annual condensation and sublimation of the atmospheric carbon dioxide. Pressure also exhibits short period variations associated with dust storms, tides and other atmospheric events. A series of pressure measurements can hence tell us about the large scale state and dynamics of the atmosphere. The shorter time scale phenomena are also important in contributing to our understanding of mixing and transport of heat, dust and water vapour. The pressure observations are performed by a FMI (Finnish Meteorological Institute) instrument, based on micro machined Barocap capacitic pressure sensor heads manufactured by Vaisala Inc. Similar instruments have been used in several earlier missions (Mars-96, Mars Polar Lander, Beagle-2 and Huygens), Phoenix being the first successful landing on Mars. A similar instrument is included also in the Mars Science Laboratory '09 rover. Pressure sensor technology

  15. Animation of Panorama of Phoenix's Solar Panel and Robotic Arm

    NASA Technical Reports Server (NTRS)

    2008-01-01

    [figure removed for brevity, see original site] Click on image for animation

    This is an animation of panorama images of NASA's Phoenix Mars Lander's solar panel and the lander's Robotic Arm with a sample in the scoop. The image was taken just before the sample was delivered to the Optical Microscope.

    The images making up this animation were taken by the lander's Surface Stereo Imager looking west during Phoenix's Sol 16 (June 10, 2008), or the 16th Martian day after landing. This view is a part of the 'mission success' panorama that will show the whole landing site in color.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  16. Animation of Panorama of Phoenix's Solar Panel and Robotic Arm

    NASA Technical Reports Server (NTRS)

    2008-01-01

    [figure removed for brevity, see original site] Click on image for animation

    This is an animation of panorama images of NASA's Phoenix Mars Lander's solar panel and the lander's Robotic Arm with a sample in the scoop. The image was taken just before the sample was delivered to the Optical Microscope.

    The images making up this animation were taken by the lander's Surface Stereo Imager looking west during Phoenix's Sol 16 (June 10, 2008), or the 16th Martian day after landing. This view is a part of the 'mission success' panorama that will show the whole landing site in color.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  17. Phoenix Dodo Trench

    NASA Image and Video Library

    2008-06-04

    This image was taken by NASA's Phoenix Mars Lander's Robotic Arm Camera (RAC) on the ninth Martian day of the mission, or Sol 9 (June 3, 2008). The center of the image shows a trench informally called "Dodo" after the second dig. "Dodo" is located within the previously determined digging area, informally called "Knave of Hearts." The light square to the right of the trench is the Robotic Arm's Thermal and Electrical Conductivity Probe (TECP). The Robotic Arm has scraped to a bright surface which indicated the Arm has reached a solid structure underneath the surface, which has been seen in other images as well. http://photojournal.jpl.nasa.gov/catalog/PIA10763

  18. Animation of Phoenix Wrist Unlatching

    NASA Image and Video Library

    2008-05-29

    This image shows what happened underneath NASA Phoenix Mars Lander Robotic Arm wrist on Sol 3. The pin that goes through the loop is what holds the wrist in place. The rotation of the wrist pops the pin free.

  19. Greening America's Capitals - Phoenix, AZ

    EPA Pesticide Factsheets

    This report shows design concepts to make pedestrians and bicyclists safer while maintaining on-street parking and providing space for a future streetcar or trolley in Phoenix, AZ. It also shows green infrastructure strategies for arid places.

  20. Phoenix Lander on Mars Stereo

    NASA Image and Video Library

    2007-05-10

    NASA Phoenix Mars Lander monitors the atmosphere overhead and reaches out to the soil below in this stereo illustration of the spacecraft fully deployed on the surface of Mars. 3D glasses are necessary to view this image.

  1. Images from Phoenix's MECA Instruments

    NASA Technical Reports Server (NTRS)

    2008-01-01

    The image on the upper left is from NASA's Phoenix Mars Lander's Optical Microscope after a sample informally called 'Sorceress' was delivered to its silicon substrate on the 38th Martian day, or sol, of the mission (July 2, 2008).

    A 3D representation of the same sample is on the right, as seen by Phoenix's Atomic Force Microscope. This is 100 times greater magnification than the view from the Optical Microscope, and the most highly magnified image ever seen from another world.

    The Optical Microscope and the Atomic Force Microscope are part of Phoenix's Microscopy, Electrochemistry and Conductivity Analyzer instrument.

    The Atomic Force Microscope was developed by a Swiss-led consortium in collaboration with Imperial College London.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  2. How Phoenix Looks Under Itself

    NASA Image and Video Library

    2008-06-04

    NASA Phoenix Mars Lander reaching with its Robotic Arm and taking a picture of the surface underneath the lander. The light feature in the middle of the image below the leg is informally called Holy Cow.

  3. Animation of the Phoenix Cluster

    NASA Image and Video Library

    This animation shows how large numbers of stars form in the Phoenix Cluster. It begins by showing several galaxies in the cluster and hot gas (in red). This hot gas contains more normal matter than...

  4. Animation of Phoenix's Wrist Unlatching

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This animation shows what happened underneath Phoenix's Robotic Arm wrist on Sol 3. The pin that goes through the loop is what holds the wrist in place. The rotation of the wrist pops the pin free.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  5. Phoenix Telemetry Processor

    NASA Technical Reports Server (NTRS)

    Stanboli, Alice

    2013-01-01

    Phxtelemproc is a C/C++ based telemetry processing program that processes SFDU telemetry packets from the Telemetry Data System (TDS). It generates Experiment Data Records (EDRs) for several instruments including surface stereo imager (SSI); robotic arm camera (RAC); robotic arm (RA); microscopy, electrochemistry, and conductivity analyzer (MECA); and the optical microscope (OM). It processes both uncompressed and compressed telemetry, and incorporates unique subroutines for the following compression algorithms: JPEG Arithmetic, JPEG Huffman, Rice, LUT3, RA, and SX4. This program was in the critical path for the daily command cycle of the Phoenix mission. The products generated by this program were part of the RA commanding process, as well as the SSI, RAC, OM, and MECA image and science analysis process. Its output products were used to advance science of the near polar regions of Mars, and were used to prove that water is found in abundance there. Phxtelemproc is part of the MIPL (Multi-mission Image Processing Laboratory) system. This software produced Level 1 products used to analyze images returned by in situ spacecraft. It ultimately assisted in operations, planning, commanding, science, and outreach.

  6. Comparing Baltimore and Phoenix

    NASA Technical Reports Server (NTRS)

    2002-01-01

    The 'zoom lens' aboard NASA's Terra spacecraft acquired these views of two U.S. cities: Baltimore, Maryland (left), and Phoenix, Arizona (right). Acquired by the Advanced Spaceborne Thermal Emission and Reflection Radiometer (ASTER), red in these false-colored images indicates vegetation. The turquoise pixels show paved areas while darker greens and browns show bare earth and rock surfaces. The 'true' constructed nature of these cities is not easy to see. Ecologists now accept human beings and our activities as a significant factor in studying the Earth's ecology. ASTER data are being used to better understand urban ecology, in particular how humans build their cities and affect the surrounding environment. At the recent American Geophysical Union (AGU) meeting in Boston, Will Stefanov of Arizona State University presented the first set of ASTER images of the urban 'skeletons' of the amount of built structures in twelve cities around the world. He also discussed the Urban Environmental Monitoring project, in which scientists are examining 100 urban centers to look for common features (or lack of them) in global city structure as well as to monitor their changes over time.

  7. Martian Surface as Seen by Phoenix

    NASA Image and Video Library

    2008-07-28

    This anaglyph was acquired by NASA Phoenix Lander; in the bottom left is a trench dug by Phoenix Robotic Arm. In the bottom right is one of Phoenix two solar panels. You will need 3-D glasses to view this image.

  8. Site Investigation Report. 161st Air Refueling Group, Arizona National Guard, Sky Harbor International Airport and Papago Military Reservation, Phoenix, Arizona. Volume 1. Report, Tables and Figures

    DTIC Science & Technology

    1992-11-01

    Site 5. Ammunition Dumo SI activities consisted of conducting geophysical surveys to ascertain the location of suspected historical ammunition disposal...the Toxic Substances Control Act (TSCA), the Safe Drinking Water Act (SDWA) , the Clean Air Act (CAA), the Clean Water Act (CV;7A), and the Marine ...Treaty Acv Federal Insecticide, Fungi’:ide, 3nd Rodenticide Acc Wild and Scenic Rivers Act Clean Air Act M4arine Mammal Protection Act Marine

  9. Discovering Diversity Downtown: Questioning Phoenix

    ERIC Educational Resources Information Center

    Talmage, Craig A.; Dombrowski, Rosemarie; Pstross, Mikulas; Peterson, C. Bjørn; Knopf, Richard C.

    2015-01-01

    Applied community learning experiences for university students are promising endeavors in downtown urban environments. Past research is applied to help better comprehend a community engagement initiative conducted in downtown Phoenix, Arizona. The initiative aimed to illuminate the socio-cultural diversity of the downtown area utilizing…

  10. Floral development in Phoenix dactylifera

    Treesearch

    Darleen A. De Mason; Kenneth W. Stolte; Brent Tisserat

    1982-01-01

    Inflorescence primordia in the date palm (Phoenix dactylifera L.) differentiate within axillary buds in November in the Coachella Valley, California. The rachillae are initiated as small mounds without subtending bracts on the flattened apex of the rachis and are enclosed by the prophyll. A single bract subtends each flower primordium. Flower...

  11. Phoenix Mars Lander in Testing

    NASA Technical Reports Server (NTRS)

    2006-01-01

    NASA's next Mars-bound spacecraft, the Phoenix Mars Lander, was partway through assembly and testing at Lockheed Martin Space Systems, Denver, in September 2006, progressing toward an August 2007 launch from Florida. In this photograph, spacecraft specialists work on the lander after its fan-like circular solar arrays have been spread open for testing. The arrays will be in this configuration when the spacecraft is active on the surface of Mars.

    Phoenix will land in icy soils near the north polar permanent ice cap of Mars and explore the history of the water in these soils and any associated rocks, while monitoring polar climate. It will dig into the surface, test scooped-up samples for carbon-bearing compounds and serve as NASA's first exploration of a potential modern habitat on Mars.

    Phoenix mission is led by Principal Investigator Peter H. Smith of the University of Arizona, Tucson, with project management at NASA's Jet Propulsion Laboratory and development partnership with Lockheed Martin Space Systems. International contributions for Phoenix are provided by the Canadian Space Agency, the University of Neuchatel (Switzerland), the University of Copenhagen, and the Max Planck Institute in Germany. JPL is a division of the California Institute of Technology in Pasadena.

  12. View - Phoenix, AZ - Metropolitan Area - AZ

    NASA Image and Video Library

    1973-08-15

    S73-35078 (July-Sept. 1973) --- A nearly vertical view of the Phoenix, Arizona metropolitan area is seen in this Skylab 3 (second manning) Earth Resources Experiments Package S190-B (five-inch Earth terrain camera) photograph taken from the Skylab space station in Earth orbit. Also in the picture are Scottsdale, Paradise Valley, Tempe, Mesa, Komatke, Salt River Indian Reservation and part of the Gila River Indian Reservation. Features which can be delineated from the photograph include: cultural patterns defined by commercial, industrial, agricultural and residential areas; transportation networks consisting of major corridors, primary, secondary and feeder streets; major urban developments in the area such as airports, Squaw Peak City Park, Turf Paradise Race Track and the State Fairgrounds. Phoenix is one of the 27 census cities of interest under study by the U.S. Geological Survey and is the center of the Arizona Regional Ecological Test Site. A large number of investigators will be using the Skylab data. This photo will be compared to earlier ones to document changes in the urban area with time. The landscape is well defined in terms of mountains, alluvial fans and river flood plains. Several different types of natural vegetation and irrigated crop lands can be mapped. Geological features are not well displayed but mining activities are readily identified. Photo credit: NASA

  13. Vertical Distribution of Water at Phoenix

    NASA Technical Reports Server (NTRS)

    Tamppari, L. K.; Lemmon, M. T.

    2011-01-01

    Phoenix results, combined with coordinated observations from the Mars Reconnaissance Orbiter of the Phoenix lander site, indicate that the water vapor is nonuniform (i.e., not well mixed) up to a calculated cloud condensation level. It is important to understand the mixing profile of water vapor because (a) the assumption of a well-mixed atmosphere up to a cloud condensation level is common in retrievals of column water abundances which are in turn used to understand the seasonal and interannual behavior of water, (b) there is a long history of observations and modeling that conclude both that water vapor is and is not well-mixed, and some studies indicate that the water vapor vertical mixing profile may, in fact, change with season and location, (c) the water vapor in the lowest part of the atmosphere is the reservoir that can exchange with the regolith and higher amounts may have an impact on the surface chemistry, and (d) greater water vapor abundances close to the surface may enhance surface exchange thereby reducing regional transport, which in turn has implications to the net transport of water vapor over seasonal and annual timescales.

  14. Schematic Animation of Phoenix's Microscope Station

    NASA Technical Reports Server (NTRS)

    2008-01-01

    [figure removed for brevity, see original site] Click on image for animation

    This animation shows the workings of the microscope station of the Microscopy, Electrochemistry and Conductivity Analyzer (MECA) instrument suite of NASA's Phoenix Mars Lander.

    Samples are delivered to the horizontal portion of the sample wheel (yellow) that pokes outside an opening in the box enclosure. The wheel rotates to present the sample to the microscopes. The Optical Microscope (red) can see particles a little smaller than one-tenth the diameter of a human hair. The Atomic Force Microscope (pink) can see particles forty time smaller. The samples are on a variety of substrate surfaces, the small circles on the beveled edge of the sample wheel. For scale, the diameter of the wheel is about 14 centimeters (5.5 inches). Each substrate is a circle 3 millimeters (0.1 inch) in diameter.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  15. Phoenix Scoop Inverted Showing Rasp

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This image taken by the Surface Stereo Imager on Sol 49, or the 49th Martian day of the mission (July 14, 2008), shows the silver colored rasp protruding from NASA's Phoenix Mars Lander's Robotic Arm scoop. The scoop is inverted and the rasp is pointing up.

    Shown with its forks pointing toward the ground is the thermal and electrical conductivity probe, at the lower right. The Robotic Arm Camera is pointed toward the ground.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is led by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  16. Phoenix Deepens Trenches on Mars

    NASA Technical Reports Server (NTRS)

    2008-01-01

    The Surface Stereo Imager on NASA's Phoenix Mars Lander took this false color image on Oct. 21, 2008, during the 145th Martian day, or sol, since landing. The white areas seen in these trenches are part of an ice layer beneath the soil.

    The trench on the upper left, called 'Upper Cupboard,' is about 60 centimeters (24 inches) long and 3 centimeters (1 inch) deep. The trench in the middle, called 'Ice Man,' is about 30 centimeters (12 inches) long and 3 centimeters (1 inch) deep. The trench on the right, called 'La Mancha,' is about 31 centimeters (12 inches) and 5 centimeters (2 inches) deep.

    The Phoenix mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  17. Phoenix Deepens Trenches on Mars

    NASA Technical Reports Server (NTRS)

    2008-01-01

    The Surface Stereo Imager on NASA's Phoenix Mars Lander took this false color image on Oct. 21, 2008, during the 145th Martian day, or sol, since landing. The bluish-white areas seen in these trenches are part of an ice layer beneath the soil.

    The trench on the upper left, called 'Dodo-Goldilocks,' is about 38 centimeters (15 inches) long and 4 centimeters (1.5 inches) deep. The trench on the right, called 'Upper Cupboard,' is about 60 centimeters (24 inches) long and 3 centimeters (1 inch) deep. The trench in the lower middle is called 'Stone Soup.'

    The Phoenix mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  18. Working End of Robotic Arm on Phoenix

    NASA Technical Reports Server (NTRS)

    2007-01-01

    [figure removed for brevity, see original site] Annotated Version

    This illustration shows some of the components on and near the end of the robotic arm on NASA's Phoenix Mars Lander. Primary and secondary blades on the scoop will aid in the collection of soil samples. A powered rasp will allow the arm to sample an icy layer expected to be about as hard as concrete. The thermal and electrical conductivity probe, which is one part of the Microscopy, Electrochemistry and Conductivity Analyzer, will assess how heat and electrons move through the soil from one spike to another of a four-spike electronic fork that will be pushed into the soil at different stages of digging by the arm.

  19. Working End of Robotic Arm on Phoenix

    NASA Technical Reports Server (NTRS)

    2007-01-01

    [figure removed for brevity, see original site] Annotated Version

    This illustration shows some of the components on and near the end of the robotic arm on NASA's Phoenix Mars Lander. Primary and secondary blades on the scoop will aid in the collection of soil samples. A powered rasp will allow the arm to sample an icy layer expected to be about as hard as concrete. The thermal and electrical conductivity probe, which is one part of the Microscopy, Electrochemistry and Conductivity Analyzer, will assess how heat and electrons move through the soil from one spike to another of a four-spike electronic fork that will be pushed into the soil at different stages of digging by the arm.

  20. Images from Phoenix's MECA Instruments

    NASA Technical Reports Server (NTRS)

    2008-01-01

    The image on the upper left is from NASA's Phoenix Mars Lander's Optical Microscope after a sample informally called 'Sorceress' was delivered to its silicon substrate on the 38th Martian day, or sol, of the mission (July 2, 2008).

    A 3D representation of the same sample is on the right, as seen by Phoenix's Atomic Force Microscope. This is 200 times greater magnification than the view from the Optical Microscope, and the most highly magnified image ever seen from another world.

    The image shows four round pits, only 5 microns in depth, that were micromachined into the silicon substrate, which is the background plane shown in red. This image has been processed to reflect the levelness of the substrate.

    A Martian particle only one micrometer, or one millionth of a meter, across is held in the upper left pit.

    The rounded particle shown at the highest magnification ever seen from another world is a particle of the dust that cloaks Mars. Such dust particles color the Martian sky pink, feed storms that regularly envelop the planet and produce Mars' distinctive red soil.

    The Optical Microscope and the Atomic Force Microscope are part of Phoenix's Microscopy, Electrochemistry and Conductivity Analyzer instrument.

    The AFM was developed by a Swiss-led consortium, with Imperial College London producing the silicon substrate that holds sampled particles.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  1. Simulating the Phoenix Lander meteorological conditions with a Mars GCM

    NASA Astrophysics Data System (ADS)

    Daerden, F.; Neary, L.; Whiteway, J.; Dickinson, C.; Komguem, L.; McConnell, J. C.; Kaminski, J. W.

    2012-04-01

    An updated version of the GEM-Mars Global Circulation Model [1] is applied for the simulation of the meteorological conditions at the Phoenix lander site for the time period of the surface operations (Ls=76-150). The simulation results for pressure and temperature at the surface are compared to data from the Phoenix Meteorological Station (MET). The vertical profiles of dust and temperature are compared to Phoenix LIDAR measurements and data from orbit (CRISM and MCS on MRO). The simulated conditions in the PBL are compared to those obtained in a dedicated PBL-Aeolian dust model [2] which was successfully applied to drive a detailed microphysical model [3] for the interpretation of clouds and precipitation observed by the LIDAR on Phoenix [4,5]. [1] Moudden, Y. and J.C. McConnell (2005): A new model for multiscale modeling of the Martian atmosphere, GM3, J. Geophys. Res. 110, E04001, doi:10.1029/2004JE002354 [2] Davy, R., P. A. Taylor, W. Weng, and P.-Y. Li (2009), A model of dust in the Martian lower atmosphere, J. Geophys. Res., 114, D04108, doi:10.1029/2008JD010481. [3] Daerden, F., J.A. Whiteway, R. Davy, C. Verhoeven, L. Komguem, C. Dickinson, P. A. Taylor, and N. Larsen (2010), Simulating Observed Boundary Layer Clouds on Mars, Geophys. Res. Lett., 37, L04203, doi:10.1029/2009GL041523 [4] Whiteway, J., M. Daly, A. Carswell, T. Duck, C. Dickinson, L. Komguem, and C. Cook (2008), Lidar on the Phoenix mission to Mars, J. Geophys. Res., 113, E00A08, doi:10.1029/2007JE003002. [5] Whiteway, J., et al. (2009), Mars water ice clouds and precipitation, Science, 325, 68 - 70.

  2. Work on Phoenix Science Deck

    NASA Technical Reports Server (NTRS)

    2007-01-01

    Lockheed Martin Space Systems technicians Jim Young (left) and Jack Farmerie (right) work on the science deck of NASA's Phoenix Mars Lander.

    The spacecraft was built in a 100,000-class clean room near Denver under NASA's planetary protection practices to keep organics from being taken to Mars. The lander's robotic arm, built by the Jet Propulsion Laboratory, Pasadena, is seen at the top of the picture. The color and grey dots will be used to calibrate the spacecraft's Surface Stereoscopic Imager camera once the spacecraft has landed on the red planet.

    The Phoenix mission is led by Principal Investigator Peter H. Smith of the University of Arizona, Tucson, with project management at NASA's Jet Propulsion Laboratory and development partnership with Lockheed Martin Space Systems. International contributions for Phoenix are provided by the Canadian Space Agency, the University of Neuchatel (Switzerland), the University of Copenhagen, and the Max Planck Institute in Germany. JPL is a division of the California Institute of Technology in Pasadena.

  3. Work on Phoenix Science Deck

    NASA Technical Reports Server (NTRS)

    2007-01-01

    Lockheed Martin Space Systems technicians Jim Young (left) and Jack Farmerie (right) work on the science deck of NASA's Phoenix Mars Lander.

    The spacecraft was built in a 100,000-class clean room near Denver under NASA's planetary protection practices to keep organics from being taken to Mars. The lander's robotic arm, built by the Jet Propulsion Laboratory, Pasadena, is seen at the top of the picture. The color and grey dots will be used to calibrate the spacecraft's Surface Stereoscopic Imager camera once the spacecraft has landed on the red planet.

    The Phoenix mission is led by Principal Investigator Peter H. Smith of the University of Arizona, Tucson, with project management at NASA's Jet Propulsion Laboratory and development partnership with Lockheed Martin Space Systems. International contributions for Phoenix are provided by the Canadian Space Agency, the University of Neuchatel (Switzerland), the University of Copenhagen, and the Max Planck Institute in Germany. JPL is a division of the California Institute of Technology in Pasadena.

  4. Phoenix Robotic Arm connects with `Alice'

    NASA Technical Reports Server (NTRS)

    2008-01-01

    NASA's Phoenix Mars Lander's Robotic Arm comes into contact with a rock informally named 'Alice' near the 'Snow White' trench.

    This image was acquired by Phoenix's NASA's Surface Stereo Imager on July 13 during the 48th Martian day, or sol, since Phoenix landed.

    For scale, the width of the scoop at the end of the arm is about 8.5 centimeters (3.3 inches).

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  5. Martian Surface as Seen by Phoenix

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This anaglyph, formed from a mosaic of images acquired by NASA's Phoenix Lander's Surface Stereo Imager on the 13th through the 36th sols, or Martian days, of the mission (June 7, 2008 to July 1, 2008), shows a stereoscopic 3D view of the Martian surface near the lander. In the bottom left is a trench dug by Phoenix's Robotic Arm. In the bottom right is one of Phoenix's two solar panels.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  6. Phoenix Robotic Arm connects with `Alice'

    NASA Technical Reports Server (NTRS)

    2008-01-01

    NASA's Phoenix Mars Lander's Robotic Arm comes into contact with a rock informally named 'Alice' near the 'Snow White' trench.

    This image was acquired by Phoenix's NASA's Surface Stereo Imager on July 13 during the 48th Martian day, or sol, since Phoenix landed.

    For scale, the width of the scoop at the end of the arm is about 8.5 centimeters (3.3 inches).

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  7. 1. Site of Mormon Flat Dam looking upstream. Photographer unknown, ...

    Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

    1. Site of Mormon Flat Dam looking upstream. Photographer unknown, 1923. Source: Salt River Project. - Mormon Flat Dam, On Salt River, Eastern Maricopa County, east of Phoenix, Phoenix, Maricopa County, AZ

  8. Adsorption Driven Regolith-Atmospheric Water Vapor Transfer on Mars: Analysis of Phoenix TECP and MSL REMS Data

    NASA Astrophysics Data System (ADS)

    Farris, H. N.; Conner, M. B.; Chevrier, V. F.; Rivera-Valentin, E. G.

    2016-09-01

    BET adsorption theory is implemented to explain sol-to-sol dependencies of temperature and humidity at the Phoenix landing site and along the MSL traverse and thus, the implications for transient, adsorbed, liquid water at the surface.

  9. Zenith Movie showing Phoenix Lidar Beam Animation

    NASA Image and Video Library

    2008-08-04

    A laser beam from the Canadian-built lidar instrument on NASA Phoenix Mars Lander can be seen in this contrast-enhanced image taken by Phoenix Surface Stereo Imager on July 26, 2008, during early Martian morning hours of the 61st Martian day.

  10. Resurrecting Phoenix: Lessons in COIN Operations

    DTIC Science & Technology

    2006-05-16

    rallied 10 Mark Moyar, Phoenix and the Birds of Prey (Annapolis, MD: Naval Institute Press, 1997). P...Strategic Studies Institute: U.S. Army War College, 1995. Moyer, Mark. Phoenix and the birds of prey. Naval Institute Press: Annapolis, MD, 1997

  11. False Color Terrain Model of Phoenix Workspace

    NASA Image and Video Library

    2008-05-28

    This is a terrain model of Phoenix Robotic Arm workspace. It has been color coded by depth with a lander model for context. The model has been derived using images from the depth perception feature from Phoenix Surface Stereo Imager SSI.

  12. Overview of the Phoenix Entry, Descent and Landing System Architecture

    NASA Technical Reports Server (NTRS)

    Grover, Myron R., III; Cichy, Benjamin D.; Desai, Prasun N.

    2008-01-01

    NASA s Phoenix Mars Lander began its journey to Mars from Cape Canaveral, Florida in August 2007, but its journey to the launch pad began many years earlier in 1997 as NASA s Mars Surveyor Program 2001 Lander. In the intervening years, the entry, descent and landing (EDL) system architecture went through a series of changes, resulting in the system flown to the surface of Mars on May 25th, 2008. Some changes, such as entry velocity and landing site elevation, were the result of differences in mission design. Other changes, including the removal of hypersonic guidance, the reformulation of the parachute deployment algorithm, and the addition of the backshell avoidance maneuver, were driven by constant efforts to augment system robustness. An overview of the Phoenix EDL system architecture is presented along with rationales driving these architectural changes.

  13. Modeling Kilonova Spectra Using PHOENIX

    NASA Astrophysics Data System (ADS)

    Vallely, Patrick; Baron, Edward A.

    2017-06-01

    Powered by the radioactive decay of r-process nuclei, kilonova (alternatively referred to as macronova) emission provides an electromagnetic counterpart to the gravitational waves expected to be produced during binary neutron star and neutron star - black hole mergers. As such, kilonovae are potentially powerful tools for localizing gravitational wave sources and better probing the physics behind the events that generate them. We utilize the detailed Non-LTE code PHOENIX to simulate kilonova spectra by modeling r-process-rich ejecta, and we present the very preliminary results of these models.

  14. View from Above of Phoenix's Stowed Robotic Arm Camera

    NASA Technical Reports Server (NTRS)

    2008-01-01

    [figure removed for brevity, see original site] Click on image for animation

    This artist's animation of an imaginary camera zooming in from above shows the location of the Robotic Arm Camera on NASA's Phoenix Mars Lander as it acquires an image of the scoop at the end of the arm. Located just beneath the Robotic Arm Camera lens, the scoop is folded in the stowed position, with its open end facing the Robotic Arm Camera.

    The last frame in the animation shows the first image taken by the Robotic Arm Camera, one day after Phoenix landed on Mars. In the center of the image is the robotic scoop the lander will use to dig into the surface, collect samples and touch water ice on Mars for the first time. The scoop is in the stowed position, awaiting deployment of the robotic arm.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  15. View from Above of Phoenix's Stowed Robotic Arm Camera

    NASA Technical Reports Server (NTRS)

    2008-01-01

    [figure removed for brevity, see original site] Click on image for animation

    This artist's animation of an imaginary camera zooming in from above shows the location of the Robotic Arm Camera on NASA's Phoenix Mars Lander as it acquires an image of the scoop at the end of the arm. Located just beneath the Robotic Arm Camera lens, the scoop is folded in the stowed position, with its open end facing the Robotic Arm Camera.

    The last frame in the animation shows the first image taken by the Robotic Arm Camera, one day after Phoenix landed on Mars. In the center of the image is the robotic scoop the lander will use to dig into the surface, collect samples and touch water ice on Mars for the first time. The scoop is in the stowed position, awaiting deployment of the robotic arm.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  16. False Color Terrain Model of Phoenix Workspace

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This is a terrain model of Phoenix's Robotic Arm workspace. It has been color coded by depth with a lander model for context. The model has been derived using images from the depth perception feature from Phoenix's Surface Stereo Imager (SSI). Red indicates low-lying areas that appear to be troughs. Blue indicates higher areas that appear to be polygons.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  17. Rasp Tool on Phoenix Robotic Arm Model

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This close-up photograph taken at the Payload Interoperability Testbed at the University of Arizona, Tucson, shows the motorized rasp protruding from the bottom of the scoop on the engineering model of NASA's Phoenix Mars Lander's Robotic Arm.

    The rasp will be placed against the hard Martian surface to cut into the hard material and acquire an icy soil sample for analysis by Phoenix's scientific instruments.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is led by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  18. Phoenix's Probe Inserted in Martian Soil

    NASA Technical Reports Server (NTRS)

    2008-01-01

    The Phoenix Mars lander's robotic-arm camera took this image of the spacecraft's thermal and electrical-conductivity probe (TECP) inserted into Martian soil on day 149 of the mission. Phoenix landed on Mars' northern plains on May 25, 2008, landing.

    The robotic-arm camera acquired this image at 16:02:41 local solar time. The camera pointing was elevation -72.6986 degrees and azimuth 2.1093 degrees.

    The Phoenix mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  19. Phoenix Spacecraft Heat Shield Deployment Test

    NASA Image and Video Library

    2007-05-16

    In the Payload Hazardous Servicing Facility, workers monitor the Phoenix spacecraft during a heat shield deployment test, with a firing of ordnance associated with the separation device. Phoenix will land in icy soils near the north polar permanent ice cap of Mars and explore the history of the water in these soils and any associated rocks, while monitoring polar climate. Landing is planned in May 2008 on arctic ground where a mission currently in orbit, Mars Odyssey, has detected high concentrations of ice just beneath the top layer of soil. Launch of Phoenix aboard a Delta II rocket is targeted for Aug. 3 from Cape Canaveral Air Force Station in Florida.

  20. Phoenix Spacecraft Heat Shield Deployment Test

    NASA Image and Video Library

    2007-05-16

    In the Payload Hazardous Servicing Facility, a worker monitors the Phoenix spacecraft during a heat shield deployment test, with a firing of ordnance associated with the separation device. Phoenix will land in icy soils near the north polar permanent ice cap of Mars and explore the history of the water in these soils and any associated rocks, while monitoring polar climate. Landing is planned in May 2008 on arctic ground where a mission currently in orbit, Mars Odyssey, has detected high concentrations of ice just beneath the top layer of soil. Launch of Phoenix aboard a Delta II rocket is targeted for Aug. 3 from Cape Canaveral Air Force Station in Florida.

  1. Phoenix - The First Mars Scout Mission

    NASA Technical Reports Server (NTRS)

    Goldstein, Barry; Shotwell, Robert

    2008-01-01

    As the first of the new Mars Scouts missions, the Phoenix project was selected by NASA in August of 2003. Four years later, almost to the day, Phoenix was launched from Cape Canaveral Air Station and successfully injected into an interplanetary trajectory on its way to Mars. On May 25, 2008 Phoenix conducted the first successful powered decent on Mars in over 30 years. This paper will highlight some of the key changes since the 2008 IEEE paper of the same name, as well as performance through cruise, landing at the north pole of Mars and some of the preliminary results of the surface mission.

  2. Phoenix - The First Mars Scout Mission

    NASA Technical Reports Server (NTRS)

    Goldstein, Barry; Shotwell, Robert

    2008-01-01

    As the first of the new Mars Scouts missions, the Phoenix project was selected by NASA in August of 2003. Four years later, almost to the day, Phoenix was launched from Cape Canaveral Air Station and successfully injected into an interplanetary trajectory on its way to Mars. On May 25, 2008 Phoenix conducted the first successful powered decent on Mars in over 30 years. This paper will highlight some of the key changes since the 2008 IEEE paper of the same name, as well as performance through cruise, landing at the north pole of Mars and some of the preliminary results of the surface mission.

  3. The Phoenix Program and Contemporary Counterinsurgency

    DTIC Science & Technology

    2009-01-01

    Counterinsurgency Lessons from Vietnam for the Future,” Military Review, March–April 2006, p. 17. 7 Mark Moyar, Phoenix and the Birds of Prey: The CIA’s...director for operations, and the CIA’s director of central intelligence. 10 Moyar, Phoenix and the Birds of Prey, pp. 37–38. 11 Moyar, Phoenix and...the Birds of Prey, p. 42. 12 Douglas S. Blaufarb, The Counterinsurgency Era: U.S. Doctrine and Performance, 1950 to the Present, New York: The Free

  4. Phoenix's Probe Inserted in Martian Soil

    NASA Technical Reports Server (NTRS)

    2008-01-01

    The Phoenix Mars lander's robotic-arm camera took this image of the spacecraft's thermal and electrical-conductivity probe (TECP) inserted into Martian soil on day 149 of the mission. Phoenix landed on Mars' northern plains on May 25, 2008, landing.

    The robotic-arm camera acquired this image at 16:02:41 local solar time. The camera pointing was elevation -72.6986 degrees and azimuth 2.1093 degrees.

    The Phoenix mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  5. Rasp Tool on Phoenix Robotic Arm Model

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This close-up photograph taken at the Payload Interoperability Testbed at the University of Arizona, Tucson, shows the motorized rasp protruding from the bottom of the scoop on the engineering model of NASA's Phoenix Mars Lander's Robotic Arm.

    The rasp will be placed against the hard Martian surface to cut into the hard material and acquire an icy soil sample for analysis by Phoenix's scientific instruments.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is led by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  6. Measurements of nonmethane hydrocarbons in Phoenix, Arizona

    SciTech Connect

    Doskey, P. V.; Kotamarthi, V. R.; Rudolph, J.

    1999-10-12

    Nonmethane hydrocarbons (NMHCs) are precursors to oxidant formation. They are oxidized by hydroxyl radical (OH), forming a complex mixture of peroxy radicals that oxidize NO to NO{sub 2} without consuming ozone (O{sub 3}) and thus allow O{sub 3} to increase in the atmospheric boundary layer. The reactivities of the NMHCs that compose biogenic and anthropogenic emissions vary greatly. For example, isoprene, which is emitted by deciduous vegetation, has an atmospheric lifetime with respect to oxidation by OH of about 20 min in polluted air ([OH] = 10{sup 7} radicals cm{sup {minus}3}). The atmospheric lifetimes of 2-methylpropene, 2-methylbutane, and the xylenes, which are found in vehicle emissions, are approximately 30 min, 7 hr, and 1.5 hr, respectively. The authors made measurements of the NMHCs at a surface site and aloft aboard the Battelle Gulfstream (G-1) aircraft, as part of an air quality study in the Phoenix area during May 1998. Diurnal variations in the NMHC distributions and their propene-equivalent concentrations are used to examine origins and reactivities of the air masses that were sampled at the surface site.

  7. Animated Optical Microscope Zoom in from Phoenix Launch to Martian Surface

    NASA Technical Reports Server (NTRS)

    2008-01-01

    [figure removed for brevity, see original site] Click on image for animation

    This animated camera view zooms in from NASA's Phoenix Mars Lander launch site all the way to Phoenix's Microscopy and Electrochemistry and C Eonductivity Analyzer (MECA) aboard the spacecraft on the Martian surface. The final frame shows the soil sample delivered to MECA as viewed through the Optical Microscope (OM) on Sol 17 (June 11, 2008), or the 17th Martian day.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  8. Animated Optical Microscope Zoom in from Phoenix Launch to Martian Surface

    NASA Technical Reports Server (NTRS)

    2008-01-01

    [figure removed for brevity, see original site] Click on image for animation

    This animated camera view zooms in from NASA's Phoenix Mars Lander launch site all the way to Phoenix's Microscopy and Electrochemistry and C Eonductivity Analyzer (MECA) aboard the spacecraft on the Martian surface. The final frame shows the soil sample delivered to MECA as viewed through the Optical Microscope (OM) on Sol 17 (June 11, 2008), or the 17th Martian day.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  9. The Goals and Approach of the Phoenix Mission for Evaluating the Habitabiity of the Northern Plains on Mars

    NASA Technical Reports Server (NTRS)

    Stoker, Carol R.

    2006-01-01

    The first goal of the Mars Exploration program, as defined by the Mars Exploration Payload Analysis Group (MEPAG) is to determine if life ever arose on Mars [1]. The Phoenix landing site was chosen to sample near surface ground ice in the Northern Plains discovered by the GRS experiment on Mars Odyssey [2]. A goal of Phoenix is to determine whether this environment was habitable for life at some time in its history.

  10. Project Phoenix: the Australian deployment

    NASA Astrophysics Data System (ADS)

    Tarter, Jill C.

    1996-06-01

    From February 2 until June 6 of 1995, the Phoenix Team conducted SETI observations using the 64 m radio telescope at Parkes and a remotely operated 22 m antenna at Connabarabran. The dual polarization observations covered the frequency range from 1.2 to 3 GHz using a single wideband receiver and two feeds built by CSIRO to support this project. The two antennas simultaneously observed a target list of 202 solar-type stars located at declinations south of -35 degrees. Individual observations lasted up to 276 seconds and examined 20 MHz of the spectrum with resolutions as fine as 1 Hz using hardware pattern detectors to search for narrowband, continuous or pulsed signals whose frequency might be slowly changing in time. The data were analyzed, and candidate signals were identified in near-real-time (before the end of the next data acquisition cycle). Those candidate signals not matched against an on-line RFI database were automatically reobserved with finer resolution by another set of detectors and followed in phase in order to permit a pseudo-interferometric measurement between the two telescopes. This two stage approach (detection on the 64 m antenna and immediate interferometric follow up of candidates) was part of a pipelined observational sequence and proved to be an extremely effective and efficient method of discriminating against RFI. Detection thresholds were set to produce a few candidate signals per observation, yet for more than 23,000 completed observations, the programmed sequence had to be interrupted fewer than 100 times to move the antennas off source for further verification procedures. In each case the candidate signals were found to be of our own technological making. The Phoenix observations in Australia failed to detect any ETI signals, but they also left no mysterious or unexplained signals hanging around. The deployment was a logistical and technological success, and reaffirms our opinion that one telescope is not enough.

  11. Working End of Robotic Arm on Phoenix

    NASA Image and Video Library

    2007-08-02

    This illustration shows some of the components on and near the end of the robotic arm on NASA Phoenix Mars Lander. Primary and secondary blades on the scoop that aided in the collection of soil samples.

  12. Phoenix v. 1.0-SNAPSHOT

    SciTech Connect

    Bastian, Mark; Trigueros, Jose V.

    2016-09-21

    Phoenix is a Java Virtual Machine (JVM) based library for performing mathematical and astrodynamics calculations. It consists of two primary sub-modules, phoenix-math and phoenix-astrodynamics. The mathematics package has a variety of mathematical classes for performing 3D transformations, geometric reasoning, and numerical analysis. The astrodynamics package has various classes and methods for computing locations, attitudes, accesses, and other values useful for general satellite modeling and simulation. Methods for computing celestial locations, such as the location of the Sun and Moon, are also included. Phoenix is meant to be used as a library within the context of a larger application. For example, it could be used for a web service, desktop client, or to compute simple values in a scripting environment.

  13. Rasp Tool on Phoenix Robotic Arm Model

    NASA Image and Video Library

    2008-07-15

    This close-up photograph taken at the Payload Interoperability Testbed at the University of Arizona, Tucson, shows the motorized rasp protruding from the bottom of the scoop on the engineering model of NASA Phoenix Mars Lander Robotic Arm.

  14. Astronaut Alvin Drew Speaks With Phoenix Students

    NASA Image and Video Library

    From NASA's International Space Station Mission Control Center, NASA astronaut Alvin Drew participates in a Digital Learning Network (DLN) event with students at Monterey Park in Phoenix. The DLN c...

  15. Martian Surface as Seen by Phoenix

    NASA Image and Video Library

    2008-07-28

    This anaglyph, acquired by NASA Phoenix Lander Surface Stereo Imager on June 19, 2008, shows a view of the Martian surface near the lander. The trench shown here is informally called Snow White 1. 3D glasses are necessary.

  16. Vertical Water Vapor Distribution at Phoenix

    NASA Astrophysics Data System (ADS)

    Tamppari, L. K.; Lemmon, M. T.

    2016-09-01

    The Phoenix SSI camera data along with radiative transfer modeling are used to retrieve the vertical water vapor profile. Preliminary results indicate that water vapor is often confined near the surface.

  17. Testing Phoenix Mars Lander Parachute in Idaho

    NASA Image and Video Library

    2008-05-24

    NASA Phoenix Mars Lander parachuted for nearly three minutes as it descended through the Martian atmosphere on May 25, 2008. Extensive preparations for that crucial period included this drop test near Boise, Idaho, in October 2006.

  18. Powered Landing of Phoenix Artist Concept

    NASA Image and Video Library

    2007-07-30

    This artist concept depicts NASA Phoenix Mars Lander a moment before its 2008 touchdown on the arctic plains of Mars. Pulsed rocket engines control the spacecraft speed during the final seconds of descent.

  19. Temperature Measurements Taken by Phoenix Spacecraft

    NASA Image and Video Library

    2008-09-30

    This chart plots the minimum daily atmospheric temperature measured by NASA Phoenix Mars Lander spacecraft since landing on Mars. As the temperature increased through the summer season, the atmospheric humidity also increased.

  20. A case study in resort climatology of Phoenix, Arizona, USA.

    PubMed

    Hartz, Donna A; Brazel, Anthony J; Heisler, Gordon M

    2006-09-01

    Tourists often use weather data as a factor for determining vacation timing and location. Accuracy and perceptions of weather information may impact these decisions. This study: (a) examines air temperature and dew points from seven exclusive resorts in the Phoenix metropolitan area and compares them with official National Weather Service data for the same period, and (b) utilizes a comfort model called OUTCOMES-OUTdoor COMfort Expert System-in a seasonal appraisal of two resorts, one mesic and one xeric, compared with the urban Sky Harbor International Airport first-order weather station site in the central urban area of Phoenix, Arizona, USA (lat. 33.43 degrees N; long. 112.02 degrees W; elevation at 335 m). Temperature and humidity recording devices were placed within or immediately adjacent to common-use areas of the resorts, the prime recreational sites used by guests on most resort properties. Recorded data were compared with that of the official weather information from the airport station, a station most accessible to potential tourists through media and Web sites, to assess predicted weather for vacation planning. For the most part, Sky Harbor's recorded air temperatures and often dew points were higher than those recorded at the resorts. We extrapolate our findings to a year-round estimate of human outdoor comfort for weather-station sites typical of resort landscapes and the Sky Harbor location using the OUTCOMES model to refine ideas on timing of comfortable conditions at resorts on a diurnal and seasonal basis.

  1. Far-Northern Destination for Phoenix Mars Lander

    NASA Technical Reports Server (NTRS)

    2007-01-01

    The planned landing site for NASA's Phoenix Mars Lander lies at a latitude on Mars equivalent to northern Alaska on Earth. It is within the region designated 'D' on this global image.

    This is an orthographic projection with color-coded elevation contours and shaded relief based on data from the Mars Orbiter Laser Altimeter on NASA's Mars Global Surveyor orbiter. Total vertical relief is about 28 kilometers (17 miles) from the top of the highest volcano (red) to the northern lowlands (blue). North pole is where the longitude lines converge.

  2. Mars 2007 Phoenix Scout Mission Organic Free Blank: Method to Distinguish Mars Organics from Terrestrial Organics

    NASA Technical Reports Server (NTRS)

    Ming, D. W.; Morris, R. V.; Woida, R.; Sutter, B.; Lauer, H. V.; Shinohara, C.; Golden, D. C.; Boynton, W. V.; Arvidson, R. E.; Stewart, R. L.; hide

    2008-01-01

    The Mars 2007 Phoenix Scout Mission successfully launched on August 4, 2007, for a 10-month journey to Mars. The Phoenix spacecraft is scheduled to land on May 25, 2008. The primary mission objective is to study the history of water and evaluate the potential for past and present habitability in Martian arctic ice-rich soil [1]. Phoenix will land near 68 N latitude on polygonal terrain presumably created by ice layers that are expected to be a few centimeters under loose soil materials [2,3]. The Phoenix Mission will assess the potential for habitability by searching for organic molecules in ice or icy soils at the landing site. Organic molecules are necessary building blocks for life, although their presence in the ice or soil does not indicate life itself. Phoenix will search for organic molecules by heating soil/ice samples in the Thermal and Evolved-Gas Analyzer (TEGA, [4]). TEGA consists of 8 differential scanning calorimeter (DSC) ovens integrated with a magnetic-sector mass spectrometer with a mass range of 2-140 daltons [4]. Endothermic and exothermic reactions are recorded by the TEGA DSC as samples are heated from ambient to approx.1000 C. Evolved gases, including organic molecules and fragments if present, are simultaneously measured by the mass spectrometer during heating.

  3. Zeroing In on Phoenix's Final Destination

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This image shows the latest estimate, marked by a green crosshair, of the location of NASA's Phoenix Mars Lander. Radio communications between Phoenix and spacecraft flying overhead have allowed engineers to narrow the lander's location to an area about 300 meters (984) long by 100 meters (328 feet) across, or about three football fields long and one football field wide.

    During landing, Phoenix traveled across the field of view shown here from the upper left to the lower right. The area outlined in blue represents the area where Phoenix was predicted to land before arriving on Mars. During Phoenix's descent through the Martian atmosphere to the surface of the Red Planet, continuous measurements of the distance the spacecraft traveled enabled engineers to narrow its location further to the circular area outlined in red.

    Using radio signals to home in on Phoenix's final location is sort of like trying to find a kitten by listening to the sound of its meows. As NASA's Odyssey spacecraft passes overhead, it receives radio transmissions from the lander. When Odyssey passes overhead again along a slightly different path, it receives new radio signals. With each successive pass, it is able to 'fix' the location of Phoenix a little more precisely.

    Meanwhile, NASA's Mars Reconnaissance Orbiter has taken actual images of the spacecraft on the surface, enabling scientists to match the lander's location to geologic features seen from orbit.

    The large crater to the right is 'Heimdall crater,' the slopes of which are visible in images of the parachute that lowered Phoenix to the surface, taken by the High Resolution Imaging Science Experiment instrument on the Mars Reconnaissance Orbiter. The map shown here is made up of topography data taken by NASA's Mars Global Surveyor. It shows exaggerated differences in the height of the terrain.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the

  4. Zeroing In on Phoenix's Final Destination

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This image shows the latest estimate, marked by a green crosshair, of the location of NASA's Phoenix Mars Lander. Radio communications between Phoenix and spacecraft flying overhead have allowed engineers to narrow the lander's location to an area about 300 meters (984) long by 100 meters (328 feet) across, or about three football fields long and one football field wide.

    During landing, Phoenix traveled across the field of view shown here from the upper left to the lower right. The area outlined in blue represents the area where Phoenix was predicted to land before arriving on Mars. During Phoenix's descent through the Martian atmosphere to the surface of the Red Planet, continuous measurements of the distance the spacecraft traveled enabled engineers to narrow its location further to the circular area outlined in red.

    Using radio signals to home in on Phoenix's final location is sort of like trying to find a kitten by listening to the sound of its meows. As NASA's Odyssey spacecraft passes overhead, it receives radio transmissions from the lander. When Odyssey passes overhead again along a slightly different path, it receives new radio signals. With each successive pass, it is able to 'fix' the location of Phoenix a little more precisely.

    Meanwhile, NASA's Mars Reconnaissance Orbiter has taken actual images of the spacecraft on the surface, enabling scientists to match the lander's location to geologic features seen from orbit.

    The large crater to the right is 'Heimdall crater,' the slopes of which are visible in images of the parachute that lowered Phoenix to the surface, taken by the High Resolution Imaging Science Experiment instrument on the Mars Reconnaissance Orbiter. The map shown here is made up of topography data taken by NASA's Mars Global Surveyor. It shows exaggerated differences in the height of the terrain.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the

  5. Deep 'Stone Soup' Trenching by Phoenix (Stereo)

    NASA Technical Reports Server (NTRS)

    2008-01-01

    Digging by NASA's Phoenix Mars Lander on Aug. 23, 2008, during the 88th sol (Martian day) since landing, reached a depth about three times greater than in any trench Phoenix has excavated. The deep trench, informally called 'Stone Soup' is at the borderline between two of the polygon-shaped hummocks that characterize the arctic plain where Phoenix landed.

    Stone Soup is in the center foreground of this stereo view, which appears three dimensional when seen through red-blue glasses. The view combines left-eye and right-eye images taken by the lander's Surface Stereo Imager on Sol 88 after the day's digging. The trench is about 25 centimeters (10 inches) wide and about 18 centimeters (7 inches) deep.

    When digging trenches near polygon centers, Phoenix has hit a layer of icy soil, as hard as concrete, about 5 centimeters or 2 inches beneath the ground surface. In the Stone Soup trench at a polygon margin, the digging has not yet hit an icy layer like that.

    Stone Soup is toward the left, or west, end of the robotic arm's work area on the north side of the lander.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  6. Sustainable Phoenix: Lessons from the Dutch Model

    NASA Astrophysics Data System (ADS)

    Lara, Jesus J.

    In only fifty years, the Phoenix metropolitan area has expanded from a small desert town into one of the largest urban areas in the United States. Today, it has one of the fastest rates of growth in the nation with an annual rate of 4.5%. This area has grown during a period in urban development that largely ignored local topography, climate, culture, and history. The result has been a sprawling metropolitan area with an ever increasing ecological footprint and a standardized urban design and infrastructure that works against its environmental setting rather than with it. Currently, the city of Phoenix is going through a process of urban revitalization with an increasing demand for urban living and commerce. This research explores sustainable urban design and its potential applications in the metropolitan Phoenix area through an investigation of the Dutch model. The Dutch have successfully dealt with sustainable urban design approaches and their practices represent an unusual learning opportunity for Phoenix. The Netherlands' experience suggests three strategies/themes for rendering Phoenix a more sustainable urban form. These include the strategic planning and development of urban extensions, compact infill, and modernizing infrastructure.

  7. Deep 'Stone Soup' Trenching by Phoenix (Stereo)

    NASA Technical Reports Server (NTRS)

    2008-01-01

    Digging by NASA's Phoenix Mars Lander on Aug. 23, 2008, during the 88th sol (Martian day) since landing, reached a depth about three times greater than in any trench Phoenix has excavated. The deep trench, informally called 'Stone Soup' is at the borderline between two of the polygon-shaped hummocks that characterize the arctic plain where Phoenix landed.

    Stone Soup is in the center foreground of this stereo view, which appears three dimensional when seen through red-blue glasses. The view combines left-eye and right-eye images taken by the lander's Surface Stereo Imager on Sol 88 after the day's digging. The trench is about 25 centimeters (10 inches) wide and about 18 centimeters (7 inches) deep.

    When digging trenches near polygon centers, Phoenix has hit a layer of icy soil, as hard as concrete, about 5 centimeters or 2 inches beneath the ground surface. In the Stone Soup trench at a polygon margin, the digging has not yet hit an icy layer like that.

    Stone Soup is toward the left, or west, end of the robotic arm's work area on the north side of the lander.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  8. Deep 'Stone Soup' Trenching by Phoenix

    NASA Technical Reports Server (NTRS)

    2008-01-01

    Digging by NASA's Phoenix Mars Lander on Aug. 23, 2008, during the 88th sol (Martian day) since landing, reached a depth about three times greater than in any trench Phoenix has excavated. The deep trench, informally called 'Stone Soup' is at the borderline between two of the polygon-shaped hummocks that characterize the arctic plain where Phoenix landed.

    The lander's Surface Stereo Imager took this picture of Stone Soup trench on Sol 88 after the day's digging. The trench is about 25 centimeters (10 inches) wide and about 18 centimeters (7 inches) deep.

    When digging trenches near polygon centers, Phoenix has hit a layer of icy soil, as hard as concrete, about 5 centimeters or 2 inches beneath the ground surface. In the Stone Soup trench at a polygon margin, the digging has not yet hit an icy layer like that.

    Stone Soup is toward the left, or west, end of the robotic arm's work area on the north side of the lander.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  9. Testing Phoenix Mars Lander Parachute in Idaho

    NASA Technical Reports Server (NTRS)

    2008-01-01

    NASA's Phoenix Mars Lander will parachute for nearly three minutes as it descends through the Martian atmosphere on May 25, 2008. Extensive preparations for that crucial period included this drop test near Boise, Idaho, in October 2006.

    The parachute used for the Phoenix mission is similar to ones used by NASA's Viking landers in 1976. It is a 'disk-gap-band' type of parachute, referring to two fabric components -- a central disk and a cylindrical band -- separated by a gap.

    Although the Phoenix parachute has a smaller diameter (11.8 meters or 39 feet) than the parachute for the 2007 Mars Pathfinder landing (12.7 meters or 42 feet), its Viking configuration results in slightly larger drag area. The smaller physical size allows for a stronger system because, given the same mass and volume restrictions, a smaller parachute can be built using higher strength components. The Phoenix parachute is approximately 1.5 times stronger than Pathfinder's. Testing shows that it is nearly two times stronger than the maximum opening force expected during its use at Mars.

    Engineers used a dart-like weight for the drop testing in Idaho. On the Phoenix spacecraft, the parachute is attached the the backshell. The backshell is the upper portion of a capsule around the lander during the flight from Earth to Mars and protects Phoenix during the initial portion of the descent through Mars' atmosphere.

    Phoenix will deploy its parachute at about 12.6 kilometers (7.8 miles) in altitude and at a velocity of 1.7 times the speed of sound. A mortar on the spacecraft fires to deploy the parachute, propelling it away from the backshell into the supersonic flow. The mortar design for Phoenix is essentially the same as Pathfinder's. The parachute and mortar are collectively called the 'parachute decelerator system.' Pioneer Aerospace, South Windsor, Conn., produced this system for Phoenix. The same company provided the parachute decelerator systems for Pathfinder, Mars Polar

  10. 'Rosy Red' Soil in Phoenix's Scoop

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This image shows fine-grained material inside the Robotic Arm scoop as seen by the Robotic Arm Camera (RAC) aboard NASA's Phoenix Mars Lander on June 25, 2008, the 30th Martian day, or sol, of the mission.

    The image shows fine, fluffy, red soil particles collected in a sample called 'Rosy Red.' The sample was dug from the trench named 'Snow White' in the area called 'Wonderland.' Some of the Rosy Red sample was delivered to Phoenix's Optical Microscope and Wet Chemistry Laboratory for analysis.

    The RAC provides its own illumination, so the color seen in RAC images is color as seen on Earth, not color as it would appear on Mars.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  11. Martian Dust Collected by Phoenix's Arm

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This image from NASA's Phoenix Lander's Optical Microscope shows particles of Martian dust lying on the microscope's silicon substrate. The Robotic Arm sprinkled a sample of the soil from the Snow White trench onto the microscope on July 2, 2008, the 38th Martian day, or sol, of the mission after landing.

    Subsequently, the Atomic Force Microscope, or AFM, zoomed in one of the fine particles, creating the first-ever image of a particle of Mars' ubiquitous fine dust, the most highly magnified image ever seen from another world.

    The Atomic Force Microscope was developed by a Swiss-led consortium in collaboration with Imperial College London. The AFM is part of Phoenix's Microscopy, Electrochemistry and Conductivity Analyzer instrument.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  12. Phoenix Lowered into Thermal Vacuum Chamber

    NASA Technical Reports Server (NTRS)

    2007-01-01

    NASA's Phoenix Mars Lander was lowered into a thermal vacuum chamber at Lockheed Martin Space Systems, Denver, in December 2006.

    The spacecraft was folded in its aeroshell and underwent environmental testing that simulated the extreme conditions the spacecraft will see during its nine-and-a-half-month cruse to Mars.

    The Phoenix mission is led by Principal Investigator Peter H. Smith of the University of Arizona, Tucson, with project management at NASA's Jet Propulsion Laboratory and development partnership with Lockheed Martin Space Systems. International contributions for Phoenix are provided by the Canadian Space Agency, the University of Neuchatel (Switzerland), the University of Copenhagen, and the Max Planck Institute in Germany. JPL is a division of the California Institute of Technology in Pasadena.

  13. 'Rosy Red' Soil in Phoenix's Scoop

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This image shows fine-grained material inside the Robotic Arm scoop as seen by the Robotic Arm Camera (RAC) aboard NASA's Phoenix Mars Lander on June 25, 2008, the 30th Martian day, or sol, of the mission.

    The image shows fine, fluffy, red soil particles collected in a sample called 'Rosy Red.' The sample was dug from the trench named 'Snow White' in the area called 'Wonderland.' Some of the Rosy Red sample was delivered to Phoenix's Optical Microscope and Wet Chemistry Laboratory for analysis.

    The RAC provides its own illumination, so the color seen in RAC images is color as seen on Earth, not color as it would appear on Mars.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  14. Phoenix Deepens Trenches on Mars (3D)

    NASA Technical Reports Server (NTRS)

    2008-01-01

    The Surface Stereo Imager on NASA's Phoenix Mars Lander took this anaglyph on Oct. 21, 2008, during the 145th Martian day, or sol. Phoenix landed on Mars' northern plains on May 25, 2008.

    The trench on the upper left, called 'Upper Cupboard,' is about 60 centimeters (24 inches) long and 3 centimeters (1 inch) deep. The trench in the middle,called 'Ice Man,' is about 30 centimeters (12 inches) long and 3 centimeters (1 inch) deep. The trench on the right, called 'La Mancha,' is about 31 centimeters (12 inches) and 5 centimeters (2 inches) deep.

    The Phoenix mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  15. Phoenix Deepens Trenches on Mars (3D)

    NASA Technical Reports Server (NTRS)

    2008-01-01

    The Surface Stereo Imager on NASA's Phoenix Mars Lander took this anaglyph on Oct. 21, 2008, during the 145th Martian day, or sol. Phoenix landed on Mars' northern plains on May 25, 2008.

    The trench on the upper left, called 'Dodo-Goldilocks,' is about 38 centimeters (15 inches) long and 4 centimeters (1.5 inches) deep. The trench on the right, called 'Upper Cupboard,' is about 60 centimeters (24 inches) long and 3 centimeters (1 inch) deep. The trench in the lower middle is called 'Stone Soup.'

    The Phoenix mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  16. Dust Storm Moving Near Phoenix Lander

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This series of images show the movement of several dust storms near NASA's Phoenix Mars Lander. These images were taken by the lander's Surface Stereo Imager (SSI) on the 137th Martian day, or sol, of the mission (Oct. 13, 2008).

    These images were taken about 50 seconds apart, showing the formation and movement of dust storms for nearly an hour. Phoenix scientists are still figuring out the exact distances these dust storms occurred from the lander, but they estimate them to be about 1 to 2 kilometers (.6 or 1.2 miles) away.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  17. Doors Fully Open on Phoenix's Next Oven

    NASA Technical Reports Server (NTRS)

    2008-01-01

    The double doors on the right are wide open in this image of four pairs of oven doors on Phoenix's Thermal and Evolved-Gas Analyzer (TEGA).

    This pair of doors goes to TEGA's oven number zero, the third of the instrument's three ovens to be opened and the first for which both doors have opened fully. The lander's Surface Stereo Imager took this photo on July 19, 2008, during the 53rd Martian day, or sol, since Phoenix landed.

    The doors are about 10 centimeters (4 inches) tall.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is led by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  18. Doors Fully Open on Phoenix's Next Oven

    NASA Technical Reports Server (NTRS)

    2008-01-01

    The double doors on the right are wide open in this image of four pairs of oven doors on Phoenix's Thermal and Evolved-Gas Analyzer (TEGA).

    This pair of doors is for TEGA's oven number zero, the third of the instrument's ovens to be opened and the first for which both doors have opened fully. The lander's Surface Stereo Imager took this photo on July 18, 2008, during the 53rd Martian day, or sol, since Phoenix landed. The image has been brightened to show the fine mesh.

    The doors are about 10 centimeters (4 inches) tall.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  19. Martian Dust Collected by Phoenix's Arm

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This image from NASA's Phoenix Lander's Optical Microscope shows particles of Martian dust lying on the microscope's silicon substrate. The Robotic Arm sprinkled a sample of the soil from the Snow White trench onto the microscope on July 2, 2008, the 38th Martian day, or sol, of the mission after landing.

    Subsequently, the Atomic Force Microscope, or AFM, zoomed in one of the fine particles, creating the first-ever image of a particle of Mars' ubiquitous fine dust, the most highly magnified image ever seen from another world.

    The Atomic Force Microscope was developed by a Swiss-led consortium in collaboration with Imperial College London. The AFM is part of Phoenix's Microscopy, Electrochemistry and Conductivity Analyzer instrument.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  20. Assessment of Mars Phoenix EDL Performance

    NASA Technical Reports Server (NTRS)

    Oberhettinger, David; Skulsky, Eli D.; Bailey, Erik S.

    2011-01-01

    Entry, Descent, and Landing (EDL) is an especially risky phase of a planetary mission, and detailed information on the performance of a lander's EDL design is critical to mitigating the risks of future missions. 12However, the study of actual EDL performance and comparison with the pre-entry predictions has not typically been given a high priority following spacecraft landings, mainly for budgetary reasons. Because Mars Phoenix inherited hardware and design elements from a similar mission that appears to have failed during Mars EDL, NASA was particularly interested in identifying the reasons for the Phoenix mission success. Therefore, NASA sponsored a reconstruction and analysis of the downlinked Phoenix telemetry that would tell the story of this critical event sequence--focusing on the 14 minutes from cruise stage separation to landing--and identify lessons learned.

  1. Dust Storm Moving Near Phoenix Lander

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This series of images show the movement of several dust storms near NASA's Phoenix Mars Lander. These images were taken by the lander's Surface Stereo Imager (SSI) on the 137th Martian day, or sol, of the mission (Oct. 13, 2008).

    These images were taken about 50 seconds apart, showing the formation and movement of dust storms for nearly an hour. Phoenix scientists are still figuring out the exact distances these dust storms occurred from the lander, but they estimate them to be about 1 to 2 kilometers (.6 or 1.2 miles) away.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  2. Phoenix Lowered into Thermal Vacuum Chamber

    NASA Technical Reports Server (NTRS)

    2007-01-01

    NASA's Phoenix Mars Lander was lowered into a thermal vacuum chamber at Lockheed Martin Space Systems, Denver, in December 2006.

    The spacecraft was folded in its aeroshell and underwent environmental testing that simulated the extreme conditions the spacecraft will see during its nine-and-a-half-month cruse to Mars.

    The Phoenix mission is led by Principal Investigator Peter H. Smith of the University of Arizona, Tucson, with project management at NASA's Jet Propulsion Laboratory and development partnership with Lockheed Martin Space Systems. International contributions for Phoenix are provided by the Canadian Space Agency, the University of Neuchatel (Switzerland), the University of Copenhagen, and the Max Planck Institute in Germany. JPL is a division of the California Institute of Technology in Pasadena.

  3. Phoenix Makes an Impression on Mars

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This view from the Surface Stereo Imager on NASA's Phoenix Mars Lander shows the first impression dubbed Yeti and looking like a wide footprint -- made on the Martian soil by the Robotic Arm scoop on Sol 6, the sixth Martian day of the mission, (May 31, 2008).

    Touching the ground is the first step toward scooping up soil and ice and delivering the samples to the lander's experiments.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  4. Phoenix Carries Soil to Wet Chemistry Lab

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This image taken by the Surface Stereo Imager on NASA's Phoenix Mars Lander shows the lander's Robotic Arm scoop positioned over the Wet Chemistry Lab delivery funnel on Sol 29, the 29th Martian day after landing, or June 24, 2008. The soil will be delivered to the instrument on Sol 30.

    This image has been enhanced to brighten the scene.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  5. Phoenix Deploying its Robotic Arm Elbow

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This animated gif is compiled of images from Phoenix's Stereo Surface Imager (SSI) taken on Sol 3. It shows the stair-step motion used to unstow the arm from a protective covering called the biobarrier. The last two moves allow the arm to stand straight up.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  6. Martian Soil Inside Phoenix's Robotic Arm Scoop

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This image from NASA's Phoenix Mars Lander's Robotic Arm Camera (RAC) shows material from the Martian surface captured by the Robotic Arm (RA) scoop during its first test dig and dump on the seventh Martian day of the mission, or Sol 7 (June 1, 2008). The test sample shown was taken from the digging area informally known as 'Knave of Hearts.'

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  7. Rasped Soil Sample in Phoenix Scoop

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This image, taken by NASA's Phoenix Mars Lander's Robotic Arm Camera on Sol 50, the 50th day of the mission, July 15, 2008, shows material collected in the lander's scoop from the rasping activity on the Martian surface.

    The collected material, believed to be icy soil, is near the bottom of the image. The width of the scoop is 8.5 centimeters (3.3 inches).

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is led by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  8. Phoenix 'Gets the Scoop' on the Scoop

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This is the first image taken by the Robotic Arm Camera on NASA's Phoenix Mars Lander, one day after landing. In the center of the image is the robotic scoop the lander will use to dig into the surface, collect samples and touch water ice on Mars for the first time. The scoop is in the stowed position, awaiting deployment of the robotic arm.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  9. Color view to Northwest of Phoenix

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This approximate color (SSI's red, green, and blue filters: 600, 530, and 480 nanometers) view was obtained on sol 2 by the Surface Stereo Imager (SSI) on board the Phoenix lander. The view is toward the northwest, showing polygonal terrain near the lander and out to the horizon.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  10. Phoenix's La Mancha Trench in 3D

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This anaglyph, taken by NASA's Phoenix Mars Lander's Surface Stereo Imager, was taken on the 131st Martian day, or sol, of the mission (Oct. 7, 2008). The anaglyph highlights the depth of the trench, informally named 'La Mancha,' and reveals the ice layer beneath the soil surface. The trench's depth is about 5 centimeters deep.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  11. Color view to Northwest of Phoenix

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This approximate color (SSI's red, green, and blue filters: 600, 530, and 480 nanometers) view was obtained on sol 2 by the Surface Stereo Imager (SSI) on board the Phoenix lander. The view is toward the northwest, showing polygonal terrain near the lander and out to the horizon.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  12. Phoenix Carries Soil to Wet Chemistry Lab

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This image taken by the Surface Stereo Imager on NASA's Phoenix Mars Lander shows the lander's Robotic Arm scoop positioned over the Wet Chemistry Lab delivery funnel on Sol 29, the 29th Martian day after landing, or June 24, 2008. The soil will be delivered to the instrument on Sol 30.

    This image has been enhanced to brighten the scene.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  13. Martian Soil Inside Phoenix's Robotic Arm Scoop

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This image from NASA's Phoenix Mars Lander's Robotic Arm Camera (RAC) shows material from the Martian surface captured by the Robotic Arm (RA) scoop during its first test dig and dump on the seventh Martian day of the mission, or Sol 7 (June 1, 2008). The test sample shown was taken from the digging area informally known as 'Knave of Hearts.'

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  14. Phoenix Deploying its Robotic Arm Elbow

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This animated gif is compiled of images from Phoenix's Stereo Surface Imager (SSI) taken on Sol 3. It shows the stair-step motion used to unstow the arm from a protective covering called the biobarrier. The last two moves allow the arm to stand straight up.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  15. Phoenix Mission Lander on Mars, Artist Concept

    NASA Image and Video Library

    2005-06-01

    NASA Phoenix Mars Lander, landed on May 25, 2008, and explored the history of water and monitored polar climate on Mars until communications ended in November, 2008, about six months after landing, when its solar panels ceased operating in the winter.

  16. Overnight Changes Recorded by Phoenix Conductivity Probe

    NASA Image and Video Library

    2008-12-15

    This graph presents simplified data from overnight measurements by the Thermal and Electrical Conductivity Probe on NASA Phoenix Mars Lander from noon of the mission 70th Martian day, or sol, to noon the following sol Aug. 5 to Aug. 6, 2008.

  17. Phoenix College Institutional Effectiveness, 1999-2000.

    ERIC Educational Resources Information Center

    Phoenix Coll., AZ.

    This report presents Phoenix College's (PC's) 1999-2000 institutional effectiveness annual report. The 1998-99 academic year was most notable for an important upswing in enrollment, the opening of the Fannin Library, and a continued increase in the diversity of students. Enrollment increases were noted in both fall and spring semesters, with a…

  18. Phoenix Violence Prevention Initiative, Phase II Report.

    ERIC Educational Resources Information Center

    Waits, Mary Jo; Johnson, Ryan; Kornreich, Toby; Klym, Mark; Leland, Karen

    In 1996, drawing from religious, educational, social services, media, neighborhoods, nonprofits, and health-providing sectors of the community, the Phoenix Violence Prevention Initiative (PVPI) was conceived. During Phase One of the initiative, the following seven points regarding prevention and prevention design strategies were assembled: (1)…

  19. Phoenix Conductivity Probe Inserted in Martian Soil

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This series of six images from the Robotic Arm Camera on NASA's Phoenix Mars Lander records the first time that the four spikes of the lander's thermal and electrical conductivity probe were inserted into Martian soil.

    The images were taken on July 8, 2008, during the Phoenix mission's 43rd Martian day, or sol, since landing. The insertion visible from the shadows cast on the ground on that sol was a validation test of the procedure. The spikes on the probe are about 1.5 centimeters or half an inch long.

    The science team will use the probe tool to assess how easily heat and electricity move through the soil from one spike to another. Such measurements can provide information about frozen or unfrozen water in the soil. The probe is mounted on the 'knuckle' of Phoenix's Robotic Arm. It has already been used for assessing water vapor in the atmosphere when it is held above the ground.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is led by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  20. Phoenix Conductivity Probe with Shadow and Toothmark

    NASA Technical Reports Server (NTRS)

    2008-01-01

    NASA's Phoenix Mars Lander inserted the four needles of its thermal and conductivity probe into Martian soil during the 98th Martian day, or sol, of the mission and left it in place until Sol 99 (Sept. 4, 2008).

    The Robotic Arm Camera on Phoenix took this image on the morning of Sol 99 after the probe was lifted away from the soil. The imprint left by the insertion is visible below the probe, and a shadow showing the probe's four needles is cast on a rock to the left.

    The thermal and conductivity probe measures how fast heat and electricity move from one needle to an adjacent one through the soil or air between the needles. Conductivity readings can be indicators about water vapor, water ice and liquid water.

    The probe is part of Phoenix's Microscopy, Electrochemistry and Conductivity suite of instruments.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  1. Phoenix Conductivity Probe Inserted into Martian Soil

    NASA Technical Reports Server (NTRS)

    2008-01-01

    NASA's Phoenix Mars Lander inserted the four needles of its thermal and conductivity probe into Martian soil during the 98th Martian day, or sol, of the mission and left it in place until Sol 99 (Sept. 4, 2008).

    The Robotic Arm Camera on Phoenix took this image on the morning of Sol 99 while the probe's needles were in the ground. The science team informally named this soil target 'Gandalf.'

    The thermal and conductivity probe measures how fast heat and electricity move from one needle to an adjacent one through the soil or air between the needles. Conductivity readings can be indicators about water vapor, water ice and liquid water.

    The probe is part of Phoenix's Microscopy, Electrochemistry and Conductivity suite of instruments.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  2. Phoenix La Mancha Trench in 3-D

    NASA Image and Video Library

    2008-10-09

    This anaglyph was taken by NASA Phoenix Mars Lander Surface Stereo Imager Oct. 7, 2008. The anaglyph highlights the depth of the trench, informally named La Mancha, and reveals the ice layer beneath the soil surface. 3D glasses are necessary.

  3. Contour Map of Mars Surface Beside Phoenix

    NASA Image and Video Library

    2008-12-15

    This color-coded elevation map of the local terrain on the north side of NASA Phoenix Mars Lander shows the contours of polygons and relationship of polygon boundaries to trenches and other features in the workspace of the lander Robotic Arm.

  4. Phoenix Award Winners: Books Worth Remembering.

    ERIC Educational Resources Information Center

    Piehl, Kathy

    1998-01-01

    Describes the Phoenix Award, which honors children's books which did not receive an award at publication (20 years in the past), but have withstood the test of time. Presents an annotated bibliography of winning titles under the categories of: Fantasy/Science Fiction; Historical Fiction (British, Depression Era, World War II, Other Wars, Other…

  5. Phoenix Laser Beam in Action on Mars

    NASA Image and Video Library

    2008-09-30

    The Surface Stereo Imager camera aboard NASA Phoenix Mars Lander acquired a series of images of the laser beam in the Martian night sky. Bright spots in the beam are reflections from ice crystals in the low level ice-fog.

  6. Digibaro pressure instrument onboard the Phoenix Lander

    NASA Astrophysics Data System (ADS)

    Harri, A.-M.; Polkko, J.; Kahanpää, H. H.; Schmidt, W.; Genzer, M. M.; Haukka, H.; Savijarv1, H.; Kauhanen, J.

    2009-04-01

    The Phoenix Lander landed successfully on the Martian northern polar region. The mission is part of the National Aeronautics and Space Administration's (NASA's) Scout program. Pressure observations onboard the Phoenix lander were performed by an FMI (Finnish Meteorological Institute) instrument, based on a silicon diaphragm sensor head manufactured by Vaisala Inc., combined with MDA data processing electronics. The pressure instrument performed successfully throughout the Phoenix mission. The pressure instrument had 3 pressure sensor heads. One of these was the primary sensor head and the other two were used for monitoring the condition of the primary sensor head during the mission. During the mission the primary sensor was read with a sampling interval of 2 s and the other two were read less frequently as a check of instrument health. The pressure sensor system had a real-time data-processing and calibration algorithm that allowed the removal of temperature dependent calibration effects. In the same manner as the temperature sensor, a total of 256 data records (8.53 min) were buffered and they could either be stored at full resolution, or processed to provide mean, standard deviation, maximum and minimum values for storage on the Phoenix Lander's Meteorological (MET) unit.The time constant was approximately 3s due to locational constraints and dust filtering requirements. Using algorithms compensating for the time constant effect the temporal resolution was good enough to detect pressure drops associated with the passage of nearby dust devils.

  7. Phoenix Conductivity Probe Inserted into Martian Soil

    NASA Technical Reports Server (NTRS)

    2008-01-01

    NASA's Phoenix Mars Lander inserted the four needles of its thermal and conductivity probe into Martian soil during the 98th Martian day, or sol, of the mission and left it in place until Sol 99 (Sept. 4, 2008).

    The Robotic Arm Camera on Phoenix took this image on the morning of Sol 99 while the probe's needles were in the ground. The science team informally named this soil target 'Gandalf.'

    The thermal and conductivity probe measures how fast heat and electricity move from one needle to an adjacent one through the soil or air between the needles. Conductivity readings can be indicators about water vapor, water ice and liquid water.

    The probe is part of Phoenix's Microscopy, Electrochemistry and Conductivity suite of instruments.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  8. Temperature Measurements Taken by Phoenix Spacecraft

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This chart plots the minimum daily atmospheric temperature measured by NASA's Phoenix Mars Lander spacecraft since landing on Mars. As the temperature increased through the summer season, the atmospheric humidity also increased. Clouds, ground fog, and frost were observed each night after the temperature started dropping.

  9. Faculty Web Grade Entry: University of Phoenix

    ERIC Educational Resources Information Center

    Elisala, Tandy R.

    2005-01-01

    The University of Phoenix is a large, private, four-year university with a commitment to providing timely and efficient student services. With continued growth and process improvement opportunities utilizing technology, the institution had an opportunity to automate and streamline grade processing. This article focuses on the Faculty Web Grade…

  10. Phoenix Mars Lander with Solar Arrays Open

    NASA Technical Reports Server (NTRS)

    2006-01-01

    NASA's next Mars-bound spacecraft, the Phoenix Mars Lander, was partway through assembly and testing at Lockheed Martin Space Systems, Denver, in September 2006, progressing toward an August 2007 launch from Florida. In this photograph, spacecraft specialists work on the lander after its fan-like circular solar arrays have been spread open for testing. The arrays will be in this configuration when the spacecraft is active on the surface of Mars.

    Phoenix will land in icy soils near the north polar permanent ice cap of Mars and explore the history of the water in these soils and any associated rocks, while monitoring polar climate. It will dig into the surface, test scooped-up samples for carbon-bearing compounds and serve as NASA's first exploration of a potential modern habitat on Mars.

    The Phoenix mission is led by Principal Investigator Peter H. Smith of the University of Arizona, Tucson, with project management at NASA's Jet Propulsion Laboratory and development partnership with Lockheed Martin Space Systems. International contributions for Phoenix are provided by the Canadian Space Agency, the University of Neuchatel (Switzerland), the University of Copenhagen, and the Max Planck Institute in Germany. JPL is a division of the California Institute of Technology in Pasadena.

  11. How Phoenix Gets a Look at its Footing

    NASA Technical Reports Server (NTRS)

    2008-01-01

    [figure removed for brevity, see original site] Click on the image for the animation

    This artist's animation shows how NASA's three-legged Phoenix Mars Lander is able to get a better look at its footing and the physical characteristics of the underlying soil on the surface of the Red Planet. Because the Surface Stereo Imager is able to swivel in any compass direction as well as up and down, it can 'see' and take snapshots of the footpad beneath the camera's location near one edge of the spacecraft deck.

    Each footpad is about the size of a large dinner plate, measuring 11.5 inches from rim to rim. The base of the footpad is shaped like the bottom of a shallow bowl to provide stability.

    The footpad image was taken by the spacecraft's Surface Stereo Imager at 17:07 local Mars time, shortly after landing May 25, 2008.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  12. Phoenix Lander on Mars with Surrounding Terrain, Polar Projection

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This view is a polar projection that combines more than 500 exposures taken by the Surface Stereo Imager camera on NASA's Mars Phoenix Lander and projects them as if looking down from above.

    The black circle on the spacecraft is where the camera itself is mounted on the lander, out of view in images taken by the camera. North is toward the top of the image. The lander's meteorology mast extends above the southwest horzon and is topped by the telltale wind gauge.

    The ground surface around the lander has polygonal patterning similar to patterns in permafrost areas on Earth. The landing site is at 68.22 degrees north latitude, 234.25 degrees east longitude on Mars.

    This view in approximately true color comprises more than 100 different Stereo Surface Imager pointings, with images taken through three different filters at each pointing. The images were taken throughout the period from the 13th Martian day, or sol, after landing to the 47th sol (June 5 through July 12, 2008). The lander's Robotic Arm is cut off in this mosaic view because component images were taken when the arm was out of the frame.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  13. Martian Arctic Dust Devil, Phoenix Sol 104

    NASA Technical Reports Server (NTRS)

    2008-01-01

    The Surface Stereo Imager on NASA's Phoenix Mars Lander caught this dust devil in action west-southwest of the lander at 11:16 a.m. local Mars time on Sol 104, or the 104th Martian day of the mission, Sept. 9, 2008.

    Dust devils have not been detected in any Phoenix images from earlier in the mission, but at least six were observed in a dozen images taken on Sol 104.

    Dust devils are whirlwinds that often occur when the Sun heats the surface of Mars, or some areas on Earth. The warmed surface heats the layer of atmosphere closest to it, and the warm air rises in a whirling motion, stirring dust up from the surface like a miniature tornado.

    The dust devil visible in the center of this image just below the horizon is estimated to be about 400 meters (about 1,300 feet) from Phoenix, and 4 meters (13 feet) in diameter. It is much smaller than dust devils that have been observed by NASA's Mars Exploration Rover Spirit much closer to the equator. It is closer in size to dust devils seen from orbit in the Phoenix landing region, though still smaller than those.

    The image has been enhanced to make the dust devil easier to see.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  14. More Soil Delivered to Phoenix Lab

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This image, taken by NASA's Phoenix Mars Lander's Surface Stereo Imager, documents the delivery of a soil sample from the 'Snow White' trench to the Wet Chemistry Laboratory. A small pile of soil is visible on the lower edge of the second cell from the top.This deck-mounted lab is part of Phoenix's Microscopy, Electrochemistry and Conductivity Analyzer (MECA).

    The delivery was made on Sept. 12, 2008, which was Sol 107 (the 107th Martian day) of the mission, which landed on May 25, 2008.

    The Wet Chemistry Laboratory mixes Martian soil with an aqueous solution from Earth as part of a process to identify soluble nutrients and other chemicals in the soil. Preliminary analysis of this soil confirms that it is alkaline, and composed of salts and other chemicals such as perchlorate, sodium, magnesium, chloride and potassium. This data validates prior results from that same location, said JPL's Michael Hecht, the lead scientist for MECA.

    In the coming days, the Phoenix team will also fill the final four of eight single-use ovens on another soil-analysis instrument, the Thermal and Evolved Gas Analyzer, or TEGA. The team's strategy is to deliver as many samples as possible before the power produced by Phoenix's solar panels declines due to the end of the Martian summer.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  15. Martian Arctic Dust Devil, Phoenix Sol 104

    NASA Technical Reports Server (NTRS)

    2008-01-01

    The Surface Stereo Imager on NASA's Phoenix Mars Lander caught this dust devil in action west-southwest of the lander at 11:16 a.m. local Mars time on Sol 104, or the 104th Martian day of the mission, Sept. 9, 2008.

    Dust devils have not been detected in any Phoenix images from earlier in the mission, but at least six were observed in a dozen images taken on Sol 104.

    Dust devils are whirlwinds that often occur when the Sun heats the surface of Mars, or some areas on Earth. The warmed surface heats the layer of atmosphere closest to it, and the warm air rises in a whirling motion, stirring dust up from the surface like a miniature tornado.

    The dust devil visible in the center of this image just below the horizon is estimated to be about 400 meters (about 1,300 feet) from Phoenix, and 4 meters (13 feet) in diameter. It is much smaller than dust devils that have been observed by NASA's Mars Exploration Rover Spirit much closer to the equator. It is closer in size to dust devils seen from orbit in the Phoenix landing region, though still smaller than those.

    The image has been enhanced to make the dust devil easier to see.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  16. Phoenix - the First Mars Scout Mission

    NASA Technical Reports Server (NTRS)

    Goldstein, Barry; Shotwell, Robert

    2008-01-01

    As the first of the new Mars Scouts missions, the Phoenix project was selected by NASA in August of 2003. Four years later, almost to the day, Phoenix was launched from Cape Canaveral Air Station and successfully injected into an interplanetary trajectory on its way to Mars. This paper will highlight some of the key changes since the 2006 IEEE paper of the same name, as well as activities, challenges and problems encountered on the way to the launch pad. Phoenix Follows the water responding directly to the recently published data from Dr. William Boynton, PI (and Phoenix co-I) of the Mars Odyssey Gamma Ray Spectrometer (GRS). GRS data indicate extremely large quantities of water ice (up to 50% by mass) within the upper 50 cm of the northern polar regolith. Phoenix will land within the north polar region at 68.2 N, 233.4 W identified by GRS to harbor near surface water ice and provide in-situ confirmation of this extraordinary find. Our mission will investigate water in all its phases, and will investigate the history of water as evidenced in the soil characteristics that will be carefully examined by the powerful suite of onboard instrumentation. Access to the critical subsurface region expected to contain this information is made possible by a third generation robotic arm capable of excavating the expected Martian regolith to a depth of 1m. Phoenix has four primary science objectives: 1) Determine the polar climate and weather, interaction with the surface, and composition of the lower atmosphere around 70 N for at least 90 sols focusing on water, ice, dust, noble gases, and CO2. Determine the atmospheric characteristics during descent through the atmosphere. 2) Characterize the geomorphology and active processes shaping the northern plains and the physical properties of the near surface regolith focusing on the role of water. 3) Determine the aqueous mineralogy and chemistry as well as the adsorbed gases and organic content of the regolith. Verify the Odyssey

  17. The Return of the PHOENIX Universe

    NASA Astrophysics Data System (ADS)

    Lehners, Jean-Luc; Steinhardt, Paul J.; Turok, Neil

    Georges Lemaitre introduced the term "phoenix universe" to describe an oscillatory cosmology with alternating periods of gravitational collapse and expansion. This model is ruled out observationally, because it requires a supercritical mass density and cannot accommodate dark energy. However, a new cyclic theory of the universe has been proposed that evades these problems. In a recent elaboration of this picture, almost the entire universe observed today is fated to become entrapped inside black holes, but a tiny region will emerge from these ashes like a phoenix to form an even larger smooth, flat universe filled with galaxies, stars, planets, and, presumably, life. Survival depends crucially on dark energy and suggests a reason why its density is small and positive today.

  18. Phoenix Robotic Arm Scoop with Rasp

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This drawing shows a side view of NASA's Phoenix Mars Lander's scoop with various tools for acquiring soil, icy soil and ice samples.

    The front blade, at left, is for scraping. A secondary blade can scrape hard materials.

    The motorized rasp, protruding at the bottom on the image, can penetrate the hard icy soil and acquire the cuttings produced through the rear chamber of the scoop. The rasp is a tungsten carbide cutting bit mounted within a pivoting housing that allows the bit to protrude during sample acquisition.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is led by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  19. Phoenix Robotic Arm's Workspace After 90 Sols

    NASA Technical Reports Server (NTRS)

    2008-01-01

    During the first 90 Martian days, or sols, after its May 25, 2008, landing on an arctic plain of Mars, NASA's Phoenix Mars Lander dug several trenches in the workspace reachable with the lander's robotic arm.

    The lander's Surface Stereo Imager camera recorded this view of the workspace on Sol 90, early afternoon local Mars time (overnight Aug. 25 to Aug. 26, 2008). The shadow of the the camera itself, atop its mast, is just left of the center of the image and roughly a third of a meter (one foot) wide.

    The workspace is on the north side of the lander. The trench just to the right of center is called 'Neverland.'

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  20. Results from the Phoenix Mars Mission

    NASA Astrophysics Data System (ADS)

    Smith, Peter

    The Phoenix mission investigated the soil-ice interface in the martian arctic for 5 months starting May 25, 2008. Major goals of the mission were the examination of physical environment as well as the soil chemistry and mineralogy to understand the role of water, if any, in their formation. An additional goal was to assess the habitability in terms of the necessary ingredients to support life as we know it on Earth. An ice layer was uncovered at an average depth of 5 cm. Both a pure ice lens and ice-cemented soil were examined; the TEGA instrument confirmed water ice. First results from the mission revealed calcium carbonate composed 5 The Phoenix mission was a collaboration between the University of Arizona, the Jet Propulsion Lab, and Lockheed Martin. An international team of scientists supported the collection and analysis of data.

  1. Astronomical research at the Hopkins Phoenix Observatory

    NASA Technical Reports Server (NTRS)

    Hopkins, J. L.

    1985-01-01

    After trying astrophotography and radio astronomy it was decided that the best way to do meaningful astronomical research at a small private observatory was by doing photoelectric photometry. Having the observatory located in the back yard of a private residence affors the luxury of observing any time the sky conditions permit. Also modest equipment is all that is needed to do accurate UBV photometry of stars 8th magnitude and brighter. Since beginning in 1980 the Hopkins Phoenix Observatory has published papers on several RS CVn star systems, 31 Cygni, 22 Vul, 18 Tau Per, and has followed the 1982-1984 eclipse of Epsilon Aurigae from its start to the present with over 1000 UBV measurements. In addition the Hopkins Phoenix Observatory has developed several pieces of photometry equipment including the HPO PEPH-101 photometer head and photon counting electronics.

  2. Phoenix--the first Mars Scout mission.

    PubMed

    Shotwell, Robert

    2005-01-01

    NASA has initiated the first of a new series of missions to augment the current Mars Program. In addition to the systematic series of planned, directed missions currently comprising the Mars Program plan, NASA has started a series of Mars Scout missions that are low cost, price fixed, Principal [correction of Principle] Investigator-led projects. These missions are intended to provide an avenue for rapid response to discoveries made as a result of the primary Mars missions, as well as allow more risky technologies and approaches to be applied in the investigation of Mars. The first in this new series is the Phoenix mission which was selected as part of a highly competitive process. Phoenix will use the Mars 2001 Lander that was discontinued in 2000 and apply a new set of science objectives and mission objectives and will validate this soft lander architecture for future applications. This paper will provide an overview of both the Program and the Project.

  3. Overnight Changes Recorded by Phoenix Conductivity Probe

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This graph presents simplified data from overnight measurements by the Thermal and Electrical Conductivity Probe on NASA's Phoenix Mars Lander from noon of the mission's 70th Martian day, or sol, to noon the following sol (Aug. 5 to Aug. 6, 2008).

    The graph shows that water disappeared from the atmosphere overnight, at the same time that electrical measurements detected changes consistent with addition of water to the soil.

    Water in soil appears to increase overnight, when water in the atmosphere disappears.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  4. Overnight Changes Recorded by Phoenix Conductivity Probe

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This graph presents simplified data from overnight measurements by the Thermal and Electrical Conductivity Probe on NASA's Phoenix Mars Lander from noon of the mission's 70th Martian day, or sol, to noon the following sol (Aug. 5 to Aug. 6, 2008).

    The graph shows that water disappeared from the atmosphere overnight, at the same time that electrical measurements detected changes consistent with addition of water to the soil.

    Water in soil appears to increase overnight, when water in the atmosphere disappears.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  5. Phoenix Robotic Arm Scoop with Rasp

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This drawing shows a side view of NASA's Phoenix Mars Lander's scoop with various tools for acquiring soil, icy soil and ice samples.

    The front blade, at left, is for scraping. A secondary blade can scrape hard materials.

    The motorized rasp, protruding at the bottom on the image, can penetrate the hard icy soil and acquire the cuttings produced through the rear chamber of the scoop. The rasp is a tungsten carbide cutting bit mounted within a pivoting housing that allows the bit to protrude during sample acquisition.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is led by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  6. Phoenix Robotic Arm's Workspace After 90 Sols

    NASA Technical Reports Server (NTRS)

    2008-01-01

    During the first 90 Martian days, or sols, after its May 25, 2008, landing on an arctic plain of Mars, NASA's Phoenix Mars Lander dug several trenches in the workspace reachable with the lander's robotic arm.

    The lander's Surface Stereo Imager camera recorded this view of the workspace on Sol 90, early afternoon local Mars time (overnight Aug. 25 to Aug. 26, 2008). The shadow of the the camera itself, atop its mast, is just left of the center of the image and roughly a third of a meter (one foot) wide.

    The workspace is on the north side of the lander. The trench just to the right of center is called 'Neverland.'

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  7. Phoenix Mars Lander's Chemistry Lab in a Box

    NASA Technical Reports Server (NTRS)

    2007-01-01

    The wet chemistry laboratory on NASA's Phoenix Mars Lander has four teacup-size beakers. This photograph shows one of them. The laboratory is part of the spacecraft's Microscopy, Electrochemistry and Conductivity Analyzer.

    Each beaker will be used only once, for assessing soluble chemicals in a sample of Martian soil by mixing water with the sample to a soupy consistency and keeping it warm enough to remain liquid during the analysis.

    On the inner surface of the beaker are 26 sensors, mostly electrodes behind selectively permeable membranes or gels. Some sensors will give information about the acidity or alkalinity of the soil sample. Others will gauge concentrations of such ions as chlorides, bromides, magnesium, calcium and potassium. Comparisons of the concentrations of water-soluble ions in soil samples from different depths below the surface of the landing site may provide clues to the history of the water in the soil.

  8. Phoenix Mars Lander's Chemistry Lab in a Box

    NASA Technical Reports Server (NTRS)

    2007-01-01

    The wet chemistry laboratory on NASA's Phoenix Mars Lander has four teacup-size beakers. This photograph shows one of them. The laboratory is part of the spacecraft's Microscopy, Electrochemistry and Conductivity Analyzer.

    Each beaker will be used only once, for assessing soluble chemicals in a sample of Martian soil by mixing water with the sample to a soupy consistency and keeping it warm enough to remain liquid during the analysis.

    On the inner surface of the beaker are 26 sensors, mostly electrodes behind selectively permeable membranes or gels. Some sensors will give information about the acidity or alkalinity of the soil sample. Others will gauge concentrations of such ions as chlorides, bromides, magnesium, calcium and potassium. Comparisons of the concentrations of water-soluble ions in soil samples from different depths below the surface of the landing site may provide clues to the history of the water in the soil.

  9. Sprinkle Test by Phoenix's Robotic Arm (Movie)

    NASA Technical Reports Server (NTRS)

    2008-01-01

    NASA's Phoenix Mars Lander used its Robotic Arm during the mission's 15th Martian day since landing (June 9, 2008) to test a 'sprinkle' method for delivering small samples of soil to instruments on the lander deck. This sequence of four images from the spacecraft's Surface Stereo Imager covers a period of 20 minutes from beginning to end of the activity.

    In the single delivery of a soil sample to a Phoenix instrument prior to this test, the arm brought the scooped up soil over the instrument's opened door and turned over the scoop to release the soil. The sprinkle technique, by contrast, holds the scoop at a steady angle and vibrates the scoop by running the motorized rasp located beneath the scoop. This gently jostles some material out of the scoop to the target below.

    For this test, the target was near the upper end the cover of the Microscopy, Electrochemistry and Conductivity Analyzer instrument suite, or MECA. The cover is 20 centimeters (7.9 inches) across. The scoop is about 8.5 centimeters (3.3 inches) across.

    Based on the test's success in delivering a small quantity and fine-size particles, the Phoenix team plans to use the sprinkle method for delivering samples to MECA and to the Thermal and Evolved-Gas Analyzer, or TEGA. The next planned delivery is to MECA's Optical Microscope, via the port in the MECA cover visible at the bottom of these images.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  10. Merged dust climatology in Phoenix, Arizona based on satellite and station data

    NASA Astrophysics Data System (ADS)

    Lei, Hang; Wang, Julian X. L.; Tong, Daniel Q.; Lee, Pius

    2016-11-01

    In order to construct climate quality long-term dust storm dataset, merged dust storm climatology in Phoenix is developed based on three data sources: regular meteorological records, in situ air quality measurements, and satellite remote sensing observations. The result presented in this paper takes into account the advantages of each dataset and integrates individual analyses demonstrated and presented in previous studies that laid foundation to reconstruct a consistent and continuous time series of dust frequency. A key for the merging procedure is to determine analysis criteria suitable for each individual data source. A practical application to historic records of dust storm activities over the Phoenix area is presented to illustrate detailed steps, advantages, and limitations of the newly developed process. Three datasets are meteorological records from the Sky Harbor station, satellite observed aerosol optical depth data from moderate resolution imaging spectroradiometer, and the U.S. Environmental Protection Agency Air Quality System particulate matter data of eight sites surrounding Phoenix. Our purpose is to construct dust climatology over the Phoenix region for the period 1948-2012. Data qualities of the reconstructed dust climatology are assessed based on the availability and quality of the input data. The period during 2000-2012 has the best quality since all datasets are well archived. The reconstructed climatology shows that dust storm activities over the Phoenix region have large interannual variability. However, seasonal variations show a skewed distribution with higher frequency of dust storm activities in July and August and relatively quiet during the rest of months. Combining advantages of all the available datasets, this study presents a merged product that provides a consistent and continuous time series of dust storm activities suitable for climate studies.

  11. Digging Movie from Phoenix's Sol 18

    NASA Technical Reports Server (NTRS)

    2008-01-01

    The Surface Stereo Imager on NASA's Phoenix Mars Lander recorded the images combined into this movie of the lander's Robotic Arm enlarging and combining the two trenches informally named 'Dodo' (left) and 'Goldilocks.'

    The 21 images in this sequence were taken over a period of about 2 hours during Phoenix's Sol 18 (June 13, 2008), or the 18th Martian day since landing.

    The main purpose of the Sol 18 dig was to dig deeper for learning the depth of a hard underlying layer. A bright layer, possibly ice, was increasingly exposed as the digging progressed. Further digging and scraping in the combined Dodo-Goldilocks trench was planned for subsequent sols.

    The combined trench is about 20 centimeters (about 8 inches) wide. The depth at the end of the Sol 18 digging is 5 to 6 centimeters (about 2 inches).

    The Goldilocks trench was the source of soil samples 'Baby Bear' and 'Mama Bear,' which were collected on earlier sols and delivered to instruments on the lander deck. The Dodo trench was originally dug for practice in collecting and depositing soil samples.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  12. Digging Movie from Phoenix's Sol 18

    NASA Technical Reports Server (NTRS)

    2008-01-01

    The Surface Stereo Imager on NASA's Phoenix Mars Lander recorded the images combined into this movie of the lander's Robotic Arm enlarging and combining the two trenches informally named 'Dodo' (left) and 'Goldilocks.'

    The 21 images in this sequence were taken over a period of about 2 hours during Phoenix's Sol 18 (June 13, 2008), or the 18th Martian day since landing.

    The main purpose of the Sol 18 dig was to dig deeper for learning the depth of a hard underlying layer. A bright layer, possibly ice, was increasingly exposed as the digging progressed. Further digging and scraping in the combined Dodo-Goldilocks trench was planned for subsequent sols.

    The combined trench is about 20 centimeters (about 8 inches) wide. The depth at the end of the Sol 18 digging is 5 to 6 centimeters (about 2 inches).

    The Goldilocks trench was the source of soil samples 'Baby Bear' and 'Mama Bear,' which were collected on earlier sols and delivered to instruments on the lander deck. The Dodo trench was originally dug for practice in collecting and depositing soil samples.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  13. Flight Testing and Test Instrumentation of PHOENIX

    NASA Astrophysics Data System (ADS)

    Janovsky, R.; Behr, R.

    2005-02-01

    Within the frame of the German national ASTRA program, the need for in-flight experimentation as a key element in the development of the next generation launcher was addressed by the Phoenix project. The Phoenix 1 flight test vehicle was designed to demonstrate the un-powered horizontal landing of a representative, winged RLV configuration. The Phoenix 1 flight test vehicle is downscaled from the reference RLV shape "Hopper", with the dimensions of 7.8m overall length, 3.8m span, and 1200kg mass. In order to be representative of a full scale RLV, the scaling method preserves all features challenging the automatic landing from the flight control point of view. These are in particular the poor flying qualities of the static unstable vehicle and the high landing velocity of 71m/s, which is same as for the full scale vehicle. The landing demonstration scenario comprises a drop from the helicopter approximately 6km ahead of the runway threshold at 2.4km above runway level. The subsequent free flight includes an accelerating dive to merge with a steep final approach path representative of an RLV, followed by a long flare, touch down on the runway, and rollout to standstill. Besides its mandatory avionics system, the vehicle is also equipped with an additional flight test instrumentation to identify local aerodynamic flow and structural stress. This FTI system is designed to collect data by recording about 130 sensor signals during flight. This test instrumentation system was operated during a test campaign dedicated to verify the aerodynamic data base of Phoenix in the Dutch-German Wind-tunnel (DNW) in August 2003 and during three automatic landing flight tests after helicopter drop in May 2004. Post flight analysis of these data allows to validate the design models and the development tools in order to establish a flight validated data base for future work. This paper gives an overview on the Phoenix system including the flight test instrumentation, the test program and

  14. Martian Dust Devil Movie, Phoenix Sol 104

    NASA Technical Reports Server (NTRS)

    2008-01-01

    The Surface Stereo Imager on NASA's Phoenix Mars Lander caught this dust devil in action west of the lander in four frames shot about 50 seconds apart from each other between 11:53 a.m. and 11:56 a.m. local Mars time on Sol 104, or the 104th Martian day of the mission, Sept. 9, 2008.

    Dust devils have not been detected in any Phoenix images from earlier in the mission, but at least six were observed in a dozen images taken on Sol 104.

    Dust devils are whirlwinds that often occur when the Sun heats the surface of Mars, or some areas on Earth. The warmed surface heats the layer of atmosphere closest to it, and the warm air rises in a whirling motion, stirring dust up from the surface like a miniature tornado.

    The dust devil visible in this sequence was about 1,000 meters (about 3,300 feet) from the lander when the first frame was taken, and had moved to about 1,700 meters (about 5,600 feet) away by the time the last frame was taken about two and a half minutes later. The dust devil was moving westward at an estimated speed of 5 meters per second (11 miles per hour), which is similar to typical late-morning wind speed and direction indicated by the telltale wind gauge on Phoenix.

    This dust devil is about 5 meters (16 feet) in diameter. This is much smaller than dust devils that have been observed by NASA's Mars Exploration Rover Spirit much closer to the equator. It is closer in size to dust devils seen from orbit in the Phoenix landing region, though still smaller than those..

    The image has been enhanced to make the dust devil easier to see. Some of the frame-to-frame differences in the appearance of foreground rocks is because each frame was taken through a different color filter.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  15. Phoenix Lander on Mars with Surrounding Terrain, Vertical Projection

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This view is a vertical projection that combines more than 500 exposures taken by the Surface Stereo Imager camera on NASA's Mars Phoenix Lander and projects them as if looking down from above.

    The black circle on the spacecraft is where the camera itself is mounted on the lander, out of view in images taken by the camera. North is toward the top of the image. The height of the lander's meteorology mast, extending toward the southwest, appears exaggerated because that mast is taller than the camera mast.

    This view in approximately true color covers an area about 30 meters by 30 meters (about 100 feet by 100 feet). The landing site is at 68.22 degrees north latitude, 234.25 degrees east longitude on Mars.

    The ground surface around the lander has polygonal patterning similar to patterns in permafrost areas on Earth.

    This view comprises more than 100 different Stereo Surface Imager pointings, with images taken through three different filters at each pointing. The images were taken throughout the period from the 13th Martian day, or sol, after landing to the 47th sol (June 5 through July 12, 2008). The lander's Robotic Arm is cut off in this mosaic view because component images were taken when the arm was out of the frame.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  16. Program Description for the Phoenix Reception and Assessment Center.

    ERIC Educational Resources Information Center

    Datema, Thea; And Others

    Phoenix Reception and Assessment Center (PRAC) is a non-secure detention and assessment center for up to 15 Wayne County delinquent, adolescent males who have been committed to the Michigan Department of Social Services for care, treatment and supervision. Adolescents, ages 12 through 18, are eligible for placement at Phoenix according to the…

  17. University of Phoenix Lets Students Find Answers Virtually

    ERIC Educational Resources Information Center

    Wasley, Paula

    2008-01-01

    This article talks about a software designed by the University of Phoenix for its business, information-technology, education, and health-care courses. Through the university's "virtual organizations"--online teaching tools designed to simulate the experience of working at a typical corporation, school, or government agency, Phoenix students can…

  18. Selected Hydrologic Applications of LANDSAT-2 Data: an Evaluation. [Snowmelt in the American River Basin and soil moisture studies at the Phoenix, Arizona Test Site and at Luverne, Minnesota

    NASA Technical Reports Server (NTRS)

    Wiesnet, D. R.; Mcginnis, D. F., Jr.; Matson, M. (Principal Investigator)

    1978-01-01

    The author has identified the following significant results. Estimates of soil moisture were obtained from visible, near-IR gamma ray and microwave data. Attempts using GOES thermal-IR were unsuccessful due to resolutions (8 km). Microwaves were the most effective at soil moisture estimates, with and without vegetative cover. Gamma rays provided only one value for the test site, produced by many data points obtained from overlapping 150 meter diameter circles. Even though the resulting averaged value was near the averaged field moisture value, this method suffers from atmospheric contaminants, the need to fly at low altitudes, and the necessity of prior calibration of a given site. Visible and near-IR relationships are present for bare fields but appear to be limited to soil moisture levels between 5 and 20%. The densely vegetated alfalfa fields correlated with near-IR reflectance only; soil moisture values from wheat fields showed no relation to either or near-IR MSS data.

  19. Microscopes for NASA's Phoenix Mars Lander

    NASA Technical Reports Server (NTRS)

    2007-01-01

    One part of the Microscopy, Electrochemistry, and Conductivity Analyzer instrument for NASA's Phoenix Mars Lander is a pair of telescopes with a special wheel (on the right in this photograph) for presenting samples to be inspected with the microscopes. A horizontally mounted optical microscope (on the left in this photograph) and an atomic force microscope will examine soil particles and possibly ice particles.

    The shapes and the size distributions of soil particles may tell scientists about environmental conditions the material has experienced. Tumbling rounds the edges. Repeated wetting and freezing causes cracking. Clay minerals formed during long exposure to water have distinctive, platy particles shapes.

  20. Microscopes for NASA's Phoenix Mars Lander

    NASA Technical Reports Server (NTRS)

    2007-01-01

    One part of the Microscopy, Electrochemistry, and Conductivity Analyzer instrument for NASA's Phoenix Mars Lander is a pair of telescopes with a special wheel (on the right in this photograph) for presenting samples to be inspected with the microscopes. A horizontally mounted optical microscope (on the left in this photograph) and an atomic force microscope will examine soil particles and possibly ice particles.

    The shapes and the size distributions of soil particles may tell scientists about environmental conditions the material has experienced. Tumbling rounds the edges. Repeated wetting and freezing causes cracking. Clay minerals formed during long exposure to water have distinctive, platy particles shapes.

  1. Chemistry Lab for Phoenix Mars Lander

    NASA Technical Reports Server (NTRS)

    2007-01-01

    The science payload of NASA's Phoenix Mars Lander includes a multi-tool instrument named the Microscopy, Electrochemistry, and Conductivity Analyzer (MECA). The instrument's wet chemistry laboratory, prominent in this photograph, will measure a range of chemical properties of Martian soil samples, such as the presence of dissolved salts and the level of acidity or alkalinity. Other tools that are parts of the instrument are microscopes that will examine samples' mineral grains and a probe that will check the soil's thermal and electrical properties.

  2. Chemistry Lab for Phoenix Mars Lander

    NASA Technical Reports Server (NTRS)

    2007-01-01

    The science payload of NASA's Phoenix Mars Lander includes a multi-tool instrument named the Microscopy, Electrochemistry, and Conductivity Analyzer (MECA). The instrument's wet chemistry laboratory, prominent in this photograph, will measure a range of chemical properties of Martian soil samples, such as the presence of dissolved salts and the level of acidity or alkalinity. Other tools that are parts of the instrument are microscopes that will examine samples' mineral grains and a probe that will check the soil's thermal and electrical properties.

  3. The Phoenix Mars Lander Robotic Arm

    NASA Technical Reports Server (NTRS)

    Bonitz, Robert; Shiraishi, Lori; Robinson, Matthew; Carsten, Joseph; Volpe, Richard; Trebi-Ollennu, Ashitey; Arvidson, Raymond E.; Chu, P. C.; Wilson, J. J.; Davis, K. R.

    2009-01-01

    The Phoenix Mars Lander Robotic Arm (RA) has operated for over 150 sols since the Lander touched down on the north polar region of Mars on May 25, 2008. During its mission it has dug numerous trenches in the Martian regolith, acquired samples of Martian dry and icy soil, and delivered them to the Thermal Evolved Gas Analyzer (TEGA) and the Microscopy, Electrochemistry, and Conductivity Analyzer (MECA). The RA inserted the Thermal and Electrical Conductivity Probe (TECP) into the Martian regolith and positioned it at various heights above the surface for relative humidity measurements. The RA was used to point the Robotic Arm Camera to take images of the surface, trenches, samples within the scoop, and other objects of scientific interest within its workspace. Data from the RA sensors during trenching, scraping, and trench cave-in experiments have been used to infer mechanical properties of the Martian soil. This paper describes the design and operations of the RA as a critical component of the Phoenix Mars Lander necessary to achieve the scientific goals of the mission.

  4. The Phoenix Mars Lander Robotic Arm

    NASA Technical Reports Server (NTRS)

    Bonitz, Robert; Shiraishi, Lori; Robinson, Matthew; Carsten, Joseph; Volpe, Richard; Trebi-Ollennu, Ashitey; Arvidson, Raymond E.; Chu, P. C.; Wilson, J. J.; Davis, K. R.

    2009-01-01

    The Phoenix Mars Lander Robotic Arm (RA) has operated for over 150 sols since the Lander touched down on the north polar region of Mars on May 25, 2008. During its mission it has dug numerous trenches in the Martian regolith, acquired samples of Martian dry and icy soil, and delivered them to the Thermal Evolved Gas Analyzer (TEGA) and the Microscopy, Electrochemistry, and Conductivity Analyzer (MECA). The RA inserted the Thermal and Electrical Conductivity Probe (TECP) into the Martian regolith and positioned it at various heights above the surface for relative humidity measurements. The RA was used to point the Robotic Arm Camera to take images of the surface, trenches, samples within the scoop, and other objects of scientific interest within its workspace. Data from the RA sensors during trenching, scraping, and trench cave-in experiments have been used to infer mechanical properties of the Martian soil. This paper describes the design and operations of the RA as a critical component of the Phoenix Mars Lander necessary to achieve the scientific goals of the mission.

  5. Propulsive Maneuver Design for the 2007 Mars Phoenix Lander Mission

    NASA Technical Reports Server (NTRS)

    Raofi, Behzad; Bhat, Ramachandra S.; Helfrich, Cliff

    2008-01-01

    On May 25, 2008, the Mars Phoenix Lander (PHX) successfully landed in the northern planes of Mars in order to continue and complement NASA's "follow the water" theme as its predecessor Mars missions, such as Mars Odyssey (ODY) and Mars Exploration Rovers, have done in recent years. Instruments on the lander, through a robotic arm able to deliver soil samples to the deck, will perform in-situ and remote-sensing investigations to characterize the chemistry of materials at the local surface, subsurface, and atmosphere. Lander instruments will also identify the potential history of key indicator elements of significance to the biological potential of Mars, including potential organics within any accessible water ice. Precise trajectory control and targeting were necessary in order to achieve the accurate atmospheric entry conditions required for arriving at the desired landing site. The challenge for the trajectory control maneuver design was to meet or exceed these requirements in the presence of spacecraft limitations as well as other mission constraints. This paper describes the strategies used, including the specialized targeting specifically developed for PHX, in order to design and successfully execute the propulsive maneuvers that delivered the spacecraft to its targeted landing site while satisfying the planetary protection requirements in the presence of flight system constraints.

  6. The 2001 Phoenix Sunrise Experiment: Vertical Mixing and Chemistry During the Morning Transition in Phoenix

    SciTech Connect

    Doran, J C.; Berkowitz, Carl M.; Coulter, Richard L.; Shaw, William J.; Spicer, Chet W.

    2003-05-01

    A field experiment was carried out in Phoenix during June 2001 to examine the role of vertical mixing on the ozone chemistry of the boundary layer during the morning transition from stable to unstable atmospheric conditions. A combination of surface instruments, instruments located on two floors of a 39-story building in downtown Phoenix, and an instrumented airplane was used to characterize the evolving chemistry in the lowest 650 m of the atmosphere. Remote sensing and in situ platforms were used to obtained detailed profiles of winds and temperatures during the early morning hours and for several hours after sunrise. The analysis presented in this paper focuses on vertical profiles of CO, ozone, and NO/NOy measured on the building and their relationship to the morning boundary layer evolution over Phoenix. Some features were found that are consistent with a simple conceptual picture of nighttime trapping of pollutants in a stable surface layer and a subsequent release the following morning. In some instances, however, evidence of significant vertical mixing was found during the early morning well before the times expected for the development of convective mixing after sunrise. A satisfactory explanation for these observations has not yet been found.

  7. Project Phoenix and beyond. Pesek Lecture.

    PubMed

    Tarter, J

    1997-01-01

    Although there are no federally funded projects at this time, SETI (the search for extraterrestrial intelligence) is a vigorous exploratory science. There are currently eight observational programs on telescopes around the world, of which the Phoenix Project is the most comprehensive. Most of these projects are rooted in the conclusions of the pioneering studies of the early 1970's that are summarized in the Cyclops Report. Technology has experienced an exponential growth over the past two and a half decades. It is reasonable to reassess the Cyclops conclusions as SETI enters the next century. Listening for radio signals is still the preferred method of searching, however new technologies are making searches at other wavelengths possible and are modifying the ways in which the radio searches can and should be conducted. It may be economically feasible to undertake the construction of very large telescopes that can simultaneously provide multiple beams on the sky for use by SETI and the radioastronomy community.

  8. View of Phoenix, Arizona metropolitan area

    NASA Technical Reports Server (NTRS)

    1973-01-01

    A near vertical view of the Phoenix, Arizona metropolitan area is seen in this Skyalb 3 Earth Resources Experiments Package S190-B (five-inch earth terrain camera) photograph taken from the Skylab space station in earth orbit. Also in the picture are Scottsdale, Paradise Valley, Tempe, Mesa, Laveen, Komatke, Salt River Indian Reseravation, and part of the Gila River Indian Reservation. Features which can be detected from the photograph include: cultural patterns defined by commercial, industrial, agricultural and residential areas; transportation networks consisting of major corridors, primary, secondary, and feeder streets; major urban developments on the area such as airports, Squaw Peak CIty Park, Turf Paradise Race Track and the State Fair grounds.

  9. The Phoenix Mission Explores the Martian Arctic

    NASA Astrophysics Data System (ADS)

    Smith, P. H.; Team, P. S.

    2008-12-01

    After a thrilling landing on May 25, 2008, Phoenix has conducted a series of science experiments designed to unlock the secrets of the northern, ice-rich plains. The overarching goals are to determine the history of the water ice, to check for the signatures of a habitable zone, and to monitor the polar weather from Summer to late Fall. These goals are achieved in three ways: geologically with cameras and a robotic arm to image and interact with the surface, analytically using three instruments on the deck to assess the chemistry and mineralogy of samples, and observationally using a powerful weather station operating around the clock. Phoenix landed on the fluidized ejecta from the nearby Heimdal crater where the surface is molded into polygonal shapes characteristic of icy polar terrain. After trenching several inches beneath the surface to an ice table and examining samples from each layer, samples from different depths were collected and studied. The chemistry is alkaline with calcium carbonate associated with the ice; this is very different from the sulfate-rich acidic soil seen by the MER rovers. A surprisingly large amount of perchlorate, likely magnesium perchlorate, is seen in the wet chemistry lab. Microscopic images reveal three classes of soil particles: iron- rich clay-sized particles with larger grains of two types. These are compared with the phyllosilicates and carbonates discovered in the TEGA experiment. The transition of the seasons is recorded in the detailed data sets collected with our weather station. Ice clouds and ground fogs are evident with frost in the coldest areas late at night. Taken together a new understanding of the complex interaction of atmosphere, dry soil, and ice is revealed.

  10. Color Image of Phoenix Lander on Mars Surface

    NASA Image and Video Library

    2008-05-27

    This is an enhanced-color image from Mars Reconnaissance Orbiter High Resolution Imaging Science Experiment HiRISE camera. It shows the NASA Mars Phoenix lander with its solar panels deployed on the Mars surface

  11. RadNet Air Data From Phoenix, AZ

    EPA Pesticide Factsheets

    This page presents radiation air monitoring and air filter analysis data for Phoenix, AZ from EPA's RadNet system. RadNet is a nationwide network of monitoring stations that measure radiation in air, drinking water and precipitation.

  12. Phoenix Production Company – Rolff Lake Unit NPDES Permit

    EPA Pesticide Factsheets

    Under NPDES permit WY-002494, Phoenix Production Company is authorized to discharge from its Rolff Lake Unit wastewater treatment facility in Fremont County, Wyoming, to an unnamed ephemeral tributary of Dry Creek, which is tributary to the Wind River.

  13. Phoenix Production Company – Sheldon Dome Field NPDES Permit

    EPA Pesticide Factsheets

    Under NPDES permit WY-0024953, Phoenix Production Company is authorized to discharge from its Sheldon Dome Field wastewater treatment facility in Fremont County, Wyoming, to an unnamed ephemeral tributary of Dry Creek, which is tributary to the Wind River.

  14. Arch construction at south end, looking east with Phoenix Iron ...

    Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

    Arch construction at south end, looking east with Phoenix Iron Company foundry in background. - Gay Street Bridge, Spanning French Creek at Gay Street (State Route 113), Phoenixville, Chester County, PA

  15. Geomorphic Map of Region Around Phoenix Mars Lander

    NASA Image and Video Library

    2008-12-15

    This map shows a color-coded interpretation of geomorphic units -- categories based on surface textures and contour -- in the region where NASA Phoenix Mars Lander has studied an arctic Martian plain.

  16. Phoenix Missile Hypersonic Testbed (PMHT): System Concept Overview

    NASA Technical Reports Server (NTRS)

    Jones, Thomas P.

    2007-01-01

    A viewgraph presentation of the Phoenix Missile Hypersonic Testbed (PMHT) is shown. The contents include: 1) Need and Goals; 2) Phoenix Missile Hypersonic Testbed; 3) PMHT Concept; 4) Development Objectives; 5) Possible Research Payloads; 6) Possible Research Program Participants; 7) PMHT Configuration; 8) AIM-54 Internal Hardware Schematic; 9) PMHT Configuration; 10) New Guidance and Armament Section Profiles; 11) Nomenclature; 12) PMHT Stack; 13) Systems Concept; 14) PMHT Preflight Activities; 15) Notional Ground Path; and 16) Sample Theoretical Trajectories.

  17. Color Image of Phoenix Heat Shield and Bounce Mark

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This shows a color image from Mars Reconnaissance Orbiter's High Resolution Imaging Science Experiment camera. It shows the Phoenix heat shield and bounce mark on the Mars surface.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  18. View of Phoenix's Surroundings as of Sol 2

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This is a cylindrical mosaic of all data, as of the end of sol 2, from the right eye of the Surface Stereo Imager (SSI) instrument on board the Phoenix lander.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  19. View of Phoenix's Surroundings as of Sol 2

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This is a cylindrical mosaic of all data, as of the end of sol 2, from the right eye of the Surface Stereo Imager (SSI) instrument on board the Phoenix lander.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  20. Assessment of Debris Flow Hazards, North Mountain, Phoenix, AZ

    NASA Astrophysics Data System (ADS)

    Reavis, K. J.; Wasklewicz, T. A.

    2014-12-01

    Urban sprawl in many western U.S. cities has expanded development onto alluvial fans. In the case of metropolitan Phoenix, AZ (MPA), urban sprawl has led to an exponential outward growth into surrounding mountainous areas and onto alluvial fans. Building on alluvial fans places humans at greater risk to flooding and debris flow hazards. Recent research has shown debris flows often supply large quantities of material to many alluvial fans in MPA. However, the risk of debris flows to built environments is relatively unknown. We use a 2D debris flow modeling approach, aided by high-resolution airborne LiDAR and terrestrial laser scanning (TLS) topographic data, to examine debris flow behavior in a densely populated portion of the MPA to assess the risk and vulnerability of debris flow damage to the built infrastructure. A calibrated 2D debris flow model is developed for a "known" recent debris flow at an undeveloped site in MPA. The calibrated model and two other model scenarios are applied to a populated area with historical evidence of debris flow activity. Results from the modeled scenarios show evidence of debris flow damage to houses built on the alluvial fan. Debris flow inundation is also evident on streets on the fan. We use housing values and building damage to estimate the costs assocaited with various modeled debris flow scenarios.

  1. 3D Visualization for Phoenix Mars Lander Science Operations

    NASA Technical Reports Server (NTRS)

    Edwards, Laurence; Keely, Leslie; Lees, David; Stoker, Carol

    2012-01-01

    Planetary surface exploration missions present considerable operational challenges in the form of substantial communication delays, limited communication windows, and limited communication bandwidth. A 3D visualization software was developed and delivered to the 2008 Phoenix Mars Lander (PML) mission. The components of the system include an interactive 3D visualization environment called Mercator, terrain reconstruction software called the Ames Stereo Pipeline, and a server providing distributed access to terrain models. The software was successfully utilized during the mission for science analysis, site understanding, and science operations activity planning. A terrain server was implemented that provided distribution of terrain models from a central repository to clients running the Mercator software. The Ames Stereo Pipeline generates accurate, high-resolution, texture-mapped, 3D terrain models from stereo image pairs. These terrain models can then be visualized within the Mercator environment. The central cross-cutting goal for these tools is to provide an easy-to-use, high-quality, full-featured visualization environment that enhances the mission science team s ability to develop low-risk productive science activity plans. In addition, for the Mercator and Viz visualization environments, extensibility and adaptability to different missions and application areas are key design goals.

  2. Superfund Record of Decision (EPA Region 9): Litchfield Airport/Phoenix, Arizona (first remedial action), September 1987. Final report

    SciTech Connect

    Not Available

    1987-09-29

    The Litchfield/Phoenix-Goodyear Airport (PGA) site is divided into a northern and a southern area by a ground-water divide running under the Yuma Road area. Section 16 (approximately 17 acres) lies in the southern area and includes the Loral Corporation facility (formerly owned by Goodyear Aerospace Corporation) and the Phoenix-Goodyear Airport (formerly owned by U.S. Navy), both being potential sources of VOC contamination. Ground-water contaminant concentrations in Section 16 are at least 100 times greater than down-gradient levels. The Arizona Department of Health Services discovered solvent and chromium contamination in the ground water within the PGA area. Additional sampling in 1982 and 1983 found 18 wells contaminated with TCE. The primary contaminants of concern include: trichloroethene, volatile organic compounds and chromium. Interim remedial action for the site is proposed.

  3. Atmospheric results from the Phoenix Mars Mission

    NASA Astrophysics Data System (ADS)

    Smith, Peter

    The Phoenix Mission operated in the northern plains of Mars for 5 months starting May 25, 2008 spanning solar longitudes from 78 to 143 (summer). Throughout this period a diverse set of atmospheric measurements were taken and analyzed. The data sets provide information on the diurnal temperatures at 2 m above the surface, diurnal pressure, wind vectors, cloud properties, dust devils, the boundary layer, and humidity. In addition, coordinated observations were obtained with orbital instruments from Mars Reconnaissance Orbiter, Odyssey, and Mars Express. The measurements have been compared with predictions from Global Climate Models and found to agree in most regards. Taken as a whole this represents a unique description of the summer weather in a heretofore unexplored region of Mars. The Canadian LIDAR experiment gives us the first direct measurement of the boundary layer height. The first 90 sols of the mission were conducted under dusty conditions and the height of the dust layer was determined as 4-5 km above the surface. After 90 sols, the dust dispersed and water ice clouds were seen at ever lower altitudes and the boundary layer dropped to as low as 3 km. Snowfall was observed and frost imaged on the surface. Winds swirled around the lander completing a full circle each sol; typical wind speeds were 5-10 m/s. From near surface humidity measurements, a diurnal cycle sublimates ice and adsorbed water from the surface soil as the Sun heats it forming water ice clouds at the boundary layer. As temperatures cool in the night the water is returned as snow and frost to the soil. Temperatures ranged from -30 C to -90 C, but never exceed the melting point; even though atmospheric pressures are always above the triple point, liquid water is not allowed at this time. The lack of dune forms and the presence of dust devils suggest that wind erosion is a strong force despite the constant dust fall observed on the spacecraft deck. Local dust storms are often seen by the

  4. Phoenix Union High School District #210 Adult Academy Evaluation Report, 1980-81. Research Services Report No. 33:08:80/81:010.

    ERIC Educational Resources Information Center

    Norris, Carol A.; Wheeler, Linda

    The Adult Reading Academy, a federally-funded service of the Phoenix Union High School District, serves native- and foreign-born adult students who are deficient in the basic skills of reading, writing, arithmetic, and oral communication. In 1980/81, the program served 476 students at 17 sites. Approximately 24 percent of the clients served were…

  5. EnviroAtlas - Metrics for Phoenix, AZ

    EPA Pesticide Factsheets

    These EnviroAtlas web services support research and online mapping activities related to EnviroAtlas (https://www.epa.gov/enviroatlas). The layers in these web services depict ecosystem services at the census block group level for the community of Phoenix, Arizona. These layers illustrate the ecosystems and natural resources that are associated with clean air (https://enviroatlas.epa.gov/arcgis/rest/services/Communities/ESC_PAZ_CleanAir/MapServer); clean and plentiful water (https://enviroatlas.epa.gov/arcgis/rest/services/Communities/ESC_PAZ_CleanPlentifulWater/MapServer); natural hazard mitigation (https://enviroatlas.epa.gov/arcgis/rest/services/Communities/ESC_PAZ_NaturalHazardMitigation/MapServer); climate stabilization (https://enviroatlas.epa.gov/arcgis/rest/services/Communities/ESC_PAZ_ClimateStabilization/MapServer); food, fuel, and materials (https://enviroatlas.epa.gov/arcgis/rest/services/Communities/ESC_PAZ_FoodFuelMaterials/MapServer); recreation, culture, and aesthetics (https://enviroatlas.epa.gov/arcgis/rest/services/Communities/ESC_PAZ_RecreationCultureAesthetics/MapServer); and biodiversity conservation (https://enviroatlas.epa.gov/arcgis/rest/services/Communities/ESC_PAZ_BiodiversityConservation/MapServer), and factors that place stress on those resources. EnviroAtlas allows the user to interact with a web-based, easy-to-use, mapping application to view and analyze multiple ecosystem services for the conterminous United States as well as deta

  6. Aerodynamics for the Mars Phoenix Entry Capsule

    NASA Technical Reports Server (NTRS)

    Edquist, Karl T.; Desai, Prasun N.; Schoenenberger, Mark

    2008-01-01

    Pre-flight aerodynamics data for the Mars Phoenix entry capsule are presented. The aerodynamic coefficients were generated as a function of total angle-of-attack and either Knudsen number, velocity, or Mach number, depending on the flight regime. The database was constructed using continuum flowfield computations and data from the Mars Exploration Rover and Viking programs. Hypersonic and supersonic static coefficients were derived from Navier-Stokes solutions on a pre-flight design trajectory. High-altitude data (free-molecular and transitional regimes) and dynamic pitch damping characteristics were taken from Mars Exploration Rover analysis and testing. Transonic static coefficients from Viking wind tunnel tests were used for capsule aerodynamics under the parachute. Static instabilities were predicted at two points along the reference trajectory and were verified by reconstructed flight data. During the hypersonic instability, the capsule was predicted to trim at angles as high as 2.5 deg with an on-axis center-of-gravity. Trim angles were predicted for off-nominal pitching moment (4.2 deg peak) and a 5 mm off-axis center-ofgravity (4.8 deg peak). Finally, hypersonic static coefficient sensitivities to atmospheric density were predicted to be within uncertainty bounds.

  7. Project PHOENIX SETI Observations at Parkes

    NASA Astrophysics Data System (ADS)

    Backus, P. R.

    1995-12-01

    For sixteen weeks (February to June of 1995), Project Phoenix had the exclusive use of the 64 m Parkes radio telescope in New South Wales, Australia, as well as another element of the Australian Telescope National Facility (ATNF), the 22 m Mopra telescope, 200 km to the north at Coonabarabran. With these two telescopes, we conducted a targeted search of nearly two hundred solar-type stars covering the frequency range from 1.2 to 3 GHz. The signal detection system was optimized to detect narrowband signals (presumed to be transmitted by another technological civilization) originating in the vicinity of these targets. The system was sensitive to signals that were continuously present, or pulsed regularly, even if their frequencies drifted, or changed slowly in time. Many signals of precisely this nature were detected, but all were coming from our own technology! All manner of transmitters, from microwave ovens to satellite downlinks, are rapidly making this naturally quiet portion of the electromagnetic spectrum extremely noisy. The use of the two widely separated telescopes as a pseudo-interferometer was essential to discriminate against signals of terrestrial origin. The architecture and performance of the system and the results of the observing campaign are presented in this paper.

  8. The Phoenix search results at Parkes

    NASA Astrophysics Data System (ADS)

    Backus, Peter R.

    For 16 weeks (February to June of 1995), Project Phoenix had the exclusive use of the 64 m Parkes radio telescope in New South Wales, Australia, as well as another element of the Australian Telescope National Facility (ATNF), the 22 m Mopra telescope, 200 km to the north at Coonabarabran. With these two telescopes, we conducted a targeted search of nearly two hundred solar-type stars covering the frequency range from 1.2-3 GHz. The signal detection system described in the paper by Dreher [1]was optimized to detect narrowband signals (presumed to be transmitted by another technological civilization) originating in the vicinity of these targets. The system was sensitive to signals that were continuously present, or pulsed regularly, even if their frequencies drifted, or changed slowly in time. Many signals of precisely this nature were detected—coming from our own technology! All manner of transmitters, from microwave ovens to satellite downlinks, are rapidly making this naturally quiet portion of the electromagnetic spectrum extremely noisy. The use of the two widely separated telescopes as a pseudo-interferometer was essential to discriminate against signals of terrestrial origin. The performance of the system and the results of the observing campaign are presented in this paper, while the cooperative science observations that were undertaken with Australian PIs are described in a companion paper.

  9. Entry, Descent, and Landing Performance of the Mars Phoenix Lander

    NASA Technical Reports Server (NTRS)

    Desai, Prasun N.; Prince, Jill L.; Wueen, Eric M.; Cruz, Juan R.; Grover, Myron R.

    2008-01-01

    On May 25, 2008, the Mars Phoenix Lander successfully landed on the northern arctic plains of Mars. An overview of a preliminary reconstruction analysis performed on each entry, descent, and landing phase to assess the performance of Phoenix as it descended is presented and a comparison to pre-entry predictions is provided. The landing occurred 21 km further downrange than the predicted landing location. Analysis of the flight data revealed that the primary cause of Phoenix s downrange landing was a higher trim total angle of attack during the hypersonic phase of the entry, which resulted in Phoenix flying a slightly lifting trajectory. The cause of this higher trim attitude is not known at this time. Parachute deployment was 6.4 s later than prediction. This later deployment time was within the variations expected and is consistent with a lifting trajectory. The parachute deployment and inflation process occurred as expected with no anomalies identified. The subsequent parachute descent and powered terminal landing also behaved as expected. A preliminary reconstruction of the landing day atmospheric density profile was found to be lower than the best apriori prediction, ranging from a few percent less to a maximum of 8%. A comparison of the flight reconstructed trajectory parameters shows that the actual Phoenix entry, descent, and landing was close to pre-entry predictions. This reconstruction investigation is currently ongoing and the results to date are in the process of being refined.

  10. 76 FR 23787 - Voluntary Termination of Foreign-Trade Subzone 75D, STMicroelectronics, Inc., Phoenix, AZ

    Federal Register 2010, 2011, 2012, 2013, 2014

    2011-04-28

    ...., Phoenix, AZ Pursuant to its authority under the Foreign-Trade Zones Act of June 18, 1934, as amended (19 U... issued a grant of authority to the City of Phoenix (grantee of FTZ 75) authorizing the establishment of Foreign-Trade Subzone 75D at the STMicroelectronics, Inc., facility in Phoenix, Arizona (Board Order...

  11. 78 FR 56859 - Foreign-Trade Zone 75-Phoenix, Arizona, Authorization of Limited Production Activity, Honeywell...

    Federal Register 2010, 2011, 2012, 2013, 2014

    2013-09-16

    ... Foreign-Trade Zones Board Foreign-Trade Zone 75--Phoenix, Arizona, Authorization of Limited Production Activity, Honeywell Aerospace, Inc. (Aircraft Engines, Systems and Components), Phoenix and Tempe, Arizona On May 3, 2013, the City of Phoenix, grantee of FTZ 75, submitted a notification of...

  12. 75 FR 63139 - Approval and Promulgation of Implementation Plans-Maricopa County (Phoenix) PM-10 Nonattainment...

    Federal Register 2010, 2011, 2012, 2013, 2014

    2010-10-14

    ... AGENCY 40 CFR Part 52 Approval and Promulgation of Implementation Plans--Maricopa County (Phoenix) PM-10... County (Phoenix) nonattainment area (Maricopa area). Specifically, EPA proposed to disapprove provisions... County (Phoenix) nonattainment area (Maricopa area). These requirements apply to the Maricopa...

  13. Team Huddle Before Lifting Phoenix into Test Chamber

    NASA Technical Reports Server (NTRS)

    2007-01-01

    Spacecraft specialists huddle to discuss the critical lift of NASA's Phoenix Mars Lander into a thermal vacuum chamber.

    In December 2006, the spacecraft was in a cruise configuration prior to going into environmental testing at a Lockheed Martin Space Systems facility near Denver. At all stages of assembly and testing, the spacecraft is handled with extreme care and refinement.

    The Phoenix mission is led by Principal Investigator Peter H. Smith of the University of Arizona, Tucson, with project management at NASA's Jet Propulsion Laboratory and development partnership with Lockheed Martin Space Systems. International contributions for Phoenix are provided by the Canadian Space Agency, the University of Neuchatel (Switzerland), the University of Copenhagen, and the Max Planck Institute in Germany. JPL is a division of the California Institute of Technology in Pasadena.

  14. Team Huddle Before Lifting Phoenix into Test Chamber

    NASA Technical Reports Server (NTRS)

    2007-01-01

    Spacecraft specialists huddle to discuss the critical lift of NASA's Phoenix Mars Lander into a thermal vacuum chamber.

    In December 2006, the spacecraft was in a cruise configuration prior to going into environmental testing at a Lockheed Martin Space Systems facility near Denver. At all stages of assembly and testing, the spacecraft is handled with extreme care and refinement.

    The Phoenix mission is led by Principal Investigator Peter H. Smith of the University of Arizona, Tucson, with project management at NASA's Jet Propulsion Laboratory and development partnership with Lockheed Martin Space Systems. International contributions for Phoenix are provided by the Canadian Space Agency, the University of Neuchatel (Switzerland), the University of Copenhagen, and the Max Planck Institute in Germany. JPL is a division of the California Institute of Technology in Pasadena.

  15. 38. VIEW SHOWING SITE OF THE OLD ARIZONA CANAL POWER ...

    Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

    38. VIEW SHOWING SITE OF THE OLD ARIZONA CANAL POWER HOUSE, LOOKING SOUTH ON THE SALT RIVER INDIAN RESERVATION (NOW SPILLWAY A) Photographer: James Eastwood, June 1990 - Arizona Canal, North of Salt River, Phoenix, Maricopa County, AZ

  16. 52. VIEW SHOWING SITE OF ARIZONA FALL POWER PLANT, LOOKING ...

    Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

    52. VIEW SHOWING SITE OF ARIZONA FALL POWER PLANT, LOOKING EAST. CURRENT LOCATION OF THE REAL-TIME WATER QUALITY MONITORING STATION Photographer: James Eastwood, July 1990 - Arizona Canal, North of Salt River, Phoenix, Maricopa County, AZ

  17. Martian Arctic Dust Devil and Phoenix Meteorology Mast

    NASA Technical Reports Server (NTRS)

    2008-01-01

    The Surface Stereo Imager on NASA's Phoenix Mars Lander caught this dust devil in action west-southwest of the lander at 11:16 a.m. local Mars time on Sol 104, or the 104th Martian day of the mission, Sept. 9, 2008.

    Dust devils have not been detected in any Phoenix images from earlier in the mission, but at least six were observed in a dozen images taken on Sol 104.

    Dust devils are whirlwinds that often occur when the Sun heats the surface of Mars, or some areas on Earth. The warmed surface heats the layer of atmosphere closest to it, and the warm air rises in a whirling motion, stirring dust up from the surface like a miniature tornado.

    The vertical post near the left edge of this image is the mast of the Meteorological Station on Phoenix. The dust devil visible at the horizon just to the right of the mast is estimated to be 600 to 700 meters (about 2,000 to 2,300 feet) from Phoenix, and 4 to 5 meters (10 to 13 feet) in diameter. It is much smaller than dust devils that have been observed by NASA's Mars Exploration Rover Spirit much closer to the equator. It is closer in size to dust devils seen from orbit in the Phoenix landing region, though still smaller than those.

    The image has been enhanced to make the dust devil easier to see.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  18. The RR Lyrae variable population in the Phoenix dwarf galaxy

    SciTech Connect

    Ordoñez, Antonio J.; Sarajedini, Ata; Yang, Soung-Chul E-mail: ata@astro.ufl.edu

    2014-05-10

    We present the first detailed study of the RR Lyrae variable population in the Local Group dSph/dIrr transition galaxy, Phoenix, using previously obtained HST/WFPC2 observations of the galaxy. We utilize template light curve fitting routines to obtain best fit light curves for RR Lyrae variables in Phoenix. Our technique has identified 78 highly probable RR Lyrae stars (54 ab-type; 24 c-type) with about 40 additional candidates. We find mean periods for the two populations of (P {sub ab}) = 0.60 ± 0.03 days and (P{sub c} ) = 0.353 ± 0.002 days. We use the properties of these light curves to extract, among other things, a metallicity distribution function for ab-type RR Lyrae. Our analysis yields a mean metallicity of ([Fe/H]) = –1.68 ± 0.06 dex for the RRab stars. From the mean period and metallicity calculated from the ab-type RR Lyrae, we conclude that Phoenix is more likely of intermediate Oosterhoff type; however the morphology of the Bailey diagram for Phoenix RR Lyraes appears similar to that of an Oosterhoff type I system. Using the RRab stars, we also study the chemical enrichment law for Phoenix. We find that our metallicity distribution is reasonably well fitted by a closed-box model. The parameters of this model are compatible with the findings of Hidalgo et al., further supporting the idea that Phoenix appears to have been chemically enriched as a closed-box-like system during the early stage of its formation and evolution.

  19. Dinosaur or Phoenix: Nuclear Bombers in the 21st Century

    DTIC Science & Technology

    2010-04-12

    REPORT DATE 02-04-10 2. REPORT TYPE Master’s Thesis 3. DATES COVERED 31-07-09 to 16-06-10 4. TITLE AND SUBTITLE Dinosaur or Phoenix: Nuclear...WARFIGHTING SCHOOL DINOSAUR OR PHOENIX: NUCLEAR BOMBERS IN THE 21ST CENTURY by John W. Morehead Colonel, United States Air Force A paper...can argue Secretary Gates’ decision to halt development of a follow-on bomber indicates the DOD views nuclear bombers as dinosaurs no longer needed as

  20. Earthshots: Satellite images of environmental change - Phoenix, Arizona, USA

    USGS Publications Warehouse

    Adamson, Thomas

    2013-01-01

    Phoenix doesn’t have many cloudy days, so it’s perfect for studying urban growth with satellite images. Scientists and city planners study population growth and urban expansion in fast-growing cities like Phoenix to determine the changes that have occurred over time and to see how those changes impact the surrounding environment, affect the availability of natural resources such as water, and alter the landscape and how it’s used. That information can help people plan for future changes as cities continue to grow.

  1. Geomorphic Map of Region Around Phoenix Mars Lander

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This map shows shows a color-coded interpretation of geomorphic units categories based on surface textures and contours in the region where NASA's Phoenix Mars Lander has studied an arctic Martian plain. It covers an area about 65 kilometers by 65 kilometers (40 miles by 40 miles).

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  2. Orbit Determination for the 2007 Mars Phoenix Lander

    NASA Technical Reports Server (NTRS)

    Ryne, Mark S.; Graat, Eric; Haw, Robert; Kruizinga, Gerhard; Lau, Eunice; Martin-Mur, Tomas; McElrath, Timothy; Nandi, Sumita; Portock, Brian

    2008-01-01

    The Phoenix mission is designed to study the arctic region of Mars. To achieve this goal, the spacecraft must be delivered to a narrow corridor at the top of the Martian atmosphere, which is approximately 20 km wide. This paper will discuss the details of the Phoenix orbit determination process and the effort to reduce errors below the level necessary to achieve successful atmospheric entry at Mars. Emphasis will be placed on properly modeling forces that perturb the spacecraft trajectory and the errors and uncertainties associated with those forces. Orbit determination covariance analysis strongly influenced mission operations scenarios, which were chosen to minimize errors and associated uncertainties.

  3. Color Image of Phoenix Lander on Mars Surface

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This is an enhanced-color image from Mars Reconnaissance Orbiter's High Resolution Imaging Science Experiment (HiRISE) camera. It shows the Phoenix lander with its solar panels deployed on the Mars surface. The spacecraft appears more blue than it would in reality.

    The blue/green and red filters on the HiRISE camera were used to make this picture.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  4. Thermal Design Validation of the Mars Scout Phoenix Payload

    NASA Technical Reports Server (NTRS)

    Tsuyuki, Glenn T.; Lee, Chern-Jiin

    2007-01-01

    This slide presentation reviews the validation of the thermal design for the Mars Scout Phoenix Payload. It includes a description of the Phoenix Mission, the science objectives, the timeline, and the flight system and payloads that were on the lander. The initial responsibility for the development and validation the thermal design was with the developers. This process lacked overall system engineering, there was a difference of thermal expertise, and the number of institutions involved complicated the interactions. The revised approach for payload thermal design validation is described.

  5. Geomorphic Map of Region Around Phoenix Mars Lander

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This map shows shows a color-coded interpretation of geomorphic units categories based on surface textures and contours in the region where NASA's Phoenix Mars Lander has studied an arctic Martian plain. It covers an area about 65 kilometers by 65 kilometers (40 miles by 40 miles).

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  6. Establishment, management, and maintenance of the phoenix islands protected area.

    PubMed

    Rotjan, Randi; Jamieson, Regen; Carr, Ben; Kaufman, Les; Mangubhai, Sangeeta; Obura, David; Pierce, Ray; Rimon, Betarim; Ris, Bud; Sandin, Stuart; Shelley, Peter; Sumaila, U Rashid; Taei, Sue; Tausig, Heather; Teroroko, Tukabu; Thorrold, Simon; Wikgren, Brooke; Toatu, Teuea; Stone, Greg

    2014-01-01

    The Republic of Kiribati's Phoenix Islands Protected Area (PIPA), located in the equatorial central Pacific, is the largest and deepest UNESCO World Heritage site on earth. Created in 2008, it was the first Marine Protected Area (MPA) of its kind (at the time of inception, the largest in the world) and includes eight low-lying islands, shallow coral reefs, submerged shallow and deep seamounts and extensive open-ocean and ocean floor habitat. Due to their isolation, the shallow reef habitats have been protected de facto from severe exploitation, though the surrounding waters have been continually fished for large pelagics and whales over many decades. PIPA was created under a partnership between the Government of Kiribati and the international non-governmental organizations-Conservation International and the New England Aquarium. PIPA has a unique conservation strategy as the first marine MPA to use a conservation contract mechanism with a corresponding Conservation Trust established to be both a sustainable financing mechanism and a check-and-balance to the oversight and maintenance of the MPA. As PIPA moves forward with its management objectives, it is well positioned to be a global model for large MPA design and implementation in similar contexts. The islands and shallow reefs have already shown benefits from protection, though the pending full closure of PIPA (and assessments thereof) will be critical for determining success of the MPA as a refuge for open-ocean pelagic and deep-sea marine life. As global ocean resources are continually being extracted to support a growing global population, PIPA's closure is both timely and of global significance.

  7. Results from the Mars Phoenix Lander Robotic Arm experiment

    NASA Astrophysics Data System (ADS)

    Arvidson, R. E.; Bonitz, R. G.; Robinson, M. L.; Carsten, J. L.; Volpe, R. A.; Trebi-Ollennu, A.; Mellon, M. T.; Chu, P. C.; Davis, K. R.; Wilson, J. J.; Shaw, A. S.; Greenberger, R. N.; Siebach, K. L.; Stein, T. C.; Cull, S. C.; Goetz, W.; Morris, R. V.; Ming, D. W.; Keller, H. U.; Lemmon, M. T.; Sizemore, H. G.; Mehta, M.

    2009-10-01

    The Mars Phoenix Lander was equipped with a 2.4 m Robotic Arm (RA) with an Icy Soil Acquisition Device capable of excavating trenches in soil deposits, grooming hard icy soil surfaces with a scraper blade, and acquiring icy soil samples using a rasp tool. A camera capable of imaging the scoop interior and a thermal and electrical conductivity probe were also included on the RA. A dozen trench complexes were excavated at the northern plains landing site and 31 samples (including water-ice-bearing soils) were acquired for delivery to instruments on the Lander during the 152 sol mission. Deliveries included sprinkling material from several centimeters height to break up cloddy soils on impact with instrument portals. Excavations were done on the side of the Humpty Dumpty and the top of the Wonderland polygons, and in nearby troughs. Resistive forces encountered during backhoe operations show that soils above the 3-5 cm deep icy soil interfaces are stronger with increasing depth. Further, soils are similar in appearance and properties to the weakly cohesive crusty and cloddy soils imaged and excavated by the Viking Lander 2, which also landed on the northern plains. Adsorbed H2O is inferred to be responsible for the variable nature and cohesive strength of the soils. Backhoe blade chatter marks on excavated icy soil surfaces, combined with rasp motor currents, are consistent with laboratory experiments using grain-supported icy soil deposits, as is the relatively rapid decrease in icy soil strength over time as the ice sublimated on Mars.

  8. Identification of sources of Phoenix aerosol by positive matrix factorization.

    PubMed

    Ramadan, Z; Song, X H; Hopke, P K

    2000-08-01

    Chemical composition data for fine and coarse particles collected in Phoenix, AZ, were analyzed using positive matrix factorization (PMF). The objective was to identify the possible aerosol sources at the sampling site. PMF uses estimates of the error in the data to provide optimum data point scaling and permits a better treatment of missing and below-detection-limit values. It also applies nonnegativity constraints to the factors. Two sets of fine particle samples were collected by different samplers. Each of the resulting fine particle data sets was analyzed separately. For each fine particle data set, eight factors were obtained, identified as (1) biomass burning characterized by high concentrations of organic carbon (OC), elemental carbon (EC), and K; (2) wood burning with high concentrations of Na, K, OC, and EC; (3) motor vehicles with high concentrations of OC and EC; (4) nonferrous smelting process characterized by Cu, Zn, As, and Pb; (5) heavy-duty diesel characterized by high EC, OC, and Mn; (6) sea-salt factor dominated by Na and Cl; (7) soil with high values for Al, Si, Ca, Ti, and Fe; and (8) secondary aerosol with SO4(-2) and OC that may represent coal-fired power plant emissions. For the coarse particle samples, a five-factor model gave source profiles that are attributed to be (1) sea salt, (2) soil, (3) Fe source/motor vehicle, (4) construction (high Ca), and (5) coal-fired power plant. Regression of the PM mass against the factor scores was performed to estimate the mass contributions of the resolved sources. The major sources for the fine particles were motor vehicles, vegetation burning factors (biomass and wood burning), and coal-fired power plants. These sources contributed most of the fine aerosol mass by emitting carbonaceous particles, and they have higher contributions in winter. For the coarse particles, the major source contributions were soil and construction (high Ca). These sources also peaked in winter.

  9. Permafrost as a habitable environment on Mars: Insights from the Phoenix Mars Mission

    NASA Astrophysics Data System (ADS)

    Stoker, C.

    2011-12-01

    The Phoenix mission landed in the northern plains of Mars (68.2°N, 234.3°E) in May 2009, at a location with ground ice within 10 cm of the surface(1). A mission objective was to determine whether conditions at the surface or near subsurface could supporting living organisms with capabilities similar to terrestrial microbes, either at present or in the recent past(2). The lander carried a robotic arm with digging scoop to collect soil and icy material and performed volatile mineral and organic analysis(3) and wet chemical analysis(4). Results from Phoenix along with theoretical modeling and other previous mission results can be used to evaluate the habitability of the landing site(2). Factors that characterize the environments' ability to support life as we know it are the presence of liquid water, the presence of an energy source to support metabolism, the presence of nutrients containing the fundamental building blocks of life, and the absence of environmental conditions that are toxic to or preclude life. Phoenix observational evidence for the presence of liquid water (past or present) includes clean segregated ice(1), chemical etching of soil grains(2), calcite minerals in the soil(3), and variable concentrations of soluble salts(5). The present maximum surface temperature measured is 260K(6) so unfrozen water can form only in adsorbed films or saline brines but warmer climates occur cyclically on geologically short time scales due to variations in orbital parameters. During the most clement periods, temperatures allowing metabolism extend nearly a meter into the subsurface(7). Energy to drive metabolism is available from sunlight, beneath semi-transparent soil grains that can provide shielding from UV radiation. Phoenix also discovered perchlorate(4),a chemical energy source utilized by a wide range of microbes, occurs in high soil concentrations. Biologically available C, H, N, O, P and S compounds are supplied by known atmospheric sources or global dust

  10. Genetic erosion of Phoenix dactylifera L.: Perceptible, probable or possible?

    USDA-ARS?s Scientific Manuscript database

    Genetic diversity of date palm (Phoenix dactylefera L.) encompasses genetic differences among and within species, subspecies, populations, cultivars, and individual clones in traditional oases and plantations. Components of this diversity can be estimated, throughout the tree’s ontogeny, at the phen...

  11. Panorama of Phoenix Solar Panel and Robotic Arm

    NASA Image and Video Library

    2008-06-13

    This panorama image of NASA’s Phoenix Mars Lander’s solar panel and the lander’s Robotic Arm with a sample in the scoop. The image was taken just before the sample was delivered to the Optical Microscope.

  12. The Flight of the Phoenix: Interpersonal Aspects of Project Management

    ERIC Educational Resources Information Center

    Huffman, Brian J.; Kilian, Claire McCarty

    2012-01-01

    Although many classroom exercises use movies to focus on management and organizational behavior issues, none of those do so in the context of project management. This article presents such an exercise using "The Flight of the Phoenix", an incredibly rich story for any management class, which provides clear examples of organizational behavior…

  13. Summary of the Evaluation of the Phoenix Pilot Drug Program.

    ERIC Educational Resources Information Center

    Emrich, Robert L.; Green, Patricia

    The goal of the Phoenix Pilot Drug Program is to provide a drug/alcohol free educational environment which will enable students to reduce their drug/alcohol usage and function in a regular school program. To determine the degree to which the program is accomplishing these short-term goals, and also to examine the adequacy of the counseling…

  14. Unemployed Native Americans in a Work Orientation Program in Phoenix.

    ERIC Educational Resources Information Center

    McIntosh, Billie Jane

    The unemployment rate for Native Americans is 49% nationwide and 54% in Arizona. The Job Training Partnership Act (JPTA) program at the Phoenix Indian Center trains Native American adults to enter the urban work force. The Center offers work orientation programs, individual counseling, and work experience programs. The majority of the participants…

  15. Vaccination Coverage among Kindergarten Children in Phoenix, Arizona

    ERIC Educational Resources Information Center

    Frimpong, Jemima A.; Rivers, Patrick A.; Bae, Sejong

    2008-01-01

    Objective: To evaluate school immunization records and document the immunization coverage and compliance level of children enrolled in kindergarten in Phoenix during the 2001-2002 school year. The purpose was to obtain information on: 1) immunization status by age two; 2) under-immunization in kindergarten; 3) administration error; and 4)…

  16. Phoenix Indian School: The Second Half-Century.

    ERIC Educational Resources Information Center

    Parker, Dorothy R.

    This book recounts the Phoenix Indian School's history from 1935 to its closing in 1990. In the 1930s, the Bureau of Indian Affairs' philosophy of assimilation declined in importance, as evidenced by termination of the boarding school's militaristic discipline, greater recognition of tribal traditions, and early experimentation in bilingual…

  17. The Flight of the Phoenix: Interpersonal Aspects of Project Management

    ERIC Educational Resources Information Center

    Huffman, Brian J.; Kilian, Claire McCarty

    2012-01-01

    Although many classroom exercises use movies to focus on management and organizational behavior issues, none of those do so in the context of project management. This article presents such an exercise using "The Flight of the Phoenix", an incredibly rich story for any management class, which provides clear examples of organizational behavior…

  18. Giving Teens a Chance: Karl Kendall--Phoenix Public Library

    ERIC Educational Resources Information Center

    Library Journal, 2004

    2004-01-01

    Karl Kendall knows that while comic books, computers, and daily movies will grab teens' interest, what they long for most is respect. As head of Teen Central, a 4,000 square foot space on the fourth floor of Phoenix's Burton Barr Central Library, Kendall provides teens with a place where their ideas and opinions are listened to, their talents…

  19. Public School Choice and Student Mobility in Metropolitan Phoenix

    ERIC Educational Resources Information Center

    Powers, Jeanne M.; Topper, Amelia M.; Silver, Michael

    2012-01-01

    Arizona's interdistrict open enrollment and charter schools laws allow families to send their children to the public schools of their choice. We assessed how public school choice affected elementary school enrollments in 27 metropolitan Phoenix school districts. Student mobility rates varied widely between districts and by location. The higher…

  20. Giving Teens a Chance: Karl Kendall--Phoenix Public Library

    ERIC Educational Resources Information Center

    Library Journal, 2004

    2004-01-01

    Karl Kendall knows that while comic books, computers, and daily movies will grab teens' interest, what they long for most is respect. As head of Teen Central, a 4,000 square foot space on the fourth floor of Phoenix's Burton Barr Central Library, Kendall provides teens with a place where their ideas and opinions are listened to, their talents…

  1. University of Phoenix Says Test Scores Vindicate Its Academic Model

    ERIC Educational Resources Information Center

    Blumenstyk, Goldie

    2008-01-01

    The University of Phoenix is often derided by traditional academics for caring more about its bottom line than about academic quality, and every year, the annual report issued by its parent company focuses more on profits than student performance. This article reports that the institution that has become the largest private university in North…

  2. Vaccination Coverage among Kindergarten Children in Phoenix, Arizona

    ERIC Educational Resources Information Center

    Frimpong, Jemima A.; Rivers, Patrick A.; Bae, Sejong

    2008-01-01

    Objective: To evaluate school immunization records and document the immunization coverage and compliance level of children enrolled in kindergarten in Phoenix during the 2001-2002 school year. The purpose was to obtain information on: 1) immunization status by age two; 2) under-immunization in kindergarten; 3) administration error; and 4)…

  3. Phoenix project at the University of Michigan, 1945-60

    SciTech Connect

    Calkins, L.M.; Kearfott, K.J.

    1997-12-01

    Several years before the formal U.S. Atoms for Peace program in the mid-1950s, the University of Michigan (UM) developed a comprehensive and continuing program of research on the peaceful applications of nuclear science known as the Michigan Memorial Phoenix Project, which was supported by individual, corporate, and government sponsorship.

  4. RS-34 Phoenix (Peacekeeper Post Boost Propulsion System) Utilization Study

    NASA Technical Reports Server (NTRS)

    Esther, Elizabeth A.; Kos, Larry; Burnside, Christopher G.; Bruno, Cy

    2013-01-01

    The Advanced Concepts Office (ACO) at the NASA Marshall Space Flight Center (MSFC) in conjunction with Pratt & Whitney Rocketdyne conducted a study to evaluate potential in-space applications for the Rocketdyne produced RS-34 propulsion system. The existing RS-34 propulsion system is a remaining asset from the de-commissioned United States Air Force Peacekeeper ICBM program, specifically the pressure-fed storable bipropellant Stage IV Post Boost Propulsion System, renamed Phoenix. MSFC gained experience with the RS-34 propulsion system on the successful Ares I-X flight test program flown in October 2009. RS-34 propulsion system components were harvested from stages supplied by the USAF and used on the Ares I-X Roll control system (RoCS). The heritage hardware proved extremely robust and reliable and sparked interest for further utilization on other potential in-space applications. MSFC is working closely with the USAF to obtain RS-34 stages for re-use opportunities. Prior to pursuit of securing the hardware, MSFC commissioned the Advanced Concepts Office to understand the capability and potential applications for the RS-34 Phoenix stage as it benefits NASA, DoD, and commercial industry. As originally designed, the RS-34 Phoenix provided in-space six-degrees-of freedom operational maneuvering to deploy multiple payloads at various orbital locations. The RS-34 Phoenix Utilization Study sought to understand how the unique capabilities of the RS-34 Phoenix and its application to six candidate missions: 1) small satellite delivery (SSD), 2) orbital debris removal (ODR), 3) ISS re-supply, 4) SLS kick stage, 5) manned GEO servicing precursor mission, and an Earth-Moon L-2 Waypoint mission. The small satellite delivery and orbital debris removal missions were found to closely mimic the heritage RS-34 mission. It is believed that this technology will enable a small, low-cost multiple satellite delivery to multiple orbital locations with a single boost. For both the small

  5. RS-34 Phoenix (Peacekeeper Post Boost Propulsion System) Utilization Study

    NASA Technical Reports Server (NTRS)

    Esther, Elizabeth A.; Kos, Larry; Bruno, Cy

    2012-01-01

    The Advanced Concepts Office (ACO) at the NASA Marshall Space Flight Center (MSFC) in conjunction with Pratt & Whitney Rocketdyne conducted a study to evaluate potential in-space applications for the Rocketdyne produced RS-34 propulsion system. The existing RS-34 propulsion system is a remaining asset from the decommissioned United States Air Force Peacekeeper ICBM program; specifically the pressure-fed storable bipropellant Stage IV Post Boost Propulsion System, renamed Phoenix. MSFC gained experience with the RS-34 propulsion system on the successful Ares I-X flight test program flown in October 2009. RS-34 propulsion system components were harvested from stages supplied by the USAF and used on the Ares I-X Roll control system (RoCS). The heritage hardware proved extremely robust and reliable and sparked interest for further utilization on other potential in-space applications. Subsequently, MSFC is working closely with the USAF to obtain all the remaining RS-34 stages for re-use opportunities. Prior to pursuit of securing the hardware, MSFC commissioned the Advanced Concepts Office to understand the capability and potential applications for the RS-34 Phoenix stage as it benefits NASA, DoD, and commercial industry. Originally designed, the RS-34 Phoenix provided in-space six-degrees-of freedom operational maneuvering to deploy multiple payloads at various orbital locations. The RS-34 Phoenix Utilization Study sought to understand how the unique capabilities of the RS-34 Phoenix and its application to six candidate missions: 1) small satellite delivery (SSD), 2) orbital debris removal (ODR), 3) ISS re-supply, 4) SLS kick stage, 5) manned GEO servicing precursor mission, and an Earth-Moon L-2 Waypoint mission. The small satellite delivery and orbital debris removal missions were found to closely mimic the heritage RS-34 mission. It is believed that this technology will enable a small, low-cost multiple satellite delivery to multiple orbital locations with a single

  6. Phoenix Water Vapor Measurements using the SSI Camera

    NASA Astrophysics Data System (ADS)

    Tamppari, Leslie; Lemmon, Mark T.

    2016-10-01

    The Phoenix and Mars Reconnaissance Orbiter (MRO) spacecraft participated together in an observation campaign that was a coordinated effort to study the Martian atmosphere. These coordinated observations were designed to provide near-simultaneous observations of the same column of atmosphere over the Phoenix lander. Seasonal coverage was obtained at Ls=5-10° resolution and diurnal coverage was obtained as often as possible and with as many times of day as possible. One key aspect of this observation set was the means to compare the amount of water measured in the whole column (via the MRO Compact Reconnaissance Imaging Spectrometer for Mars (CRISM; Murchie et al., 2007) and the Phoenix Surface Stereo Imager (SSI) with that measured at the surface (via the Phoenix Thermal and Electrical Conductivity probe (TECP; Zent et al., 2008) which contained a humidity sensor). This comparison, along with the Phoenix LIDAR observations of the depth to which aerosols are mixed (Whiteway et al., 2008, 2009), provides clues to the water vapor mixing ratio profile. Tamppari et al. (2009) showed that examination of a subset of these coordinated observations indicate that the water vapor is not well mixed in the atmosphere up to a cloud condensation height at the Phoenix location during northern summer, and results indicated that a large amount of water must be confined to the lowest 0.5-1 km. This is contrary to the typical assumption that water vapor is "well-mixed."Following a similar approach to Titov et al. (2000), we use the Phoenix SSI camera [Lemmon et al., 2008] filters to detect water vapor: LA = 930.7 nm (broad), R4 = 935.5 nm (narrow), and R5 = 935.7 nm (narrow). We developed a hybrid DISORT-spherical model (DISORT model, Stamnes et al. 1988) to model the expected absorption due to a prescribed water vapor content and profile, to search for matches to the observations. Improvements to the model have been made and recent analysis using this model and comparisons to

  7. Comparison of the Phoenix Mars Lander WCL soil analyses with Antarctic Dry Valley soils, Mars meteorite EETA79001 sawdust, and a Mars simulant

    NASA Astrophysics Data System (ADS)

    Stroble, Shannon T.; McElhoney, Kyle M.; Kounaves, Samuel P.

    2013-08-01

    The results of the Mars Phoenix Lander's Wet Chemistry Laboratory (WCL) for the analyses of the soluble ionic species present in the soil at the northern polar plains of Mars are compared to soil from the Antarctic Dry Valleys (ADVs), martian meteorite EETA79001 sawdust, and a Mars simulant. The ADV soil was compared to the Phoenix site by averaging the samples at analogous 0-5 cm depths and also all the samples from the pavement to the ice-table. Results from each analysis reveal similar ion concentrations ranging plus or minus one order-of-magnitude for all ions except perchlorate (ClO4-), which was three orders-of-magnitude greater in the Phoenix soil. The pH and solution electrical conductivity were also found to be similar for the ADV and Mars soils. The ADV profiles confirm that ClO4- gradients are sensitive indicators for the presence and form of liquid H2O on both Earth and Mars. The Phoenix and meteorite samples contained similar species and ratios but the meteorite concentrations were on average ˜4% of those for the Phoenix soil. The only exception was the ˜16% higher level of Ca2+ in the meteorite due to the CaCO3 druse. The ADV results imply that the Phoenix site is significantly more arid than University Valley, and has been for a greater period of time, as evidenced by the lack of salt gradients and the age of the soils. A Mars simulant was also formulated according to a MINEQL equilibrium model of the WCL results, and its analysis provides confidence that the soluble composition and parent salts at the Phoenix site are reasonably constrained. Overall, comparison of these samples of soil and sawdust indicates that not only does the martian meteorite EETA79001 contain similar soluble ionic species as the martian soil from the northern polar plains, but also that the soils from the ADV are similar to both, thus strengthening the argument for the ADV as a suitable terrestrial Mars analog environment.

  8. Analysis of the Phoenix Mission's Thermal and Electrical Conductivity Probe (TECP) Relative Humidity Data

    NASA Astrophysics Data System (ADS)

    Fischer, E.; Martinez, G.; Renno, N. O.; Tamppari, L.; Zent, A.

    2015-12-01

    With funding from NASA's Mars Data Analysis Program, we plan to enhance the scientific return of the Phoenix mission by producing and archiving high-level relative humidity (RH) data from the measurements made by the Thermal and Electrical Conductivity Probe (TECP). Values of temperature and RH covered in the pre-flight calibration [1] overlap only partially with the environmental conditions found at the Phoenix landing site [2,3]. In particular, there is no overlap at dawn, when temperatures are the lowest and the expected RH is the highest [4] and in the middle of the day, when temperatures are relatively high and the expected RH is very low [5]. Here we plan to produce high-level RH data by calibrating an Engineering Model of the TECP in the Michigan Mars Environmental Chamber (MMEC). The MMEC is capable of simulating the entire range of environmental conditions found at the Phoenix landing site. The MMEC is a cylindrical chamber with internal diameter of 64 cm and length of 160 cm. It is capable of simulating temperatures ranging from 145 to 500 K, CO2 pressures ranging from 10 to 105 Pa, and relative humidity ranging from nearly 0 to 100% [6]. The analysis of high-level RH data has the potential to shed light on the formation of liquid brines at Mars' polar latitudes, where it is most likely to occur [7]. In addition, the RH sensor aboard Curiosity is similar to that on the TECP [8], allowing a direct comparison of the near-surface RH measurements at these two different locations on the surface of Mars. REFERENCES: [1] Zent, A. P., et al, 2009, JGR (1991-2012) 114.E3. [2] Tamppari, L. K., et al. 2010, JGR, 115, E00E17. [3] Davy, R., et al., 2010, JGR, 115, E00E13. [4] Whiteway, J., et al., 2009, Science, 325, 68-70. [5] Savijärvi, H., and A. Määttänen, 2010, Q. J. R. Meteorol. Soc., 136, 1497-1505. [6] Fischer, E., et al., 2014, GRL, 41, 4456-4462. [7] Martínez, G., and Rennó, N., 2013, Space Sci. Rev., 175, 29-51. [8] Harri, A-M., et al., 2014, JGR 119

  9. Census Cities experiment in urban change detection. [mapping of land use changes in San Francisco, Washington D.C., Phoenix, Tucson, Boston, New Haven, Cedar Rapids, and Pontiac

    NASA Technical Reports Server (NTRS)

    Wray, J. R. (Principal Investigator); Milazzo, V. A.

    1974-01-01

    The author has identified the following significant results. Mapping of 1970 and 1972 land use from high-flight photography has been completed for all test sites: San Francisco, Washington, Phoenix, Tucson, Boston, New Haven, Cedar Rapids, and Pontiac. Area analysis of 1970 and 1972 land use has been completed for each of the mandatory urban areas. All 44 sections of the 1970 land use maps of the San Francisco test site have been officially released through USGS Open File at 1:62,500. Five thousand copies of the Washington one-sheet color 1970 land use map, census tract map, and point line identification map are being printed by USGS Publication Division. ERTS-1 imagery for each of the eight test sites is being received and analyzed. Color infrared photo enlargements at 1:100,000 of ERTS-1 MSS images of Phoenix taken on October 16, 1972 and May 2, 1973 are being analyzed to determine to what level land use and land use changes can be identified and to what extent the ERTS-1 imagery can be used in updating the 1970 aircraft photo-derived land use data base. Work is proceeding on the analysis of ERTS-1 imagery by computer manipulation of ERTS-1 MSS data in digital format. ERTS-1 CCT maps at 1:24,000 are being analyzed for two dates over Washington and Phoenix. Anniversary tape sets have been received at Purdue LARS for some additional urban test sites.

  10. Phoenix: Preliminary design of a high speed civil transport

    NASA Technical Reports Server (NTRS)

    Aguilar, Joseph; Davis, Steven; Jett, Brian; Ringo, Leslie; Stob, John; Wood, Bill

    1992-01-01

    The goal of the Phoenix Design Project was to develop a second generation high speed civil transport (HSCT) that will meet the needs of the traveler and airline industry beginning in the 21st century. The primary emphasis of the HSCT is to take advantage of the growing needs of the Pacific Basin and the passengers who are involved in that growth. A passenger load of 150 persons, a mission range of 5150 nautical miles, and a cruise speed of Mach 2.5 constitutes the primary design points of this HSCT. The design concept is made possible with the use of a well designed double delta wing and four mixed flow engines. Passenger comfort, compatibility with existing airport infrastructure, and cost competitive with current subsonic aircraft make the Phoenix a viable aircraft for the future.

  11. Phoenix Again Carries Soil to Wet Chemistry Lab

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This image taken by the Surface Stereo Imager on NASA's Phoenix Mars Lander shows the lander's Robotic Arm scoop positioned over the Wet Chemistry Lab Cell 1 delivery funnel on Sol 41, the 42nd Martian day after landing, or July 6, 2008, after a soil sample was delivered to the instrument.

    The instrument's Cell 1 is second one from the foreground of the image. The first cell, Cell 0, received a soil sample two weeks earlier.

    This image has been enhanced to brighten the scene.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  12. Sediment transport in the nearshore area of Phoenix Island

    NASA Astrophysics Data System (ADS)

    Hu, Rijun; Ma, Fang; Wu, Jianzheng; Zhang, Wei; Jiang, Shenghui; Xu, Yongchen; Zhu, Longhai; Wang, Nan; Liu, Aijiang

    2016-10-01

    Based on the measured data, suspended sediment concentration, surface sediment grain size, current and waves, the sediment transport mechanisms and pathways in the Phoenix Island area were analyzed using methods of flux decomposition and Grain Size Trend Analysis (GSTA). The results show that net suspended sediment is mainly transported by average current, Stokes drift, and gravitational circulation. The transport direction of suspended sediment is varying and basically following the direction of residual tidal currents. Surface sediment transport pathways are primarily parallel to the coastline along with two convergent centers. Waves and longshore currents have a significant influence on sediment transport, but the influence is limited due to a steep and deep underwater bank. Tidal current is the main controlling factor for sediment transport, especially in the deep water area. Neither suspended nor surface sediment is transported towards the southwest. The South Shandong Coastal Current (SSCC) has little effect on sediment transport processes in the nearshore area of Phoenix Island.

  13. Compressed natural gas fuel may be the future for Phoenix

    SciTech Connect

    Berg, T.

    1994-08-01

    It's the law: the future must include cleaner air, and alternative fuels for vehicular engines is one way to achieve it. In Phoenix, a city beset by moderate air quality problems, equipment managers of the Public Works Department's (PWD) fleet say their future seems to be with compressed natural gas (CNG). CNG fuels a pair of refuse packer trucks that have been operating for a year with few, if any, problems. The object of buying and running them, was to see if one can run an alternate fuels vehicle on a regular route. Can the trucks adapt, can the drivers adapt So far the answer is yes. The trucks are among an assortment of municipal vehicles running on CNG and propane. CNG makes sense for Phoenix because it's modestly priced and readily available locally.

  14. Phoenix Again Carries Soil to Wet Chemistry Lab

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This image taken by the Surface Stereo Imager on NASA's Phoenix Mars Lander shows the lander's Robotic Arm scoop positioned over the Wet Chemistry Lab Cell 1 delivery funnel on Sol 41, the 42nd Martian day after landing, or July 6, 2008, after a soil sample was delivered to the instrument.

    The instrument's Cell 1 is second one from the foreground of the image. The first cell, Cell 0, received a soil sample two weeks earlier.

    This image has been enhanced to brighten the scene.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  15. Both Solar Arrays Open on Phoenix Mars Lander

    NASA Technical Reports Server (NTRS)

    2007-01-01

    NASA's next Mars-bound spacecraft, the Phoenix Mars Lander, was partway through assembly and testing at Lockheed Martin Space Systems, Denver, in September 2006, progressing toward an August 2007 launch from Florida. In this photograph, spacecraft specialists work on the lander after its fan-like circular solar arrays have been spread open for testing. The arrays will be in this configuration when the spacecraft is active on the surface of Mars.

  16. Environmental Assurance Program for the Phoenix Mars Mission

    NASA Technical Reports Server (NTRS)

    Man, Kin F.; Natour, Maher C.; Hoffman, Alan R.

    2008-01-01

    The Phoenix Mars mission involves delivering a stationary science lander on to the surface of Mars in the polar region within the latitude band 65 deg N to 72 deg N. Its primary objective is to perform in-situ and remote sensing investigations that will characterize the chemistry of the materials at the local surface, subsurface, and atmosphere. The Phoenix spacecraft was launched on August 4, 2007 and will arrive at Mars in May 2008. The lander includes a suite of seven (7) science instruments. This mission is baselined for up to 90 sols (Martian days) of digging, sampling, and analysis. Operating at the Mars polar region creates a challenging environment for the Phoenix landed subsystems and instruments with Mars surface temperature extremes between -120 deg C to 25 deg C and diurnal thermal cycling in excess of 145 deg C. Some engineering and science hardware inside the lander were qualification tested up to 80 deg C to account for self heating. Furthermore, many of the hardware for this mission were inherited from earlier missions: the lander from the Mars Surveyor Program 2001 (MSP'01) and instruments from the MSP'01 and the Mars Polar Lander. Ensuring all the hardware was properly qualified and flight acceptance tested to meet the environments for this mission required defining and implementing an environmental assurance program that included a detailed heritage review coupled with tailored flight acceptance testing. A heritage review process with defined acceptance success criteria was developed and is presented in this paper together with the lessons learned in its implementation. This paper also provides a detailed description of the environmental assurance program of the Phoenix Mars mission. This program includes assembly/subsystem and system level testing in the areas of dynamics, thermal, and electromagnetic compatibility, as well as venting/pressure, dust, radiation, and meteoroid analyses to meet the challenging environment of this mission.

  17. Environmental Assurance Program for the Phoenix Mars Mission

    NASA Technical Reports Server (NTRS)

    Man, Kin F.; Natour, Maher C.; Hoffman, Alan R.

    2008-01-01

    The Phoenix Mars mission involves delivering a stationary science lander on to the surface of Mars in the polar region within the latitude band 65 deg N to 72 deg N. Its primary objective is to perform in-situ and remote sensing investigations that will characterize the chemistry of the materials at the local surface, subsurface, and atmosphere. The Phoenix spacecraft was launched on August 4, 2007 and will arrive at Mars in May 2008. The lander includes a suite of seven (7) science instruments. This mission is baselined for up to 90 sols (Martian days) of digging, sampling, and analysis. Operating at the Mars polar region creates a challenging environment for the Phoenix landed subsystems and instruments with Mars surface temperature extremes between -120 deg C to 25 deg C and diurnal thermal cycling in excess of 145 deg C. Some engineering and science hardware inside the lander were qualification tested up to 80 deg C to account for self heating. Furthermore, many of the hardware for this mission were inherited from earlier missions: the lander from the Mars Surveyor Program 2001 (MSP'01) and instruments from the MSP'01 and the Mars Polar Lander. Ensuring all the hardware was properly qualified and flight acceptance tested to meet the environments for this mission required defining and implementing an environmental assurance program that included a detailed heritage review coupled with tailored flight acceptance testing. A heritage review process with defined acceptance success criteria was developed and is presented in this paper together with the lessons learned in its implementation. This paper also provides a detailed description of the environmental assurance program of the Phoenix Mars mission. This program includes assembly/subsystem and system level testing in the areas of dynamics, thermal, and electromagnetic compatibility, as well as venting/pressure, dust, radiation, and meteoroid analyses to meet the challenging environment of this mission.

  18. UHF Relay Antenna Measurements on Phoenix Mars Lander Mockup

    NASA Technical Reports Server (NTRS)

    Ilott, Peter; Harrel, Jefferson; Arnold, Bradford; Bliznyuk, Natalia; Nielsen, Rick; Dawson, David; McGee, Jodi

    2006-01-01

    The Phoenix Lander, a NASA Discovery mission which lands on Mars in the spring of 2008, will rely entirely on UHF relay links between it and Mars orbiting assets, (Odyssey and Mars Reconnaissance Orbiter (MRO)), to communicate with the Earth. As with the Mars Exploration Rover (MER) relay system, non directional antennas will be used to provide roughly emispherical coverage of the Martian sky. Phoenix lander deck object pattern interference and obscuration are significant, and needed to be quantified to answer system level design and operations questions. This paper describes the measurement campaign carried out at the SPAWAR (Space and Naval Warfare Research) Systems Center San Diego (SSC-SD) hemispherical antenna range, using a Phoenix deck mockup and engineering model antennas. One goal of the measurements was to evaluate two analysis tools, the time domain CST, and the moment method WIPL-D software packages. These would subsequently be used to provide pattern analysis for configurations that would be difficult and expensive to model and test on Earth.

  19. Phoenix Mars Scout UHF Relay-Only Operations

    NASA Technical Reports Server (NTRS)

    Lewicki, Christopher A.; Krajewski, Joel; Ilott, Peter; Dates, Jason

    2006-01-01

    The Phoenix Mars Scout Lander will launch in August 2007 and land on the northern plains of Mars in May of 2008. In a departure from traditional planetary surface mission operations, it will have no direct-to-Earth communications capability and will rely entirely on Mars-orbiting relays in order to facilitate command and control as well as the return of science and engineering data. The Mars Exploration Rover missions have demonstrated the robust data-return capability using this architecture, and also have demonstrated the capability of using this method for command and control. The Phoenix mission will take the next step and incorporate this as the sole communications link. Operations for 90 Sols will need to work within the constraints of Odyssey and Mars Reconnaissance Orbiter communications availability, anomalies must be diagnosed and responded to through an intermediary and on-board fault responses must be tolerant to loss of a relay. These and other issues pose interesting challenges and changes in paradigm for traditional space operations and spacecraft architecture, and the approach proposed for the Phoenix mission is detailed herein.

  20. UHF Relay Antenna Measurements on Phoenix Mars Lander Mockup

    NASA Technical Reports Server (NTRS)

    Ilott, Peter; Harrel, Jefferson; Arnold, Bradford; Bliznyuk, Natalia; Nielsen, Rick; Dawson, David; McGee, Jodi

    2006-01-01

    The Phoenix Lander, a NASA Discovery mission which lands on Mars in the spring of 2008, will rely entirely on UHF relay links between it and Mars orbiting assets, (Odyssey and Mars Reconnaissance Orbiter (MRO)), to communicate with the Earth. As with the Mars Exploration Rover (MER) relay system, non directional antennas will be used to provide roughly emispherical coverage of the Martian sky. Phoenix lander deck object pattern interference and obscuration are significant, and needed to be quantified to answer system level design and operations questions. This paper describes the measurement campaign carried out at the SPAWAR (Space and Naval Warfare Research) Systems Center San Diego (SSC-SD) hemispherical antenna range, using a Phoenix deck mockup and engineering model antennas. One goal of the measurements was to evaluate two analysis tools, the time domain CST, and the moment method WIPL-D software packages. These would subsequently be used to provide pattern analysis for configurations that would be difficult and expensive to model and test on Earth.

  1. Influence of exposure error and effect modification by socioeconomic status on the association of acute cardiovascular mortality with particulate matter in Phoenix.

    PubMed

    Wilson, William E; Mar, Therese F; Koenig, Jane Q

    2007-12-01

    Using ZIP code-level mortality data, the association of cardiovascular mortality with PM(2.5) and PM(10-2.5), measured at a central monitoring site, was determined for three populations at different distances from the monitoring site but with similar numbers of deaths and therefore similar statistical power. The % risk and statistical significance for the association of mortality with PM(2.5) fell off with distance from the monitor, as would be expected if exposure error increased with distance. However, the % risk for PM(10-2.5) increased in going from the population in Central Phoenix, where the monitoring site was located, to a population in a Middle Ring around Phoenix and fell off in an Outer Ring population. The % risks for the Outer Ring were low for each of the six lag days (0-5) and for the 6-day moving average. The lag structures for PM(2.5) and PM(10-2.5) also differed for the Central Phoenix and Middle Ring populations. These differences led us to examine the socioeconomic status (SES) of the populations. On the basis of education and income, the population in Central Phoenix had a lower SES than the Middle Ring. Thus, the differences between Central Phoenix and the Middle Ring may be due to effect modification by SES and differences in exposure error. However, the effect modification by SES may be different for thoracic coarse particulate matter (PM) than for fine PM. This study provides new information on the association of PM(10-2.5) with cardiovascular mortality. In the Middle Ring, the % risk per 10 microg/m3 increase in PM(10-2.5) concentration (lower and upper 95% confidence levels) for lag day 1 was 3.4 (1.0, 5.8) and for the 6-day distributed-lag was 3.8 (0.3, 7.5). The differences in lag structure for PM(2.5) and PM(10-2.5) provide evidence that the two particle size classes have health effects that are different and independent. This study also helps explain the high % risks for PM(2.5) found for Central Phoenix, 6.6 (1.1, 12.5) for lag day 1

  2. ON THE EXTENDED STRUCTURE OF THE PHOENIX DWARF GALAXY

    SciTech Connect

    Hidalgo, Sebastian L.; Aparicio, Antonio; MartInez-Delgado, David; Gallart, Carme E-mail: antapaj@iac.e E-mail: carme@iac.e

    2009-11-01

    We present the star formation history (SFH) and its variations with galactocentric distance for the Local Group dwarf galaxy of Phoenix. They have been derived from a (F555W, F814W) color-magnitude diagram obtained from WFPC2-HST data, which reaches the oldest main-sequence turnoffs. The IAC-star and IAC-pop codes and the MinnIAC suite have been used to obtain the star formation rate as a function of time and metallicity, psi(t, z). We find that Phoenix has had ongoing but gradually decreasing star formation over nearly a Hubble time. The highest level of star formation occurred from the formation of the galaxy till 10.5 Gyr ago, when 50% of the total star formation had already taken place. From that moment, star formation continues at a significant level until 6 Gyr ago (an additional 35% of the stars are formed in this time interval), and at a very low level till the present time. The chemical enrichment law shows a trend of slowly increasing metallicity as a function of time until 6-8 Gyr ago, when metallicity starts to increase steeply to the current value. We have paid particular attention to the study of the variations of the SFH as a function of radius. Young stars are found in the inner region of the galaxy only, but intermediate-age and old stars can be found at all galactocentric distances. The distribution of mass density in alive stars and its evolution with time has been studied. This study shows that star formation started at all galactocentric distances in Phoenix at an early epoch. If stars form in situ in Phoenix, the star formation onset took place all over the galaxy (up to a distance of about 400 pc from the center), but preferentially out of center regions. After that, our results are compatible with a scenario in which the star formation region envelope slowly shrinks as time goes on, possibly as a natural result of pressure support reduction as gas supply diminishes. As a consequence, the star formation stopped first (about 7-8 Gyr ago) in

  3. Visualizing the Operations of the Phoenix Mars Lander

    NASA Astrophysics Data System (ADS)

    Schwehr, K.; Andres, P.; Craig, J.; Deen, R.; de Jong, E.; Fortino, N.; Gorgian, Z.; Kuramura, K.; Lemmon, M.; Levoe, S.; Leung, C.; Lutz, N.; Ollerenshaw, R.; Smith, P.; Stetson, M.; Suzuki, S.; Phoenix Science Team

    2008-12-01

    With the successful landing of the Phoenix Mars Lander comes the task of visualizing the spacecraft, its operations and surrounding environment. The JPL Solar System Visualization team has brought together a wide range of talents and software to provide a suit of visualizations that shed light on the operations of this visitor to another world. The core set of tools range from web-based production tracking (Image Products Release Website), to custom 3D transformation software, through to studio quality 2D and 3D video production. We will demonstrate several of the key technologies that bring together these visualizations. Putting the scientific results of Phoenix in context requires managing the classic powers-of-10 problem. Everything from the location of polar dust storms down to the Atomic Force Microscope must be brought together in a context that communicates to both the scientific and public audiences. We used Lightwave to blend 2D and 3D visualizations into a continuous series of zooms using both simulations and actual data. Beyond the high-powered industrial strength solutions, we have strived to bring as much power down to the average computer user's standard view of the computer: the web browser. Zooming and Interactive Mosaics (ZIM) tool is a JavaScript web tool for displaying high-resolution panoramas in a spacecraft-centric view. This tool allows the user to pan and zoom through the mosaic, indentifying feature and target names, all the while maintaining a contextual frame-of-reference. Google Earth presents the possibility of taking hyperlinked web browser interaction into the 3D geo-browser modality. Until Google releases a Mars mode to Google Earth, we are forced to wrap the Earth in a Mars texture. However, this can still provide a suitable background for exploring interactive visualizations. These models range over both regional and local scales, with the lander positioned on Mars and the local environment mapped into pseudo-"Street View" modes

  4. Phosphorus in Phoenix: a budget and spatial representation of phosphorus in an urban ecosystem.

    PubMed

    Metson, Geneviève S; Hale, Rebecca L; Iwaniec, David M; Cook, Elizabeth M; Corman, Jessica R; Galletti, Christopher S; Childers, Daniel L

    2012-03-01

    As urban environments dominate the landscape, we need to examine how limiting nutrients such as phosphorus (P) cycle in these novel ecosystems. Sustainable management of P resources is necessary to ensure global food security and to minimize freshwater pollution. We used a spatially explicit budget to quantify the pools and fluxes of P in the Greater Phoenix Area in Arizona, USA, using the boundaries of the Central Arizona-Phoenix Long-Term Ecological Research site. Inputs were dominated by direct imports of food and fertilizer for local agriculture, while most outputs were small, including water, crops, and material destined for recycling. Internally, fluxes were dominated by transfers of food and feed from local agriculture and the recycling of human and animal excretion. Spatial correction of P dynamics across the city showed that human density and associated infrastructure, especially asphalt, dominated the distribution of P pools across the landscape. Phosphorus fluxes were dominated by agricultural production, with agricultural soils accumulating P. Human features (infrastructure, technology, and waste management decisions) and biophysical characteristics (soil properties, water fluxes, and storage) mediated P dynamics in Phoenix. P cycling was most notably affected by water management practices that conserve and recycle water, preventing the loss of waterborne P from the ecosystem. P is not intentionally managed, and as a result, changes in land use and demographics, particularly increased urbanization and declining agriculture, may lead to increased losses of P from this system. We suggest that city managers should minimize cross-boundary fluxes of P to the city. Reduced P fluxes may be accomplished through more efficient recycling of waste, therefore decreasing dependence on external nonrenewable P resources and minimizing aquatic pollution. Our spatial approach and consideration of both pools and fluxes across a heterogeneous urban ecosystem increases the

  5. Wet Chemistry experiments on the 2007 Phoenix Mars Scout Lander mission: Data analysis and results

    NASA Astrophysics Data System (ADS)

    Kounaves, S. P.; Hecht, M. H.; Kapit, J.; Gospodinova, K.; DeFlores, L.; Quinn, R. C.; Boynton, W. V.; Clark, B. C.; Catling, D. C.; Hredzak, P.; Ming, D. W.; Moore, Q.; Shusterman, J.; Stroble, S.; West, S. J.; Young, S. M. M.

    2010-01-01

    Chemical analyses of three Martian soil samples were performed using the Wet Chemistry Laboratories on the 2007 Phoenix Mars Scout Lander. One soil sample was obtained from the top ˜2 cm (Rosy Red) and two were obtained at ˜5 cm depth from the ice table interface (Sorceress 1 and Sorceress 2). When mixed with water in a ˜1:25 soil to solution ratio (by volume), a portion of the soil components solvated. Ion concentrations were measured using an array of ion selective electrodes and solution conductivity using a conductivity cell. The measured concentrations represent the minimum leachable ions in the soil and do not take into account species remaining in the soil. Described is the data processing and analysis for determining concentrations of seven ionic species directly measured in the soil/solution mixture. There were no significant differences in concentrations, pH, or conductivity, between the three samples. Using laboratory experiments, refinement of the surface calibrations, and modeling, we have determined a pH for the soil solution of 7.7(±0.3), under prevalent conditions, carbonate buffering, and PCO2 in the cell headspace. Perchlorate was the dominant anion in solution with a concentration for Rosy Red of 2.7(±1) mM. Equilibrium modeling indicates that measured [Ca2+] at 0.56(±0.5) mM and [Mg2+] at 2.9(±1.5) mM, are consistent with carbonate equilibrium for a saturated solution. The [Na+] and [K+] were 1.4(±0.6), and 0.36(±0.3) mM, respectively. Results indicate that the leached portion of soils at the Phoenix landing site are slightly alkaline and dominated by carbonate and perchlorate. However, it should be noted that there is a 5-15 mM discrepancy between measured ions and conductivity and another species may be present.

  6. Comparison of Phoenix Meteorological Data with Viking Data Using Model MLAM

    NASA Astrophysics Data System (ADS)

    Schmidt, Walter; Harri, Ari-Matti; Kauhanen, Janne; Merikallio, Sini; Savijärvi, Hannu

    2010-05-01

    During 151 Martian days in 2008 the Canadian Meteorology experiment (MET) [1] on board NASA's Phoenix '07 Lander was providing for the first time surface based observations of atmospheric pressure, temperature and wind as well as dust and ice particles in the Martian Northern polar regions, 20 degrees north of the location of Viking Lander 2, the until then northernmost meteorological observatory on Mars. Using the Mars Limited Area Model (MLAM), jointly developed by the Helsinki University and the Finnish Meteorological Institute to study mesoscale phenomena in the Martian Atmosphere [2], the observations can be put into a larger context suitable for comparison with long term measurements at the Viking landing site three decades earlier. The seasonal variations observed at both latitudes are very similar though the onset of winter dominated climate is faster at higher latitudes. In case the re-activation efforts of Phoenix should be successful, first results for the Martian Spring at high latitudes will be shown, too. The meteorological observations over a long period of time and at different latitudes are important for the preparation of the planned future Martian landing missions Mars Science Laboratory (MSL) 2011, the ESA - NASA ExoMars program 2016-2018 and the Finnish-Russian-Spanish MetNet mission after 2011, where different meteorological stations will be deployed at low and high latitudes and low and high altitudes. Mission optimization makes reliable climate estimates mandatory. References [1] Taylor, P. A., D. C. Catling, M. Daly, C. S. Dickinson, H. P. Gunnlaugsson, A.-M. Harri, and C. F. Lange (2008), J. Geophys. Res., 113, E00A10 [2] Kauhanen, J., Siili, T., Järvenoja, S. and Savijärvi, H. (2008), J. Geophys. Res., 113, E00A14

  7. Thermal and Evolved Gas Behavior of Calcite Under Mars Phoenix TEGA Operating Conditions

    NASA Technical Reports Server (NTRS)

    Ming, D.W.; Niles, P.B.; Morris, R.V.; Boynton, W.V.; Golden, D.C.; Lauer, H.V.; Sutter, B.

    2009-01-01

    The Mars Phoenix Scout Mission with its diverse instrument suite successfully examined several soils on the Northern plains of Mars. The Thermal and Evolved Gas Analyzer (TEGA) was employed to detect organic and inorganic materials by coupling a differential scanning calorimeter (DSC) with a magnetic-sector mass spectrometer (MS). Martian soil was heated up to 1000 C in the DSC ovens and evolved gases from mineral decomposition products were examined with the MS. TEGA s DSC has the capability to detect endothermic and exothermic reactions during heating that are characteristic of minerals present in the Martian soil. Initial TEGA results indicated the presence of endothermic peaks with onset temperatures that ranged from 675 C to 750 C with corresponding CO2 release. This result suggests the presence of calcite (CaCO3. CaO + CO2). Organic combustion to CO2 is not likely since this mostly occurs at temperatures below 550 C. Fe-carbonate and Mg-carbonate are not likely because their decomposition temperatures are less than 600 C. TEGA enthalpy determinations suggest that calcite, may occur in the Martian soil in concentrations of approx.1 to 5 wt. %. The detection of calcite could be questioned based on previous results that suggest Mars soils are mostly acidic. However, the Phoenix landing site soil pH was measured at pH 8.3 0.5, which is typical of terrestrial soils where pH is controlled by calcite solubility. The range of onset temperatures and calcite concentration as calculated by TEGA is poorly con-strained in part because of limited thermal data of cal-cite at reduced pressures. TEGA operates at <30 mbar while most calcite literature thermal data was obtained at 1000 mbar or higher pressures.

  8. Coral mortality associated with thermal fluctuations in the Phoenix Islands, 2002-2005

    NASA Astrophysics Data System (ADS)

    Obura, D.; Mangubhai, S.

    2011-09-01

    The Phoenix Islands (Republic of Kiribati, 172-170°W and 2.5-5°S) experience intra- and inter-annual sea surface temperature variability of ≈2°C and have few local anthropogenic impacts. From July 2002, a thermal stress event occurred, which peaked at 21 Degree Heating Weeks (DHW) in January 2003 and persisted for 4 years. Such thermal stress was greater than any thermal event reported in the coral reef literature. Reef surveys were conducted in July 2000, June 2002, and May 2005, for six of the eight islands. Sampling was stratified by exposure (windward, leeward, and lagoon) and depth (5, 10, 15, and 25 m). The thermal stress event caused mass coral mortality, and coral cover declined by approximately 60% between 2002 and 2005. However, mortality varied among sites (12-100%) and among islands (42-79%) and varied in accordance with the presence of a lagoon, island size, and windward vs. leeward exposure. Leeward reefs experienced the highest and most consistent decline in coral cover. Island size and the presence of a lagoon showed positive correlations with coral mortality, most likely because of the longer water residence time enhancing heating. Windward reefs showed cooler conditions than leeward reefs. Recently dead corals were observed at depths >35 m on windward and >45 m on leeward reefs. Between-island variation in temperature had no effect on between-island variation in coral mortality. Mortality levels reported here were comparable to those reported for the most extreme thermal stress events of 9-10 DHW in other regions. These results highlight the high degree of acclimation and/or adaptation of the corals in the Phoenix Islands to their local temperature regime, and their consequent vulnerability to anomalous events. Moreover, the results suggest the need to adjust thermal stress calculations to reflect local temperature variation.

  9. 77 FR 26039 - Notice of Availability of the Final Environmental Impact Statement for the Phoenix Copper Leach...

    Federal Register 2010, 2011, 2012, 2013, 2014

    2012-05-02

    ... Impact Statement for the Phoenix Copper Leach Project, Lander County, NV AGENCY: Bureau of Land... Phoenix Copper Leach Project and by this notice is announcing its availability. DATES: The BLM will not... Phoenix Copper Leach Project are available for public inspection at the BLM, 50 Bastian Road,...

  10. 76 FR 51461 - Notice of Release From Quitclaim Deed and Federal Grant Assurance Obligations for Phoenix-Mesa...

    Federal Register 2010, 2011, 2012, 2013, 2014

    2011-08-18

    ... Obligations for Phoenix-Mesa Gateway Airport, Mesa, AZ AGENCY: Federal Aviation Administration, DOT. ACTION... airport property at Phoenix-Mesa Gateway, Mesa, Arizona, from all conditions contained in the Quitclaim... FAA must be mailed or delivered to Mr. Walter Fix, Phoenix-Gateway Airport Authority, 5835 S....

  11. Report of Final Evaluation, ESEA Title I Projects, Fiscal Year 1972. Phoenix Area Bureau of Indian Affairs.

    ERIC Educational Resources Information Center

    Bureau of Indian Affairs (Dept. of Interior), Phoenix, AZ.

    Title I projects operated in the Bureau of Indian Affairs (BIA), Phoenix Area, during Fiscal 1972 are described in this final evaluation report. An overview of the geographical location of Areas within the BIA is given, along with the organization of the BIA at large and of the Phoenix Area. Enrollments in the Phoenix Area projects are presented…

  12. Near vertical view of Phoenix, Arizona as seen from Apollo 9

    NASA Image and Video Library

    1969-03-09

    AS09-22-3441 (March 1969) --- Near vertical view of the Phoenix, Arizona area as photographed from the Apollo 9 spacecraft during its Earth-orbital mission. Farmland patterns checkerboard the area along the Gila River. Phoenix is located right of center near the clouds.

  13. A Study of the Phoenix Union High School for the Citizens' Advisory Committee.

    ERIC Educational Resources Information Center

    Stanley, Harry M.

    This study identifies the educational problems found at the Phoenix Union High School, in Phoenix, Arizona, during the months of March, April, and May of 1970. A Determination was made of the opinions of the residents of the community living within the attendance area of the high school, of the students attending the high school, of some of the…

  14. Phoenix Union Bilingual Program. Content Analysis Schedule for Bilingual Education Programs.

    ERIC Educational Resources Information Center

    Nafus, C.; Shore, Marietta Saravia

    This content analysis schedule for the Phoenix Union Bilingual Program of Phoenix, Arizona, presents information on the history, funding, and scope of the project in its third year. Included are sociolinguistic process variables such as the native and dominant languages of students and their interaction. Information is provided on staff selection…

  15. Carpological analysis of Phoenix (Arecaceae): contributions to the taxonomy and evolutionary history of the genus

    USDA-ARS?s Scientific Manuscript database

    The main purpose of this study was, first, to analyze the morphology of seeds of Phoenix spp. and relevant cultivars and to assess the taxonomic value of the information generated as a means of studying the systematics and evolutionary history of the genus Phoenix. We then analyzed seed morphologica...

  16. A comprehensive sustainability appraisal of water governance in Phoenix, AZ.

    PubMed

    Larson, Kelli L; Wiek, Arnim; Withycombe Keeler, Lauren

    2013-02-15

    In Phoenix, Arizona and other metropolitan areas, water governance challenges include variable climate conditions, growing demands, and continued groundwater overdraft. Based on an actor-oriented examination of who does what with water and why, along with how people interact with hydro-ecological systems and man-made infrastructure, we present a sustainability appraisal of water governance for the Phoenix region. Broadly applicable to other areas, our systems approach to sustainable water governance overcomes prevailing limitations to research and management by: employing a comprehensive and integrative perspective on water systems; highlighting the activities, intentions, and rules that govern various actors, along with the values and goals driving decisions; and, establishing a holistic set of principles for social-ecological system integrity and interconnectivity, resource efficiency and maintenance, livelihood sufficiency and opportunity, civility and democratic governance, intra- and inter-generational equity, and finally, precaution and adaptive capacity. This study also contributes to reforming and innovating governance regimes by illuminating how these principles are being met, or not, in the study area. What is most needed in metropolitan Phoenix is enhanced attention to ecosystem functions and resource maintenance as well as social equity and public engagement in water governance. Overall, key recommendations entail: addressing interconnections across hydrologic units and sub-systems (e.g., land and water), increasing decentralized initiatives for multiple purposes (e.g., ecological and societal benefits of green infrastructure), incorporating justice goals into decisions (e.g., fair allocations and involvement), and building capacity through collaborations and social learning with diverse interests (e.g., scientists, policymakers, and the broader public).

  17. Land use mapping and modelling for the Phoenix Quadrangle

    NASA Technical Reports Server (NTRS)

    Place, J. L. (Principal Investigator)

    1974-01-01

    The author has identified the following significant results. The mapping of generalized land use (level 1) from ERTS 1 images was shown to be feasible with better than 95% accuracy in the Phoenix quadrangle. The accuracy of level 2 mapping in urban areas is still a problem. Updating existing maps also proved to be feasible, especially in water categories and agricultural uses; however, expanding urban growth has presented with accuracy. ERTS 1 film images indicated where areas of change were occurring, thus aiding focusing-in for more detailed investigation. ERTS color composite transparencies provided a cost effective source of information for land use mapping of very large regions at small map scales.

  18. Atmospheric Condensation in the Mars Phoenix TECP and MET Data

    NASA Technical Reports Server (NTRS)

    Zent, A. P.

    2015-01-01

    A new calibration function for the humidity sensor in the Thermal and Electrical Conductivity Probe (TECP), a component of the Microscopy, Electrochemistry, and Conductivity Analyzer (MECA) on the Phoenix Mars mission has been developed. The data is now cast in terms of Frost Point (T(sub f)) and some flight data, taken when the atmosphere is independently known to be saturated, is included in the calibration data set. Combined with data from the Meteorology Mast air temperature sensors, a very sensitive detection of atmospheric saturation becomes possible (Figure 1).

  19. Evaluation of the BD Phoenix system for identification of a wide spectrum of clinically important yeast species: a comparison with Vitek 2-YST.

    PubMed

    Won, Eun Jeong; Shin, Jong Hee; Kim, Mi-Na; Choi, Min Ji; Joo, Min Young; Kee, Seung Jung; Shin, Myung Geun; Suh, Soon Pal; Ryang, Dong Wook

    2014-08-01

    The Phoenix Yeast ID and Vitek 2-YST panels were compared using 351 molecularly identified yeast isolates. The Phoenix showed a comparable rate of correct identification for 4 common (Phoenix, 98%; Vitek, 94%) and 45 uncommon species (Phoenix, 70%; Vitek, 64%) and had a shorter mean identification time (6-7 h).

  20. Vulnerability assessment of climate-induced water shortage in Phoenix.

    PubMed

    Gober, Patricia; Kirkwood, Craig W

    2010-12-14

    Global warming has profound consequences for the climate of the American Southwest and its overallocated water supplies. This paper uses simulation modeling and the principles of decision making under uncertainty to translate climate information into tools for vulnerability assessment and urban climate adaptation. A dynamic simulation model, WaterSim, is used to explore future water-shortage conditions in Phoenix. Results indicate that policy action will be needed to attain water sustainability in 2030, even without reductions in river flows caused by climate change. Challenging but feasible changes in lifestyle and slower rates of population growth would allow the region to avoid shortage conditions and achieve groundwater sustainability under all but the most dire climate scenarios. Changes in lifestyle involve more native desert landscaping and fewer pools in addition to slower growth and higher urban densities. There is not a single most likely or optimal future for Phoenix. Urban climate adaptation involves using science-based models to anticipate water shortage and manage climate risk.

  1. Morning Frost in Trench Dug by Phoenix, Sol 113

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This image from the Surface Stereo Imager on NASA's Phoenix Mars Lander shows morning frost inside the 'Snow White' trench dug by the lander, in addition to subsurface ice exposed by use of a rasp on the floor of the trench.

    The camera took this image at about 9 a.m. local solar time during the 113th Martian day of the mission (Sept. 18, 2008). Bright material near and below the four-by-four set of rasp holes in the upper half of the image is water-ice exposed by rasping and scraping in the trench earlier the same morning. Other bright material especially around the edges of the trench, is frost. Earlier in the mission, when the sun stayed above the horizon all night, morning frost was not evident in the trench.

    This image is presented in approximately true color.

    The trench is 4 to 5 centimeters (about 2 inches) deep, about 23 centimeters (9 inches) wide.

    Phoenix landed on a Martian arctic plain on May 25, 2008. The mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is led by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development was by Lockheed Martin Space Systems, Denver.

  2. The Thermal Electrical Conductivity Probe (TECP) for Phoenix

    NASA Technical Reports Server (NTRS)

    Zent, Aaron P.; Hecht, Michael H.; Cobos, Doug R.; Campbell, Gaylon S.; Campbell, Colin S.; Cardell, Greg; Foote, Marc C.; Wood, Stephen E.; Mehta, Manish

    2009-01-01

    The Thermal and Electrical Conductivity Probe (TECP) is a component of the Microscopy, Electrochemistry, and Conductivity Analyzer (MECA) payload on the Phoenix Lander. TECP will measure the temperature, thermal conductivity and volumetric heat capacity of the regolith. It will also detect and quantify the population of mobile H2O molecules in the regolith, if any, throughout the polar summer, by measuring the electrical conductivity of the regolith, as well as the dielectric permittivity. In the vapor phase, TECP is capable of measuring the atmospheric H2O vapor abundance, as well as augment the wind velocity measurements from the meteorology instrumentation. TECP is mounted near the end of the 2.3 m Robotic Arm, and can be placed either in the regolith material or held aloft in the atmosphere. This paper describes the development and calibration of the TECP. In addition, substantial characterization of the instrument has been conducted to identify behavioral characteristics that might affect landed surface operations. The greatest potential issue identified in characterization tests is the extraordinary sensitivity of the TECP to placement. Small gaps alter the contact between the TECP and regolith, complicating data interpretation. Testing with the Phoenix Robotic Arm identified mitigation techniques that will be implemented during flight. A flight model of the instrument was also field tested in the Antarctic Dry Valleys during the 2007-2008 International Polar year. 2

  3. Morning Frost in Trench Dug by Phoenix, Sol 113

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This image from the Surface Stereo Imager on NASA's Phoenix Mars Lander shows morning frost inside the 'Snow White' trench dug by the lander, in addition to subsurface ice exposed by use of a rasp on the floor of the trench.

    The camera took this image at about 9 a.m. local solar time during the 113th Martian day of the mission (Sept. 18, 2008). Bright material near and below the four-by-four set of rasp holes in the upper half of the image is water-ice exposed by rasping and scraping in the trench earlier the same morning. Other bright material especially around the edges of the trench, is frost. Earlier in the mission, when the sun stayed above the horizon all night, morning frost was not evident in the trench.

    This image is presented in approximately true color.

    The trench is 4 to 5 centimeters (about 2 inches) deep, about 23 centimeters (9 inches) wide.

    Phoenix landed on a Martian arctic plain on May 25, 2008. The mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is led by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development was by Lockheed Martin Space Systems, Denver.

  4. Vulnerability assessment of climate-induced water shortage in Phoenix

    PubMed Central

    Gober, Patricia; Kirkwood, Craig W.

    2010-01-01

    Global warming has profound consequences for the climate of the American Southwest and its overallocated water supplies. This paper uses simulation modeling and the principles of decision making under uncertainty to translate climate information into tools for vulnerability assessment and urban climate adaptation. A dynamic simulation model, WaterSim, is used to explore future water-shortage conditions in Phoenix. Results indicate that policy action will be needed to attain water sustainability in 2030, even without reductions in river flows caused by climate change. Challenging but feasible changes in lifestyle and slower rates of population growth would allow the region to avoid shortage conditions and achieve groundwater sustainability under all but the most dire climate scenarios. Changes in lifestyle involve more native desert landscaping and fewer pools in addition to slower growth and higher urban densities. There is not a single most likely or optimal future for Phoenix. Urban climate adaptation involves using science-based models to anticipate water shortage and manage climate risk. PMID:21149729

  5. After Rasping by Phoenix in 'Snow White' Trench, Sol 60

    NASA Technical Reports Server (NTRS)

    2008-01-01

    NASA's Phoenix Mars Lander used the motorized rasp on the back of its robotic arm scoop during the mission's 60th Martian day, or sol, (July 26, 2008) to penetrate a hard layer at the bottom of a trench informally called 'Snow White.' This view, taken by the lander's Surface Stereo Imager and presented in approximately true color, shows the trench later the same sol.

    Most of the 16 holes left by a four-by-four array of rasp placements are visible in the central area of the image.

    A total 3 cubic centimeters, or about half a teaspoon, of material was collected in the scoop. Material in the scoop was collected both by the turning rasp, which threw material into the scoop through an opening at the back of the scoop, and by the scoop's front blade, which was run over the rasped area to pick up more shavings.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  6. After Rasping by Phoenix in 'Snow White' Trench, Sol 60

    NASA Technical Reports Server (NTRS)

    2008-01-01

    NASA's Phoenix Mars Lander used the motorized rasp on the back of its robotic arm scoop during the mission's 60th Martian day, or sol, (July 26, 2008) to penetrate a hard layer at the bottom of a trench informally called 'Snow White.' This view, taken by the lander's Surface Stereo Imager and presented in approximately true color, shows the trench later the same sol.

    Most of the 16 holes left by a four-by-four array of rasp placements are visible in the central area of the image.

    A total 3 cubic centimeters, or about half a teaspoon, of material was collected in the scoop. Material in the scoop was collected both by the turning rasp, which threw material into the scoop through an opening at the back of the scoop, and by the scoop's front blade, which was run over the rasped area to pick up more shavings.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  7. VLA, PHOENIX and BATSE observations of an X1 flare

    NASA Astrophysics Data System (ADS)

    Willson, Robert F.; Aschwanden, Marcus J.; Benz, Arnold O.

    1992-01-01

    We present observations of an X1 flare detected simultaneously with the Very Large Array (VLA), the PHOENIX Digital Radio Spectrometer, and the Burst and Transient Source Experiment (BATSE) aboard the Gamma Ray Observatory (GRO). The VLA was used to produce snapshot maps of the impulsive burst emission in the higher corona on timescales of 1.7 seconds at both 20 and 01 cm. Our results indicate electron acceleration several minutes before the onset of the hard X-ray burst detected by BATSE. Comparisons with high spectral and spatial observations by PHOENIX reveal a variety of radio bursts at 20 cm, such as type III bursts, intermediate drift bursts, and quasi-periodic pulsations during different stages of the X1 flare. From the drift rates of these radio bursts we derive information on local density scale heights, the speed of radio exciters, and the local magnetic field. Radio emission at 90 cm shows a type IV burst moving outward with a constant velocity of 240 km/sec. The described X1 flare is unique in the sense that it appeared at the east limb (N06/E88 providing the most accurate information on the vertical structure of different flare tracers visible in radio wavelengths.

  8. VLA, PHOENIX, and BATSE observations of an X1 flare

    NASA Astrophysics Data System (ADS)

    Willson, Robert F.; Aschwanden, Markus J.; Benz, Arnold O.

    1992-02-01

    We present observations of an X1 flare (18 Jul. 1991) detected simultaneously with the Very Large Array (VLA), the PHOENIX Digital Radio Spectrometer and the Burst and Transient Source Experiment (BATSE) aboard the Gamma Ray Observatory (GRO). The VLA was used to produce snapshot maps of the impulsive acceleration in the higher corona several minutes before the onset of the hard x ray burst detected by BATSE. Comparisons with high spectral and temporal observations by PHOENIX reveal a variety of radio bursts at 20 cm, such as type 3 bursts, intermediate drift bursts, and quasi-periodic pulsations during different stages of the X1 flare. From the drift rates of these radio bursts we derive information on local density scale heights, the speed of radio exciters, and the local magnetic field. Radio emission at 90 cm shows a type 4 burst moving outward with a constant velocity of 240 km/s. The described X1 flare is unique in the sense that it appeared at the east limb (N06/E88), providing the most accurate information on the vertical structure of different flare tracers visible in radio wavelengths.

  9. Analysis of Effectiveness of Phoenix Entry Reaction Control System

    NASA Technical Reports Server (NTRS)

    Dyakonov, Artem A.; Glass, Christopher E.; Desai, Prasun, N.; VanNorman, John W.

    2008-01-01

    Interaction between the external flowfield and the reaction control system (RCS) thruster plumes of the Phoenix capsule during entry has been investigated. The analysis covered rarefied, transitional, hypersonic and supersonic flight regimes. Performance of pitch, yaw and roll control authority channels was evaluated, with specific emphasis on the yaw channel due to its low nominal yaw control authority. Because Phoenix had already been constructed and its RCS could not be modified before flight, an assessment of RCS efficacy along the trajectory was needed to determine possible issues and to make necessary software changes. Effectiveness of the system at various regimes was evaluated using a hybrid DSMC-CFD technique, based on DSMC Analysis Code (DAC) code and General Aerodynamic Simulation Program (GASP), the LAURA (Langley Aerothermal Upwind Relaxation Algorithm) code, and the FUN3D (Fully Unstructured 3D) code. Results of the analysis at hypersonic and supersonic conditions suggest a significant aero-RCS interference which reduced the efficacy of the thrusters and could likely produce control reversal. Very little aero-RCS interference was predicted in rarefied and transitional regimes. A recommendation was made to the project to widen controller system deadbands to minimize (if not eliminate) the use of RCS thrusters through hypersonic and supersonic flight regimes, where their performance would be uncertain.

  10. Phoenix Lander Self Portrait on Mars, Vertical Projection

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This view is a vertical projection that combines hundreds of exposures taken by the Surface Stereo Imager camera on NASA's Mars Phoenix Lander and projects them as if looking down from above.

    The black circle is where the camera itself is mounted on the lander, out of view in images taken by the camera. North is toward the top of the image.

    This view comprises more than 100 different Stereo Surface Imager pointings, with images taken through three different filters at each pointing. The images were taken throughout the period from the 13th Martian day, or sol, after landing to the 47th sol (June 5 through July 12, 2008). The lander's Robotic Arm appears cut off in this mosaic view because component images were taken when the arm was out of the frame.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  11. Martian Soil Delivery to Analytical Instrument on Phoenix

    NASA Technical Reports Server (NTRS)

    2008-01-01

    The Robotic Arm of NASA's Phoenix Mars Lander released a sample of Martian soil onto a screened opening of the lander's Thermal and Evolved-Gas Analyzer (TEGA) during the 12th Martian day, or sol, since landing (June 6, 2008). TEGA did not confirm that any of the sample had passed through the screen.

    The Robotic Arm Camera took this image on Sol 12. Soil from the sample delivery is visible on the sloped surface of TEGA, which has a series of parallel doors. The two doors for the targeted cell of TEGA are the one positioned vertically, at far right, and the one partially open just to the left of that one. The soil between those two doors is resting on a screen designed to let fine particles through while keeping bigger ones Efrom clogging the interior of the instrument. Each door is about 10 centimeters (4 inches) long.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  12. Disbalance between mortality and non-fatal vascular events in the CHAMPION-PHOENIX trial: the cangrelor efficacy challenge.

    PubMed

    Serebruany, Victor L; Pokov, Alex N; Fortmann, Seth D; DiNicolantonio, James J

    2014-01-01

    The recently published, largest trial with cangrelor, the Cangrelor versus Standard Therapy to Achieve Optimal Management of Platelet Inhibition (CHAMPION)-PHOENIX, suggested that the experimental agent significantly reduced the rate of stent thrombosis (ST) and myocardial infarction (MI) during PCI at 48 hours (h) and 30 days. However, the declared impressive cangrelor vascular non-fatal benefit was contradicted by identical deaths at 48 h, and a trend toward excess mortality at 30 days. We analysed the mismatch between outcomes in the CHAMPION-PHOENIX trial. The trial reported identical mortality (18 death in each arm; odds ratio [OR] 1.00 (0.52-1.92); p>0.999) at 48 h, but more deaths, 60 vs 55, after cangrelor at 30 days. There was a significant reduction of ST from 0.8% (n=46) of the patients in the cangrelor group versus 1.4% (n=74) in the clopidogrel group (odds ratio, 0.62; 95% CI, 0.43 to 0.90; p= 0.01) at 48 h, and a persistent but less impressive ST prevention benefit OR of 0.68 (0.50=0.92, p = 0.01) at 30 days. There were also 48 less MI's following cangrelor usage enforced by a significant difference (odds ratio 0.80 (0.67-0.97) p = 0.02), which was also less prevalent at 30 days (OR 0.82 (0.68-0.98), p = 0.03). The reported ST/MI advantage should result in at least a trend towards numerically less deaths after cangrelor at 30 days follow-up, which was opposite of the results reported in CHAMPION-PHOENIX trial. Efficacy of cangrelor is challenged by the disproportional "reduction" of ST and MI conflicting with identical mortality at 48 h and worsened at day 30 fatalities. The dissociation between vascular mortality and non-fatal vascular ischaemic occlusions, unless compensated by some other unreported cause(s) of death, should be explored and explained. Unadjudicated 30-day outcomes, and all ST types should be fully disclosed. The ongoing FDA cangrelor review should focus on appropriate event count and/or possible mismatch between site-reported and

  13. Sublimation of Exposed Snow Queen Surface Water Ice as Observed by the Phoenix Mars Lander

    NASA Astrophysics Data System (ADS)

    Markiewicz, W. J.; Keller, H. U.; Kossacki, K. J.; Mellon, M. T.; Stubbe, H. F.; Bos, B. J.; Woida, R.; Drube, L.; Leer, K.; Madsen, M. B.; Goetz, W.; El Maarry, M. R.; Smith, P.

    2008-12-01

    One of the first images obtained by the Robotic Arm Camera on the Mars Phoenix Lander was that of the surface beneath the spacecraft. This image, taken on sol 4 (Martian day) of the mission, was intended to check the stability of the footpads of the lander and to document the effect the retro-rockets had on the Martian surface. Not completely unexpected the image revealed an oval shaped, relatively bright and apparently smooth object, later named Snow Queen, surrounded by the regolith similar to that already seen throughout the landscape of the landing site. The object was suspected to be the surface of the ice table uncovered by the blast of the retro-rockets during touchdown. High resolution HiRISE images of the landing site from orbit, show a roughly circular dark region of about 40 m diameter with the lander in the center. A plausible explanation for this region being darker than the rest of the visible Martian Northern Planes (here polygonal patterns) is that a thin layer of the material ejected by the retro-rockets covered the original surface. Alternatively the thrusters may have removed the fine surface dust during the last stages of the descent. A simple estimate requires that about 10 cm of the surface material underneath the lander is needed to be ejected and redistributed to create the observed dark circular region. 10 cm is comparable to 4-5 cm predicted depth at which the ice table was expected to be found at the latitude of the Phoenix landing site. The models also predicted that exposed water ice should sublimate at a rate not faster but probably close to 1 mm per sol. Snow Queen was further documented on sols 5, 6 and 21 with no obvious changes detected. The following time it was imaged was on sol 45, 24 sols after the previous observation. This time some clear changes were obvious. Several small cracks, most likely due to thermal cycling and sublimation of water ice appeared. Nevertheless, the bulk of Snow Queen surface remained smooth. The next

  14. Synchronous egress and ingress fluid flow related to compressional reactivation of basement faults: the Phoenix and Gryphon uranium deposits, southeastern Athabasca Basin, Saskatchewan, Canada

    NASA Astrophysics Data System (ADS)

    Li, Zenghua; Chi, Guoxiang; Bethune, Kathryn M.; Eldursi, Khalifa; Thomas, David; Quirt, David; Ledru, Patrick

    2017-05-01

    Previous studies on unconformity-related uranium deposits in the Athabasca Basin (Canada) suggest that egress flow and ingress flow can develop along single fault systems at different stages of compressional deformation. This research aims to examine whether or not both ingress and egress flow can develop at the same time within an area under a common compressional stress field, as suggested by the reverse displacement of the unconformity surface by the basement faults. The study considers the Phoenix and Gryphon uranium deposits in the Wheeler River area in the southeastern part of the Athabasca Basin. Two-dimensional numerical modeling of fluid flow, coupled with compressional deformation and thermal effects, was carried out to examine the fluid flow pattern. The results show that local variations in the basement geology under a common compressional stress field can result in both egress and ingress flow at the same time. The fault zone at Phoenix underwent a relatively low degree of deformation, as reflected by minor reverse displacement of the unconformity, and egress flow developed, whereas the fault zone at Gryphon experienced a relatively high degree of deformation, as demonstrated by significant reverse displacement of the unconformity, and ingress flow was dominant. The correlation between strain development and location of uranium mineralization, as exemplified by Gryphon and Phoenix uranium deposits, suggests that the localization of dilation predicted by numerical modeling may represent favourable sites for uranium mineralization in the Athabasca Basin.

  15. Thermal and Evolved Gas Analysis of Geologic Samples Containing Organic Materials: Implications for the 2007 Mars Phoenix Scout Mission

    NASA Technical Reports Server (NTRS)

    Lauer, H. V., Jr.; Ming, Douglas W.; Golden, D. C.; Boynton, W. V.

    2006-01-01

    The Thermal and Evolved Gas Analyzer (TEGA) instrument scheduled to fly onboard the 2007 Mars Phoenix Scout Mission will perform differential scanning calorimetry (DSC) and evolved gas analysis (EGA) of soil samples and ice collected from the surface and subsurface at a northern landing site on Mars. We have been developing a sample characterization data library using a laboratory DSC integrated with a quadrupole mass spectrometer to support the interpretations of TEGA data returned during the mission. The laboratory TEGA test-bed instrument has been modified to operate under conditions similar to TEGA, i.e., reduced pressure (e.g., 100 torr) and reduced carrier gas flow rates. We have previously developed a TEGA data library for a variety of volatile-bearing mineral phases, including Fe-oxyhydroxides, phyllosilicates, carbonates, and sulfates. Here we examine the thermal and evolved gas properties of samples that contain organics. One of the primary objectives of the Phoenix Scout Mission is to search for habitable zones by assessing organic or biologically interesting materials in icy soil. Nitrogen is currently the carrier gas that will be used for TEGA. In this study, we examine two possible modes of detecting organics in geologic samples; i.e., pyrolysis using N2 as the carrier gas and combustion using O2 as the carrier gas.

  16. Thermal and Evolved-Gas Analyzer for Phoenix Mars Lander

    NASA Technical Reports Server (NTRS)

    2007-01-01

    NASA's Phoenix Mars Lander carries an instrument to heat and sniff samples of Martian soil and ice to analyze some ingredients.

    The Thermal and Evolved-Gas Analyzer will study substances that are converted to gases by heating samples delivered to this instrument by the lander's robotic arm. It provides two types of information. One of its tools, called a differential scanning calorimeter (on the left in this photograph) monitors how much power is required to increase the temperature of the sample at a constant rate. This reveals which temperatures are transition points from solid to liquid and from liquid to gas for ingredients in the sample. The gases that are released, or 'evolved' by this heating then go to a mass spectrometer (on the right), a tool that can identify the chemicals.

  17. Evaluation of the IL-Phoenix chemistry electrolyte analyser

    PubMed Central

    Masiá, F.; Alumá, A.; Biosca, C.; Easamajó, M. T.; Antoja, F.; Galimany, R.

    1993-01-01

    This paper reports an evaluation of the IL-Phoenix Chemistry/Electrolyte Analyser; the evaluation was carried out in accordance with internationally recognized guidelines. The evaluation was performed in three steps: evaluation in routine conditions; assessment of interferences; and study of practicability. Seven constituents were studied under routine working conditions. Within-run imprecision rangedfrom 0.6% (CV) for chloride to 3.1% (CV) for glucose. Between-run imprecision ranged from 0.9% for sodium to 6.0% (CV) for urea. Sample-related carryover was not significant. The relative inaccuracy was acceptable; drift was negligible; linearity was agreed with the range showed by the supplier. Haemoglobin produced negative interferences with sodium and chloride. Turbidity interfered negatively with sodium, chloride, potassium and total calcium, andpositively with glucose. Bilirubin showed a negative interference with sodium, chloride and creatinine. PMID:18924967

  18. Vegetative community control of freshwater availability: Phoenix Islands case study

    NASA Astrophysics Data System (ADS)

    Engels, M.; Heinse, R.

    2014-12-01

    On small low islands with limited freshwater resources, terrestrial plant communities play a large role in moderating freshwater availability. Freshwater demands of vegetative communities are variable depending on the composition of the community. Hence, changes to community structure from production crop introductions, non-native species invasions, and climate change, may have significant implications for freshwater availability. Understanding how vegetative community changes impact freshwater availability will allow for better management and forecasting of limited freshwater supplies. To better understand these dynamics, we investigated three small tropical atolls in the Phoenix Island Protected Area, Kiribati. Despite their close proximity, these islands receive varying amounts of rainfall, are host to different plant communities and two of the islands have abandoned coconut plantations. Using electromagnetic induction, ground penetrating radar, soil samples, climate and satellite data, we present preliminary estimates of vegetative water demand for different tropical plant communities.

  19. Behavioral management at the Phoenix Zoo: new strategies and perspectives.

    PubMed

    Tresz, Hilda

    2006-01-01

    It all started with a seemingly simple decision to re-evaluate and document the Phoenix Zoo's behavioral management protocol. The purpose of this project was to present proactive standards for the care and psychological well-being of our living collection, while meeting or exceeding the guidelines of the Animal Welfare Act (U. S. Department of Agriculture Animal and Plant Health and Inspection Service, Animal Care, 1999). Preparing the protocol was a catalyst to re-evaluate the zoo's philosophy and application of behavioral management. It suggested a restructuring of collection management and the rethinking of future goals and practices. Gradually, the process became more focused and organized. Behavioral enrichment, training, animal behavior issues, and exhibit architecture were embraced as essential components for providing quality of life. Staff from all levels worked side-by-side on assignments. Our way of thinking and working was changing.

  20. Regional Land Use Mapping: the Phoenix Pilot Project

    NASA Technical Reports Server (NTRS)

    Anderson, J. R.; Place, J. L.

    1971-01-01

    The Phoenix Pilot Program has been designed to make effective use of past experience in making land use maps and collecting land use information. Conclusions reached from the project are: (1) Land use maps and accompanying statistical information of reasonable accuracy and quality can be compiled at a scale of 1:250,000 from orbital imagery. (2) Orbital imagery used in conjunction with other sources of information when available can significantly enhance the collection and analysis of land use information. (3) Orbital imagery combined with modern computer technology will help resolve the problem of obtaining land use data quickly and on a regular basis, which will greatly enhance the usefulness of such data in regional planning, land management, and other applied programs. (4) Agreement on a framework or scheme of land use classification for use with orbital imagery will be necessary for effective use of land use data.

  1. Phoenix Mars Scout Parachute Flight Behavior and Observations

    NASA Technical Reports Server (NTRS)

    Adams, Douglas S.; Witkowski, Allen; Kandis, Mike

    2011-01-01

    The data returned from the successful Phoenix Mars Scout mission are analyzed in order to determine characteristics and behaviors of the supersonic parachute that was used to slow the entry body during its descent to the surface. At least one significant drag reduction event was observed when the vehicle was traveling at Mach 1.6; this is consistent with previously reported terrestrial high altitude testing and is likely associated with an area oscillation of the parachute. The parachute is shown to possess some lateral instability relative to the anti-velocity vector that is also at a level that is consistent with the same historic data. Ramifications of the lateral instability and, in particular, the unsteadiness in the parachute drag are discussed as energizing elements of the entry body wrist mode. The apparent coefficient of drag for the parachute is calculated and shown to have relatively small variations on an average basis over the supersonic portion of flight.

  2. Phoenix Mars Scout Parachute Flight Behavior and Observations

    NASA Technical Reports Server (NTRS)

    Adams, Douglas S.; Witkowski, Allen; Kandis, Mike

    2011-01-01

    The data returned from the successful Phoenix Mars Scout mission are analyzed in order to determine characteristics and behaviors of the supersonic parachute that was used to slow the entry body during its descent to the surface. At least one significant drag reduction event was observed when the vehicle was traveling at Mach 1.6; this is consistent with previously reported terrestrial high altitude testing and is likely associated with an area oscillation of the parachute. The parachute is shown to possess some lateral instability relative to the anti-velocity vector that is also at a level that is consistent with the same historic data. Ramifications of the lateral instability and, in particular, the unsteadiness in the parachute drag are discussed as energizing elements of the entry body wrist mode. The apparent coefficient of drag for the parachute is calculated and shown to have relatively small variations on an average basis over the supersonic portion of flight.

  3. Developing Carbon Budgets for Cities: Phoenix as a Case Study

    NASA Astrophysics Data System (ADS)

    McHale, M. R.; Baker, L. A.; Koerner, B. A.; Grimm, N. B.

    2008-12-01

    Studies have shown that cities can alter regional carbon dynamics through changing ecosystem productivity, overall carbon cycling rate, and total carbon storage in vegetation and soils. Furthermore, people in urban regions import a large amount of carbon in food and fuel, as well as release an exceptional amount of CO2 into the atmosphere. Numerous studies have attempted to quantify some sources and sinks of carbon in urban areas, although a complete carbon budget for a city that accounts for total inputs, outputs, and storage within the ecosystem has yet to be fully accomplished. One challenge is associated with attaining the data necessary to accurately account for all carbon dynamics in these heterogeneous and complex ecosystems. Our goal was to estimate a budget for the Phoenix metropolitan area while developing methodology to calculate carbon dynamics in urban systems that can be applied to cities across the US. Only with comparable carbon budgets for multiple cities will we finally begin to understand the influence of urbanization on carbon dynamics. Our analysis shows when calculating certain variables like transportation emissions, results can vary radically (up to 250%) depending on the data source and methodology implemented (i.e. bottom-up vs. top-down). A common assumption is that productivity and carbon storage will increase with urbanization in arid systems due to water and nutrient inputs, as well as changes in vegetation structure; however, our results indicated that this may not actually be the case in Phoenix where a large number of residents design landscapes to conserve water. Even if all urban expansion was dedicated to landscapes designed for carbon sequestration and storage, vegetation and soils will unlikely have a large effect on the C budget without significant changes in transportation and lifestyle choices.

  4. Ground truth report 1975 Phoenix microwave experiment. [Joint Soil Moisture Experiment

    NASA Technical Reports Server (NTRS)

    Blanchard, B. J.

    1975-01-01

    Direct measurements of soil moisture obtained in conjunction with aircraft data flights near Phoenix, Arizona in March, 1975 are summarized. The data were collected for the Joint Soil Moisture Experiment.

  5. Phoenix's view of Mars as of the end of Sol 2

    NASA Technical Reports Server (NTRS)

    2008-01-01

    This image shows a polar projection mosaic of all data received as of the end of sol 2 from the right eye of the Surface Stereo Imager (SSI) instrument on board the Phoenix lander.

    The Phoenix Mission is led by the University of Arizona, Tucson, on behalf of NASA. Project management of the mission is by NASA's Jet Propulsion Laboratory, Pasadena, Calif. Spacecraft development is by Lockheed Martin Space Systems, Denver.

  6. Relationship between particulate matter and childhood asthma - basis of a future warning system for Central Phoenix

    NASA Astrophysics Data System (ADS)

    Dimitrova, R.; Lurponglukana, N.; Fernando, H. J. S.; Runger, G. C.; Hyde, P.; Hedquist, B. C.; Anderson, J.; Bannister, W.; Johnson, W.

    2011-10-01

    Statistically significant correlations between increase of asthma attacks in children and elevated concentrations of particulate matter of diameter 10 microns and less (PM10) were determined for metropolitan Phoenix, Arizona. Interpolated concentrations from a five-site network provided spatial distribution of PM10 that was mapped onto census tracts with population health records. The case-crossover statistical method was applied to determine the relationship between PM10 concentration and asthma attacks. For children ages 5-17, a significant relationship was discovered between the two, while children ages 0-4 exhibited virtually no relationship. The risk of adverse health effects was expressed as a function of the change from the 25th to 75th percentiles of mean level PM10 (36 μg m-3). This increase in concentration was associated with a 12.6% (95% CI: 5.8%, 19.4%) increase in the log odds of asthma attacks among children ages 5-17. Neither gender nor other demographic variables were significant. The results are being used to develop an asthma early warning system for the study area.

  7. Relationship between particulate matter and childhood asthma - basis of a future warning system for central Phoenix

    NASA Astrophysics Data System (ADS)

    Dimitrova, R.; Lurponglukana, N.; Fernando, H. J. S.; Runger, G. C.; Hyde, P.; Hedquist, B. C.; Anderson, J.; Bannister, W.; Johnson, W.

    2012-03-01

    Statistically significant correlations between increase of asthma attacks in children and elevated concentrations of particulate matter of diameter 10 microns and less (PM10) were determined for metropolitan Phoenix, Arizona. Interpolated concentrations from a five-site network provided spatial distribution of PM10 that was mapped onto census tracts with population health records. The case-crossover statistical method was applied to determine the relationship between PM10 concentration and asthma attacks. For children ages 5-17, a significant relationship was discovered between the two, while children ages 0-4 exhibited virtually no relationship. The risk of adverse health effects was expressed as a function of the change from the 25th to 75th percentiles of mean level PM10 (36 μg m-3). This increase in concentration was associated with a 12.6% (95% CI: 5.8%, 19.4%) increase in the log odds of asthma attacks among children ages 5-17. Neither gender nor other demographic variables were significant. The results are being used to develop an asthma early warning system for the study area.

  8. Solar energy system performance evaluation - final report for Honeywell OTS 45, Salt River Project, Phoenix, Arizona

    SciTech Connect

    Mathur, A K

    1983-09-01

    This report describes the operation and technical performance of the Solar Operational Test Site (OTS 45) at Salt River Project in Phoenix, Arizona, based on the analysis of data collected between April 1981 and March 31, 1982. The following topics are discussed: system description, performance assessment, operating energy, energy savings, system maintenance, and conclusions. The solar energy system at OTS 45 is a hydronic heating and cooling system consisting of 8208 square feet of liquid-cooled flat-plate collectors; a 2500-gallon thermal storage tank; two 25-ton capacity organic Rankine-cycle-engine-assisted water chillers; a forced-draft cooling tower; and associated piping, pumps, valves, controls and heat rejection equipment. The solar system has eight basic modes of operation and several combination modes. The system operation is controlled automatically by a Honeywell-designed microprocessor-based control system, which also provides diagnostics. Based on the instrumented test data monitored and collected during the 8 months of the Operational Test Period, the solar system collected 1143 MMBtu of thermal energy of the total incident solar energy of 3440 MMBtu and provided 241 MMBtu for cooling and 64 MMBtu for heating. The projected net annual electrical energy savings due to the solar system was approximately 40,000 kWh(e).

  9. Phoenix Indian School. Oversight Hearings on Phoenix Indian School before the Committee on Interior and Insular Affairs. House of Representatives, One Hundredth Congress, First Session (Phoenix, AZ, February 13, 1987; Washington, DC, July 30, 1987).

    ERIC Educational Resources Information Center

    Congress of the U.S., Washington, DC. House Committee on Interior and Insular Affairs.

    Since 1891, Phoenix Indian High School has served as a boarding school for Indian students. In February 1987, the Bureau of Indian Affairs (BIA) recommended that the school be closed, and that students be transferred to Sherman Indian School in Riverside, California. Congressional hearings in February and July 1987 received testimony on this…

  10. Radial Velocity of the Phoenix Dwarf Galaxy: Linking Stars and H I Gas

    NASA Astrophysics Data System (ADS)

    Gallart, C.; Martínez-Delgado, D.; Gómez-Flechoso, M. A.; Mateo, M.

    2001-05-01

    We present the first radial velocity measurement of the stellar component of the Local Group dwarf galaxy Phoenix, using the FORS1 instrument at the VLT's Unit Telescope 1 (Antu). From the spectra of 31 red giant branch stars, we derive a heliocentric optical radial velocity for Phoenix of Vsolar=-52+/-6 km s-1. On the basis of this velocity, and taking into account the results of a series of semianalytical and numerical simulations, we discuss the possible association of the H I clouds observed in the Phoenix vicinity. We conclude that the characteristics of the H I cloud with heliocentric velocity -23 km s-1 are consistent with this gas having been associated with Phoenix in the past and being lost by the galaxy after the last event of star formation in the galaxy, about 100 Myr ago. Two possible scenarios are discussed: the ejection of the gas by the energy released by the supernovae (SNe) produced in that last event of star formation and a ram pressure stripping scenario. We derive that the kinetic energy necessary to eject the gas is ESNe~2×1051 ergs and that the number of SNe necessary to transfer this amount of kinetic energy to the gas cloud is ~20. This is consistent with the number of SNe expected for the last event of star formation in Phoenix, according to the star formation history derived by Martínez-Delgado, Gallart, & Aparicio. The drawback of this scenario is the regular appearance of the H I cloud and its anisotropic distribution with respect to the stellar component. Another possibility is that the H I gas was stripped as a consequence of ram pressure by the intergalactic medium. In our simulations, the structure of the gas remains quite smooth as it is stripped from Phoenix, keeping a distribution similar to that of the observed H I cloud. Both in the SNe ejection case and in the ram pressure sweeping scenario, the distances and relative velocities imply that the H I cloud is not gravitationally bound to Phoenix, since this would require a

  11. The Domestication Syndrome in Phoenix dactylifera Seeds: Toward the Identification of Wild Date Palm Populations

    PubMed Central

    Gros-Balthazard, Muriel; Newton, Claire; Ivorra, Sarah; Pierre, Marie-Hélène; Terral, Jean-Frédéric

    2016-01-01

    Investigating crop origins is a priority to understand the evolution of plants under domestication, develop strategies for conservation and valorization of agrobiodiversity and acquire fundamental knowledge for cultivar improvement. The date palm (Phoenix dactylifera L.) belongs to the genus Phoenix, which comprises 14 species morphologically very close, sometimes hardly distinguishable. It has been cultivated for millennia in the Middle East and in North Africa and constitutes the keystone of oasis agriculture. Yet, its origins remain poorly understood as no wild populations are identified. Uncultivated populations have been described but they might represent feral, i.e. formerly cultivated, abandoned forms rather than truly wild populations. In this context, this study based on morphometrics applied to 1625 Phoenix seeds aims to (1) differentiate Phoenix species and (2) depict the domestication syndrome observed in cultivated date palm seeds using other Phoenix species as a “wild” reference. This will help discriminate truly wild from feral forms, thus providing new insights into the evolutionary history of this species. Seed size was evaluated using four parameters: length, width, thickness and dorsal view surface. Seed shape was quantified using outline analyses based on the Elliptic Fourier Transform method. The size and shape of seeds allowed an accurate differentiation of Phoenix species. The cultivated date palm shows distinctive size and shape features, compared to other Phoenix species: seeds are longer and elongated. This morphological shift may be interpreted as a domestication syndrome, resulting from the long-term history of cultivation, selection and human-mediated dispersion. Based on seed attributes, some uncultivated date palms from Oman may be identified as wild. This opens new prospects regarding the possible existence and characterization of relict wild populations and consequently for the understanding of the date palm origins. Finally, we

  12. Analysis of the Comparative Workflow and Performance Characteristics of the VITEK 2 and Phoenix Systems

    PubMed Central

    Eigner, U.; Schmid, A.; Wild, U.; Bertsch, D.; Fahr, A.-M.

    2005-01-01

    The VITEK 2 (bioMérieux, Marcy L′Ètoile, France) and the Phoenix systems (BD Diagnostic Systems, Sparks, Md.) are automated instruments for rapid organism identification and susceptibility testing. We evaluated the workflow, the time to result, and the performance of identification and susceptibility testing of both instruments. A total of 307 fresh clinical isolates were tested: 141 Enterobacteriaceae, 22 nonfermenters, 93 Staphylococcus spp., and 51 Enterococcus spp. Manipulation time was measured in batches, each with seven isolates, for a total of 39 batches. The mean (± standard deviation [SD]) manipulation time per batch was 20.9 ± 1.8 min for Phoenix and 10.6 ± 1.0 min for VITEK 2 (P < 0.001). Mean (±SD) time to result for all bacterial groups was 727 ± 162 min for Phoenix and 506 ± 120 min for VITEK 2 (P < 0.001). Concerning identification, Phoenix and VITEK 2 yielded the same results for nonfermenters (100%), staphylococci (97%), and enterococci (100%). For 140 Enterobacteriaceae strains evaluated, 135 (96%) were correctly identified by Phoenix and 137 (98%) by VITEK 2 (P = 0.72). The overall category agreement for all isolates was 97.0% for both instruments. The minor error rate, major error rate, and very major error rate for all bacterial isolates tested were 3.0, 0.3, and 0.6 and 2.8, 0.2, and 1.7 for Phoenix and VITEK 2, respectively (P values of 0.76, 0.75, and 0.09). The VITEK 2 system required less manual manipulation time and less time than the Phoenix system to yield results. PMID:16081919

  13. The Domestication Syndrome in Phoenix dactylifera Seeds: Toward the Identification of Wild Date Palm Populations.

    PubMed

    Gros-Balthazard, Muriel; Newton, Claire; Ivorra, Sarah; Pierre, Marie-Hélène; Pintaud, Jean-Christophe; Terral, Jean-Frédéric

    2016-01-01

    Investigating crop origins is a priority to understand the evolution of plants under domestication, develop strategies for conservation and valorization of agrobiodiversity and acquire fundamental knowledge for cultivar improvement. The date palm (Phoenix dactylifera L.) belongs to the genus Phoenix, which comprises 14 species morphologically very close, sometimes hardly distinguishable. It has been cultivated for millennia in the Middle East and in North Africa and constitutes the keystone of oasis agriculture. Yet, its origins remain poorly understood as no wild populations are identified. Uncultivated populations have been described but they might represent feral, i.e. formerly cultivated, abandoned forms rather than truly wild populations. In this context, this study based on morphometrics applied to 1625 Phoenix seeds aims to (1) differentiate Phoenix species and (2) depict the domestication syndrome observed in cultivated date palm seeds using other Phoenix species as a "wild" reference. This will help discriminate truly wild from feral forms, thus providing new insights into the evolutionary history of this species. Seed size was evaluated using four parameters: length, width, thickness and dorsal view surface. Seed shape was quantified using outline analyses based on the Elliptic Fourier Transform method. The size and shape of seeds allowed an accurate differentiation of Phoenix species. The cultivated date palm shows distinctive size and shape features, compared to other Phoenix species: seeds are longer and elongated. This morphological shift may be interpreted as a domestication syndrome, resulting from the long-term history of cultivation, selection and human-mediated dispersion. Based on seed attributes, some uncultivated date palms from Oman may be identified as wild. This opens new prospects regarding the possible existence and characterization of relict wild populations and consequently for the understanding of the date palm origins. Finally, we

  14. Navigation Challenges of the Mars Phoenix Lander Mission

    NASA Technical Reports Server (NTRS)

    Portock, Brian M.; Kruizinga, Gerhard; Bonfiglio, Eugene; Raofi, Behzad; Ryne, Mark

    2008-01-01

    The Mars Phoenix Lander mission was launched on August 4th, 2007. To land safely at the desired landing location on the Mars surface, the spacecraft trajectory had to be controlled to a set of stringent atmospheric entry and landing conditions. The landing location needed to be controlled to an elliptical area with dimensions of 100km by 20km. The two corresponding critical components of the atmospheric entry conditions are the entry flight path angle (target: -13.0 deg +/-0.21 deg) and the entry time (within +/-30 seconds). The purpose of this paper is to describe the navigation strategies used to overcome the challenges posed during spacecraft operations, which included an attitude control thruster calibration campaign, a trajectory control strategy, and a trajectory reconstruction strategy. Overcoming the navigation challenges resulted in final Mars atmospheric entry conditions just 0.007 deg off in entry flight path angle and 14.9 sec early in entry time. These entry dispersions in addition to the entry, descent, and landing trajectory dispersion through the atmosphere, lead to a final landing location just 7 km away from the desired landing target.

  15. Phoenix Mars Mission--the thermal evolved gas analyzer.

    PubMed

    Hoffman, John H; Chaney, Roy C; Hammack, Hilton

    2008-10-01

    The Phoenix spacecraft that was launched to Mars in August 2007 landed safely on the Martian northern arctic region on May 25, 2008. It carried six experiments to study the history of water on the planet and search for organic molecules in the icy subsurface Martian soil. The spacecraft is a lander with an arm and scoop designed to dig a trench though the top soil to reach an expected ice layer near the surface. One of the instruments on board is the thermal evolved gas analyzer (TEGA), which consists of two components, a set of eight very small ovens that will heat samples of the ice soil mixtures from the trench to release imbedded gases and mineral decomposition products, and a mass spectrometer that serves as the analysis tool for the evolved gases, and also for measurements of the composition and isotopic ratios of the gases that comprise the atmosphere of Mars. The mass spectrometer is a miniature magnetic sector instrument controlled by microprocessor-driven power supplies. One feature is the gas enrichment cell that will increase the partial pressures of the noble gases in an atmosphere sample by removing all the active gases, carbon dioxide, and nitrogen, to improve the accuracy of their isotopic ratio measurements.

  16. Decimetric solar type U bursts - VLA and Phoenix observations

    NASA Technical Reports Server (NTRS)

    Aschwanden, Markus J.; Bastian, T. S.; Benz, A. O.; Brosius, J. W.

    1992-01-01

    Observations of type U bursts, simultaneously detected by the VLA at 1.446 GHz and by the broadband spectrometer Phoenix in the 1.1-1.7 GHz frequency band on August 13, 1989 are reported. Extrapolations of the coronal magnetic field, assuming a potential configuration, indicate that the VLA 20 cm source demarcates an isodensity level. The source covers a wide angle of diverging magnetic field lines whose footpoints originate close to a magnetic intrusion of negative polarity into the main sunspot group of the active region with dominant positive polarity. The centroid of the 20-cm U-burst emission, which corresponds to the turnover frequency of the type U bursts and remains stationary during all U bursts, coincides with the apex of extrapolated potential field lines at a height of about 130,000 km. It is demonstrated that the combination of radio imaging and broadband dynamic spectra, combined with the magnetic field reconstruction from magnetograms, can constrain all physical parameters of a magnetic loop system.

  17. Land use mapping and modelling for the Phoenix Quadrangle

    NASA Technical Reports Server (NTRS)

    Place, J. L. (Principal Investigator)

    1974-01-01

    The author has identified the following significant results. Changes in the land use in the Phoenix (1:250,000 scale) Quadrangle in Arizona have been mapped using only the images from ERTS-1, tending to verify the utility of a land use classification system proposed for use with ERTS images. Seasonal changes were studied on successive ERTS-1 images, particularly large scale color composite transparencies for August, October, February, and May, and this seasonal variation aided delineation of land use boundaries. Types of equipment used to aid interpretation included color additive viewer, a twenty-power magnifier, a density slicer, and a diazo copy machine. A Zoom Transfer Scope was used for scale and photogrammetric adjustments. Types of changes detected have been: (1) cropland or rangeland developed as new residential areas; (2) rangeland converted to new cropland or to new reservoirs; and (3) possibly new activity by the mining industries. A map of land use previously compiled from air photos was updated in this manner. ERTS-1 images complemented air photos: the photos gave detail on a one-shot basis; the ERTS-1 images provided currency and revealed seasonal variation in vegetation which aided interpretation of land use.

  18. Navigation Challenges of the Mars Phoenix Lander Mission

    NASA Technical Reports Server (NTRS)

    Portock, Brian M.; Kruizinga, Gerhard; Bonfiglio, Eugene; Raofi, Behzad; Ryne, Mark

    2008-01-01

    The Mars Phoenix Lander mission was launched on August 4th, 2007. To land safely at the desired landing location on the Mars surface, the spacecraft trajectory had to be controlled to a set of stringent atmospheric entry and landing conditions. The landing location needed to be controlled to an elliptical area with dimensions of 100km by 20km. The two corresponding critical components of the atmospheric entry conditions are the entry flight path angle (target: -13.0 deg +/-0.21 deg) and the entry time (within +/-30 seconds). The purpose of this paper is to describe the navigation strategies used to overcome the challenges posed during spacecraft operations, which included an attitude control thruster calibration campaign, a trajectory control strategy, and a trajectory reconstruction strategy. Overcoming the navigation challenges resulted in final Mars atmospheric entry conditions just 0.007 deg off in entry flight path angle and 14.9 sec early in entry time. These entry dispersions in addition to the entry, descent, and landing trajectory dispersion through the atmosphere, lead to a final landing location just 7 km away from the desired landing target.

  19. Land use mapping and modelling for the Phoenix Quadrangle

    NASA Technical Reports Server (NTRS)

    Place, J. L. (Principal Investigator)

    1973-01-01

    The author has identified the following significant results. In comparing the land use changes from the overlay as detected from ERTS-1 and the high altitude change overlay, total areas of change were of the same magnitude. The greatest variations were a result of differences in dates and areas of coverage between ERTS-1 images and aerial photographs. Separation of citrus from other agricultural land has been moderately successful in the ERTS-1 1:100,000 scale Level 2 land use mapping around Phoenix, although accuracy estimates are not yet available. No feeding operations have been detected from ERTS-1 so far. Preliminary indications are that commercial and services, industrial, and institutional land are not separable from each other using present image interpretation techniques. Urban open areas such as parks and golf courses are readily detectable, particularly when local maps are consulted even though out-of-date. Strip and clustered settlements may be detected depending upon their size and contrast with the surrounding area on the ERTS-1 image.

  20. Thermal and Electrical Conductivity Probe for Phoenix Mars Lander

    NASA Technical Reports Server (NTRS)

    2007-01-01

    NASA's Phoenix Mars Lander will assess how heat and electricity move through Martian soil from one spike or needle to another of a four-spike electronic fork that will be pushed into the soil at different stages of digging by the lander's Robotic Arm.

    The four-spike tool, called the thermal and electrical conductivity probe, is in the middle-right of this photo, mounted near the end of the arm near the lander's scoop (upper left).

    In one type of experiment with this tool, a pulse of heat will be put into one spike, and the rate at which the temperature rises on the nearby spike will be recorded, along with the rate at which the heated spike cools. A little bit of ice can make a big difference in how well soil conducts heat. Similarly, soil's electrical conductivity -- also tested with this tool -- is a sensitive

    indicator of moisture in the soil. This device adapts technology used in soil-moisture gauges for irrigation-control systems. The conductivity probe has an additional role besides soil analysis. It will serve as a hunidity sensor when held in the air.