Image quality enhancement method for on-orbit remote sensing cameras using invariable modulation transfer function.

PubMed

Li, Jin; Liu, Zilong

2017-07-24

Remote sensing cameras in the visible/near infrared range are essential tools in Earth-observation, deep-space exploration, and celestial navigation. Their imaging performance, i.e. image quality here, directly determines the target-observation performance of a spacecraft, and even the successful completion of a space mission. Unfortunately, the camera itself, such as a optical system, a image sensor, and a electronic system, limits the on-orbit imaging performance. Here, we demonstrate an on-orbit high-resolution imaging method based on the invariable modulation transfer function (IMTF) of cameras. The IMTF, which is stable and invariable to the changing of ground targets, atmosphere, and environment on orbit or on the ground, depending on the camera itself, is extracted using a pixel optical focal-plane (PFP). The PFP produces multiple spatial frequency targets, which are used to calculate the IMTF at different frequencies. The resulting IMTF in combination with a constrained least-squares filter compensates for the IMTF, which represents the removal of the imaging effects limited by the camera itself. This method is experimentally confirmed. Experiments on an on-orbit panchromatic camera indicate that the proposed method increases 6.5 times of the average gradient, 3.3 times of the edge intensity, and 1.56 times of the MTF value compared to the case when IMTF is not used. This opens a door to push the limitation of a camera itself, enabling high-resolution on-orbit optical imaging.

Processing of A New Digital Orthoimage Map of The Martian Western Hemisphere Using Data Obtained From The Mars Orbiter Camera At A Resolution of 256 Pixel/deg

NASA Astrophysics Data System (ADS)

Wählisch, M.; Niedermaier, G.; van Gasselt, S.; Scholten, F.; Wewel, F.; Roatsch, T.; Matz, K.-D.; Jaumann, R.

We present a new digital orthoimage map of Mars using data obtained from the CCD line scanner Mars Orbiter Camera (MOC) of the Mars Global Surveyor Mis- sion (MGS) [1,2]. The map covers the Mars surface from 0 to 180 West and from 60 South to 60 North with the MDIM2 resolution of 256 pixel/degree and size. Image data processing has been performed using multiple programs, developed by DLR, Technical University of Berlin [3], JPL, and the USGS. 4,339 Context and 183 Geodesy images [2] were included. After radiometric corrections, the images were Mars referenced [4], geometrically corrected [5] and orthoprojected using a global Martian Digital Terrain Model (DTM) with a resolution of 64 pixel/degree, developed at DLR and based on MGS Mars Orbiter Laser Altimeter (MOLA) data [6]. To elim- inate major differences in brightness between the individual images of the mosaics, high- and low-pass filter processing techniques were applied for each image. After filtering, the images were mosaicked without registering or using block adjustment techniques in order to improve the geometric quality. It turns out that the accuracy of the navigation data has such a good quality that the orthoimages fit very well to each other. When merging the MOC mosaic with the MOLA data using IHS- trans- formation, we recognized very good correspondence between these two datasets. We create a topographic image map of the Coprates region (MC­18) adding contour lines derived from the global DTM to the mosaic. These maps are used for geological and morphological interpretations in order to review and improve our current Viking-based knowledge about the Martian surface. References: [1] www.mssss.com, [2] Caplinger, M. and M. Malin, "The Mars Or- biter Camera Geodesy Campaign, JGR, in press, [3] Scholten, F., Vol XXXI, Part B2, Wien 1996, p.351-356, [4] naïf.jpl.nasa.gov, [5] R.L.Kirk. et al. (2001), "Geometric Calibration of the Mars Orbiter Cameras and Coalignment with Mars Orbiter Laser Altimeter", LPSC XXXII, [6] wufs.wustl.edu

The Orbiter camera payload system's large-format camera and attitude reference system

NASA Technical Reports Server (NTRS)

Schardt, B. B.; Mollberg, B. H.

1985-01-01

The Orbiter camera payload system (OCPS) is an integrated photographic system carried into earth orbit as a payload in the Space Transportation System (STS) Orbiter vehicle's cargo bay. The major component of the OCPS is a large-format camera (LFC), a precision wide-angle cartographic instrument capable of producing high-resolution stereophotography of great geometric fidelity in multiple base-to-height ratios. A secondary and supporting system to the LFC is the attitude reference system (ARS), a dual-lens stellar camera array (SCA) and camera support structure. The SCA is a 70 mm film system that is rigidly mounted to the LFC lens support structure and, through the simultaneous acquisition of two star fields with each earth viewing LFC frame, makes it possible to precisely determine the pointing of the LFC optical axis with reference to the earth nadir point. Other components complete the current OCPS configuration as a high-precision cartographic data acquisition system. The primary design objective for the OCPS was to maximize system performance characteristics while maintaining a high level of reliability compatible with rocket launch conditions and the on-orbit environment. The full OCPS configuration was launched on a highly successful maiden voyage aboard the STS Orbiter vehicle Challenger on Oct. 5, 1984, as a major payload aboard the STS-41G mission.

Lunar Reconnaissance Orbiter Camera (LROC) instrument overview

USGS Publications Warehouse

Robinson, M.S.; Brylow, S.M.; Tschimmel, M.; Humm, D.; Lawrence, S.J.; Thomas, P.C.; Denevi, B.W.; Bowman-Cisneros, E.; Zerr, J.; Ravine, M.A.; Caplinger, M.A.; Ghaemi, F.T.; Schaffner, J.A.; Malin, M.C.; Mahanti, P.; Bartels, A.; Anderson, J.; Tran, T.N.; Eliason, E.M.; McEwen, A.S.; Turtle, E.; Jolliff, B.L.; Hiesinger, H.

2010-01-01

The Lunar Reconnaissance Orbiter Camera (LROC) Wide Angle Camera (WAC) and Narrow Angle Cameras (NACs) are on the NASA Lunar Reconnaissance Orbiter (LRO). The WAC is a 7-color push-frame camera (100 and 400 m/pixel visible and UV, respectively), while the two NACs are monochrome narrow-angle linescan imagers (0.5 m/pixel). The primary mission of LRO is to obtain measurements of the Moon that will enable future lunar human exploration. The overarching goals of the LROC investigation include landing site identification and certification, mapping of permanently polar shadowed and sunlit regions, meter-scale mapping of polar regions, global multispectral imaging, a global morphology base map, characterization of regolith properties, and determination of current impact hazards.

KENNEDY SPACE CENTER, FLA. - In the Orbiter Processing Facility, Richard Parker, with NASA, watches a monitor showing images from a camera inserted beneath tiles of the orbiter Endeavour to inspect for corrosion.

NASA Image and Video Library

2003-09-04

KENNEDY SPACE CENTER, FLA. - In the Orbiter Processing Facility, Richard Parker, with NASA, watches a monitor showing images from a camera inserted beneath tiles of the orbiter Endeavour to inspect for corrosion.

Fifty Years of Mars Imaging: from Mariner 4 to HiRISE

NASA Image and Video Library

2017-11-20

This image from NASA's Mars Reconnaissance Orbiter (MRO) shows Mars' surface in detail. Mars has captured the imagination of astronomers for thousands of years, but it wasn't until the last half a century that we were able to capture images of its surface in detail. This particular site on Mars was first imaged in 1965 by the Mariner 4 spacecraft during the first successful fly-by mission to Mars. From an altitude of around 10,000 kilometers, this image (the ninth frame taken) achieved a resolution of approximately 1.25 kilometers per pixel. Since then, this location has been observed by six other visible cameras producing images with varying resolutions and sizes. This includes HiRISE (highlighted in yellow), which is the highest-resolution and has the smallest "footprint." This compilation, spanning Mariner 4 to HiRISE, shows each image at full-resolution. Beginning with Viking 1 and ending with our HiRISE image, this animation documents the historic imaging of a particular site on another world. In 1976, the Viking 1 orbiter began imaging Mars in unprecedented detail, and by 1980 had successfully mosaicked the planet at approximately 230 meters per pixel. In 1999, the Mars Orbiter Camera onboard the Mars Global Surveyor (1996) also imaged this site with its Wide Angle lens, at around 236 meters per pixel. This was followed by the Thermal Emission Imaging System on Mars Odyssey (2001), which also provided a visible camera producing the image we see here at 17 meters per pixel. Later in 2012, the High-Resolution Stereo Camera on the Mars Express orbiter (2003) captured this image of the surface at 25 meters per pixel. In 2010, the Context Camera on the Mars Reconnaissance Orbiter (2005) imaged this site at about 5 meters per pixel. Finally, in 2017, HiRISE acquired the highest resolution image of this location to date at 50 centimeters per pixel. When seen at this unprecedented scale, we can discern a crater floor strewn with small rocky deposits, boulders several meters across, and wind-blown deposits in the floors of small craters and depressions. This compilation of Mars images spanning over 50 years gives us a visual appreciation of the evolution of orbital Mars imaging over a single site. The map is projected here at a scale of 50 centimeters (19.7 inches) per pixel. [The original image scale is 52.2 centimeters (20.6 inches) per pixel (with 2 x 2 binning); objects on the order of 156 centimeters (61.4 inches) across are resolved.] North is up. https://photojournal.jpl.nasa.gov/catalog/PIA22115

Segments on Western Rim of Endeavour Crater, Mars

NASA Image and Video Library

2017-04-19

This orbital image of the western rim of Mars' Endeavour Crater covers an area about 5 miles (8 kilometers) east-west by about 9 miles (14 kilometers) north-south and indicates the names of some of the raised segments of the rim. NASA's Mars Exploration Rover Opportunity arrived at Endeavour in 2011 after exploring smaller craters to the northwest during its first six years on Mars. It initially explored the "Cape York" segment, then headed south. It reached the northern end of "Cape Tribulation" in late 2014 and the southern tip of that segment in April 2017. A key destination in the "Cape Byron" segment is "Perseverance Valley," where the rover team plans to investigate whether the valley was carved by water, wind or a debris flow initiated by water. This image is from the Context Camera on NASA's Mars Reconnaissance Orbiter. Malin Space Science Systems, San Diego, California, built and operates that camera. NASA's Jet Propulsion Laboratory, a division of Caltech in Pasadena, California, built and operates Opportunity. https://photojournal.jpl.nasa.gov/catalog/PIA21490

Candidate cave entrances on Mars

USGS Publications Warehouse

Cushing, Glen E.

2012-01-01

This paper presents newly discovered candidate cave entrances into Martian near-surface lava tubes, volcano-tectonic fracture systems, and pit craters and describes their characteristics and exploration possibilities. These candidates are all collapse features that occur either intermittently along laterally continuous trench-like depressions or in the floors of sheer-walled atypical pit craters. As viewed from orbit, locations of most candidates are visibly consistent with known terrestrial features such as tube-fed lava flows, volcano-tectonic fractures, and pit craters, each of which forms by mechanisms that can produce caves. Although we cannot determine subsurface extents of the Martian features discussed here, some may continue unimpeded for many kilometers if terrestrial examples are indeed analogous. The features presented here were identified in images acquired by the Mars Odyssey's Thermal Emission Imaging System visible-wavelength camera, and by the Mars Reconnaissance Orbiter's Context Camera. Select candidates have since been targeted by the High-Resolution Imaging Science Experiment. Martian caves are promising potential sites for future human habitation and astrobiology investigations; understanding their characteristics is critical for long-term mission planning and for developing the necessary exploration technologies.

Surface albedo observations at Gusev Crater and Meridiani Planum, Mars

USGS Publications Warehouse

Bell, J.F.; Rice, M.S.; Johnson, J. R.; Hare, T.M.

2008-01-01

During the Mars Exploration Rover mission, the Pancam instrument has periodically acquired large-scale panoramic images with its broadband (739??338 nm) filter in order to estimate the Lambert bolometric albedo of the surface along each rover's traverse. In this work we present the full suite of such estimated albedo values measured to date by the Spirit and Opportunity rovers along their traverses in Gusev Crater and Meridiani Planum, respectively. We include estimated bolometric albedo values of individual surface features (e.g., outcrops, dusty plains, aeolian bed forms, wheel tracks, light-toned soils, and crater walls) as well as overall surface averages of the 43 total panoramic albedo data sets acquired to date. We also present comparisons to estimated Lambert albedo values taken from the Mars Global Surveyor Mars Orbiter Camera (MOC) along the rovers' traverses, and to the large-scale bolometric albedos of the sites from the Viking Orbiter Infrared Thermal Mapper (IRTM) and Mars Global Surveyor/Thermal Emission Spectrometer (TES). The ranges of Pancam-derived albedos at Gusev Crater (0.14 to 0.25) and in Meridiani Planum. (0.10 to 0.18) are in good agreement with IRTM, TES, and MOC orbital measurements. These data sets will be a useful tool and benchmark for future investigations of albodo variations with time, including measurements from orbital instruments like the Context Camera and High Resolution Imaging Science Experiment on Mars Reconnaissance Orbiter. Long-term, accurate albedo measurements could also be important for future efforts in climate modeling as well as for studies of active surface processes. Copyright 2008 by the American Geophysical Union.

Surface albedo observations at Gusev Crater and Meridiani Planum, Mars

NASA Astrophysics Data System (ADS)

Bell, J. F.; Rice, M. S.; Johnson, J. R.; Hare, T. M.

2008-05-01

During the Mars Exploration Rover mission, the Pancam instrument has periodically acquired large-scale panoramic images with its broadband (739 +/- 338 nm) filter in order to estimate the Lambert bolometric albedo of the surface along each rover's traverse. In this work we present the full suite of such estimated albedo values measured to date by the Spirit and Opportunity rovers along their traverses in Gusev Crater and Meridiani Planum, respectively. We include estimated bolometric albedo values of individual surface features (e.g., outcrops, dusty plains, aeolian bed forms, wheel tracks, light-toned soils, and crater walls) as well as overall surface averages of the 43 total panoramic albedo data sets acquired to date. We also present comparisons to estimated Lambert albedo values taken from the Mars Global Surveyor Mars Orbiter Camera (MOC) along the rovers' traverses, and to the large-scale bolometric albedos of the sites from the Viking Orbiter Infrared Thermal Mapper (IRTM) and Mars Global Surveyor/Thermal Emission Spectrometer (TES). The ranges of Pancam-derived albedos at Gusev Crater (0.14 to 0.25) and in Meridiani Planum (0.10 to 0.18) are in good agreement with IRTM, TES, and MOC orbital measurements. These data sets will be a useful tool and benchmark for future investigations of albedo variations with time, including measurements from orbital instruments like the Context Camera and High Resolution Imaging Science Experiment on Mars Reconnaissance Orbiter. Long-term, accurate albedo measurements could also be important for future efforts in climate modeling as well as for studies of active surface processes.

Comparing orbiter and rover image-based mapping of an ancient sedimentary environment, Aeolis Palus, Gale crater, Mars

NASA Astrophysics Data System (ADS)

Stack, K. M.; Edwards, C. S.; Grotzinger, J. P.; Gupta, S.; Sumner, D. Y.; Calef, F. J.; Edgar, L. A.; Edgett, K. S.; Fraeman, A. A.; Jacob, S. R.; Le Deit, L.; Lewis, K. W.; Rice, M. S.; Rubin, D.; Williams, R. M. E.; Williford, K. H.

2016-12-01

This study provides the first systematic comparison of orbital facies maps with detailed ground-based geology observations from the Mars Science Laboratory (MSL) Curiosity rover to examine the validity of geologic interpretations derived from orbital image data. Orbital facies maps were constructed for the Darwin, Cooperstown, and Kimberley waypoints visited by the Curiosity rover using High Resolution Imaging Science Experiment (HiRISE) images. These maps, which represent the most detailed orbital analysis of these areas to date, were compared with rover image-based geologic maps and stratigraphic columns derived from Curiosity's Mast Camera (Mastcam) and Mars Hand Lens Imager (MAHLI). Results show that bedrock outcrops can generally be distinguished from unconsolidated surficial deposits in high-resolution orbital images and that orbital facies mapping can be used to recognize geologic contacts between well-exposed bedrock units. However, process-based interpretations derived from orbital image mapping are difficult to infer without known regional context or observable paleogeomorphic indicators, and layer-cake models of stratigraphy derived from orbital maps oversimplify depositional relationships as revealed from a rover perspective. This study also shows that fine-scale orbital image-based mapping of current and future Mars landing sites is essential for optimizing the efficiency and science return of rover surface operations.

Comparing orbiter and rover image-based mapping of an ancient sedimentary environment, Aeolis Palus, Gale crater, Mars

USGS Publications Warehouse

Stack, Kathryn M.; Edwards, Christopher; Grotzinger, J. P.; Gupta, S.; Sumner, D.; Edgar, Lauren; Fraeman, A.; Jacob, S.; LeDeit, L.; Lewis, K.W.; Rice, M.S.; Rubin, D.; Calef, F.; Edgett, K.; Williams, R.M.E.; Williford, K.H.

2016-01-01

This study provides the first systematic comparison of orbital facies maps with detailed ground-based geology observations from the Mars Science Laboratory (MSL) Curiosity rover to examine the validity of geologic interpretations derived from orbital image data. Orbital facies maps were constructed for the Darwin, Cooperstown, and Kimberley waypoints visited by the Curiosity rover using High Resolution Imaging Science Experiment (HiRISE) images. These maps, which represent the most detailed orbital analysis of these areas to date, were compared with rover image-based geologic maps and stratigraphic columns derived from Curiosity’s Mast Camera (Mastcam) and Mars Hand Lens Imager (MAHLI). Results show that bedrock outcrops can generally be distinguished from unconsolidated surficial deposits in high-resolution orbital images and that orbital facies mapping can be used to recognize geologic contacts between well-exposed bedrock units. However, process-based interpretations derived from orbital image mapping are difficult to infer without known regional context or observable paleogeomorphic indicators, and layer-cake models of stratigraphy derived from orbital maps oversimplify depositional relationships as revealed from a rover perspective. This study also shows that fine-scale orbital image-based mapping of current and future Mars landing sites is essential for optimizing the efficiency and science return of rover surface operations.

Engineering study for pallet adapting the Apollo laser altimeter and photographic camera system for the Lidar Test Experiment on orbital flight tests 2 and 4

NASA Technical Reports Server (NTRS)

Kuebert, E. J.

1977-01-01

A Laser Altimeter and Mapping Camera System was included in the Apollo Lunar Orbital Experiment Missions. The backup system, never used in the Apollo Program, is available for use in the Lidar Test Experiments on the STS Orbital Flight Tests 2 and 4. Studies were performed to assess the problem associated with installation and operation of the Mapping Camera System in the STS. They were conducted on the photographic capabilities of the Mapping Camera System, its mechanical and electrical interface with the STS, documentation, operation and survivability in the expected environments, ground support equipment, test and field support.

Camera Ready to Install on Mars Reconnaissance Orbiter

NASA Image and Video Library

2005-01-07

A telescopic camera called the High Resolution Imaging Science Experiment, or HiRISE, right was installed onto the main structure of NASA Mars Reconnaissance Orbiter left on Dec. 11, 2004 at Lockheed Martin Space Systems, Denver.

Mission Report on the Orbiter Camera Payload System (OCPS) Large Format Camera (LFC) and Attitude Reference System (ARS)

NASA Technical Reports Server (NTRS)

Mollberg, Bernard H.; Schardt, Bruton B.

1988-01-01

The Orbiter Camera Payload System (OCPS) is an integrated photographic system which is carried into earth orbit as a payload in the Space Transportation System (STS) Orbiter vehicle's cargo bay. The major component of the OCPS is a Large Format Camera (LFC), a precision wide-angle cartographic instrument that is capable of producing high resolution stereo photography of great geometric fidelity in multiple base-to-height (B/H) ratios. A secondary, supporting system to the LFC is the Attitude Reference System (ARS), which is a dual lens Stellar Camera Array (SCA) and camera support structure. The SCA is a 70-mm film system which is rigidly mounted to the LFC lens support structure and which, through the simultaneous acquisition of two star fields with each earth-viewing LFC frame, makes it possible to determine precisely the pointing of the LFC optical axis with reference to the earth nadir point. Other components complete the current OCPS configuration as a high precision cartographic data acquisition system. The primary design objective for the OCPS was to maximize system performance characteristics while maintaining a high level of reliability compatible with Shuttle launch conditions and the on-orbit environment. The full-up OCPS configuration was launched on a highly successful maiden voyage aboard the STS Orbiter vehicle Challenger on October 5, 1984, as a major payload aboard mission STS 41-G. This report documents the system design, the ground testing, the flight configuration, and an analysis of the results obtained during the Challenger mission STS 41-G.

Surveying the Newly Digitized Apollo Metric Images for Highland Fault Scarps on the Moon

NASA Astrophysics Data System (ADS)

Williams, N. R.; Pritchard, M. E.; Bell, J. F.; Watters, T. R.; Robinson, M. S.; Lawrence, S.

2009-12-01

The presence and distribution of thrust faults on the Moon have major implications for lunar formation and thermal evolution. For example, thermal history models for the Moon imply that most of the lunar interior was initially hot. As the Moon cooled over time, some models predict global-scale thrust faults should form as stress builds from global thermal contraction. Large-scale thrust fault scarps with lengths of hundreds of kilometers and maximum relief of up to a kilometer or more, like those on Mercury, are not found on the Moon; however, relatively small-scale linear and curvilinear lobate scarps with maximum lengths typically around 10 km have been observed in the highlands [Binder and Gunga, Icarus, v63, 1985]. These small-scale scarps are interpreted to be thrust faults formed by contractional stresses with relatively small maximum (tens of meters) displacements on the faults. These narrow, low relief landforms could only be identified in the highest resolution Lunar Orbiter and Apollo Panoramic Camera images and under the most favorable lighting conditions. To date, the global distribution and other properties of lunar lobate faults are not well understood. The recent micron-resolution scanning and digitization of the Apollo Mapping Camera (Metric) photographic negatives [Lawrence et al., NLSI Conf. #1415, 2008; http://wms.lroc.asu.edu/apollo] provides a new dataset to search for potential scarps. We examined more than 100 digitized Metric Camera image scans, and from these identified 81 images with favorable lighting (incidence angles between about 55 and 80 deg.) to manually search for features that could be potential tectonic scarps. Previous surveys based on Panoramic Camera and Lunar Orbiter images found fewer than 100 lobate scarps in the highlands; in our Apollo Metric Camera image survey, we have found additional regions with one or more previously unidentified linear and curvilinear features on the lunar surface that may represent lobate thrust fault scarps. In this presentation we review the geologic characteristics and context of these newly-identified, potentially tectonic landforms. The lengths and relief of some of these linear and curvilinear features are consistent with previously identified lobate scarps. Most of these features are in the highlands, though a few occur along the edges of mare and/or crater ejecta deposits. In many cases the resolution of the Metric Camera frames (~10 m/pix) is not adequate to unequivocally determine the origin of these features. Thus, to assess if the newly identified features have tectonic or other origins, we are examining them in higher-resolution Panoramic Camera (currently being scanned) and Lunar Reconnaissance Orbiter Camera Narrow Angle Camera images [Watters et al., this meeting, 2009].

Feasibility study for the application of the large format camera as a payload for the Orbiter program

NASA Technical Reports Server (NTRS)

1978-01-01

The large format camera (LFC) designed as a 30 cm focal length cartographic camera system that employs forward motion compensation in order to achieve the full image resolution provided by its 80 degree field angle lens is described. The feasibility of application of the current LFC design to deployment in the orbiter program as the Orbiter Camera Payload System was assessed and the changes that are necessary to meet such a requirement are discussed. Current design and any proposed design changes were evaluated relative to possible future deployment of the LFC on a free flyer vehicle or in a WB-57F. Preliminary mission interface requirements for the LFC are given.

Context of Carbonate Rocks in Heavily Eroded Martian Terrain

NASA Technical Reports Server (NTRS)

2008-01-01

The color coding on this composite image of an area about 20 kilometers (12 miles) wide on Mars is based on infrared spectral information interpreted as evidence of various minerals present. Carbonate, which is indicative of a wet and non-acidic history, occurs in very small patches of exposed rock appearing green in this color representation, such as near the lower right corner.

The scene is heavily eroded terrain to the west of a small canyon in the Nili Fossae region of Mars. It was one of the first areas where researchers on the Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) science team detected carbonate in Mars rocks. The spectral information comes from infrared imaging by CRISM, one of six science instruments on NASA's Mars Reconnaissance Orbiter. That coloring is overlaid on a grayscale image from the same orbiter's Context Camera.

The uppermost capping rock unit (purple) is underlain successively by banded olivine-bearing rocks (yellow) and rocks bearing iron-magnesium smectite clay (blue). Where the olivine is a greenish hue, it has been partially altered by interaction with water. The carbonate and olivine occupy the same level in the stratigraphy, and it is thought that the carbonate formed by aqueous alteration of olivine. The channel running from upper left to lower right through the image and eroding into the layers of bedrock testifies to the past presence of water in this region. That some of the channels are closely associated with carbonate (lower right) indicates that waters interacting with the carbonate were neutral to alkaline because acidic waters would have dissolved the carbonate.

Information for the color coding came from CRISM images catalogued as FRT0000B438, FRT0000A4FC, and FRT00003E12. This composite was made using 2.38-micrometer-wavelenghth data as red, 1.80 micrometer as green and 1.15 micrometer as blue.

The base black-and-white image, acquired at a resolution of 5 meters (16 feet) per pixel, is catalogued as CTX P03_002176_2024_XI_22N283W_070113 by the Context Camera science team.

NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology, Pasadena, manages the Mars Reconnaissance Orbiter for the NASA Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The Johns Hopkins University Applied Physics Laboratory led the effort to build the CRISM instrument and operates CRISM in coordination with an international team of researchers from universities, government and the private sector. Malin Space Science Systems, San Diego, provided and operates the Context Camera.

Mounted Video Camera Captures Launch of STS-112, Shuttle Orbiter Atlantis

NASA Technical Reports Server (NTRS)

2002-01-01

A color video camera mounted to the top of the External Tank (ET) provided this spectacular never-before-seen view of the STS-112 mission as the Space Shuttle Orbiter Atlantis lifted off in the afternoon of October 7, 2002, The camera provided views as the the orbiter began its ascent until it reached near-orbital speed, about 56 miles above the Earth, including a view of the front and belly of the orbiter, a portion of the Solid Rocket Booster, and ET. The video was downlinked during flight to several NASA data-receiving sites, offering the STS-112 team an opportunity to monitor the shuttle's performance from a new angle. Atlantis carried the S1 Integrated Truss Structure and the Crew and Equipment Translation Aid (CETA) Cart. The CETA is the first of two human-powered carts that will ride along the International Space Station's railway providing a mobile work platform for future extravehicular activities by astronauts. Landing on October 18, 2002, the Orbiter Atlantis ended its 11-day mission.

Mounted Video Camera Captures Launch of STS-112, Shuttle Orbiter Atlantis

NASA Technical Reports Server (NTRS)

2002-01-01

A color video camera mounted to the top of the External Tank (ET) provided this spectacular never-before-seen view of the STS-112 mission as the Space Shuttle Orbiter Atlantis lifted off in the afternoon of October 7, 2002. The camera provided views as the orbiter began its ascent until it reached near-orbital speed, about 56 miles above the Earth, including a view of the front and belly of the orbiter, a portion of the Solid Rocket Booster, and ET. The video was downlinked during flight to several NASA data-receiving sites, offering the STS-112 team an opportunity to monitor the shuttle's performance from a new angle. Atlantis carried the S1 Integrated Truss Structure and the Crew and Equipment Translation Aid (CETA) Cart. The CETA is the first of two human-powered carts that will ride along the International Space Station's railway providing a mobile work platform for future extravehicular activities by astronauts. Landing on October 18, 2002, the Orbiter Atlantis ended its 11-day mission.

The Fifteen-Year Attitude History of the Wide Field Planetary Camera 2 Radiator and Collection Efficiencies for Micrometeoroids and Orbital Debris

NASA Technical Reports Server (NTRS)

Anz-Meador, Phillip D.; Liou, Jer-Chyi; Cooke, William J.; Koehler, H.

2010-01-01

An examination of the Hubble Space Telescope (HST) Wide Field Planetary Camera 2 (WFPC-2) radiator assembly was conducted at NASA Goddard Space Flight Center (GSFC) during the summer of 2009. Immediately apparent was a distinct biasing of the largest 45 impact features towards one side of the radiator, in contrast to an approximately uniform distribution of smaller impacts. Such a distribution may be a consequence of the HST s attitude history and pointing requirements for the cold radiator, or of environmental effects, such as an anisotropic distribution of the responsible population in that size regime. Understanding the size-dependent spatial distribution of impact features is essential to the general analysis of these features. We have obtained from GSFC a 15 minute temporal resolution record of the state vector (Earth Centered Inertial position and velocity) and HST attitude, consisting of the orientation of the velocity and HST-sun vectors in HST body coordinates. This paper reviews the actual state vector and attitude history of the radiator in the context of the randomly tumbling plate assumption and assesses the statistical likelihood (or collection efficiency) of the radiator for the micrometeoroid and orbital debris environments. The NASA Marshall Space Flight Center s Meteoroid Environment Model is used to assess the micrometeoroid component. The NASA Orbital Debris Engineering Model (ORDEM) is used to model the orbital debris component. Modeling results are compared with observations of the impact feature spatial distribution, and the relative contribution of each environmental component are examined in detail.

Report Of The HST Strategy Panel: A Strategy For Recovery

DTIC Science & Technology

1991-01-01

orbit change out: the Wide Field/Planetary Camera II (WFPC II), the Near-Infrared Camera and Multi- Object Spectrometer (NICMOS) and the Space ...are the Space Telescope Imaging Spectrograph (STB), the Near-Infrared Camera and Multi- Object Spectrom- eter (NICMOS), and the second Wide Field and...expected to fail to lock due to duplicity was 20%; on- orbit data indicates that 10% may be a better estimate, but the guide stars were preselected

Sinus Meridiani: uncontrolled Mars Global Surveyor (MGS) Mars Orbital Camera (MOC): digital context photomosaic (250 megapixel resolution)

USGS Publications Warehouse

Noreen, Eric

2000-01-01

These images were processed from a raw format using Integrated Software for Images and Spectrometers (ISIS) to perform radiometric corrections and projection. All the images were projected in sinusoidal using a center longitude of 0 degrees. There are two versions of the mosaic, one unfiltered (sinusmos.tif), and one produced with all images processed through a box filter with an averaged pixel tone of 7.5 (sinusmosflt.tif). Both mosaics are ArcView-ArcInfo(2) ready in TIF format with associated world files (*.tfw).

Central Valles Marineris: uncontrolled Mars Global Surveyor (MGS) Mars Orbital Camera (MOC) digital context photomosaic (250 megapixel resolution)

USGS Publications Warehouse

Noreen, Eric

2000-01-01

These images were processed from a raw format using Integrated Software for Images and Spectrometers (ISIS) to perform radiometric corrections and projection. All the images were projected in sinusoidal using a center longitude of 70 degrees. There are two versions of the mosaic, one unfiltered (vallesmos.tif), and one produced with all images processed through a box filter with an averaged pixel tone of 7.699 (vallesmosflt.tif). Both mosaics are ArcView-ArcInfo ready in TIF format with associated world files (*.tfw).

LROC Targeted Observations for the Next Generation of Scientific Exploration

NASA Astrophysics Data System (ADS)

Jolliff, B. L.

2015-12-01

Imaging of the Moon at high spatial resolution (0.5 to 2 mpp) by the Lunar Reconnaissance Orbiter Camera (LROC) Narrow Angle Cameras (NAC) plus topographic data derived from LROC NAC and WAC (Wide Angle Camera) and LOLA (Lunar Orbiting Laser Altimeter), coupled with recently obtained hyperspectral NIR and thermal data, permit studies of composition, mineralogy, and geologic context at essentially an outcrop scale. Such studies pave the way for future landed and sample return missions for high science priority targets. Among such targets are (1) the youngest volcanic rocks on the Moon, including mare basalts formed as recently as ~1 Ga, and irregular mare patches (IMPs) that appear to be even younger [1]; (2) volcanic rocks and complexes with compositions more silica-rich than mare basalts [2-4]; (3) differentiated impact-melt deposits [5,6], ancient volcanics, and compositional anomalies within the South Pole-Aitken basin; (4) exposures of recently discovered key crustal rock types in uplifted structures such as essentially pure anorthosite [7] and spinel-rich rocks [8]; and (5) frozen volatile-element-rich deposits in polar areas [9]. Important data sets include feature sequences of paired NAC images obtained under similar illumination conditions, NAC geometric stereo, from which high-resolution DTMs can be made, and photometric sequences useful for assessing composition in areas of mature cover soils. Examples of each of these target types will be discussed in context of potential future missions. References: [1] Braden et al. (2014) Nat. Geo. 7, 787-791. [2] Glotch et al. (2010) Science, 329, 1510-1513. [3] Greenhagen et al. (2010) Science, 329, 1507-1509. [4] Jolliff et al. (2011) Nat. Geo. 4, 566-571. [5] Vaughan et al (2013) PSS 91, 101-106. [6] Hurwitz and Kring (2014) J. Geophys. Res. 119, 1110-1133 [7] Ohtake et al. (2009) Nature, 461, 236-241 [8] Pieters et al. (2014) Am. Min. 99, 1893-1910. [9] Colaprete et al. (2010) Science 330, 463-468.

EU-FP7-iMARS: Analysis of Mars Multi-Resolution Images Using Auto-Coregistration Data Mining and Crowd Source Techniques: Processed Results - a First Look

NASA Astrophysics Data System (ADS)

Muller, Jan-Peter; Tao, Yu; Sidiropoulos, Panagiotis; Gwinner, Klaus; Willner, Konrad; Fanara, Lida; Waehlisch, Marita; van Gasselt, Stephan; Walter, Sebastian; Steikert, Ralf; Schreiner, Bjoern; Ivanov, Anton; Cantini, Federico; Wardlaw, Jessica; Morley, Jeremy; Sprinks, James; Giordano, Michele; Marsh, Stuart; Kim, Jungrack; Houghton, Robert; Bamford, Steven

2016-06-01

Understanding planetary atmosphere-surface exchange and extra-terrestrial-surface formation processes within our Solar System is one of the fundamental goals of planetary science research. There has been a revolution in planetary surface observations over the last 15 years, especially in 3D imaging of surface shape. This has led to the ability to overlay image data and derived information from different epochs, back in time to the mid 1970s, to examine changes through time, such as the recent discovery of mass movement, tracking inter-year seasonal changes and looking for occurrences of fresh craters. Within the EU FP-7 iMars project, we have developed a fully automated multi-resolution DTM processing chain, called the Coregistration ASP-Gotcha Optimised (CASP-GO), based on the open source NASA Ames Stereo Pipeline (ASP) [Tao et al., this conference], which is being applied to the production of planetwide DTMs and ORIs (OrthoRectified Images) from CTX and HiRISE. Alongside the production of individual strip CTX & HiRISE DTMs & ORIs, DLR [Gwinner et al., 2015] have processed HRSC mosaics of ORIs and DTMs for complete areas in a consistent manner using photogrammetric bundle block adjustment techniques. A novel automated co-registration and orthorectification chain has been developed by [Sidiropoulos & Muller, this conference]. Using the HRSC map products (both mosaics and orbital strips) as a map-base it is being applied to many of the 400,000 level-1 EDR images taken by the 4 NASA orbital cameras. In particular, the NASA Viking Orbiter camera (VO), Mars Orbiter Camera (MOC), Context Camera (CTX) as well as the High Resolution Imaging Science Experiment (HiRISE) back to 1976. A webGIS has been developed [van Gasselt et al., this conference] for displaying this time sequence of imagery and will be demonstrated showing an example from one of the HRSC quadrangle map-sheets. Automated quality control [Sidiropoulos & Muller, 2015] techniques are applied to screen for suitable images and these are extended to detect temporal changes in features on the surface such as mass movements, streaks, spiders, impact craters, CO2 geysers and Swiss Cheese terrain. For result verification these data mining techniques are then being employed within a citizen science project within the Zooniverse family. Examples of data mining and its verification will be presented.

KENNEDY SPACE CENTER, FLA. - In the Orbiter Processing Facility, while Greg Harlow, with United Space Alliance (USA) (above) threads a camera under the tiles of the orbiter Endeavour, Peggy Ritchie, USA, (behind the stand) and NASA’s Richard Parker (seated) watch the images on a monitor to inspect for corrosion.

NASA Image and Video Library

2003-09-04

KENNEDY SPACE CENTER, FLA. - In the Orbiter Processing Facility, while Greg Harlow, with United Space Alliance (USA) (above) threads a camera under the tiles of the orbiter Endeavour, Peggy Ritchie, USA, (behind the stand) and NASA’s Richard Parker (seated) watch the images on a monitor to inspect for corrosion.

KENNEDY SPACE CENTER, FLA. - In the Orbiter Processing Facility, while Greg Harlow, with United Space Alliance (USA), (above) threads a camera under the tiles of the orbiter Endeavour, NASA’s Richard Parker (below left) and Peggy Ritchie, with USA, (at right) watch the images on a monitor to inspect for corrosion.

NASA Image and Video Library

2003-09-04

KENNEDY SPACE CENTER, FLA. - In the Orbiter Processing Facility, while Greg Harlow, with United Space Alliance (USA), (above) threads a camera under the tiles of the orbiter Endeavour, NASA’s Richard Parker (below left) and Peggy Ritchie, with USA, (at right) watch the images on a monitor to inspect for corrosion.

KENNEDY SPACE CENTER, FLA. - In the Orbiter Processing Facility, while Greg Harlow, with United Space Alliance (USA), (above) threads a camera under the tiles of the orbiter Endeavour, Peggy Ritchie, with USA, (behind the stand) and NASA’s Richard Parker watch the images on a monitor to inspect for corrosion.

NASA Image and Video Library

2003-09-04

KENNEDY SPACE CENTER, FLA. - In the Orbiter Processing Facility, while Greg Harlow, with United Space Alliance (USA), (above) threads a camera under the tiles of the orbiter Endeavour, Peggy Ritchie, with USA, (behind the stand) and NASA’s Richard Parker watch the images on a monitor to inspect for corrosion.

The Camera of the MASCOT Asteroid Lander on Board Hayabusa 2

NASA Astrophysics Data System (ADS)

Jaumann, R.; Schmitz, N.; Koncz, A.; Michaelis, H.; Schroeder, S. E.; Mottola, S.; Trauthan, F.; Hoffmann, H.; Roatsch, T.; Jobs, D.; Kachlicki, J.; Pforte, B.; Terzer, R.; Tschentscher, M.; Weisse, S.; Mueller, U.; Perez-Prieto, L.; Broll, B.; Kruselburger, A.; Ho, T.-M.; Biele, J.; Ulamec, S.; Krause, C.; Grott, M.; Bibring, J.-P.; Watanabe, S.; Sugita, S.; Okada, T.; Yoshikawa, M.; Yabuta, H.

2017-07-01

The MASCOT Camera (MasCam) is part of the Mobile Asteroid Surface Scout (MASCOT) lander's science payload. MASCOT has been launched to asteroid (162173) Ryugu onboard JAXA's Hayabusa 2 asteroid sample return mission on Dec 3rd, 2014. It is scheduled to arrive at Ryugu in 2018, and return samples to Earth by 2020. MasCam was designed and built by DLR's Institute of Planetary Research, together with Airbus-DS Germany. The scientific goals of the MasCam investigation are to provide ground truth for the orbiter's remote sensing observations, provide context for measurements by the other lander instruments (radiometer, spectrometer and magnetometer), the orbiter sampling experiment, and characterize the geological context, compositional variations and physical properties of the surface (e.g. rock and regolith particle size distributions). During daytime, clear filter images will be acquired. During night, illumination of the dark surface is performed by an LED array, equipped with 4×36 monochromatic light-emitting diodes (LEDs) working in four spectral bands. Color imaging will allow the identification of spectrally distinct surface units. Continued imaging during the surface mission phase and the acquisition of image series at different sun angles over the course of an asteroid day will contribute to the physical characterization of the surface and also allow the investigation of time-dependent processes and to determine the photometric properties of the regolith. The MasCam observations, combined with the MASCOT hyperspectral microscope (MMEGA) and radiometer (MARA) thermal observations, will cover a wide range of observational scales and serve as a strong tie point between Hayabusa 2's remote-sensing scales (103-10^{-3} m) and sample scales (10^{-3}-10^{-6} m). The descent sequence and the close-up images will reveal the surface features over a broad range of scales, allowing an assessment of the surface's diversity and close the gap between the orbital observations and those made by the in-situ measurements. The MasCam is mounted inside the lander slightly tilted, such that the center of its 54.8° square field-of-view is directed towards the surface at an angle of 22° with respect to the surface plane. This is to ensure that both the surface close to the lander and the horizon are observable. The camera optics is designed according to the Scheimpflug principle, thus that the entire scene along the camera's depth of field (150 mm to infinity) is in focus. The camera utilizes a 1024×1024 pixel CMOS sensor sensitive in the 400-1000 nm wavelength range, peaking at 600-700 nm. Together with the f-16 optics, this yields a nominal ground resolution of 150 micron/px at 150 mm distance (diffraction limited). The camera flight model has undergone standard radiometric and geometric calibration both at the component and system (lander) level. MasCam relies on the use of wavelet compression to maximize data return within stringent mission downlink limits. All calibration and flight data products will be generated and archived in the Planetary Data System in PDS image format.

STS-34 Pilot Michael J. McCulley uses ARRIFLEX camera equipment

NASA Image and Video Library

1989-04-13

STS-34 Atlantis, Orbiter Vehicle (OV) 104, Pilot Michael J. McCulley squints while looking through ARRIFLEX camera eye piece during camera briefing at JSC. McCulley rests part of the camera on his shoulder as he operates it.

Camera for detection of cosmic rays of energy more than 10 Eev on the ISS orbit

DOE Office of Scientific and Technical Information (OSTI.GOV)

Garipov, G. K.; Khrenov, B. A.; Panasyuk, M. I.

1998-06-15

Concept of the EHE CR observation from the ISS orbit is discussed. A design of the camera at the Russian segment of the ISS comprising a large area (60 m{sup 2}) parabolic mirror with a photo multiplier pixel retina in its focal plane is described.

Mapping the Apollo 17 landing site area based on Lunar Reconnaissance Orbiter Camera images and Apollo surface photography

NASA Astrophysics Data System (ADS)

Haase, I.; Oberst, J.; Scholten, F.; Wählisch, M.; Gläser, P.; Karachevtseva, I.; Robinson, M. S.

2012-05-01

Newly acquired high resolution Lunar Reconnaissance Orbiter Camera (LROC) images allow accurate determination of the coordinates of Apollo hardware, sampling stations, and photographic viewpoints. In particular, the positions from where the Apollo 17 astronauts recorded panoramic image series, at the so-called “traverse stations”, were precisely determined for traverse path reconstruction. We analyzed observations made in Apollo surface photography as well as orthorectified orbital images (0.5 m/pixel) and Digital Terrain Models (DTMs) (1.5 m/pixel and 100 m/pixel) derived from LROC Narrow Angle Camera (NAC) and Wide Angle Camera (WAC) images. Key features captured in the Apollo panoramic sequences were identified in LROC NAC orthoimages. Angular directions of these features were measured in the panoramic images and fitted to the NAC orthoimage by applying least squares techniques. As a result, we obtained the surface panoramic camera positions to within 50 cm. At the same time, the camera orientations, North azimuth angles and distances to nearby features of interest were also determined. Here, initial results are shown for traverse station 1 (northwest of Steno Crater) as well as the Apollo Lunar Surface Experiment Package (ALSEP) area.

Present status of the Japanese Venus climate orbiter

NASA Astrophysics Data System (ADS)

Nakamura, M.; Imamura, T.; Abe, T.; Ishii, N.

The code name of 24th science spacecraft of ISAS/JAXA is Planet-C. It is the first Venus Climate Orbiter (VCO) of Japan. The ministry of finance of Japan finally agreed to start phase B study of VCO from this April, 2004. We plan 1-2 years phase B study followed by 2 years of flight model integration. The spacecraft will be launched between 2009 and 2010. After arriving Venus, 2 years of operation is expected. VCO will complemet the ESA's Venus Express mission which have several spectrometers and will reveal the composition of the Venusian atmosphere. On the other hand, VCO is designed to reveal the details of the atmospheric motion on Venus and approach the dynamics of the Venusian climate. Cooperation between Japanese VCO and ESA's Venus Express, in the colaboration framework of U.S., Europian, and Japanese scienctist is very important. To elucidate the driving mechanism of the 4-days super-rotation is one of our main targets. We have 4 cameras to take snap shots of the planets in different wave lengths. They are the IR1 camera (1 micron-meter), the IR2 camera (2.4 micron-meter), the LIR camera (10-12 micron-meter), and the UVI camera (340nm). They are attached to the side panel of the 3-axis stabilized spacecraft, and are directed to Venus with the spacecraft's attitude control. Snap shots are expected to be taken every 2 hours. The spacecraft has an orbit of 300km x 13Rv (Venusian radii) with 172 degrees inclination. Orbital period is 30 hours. The angular position of the spacecraft on this orbit is synchronized for 20 hours at its apoapsis with the global atmospheric circulation at the altitude of 50km, thus the snap shots of every 2 hours will be the images of the same side of the atmosphere. In addition to these 4 cameras, we have a Lightning and Airglow camera (LAC) in visible range. This will be operated when the orbiter is close to the planet.

Full-Frame Reference for Test Photo of Moon

NASA Technical Reports Server (NTRS)

2005-01-01

This pair of views shows how little of the full image frame was taken up by the Moon in test images taken Sept. 8, 2005, by the High Resolution Imaging Science Experiment (HiRISE) camera on NASA's Mars Reconnaissance Orbiter. The Mars-bound camera imaged Earth's Moon from a distance of about 10 million kilometers (6 million miles) away -- 26 times the distance between Earth and the Moon -- as part of an activity to test and calibrate the camera. The images are very significant because they show that the Mars Reconnaissance Orbiter spacecraft and this camera can properly operate together to collect very high-resolution images of Mars. The target must move through the camera's telescope view in just the right direction and speed to acquire a proper image. The day's test images also demonstrate that the focus mechanism works properly with the telescope to produce sharp images.

Out of the 20,000-pixel-by-6,000-pixel full frame, the Moon's diameter is about 340 pixels, if the full Moon could be seen. The illuminated crescent is about 60 pixels wide, and the resolution is about 10 kilometers (6 miles) per pixel. At Mars, the entire image region will be filled with high-resolution information.

The Mars Reconnaissance Orbiter, launched on Aug. 12, 2005, is on course to reach Mars on March 10, 2006. After gradually adjusting the shape of its orbit for half a year, it will begin its primary science phase in November 2006. From the mission's planned science orbit about 300 kilometers (186 miles) above the surface of Mars, the high resolution camera will be able to discern features as small as one meter or yard across.

The Mars Reconnaissance Orbiter mission is managed by NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology, Pasadena, for the NASA Science Mission Directorate. Lockheed Martin Space Systems, Denver, prime contractor for the project, built the spacecraft. Ball Aerospace & Technologies Corp., Boulder, Colo., built the High Resolution Imaging Science Experiment instrument for the University of Arizona, Tucson, to provide to the mission. The HiRISE Operations Center at the University of Arizona processes images from the camera.

A system for simulating aerial or orbital TV observations of geographic patterns

NASA Technical Reports Server (NTRS)

Latham, J. P.

1972-01-01

A system which simulates observation of the earth surface by aerial or orbiting television devices has been developed. By projecting color slides of photographs taken by aircraft and orbiting sensors upon a rear screen system, and altering scale of projected image, screen position, or TV camera position, it is possible to simulate alternatives of altitude, or optical systems. By altering scan line patterns in COHU 3200 series camera from 525 to 945 scan lines, it is possible to study implications of scan line resolution upon the detection and analysis of geographic patterns observed by orbiting TV systems.

Mars Odyssey from Two Distances in One Image

NASA Technical Reports Server (NTRS)

2005-01-01

[figure removed for brevity, see original site] Figure 1: Why There are Two Images of Odyssey

NASA's Mars Odyssey spacecraft appears twice in the same frame in this image from the Mars Orbiter Camera aboard NASA's Mars Global Surveyor. The camera's successful imaging of Odyssey and of the European Space Agency's Mars Express in April 2005 produced the first pictures of any spacecraft orbiting Mars taken by another spacecraft orbiting Mars.

Mars Global Surveyor and Mars Odyssey are both in nearly circular, near-polar orbits. Odyssey is in an orbit slightly higher than that of Global Surveyor in order to preclude the possibility of a collision. However, the two spacecraft occasionally come as close together as 15 kilometers (9 miles).

The images were obtained by the Mars Global Surveyor operations teams at Lockheed Martin Space System, Denver; JPL and Malin Space Science Systems.

The two views of Mars Odyssey in this image were acquired a little under 7.5 seconds apart as Odyssey receded from a close flyby of Mars Global Surveyor. The geometry of the flyby (see Figure 1) and the camera's way of acquiring an image line-by-line resulted in the two views of Odyssey in the same frame. The first view (right) was taken when Odyssey was about 90 kilometers (56 miles) from Global Surveyor and moving more rapidly than Global Surveyor was rotating, as seen from Global Surveyor. A few seconds later, Odyssey was farther away -- about 135 kilometers (84 miles) -- and appeared to be moving more slowly. In this second view of Odyssey (left), the Mars Orbiter Camera's field-of-view overtook Odyssey.

The Mars Orbiter Camera can resolve features on the surface of Mars as small as a few meters or yards across from Mars Global Surveyor's orbital altitude of 350 to 405 kilometers (217 to 252 miles). From a distance of 100 kilometers (62 miles), the camera would be able to resolve features substantially smaller than 1 meter or yard across.

Mars Odyssey was launched on April 7, 2001, and reached Mars on Oct. 24, 2001. Mars Global Surveyor left Earth on Nov. 7, 1996, and arrived in Mars orbit on Sept. 12, 1997. Both orbiters are in an extended mission phase, both have relayed data from the Mars Exploration Rovers, and both are continuing to return exciting new results from Mars. JPL, a division of the California Institute of Technology, Pasadena, manages both missions for NASA's Science Mission Directorate, Washington, D.C.

Examining Mars at Many Levels (Artist Concept)

NASA Image and Video Library

2005-03-23

This artist's concept represents the "Follow the Water" theme of NASA's Mars Reconnaissance Orbiter mission. The orbiter's science instruments monitor the present water cycle in the Mars atmosphere and the associated deposition and sublimation of water ice on the surface, while probing the subsurface to see how deep the water-ice reservoir detected by Mars Odyssey extends. At the same time, Mars Reconnaissance Orbiter will search for surface features and minerals (such as carbonates and sulfates) that record the extended presence of liquid water on the surface earlier in the planet's history. The instruments involved are the Shallow Subsurface Radar, the Compact Reconnaissance Imaging Spectrometer for Mars, the Mars Color Imager, the High Resolution Imaging Science Experiment, the Context Camera and the Mars Climate Sounder. To the far left, the radar antenna beams down and "sees" into the first few hundred feet (up to 1 kilometer) of Mars' crust. Just to the right of that, the next beam highlights the data received from the imaging spectrometer, which identifies minerals on the surface. The next beam represents the high-resolution camera, which can "zoom in" on local targets, providing the highest-resolution orbital images yet of features such as craters and gullies and rocks. The beam that shines almost horizontally is that of the Mars Climate Sounder. This instrument is critical to analyzing the current climate of Mars since it observes the temperature, humidity, and dust content of the martian atmosphere, and their seasonal and year-to-year variations. Meanwhile, the Mars Color Imager observes ice clouds, dust clouds and hazes, and the ozone distribution, producing daily global maps in multiple colors to monitor daily weather and seasonal changes. The electromagnetic spectrum is represented on the top right and individual instruments are placed where their capability lies. http://photojournal.jpl.nasa.gov/catalog/PIA07241

Inflight Calibration of the Lunar Reconnaissance Orbiter Camera Wide Angle Camera

NASA Astrophysics Data System (ADS)

Mahanti, P.; Humm, D. C.; Robinson, M. S.; Boyd, A. K.; Stelling, R.; Sato, H.; Denevi, B. W.; Braden, S. E.; Bowman-Cisneros, E.; Brylow, S. M.; Tschimmel, M.

2016-04-01

The Lunar Reconnaissance Orbiter Camera (LROC) Wide Angle Camera (WAC) has acquired more than 250,000 images of the illuminated lunar surface and over 190,000 observations of space and non-illuminated Moon since 1 January 2010. These images, along with images from the Narrow Angle Camera (NAC) and other Lunar Reconnaissance Orbiter instrument datasets are enabling new discoveries about the morphology, composition, and geologic/geochemical evolution of the Moon. Characterizing the inflight WAC system performance is crucial to scientific and exploration results. Pre-launch calibration of the WAC provided a baseline characterization that was critical for early targeting and analysis. Here we present an analysis of WAC performance from the inflight data. In the course of our analysis we compare and contrast with the pre-launch performance wherever possible and quantify the uncertainty related to various components of the calibration process. We document the absolute and relative radiometric calibration, point spread function, and scattered light sources and provide estimates of sources of uncertainty for spectral reflectance measurements of the Moon across a range of imaging conditions.

KSC-04PD-1812

NASA Technical Reports Server (NTRS)

2004-01-01

KENNEDY SPACE CENTER, FLA. In the Orbiter Processing Facility, United Space Alliance worker Craig Meyer fits an External Tank (ET) digital still camera in the right-hand liquid oxygen umbilical well on Space Shuttle Atlantis. NASA is pursuing use of the camera, beginning with the Shuttles Return To Flight, to obtain and downlink high-resolution images of the ET following separation of the ET from the orbiter after launch. The Kodak camera will record 24 images, at one frame per 1.5 seconds, on a flash memory card. After orbital insertion, the crew will transfer the images from the memory card to a laptop computer. The files will then be downloaded through the Ku-band system to the Mission Control Center in Houston for analysis.

KSC-04PD-1813

NASA Technical Reports Server (NTRS)

2004-01-01

KENNEDY SPACE CENTER, FLA. In the Orbiter Processing Facility, an External Tank (ET) digital still camera is positioned into the right-hand liquid oxygen umbilical well on Space Shuttle Atlantis to determine if it fits properly. NASA is pursuing use of the camera, beginning with the Shuttles Return To Flight, to obtain and downlink high-resolution images of the ET following separation of the ET from the orbiter after launch. The Kodak camera will record 24 images, at one frame per 1.5 seconds, on a flash memory card. After orbital insertion, the crew will transfer the images from the memory card to a laptop computer. The files will then be downloaded through the Ku-band system to the Mission Control Center in Houston for analysis.

KSC-04pd1813

NASA Image and Video Library

2004-09-17

KENNEDY SPACE CENTER, FLA. - In the Orbiter Processing Facility, an External Tank (ET) digital still camera is positioned into the right-hand liquid oxygen umbilical well on Space Shuttle Atlantis to determine if it fits properly. NASA is pursuing use of the camera, beginning with the Shuttle’s Return To Flight, to obtain and downlink high-resolution images of the ET following separation of the ET from the orbiter after launch. The Kodak camera will record 24 images, at one frame per 1.5 seconds, on a flash memory card. After orbital insertion, the crew will transfer the images from the memory card to a laptop computer. The files will then be downloaded through the Ku-band system to the Mission Control Center in Houston for analysis.

KSC-04pd1812

NASA Image and Video Library

2004-09-17

KENNEDY SPACE CENTER, FLA. - In the Orbiter Processing Facility, United Space Alliance worker Craig Meyer fits an External Tank (ET) digital still camera in the right-hand liquid oxygen umbilical well on Space Shuttle Atlantis. NASA is pursuing use of the camera, beginning with the Shuttle’s Return To Flight, to obtain and downlink high-resolution images of the ET following separation of the ET from the orbiter after launch. The Kodak camera will record 24 images, at one frame per 1.5 seconds, on a flash memory card. After orbital insertion, the crew will transfer the images from the memory card to a laptop computer. The files will then be downloaded through the Ku-band system to the Mission Control Center in Houston for analysis.

The High Resolution Stereo Camera (HRSC): 10 Years of Imaging Mars

NASA Astrophysics Data System (ADS)

Jaumann, R.; Neukum, G.; Tirsch, D.; Hoffmann, H.

2014-04-01

The HRSC Experiment: Imagery is the major source for our current understanding of the geologic evolution of Mars in qualitative and quantitative terms.Imaging is required to enhance our knowledge of Mars with respect to geological processes occurring on local, regional and global scales and is an essential prerequisite for detailed surface exploration. The High Resolution Stereo Camera (HRSC) of ESA's Mars Express Mission (MEx) is designed to simultaneously map the morphology, topography, structure and geologic context of the surface of Mars as well as atmospheric phenomena [1]. The HRSC directly addresses two of the main scientific goals of the Mars Express mission: (1) High-resolution three-dimensional photogeologic surface exploration and (2) the investigation of surface-atmosphere interactions over time; and significantly supports: (3) the study of atmospheric phenomena by multi-angle coverage and limb sounding as well as (4) multispectral mapping by providing high-resolution threedimensional color context information. In addition, the stereoscopic imagery will especially characterize landing sites and their geologic context [1]. The HRSC surface resolution and the digital terrain models bridge the gap in scales between highest ground resolution images (e.g., HiRISE) and global coverage observations (e.g., Viking). This is also the case with respect to DTMs (e.g., MOLA and local high-resolution DTMs). HRSC is also used as cartographic basis to correlate between panchromatic and multispectral stereo data. The unique multi-angle imaging technique of the HRSC supports its stereo capability by providing not only a stereo triplet but also a stereo quintuplet, making the photogrammetric processing very robust [1, 3]. The capabilities for three dimensional orbital reconnaissance of the Martian surface are ideally met by HRSC making this camera unique in the international Mars exploration effort.

Identification of Martian Cave Skylights Using the Temperature Change During Day and Night

NASA Astrophysics Data System (ADS)

Jung, Jongil; Yi, Yu; Kim, Eojin

2014-06-01

Recently, cave candidates have been discovered on other planets besides the Earth, such as the Moon and Mars. When we go to other planets, caves could be possible human habitats providing natural protection from cosmic threats. In this study, seven cave candidates have been found on Pavonis Mons and Ascraeus Mons in Tharsis Montes on Mars. The cave candidates were selected using the images of the Context Camera (CTX) on the Mars Reconnaissance Orbiter (MRO). The Context Camera could provide images with the high resolution of 6 meter per pixel. The diameter of the candidates ranges from 50 to 100m. Cushing et al. (2007) have analyzed the temperature change at daytime and nighttime using the Thermal Emission Imaging System (THEMIS) for the sites of potential cave candidates. Similarly, we have examined the temperature change at daytime and at nighttime for seven cave candidates using the method of Cushing et al. (2007). Among those, only one candidate showed a distinct temperature change. However, we cannot verify a cave based on the temperature change only and further study is required for the improvement of this method to identify caves more clearly.

Deployable Wireless Camera Penetrators

NASA Technical Reports Server (NTRS)

Badescu, Mircea; Jones, Jack; Sherrit, Stewart; Wu, Jiunn Jeng

2008-01-01

A lightweight, low-power camera dart has been designed and tested for context imaging of sampling sites and ground surveys from an aerobot or an orbiting spacecraft in a microgravity environment. The camera penetrators also can be used to image any line-of-sight surface, such as cliff walls, that is difficult to access. Tethered cameras to inspect the surfaces of planetary bodies use both power and signal transmission lines to operate. A tether adds the possibility of inadvertently anchoring the aerobot, and requires some form of station-keeping capability of the aerobot if extended examination time is required. The new camera penetrators are deployed without a tether, weigh less than 30 grams, and are disposable. They are designed to drop from any altitude with the boost in transmitting power currently demonstrated at approximately 100-m line-of-sight. The penetrators also can be deployed to monitor lander or rover operations from a distance, and can be used for surface surveys or for context information gathering from a touch-and-go sampling site. Thanks to wireless operation, the complexity of the sampling or survey mechanisms may be reduced. The penetrators may be battery powered for short-duration missions, or have solar panels for longer or intermittent duration missions. The imaging device is embedded in the penetrator, which is dropped or projected at the surface of a study site at 90 to the surface. Mirrors can be used in the design to image the ground or the horizon. Some of the camera features were tested using commercial "nanny" or "spy" camera components with the charge-coupled device (CCD) looking at a direction parallel to the ground. Figure 1 shows components of one camera that weighs less than 8 g and occupies a volume of 11 cm3. This camera could transmit a standard television signal, including sound, up to 100 m. Figure 2 shows the CAD models of a version of the penetrator. A low-volume array of such penetrator cameras could be deployed from an aerobot or a spacecraft onto a comet or asteroid. A system of 20 of these penetrators could be designed and built in a 1- to 2-kg mass envelope. Possible future modifications of the camera penetrators, such as the addition of a chemical spray device, would allow the study of simple chemical reactions of reagents sprayed at the landing site and looking at the color changes. Zoom lenses also could be added for future use.

NASA's Optical Program on Ascension Island: Bringing MCAT to Life as the Eugene Stansbery-Meter Class Autonomous Telescope (ES-MCAT)

NASA Astrophysics Data System (ADS)

Lederer, S. M.; Hickson, P.; Cowardin, H. M.; Buckalew, B.; Frith, J.; Alliss, R.

In June 2015, the construction of the Meter Class Autonomous Telescope was completed and MCAT saw the light of the stars for the first time. In 2017, MCAT was newly dedicated as the Eugene Stansbery-MCAT telescope by NASA’s Orbital Debris Program Office (ODPO), in honour of his inspiration and dedication to this newest optical member of the NASA ODPO. Since that time, MCAT has viewed the skies with one engineering camera and two scientific cameras, and the ODPO optical team has begun the process of vetting the entire system. The full system vetting includes verification and validation of: (1) the hardware comprising the system (e.g. the telescopes and its instruments, the dome, weather systems, all-sky camera, FLIR cloud infrared camera, etc.), (2) the custom-written Observatory Control System (OCS) master software designed to autonomously control this complex system of instruments, each with its own control software, and (3) the custom written Orbital Debris Processing software for post-processing the data. ES-MCAT is now capable of autonomous observing to include Geosyncronous survey, TLE (Two-line element) tracking of individual catalogued debris at all orbital regimes (Low-Earth Orbit all the way to Geosynchronous (GEO) orbit), tracking at specified non-sidereal rates, as well as sidereal rates for proper calibration with standard stars. Ultimately, the data will be used for validation of NASA’s Orbital Debris Engineering Model, ORDEM, which aids in engineering designs of spacecraft that require knowledge of the orbital debris environment and long-term risks for collisions with Resident Space Objects (RSOs).

NASA's Optical Program on Ascension Island: Bringing MCAT to Life as the Eugene Stansbery-Meter Class Autonomous Telescope (ES-MCAT)

NASA Technical Reports Server (NTRS)

Lederer, S. M.; Hickson, P.; Cowardin, H. M.; Buckalew, B.; Frith, J.; Alliss, R.

2017-01-01

In June 2015, the construction of the Meter Class Autonomous Telescope was completed and MCAT saw the light of the stars for the first time. In 2017, MCAT was newly dedicated as the Eugene Stansbery-MCAT telescope by NASA's Orbital Debris Program Office (ODPO), in honor of his inspiration and dedication to this newest optical member of the NASA ODPO. Since that time, MCAT has viewed the skies with one engineering camera and two scientific cameras, and the ODPO optical team has begun the process of vetting the entire system. The full system vetting includes verification and validation of: (1) the hardware comprising the system (e.g. the telescopes and its instruments, the dome, weather systems, all-sky camera, FLIR cloud infrared camera, etc.), (2) the custom-written Observatory Control System (OCS) master software designed to autonomously control this complex system of instruments, each with its own control software, and (3) the custom written Orbital Debris Processing software for post-processing the data. ES-MCAT is now capable of autonomous observing to include Geosynchronous survey, TLE (Two-line element) tracking of individual catalogued debris at all orbital regimes (Low-Earth Orbit all the way to Geosynchronous (GEO) orbit), tracking at specified non-sidereal rates, as well as sidereal rates for proper calibration with standard stars. Ultimately, the data will be used for validation of NASA's Orbital Debris Engineering Model, ORDEM, which aids in engineering designs of spacecraft that require knowledge of the orbital debris environment and long-term risks for collisions with Resident Space Objects (RSOs).

Public-Requested Mars Image: Crater on Pavonis Mons

NASA Technical Reports Server (NTRS)

2003-01-01

MGS MOC Release No. MOC2-481, 12 September 2003

This image is in the first pair obtained in the Public Target Request program, which accepts suggestions for sites to photograph with the Mars Orbiter Camera on NASA's Mars Global Surveyor spacecraft.

It is a narrow-angle (high-resolution) view of a portion of the lower wall and floor of the caldera at the top of a martian volcano named Pavonis Mons. A companion picture is a wide-angle context image, taken at the same time as the high-resolution view. The white box in the context frame shows the location of the high-resolution picture.

[figure removed for brevity, see original site]

Pavonis Mons is a broad shield volcano. Its summit region is about 14 kilometers (8.7 miles) above the martian datum (zero-elevation reference level). The caldera is about 4.6 kilometers (2.8 miles) deep. The caldera formed by collapse--long ago--as molten rock withdrew to greater depths within the volcano. The high-resolution picture shows that today the floor and walls of this caldera are covered by a thick, textured mantle of dust, perhaps more than 1 meter (1 yard) deep. Larger boulders and rock outcroppings poke out from within this dust mantle. They are seen as small, dark dots and mounds on the lower slopes of the wall in the high-resolution image.

The narrow-angle Mars Orbiter Camera image has a resolution of 1.5 meters (about 5 feet) per pixel and covers an area 1.5 kilometers (0.9 mile) wide by 9 kilometers (5.6 miles) long. The context image, covering much of the summit region of Pavonis Mons, is about 115 kilometers (72 miles) wide. Sunlight illuminates both images from the lower left; north is toward the upper right; east to the right. The high-resolution view is located near 0.4 degrees north latitude, 112.8 degrees west longitude.

KSC-04PD-1810

NASA Technical Reports Server (NTRS)

2004-01-01

KENNEDY SPACE CENTER, FLA. In the Orbiter Processing Facility, from left, United Space Alliance workers Loyd Turner, Craig Meyer and Erik Visser prepare to conduct a fit check of an External Tank (ET) digital still camera in the right-hand liquid oxygen umbilical well on Space Shuttle Atlantis. NASA is pursuing use of the camera, beginning with the Shuttles Return To Flight, to obtain and downlink high-resolution images of the ET following separation of the ET from the orbiter after launch. The Kodak camera will record 24 images, at one frame per 1.5 seconds, on a flash memory card. After orbital insertion, the crew will transfer the images from the memory card to a laptop computer. The files will then be downloaded through the Ku-band system to the Mission Control Center in Houston for analysis.

KSC-04PD-1811

NASA Technical Reports Server (NTRS)

2004-01-01

KENNEDY SPACE CENTER, FLA. In the Orbiter Processing Facility, from left, United Space Alliance workers Loyd Turner, Craig Meyer and Erik Visser conduct a fit check of an External Tank (ET) digital still camera in the right-hand liquid oxygen umbilical well on Space Shuttle Atlantis. NASA is pursuing use of the camera, beginning with the Shuttles Return To Flight, to obtain and downlink high-resolution images of the ET following separation of the ET from the orbiter after launch. The Kodak camera will record 24 images, at one frame per 1.5 seconds, on a flash memory card. After orbital insertion, the crew will transfer the images from the memory card to a laptop computer. The files will then be downloaded through the Ku-band system to the Mission Control Center in Houston for analysis.

KSC-04pd1811

NASA Image and Video Library

2004-09-17

KENNEDY SPACE CENTER, FLA. - In the Orbiter Processing Facility, from left, United Space Alliance workers Loyd Turner, Craig Meyer and Erik Visser conduct a fit check of an External Tank (ET) digital still camera in the right-hand liquid oxygen umbilical well on Space Shuttle Atlantis. NASA is pursuing use of the camera, beginning with the Shuttle’s Return To Flight, to obtain and downlink high-resolution images of the ET following separation of the ET from the orbiter after launch. The Kodak camera will record 24 images, at one frame per 1.5 seconds, on a flash memory card. After orbital insertion, the crew will transfer the images from the memory card to a laptop computer. The files will then be downloaded through the Ku-band system to the Mission Control Center in Houston for analysis.

KSC-04pd1810

NASA Image and Video Library

2004-09-17

KENNEDY SPACE CENTER, FLA. - In the Orbiter Processing Facility, from left, United Space Alliance workers Loyd Turner, Craig Meyer and Erik Visser prepare to conduct a fit check of an External Tank (ET) digital still camera in the right-hand liquid oxygen umbilical well on Space Shuttle Atlantis. NASA is pursuing use of the camera, beginning with the Shuttle’s Return To Flight, to obtain and downlink high-resolution images of the ET following separation of the ET from the orbiter after launch. The Kodak camera will record 24 images, at one frame per 1.5 seconds, on a flash memory card. After orbital insertion, the crew will transfer the images from the memory card to a laptop computer. The files will then be downloaded through the Ku-band system to the Mission Control Center in Houston for analysis.

KSC-05PD-0820

NASA Technical Reports Server (NTRS)

2005-01-01

KENNEDY SPACE CENTER, FLA. At Kennedy Space Centers Shuttle Landing Facility, the second of two containers with the Mars Reconnaissance Orbiter (MRO) equipment is lifted onto a flatbed truck for transport to the Payload Hazardous Servicing Facility. The MRO was built by Lockheed-Martin for NASAs Jet Propulsion Laboratory in California. It is the next major step in Mars exploration and scheduled for launch from Cape Canaveral Air Force Station in a window opening Aug. 10. The MRO carries six primary instruments: the High Resolution Imaging Science Experiment, Context Camera, Mars Color Imager, Compact Reconnaissance Imaging Spectrometer for Mars, Mars Climate Sounder and Shallow Radar. By 2007, the MRO will begin a series of global mapping, regional survey and targeted observations from a near-polar, low-altitude Mars orbit. It will observe the atmosphere and surface of Mars while probing its shallow subsurface as part of a follow the water strategy.

Measuring the Orbital Period of the Moon Using a Digital Camera

ERIC Educational Resources Information Center

Hughes, Stephen W.

2006-01-01

A method of measuring the orbital velocity of the Moon around the Earth using a digital camera is described. Separate images of the Moon and stars taken 24 hours apart were loaded into Microsoft PowerPoint and the centre of the Moon marked on each image. Four stars common to both images were connected together to form a "home-made" constellation.…

Synchrotron emission diagnostic of full-orbit kinetic simulations of runaway electrons in tokamaks plasmas

NASA Astrophysics Data System (ADS)

Carbajal Gomez, Leopoldo; Del-Castillo-Negrete, Diego

2017-10-01

Developing avoidance or mitigation strategies of runaway electrons (RE) for the safe operation of ITER is imperative. Synchrotron radiation (SR) of RE is routinely used in current tokamak experiments to diagnose RE. We present the results of a newly developed camera diagnostic of SR for full-orbit kinetic simulations of RE in DIII-D-like plasmas that simultaneously includes: full-orbit effects, information of the spectral and angular distribution of SR of each electron, and basic geometric optics of a camera. We observe a strong dependence of the SR measured by the camera on the pitch angle distribution of RE, namely we find that crescent shapes of the SR on the camera pictures relate to RE distributions with small pitch angles, while ellipse shapes relate to distributions of RE with larger pitch angles. A weak dependence of the SR measured by the camera with the RE energy, value of the q-profile at the edge, and the chosen range of wavelengths is found. Furthermore, we observe that oversimplifying the angular distribution of the SR changes the synchrotron spectra and overestimates its amplitude. Research sponsored by the LDRD Program of ORNL, managed by UT-Battelle, LLC, for the U. S. DoE.

High-Resolution Mars Camera Test Image of Moon Infrared

NASA Image and Video Library

2005-09-13

This crescent view of Earth Moon in infrared wavelengths comes from a camera test by NASA Mars Reconnaissance Orbiter spacecraft on its way to Mars. This image was taken by taken by the High Resolution Imaging Science Experiment camera Sept. 8, 2005.

Focus adjustment method for CBERS 3 and 4 satellites Mux camera to be performed in air condition and its experimental verification for best performance in orbital vacuum condition

NASA Astrophysics Data System (ADS)

Scaduto, Lucimara C. N.; Malavolta, Alexandre T.; Modugno, Rodrigo G.; Vales, Luiz F.; Carvalho, Erica G.; Evangelista, Sérgio; Stefani, Mario A.; de Castro Neto, Jarbas C.

2017-11-01

The first Brazilian remote sensing multispectral camera (MUX) is currently under development at Opto Eletronica S.A. It consists of a four-spectral-band sensor covering a 450nm to 890nm wavelength range. This camera will provide images within a 20m ground resolution at nadir. The MUX camera is part of the payload of the upcoming Sino-Brazilian satellites CBERS 3&4 (China-Brazil Earth Resource Satellite). The preliminary alignment between the optical system and the CCD sensor, which is located at the focal plane assembly, was obtained in air condition, clean room environment. A collimator was used for the performance evaluation of the camera. The preliminary performance evaluation of the optical channel was registered by compensating the collimator focus position due to changes in the test environment, as an air-to-vacuum environment transition leads to a defocus process in this camera. Therefore, it is necessary to confirm that the alignment of the camera must always be attained ensuring that its best performance is reached for an orbital vacuum condition. For this reason and as a further step on the development process, the MUX camera Qualification Model was tested and evaluated inside a thermo-vacuum chamber and submitted to an as-orbit vacuum environment. In this study, the influence of temperature fields was neglected. This paper reports on the performance evaluation and discusses the results for this camera when operating within those mentioned test conditions. The overall optical tests and results show that the "in air" adjustment method was suitable to be performed, as a critical activity, to guarantee the equipment according to its design requirements.

In-flight Video Captured by External Tank Camera System

NASA Technical Reports Server (NTRS)

2005-01-01

In this July 26, 2005 video, Earth slowly fades into the background as the STS-114 Space Shuttle Discovery climbs into space until the External Tank (ET) separates from the orbiter. An External Tank ET Camera System featuring a Sony XC-999 model camera provided never before seen footage of the launch and tank separation. The camera was installed in the ET LO2 Feedline Fairing. From this position, the camera had a 40% field of view with a 3.5 mm lens. The field of view showed some of the Bipod area, a portion of the LH2 tank and Intertank flange area, and some of the bottom of the shuttle orbiter. Contained in an electronic box, the battery pack and transmitter were mounted on top of the Solid Rocker Booster (SRB) crossbeam inside the ET. The battery pack included 20 Nickel-Metal Hydride batteries (similar to cordless phone battery packs) totaling 28 volts DC and could supply about 70 minutes of video. Located 95 degrees apart on the exterior of the Intertank opposite orbiter side, there were 2 blade S-Band antennas about 2 1/2 inches long that transmitted a 10 watt signal to the ground stations. The camera turned on approximately 10 minutes prior to launch and operated for 15 minutes following liftoff. The complete camera system weighs about 32 pounds. Marshall Space Flight Center (MSFC), Johnson Space Center (JSC), Goddard Space Flight Center (GSFC), and Kennedy Space Center (KSC) participated in the design, development, and testing of the ET camera system.

STS-32 photographic equipment (cameras,lenses,film magazines) on flight deck

NASA Technical Reports Server (NTRS)

1990-01-01

STS-32 photographic equipment is displayed on the aft flight deck of Columbia, Orbiter Vehicle (OV) 102. On the payload station are a dual camera mount with two handheld HASSELBLAD cameras, camera lenses, and film magazines. This array of equipment will be used to record onboard activities and observations of the Earth's surface.

The on-orbit calibration of geometric parameters of the Tian-Hui 1 (TH-1) satellite

NASA Astrophysics Data System (ADS)

Wang, Jianrong; Wang, Renxiang; Hu, Xin; Su, Zhongbo

2017-02-01

The on-orbit calibration of geometric parameters is a key step in improving the location accuracy of satellite images without using Ground Control Points (GCPs). Most methods of on-orbit calibration are based on the self-calibration using additional parameters. When using additional parameters, different number of additional parameters may lead to different results. The triangulation bundle adjustment is another way to calibrate the geometric parameters of camera, which can describe the changes in each geometric parameter. When triangulation bundle adjustment method is applied to calibrate geometric parameters, a prerequisite is that the strip model can avoid systematic deformation caused by the rate of attitude changes. Concerning the stereo camera, the influence of the intersection angle should be considered during calibration. The Equivalent Frame Photo (EFP) bundle adjustment based on the Line-Matrix CCD (LMCCD) image can solve the systematic distortion of the strip model, and obtain high accuracy location without using GCPs. In this paper, the triangulation bundle adjustment is used to calibrate the geometric parameters of TH-1 satellite cameras based on LMCCD image. During the bundle adjustment, the three-line array cameras are reconstructed by adopting the principle of inverse triangulation. Finally, the geometric accuracy is validated before and after on-orbit calibration using 5 testing fields. After on-orbit calibration, the 3D geometric accuracy is improved to 11.8 m from 170 m. The results show that the location accuracy of TH-1 without using GCPs is significantly improved using the on-orbit calibration of the geometric parameters.

Schiaparelli Crater Rim and Interior Deposits

NASA Technical Reports Server (NTRS)

1998-01-01

A portion of the rim and interior of the large impact crater Schiaparelli is seen at different resolutions in images acquired October 18, 1997 by the Mars Global Surveyor Orbiter Camera (MOC) and by the Viking Orbiter 1 twenty years earlier. The left image is a MOC wide angle camera 'context' image showing much of the eastern portion of the crater at roughly 1 km (0.6 mi) per picture element. The image is about 390 by 730 km (240 X 450 miles). Shown within the wide angle image is the outline of a portion of the best Viking image (center, 371S53), acquired at a resolution of about 240 m/pixel (790 feet). The area covered is 144 X 144 km (89 X 89 miles). The right image is the high resolution narrow angle camera view. The area covered is very small--3.9 X 10.2 km (2.4 X 6.33 mi)--but is seen at 63 times higher resolution than the Viking image. The subdued relief and bright surface are attributed to blanketing by dust; many small craters have been completely filled in, and only the most recent (and very small) craters appear sharp and bowl-shaped. Some of the small craters are only 10-12 m (30-35 feet) across. Occasional dark streaks on steeper slopes are small debris slides that have probably occurred in the past few decades. The two prominent, narrow ridges in the center of the image may be related to the adjustment of the crater floor to age or the weight of the material filling the basin.

Malin Space Science Systems (MSSS) and the California Institute of Technology built the MOC using spare hardware from the Mars Observer mission. MSSS operates the camera from its facilities in San Diego, CA. The Jet Propulsion Laboratory's Mars Surveyor Operations Project operates the Mars Global Surveyor spacecraft with its industrial partner, Lockheed Martin Astronautics, from facilities in Pasadena, CA and Denver, CO.

Mission Specialist Michael Lopez-Alegria changes out film in camera

NASA Image and Video Library

1995-11-05

STS073-335-009 (20 October-5 November 1995) --- Astronaut Michael E. Lopez-Alegria, STS-73 mission specialist, changes the film in a 35mm camera on the flight deck of the Earth-orbiting Space Shuttle Columbia. Alegria joined four other NASA astronauts and two guest researchers for almost 16-days of Earth-orbit research in support of the U.S. Microgravity Laboratory (USML-2) mission.

Infrared On-Orbit RCC Inspection With the EVA IR Camera: Development of Flight Hardware From a COTS System

NASA Technical Reports Server (NTRS)

Gazanik, Michael; Johnson, Dave; Kist, Ed; Novak, Frank; Antill, Charles; Haakenson, David; Howell, Patricia; Jenkins, Rusty; Yates, Rusty; Stephan, Ryan;

Curiosity Spotted on Parachute by Orbiter

NASA Image and Video Library

2012-08-06

NASA Curiosity rover and its parachute were spotted by NASA Mars Reconnaissance Orbiter as Curiosity descended to the surface. The HiRISE camera captured this image of Curiosity while the orbiter was listening to transmissions from the rover.

Mars Express Seen by Mars Global Surveyor

NASA Image and Video Library

2005-05-19

This picture of the European Space Agency Mars Express spacecraft by the Mars Orbiter Camera on NASA Mars Global Surveyor is from the first successful imaging of any spacecraft orbiting Mars taken by another spacecraft orbiting Mars.

STS-47 MS Apt with LINHOF camera on JSC's Bldg 1 rooftop during training

NASA Technical Reports Server (NTRS)

1992-01-01

STS-47 Endeavour, Orbiter Vehicle (OV) 105, Mission Specialist (MS) Jerome Apt sets LINHOF camera lens during photography training session conducted on JSC's Project Management Building Bldg 1 rooftop. Using such a high vantage point as this nine-floor facility, Apt was able to become familiar with Earth Observations camera hadware such as the LINHOF camera.

Lunar orbital photogaphic planning charts for candidate Apollo J-missions

NASA Technical Reports Server (NTRS)

Hickson, P. J.; Piotrowski, W. L.

1971-01-01

A technique is presented for minimizing Mapping Camera film usage by reducing redundant coverage while meeting the desired sidelap of greater than or equal to 55%. The technique uses the normal groundtrack separation determined as a function of the number of revolutions between the respective tracks, of the initial and final nodal azimuths (or orbital inclination), and of the lunar latitude. The technique is also applicable for planning Panoramic Camera photography such that photographic contiguity is attained but redundant coverage is minimized. Graphs are included for planning mapping camera (MC) and panoramic camera (PC) photographic passes for a specific mission (i.e., specific groundtracks) to Descartes (Apollo 16), for specific missions to potential Apollo 17 sites such as Alphonsus, Proclus, Gassendi, Davy, and Tycho, and for a potential Apollo orbit-only mission with a nodal azimuth of 85 deg. Graphs are also included for determining the maximum number of revolutions which can elapse between successive MC and PC passes, for greater than or equal 55% sidelap and rectified contiguity respectively, for nodal azimuths between 5 deg and 85 deg.

Outflow Stream from Relatively Recent Martian Lake

NASA Image and Video Library

2016-09-15

Streamlined forms and channel bars in this Martian valley resulted from the outflow of a lake hundreds of millions years more recently than an era of Martian lakes previously confirmed, according to 2016 findings. This excerpt from an image taken by the Context Camera on NASA's Mars Reconnaissance Orbiter covers an area about 8 miles (13 kilometers) wide in the northern Arabia Terra region of Mars. The flow direction was generally northward (toward the top of this image). The channel breached a water-filled basin identified as "B" in a hydrologic-modeling map at PIA20839 and flowed toward a larger basin, informally called "Heart Lake," about 50 miles (80 kilometers) to the northwest. Researchers estimate this stream and the lakes it linked held water at some time in the range of 2 billion to 3 billion years ago. That is several hundred million to about 1 billion years later than better-known ancient lake environments on Mars, such as those documented by NASA's Curiosity rover mission. The later wet period came after it is generally thought that most of Mars' original atmosphere had been lost and most of the remaining water on the planet had frozen. Seasonal melting may have fed this stream. This is a portion of Context Camera image B18_016815_2151. http://photojournal.jpl.nasa.gov/catalog/PIA20837

STS-125 Space Shuttle Atlantis Documentation

NASA Image and Video Library

2009-06-01

Multiple camera documentation of STS-125 Atlantis landing and turnaround at Nasa Dryden Flight Research Center. Highlights: • 5th and final HST servicing mission • IMAX camera used to document mission highlights • 5 EVA’s • Orbital Altitude: 338.67 statute miles • Orbits: 197 (landed on orbit 198) • Duration: 12D 21H 37M 18S • Traveled: 5.28 million statute miles • 1st Shuttle landing on the refurbished EDW concrete runway • Orbiter Turnaround: 7 Days Crew: CDR: Scott Altman PLT: Gregory “Greg” Johnson MS1/EV4: Michael “Mike” Good MS2: Megan MacArthur MS3/EV1: John Grunsfeld MS4/EV3: Michael Massamino MS5/EV2: Andrew “Drew” Feustel

Research on camera on orbit radial calibration based on black body and infrared calibration stars

NASA Astrophysics Data System (ADS)

Wang, YuDu; Su, XiaoFeng; Zhang, WanYing; Chen, FanSheng

2018-05-01

Affected by launching process and space environment, the response capability of a space camera must be attenuated. So it is necessary for a space camera to have a spaceborne radiant calibration. In this paper, we propose a method of calibration based on accurate Infrared standard stars was proposed for increasing infrared radiation measurement precision. As stars can be considered as a point target, we use them as the radiometric calibration source and establish the Taylor expansion method and the energy extrapolation model based on WISE catalog and 2MASS catalog. Then we update the calibration results from black body. Finally, calibration mechanism is designed and the technology of design is verified by on orbit test. The experimental calibration result shows the irradiance extrapolation error is about 3% and the accuracy of calibration methods is about 10%, the results show that the methods could satisfy requirements of on orbit calibration.

Martian 'Spiders' in Sharper Look, Thanks to Volunteers

NASA Image and Video Library

2016-10-20

This image shows spidery channels eroded into Martian ground. It is an example from high-resolution observation of more than 20 places that were chosen in 2016 on the basis of about 10,000 volunteers' examination of lower-resolution images of larger areas near Mars' south pole. These sharper looks use the High Resolution Imaging Science Experiment (HiRISE) camera on NASA's Mars Reconnaissance Orbiter. The volunteers, through the Planet Four: Terrains website, categorize surface features in images from the same orbiter's Context Camera (CTX). This image is a portion of HiRISE observation ESP_047487_1005, taken on Sept. 12, 2016, of a site at 79.4 degrees south latitude, 18.8 degrees east longitude. The ground area shown is about half a mile (0.8 kilometer) wide. This terrain type, called spiders or "araneiform" (from the Latin word for spiders), appears in some areas of far-southern Mars that are covered by sheets of frozen carbon dioxide ("dry ice") during the winter. When the slab ice thaws from the underneath side in the spring, carbon dioxide gas trapped beneath the ice builds pressure until it rushes toward a fissure or vent where it bursts out. The venting gas carries dust and sand that it picks up as it carves these channels. At this location, the spiders are surrounded by ground called "basketball terrain" because of its texture. http://photojournal.jpl.nasa.gov/catalog/PIA21126

In-Flight performance of MESSENGER's Mercury dual imaging system

USGS Publications Warehouse

Hawkins, S.E.; Murchie, S.L.; Becker, K.J.; Selby, C.M.; Turner, F.S.; Noble, M.W.; Chabot, N.L.; Choo, T.H.; Darlington, E.H.; Denevi, B.W.; Domingue, D.L.; Ernst, C.M.; Holsclaw, G.M.; Laslo, N.R.; Mcclintock, W.E.; Prockter, L.M.; Robinson, M.S.; Solomon, S.C.; Sterner, R.E.

2009-01-01

The Mercury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) spacecraft, launched in August 2004 and planned for insertion into orbit around Mercury in 2011, has already completed two flybys of the innermost planet. The Mercury Dual Imaging System (MDIS) acquired nearly 2500 images from the first two flybys and viewed portions of Mercury's surface not viewed by Mariner 10 in 1974-1975. Mercury's proximity to the Sun and its slow rotation present challenges to the thermal design for a camera on an orbital mission around Mercury. In addition, strict limitations on spacecraft pointing and the highly elliptical orbit create challenges in attaining coverage at desired geometries and relatively uniform spatial resolution. The instrument designed to meet these challenges consists of dual imagers, a monochrome narrow-angle camera (NAC) with a 1.5?? field of view (FOV) and a multispectral wide-angle camera (WAC) with a 10.5?? FOV, co-aligned on a pivoting platform. The focal-plane electronics of each camera are identical and use a 1024??1024 charge-coupled device detector. The cameras are passively cooled but use diode heat pipes and phase-change-material thermal reservoirs to maintain the thermal configuration during the hot portions of the orbit. Here we present an overview of the instrument design and how the design meets its technical challenges. We also review results from the first two flybys, discuss the quality of MDIS data from the initial periods of data acquisition and how that compares with requirements, and summarize how in-flight tests are being used to improve the quality of the instrument calibration. ?? 2009 SPIE.

The Specters of Mars

NASA Image and Video Library

2017-07-13

This image from NASA's Mars Reconnaissance Orbiter shows Malea Planum,a polar region in the Southern hemisphere of Mars, directly south of Hellas Basin, which contains the lowest point of elevation on the planet. The region contains ancient volcanoes of a certain type, referred to as "paterae." Patera is the Latin word for a shallow drinking bowl, and was first applied to volcanic-looking features, with scalloped-edged calderas. Malea is also a low-lying plain, known to be covered in dust. These two pieces of information provide regional context that aid our understanding of the scene and features contained in our image. The area rises gradually to a ridge (which can be seen in this Context Camera image) and light-colored dust is blown away by gusts of the Martian wind, which accelerate up the slope to the ridge, leading to more sharp angles of contact between light and dark surface materials. https://photojournal.jpl.nasa.gov/catalog/PIA21784

Current status of Polish Fireball Network

NASA Astrophysics Data System (ADS)

Wiśniewski, M.; Żołądek, P.; Olech, A.; Tyminski, Z.; Maciejewski, M.; Fietkiewicz, K.; Rudawska, R.; Gozdalski, M.; Gawroński, M. P.; Suchodolski, T.; Myszkiewicz, M.; Stolarz, M.; Polakowski, K.

2017-09-01

The Polish Fireball Network (PFN) is a project to monitor regularly the sky over Poland in order to detect bright fireballs. In 2016 the PFN consisted of 36 continuously active stations with 57 sensitive analogue video cameras and 7 high resolution digital cameras. In our observations we also use spectroscopic and radio techniques. A PyFN software package for trajectory and orbit determination was developed. The PFN project is an example of successful participation of amateur astronomers who can provide valuable scientific data. The network is coordinated by astronomers from Copernicus Astronomical Centre in Warsaw, Poland. In 2011-2015 the PFN cameras recorded 214,936 meteor events. Using the PFN data and the UFOOrbit software 34,609 trajectories and orbits were calculated. In the following years we are planning intensive modernization of the PFN network including installation of dozens of new digital cameras.

STS-32 Commander Brandenstein adjusts IMAX camera during training session

NASA Technical Reports Server (NTRS)

1989-01-01

STS-32 Commander Daniel C. Brandenstein adjusts IMAX camera setting during briefing and training session as technician looks on. The session was conducted in the JSC Mockup and Integration Laboratory (MAIL) Bldg 9B. The IMAX camera will be used onboard Columbia, Orbiter Vehicle (OV) 102, during the STS-32 mission.

MS Kavandi with camera in Service Module

NASA Image and Video Library

2001-07-16

STS104-E-5125 (16 July 2001) --- Astronaut Janet L. Kavandi, STS-104 mission specialist, uses a camera as she floats through the Zvezda service module aboard the International Space Station (ISS). The five STS-104 crew members were visiting the orbital outpost to perform various tasks. The image was recorded with a digital still camera.

Clouds over Tharsis

NASA Technical Reports Server (NTRS)

1998-01-01

Color composite of condensate clouds over Tharsis made from red and blue images with a synthesized green channel. Mars Orbiter Camera wide angle frames from Orbit 48.

Figure caption from Science Magazine

KSC-05PD-0565

NASA Technical Reports Server (NTRS)

2005-01-01

KENNEDY SPACE CENTER, FLA. In the Vehicle Assembly Building at NASAs Kennedy Space Center, a digital still camera has been mounted in the External Tank (ET) umbilical well on the aft end of Space Shuttle Discovery. The camera is being used to obtain and downlink high-resolution images of the disconnect point on the ET following ET separation from the orbiter after launch. The Kodak camera will record 24 images, at one frame per 1.5 seconds, on a flash memory card. After orbital insertion, the crew will transfer the images from the memory card to a laptop computer. The files will then be downloaded through the Ku-band system to the Mission Control Center in Houston for analysis.

KSC-05PD-0562

NASA Technical Reports Server (NTRS)

2005-01-01

KENNEDY SPACE CENTER, FLA. In the Vehicle Assembly Building at NASAs Kennedy Space Center, workers check the digital still camera they will mount in the External Tank (ET) umbilical well on the aft end of Space Shuttle Discovery. The camera is being used to obtain and downlink high-resolution images of the disconnect point on the ET following the tank's separation from the orbiter after launch. The Kodak camera will record 24 images, at one frame per 1.5 seconds, on a flash memory card. After orbital insertion, the crew will transfer the images from the memory card to a laptop computer. The files will then be downloaded through the Ku-band system to the Mission Control Center in Houston for analysis.

KSC-05PD-0564

NASA Technical Reports Server (NTRS)

2005-01-01

KENNEDY SPACE CENTER, FLA. In the Vehicle Assembly Building at NASAs Kennedy Space Center, a worker mounts a digital still camera in the External Tank (ET) umbilical well on the aft end of Space Shuttle Discovery. The camera is being used to obtain and downlink high-resolution images of the disconnect point on the ET following the ET separation from the orbiter after launch. The Kodak camera will record 24 images, at one frame per 1.5 seconds, on a flash memory card. After orbital insertion, the crew will transfer the images from the memory card to a laptop computer. The files will then be downloaded through the Ku-band system to the Mission Control Center in Houston for analysis.

KSC-05PD-0561

NASA Technical Reports Server (NTRS)

2005-01-01

KENNEDY SPACE CENTER, FLA. In the Vehicle Assembly Building at NASAs Kennedy Space Center, workers prepare a digital still camera they will mount in the External Tank (ET) umbilical well on the aft end of Space Shuttle Discovery. The camera is being used to obtain and downlink high-resolution images of the disconnect point on the ET following its separation from the orbiter after launch. The Kodak camera will record 24 images, at one frame per 1.5 seconds, on a flash memory card. After orbital insertion, the crew will transfer the images from the memory card to a laptop computer. The files will then be downloaded through the Ku-band system to the Mission Control Center in Houston for analysis.

KSC-05PD-0563

NASA Technical Reports Server (NTRS)

2005-01-01

KENNEDY SPACE CENTER, FLA. In the Vehicle Assembly Building at NASAs Kennedy Space Center, workers prepare a digital still camera they will mount in the External Tank (ET) umbilical well on the aft end of Space Shuttle Discovery. The camera is being used to obtain and downlink high-resolution images of the disconnect point on the ET following the ET separation from the orbiter after launch. The Kodak camera will record 24 images, at one frame per 1.5 seconds, on a flash memory card. After orbital insertion, the crew will transfer the images from the memory card to a laptop computer. The files will then be downloaded through the Ku-band system to the Mission Control Center in Houston for analysis.

Line drawing Scientific Instrument Module and lunar orbital science package

NASA Technical Reports Server (NTRS)

1970-01-01

A line drawing of the Scientific Instrument Module (SIM) with its lunar orbital science package. The SIM will be mounted in a previously vacant sector of the Apollo Service Module. It will carry specialized cameras and instrumentation for gathering lunar orbit scientific data.

KENNEDY SPACE CENTER, FLA. - NASA Vehicle Manager Scott Thurston (facing camera) talks to the media in the Orbiter Processing Facility. The media was invited to see the orbiter Atlantis as it is being prepared for Return to Flight. Both local and national reporters representing print and TV networks were able to see work in progress on Atlantis, including the reinstallation of the Reinforced Carbon-Carbon panels on the orbiter’s wing leading edge; wiring inspections; and checks of the engines in the Orbital Maneuvering System.

NASA Image and Video Library

2003-09-26

KENNEDY SPACE CENTER, FLA. - NASA Vehicle Manager Scott Thurston (facing camera) talks to the media in the Orbiter Processing Facility. The media was invited to see the orbiter Atlantis as it is being prepared for Return to Flight. Both local and national reporters representing print and TV networks were able to see work in progress on Atlantis, including the reinstallation of the Reinforced Carbon-Carbon panels on the orbiter’s wing leading edge; wiring inspections; and checks of the engines in the Orbital Maneuvering System.

Astronaut Akers packs IMAX camera film roll

NASA Image and Video Library

1996-09-23

STS79-E-5274 (23 September 1996) --- Onboard Spacehab, in the Earth-orbiting Space Shuttle Atlantis, astronaut Thomas D. Akers stows an exposed film can from the IMAX in-cabin camera, during Flight Day 8.

Relative attitude dynamics and control for a satellite inspection mission

NASA Astrophysics Data System (ADS)

Horri, Nadjim M.; Kristiansen, Kristian U.; Palmer, Phil; Roberts, Mark

2012-02-01

The problem of conducting an inspection mission from a chaser satellite orbiting a target spaceraft is considered. It is assumed that both satellites follow nearly circular orbits. The relative orbital motion is described by the Hill-Clohessy-Wiltshire equation. In the case of an elliptic relative orbit, it is shown that an inspection mission is feasible when the chaser is inertially pointing, provided that the camera mounted on the chaser satellite has sufficiently large field of view. The same possibility is shown when the optical axis of the chaser's camera points in, or opposite to, the tangential direction of the local vertical local horizontal frame. For an arbitrary relative orbit and arbitrary initial conditions, the concept of relative Euler angles is defined for this inspection mission. The expression of the desired relative angular velocity vector is derived as a function of Cartesian coordinates of the relative orbit. A quaternion feedback controller is then designed and shown to perform relative attitude control with admissible internal torques. Three different types of relative orbits are considered, namely the elliptic, Pogo and drifting relative orbits. Measurements of the relative orbital motion are assumed to be available from optical navigation.

Coregistration of high-resolution Mars orbital images

NASA Astrophysics Data System (ADS)

Sidiropoulos, Panagiotis; Muller, Jan-Peter

2015-04-01

The systematic orbital imaging of the Martian surface started 4 decades ago from NASA's Viking Orbiter 1 & 2 missions, which were launched in August 1975, and acquired orbital images of the planet between 1976 and 1980. The result of this reconnaissance was the first medium-resolution (i.e. ≤ 300m/pixel) global map of Mars, as well as a variety of high-resolution images (reaching up to 8m/pixel) of special regions of interest. Over the last two decades NASA has sent 3 more spacecraft with onboard instruments for high-resolution orbital imaging: Mars Global Surveyor (MGS) having onboard the Mars Orbital Camera - Narrow Angle (MOC-NA), Mars Odyssey having onboard the Thermal Emission Imaging System - Visual (THEMIS-VIS) and the Mars Reconnaissance Orbiter (MRO) having on board two distinct high-resolution cameras, Context Camera (CTX) and High-Resolution Imaging Science Experiment (HiRISE). Moreover, ESA has the multispectral High resolution Stereo Camera (HRSC) onboard ESA's Mars Express with resolution up to 12.5m since 2004. Overall, this set of cameras have acquired more than 400,000 high-resolution images, i.e. with resolution better than 100m and as fine as 25 cm/pixel. Notwithstanding the high spatial resolution of the available NASA orbital products, their accuracy of areo-referencing is often very poor. As a matter of fact, due to pointing inconsistencies, usually form errors in roll attitude, the acquired products may actually image areas tens of kilometers far away from the point that they are supposed to be looking at. On the other hand, since 2004, the ESA Mars Express has been acquiring stereo images through the High Resolution Stereo Camera (HRSC), with resolution that is usually 12.5-25 metres per pixel. The achieved coverage is more than 64% for images with resolution finer than 20 m/pixel, while for ~40% of Mars, Digital Terrain Models (DTMs) have been produced with are co-registered with MOLA [Gwinner et al., 2010]. The HRSC images and DTMs represent the best available 3D reference frame for Mars showing co-registration with MOLA<25m (loc.cit.). In our work, the reference generated by HRSC terrain corrected orthorectified images is used as a common reference frame to co-register all available high-resolution orbital NASA products into a common 3D coordinate system, thus allowing the examination of the changes that happen on the surface of Mars over time (such as seasonal flows [McEwen et al., 2011] or new impact craters [Byrne, et al., 2009]). In order to accomplish such a tedious manual task, we have developed an automatic co-registration pipeline that produces orthorectified versions of the NASA images in realistic time (i.e. from ~15 minutes to 10 hours per image depending on size). In the first step of this pipeline, tie-points are extracted from the target NASA image and the reference HRSC image or image mosaic. Subsequently, the HRSC areo-reference information is used to transform the HRSC tie-points pixel coordinates into 3D "world" coordinates. This way, a correspondence between the pixel coordinates of the target NASA image and the 3D "world" coordinates is established for each tie-point. This set of correspondences is used to estimate a non-rigid, 3D to 2D transformation model, which transforms the target image into the HRSC reference coordinate system. Finally, correlation of the transformed target image and the HRSC image is employed to fine-tune the orthorectification results, thus generating results with sub-pixel accuracy. This method, which has been proven to be accurate, robust to resolution differences and reliable when dealing with partially degraded data and fast, will be presented, along with some example co-registration results that have been achieved by using it. Acknowledgements: The research leading to these results has received partial funding from the STFC "MSSL Consolidated Grant" ST/K000977/1 and partial support from the European Union's Seventh Framework Programme (FP7/2007-2013) under iMars grant agreement n° 607379. References: [1] K. F. Gwinner, et al. (2010) Topography of Mars from global mapping by HRSC high-resolution digital terrain models and orthoimages: characteristics and performance. Earth and Planetary Science Letters 294, 506-519, doi:10.1016/j.epsl.2009.11.007. [2] A. McEwen, et al. (2011) Seasonal flows on warm martian slopes. Science , 333 (6043): 740-743. [3] S. Byrne, et al. (2009) Distribution of mid-latitude ground ice on mars from new impact craters. Science, 325(5948):1674-1676.

Sirenum Fossae Trough

NASA Technical Reports Server (NTRS)

2000-01-01

[figure removed for brevity, see original site]

The Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) orbits the red planet twelve times each day. The number of pictures that MOC can take varies from orbit to orbit, depending upon whether the data are being stored in MGS's onboard tape recorder for playback at a later time, or whether the data are being sent directly back to Earth via a real-time radio link. More data can be acquired during orbits with real-time downlink.

During real-time orbits, the MOC team often will take a few random or semi-random pictures in between the carefully-selected, hand-targeted images. On rare occasions, one of these random pictures will surprise the MOC team. The picture shown here is an excellent example, because the high resolution view (top) is centered so nicely on a trough and an adjacent, shallow crater that it is as if someone very carefully selected the target for MOC. The high-resolution view covers an area only 1.1 km (0.7 mi) wide by 2.3 km (1.4 mi) long. Hitting a target such as this with such a small image is very difficult to do, on purpose, because there are small uncertainties in the predicted orbit, the maps used to select targets, and the minor adjustments of spacecraft pointing at any given moment. Nevertheless, a very impressive image was received.

The high resolution view crosses one of the troughs of the Sirenum Fossae near 31.2oS, 152.3oW. The context image (above) was acquired at the same time as the high resolution view on July 23, 2000. The small white box shows the location of the high resolution picture. The lines running diagonally across the context image from upper right toward lower left are the Sirenum Fossae troughs, formed by faults that are radial to the volcanic region of Tharsis. Both pictures are illuminated from the upper left. The scene shows part of the martian southern hemisphere nearly autumn.

Stray light lessons learned from the Mars reconnaissance orbiter's optical navigation camera

NASA Astrophysics Data System (ADS)

Lowman, Andrew E.; Stauder, John L.

2004-10-01

The Optical Navigation Camera (ONC) is a technical demonstration slated to fly on NASA"s Mars Reconnaissance Orbiter in 2005. Conventional navigation methods have reduced accuracy in the days immediately preceding Mars orbit insertion. The resulting uncertainty in spacecraft location limits rover landing sites to relatively safe areas, away from interesting features that may harbor clues to past life on the planet. The ONC will provide accurate navigation on approach for future missions by measuring the locations of the satellites of Mars relative to background stars. Because Mars will be a bright extended object just outside the camera"s field of view, stray light control at small angles is essential. The ONC optomechanical design was analyzed by stray light experts and appropriate baffles were implemented. However, stray light testing revealed significantly higher levels of light than expected at the most critical angles. The primary error source proved to be the interface between ground glass surfaces (and the paint that had been applied to them) and the polished surfaces of the lenses. This paper will describe troubleshooting and correction of the problem, as well as other lessons learned that affected stray light performance.

On-orbit Passive Thermography

NASA Technical Reports Server (NTRS)

Howell, Patricia A.; Winfree, William P.; Cramer, K. Elliott

2008-01-01

On July 12, 2006, British-born astronaut Piers Sellers became the first person to conduct thermal nondestructive evaluation experiments in space, demonstrating the feasibility of a new tool for detecting damage to the reinforced carbon-carbon (RCC) structures of the Shuttle. This new tool was an EVA (Extravehicular Activity, or spacewalk) compatible infrared camera developed by NASA engineers. Data was collected both on the wing leading edge of the Orbiter and on pre-damaged samples mounted in the Shuttle s cargo bay. A total of 10 infrared movies were collected during the EVA totaling over 250 megabytes of data. Images were downloaded from the orbiting Shuttle to Johnson Space Center for analysis and processing. Results are shown to be comparable to ground-based thermal inspections performed in the laboratory with the same type of camera and simulated solar heating. The EVA camera system detected flat-bottom holes as small as 2.54cm in diameter with 50% material loss from the back (hidden) surface in RCC during this first test of the EVA IR Camera. Data for the time history of the specimen temperature and the capability of the inspection system for imaging impact damage are presented.

Orbit analysis of a bright Southern sigma Sagittariids fireball

NASA Astrophysics Data System (ADS)

Koukal, Jakub

2018-02-01

During twilight on June 14, 2017, CEMeNt network cameras recorded a long and bright fireball with an absolute magnitude of -7.9 ± 0.2m, whose atmospheric path began over the northwest of Romania and ended up above southern Poland. This fireball belongs to the Southern sigma Sagittariids meteor shower and was recorded from 9 cameras of the CEMeNt network. The atmospheric path of the fireball as well as the heliocentric orbit of the meteoroid are analyzed in this article.

THE MARS ORBITER CAMERA IS INSTALLED ON THE MARS GLOBAL SURVEYOR

NASA Technical Reports Server (NTRS)

1996-01-01

In the Payload Hazardous Servicing Facility at KSC, installation is under way of the Mars Orbiter Camera (MOC) on the Mars Global Surveyor spacecraft. The MOC is one of a suite of six scientific instruments that will gather data during a two-year period about Martian topography, mineral distribution and weather. The Mars Global Surveyor is slated for launch aboard a Delta II expendable launch vehicle on November 6, the beginning of a 20-day launch period.

Clouds over Tharsis

NASA Image and Video Library

1998-03-13

Color composite of condensate clouds over Tharsis made from red and blue images with a synthesized green channel. Mars Orbiter Camera wide angle frames from Orbit 48. http://photojournal.jpl.nasa.gov/catalog/PIA00812

MS Walheim poses with a Hasselblad camera on the flight deck of Atlantis during STS-110

NASA Image and Video Library

2002-04-08

STS110-E-5017 (8 April 2002) --- Astronaut Rex J. Walheim, STS-110 mission specialist, holds a camera on the aft flight deck of the Space Shuttle Atlantis. A blue and white Earth is visible through the overhead windows of the orbiter. The image was taken with a digital still camera.

Wrist Camera Orientation for Effective Telerobotic Orbital Replaceable Unit (ORU) Changeout

NASA Technical Reports Server (NTRS)

Jones, Sharon Monica; Aldridge, Hal A.; Vazquez, Sixto L.

1997-01-01

The Hydraulic Manipulator Testbed (HMTB) is the kinematic replica of the Flight Telerobotic Servicer (FTS). One use of the HMTB is to evaluate advanced control techniques for accomplishing robotic maintenance tasks on board the Space Station. Most maintenance tasks involve the direct manipulation of the robot by a human operator when high-quality visual feedback is important for precise control. An experiment was conducted in the Systems Integration Branch at the Langley Research Center to compare several configurations of the manipulator wrist camera for providing visual feedback during an Orbital Replaceable Unit changeout task. Several variables were considered such as wrist camera angle, camera focal length, target location, lighting. Each study participant performed the maintenance task by using eight combinations of the variables based on a Latin square design. The results of this experiment and conclusions based on data collected are presented.

High resolution imaging science experiment (HiRISE) images of volcanic terrains from the first 6 months of the Mars reconnaissance orbiter primary science phase

USGS Publications Warehouse

Keszthelyi, L.; Jaeger, W.; McEwen, A.; Tornabene, L.; Beyer, R.A.; Dundas, C.; Milazzo, M.

2008-01-01

In the first 6 months of the Mars Reconnaissance Orbiter's Primary Science Phase, the High Resolution Imaging Science Experiment (HiRISE) camera has returned images sampling the diversity of volcanic terrains on Mars. While many of these features were noted in earlier imaging, they are now seen with unprecedented clarity. We find that some volcanic vents produced predominantly effusive products while others generated mostly pyroclastics. Flood lavas were emplaced in both turbulent and gentle eruptions, producing roofed channels and inflation features. However, many areas on Mars are too heavily mantled to allow meter-scale volcanic features to be discerned. In particular, the major volcanic edifices are extensively mantled, though it is possible that some of the mantle is pyroclastic material rather than atmospheric dust. Support imaging by the Context Imager (CTX) and topographic information derived from stereo imaging are both invaluable in interpreting the HiRISE data. Copyright 2008 by the American Geophysical Union.

Exploring Solar System Origins With The Desert Fireball Network

NASA Astrophysics Data System (ADS)

Day, B. H.; Bland, P.

2016-12-01

Fireball camera networks are designed to recover meteorites with orbits. A geological context is a prerequisite for understanding terrestrial rocks. An improved dynamical context would benefit our understanding of extraterrestrial geology. A dozen projects - professional and amateur - have pursued this goal over the years. The effort has yielded 10 meteorites with orbits. Why so few? All these projects were in the temperate zone of the northern hemisphere: areas where meteorite recovery is marginal. Deserts are one of the few places on Earth where field searches for meteorites can be mounted with a realistic chance of success. This was the driver behind the Desert Fireball Network. The Desert Fireball Network (DFN) uses automated observatories across Australia to triangulate trajectories of meteorites entering the atmosphere, determine pre-entry orbits, and pinpoint their fall positions. Each observatory is an autonomous intelligent imaging system, taking 1000×36Megapixel all-sky images throughout the night, using neural network algorithms to recognise events. They are capable of operating for 12 months in a harsh environment, and store all imagery collected. We developed a completely automated software pipeline for data reduction, and built a supercomputer database for storage, allowing us to process our entire archive. We successfully recovered a meteorite from Lake Eyre on 31st December 2015, using this pipeline. By February 2016 we had reduced our complete fireball dataset, deriving precise orbits for >350 events: a dataset that provides a unique window on the dynamics of material in the inner solar system. The DFN currently stands at 50 stations distributed across the Australian continent, covering an area of 2.5 million km2. The fireball and meteorite orbital data that it can provide will deliver a new dynamical window on the inner solar system, and new insights into solar system origins. Working with DFN's partners at NASA's Solar System Exploration Research Virtual Institute, the team is now working to expand the network beyond Australia to locations around the world.

The 1997 Spring Regression of the Martian South Polar Cap: Mars Orbiter Camera Observations

USGS Publications Warehouse

James, P.B.; Cantor, B.A.; Malin, M.C.; Edgett, K.; Carr, M.H.; Danielson, G.E.; Ingersoll, A.P.; Davies, M.E.; Hartmann, W.K.; McEwen, A.S.; Soderblom, L.A.; Thomas, P.C.; Veverka, J.

2000-01-01

The Mars Orbiter cameras (MOC) on Mars Global Surveyor observed the south polar cap of Mars during its spring recession in 1997. The images acquired by the wide angle cameras reveal a pattern of recession that is qualitatively similar to that observed by Viking in 1977 but that does differ in at least two respects. The 1977 recession in the 0o to 120o longitude sector was accelerated relative to the 1997 observations after LS = 240o; the Mountains of Mitchel also detached from the main cap earlier in 1997. Comparison of the MOC images with Mars Orbiter Laser Altimeter data shows that the Mountains of Mitchel feature is controlled by local topography. Relatively dark, low albedo regions well within the boundaries of the seasonal cap were observed to have red-to-violet ratios that characterize them as frost units rather than unfrosted or partially frosted ground; this suggests the possibility of regions covered by CO2 frost having different grain sizes.

Geocam Space: Enhancing Handheld Digital Camera Imagery from the International Space Station for Research and Applications

NASA Technical Reports Server (NTRS)

Stefanov, William L.; Lee, Yeon Jin; Dille, Michael

2016-01-01

Handheld astronaut photography of the Earth has been collected from the International Space Station (ISS) since 2000, making it the most temporally extensive remotely sensed dataset from this unique Low Earth orbital platform. Exclusive use of digital handheld cameras to perform Earth observations from the ISS began in 2004. Nadir viewing imagery is constrained by the inclined equatorial orbit of the ISS to between 51.6 degrees North and South latitude, however numerous oblique images of land surfaces above these latitudes are included in the dataset. While unmodified commercial off-the-shelf digital cameras provide only visible wavelength, three-band spectral information of limited quality current cameras used with long (400+ mm) lenses can obtain high quality spatial information approaching 2 meters/ground pixel resolution. The dataset is freely available online at the Gateway to Astronaut Photography of Earth site (http://eol.jsc.nasa.gov), and now comprises over 2 million images. Despite this extensive image catalog, use of the data for scientific research, disaster response, commercial applications and visualizations is minimal in comparison to other data collected from free-flying satellite platforms such as Landsat, Worldview, etc. This is due primarily to the lack of fully-georeferenced data products - while current digital cameras typically have integrated GPS, this does not function in the Low Earth Orbit environment. The Earth Science and Remote Sensing (ESRS) Unit at NASA Johnson Space Center provides training in Earth Science topics to ISS crews, performs daily operations and Earth observation target delivery to crews through the Crew Earth Observations (CEO) Facility on board ISS, and also catalogs digital handheld imagery acquired from orbit by manually adding descriptive metadata and determining an image geographic centerpoint using visual feature matching with other georeferenced data, e.g. Landsat, Google Earth, etc. The lack of full geolocation information native to the data makes it difficult to integrate astronaut photographs with other georeferenced data to facilitate quantitative analysis such as urban land cover/land use classification, change detection, or geologic mapping. The manual determination of image centerpoints is both time and labor-intensive, leading to delays in releasing geolocated and cataloged data to the public, such as the timely use of data for disaster response. The GeoCam Space project was funded by the ISS Program in 2015 to develop an on-orbit hardware and ground-based software system for increasing the efficiency of geolocating astronaut photographs from the ISS (Fig. 1). The Intelligent Robotics Group at NASA Ames Research Center leads the development of both the ground and on-orbit systems in collaboration with the ESRS Unit. The hardware component consists of modified smartphone elements including cameras, central processing unit, wireless Ethernet, and an inertial measurement unit (gyroscopes/accelerometers/magnetometers) reconfigured into a compact unit that attaches to the base of the current Nikon D4 camera - and its replacement, the Nikon D5 - and connects using the standard Nikon peripheral connector or USB port. This provides secondary, side and downward facing cameras perpendicular to the primary camera pointing direction. The secondary cameras observe calibration targets with known internal X, Y, and Z position affixed to the interior of the ISS to determine the camera pose corresponding to each image frame. This information is recorded by the GeoCam Space unit and indexed for correlation to the camera time recorded for each image frame. Data - image, EXIF header, and camera pose information - is transmitted to the ground software system (GeoRef) using the established Ku-band USOS downlink system. Following integration on the ground, the camera pose information provides an initial geolocation estimate for the individual film frame. This new capability represents a significant advance in geolocation from the manual feature-matching approach for both nadir and off-nadir viewing imagery. With the initial geolocation estimate, full georeferencing of an image is completed using the rapid tie-pointing interface in GeoRef, and the resulting data is added to the Gateway to Astronaut Photography of Earth online database in both Geotiff and Keyhole Markup Language (kml) formats. The integration of the GeoRef software component of Geocam Space into the CEO image cataloging workflow is complete, and disaster response imagery acquired by the ISS crew is now fully georeferenced as a standard data product. The on-orbit hardware component (GeoSens) is in final prototyping phase, and is on-schedule for launch to the ISS in late 2016. Installation and routine use of the Geocam Space system for handheld digital camera photography from the ISS is expected to significantly improve the usefulness of this unique dataset for a variety of public- and private-sector applications.

Clementine Images of Earth and Moon

NASA Technical Reports Server (NTRS)

1997-01-01

During its flight and lunar orbit, the Clementine spacecraft returned images of the planet Earth and the Moon. This collection of UVVIS camera Clementine images shows the Earth from the Moon and 3 images of the Earth.

The image on the left shows the Earth as seen across the lunar north pole; the large crater in the foreground is Plaskett. The Earth actually appeared about twice as far above the lunar horizon as shown. The top right image shows the Earth as viewed by the UVVIS camera while Clementine was in transit to the Moon; swirling white cloud patterns indicate storms. The two views of southeastern Africa were acquired by the UVVIS camera while Clementine was in low Earth orbit early in the mission

Slight Blurring in Newer Image from Mars Orbiter

NASA Image and Video Library

2018-02-09

These two frames were taken of the same place on Mars by the same orbiting camera before (left) and after some images from the camera began showing unexpected blur. The images are from the High Resolution Imaging Science Experiment (HiRISE) camera on NASA's Mars Reconnaissance Orbiter. They show a patch of ground about 500 feet or 150 meters wide in Gusev Crater. The one on the left, from HiRISE observation ESP_045173_1645, was taken March 16, 2016. The one on the right was taken Jan. 9, 2018. Gusev Crater, at 15 degrees south latitude and 176 degrees east longitude, is the landing site of NASA's Spirit Mars rover in 2004 and a candidate landing site for a rover to be launched in 2020. HiRISE images provide important information for evaluating potential landing sites. The smallest boulders with measurable diameters in the left image are about 3 feet (90 centimeters) wide. In the blurred image, the smallest measurable are about double that width. As of early 2018, most full-resolution images from HiRISE are not blurred, and the cause of the blur is still under investigation. Even before blurred images were first seen, in 2017, observations with HiRISE commonly used a technique that covers more ground area at half the resolution. This shows features smaller than can be distinguished with any other camera orbiting Mars, and little blurring has appeared in these images. https://photojournal.jpl.nasa.gov/catalog/PIA22215

A view of the ET camera on STS-112

NASA Technical Reports Server (NTRS)

2002-01-01

KENNEDY SPACE CENTER, FLA. - A view of the camera mounted on the external tank of Space Shuttle Atlantis. The color video camera mounted to the top of Atlantis' external tank will provide a view of the front and belly of the orbiter and a portion of the solid rocket boosters (SRBs) and external tank during the launch of Atlantis on mission STS-112. It will offer the STS-112 team an opportunity to monitor the shuttle's performance from a new angle. The camera will be turned on fifteen minutes prior to launch and will show the orbiter and solid rocket boosters on the launch pad. The video will be downlinked from the external tank during flight to several NASA data-receiving sites and then relayed to the live television broadcast. The camera is expected to operate for about 15 minutes following liftoff. At liftoff, viewers will see the shuttle clearing the launch tower and, at two minutes after liftoff, see the right SRB separate from the external tank. When the external tank separates from Atlantis about eight minutes into the flight, the camera is expected to continue its live feed for about six more minutes although NASA may be unable to pick up the camera's signal because the tank may have moved out of range.

A view of the ET camera on STS-112

NASA Technical Reports Server (NTRS)

2002-01-01

KENNEDY SPACE CENTER, FLA. - A closeup view of the camera mounted on the external tank of Space Shuttle Atlantis. The color video camera mounted to the top of Atlantis' external tank will provide a view of the front and belly of the orbiter and a portion of the solid rocket boosters (SRBs) and external tank during the launch of Atlantis on mission STS-112. It will offer the STS-112 team an opportunity to monitor the shuttle's performance from a new angle. The camera will be turned on fifteen minutes prior to launch and will show the orbiter and solid rocket boosters on the launch pad. The video will be downlinked from the external tank during flight to several NASA data-receiving sites and then relayed to the live television broadcast. The camera is expected to operate for about 15 minutes following liftoff. At liftoff, viewers will see the shuttle clearing the launch tower and, at two minutes after liftoff, see the right SRB separate from the external tank. When the external tank separates from Atlantis about eight minutes into the flight, the camera is expected to continue its live feed for about six more minutes although NASA may be unable to pick up the camera's signal because the tank may have moved out of range.

STS-52 MS Shepherd during camera equipment training on JSC's Bldg 1 rooftop

NASA Technical Reports Server (NTRS)

1992-01-01

STS-52 Columbia, Orbiter Vehicle (OV) 102, Mission Specialist (MS) William M. Shepherd aims a 35mm camera at a distant subject from his vantage point atop the roof of JSC's nine-story Project Management Building Bldg 1. The training session familiarized Shepherd with camera equipment to be used in Earth observation documentation during STS-52.

First results from the TOPSAT camera

NASA Astrophysics Data System (ADS)

Greenway, Paul; Tosh, Ian; Morris, Nigel; Burton, Gary; Cawley, Steve

2017-11-01

The TopSat camera is a low cost remote sensing imager capable of producing 2.5 metre resolution panchromatic imagery, funded by the British National Space Centre's Mosaic programme. The instrument was designed and assembled at the Space Science & Technology Department of the CCLRC's Rutherford Appleton Laboratory (RAL) in the UK, and was launched on the 27th October 2005 from Plesetsk Cosmodrome in Northern Russia on a Kosmos-3M. The camera utilises an off-axis three mirror system, which has the advantages of excellent image quality over a wide field of view, combined with a compactness that makes its overall dimensions smaller than its focal length. Keeping the costs to a minimum has been a major design driver in the development of this camera. The camera is part of the TopSat mission, which is a collaboration between four UK organisations; QinetiQ, Surrey Satellite Technology Ltd (SSTL), RAL and Infoterra. Its objective is to demonstrate provision of rapid response high resolution imagery to fixed and mobile ground stations using a low cost minisatellite. The paper "Development of the TopSat Camera" presented by RAL at the 5th ICSO in 2004 described the opto-mechanical design, assembly, alignment and environmental test methods implemented. Now that the spacecraft is in orbit and successfully acquiring images, this paper presents the first results from the camera and makes an initial assessment of the camera's in-orbit performance.

Tenth Anniversary Image from Camera on NASA Mars Orbiter

NASA Image and Video Library

2012-02-29

NASA Mars Odyssey spacecraft captured this image on Feb. 19, 2012, 10 years to the day after the camera recorded its first view of Mars. This image covers an area in the Nepenthes Mensae region north of the Martian equator.

Removal of instrument signature from Mariner 9 television images of Mars

NASA Technical Reports Server (NTRS)

Green, W. B.; Jepsen, P. L.; Kreznar, J. E.; Ruiz, R. M.; Schwartz, A. A.; Seidman, J. B.

1975-01-01

The Mariner 9 spacecraft was inserted into orbit around Mars in November 1971. The two vidicon camera systems returned over 7300 digital images during orbital operations. The high volume of returned data and the scientific objectives of the Television Experiment made development of automated digital techniques for the removal of camera system-induced distortions from each returned image necessary. This paper describes the algorithms used to remove geometric and photometric distortions from the returned imagery. Enhancement processing of the final photographic products is also described.

First Results of the Juno Magnetometer Investigation in Jupiter's Magnetosphere

NASA Astrophysics Data System (ADS)

Connerney, J. E. P.; Oliversen, R. J.; Espley, J. R.; Schnurr, R.; Sheppard, D.; Odom, J.; Lawton, P.; Murphy, S.; Joergensen, J. L.; Joergensen, P. S.; Merayo, J. M. G.; Denver, T.; Benn, M.; Bjarno, J. B.; Malinnikova Bang, A.; Bloxham, J.; Smith, E. J.; Bolton, S. J.

2016-12-01

The Juno spacecraft entered polar orbit about Jupiter on July 4, 2016, after a picture perfect Jupiter Orbit Insertion (JOI) main engine burn lasting 35 minutes. Juno's science instruments were not powered during the critical maneuver sequence ( 5 days) but were fully operational shortly afterward. The 53.5-day capture orbit provides Juno's science instruments with the first opportunity to sample the Jovian environment close up and in polar orbit on August 27, 2016 (PJ1). Following a successful PJ1, a period reduction maneuver (PRM) will drop the spacecraft into its 14-day science orbit to begin the science phase of the mission. During this phase, the gravity and magnetic fields will be mapped with unprecedented accuracy as Juno conducts a study of Jupiter's interior structure and composition, in addition to the first comprehensive exploration of the polar magnetosphere. The magnetic field investigation onboard Juno is equipped with two magnetometer sensor suites, located at 10 and 12 m from the spacecraft body at the end of one of the three solar panel wings. Each contains a vector fluxgate magnetometer (FGM) sensor and a pair of co-located non-magnetic star tracker camera heads which provide accurate attitude determination for the FGM sensors. This very capable magnetic observatory samples the Jovian magnetic field at a rate of up to 64 vector samples/second. We present the first observations of Jupiter's magnetic field obtained in polar orbit and in context with prior observations and those acquired by Juno's other science instruments (waves and particles instruments, and remote-sensing infrared and ultraviolet imaging spectrographs).

Space Telescope maintenance and refurbishment

NASA Technical Reports Server (NTRS)

Trucks, H. F.

1983-01-01

The Space Telescope (ST) represents a new concept regarding spaceborne astronomical observatories. Maintenance crews will be brought to the orbital worksite to make repairs and replace scientific instruments. For major overhauls the telescope can be temporarily returned to earth with the aid of the Shuttle. It will, thus, be possible to conduct astronomical studies with the ST for two decades or more. The five first-generation scientific instruments used with the ST include a wide field/planetary camera, a faint object camera, a faint object spectrograph, a high resolution spectrograph, and a high speed photometer. Attention is given to the optical telescope assembly, the support systems module, aspects of mission and science operations, unscheduled maintenance, contingency orbital maintenance, planned on-orbit maintenance, ground maintenance, ground refurbishment, and ground logistics.

STS-36 Mission Specialist Hilmers with AEROLINHOF camera on aft flight deck

NASA Image and Video Library

1990-03-03

STS-36 Mission Specialist (MS) David C. Hilmers points the large-format AEROLINHOF camera out overhead window W7 on the aft flight deck of Atlantis, Orbiter Vehicle (OV) 104. Hilmers records Earth imagery using the camera. Hilmers and four other astronauts spent four days, 10 hours and 19 minutes aboard OV-104 for the Department of Defense (DOD) devoted mission.

STS-32 Mission Specialist (MS) Ivins peers into IMAX camera viewfinder

NASA Technical Reports Server (NTRS)

1989-01-01

STS-32 Mission Specialist (MS) Marsha S. Ivins looks through IMAX camera viewfinder during briefing and training session conducted in the JSC Mockup and Integration Laboratory (MAIL) Bldg 9B. Technicians on either side of Ivins are ready to assist with the training activity. The IMAX camera will be used onboard Columbia, Orbiter Vehicle (OV) 102, during the STS-32 mission.

Clementine Images of Earth and Moon

NASA Image and Video Library

1999-06-12

During its flight and lunar orbit, NASA’s Clementine spacecraft returned images of the planet Earth and the Moon. This collection of UVVIS camera Clementine images shows the Earth from the Moon and 3 images of the Earth. The image on the left shows the Earth as seen across the lunar north pole; the large crater in the foreground is Plaskett. The Earth actually appeared about twice as far above the lunar horizon as shown. The top right image shows the Earth as viewed by the UVVIS camera while Clementine was in transit to the Moon; swirling white cloud patterns indicate storms. The two views of southeastern Africa were acquired by the UVVIS camera while Clementine was in low Earth orbit early in the mission. http://photojournal.jpl.nasa.gov/catalog/PIA00432

Cloud formation over South America - fifth orbit pass

NASA Image and Video Library

1962-10-03

S62-06612 (3 Oct. 1962) --- Cloud formation over South America taken during the fifth orbit pass of the Mercury-Atlas 8 (MA-8) mission by astronaut Walter M. Schirra Jr. with a hand-held camera. Photo credit: NASA

Oblique View of Victoria Crater

NASA Image and Video Library

2009-08-12

This image of Victoria Crater in the Meridiani Planum region of Mars was taken by the High Resolution Imaging Science Experiment HiRISE camera on NASA Mars Reconnaissance Orbiter at more of a sideways angle than earlier orbital images of this crater.

NICMOS Focus and HST Breathing

NASA Astrophysics Data System (ADS)

Suchkov, A.; Hershey, J.

1998-09-01

The program 7608 monitored on a biweekly basis NICMOS camera foci from June 9, 1997, through February 18, 1998. Each of the biweekly observations included 17 measurements of focus position (focus sweeps), individually for each of the three cameras. The measurements for camera 1 and camera 3 foci covered one or two HST orbital periods. Comparison of these measurements with the predictions of the three OTA focus breathing models has shown the following. (1). Focus variations seen in NICMOS focus sweeps correlate well with the OTA focus thermal breathing as predicted by breathing models (“4- temperature”, “full-temperature”, and “attitude” models). Thus they can be attributed mostly to the HST orbital temperature variation. (2). The amount of breathing (breathing amplitude) has been found to be on average larger in the first orbit after a telescope slew to a new target. This is explained as being due to additional thermal perturbations caused by the change in the HST attitude as the telescope repoints to a new target. (3). In the first orbit, the amount of focus change predicted by the 4-temperature model is about the same as that seen in the focus sweeps data (breathing scale factor ~1). However the full-temperature model predicts a two times smaller breathing amplitude (breathing scale factor ~1.7). This suggests that the light shield temperatures are more responsive to the attitude change than temperatures from the other temperature sensors. The results of this study may help to better understand the HST thermal cycles and to improve the models describing the impact of those on both the OTA and NICMOS focus.

Astronaut Alan Bean looks over data acquisition camera on Skylab trainer

NASA Technical Reports Server (NTRS)

1972-01-01

Astronaut Alan L. Bean, commander for Skylab 3, the second manned Skylab mission, looks over the data acquisition camera mounted on the water tank in the upper level of the Orbital Workshop (OWS) one-G trainer at the Manned Spacecraft Center (MSC).

SHUTTLE - PAYLOADS (STS-41G) - KSC

NASA Image and Video Library

1984-10-05

Payload canister transporter in Vertical Processing Facility Clean Room loaded with Earth Radiation Budget Experiment (ERBS), Large Format Camera (LFC), and Orbital Reservicing System (ORS) for STS-41G Mission. 1. STS-41G - EXPERIMENTS 2. CAMERAS - LFC KSC, FL Also available in 4x5 CN

Absolute orbit determination using line-of-sight vector measurements between formation flying spacecraft

NASA Astrophysics Data System (ADS)

Ou, Yangwei; Zhang, Hongbo; Li, Bin

2018-04-01

The purpose of this paper is to show that absolute orbit determination can be achieved based on spacecraft formation. The relative position vectors expressed in the inertial frame are used as measurements. In this scheme, the optical camera is applied to measure the relative line-of-sight (LOS) angles, i.e., the azimuth and elevation. The LIDAR (Light radio Detecting And Ranging) or radar is used to measure the range and we assume that high-accuracy inertial attitude is available. When more deputies are included in the formation, the formation configuration is optimized from the perspective of the Fisher information theory. Considering the limitation on the field of view (FOV) of cameras, the visibility of spacecraft and the installation of cameras are investigated. In simulations, an extended Kalman filter (EKF) is used to estimate the position and velocity. The results show that the navigation accuracy can be enhanced by using more deputies and the installation of cameras significantly affects the navigation performance.

Earth elevation map production and high resolution sensing camera imaging analysis

NASA Astrophysics Data System (ADS)

Yang, Xiubin; Jin, Guang; Jiang, Li; Dai, Lu; Xu, Kai

2010-11-01

The Earth's digital elevation which impacts space camera imaging has prepared and imaging has analysed. Based on matching error that TDI CCD integral series request of the speed of image motion, statistical experimental methods-Monte Carlo method is used to calculate the distribution histogram of Earth's elevation in image motion compensated model which includes satellite attitude changes, orbital angular rate changes, latitude, longitude and the orbital inclination changes. And then, elevation information of the earth's surface from SRTM is read. Earth elevation map which produced for aerospace electronic cameras is compressed and spliced. It can get elevation data from flash according to the shooting point of latitude and longitude. If elevation data between two data, the ways of searching data uses linear interpolation. Linear interpolation can better meet the rugged mountains and hills changing requests. At last, the deviant framework and camera controller are used to test the character of deviant angle errors, TDI CCD camera simulation system with the material point corresponding to imaging point model is used to analyze the imaging's MTF and mutual correlation similarity measure, simulation system use adding cumulation which TDI CCD imaging exceeded the corresponding pixel horizontal and vertical offset to simulate camera imaging when stability of satellite attitude changes. This process is practicality. It can effectively control the camera memory space, and meet a very good precision TDI CCD camera in the request matches the speed of image motion and imaging.

Astronaut Bean - Acrobatics - Orbital Workshop (OWS)

NASA Image and Video Library

1973-08-20

S73-32632 (19 Aug. 1973) --- Astronaut Alan L. Bean, Skylab 3 commander, performs acrobatics and simulated gymnastics in the dome area of the Orbital Workshop in this photographic reproduction taken from a television transmission made by a color TV camera aboard the Skylab space station in Earth orbit. Bean appears to be floating in a diving position. Photo credit: NASA

Orbital docking system centerline color television camera system test

NASA Technical Reports Server (NTRS)

Mongan, Philip T.

1993-01-01

A series of tests was run to verify that the design of the centerline color television camera (CTVC) system is adequate optically for the STS-71 Space Shuttle Orbiter docking mission with the Mir space station. In each test, a mockup of the Mir consisting of hatch, docking mechanism, and docking target was positioned above the Johnson Space Center's full fuselage trainer, which simulated the Orbiter with a mockup of the external airlock and docking adapter. Test subjects viewed the docking target through the CTVC under 30 different lighting conditions and evaluated target resolution, field of view, light levels, light placement, and methods of target alignment. Test results indicate that the proposed design will provide adequate visibility through the centerline camera for a successful docking, even with a reasonable number of light failures. It is recommended that the flight deck crew have individual switching capability for docking lights to provide maximum shadow management and that centerline lights be retained to deal with light failures and user preferences. Procedures for light management should be developed and target alignment aids should be selected during simulated docking runs.

Using Engineering Cameras on Mars Landers and Rovers to Retrieve Atmospheric Dust Loading

NASA Astrophysics Data System (ADS)

Wolfe, C. A.; Lemmon, M. T.

2014-12-01

Dust in the Martian atmosphere influences energy deposition, dynamics, and the viability of solar powered exploration vehicles. The Viking, Pathfinder, Spirit, Opportunity, Phoenix, and Curiosity landers and rovers each included the ability to image the Sun with a science camera that included a neutral density filter. Direct images of the Sun provide the ability to measure extinction by dust and ice in the atmosphere. These observations have been used to characterize dust storms, to provide ground truth sites for orbiter-based global measurements of dust loading, and to help monitor solar panel performance. In the cost-constrained environment of Mars exploration, future missions may omit such cameras, as the solar-powered InSight mission has. We seek to provide a robust capability of determining atmospheric opacity from sky images taken with cameras that have not been designed for solar imaging, such as lander and rover engineering cameras. Operational use requires the ability to retrieve optical depth on a timescale useful to mission planning, and with an accuracy and precision sufficient to support both mission planning and validating orbital measurements. We will present a simulation-based assessment of imaging strategies and their error budgets, as well as a validation based on archival engineering camera data.

KSC-02pd1374

NASA Image and Video Library

2002-09-26

KENNEDY SPACE CENTER, FLA. - A view of the camera mounted on the external tank of Space Shuttle Atlantis. The color video camera mounted to the top of Atlantis' external tank will provide a view of the front and belly of the orbiter and a portion of the solid rocket boosters (SRBs) and external tank during the launch of Atlantis on mission STS-112. It will offer the STS-112 team an opportunity to monitor the shuttle's performance from a new angle. The camera will be turned on fifteen minutes prior to launch and will show the orbiter and solid rocket boosters on the launch pad. The video will be downlinked from the external tank during flight to several NASA data-receiving sites and then relayed to the live television broadcast. The camera is expected to operate for about 15 minutes following liftoff. At liftoff, viewers will see the shuttle clearing the launch tower and, at two minutes after liftoff, see the right SRB separate from the external tank. When the external tank separates from Atlantis about eight minutes into the flight, the camera is expected to continue its live feed for about six more minutes although NASA may be unable to pick up the camera's signal because the tank may have moved out of range.

KSC-02pd1376

NASA Image and Video Library

2002-09-26

KENNEDY SPACE CENTER, FLA. - A closeup view of the camera mounted on the external tank of Space Shuttle Atlantis. The color video camera mounted to the top of Atlantis' external tank will provide a view of the front and belly of the orbiter and a portion of the solid rocket boosters (SRBs) and external tank during the launch of Atlantis on mission STS-112. It will offer the STS-112 team an opportunity to monitor the shuttle's performance from a new angle. The camera will be turned on fifteen minutes prior to launch and will show the orbiter and solid rocket boosters on the launch pad. The video will be downlinked from the external tank during flight to several NASA data-receiving sites and then relayed to the live television broadcast. The camera is expected to operate for about 15 minutes following liftoff. At liftoff, viewers will see the shuttle clearing the launch tower and, at two minutes after liftoff, see the right SRB separate from the external tank. When the external tank separates from Atlantis about eight minutes into the flight, the camera is expected to continue its live feed for about six more minutes although NASA may be unable to pick up the camera's signal because the tank may have moved out of range.

KSC-02pd1375

NASA Image and Video Library

2002-09-26

KENNEDY SPACE CENTER, FLA. - A closeup view of the camera mounted on the external tank of Space Shuttle Atlantis. The color video camera mounted to the top of Atlantis' external tank will provide a view of the front and belly of the orbiter and a portion of the solid rocket boosters (SRBs) and external tank during the launch of Atlantis on mission STS-112. It will offer the STS-112 team an opportunity to monitor the shuttle's performance from a new angle. The camera will be turned on fifteen minutes prior to launch and will show the orbiter and solid rocket boosters on the launch pad. The video will be downlinked from the external tank during flight to several NASA data-receiving sites and then relayed to the live television broadcast. The camera is expected to operate for about 15 minutes following liftoff. At liftoff, viewers will see the shuttle clearing the launch tower and, at two minutes after liftoff, see the right SRB separate from the external tank. When the external tank separates from Atlantis about eight minutes into the flight, the camera is expected to continue its live feed for about six more minutes although NASA may be unable to pick up the camera's signal because the tank may have moved out of range.

Planet Four: Terrains - Pointing the Highest Resolution Camera Ever Sent to Mars with the Help of 10,000 Earthlings

NASA Astrophysics Data System (ADS)

Schwamb, Megan Elizabeth; Aye, Klaus-Michael; Portyankina, Ganna; Hansen, Candice; Lintott, Chris; Carstensen, Brian; Duca, Simone; Parrish, Michael; Miller, Grant

2016-10-01

Mars' south pole is sculpted by the never-ending cycle of freezing and thawing of exposed carbon dioxide ice. In the summer, carbon dioxide jets loft dust and dirt through cracks in the thawing carbon dioxide ice sheet to the surface where winds blow the material into the hundreds of thousands of dark fans observed from orbit. Built with the Zooniverse's project builder platform (http://www.zooniverse.org/lab), Planet Four: Terrains (http://terrains.planetfour.org/) is a citizen science project enlisting the general public to review mid-resolution Mars Reconnaissance Orbiter (MRO) Context Camera subimages to identify the channels and pits (dubbed araneiforms) carved during the gas jet formation process, as well as other surface features including craters and carbon dioxide ice pits dubbed 'swiss cheese terrain.'One of the key goals of the project was to identify jet locations on the Martian south pole and create a set of new targets regions for further detailed monitoring over the next southern Spring and Summer with MRO's HiRISE (High Resolution Imaging Experiment) camera. HiRISE has ~20x higher resolution than CTX, while CTX on the other hand covers more area in a single observation. In less than a year, thanks to the effort of over 10,000 volunteers worldwide, Planet Four: Terrains was able to categorize ~20,000 subimages from 90 CTX images, and identify 20+ regions selected for further HiRISE monitoring to explore the on-going seasonal processes.We present an overview of Planet Four: Terrains including the project's goals and public engagement. We will also present a summary of the over 20 target regions selected for HiRISE monitoring.Acknowledgements: This work uses data generated via the Zooniverse.org platform, development of which was supported by a Global Impact Award from Google, and by the Alfred P. Sloan Foundation. We also thank theHiRISE and MRO Teams for their help in scheduling and acquiring ourrequested observations.

Study of Pitch Attitude Estimation Using a High-Definition TV (HDTV) Camera on the Japanese Lunar Explorer SELENE (KAGUYA)

NASA Astrophysics Data System (ADS)

Sobue, Shinichi; Yamazaki, Junichi; Matsumoto, Shuichi; Konishi, Hisahiro; Maejima, Hironori; Sasaki, Susumu; Kato, Manabu; Mitsuhashi, Seiji; Tachino, Junichi

The lunar explorer SELENE (also called KAGUYA) carried thirteen scientific mission instruments to reveal the origin and evolution of Moon and to investigate the possible future utilization of Moon. In addition to the scientific instruments, a high-definition TV (HDTV) camera provided by the Japan Broadcasting Corporation (NHK) was carried on KAGUYA to promote public outreach. We usually use housekeeping telemetry data to derive the satellite attitude along with orbital determination and propagated information. However, it takes time to derive this information, since orbital determination and propagation calculation require the use of the orbital model. When a malfunction of the KAGUYA reaction wheel occurred, we could not have correct attitude information. This means that we don’t have a correct orbital determination in timely fashion. However, when we checked HDTV movies, we found that horizon information on the lunar surface derived from HDTV moving images as a horizon sensor was very useful for the detection of the attitude of KAGUYA. We then compared this information with the attitude information derived from orbital telemetry to validate the accuracy of the HDTV derived estimation. As a result of this comparison, there are good pitch attitude estimation using HDTV derived estimation and we could estimate the pitch angle change during the KAGUYA mission operation simplify and quickly. In this study, we show the usefulness of this HDTV camera as a horizon sensor.

Image Relayed by MAVEN Mars Orbiter from Curiosity Mars Rover

NASA Image and Video Library

2014-11-10

The first demonstration of NASA MAVEN Mars orbiter capability to relay data from a Mars surface mission, on Nov. 6, 2014, included this image, taken Oct. 23, 2014, by Curiosity Navigation Camera, showing part of Pahrump Hills outcrop.

Polar Views of Planet Earth.

ERIC Educational Resources Information Center

Brochu, Michel

1983-01-01

In August, 1981, National Aeronautics and Space Administration launched Dynamics Explorer 1 into polar orbit equipped with three cameras built to view the Northern Lights. The cameras can photograph aurora borealis' faint light without being blinded by the earth's bright dayside. Photographs taken by the satellite are provided. (JN)

On-ground and in-orbit characterisation plan for the PLATO CCD normal cameras

NASA Astrophysics Data System (ADS)

Gow, J. P. D.; Walton, D.; Smith, A.; Hailey, M.; Curry, P.; Kennedy, T.

2017-11-01

PLAnetary Transits and Ocillations (PLATO) is the third European Space Agency (ESA) medium class mission in ESA's cosmic vision programme due for launch in 2026. PLATO will carry out high precision un-interrupted photometric monitoring in the visible band of large samples of bright solar-type stars. The primary mission goal is to detect and characterise terrestrial exoplanets and their systems with emphasis on planets orbiting in the habitable zone, this will be achieved using light curves to detect planetary transits. PLATO uses a novel multi- instrument concept consisting of 26 small wide field cameras The 26 cameras are made up of a telescope optical unit, four Teledyne e2v CCD270s mounted on a focal plane array and connected to a set of Front End Electronics (FEE) which provide CCD control and readout. There are 2 fast cameras with high read-out cadence (2.5 s) for magnitude ~ 4-8 stars, being developed by the German Aerospace Centre and 24 normal (N) cameras with a cadence of 25 s to monitor stars with a magnitude greater than 8. The N-FEEs are being developed at University College London's Mullard Space Science Laboratory (MSSL) and will be characterised along with the associated CCDs. The CCDs and N-FEEs will undergo rigorous on-ground characterisation and the performance of the CCDs will continue to be monitored in-orbit. This paper discusses the initial development of the experimental arrangement, test procedures and current status of the N-FEE. The parameters explored will include gain, quantum efficiency, pixel response non-uniformity, dark current and Charge Transfer Inefficiency (CTI). The current in-orbit characterisation plan is also discussed which will enable the performance of the CCDs and their associated N-FEE to be monitored during the mission, this will include measurements of CTI giving an indication of the impact of radiation damage in the CCDs.

IMAX camera (12-IML-1)

NASA Technical Reports Server (NTRS)

1992-01-01

The IMAX camera system is used to record on-orbit activities of interest to the public. Because of the extremely high resolution of the IMAX camera, projector, and audio systems, the audience is afforded a motion picture experience unlike any other. IMAX and OMNIMAX motion picture systems were designed to create motion picture images of superior quality and audience impact. The IMAX camera is a 65 mm, single lens, reflex viewing design with a 15 perforation per frame horizontal pull across. The frame size is 2.06 x 2.77 inches. Film travels through the camera at a rate of 336 feet per minute when the camera is running at the standard 24 frames/sec.

SKYLAB (SL)-4 - CREW TRAINING (ORBITAL WORKSHOP [OWS]) - JSC

NASA Image and Video Library

1973-08-22

S73-32840 (10 Sept. 1973) --- Scientist-astronaut Edward G. Gibson, Skylab 4 science pilot, turns on a switch on the control box of the S190B camera, one of the components of the Earth Resources Experiments Package (EREP). The single lens Earth Terrain Camera takes five-inch photographs. Behind Gibson is the stowed suit of astronaut Gerald P. Carr, commander for the third manned mission. The crew's other member is astronaut William R. Pogue, pilot. The training exercise took place in the Orbital Workshop one-G trainer at Johnson Space Center. Photo credit: NASA

Performance evaluation and clinical applications of 3D plenoptic cameras

NASA Astrophysics Data System (ADS)

Decker, Ryan; Shademan, Azad; Opfermann, Justin; Leonard, Simon; Kim, Peter C. W.; Krieger, Axel

2015-06-01

The observation and 3D quantification of arbitrary scenes using optical imaging systems is challenging, but increasingly necessary in many fields. This paper provides a technical basis for the application of plenoptic cameras in medical and medical robotics applications, and rigorously evaluates camera integration and performance in the clinical setting. It discusses plenoptic camera calibration and setup, assesses plenoptic imaging in a clinically relevant context, and in the context of other quantitative imaging technologies. We report the methods used for camera calibration, precision and accuracy results in an ideal and simulated surgical setting. Afterwards, we report performance during a surgical task. Test results showed the average precision of the plenoptic camera to be 0.90mm, increasing to 1.37mm for tissue across the calibrated FOV. The ideal accuracy was 1.14mm. The camera showed submillimeter error during a simulated surgical task.

Documenting of Geologic Field Activities in Real-Time in Four Dimensions: Apollo 17 as a Case Study for Terrestrial Analogues and Future Exploration

NASA Technical Reports Server (NTRS)

Feist, B.; Bleacher, J. E.; Petro, N. E.; Niles, P. B.

2018-01-01

During the Apollo exploration of the lunar surface, thousands of still images, 16 mm videos, TV footage, samples, and surface experiments were captured and collected. In addition, observations and descriptions of what was observed was radioed to Mission Control as part of standard communications and subsequently transcribed. The archive of this material represents perhaps the best recorded set of geologic field campaigns and will serve as the example of how to conduct field work on other planetary bodies for decades to come. However, that archive of material exists in disparate locations and formats with varying levels of completeness, making it not easily cross-referenceable. While video and audio exist for the missions, it is not time synchronized, and images taken during the missions are not time or location tagged. Sample data, while robust, is not easily available in a context of where the samples were collected, their descriptions by the astronauts are not connected to them, or the video footage of their collection (if available). A more than five year undertaking to reconstruct and reconcile the Apollo 17 mission archive, from launch through splashdown, has generated an integrated record of the entire mission, resulting in searchable, synchronized image, voice, and video data, with geologic context provided at the time each sample was collected. Through www.apollo17.org the documentation of the field investigation conducted by the Apollo 17 crew is presented in chronologic sequence, with additional context provided by high-resolution Lunar Reconnaissance Orbiter Camera (LROC) Narrow Angle Camera (NAC) images and a corresponding digital terrain model (DTM) of the Taurus-Littrow Valley.

Utilizing ISS Camera Systems for Scientific Analysis of Lightning Characteristics and Comparison with ISS-LIS and GLM

NASA Technical Reports Server (NTRS)

Schultz, Christopher J.; Lang, Timothy J.; Leake, Skye; Runco, Mario, Jr.; Blakeslee, Richard J.

2017-01-01

Video and still frame images from cameras aboard the International Space Station (ISS) are used to inspire, educate, and provide a unique vantage point from low-Earth orbit that is second to none; however, these cameras have overlooked capabilities for contributing to scientific analysis of the Earth and near-space environment. The goal of this project is to study how geo referenced video/images from available ISS camera systems can be useful for scientific analysis, using lightning properties as a demonstration.

Geodetic results from ISAGEX data. [for obtaining center of mass coordinates for geodetic camera sites

NASA Technical Reports Server (NTRS)

Marsh, J. G.; Douglas, B. C.; Walls, D. M.

1974-01-01

Laser and camera data taken during the International Satellite Geodesy Experiment (ISAGEX) were used in dynamical solutions to obtain center-of-mass coordinates for the Astro-Soviet camera sites at Helwan, Egypt, and Oulan Bator, Mongolia, as well as the East European camera sites at Potsdam, German Democratic Republic, and Ondrejov, Czechoslovakia. The results are accurate to about 20m in each coordinate. The orbit of PEOLE (i=15) was also determined from ISAGEX data. Mean Kepler elements suitable for geodynamic investigations are presented.

Active 3D camera design for target capture on Mars orbit

NASA Astrophysics Data System (ADS)

Cottin, Pierre; Babin, François; Cantin, Daniel; Deslauriers, Adam; Sylvestre, Bruno

2010-04-01

During the ESA Mars Sample Return (MSR) mission, a sample canister launched from Mars will be autonomously captured by an orbiting satellite. We present the concept and the design of an active 3D camera supporting the orbiter navigation system during the rendezvous and capture phase. This camera aims at providing the range and bearing of a 20 cm diameter canister from 2 m to 5 km within a 20° field-of-view without moving parts (scannerless). The concept exploits the sensitivity and the gating capability of a gated intensified camera. It is supported by a pulsed source based on an array of laser diodes with adjustable amplitude and pulse duration (from nanoseconds to microseconds). The ranging capability is obtained by adequately controlling the timing between the acquisition of 2D images and the emission of the light pulses. Three modes of acquisition are identified to accommodate the different levels of ranging and bearing accuracy and the 3D data refresh rate. To come up with a single 3D image, each mode requires a different number of images to be processed. These modes can be applied to the different approach phases. The entire concept of operation of this camera is detailed with an emphasis on the extreme lighting conditions. Its uses for other space missions and terrestrial applications are also highlighted. This design is implemented in a prototype with shorter ranging capabilities for concept validation. Preliminary results obtained with this prototype are also presented. This work is financed by the Canadian Space Agency.

High-Definition Television (HDTV) Images for Earth Observations and Earth Science Applications

NASA Technical Reports Server (NTRS)

Robinson, Julie A.; Holland, S. Douglas; Runco, Susan K.; Pitts, David E.; Whitehead, Victor S.; Andrefouet, Serge M.

2000-01-01

As part of Detailed Test Objective 700-17A, astronauts acquired Earth observation images from orbit using a high-definition television (HDTV) camcorder, Here we provide a summary of qualitative findings following completion of tests during missions STS (Space Transport System)-93 and STS-99. We compared HDTV imagery stills to images taken using payload bay video cameras, Hasselblad film camera, and electronic still camera. We also evaluated the potential for motion video observations of changes in sunlight and the use of multi-aspect viewing to image aerosols. Spatial resolution and color quality are far superior in HDTV images compared to National Television Systems Committee (NTSC) video images. Thus, HDTV provides the first viable option for video-based remote sensing observations of Earth from orbit. Although under ideal conditions, HDTV images have less spatial resolution than medium-format film cameras, such as the Hasselblad, under some conditions on orbit, the HDTV image acquired compared favorably with the Hasselblad. Of particular note was the quality of color reproduction in the HDTV images HDTV and electronic still camera (ESC) were not compared with matched fields of view, and so spatial resolution could not be compared for the two image types. However, the color reproduction of the HDTV stills was truer than colors in the ESC images. As HDTV becomes the operational video standard for Space Shuttle and Space Station, HDTV has great potential as a source of Earth-observation data. Planning for the conversion from NTSC to HDTV video standards should include planning for Earth data archiving and distribution.

View of Scientific Instrument Module to be flown on Apollo 15

NASA Image and Video Library

1971-06-27

S71-2250X (June 1971) --- A close-up view of the Scientific Instrument Module (SIM) to be flown for the first time on the Apollo 15 lunar landing mission. Mounted in a previously vacant sector of the Apollo Service Module (SM), the SIM carries specialized cameras and instrumentation for gathering lunar orbit scientific data. SIM equipment includes a laser altimeter for accurate measurement of height above the lunar surface; a large-format panoramic camera for mapping, correlated with a metric camera and the laser altimeter for surface mapping; a gamma ray spectrometer on a 25-feet extendible boom; a mass spectrometer on a 21-feet extendible boom; X-ray and alpha particle spectrometers; and a subsatellite which will be injected into lunar orbit carrying a particle and magnetometer, and the S-Band transponder.

Medium-sized aperture camera for Earth observation

NASA Astrophysics Data System (ADS)

Kim, Eugene D.; Choi, Young-Wan; Kang, Myung-Seok; Kim, Ee-Eul; Yang, Ho-Soon; Rasheed, Ad. Aziz Ad.; Arshad, Ahmad Sabirin

2017-11-01

Satrec Initiative and ATSB have been developing a medium-sized aperture camera (MAC) for an earth observation payload on a small satellite. Developed as a push-broom type high-resolution camera, the camera has one panchromatic and four multispectral channels. The panchromatic channel has 2.5m, and multispectral channels have 5m of ground sampling distances at a nominal altitude of 685km. The 300mm-aperture Cassegrain telescope contains two aspheric mirrors and two spherical correction lenses. With a philosophy of building a simple and cost-effective camera, the mirrors incorporate no light-weighting, and the linear CCDs are mounted on a single PCB with no beam splitters. MAC is the main payload of RazakSAT to be launched in 2005. RazakSAT is a 180kg satellite including MAC, designed to provide high-resolution imagery of 20km swath width on a near equatorial orbit (NEqO). The mission objective is to demonstrate the capability of a high-resolution remote sensing satellite system on a near equatorial orbit. This paper describes the overview of the MAC and RarakSAT programmes, and presents the current development status of MAC focusing on key optical aspects of Qualification Model.

Orbital Debris Detection and Tracking Strategies for the NASA/AFRL Meter Class Autonomous Telescope (MCAT)

NASA Technical Reports Server (NTRS)

Mulrooney, M.; Hickson, P.; Stansbery, Eugene G.

2010-01-01

MCAT (Meter-Class Autonomous Telescope) is a 1.3m f/4 Ritchey-Chr tien on a double horseshoe equatorial mount that will be deployed in early 2011 to the western pacific island of Legan in the Kwajalein Atoll to perform orbital debris observations. MCAT will be capable of tracking earth orbital objects at all inclinations and at altitudes from 200 km to geosynchronous. MCAT s primary objective is the detection of new orbital debris in both low-inclination low-earth orbits (LEO) and at geosynchronous earth orbit (GEO). MCAT was thus designed with a fast focal ratio and a large unvignetted image circle able to accommodate a detector sized to yield a large field of view. The selected primary detector is a close-cycle cooled 4Kx4K 15um pixel CCD camera that yields a 0.9 degree diagonal field. For orbital debris detection in widely spaced angular rate regimes, the camera must offer low read-noise performance over a wide range of framing rates. MCAT s 4-port camera operates from 100 kHz to 1.5 MHz per port at 2 e- and 10 e- read noise respectively. This enables low-noise multi-second exposures for GEO observations as well as rapid (several frames per second) exposures for LEO. GEO observations will be performed using a counter-sidereal time delay integration (TDI) technique which NASA has used successfully in the past. For MCAT the GEO survey, detection, and follow-up prediction algorithms will be automated. These algorithms will be detailed herein. For LEO observations two methods will be employed. The first, Orbit Survey Mode (OSM), will scan specific orbital inclination and altitude regimes, detect new orbital debris objects against trailed background stars, and adjust the telescope track to follow the detected object. The second, Stare and Chase Mode (SCM), will perform a stare, then detect and track objects that enter the field of view which satisfy specific rate and brightness criteria. As with GEO, the LEO operational modes will be fully automated and will be described herein. The automation of photometric and astrometric processing (thus streamlining data collection for environmental modeling) will also be discussed.

STS-27 MS Mullane on aft flight deck with camera equipment

NASA Image and Video Library

1988-12-06

STS027-10-021 (2-6 Dec. 1988) --- Astronaut Richard M. (Mike) Mullane, STS-27 mission specialist, is able to handle a number of cameras with the aid of the microgravity in the shirt sleeve environment of the Earth-orbiting space shuttle Atlantis. Photo credit: NASA

Orbiter View of Curiosity From Nearly Straight Overhead

NASA Image and Video Library

2012-08-31

Details such as the shadow of the mast on NASA Mars rover Curiosity appear in an image taken Aug. 17, 2012, by the HiRISE camera on NASA Mars Reconnaissance Orbiter, from more directly overhead than previous HiRISE images of Curiosity.

Color View From Orbit Showing Opportunity in Botany Bay

NASA Image and Video Library

2013-07-17

This image taken by the HiRISE camera on NASA Mars Reconnaissance Orbiter, captures Opportunity traversing south at the end of the white arrow to new science targets and a winter haven at Solander Point, another portion of the Endeavour rim.

Horizon photo of Western horizon over South America - sixth orbit pass

NASA Image and Video Library

1962-10-03

S62-06604 (3 Oct. 1962) --- Western horizon over South America taken during the sixth orbit pass of the Mercury-Atlas 8 (MA-8) mission by astronaut Walter M. Schirra Jr. with a hand-held camera. Photo credit: NASA

Horizon photo of Western horizon over South America - sixth orbit pass

NASA Image and Video Library

1962-10-03

S62-06607 (3 Oct. 1962) --- Western horizon over South America taken during the sixth orbit pass of the Mercury-Atlas 8 (MA-8) mission by astronaut Walter M. Schirra Jr. with a hand-held camera. Photo credit: NASA

Erosion Patterns May Guide Mars Rover to Rocks Recently Exposed

NASA Image and Video Library

2013-12-09

These two images come from the HiRISE camera on NASA Mars Reconnaissance Orbiter. Images of locations in Gale Crater taken from orbit around Mars reveal evidence of erosion in recent geological times and development of small scarps, or vertical surfaces

The Value of Photographic Observations in Improving the Accuracy of Satellite Orbits.

DTIC Science & Technology

1982-02-01

cameras in the years 1971 -3 have recently become available, particularly of the balloon-satellite Explorer 19, from the observing stations at Riga...from the Russian AFU-75 cameras in the years 1971 -1973 have recently become available, particularly of the balloon- satellite Explorer 19, from the...large numbers of observations frum the Russian AFU-75 cameras have become available, covering the years 1971 -3. The observations, made during the

STS-36 Mission Specialist Mullane uses 70mm HASSELBLAD camera on flight deck

NASA Technical Reports Server (NTRS)

1990-01-01

STS-36 Mission Specialist Richard M. Mullane points 70mm HASSELBLAD camera out overhead window W8 on the aft flight deck of Atlantis, Orbiter Vehicle (OV) 104. Mullane is recording Earth imagery with the camera. Mullane and four other astronauts spent four days, 10 hours and 19 minutes aboard OV-104 for the Department of Defense (DOD) devoted mission. Note: Mullane is wearing a orange 'Tigers' t-shirt.

A Robust Camera-Based Interface for Mobile Entertainment

PubMed Central

Roig-Maimó, Maria Francesca; Manresa-Yee, Cristina; Varona, Javier

2016-01-01

Camera-based interfaces in mobile devices are starting to be used in games and apps, but few works have evaluated them in terms of usability or user perception. Due to the changing nature of mobile contexts, this evaluation requires extensive studies to consider the full spectrum of potential users and contexts. However, previous works usually evaluate these interfaces in controlled environments such as laboratory conditions, therefore, the findings cannot be generalized to real users and real contexts. In this work, we present a robust camera-based interface for mobile entertainment. The interface detects and tracks the user’s head by processing the frames provided by the mobile device’s front camera, and its position is then used to interact with the mobile apps. First, we evaluate the interface as a pointing device to study its accuracy, and different factors to configure such as the gain or the device’s orientation, as well as the optimal target size for the interface. Second, we present an in the wild study to evaluate the usage and the user’s perception when playing a game controlled by head motion. Finally, the game is published in an application store to make it available to a large number of potential users and contexts and we register usage data. Results show the feasibility of using this robust camera-based interface for mobile entertainment in different contexts and by different people. PMID:26907288

Observation sequences and onboard data processing of Planet-C

NASA Astrophysics Data System (ADS)

Suzuki, M.; Imamura, T.; Nakamura, M.; Ishi, N.; Ueno, M.; Hihara, H.; Abe, T.; Yamada, T.

Planet-C or VCO Venus Climate Orbiter will carry 5 cameras IR1 IR 1micrometer camera IR2 IR 2micrometer camera UVI UV Imager LIR Long-IR camera and LAC Lightning and Airglow Camera in the UV-IR region to investigate atmospheric dynamics of Venus During 30 hr orbiting designed to quasi-synchronize to the super rotation of the Venus atmosphere 3 groups of scientific observations will be carried out i image acquisition of 4 cameras IR1 IR2 UVI LIR 20 min in 2 hrs ii LAC operation only when VCO is within Venus shadow and iii radio occultation These observation sequences will define the scientific outputs of VCO program but the sequences must be compromised with command telemetry downlink and thermal power conditions For maximizing science data downlink it must be well compressed and the compression efficiency and image quality have the significant scientific importance in the VCO program Images of 4 cameras IR1 2 and UVI 1Kx1K and LIR 240x240 will be compressed using JPEG2000 J2K standard J2K is selected because of a no block noise b efficiency c both reversible and irreversible d patent loyalty free and e already implemented as academic commercial software ICs and ASIC logic designs Data compression efficiencies of J2K are about 0 3 reversible and 0 1 sim 0 01 irreversible The DE Digital Electronics unit which controls 4 cameras and handles onboard data processing compression is under concept design stage It is concluded that the J2K data compression logics circuits using space

Wide-Angle Polarimetric Camera for Korea Pathfinder Lunar Orbiter

NASA Astrophysics Data System (ADS)

Choi, Y. J.; Kim, S.; Kang, K. I.

2016-12-01

A polarimetry data contains valuable information about the lunar surface such as the grain size and porosity of the regolith. However, a polarimetry toward the Moon in its orbit has not been performed. We plan to perform the polarimetry in lunar orbit through Korea Pathfinder Lunar Orbiter (KPLO), which will be launched around 2018/2019 as the first Korean lunar mission. Wide-Angle Polarimetric Camera (PolCam) is selected as one of the onboard instrument for KPLO. The science objectives are ; (1) To obtain the polarization data of the whole lunar surface at wavelengths of 430nm and 650nm for phase angle range from 0° to 120° with a spatial resolution of 80 m. (2) To obtain the reflectance ratios at 320 nm and 430 nm for the whole lunar surface with a spatial resolution of 80m. We will summarize recent results of lunar surface from ground-based polarimetric observations and will briefly introduce the science rationals and operation concept of PolCam.

Miniaturized Autonomous Extravehicular Robotic Camera (Mini AERCam)

NASA Technical Reports Server (NTRS)

Fredrickson, Steven E.

2001-01-01

The NASA Johnson Space Center (JSC) Engineering Directorate is developing the Autonomous Extravehicular Robotic Camera (AERCam), a low-volume, low-mass free-flying camera system . AERCam project team personnel recently initiated development of a miniaturized version of AERCam known as Mini AERCam. The Mini AERCam target design is a spherical "nanosatellite" free-flyer 7.5 inches in diameter and weighing 1 0 pounds. Mini AERCam is building on the success of the AERCam Sprint STS-87 flight experiment by adding new on-board sensing and processing capabilities while simultaneously reducing volume by 80%. Achieving enhanced capability in a smaller package depends on applying miniaturization technology across virtually all subsystems. Technology innovations being incorporated include micro electromechanical system (MEMS) gyros, "camera-on-a-chip" CMOS imagers, rechargeable xenon gas propulsion system , rechargeable lithium ion battery, custom avionics based on the PowerPC 740 microprocessor, GPS relative navigation, digital radio frequency communications and tracking, micropatch antennas, digital instrumentation, and dense mechanical packaging. The Mini AERCam free-flyer will initially be integrated into an approximate flight-like configuration for demonstration on an airbearing table. A pilot-in-the-loop and hardware-in-the-loop simulation to simulate on-orbit navigation and dynamics will complement the airbearing table demonstration. The Mini AERCam lab demonstration is intended to form the basis for future development of an AERCam flight system that provides beneficial on-orbit views unobtainable from fixed cameras, cameras on robotic manipulators, or cameras carried by EVA crewmembers.

Orbit/attitude estimation with LANDSAT Landmark data

NASA Technical Reports Server (NTRS)

Hall, D. L.; Waligora, S.

1979-01-01

The use of LANDSAT landmark data for orbit/attitude and camera bias estimation was studied. The preliminary results of these investigations are presented. The Goddard Trajectory Determination System (GTDS) error analysis capability was used to perform error analysis studies. A number of questions were addressed including parameter observability and sensitivity, effects on the solve-for parameter errors of data span, density, and distribution an a priori covariance weighting. The use of the GTDS differential correction capability with acutal landmark data was examined. The rms line and element observation residuals were studied as a function of the solve-for parameter set, a priori covariance weighting, force model, attitude model and data characteristics. Sample results are presented. Finally, verfication and preliminary system evaluation of the LANDSAT NAVPAK system for sequential (extended Kalman Filter) estimation of orbit, and camera bias parameters is given.

Earth Observations taken by Expedition 41 crewmember

NASA Image and Video Library

2014-09-13

ISS041-E-013683 (13 Sept. 2014) --- Photographed with a mounted automated camera, this is one of a number of images featuring the European Space Agency?s Automated Transfer Vehicle (ATV-5 or Georges Lemaitre) docked with the International Space Station. Except for color changes, the images are almost identical. The variation in color from frame to frame is due to the camera?s response to the motion of the orbital outpost, relative to the illumination from the sun.

Earth Observations taken by Expedition 41 crewmember

NASA Image and Video Library

2014-09-13

ISS041-E-013687 (13 Sept. 2014) --- Photographed with a mounted automated camera, this is one of a number of images featuring the European Space Agency?s Automated Transfer Vehicle (ATV-5 or Georges Lemaitre) docked with the International Space Station. Except for color changes, the images are almost identical. The variation in color from frame to frame is due to the camera?s response to the motion of the orbital outpost, relative to the illumination from the sun.

Earth Observations taken by Expedition 41 crewmember

NASA Image and Video Library

2014-09-13

ISS041-E-013693 (13 Sept. 2014) --- Photographed with a mounted automated camera, this is one of a number of images featuring the European Space Agency?s Automated Transfer Vehicle (ATV-5 or Georges Lemaitre) docked with the International Space Station. Except for color changes, the images are almost identical. The variation in color from frame to frame is due to the camera?s response to the motion of the orbital outpost, relative to the illumination from the sun.

Astronaut Alan Bean looks over data acquisition camera on Skylab trainer

NASA Image and Video Library

1972-09-01

S72-39256 (1972) --- Astronaut Alan L. Bean, commander for Skylab 3, the second manned Skylab mission, looks over the data acquisition camera mounted on the water tank in the upper level of the Orbital Workshop (OWS) one-G trainer at the Manned Spacecraft Center (MSC). Photo credit: NASA

Astronaut John Grunsfeld uses camera to record ASTRO-2 payload

NASA Image and Video Library

1995-03-17

STS067-377-008 (2-18 March 1995) --- Astronaut John M. Grunsfeld, mission specialist, uses a handheld Hasselblad camera to record the Astro-2 payload. Orbiting Earth at 190 nautical miles, Grunsfeld joined four other NASA astronauts and two scientists for almost 17 days conducting research in support of the Astro-2 mission.

'Santa Anita' Panorama

NASA Technical Reports Server (NTRS)

2004-01-01

[figure removed for brevity, see original site] Click on the image for 'Santa Anita' Panorama (QTVR)

This color mosaic taken on May 21, 25 and 26, 2004, by the panoramic camera on NASA's Mars Exploration Rover Spirit was acquired from a position roughly three-fourths the way between 'Bonneville Crater' and the base of the 'Columbia Hills.' The area is within a low thermal inertia unit (an area that heats up and cools off quickly) identified from orbit by the Mars Odyssey thermal emission imaging system instrument. The rover was roughly 600 meters (1,968 feet) from the base of the hills.

This mosaic, referred to as the 'Santa Anita Panorama,' is comprised of 64 pointings, acquired with six of the panoramic camera's color filters, including one designed specifically to allow comparisons between orbital and surface brightness data. A total of 384 images were acquired as part of this panorama. The mosaic is an approximate true-color rendering constructed from images using the camera's 750-, 530- and and 480-nanometer filters, and is presented at the full resolution of the camera.

Characterization of previously unidentified lunar pyroclastic deposits using Lunar Reconnaissance Orbiter Camera (LROC) data

USGS Publications Warehouse

Gustafson, J. Olaf; Bell, James F.; Gaddis, Lisa R.R.; Hawke, B. Ray Ray; Giguere, Thomas A.

2012-01-01

We used a Lunar Reconnaissance Orbiter Camera (LROC) global monochrome Wide-angle Camera (WAC) mosaic to conduct a survey of the Moon to search for previously unidentified pyroclastic deposits. Promising locations were examined in detail using LROC multispectral WAC mosaics, high-resolution LROC Narrow Angle Camera (NAC) images, and Clementine multispectral (ultraviolet-visible or UVVIS) data. Out of 47 potential deposits chosen for closer examination, 12 were selected as probable newly identified pyroclastic deposits. Potential pyroclastic deposits were generally found in settings similar to previously identified deposits, including areas within or near mare deposits adjacent to highlands, within floor-fractured craters, and along fissures in mare deposits. However, a significant new finding is the discovery of localized pyroclastic deposits within floor-fractured craters Anderson E and F on the lunar farside, isolated from other known similar deposits. Our search confirms that most major regional and localized low-albedo pyroclastic deposits have been identified on the Moon down to ~100 m/pix resolution, and that additional newly identified deposits are likely to be either isolated small deposits or additional portions of discontinuous, patchy deposits.

Mars Odyssey Observes Martian Moons

NASA Image and Video Library

2018-02-22

Phobos and Deimos, the moons of Mars, are seen by the Mars Odyssey orbiter's Thermal Emission Imaging System, or THEMIS, camera. The images were taken in visible-wavelength light. THEMIS also recorded thermal-infrared imagery in the same scan. The apparent motion is due to progression of the camera's pointing during the 17-second span of the February 15, 2018, observation, not from motion of the two moons. This was the second observation of Phobos by Mars Odyssey; the first was on September 29, 2017. Researchers have been using THEMIS to examine Mars since early 2002, but the maneuver turning the orbiter around to point the camera at Phobos was developed only recently. The distance to Phobos from Odyssey during the observation was about 3,489 miles (5,615 kilometers). The distance to Deimos from Odyssey during the observation was about 12,222 miles (19,670 kilometers). An animation is available at https://photojournal.jpl.nasa.gov/catalog/PIA22248

A real-time MTFC algorithm of space remote-sensing camera based on FPGA

NASA Astrophysics Data System (ADS)

Zhao, Liting; Huang, Gang; Lin, Zhe

2018-01-01

A real-time MTFC algorithm of space remote-sensing camera based on FPGA was designed. The algorithm can provide real-time image processing to enhance image clarity when the remote-sensing camera running on-orbit. The image restoration algorithm adopted modular design. The MTF measurement calculation module on-orbit had the function of calculating the edge extension function, line extension function, ESF difference operation, normalization MTF and MTFC parameters. The MTFC image filtering and noise suppression had the function of filtering algorithm and effectively suppressing the noise. The algorithm used System Generator to design the image processing algorithms to simplify the design structure of system and the process redesign. The image gray gradient dot sharpness edge contrast and median-high frequency were enhanced. The image SNR after recovery reduced less than 1 dB compared to the original image. The image restoration system can be widely used in various fields.

CZT Detector Development for New Generation Hard-X Astronomical Instruments

NASA Astrophysics Data System (ADS)

Uslenghi, Michela; Conti, Giancarlo; D'Angelo, Sergio; Fiorini, Mauro; Quadrini, Egidio M.; Natalucci, Lorenzo; Ubertini, Pietro

2006-04-01

In the context of the definition of a future European gamma-ray mission, following the now on-orbit INTEGRAL observatory, we are carrying out a feasibility study on a Gamma Ray Wide Field Camera (5-500 KeV) for transient event detection. Recent achievements in high energy astronomy have validated the CZT detectors performances in terms of good spatial resolution, detection efficiency, energy resolution and low noise at room temperature. We started a development program aimed to explore the possibilities to improve and optimize the performance of this kind of detectors, acting at the level of both the readout system and crystal quality. Preliminary results of characterization of pixelated crystals provided by IMARAD (now Orbotech) are presented, along with their analysis and interpretation based on an analytical model of signal formation.

Eye on Io.

ERIC Educational Resources Information Center

Lewis, Scott M.

1985-01-01

"Io," one of four satellites of Jupiter, orbits its mother planet in roughly the same plane as Earth orbits the sun. Guidelines for collecting data about Io using a reflecting telescope, 35mm camera, and adapter are presented. A computer program used in studying Io's maximum distance from Jupiter is available. (DH)

The Lunar Orbiter: A Spacecraft to Advance Lunar Exploration

NASA Technical Reports Server (NTRS)

1966-01-01

The film describes the Lunar Orbiter's mission to photograph landing areas on the Moon. The Orbiter will be launched from Cape Kennedy using an Atlas Agena booster rocket. Once it is boosted in a trajectory toward the Moon, the Orbiter will deploy two-way earth communication antennas and solar panels for electricity. Attitude control jets will position the solar panels toward the sun and a tracker for a fix on its navigational star. The Orbiter will be put in an off-center orbit around the Moon where it will circle from four to six days. Scientists on Earth will study the effects of the Moon's gravitational field on the spacecraft, then the orbit will be lowered to 28 miles above the Moon's surface. Engineers will control the Orbiter manually or by computer to activate two camera lenses. The cameras will capture pictures of 12,000 square miles of lunar surface in 25 and 400 square mile increments. Pictures will be sent back to Earth using solar power to transmit electrical signals. The signals will be received by antennas at Goldstone, CA, and in Australia and Spain. Incoming photographic data will be electronically converted and processed to produce large-scale photographic images. The mission will be directed from the Space Flight Operations Facility in Pasadena, CA by NASA and Boeing engineers. After the photographic mission, the Orbiter will continue to circle the Moon providing information about micrometeoroids and radiation in the vicinity.

Impacts on the Hubble Space Telescope Wide Field and Planetary Camera 2: Experimental Simulation of Micrometeoroid Capture

NASA Technical Reports Server (NTRS)

Price, M. C.; Kearsley, A. T.; Wozniakiewicz, P. J.; Spratt, J.; Burchell, M. J.; Cole, M. J.; Anz-Meador, P.; Liou, J. C.; Ross, D. K.; Opiela, J.;

STS-36 Mission Specialist Thuot operates 16mm camera on OV-104's middeck

NASA Image and Video Library

1990-03-03

STS-36 Mission Specialist (MS) Pierre J. Thuot operates 16mm ARRIFLEX motion picture camera mounted on the open airlock hatch via a bracket. Thuot uses the camera to record activity of his fellow STS-36 crewmembers on the middeck of Atlantis, Orbiter Vehicle (OV) 104. Positioned between the airlock hatch and the starboard wall-mounted sleep restraints, Thuot, wearing a FAIRFAX t-shirt, squints into the cameras eye piece. Thuot and four other astronauts spent four days, 10 hours and 19 minutes aboard OV-104 for the Department of Defense (DOD) devoted mission.

STS-36 Mission Specialist Thuot operates 16mm camera on OV-104's middeck

NASA Technical Reports Server (NTRS)

1990-01-01

STS-36 Mission Specialist (MS) Pierre J. Thuot operates 16mm ARRIFLEX motion picture camera mounted on the open airlock hatch via a bracket. Thuot uses the camera to record activity of his fellow STS-36 crewmembers on the middeck of Atlantis, Orbiter Vehicle (OV) 104. Positioned between the airlock hatch and the starboard wall-mounted sleep restraints, Thuot, wearing a FAIRFAX t-shirt, squints into the cameras eye piece. Thuot and four other astronauts spent four days, 10 hours and 19 minutes aboard OV-104 for the Department of Defense (DOD) devoted mission.

Side View of 'Endurance Crater'

NASA Technical Reports Server (NTRS)

2004-01-01

This picture from the rear hazard-avoidance camera on NASA's Mars Exploration Rover Opportunity shows a side view of 'Endurance Crater.' Opportunity took the image on sol 188 (Aug. 4, 2004), before transmitting it and other data to the European Space Agency's Mars Express orbiter. The orbiter then relayed the data to Earth.

Clementine mission

NASA Astrophysics Data System (ADS)

Rustan, Pedro L.

1995-01-01

The U.S. Department of Defense (DoD) and the National Aeronautics and Space Administration (NASA) started a cooperative program in 1992 to flight qualify recently developed lightweight technologies in a radiation stressed environment. The spacecraft, referred to as Clementine, was designed, built, and launched in less than a two year period. The spacecraft was launched into a high inclination orbit from Vandenburg Air Force Base in California on a Titan IIG launch vehicle in January 1994. The spacecraft was injected into a 420 by 3000 km orbit around the Moon and remained there for over two months. Unfortunately, after successfully completing the Lunar phase of the mission, a software malfunction prevented the accomplishment of the near-Earth asteroid (NEA) phase. Some of the technologies incorporated in the Clementine spacecraft include: a 370 gram, 7 watt star tracker camera; a 500 gram, 6 watt, UV/Vis camera; a 1600 gram, 30 watt Indium Antimonide focal plane array NIR camera; a 1650 gram, 30 watt, Mercury Cadmium Telluride LWIR camera; a LIDAR camera which consists of a Nd:YAG diode pumped laser for ranging and an intensified photocathode charge-coupled detector for imaging. The scientific results of the mission will be first analyzed by a NASA selected team, and then will be available to the entire community.

STS-31 crew activity on the middeck of the Earth-orbiting Discovery, OV-103

NASA Image and Video Library

1990-04-29

STS031-05-002 (24-29 April 1990) --- A 35mm camera with a "fish eye" lens captured this high angle image on Discovery's middeck. Astronaut Kathryn D. Sullivan works with the IMAX camera in foreground, while Astronaut Steven A. Hawley consults a checklist in corner. An Arriflex motion picture camera records student ion arc experiment in apparatus mounted on stowage locker. The experiment was the project of Gregory S. Peterson, currently a student at Utah State University.

Identifying Surface Changes on HRSC Images of the Mars South Polar Residual CAP (sprc)

NASA Astrophysics Data System (ADS)

Putri, Alfiah Rizky Diana; Sidiropoulos, Panagiotis; Muller, Jan-Peter

2016-06-01

The surface of Mars has been an object of interest for planetary research since the launch of Mariner 4 in 1964. Since then different cameras such as the Viking Visual Imaging Subsystem (VIS), Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC), and Mars Reconnaissance Orbiter (MRO) Context Camera (CTX) and High Resolution Imaging Science Experiment (HiRISE) have been imaging its surface at ever higher resolution. The High Resolution Stereo Camera (HRSC) on board of the European Space Agency (ESA) Mars Express, has been imaging the Martian surface, since 25th December 2003 until the present-day. HRSC has covered 100 % of the surface of Mars, about 70 % of the surface with panchromatic images at 10-20 m/pixel, and about 98 % at better than 100 m/pixel (Neukum et. al., 2004), including the polar regions of Mars. The Mars polar regions have been studied intensively recently by analysing images taken by the Mars Express and MRO missions (Plaut et al., 2007). The South Polar Residual Cap (SPRC) does not change very much in volume overall but there are numerous examples of dynamic phenomena associated with seasonal changes in the atmosphere. In particular, we can examine the time variation of layers of solid carbon dioxide and water ice with dust deposition (Bibring, 2004), spider-like channels (Piqueux et al., 2003) and so-called Swiss Cheese Terrain (Titus et al., 2004). Because of seasonal changes each Martian year, due to the sublimation and deposition of water and CO2 ice on the Martian south polar region, clearly identifiable surface changes occur in otherwise permanently icy region. In this research, good quality HRSC images of the Mars South Polar region are processed based on previous identification as the optimal coverage of clear surfaces (Campbell et al., 2015). HRSC images of the Martian South Pole are categorized in terms of quality, time, and location to find overlapping areas, processed into high quality Digital Terrain Models (DTMs) and Orthorectified Images (ORIs) and projected into polar stereographic projection using DLR (Deutsches Zentrum für Luft- und Raumfahrt; German Aerospace Center)'s VICAR and GIS software with modifications developed by Kim & Muller (2009). Surface changes are identified in the Mars SPRC region and analysed based on their appearance in the HRSC images.

The Very Low Mass Component of the Gliese 105 System

NASA Astrophysics Data System (ADS)

Golimowski, David A.; Henry, Todd J.; Krist, John E.; Schroeder, Daniel J.; Marcy, Geoffrey W.; Fischer, Debra A.; Butler, R. Paul

2000-10-01

Multiple-epoch, multicolor images of the astrometric binary Gliese 105A and its very low mass companion Gliese 105C have been obtained using the Hubble Space Telescope's Wide Field Planetary Camera 2 (WFPC2) and near-infrared camera and multiobject spectrometer (NICMOS). The optical and near-infrared colors of Gl 105C strongly suggest a spectral type of M7 V for that star. Relative astrometric measurements spanning 3 yr reveal the first evidence of Gl 105C's orbital motion. Previous long-term astrometric studies at Sproul and McCormick Observatories have shown that the period of Gl 105A's perturbation is ~60 yr. To satisfy both the observed orbital motion and Gl 105A's astrometric period, Gl 105C's orbit must have an eccentricity of ~0.75 and a semimajor axis of ~15 AU. Measurements of Gl 105A's radial velocity over 12 yr show a linear trend with a slope of 11.3 m s-1 yr-1, which is consistent with these orbital constraints and a nearly face-on orbit. As no other faint companions to Gl 105A have been detected, we conclude that Gl 105C is probably the source of the 60 yr astrometric perturbation.

Apollo 17 Command/Service modules photographed from lunar module in orbit

NASA Image and Video Library

1972-12-14

AS17-145-22254 (14 Dec. 1972) --- An excellent view of the Apollo 17 Command and Service Modules (CSM) photographed from the Lunar Module (LM) "Challenger" during rendezvous and docking maneuvers in lunar orbit. The LM ascent stage, with astronauts Eugene A. Cernan and Harrison H. Schmitt aboard, had just returned from the Taurus-Littrow landing site on the lunar surface. Astronaut Ronald E. Evans remained with the CSM in lunar orbit. Note the exposed Scientific Instrument Module (SIM) Bay in Sector 1 of the Service Module (SM). Three experiments are carried in the SIM bay: S-209 lunar sounder, S-171 infrared scanning spectrometer, and the S-169 far-ultraviolet spectrometer. Also mounted in the SIM bay are the panoramic camera, mapping camera and laser altimeter used in service module photographic tasks. A portion of the LM is on the right.

STS-109 Crew Interviews - Currie

NASA Technical Reports Server (NTRS)

2002-01-01

STS-109 Mission Specialist 2 Nancy Jane Currie is seen during a prelaunch interview. She answers questions about her inspiration to become an astronaut and her career path. She gives details on the Columbia Orbiter mission which has as its main tasks the maintenance and augmentation of the Hubble Space Telescope (HST). While she will do many things during the mission, the most important will be her role as the primary operator of the robotic arm, which is responsible for grappling the HST, bringing it to the Orbiter bay, and providing support for the astronauts during their EVAs (Extravehicular Activities). Additionally, the robotic arm will be responsible for transferring new and replacement equipment from the Orbiter to the HST. This equipment includes: two solar arrays, a Power Control Unit (PCU), the Advanced Camera for Surveys, and a replacement cooling system for NICMOS (Near Infrared Camera Multi-Object Spectrometer).

Fuzzy logic in autonomous orbital operations

NASA Technical Reports Server (NTRS)

Lea, Robert N.; Jani, Yashvant

1991-01-01

Fuzzy logic can be used advantageously in autonomous orbital operations that require the capability of handling imprecise measurements from sensors. Several applications are underway to investigate fuzzy logic approaches and develop guidance and control algorithms for autonomous orbital operations. Translational as well as rotational control of a spacecraft have been demonstrated using space shuttle simulations. An approach to a camera tracking system has been developed to support proximity operations and traffic management around the Space Station Freedom. Pattern recognition and object identification algorithms currently under development will become part of this camera system at an appropriate level in the future. A concept to control environment and life support systems for large Lunar based crew quarters is also under development. Investigations in the area of reinforcement learning, utilizing neural networks, combined with a fuzzy logic controller, are planned as a joint project with the Ames Research Center.

Deployment of the RCA Satcom K-2 communications satellite

NASA Image and Video Library

1985-11-28

61B-38-36W (28 Nov 1985) --- The 4,144-pound RCA Satcom K-2 communications satellite is photographed as it spins from the cargo bay of the Earth-orbiting Atlantis. A TV camera at right records the deployment for a later playback to Earth. This frame was photographed with a handheld Hasselblad camera inside the spacecraft.

STS-46 aft flight deck payload station 'Marsha's workstation' aboard OV-104

NASA Technical Reports Server (NTRS)

1992-01-01

STS-46 payload station nicknamed 'Marsha's (Ivins) workstation' on the aft flight deck of Atlantis, Orbiter Vehicle (OV) 104, is cluttered with food, cameras, camera gear, cassettes, flight text material, and other paraphernalia. This area is just behind the commanders station. Fellow crewmembers nicknamed the station and good-naturedly kidded Ivins about the mess.

The California All-sky Meteor Surveillance (CAMS) System

NASA Astrophysics Data System (ADS)

Gural, P. S.

2011-01-01

A unique next generation multi-camera, multi-site video meteor system is being developed and deployed in California to provide high accuracy orbits of simultaneously captured meteors. Included herein is a description of the goals, concept of operations, hardware, and software development progress. An appendix contains a meteor camera performance trade study made for video systems circa 2010.

The High Resolution Stereo Camera (HRSC) of Mars Express and its approach to science analysis and mapping for Mars and its satellites

NASA Astrophysics Data System (ADS)

Gwinner, K.; Jaumann, R.; Hauber, E.; Hoffmann, H.; Heipke, C.; Oberst, J.; Neukum, G.; Ansan, V.; Bostelmann, J.; Dumke, A.; Elgner, S.; Erkeling, G.; Fueten, F.; Hiesinger, H.; Hoekzema, N. M.; Kersten, E.; Loizeau, D.; Matz, K.-D.; McGuire, P. C.; Mertens, V.; Michael, G.; Pasewaldt, A.; Pinet, P.; Preusker, F.; Reiss, D.; Roatsch, T.; Schmidt, R.; Scholten, F.; Spiegel, M.; Stesky, R.; Tirsch, D.; van Gasselt, S.; Walter, S.; Wählisch, M.; Willner, K.

2016-07-01

The High Resolution Stereo Camera (HRSC) of ESA's Mars Express is designed to map and investigate the topography of Mars. The camera, in particular its Super Resolution Channel (SRC), also obtains images of Phobos and Deimos on a regular basis. As HRSC is a push broom scanning instrument with nine CCD line detectors mounted in parallel, its unique feature is the ability to obtain along-track stereo images and four colors during a single orbital pass. The sub-pixel accuracy of 3D points derived from stereo analysis allows producing DTMs with grid size of up to 50 m and height accuracy on the order of one image ground pixel and better, as well as corresponding orthoimages. Such data products have been produced systematically for approximately 40% of the surface of Mars so far, while global shape models and a near-global orthoimage mosaic could be produced for Phobos. HRSC is also unique because it bridges between laser altimetry and topography data derived from other stereo imaging instruments, and provides geodetic reference data and geological context to a variety of non-stereo datasets. This paper, in addition to an overview of the status and evolution of the experiment, provides a review of relevant methods applied for 3D reconstruction and mapping, and respective achievements. We will also review the methodology of specific approaches to science analysis based on joint analysis of DTM and orthoimage information, or benefitting from high accuracy of co-registration between multiple datasets, such as studies using multi-temporal or multi-angular observations, from the fields of geomorphology, structural geology, compositional mapping, and atmospheric science. Related exemplary results from analysis of HRSC data will be discussed. After 10 years of operation, HRSC covered about 70% of the surface by panchromatic images at 10-20 m/pixel, and about 97% at better than 100 m/pixel. As the areas with contiguous coverage by stereo data are increasingly abundant, we also present original data related to the analysis of image blocks and address methodology aspects of newly established procedures for the generation of multi-orbit DTMs and image mosaics. The current results suggest that multi-orbit DTMs with grid spacing of 50 m can be feasible for large parts of the surface, as well as brightness-adjusted image mosaics with co-registration accuracy of adjacent strips on the order of one pixel, and at the highest image resolution available. These characteristics are demonstrated by regional multi-orbit data products covering the MC-11 (East) quadrangle of Mars, representing the first prototype of a new HRSC data product level.

A Description of Sub-Equatorial Volcanic Structures Consistent with Sub-Ice Magmatism East of Nepenthes Mensae, Mars.

NASA Astrophysics Data System (ADS)

Caprarelli, G.; de Pablo Hernandez, M. A.

2014-12-01

The Martian region located immediately north of the dichotomy scarp, between latitudes 120°E and 135°E, is covered by fretted terrains, characterised by the presence of knobs and mesas formed by eroded and reworked material of highlands provenance, and the smoother terrains between them [1]. Topographic depressions of oblong shape, generally parallel to the scarp, of rough and chaotic appearance, are also observed. The high resolution (~ 6 m/pixel, [2]) Context Camera (CTX) on board Mars Reconnaissance Orbiter (MRO) makes it possible to examine the morphologies of these topographic depressions in great detail, unveiling their complex geological histories. Here we expand on our earlier work in the adjacent Nepenthes Mensae region [3] and present the results of our observations of morphologies of likely igneous origin. We identified a variety of shapes consistent with magmatic structures and constructs: dikes, collapsed lava tubes, and lava flows are observable in the smoother terrains. Most of the elevated structures in the areas are strongly eroded knobs and mesas covered by dust and debris. In some cases however, the morphological characteristics of 2-10 km-size structures are clear and sharp, which allowed us to identify features consistent with sub-ice volcanic constructs, such as tuyas and tindars [4]. Geological reconstructions involving magma-ice interaction are supported by the presence of lobate aprons around knobs and mesas, and of scalloped ejecta surrounding complex impact craters, suggesting the existence of ice both underground and on the surface of these low elevation areas at the time of formation of these constructs. [1] Tanaka et al. (2005) Geologic Map of the Northern Plains of Mars. USGS SIM 2888. [2] Malin et al. (2007) Context Camera investigation on board the Mars Reconnaissance Orbiter. JGR 112, E05S04, 10.1029/2006JE002808. [3] dePablo and Caprarelli (2010) Possible subglacial volcanoes in Nepenthes Mensae, eastern hemisphere, Mars. LPSC 41, 1584. [4] Jakobsson and Gudmundsson (2008) Subglacial and intraglacial volcanic formations in Iceland. Jökull 58, 179-196.

Orbital Debris Quarterly News, Volume 13, No. 3

NASA Technical Reports Server (NTRS)

Liou, J.-C. (Editor); Shoots, Debi (Editor)

2009-01-01

This issue of the Orbital Debris Quarterly contains articles on the congressional hearing that was held on orbital debris and space traffic; the update received by the United Nations Committee on the Peaceful Uses of Outer Space (COPUOS) on the collision of the Iridium 33 and Cosmos 2251 satellites; the micrometeoroid and orbital debris (MMOD) inspection of the Hubble Space Telescope Wide Field Planetary Camera; an analysis of the reentry survivability of the Global Precipitation Measurement (GPM) spacecraft; an update on recent major breakup fragments; and a graph showing the current debris environment in low Earth orbit.

Surveillance of medium and high Earth orbits using large baseline stereovision

NASA Astrophysics Data System (ADS)

Danescu, Radu; Ciurte, Anca; Oniga, Florin; Cristea, Octavian; Dolea, Paul; Dascal, Vlad; Turcu, Vlad; Mircea, Liviu; Moldovan, Dan

2014-11-01

The Earth is surrounded by a swarm of satellites and associated debris known as Resident Space Objects (RSOs). All RSOs will orbit the Earth until they reentry into Earth's atmosphere. There are three main RSO categories: Low Earth Orbit (LEO), when the satellite orbits at an altitude below 1 500 km; a Medium Earth Orbit (MEO) for Global Navigation Satellite Systems (GNSS) at an altitude of around 20 000 km, and a Geostationary Earth Orbit (GEO) (also sometimes called the Clarke orbit), for geostationary satellites, at an altitude of 36 000 km. The Geostationary Earth Orbits and the orbits of higher altitude are also known as High Earth Orbits (HEO). Crucial for keeping an eye on RSOs, the Surveillance of Space (SofS) comprises detection, tracking, propagation of orbital parameters, cataloguing and analysis of these objects. This paper presents a large baseline stereovision based approach for detection and ranging of RSO orbiting at medium to high altitudes. Two identical observation systems, consisting of camera, telescope, control computer and GPS receiver are located 37 km apart, and set to observe the same region of the sky. The telescopes are placed on equatorial mounts able to compensate for the Earth's rotation, so that the stars appear stationary in the acquired images, and the satellites will appear as linear streaks. The two cameras are triggered simultaneously. The satellite streaks are detected in each image of the stereo pair using its streak-like appearance against point-like stars, the motion of the streaks between successive frames, and the stereo disparity. The detected satellite pixels are then put into correspondence using the epipolar geometry, and the 3D position of the satellite in the Earth Center, Earth Fixed (ECEF) reference frame is computed using stereo triangulation. Preliminary tests have been performed, for both MEO and HEO orbits. The preliminary results indicate a very high detection rate for MEO orbits, and good detection rate for HEO orbits, dependent on the satellite's rotation.

Mini AERCam: A Free-Flying Robot for Space Inspection

NASA Technical Reports Server (NTRS)

Fredrickson, Steven

2001-01-01

The NASA Johnson Space Center Engineering Directorate is developing the Autonomous Extravehicular Robotic Camera (AERCam), a free-flying camera system for remote viewing and inspection of human spacecraft. The AERCam project team is currently developing a miniaturized version of AERCam known as Mini AERCam, a spherical nanosatellite 7.5 inches in diameter. Mini AERCam development builds on the success of AERCam Sprint, a 1997 Space Shuttle flight experiment, by integrating new on-board sensing and processing capabilities while simultaneously reducing volume by 80%. Achieving these productivity-enhancing capabilities in a smaller package depends on aggressive component miniaturization. Technology innovations being incorporated include micro electromechanical system (MEMS) gyros, "camera-on-a-chip" CMOS imagers, rechargeable xenon gas propulsion, rechargeable lithium ion battery, custom avionics based on the PowerPC 740 microprocessor, GPS relative navigation, digital radio frequency communications and tracking, micropatch antennas, digital instrumentation, and dense mechanical packaging. The Mini AERCam free-flyer will initially be integrated into an approximate flight-like configuration for laboratory demonstration on an airbearing table. A pilot-in-the-loop and hardware-in-the-loop simulation to simulate on-orbit navigation and dynamics will complement the airbearing table demonstration. The Mini AERCam lab demonstration is intended to form the basis for future development of an AERCam flight system that provides on-orbit views of the Space Shuttle and International Space Station unobtainable from fixed cameras, cameras on robotic manipulators, or cameras carried by space-walking crewmembers.

Automatic Calibration of an Airborne Imaging System to an Inertial Navigation Unit

NASA Technical Reports Server (NTRS)

Ansar, Adnan I.; Clouse, Daniel S.; McHenry, Michael C.; Zarzhitsky, Dimitri V.; Pagdett, Curtis W.

2013-01-01

This software automatically calibrates a camera or an imaging array to an inertial navigation system (INS) that is rigidly mounted to the array or imager. In effect, it recovers the coordinate frame transformation between the reference frame of the imager and the reference frame of the INS. This innovation can automatically derive the camera-to-INS alignment using image data only. The assumption is that the camera fixates on an area while the aircraft flies on orbit. The system then, fully automatically, solves for the camera orientation in the INS frame. No manual intervention or ground tie point data is required.

LAUNCH (SOLID ROCKET BOOSTER [SRB]) - STS-1

NASA Image and Video Library

1981-04-12

S81-30505 (12 April 1981) --- Separation of space shuttle Columbia?s external tank, photographed by motion picture cameras in the umbilical bays, occurred following the shutdown of the vehicle?s three main engines. Columbia?s cameras were able to record the bottom side of the tank as the orbiter headed toward its Earth-orbital mission with astronauts John W. Young and Robert L. Crippen aboard and the fuel tank fell toward Earth, passing through the atmosphere rapidly. Liquid oxygen and liquid hydrogen umbilical connectors can be seen at the bottom of the tank. For orientation, the photo should be held with the rounded end at bottom of the frame. Photo credit: NASA

Skylab 3 crewmen shown eating in Orbital Workshop wardroom

NASA Technical Reports Server (NTRS)

1973-01-01

The three Skylab 3 crewmen are shown eating in the Orbital Workshop (OWS) wardroom of the Skylab space station in Earth orbit, in this photographic reproduction taken from a television transmission made by a color TV camera aboard the OWS. Astronaut Alan L. Bean (right), commander, illustrates eating under zero gravity conditions upsidedown. The two other crewmen are Scientist-Astronaut Owen K. Garriott (left), science pilot; and Astronaut Jack R. Lousma, pilot.

Astronaut Alan Bean shaves while aboard Skylab

NASA Technical Reports Server (NTRS)

1973-01-01

Astronaut Alan L. Bean, Skylab 3 commander, uses battery powered shaver while in the crew quarters of the Skylab space station's Orbital Workshop (OWS) crew quarters. This photograph was taken with a 35mm Nikon camera held by one of Bean's fellow crewmen during the 56.5 day second manned Skylab mission in Earth orbit.

Viking survey paper

NASA Technical Reports Server (NTRS)

Soffen, G.

1976-01-01

The paper reviews Viking injection into Mars orbit, the landing, and the Orbiter. The following Viking investigations are discussed: the search for life (photosynthetic analysis, metabolic analysis, and respiration), molecular analysis, inorganic chemistry, water detection, thermal mapping, radio science, and physical and seismic characteristics. Also considered are the imaging system, the lander camera, entry science, and Mars weather.

Comparative assessment of techniques for initial pose estimation using monocular vision

NASA Astrophysics Data System (ADS)

Sharma, Sumant; D`Amico, Simone

2016-06-01

This work addresses the comparative assessment of initial pose estimation techniques for monocular navigation to enable formation-flying and on-orbit servicing missions. Monocular navigation relies on finding an initial pose, i.e., a coarse estimate of the attitude and position of the space resident object with respect to the camera, based on a minimum number of features from a three dimensional computer model and a single two dimensional image. The initial pose is estimated without the use of fiducial markers, without any range measurements or any apriori relative motion information. Prior work has been done to compare different pose estimators for terrestrial applications, but there is a lack of functional and performance characterization of such algorithms in the context of missions involving rendezvous operations in the space environment. Use of state-of-the-art pose estimation algorithms designed for terrestrial applications is challenging in space due to factors such as limited on-board processing power, low carrier to noise ratio, and high image contrasts. This paper focuses on performance characterization of three initial pose estimation algorithms in the context of such missions and suggests improvements.

Jupiter's Magnetic Field and Magnetosphere after Juno's First 8 Orbits

NASA Astrophysics Data System (ADS)

Connerney, J. E. P.; Oliversen, R. J.; Espley, J. R.; Gruesbeck, J.; Kotsiaros, S.; DiBraccio, G. A.; Joergensen, J. L.; Joergensen, P. S.; Merayo, J. M. G.; Denver, T.; Benn, M.; Bjarno, J. B.; Malinnikova Bang, A.; Bloxham, J.; Moore, K.; Bolton, S. J.; Levin, S.; Gershman, D. J.

2016-12-01

The Juno spacecraft entered polar orbit about Jupiter on July 4, 2016, embarking upon an ambitious mission to map Jupiter's magnetic and gravitational potential fields and probe its deep atmosphere, in search of clues to the planet's formation and evolution. Juno is also instrumented to conduct the first exploration of the polar magnetosphere and to acquire images and spectra of its polar auroras and atmosphere. Juno's 53.5-day orbit trajectory carries her science instruments from pole to pole in approximately 2 hours, with a closest approach to within 1.05 Rj of the center of the planet (one Rj = 71,492 km, Jupiter's equatorial radius), just a few thousand km above the clouds. Repeated periapsis passes will eventually encircle the planet with a dense net of observations equally spaced in longitude (<12° at the equator) and optimized for characterization of the Jovian dynamo. Such close passages are sensitive to small spatial scale variations in the magnetic field and therefore many such passes are required to bring the magnetic field into focus. Nevertheless, after only 8 orbits, low-degree spherical harmonics can be extracted from a partial solution to a much more complicated representation (e.g., 20 degree/order), providing the first new information about Jupiter's magnetic field in decades. Juno is equipped with two magnetometer sensor suites, located 10 and 12 m from the center of the spacecraft at the end of one of Juno's three solar panel wings. Each contains a vector fluxgate magnetometer (FGM) sensor and a pair of co-located non-magnetic star tracker camera heads, providing accurate attitude determination for the FGM sensors. We present an overview of the magnetometer observations obtained during Juno's first year in orbit in context with prior observations and those acquired by Juno's other science instruments.

Jupiter's Magnetic Field and Magnetosphere after Juno's First 8 Orbits

NASA Astrophysics Data System (ADS)

Connerney, J. E. P.; Oliversen, R. J.; Espley, J. R.; Gruesbeck, J.; Kotsiaros, S.; DiBraccio, G. A.; Joergensen, J. L.; Joergensen, P. S.; Merayo, J. M. G.; Denver, T.; Benn, M.; Bjarno, J. B.; Malinnikova Bang, A.; Bloxham, J.; Moore, K.; Bolton, S. J.; Levin, S.; Gershman, D. J.

2017-12-01

The Juno spacecraft entered polar orbit about Jupiter on July 4, 2016, embarking upon an ambitious mission to map Jupiter's magnetic and gravitational potential fields and probe its deep atmosphere, in search of clues to the planet's formation and evolution. Juno is also instrumented to conduct the first exploration of the polar magnetosphere and to acquire images and spectra of its polar auroras and atmosphere. Juno's 53.5-day orbit trajectory carries her science instruments from pole to pole in approximately 2 hours, with a closest approach to within 1.05 Rj of the center of the planet (one Rj = 71,492 km, Jupiter's equatorial radius), just a few thousand km above the clouds. Repeated periapsis passes will eventually encircle the planet with a dense net of observations equally spaced in longitude (<12° at the equator) and optimized for characterization of the Jovian dynamo. Such close passages are sensitive to small spatial scale variations in the magnetic field and therefore many such passes are required to bring the magnetic field into focus. Nevertheless, after only 8 orbits, low-degree spherical harmonics can be extracted from a partial solution to a much more complicated representation (e.g., 20 degree/order), providing the first new information about Jupiter's magnetic field in decades. Juno is equipped with two magnetometer sensor suites, located 10 and 12 m from the center of the spacecraft at the end of one of Juno's three solar panel wings. Each contains a vector fluxgate magnetometer (FGM) sensor and a pair of co-located non-magnetic star tracker camera heads, providing accurate attitude determination for the FGM sensors. We present an overview of the magnetometer observations obtained during Juno's first year in orbit in context with prior observations and those acquired by Juno's other science instruments.

Dawn Mission: A Journey in Space and Time

NASA Technical Reports Server (NTRS)

Russell, C. T.; Coradini, A.; DeSanctis, M. C.; Feldman, W. C.; Jaumann, R.; Konopliv, A. S.; McCord, T. B.; McFadden, L. A.; McSween, H. Y.; Mottola, S.

2003-01-01

By successively orbiting both 4 Vesta and 1 Ceres the Dawn mission directly addresses the longstanding goals of NASA and the planetary community to understand the origin and evolution of the solar system by obtaining geophysical and geochemical data on diverse main belt asteroids. Ceres and Vesta are two complementary terrestrial protoplanets (one apparently "wet" and one "dry"), whose accretion was terminated by the formation of Jupiter. Ceres is little changed since it formed in the early solar system, while Vesta has experienced significant heating and differentiation. Both have remained intact over the age of the solar system, thereby retaining a record of events and processes from the time of planet formation. Detailed study of the geophysics and geochemistry of these two bodies provides critical benchmarks for the early solar system conditions and processes that shaped its subsequent evolution. Dawn provides the missing context for both primitive and evolved meteoritic data, thus playing a central role in understanding terrestrial planet formation and the evolution of the asteroid belt. Dawn is to be launched in May 2006 arriving at Vesta in 2010 and Ceres in 2014, stopping at each to make 11 months of orbital measurements. The spacecraft uses solar electric propulsion both in cruise and in orbit to make most efficient use of its xenon propellant. The spacecraft carries a framing camera, visible and infrared mapping spectrometer, gamma ray/neutron spectrometer, a laser altimeter, magnetometer, and radio science.

Investigation of small scale roughness properties of Martian terrains using Mars Reconnaissance Orbiter data.

NASA Astrophysics Data System (ADS)

Ivanov, A. B.; Rossi, A.

2009-04-01

Studies of layered terrains in polar regions as well as inside craters and other areas on Mars often require knowledge of local topography at much finer resolution than global MOLA topography allows. For example, in the polar layered deposits spatial relationships are important to understand unconformities that are observed on the edges of the layered terrains [15,3]. Their formation process is not understood at this point, yet fine scale topography, joint with ground penetrating radar like SHARAD and MARSIS may shed light on their 3D structure. Landing site analysis also requires knowledge of local slopes and roughness at scales from 1 to 10 m [1,2]. Mars Orbiter Camera [13] has taken stereo images at these scales, however interpretation was difficult due to unstable behavior of the Mars Global Surveyor spacecraft during image take (wobbling effect). Mars Reconnaissance Orbiter (MRO) is much better stabilized, since it is required for optimal operation of its high resolution camera. In this work we have utilized data from MRO sensors (CTX camera [11] and HIRISE camera [12] in order to derive digital elevation models (DEM) from images targeted as stereo pairs. We employed methods and approaches utilized for the Mars Orbiter Camera (MOC) stereo data [4,5]. CTX data varies in resolution and stereo pairs analyzed in this work can be derived at approximately 10m scale. HIRISE images allow DEM post spacing at around 1 meter. The latter are very big images and our computer infrastructure was only able to process either reduced resolution images, covering larger surface or working with smaller patches at the original resolution. We employed stereo matching technique described in [5,9], in conjunction with radiometric and geometric image processing in ISIS3 [16]. This technique is capable of deriving tiepoint co-registration at subpixel precision and has proven itself when used for Pathfinder and MER operations [8]. Considerable part of this work was to accommodate CTX and HIRISE image processing in the existing data processing pipeline and improve it at the same time. Currently the workflow is not finished: DEM units are relative and are not in elevation. We have been able to derive successful DEMs from CTX data Becquerel [14] and Crommelin craters as well as for some areas in the North Polar Layered Terrain. Due to its tremendous resolution HIRISE data showing great surface detail, hence allowing better correlation than other sensors considered in this work. In all cases DEM were showing considerable potential for exploration of terrain characteristics. Next steps include cross validation results with DEM produced by other teams and sensors (HRSC [6], HIRISE [7]) and providing elevation in terms of absolute height over a MOLA areoid. MRO imaging data allows us an unprecedented look at Martian terrain. This work provides a step forward derivation of DEM from HIRISE and CTX datasets and currently undergoing validation vs. other existing datasets. We will present our latest results for layering structures in both North and South Polar Layered deposits as well as layered structures inside Becquerel and Crommelin craters. Digital Elevation models derived from the CTX sensor can also be utilized effectively as a input for clutter reduction models, which are in turn used for the ground penetrating SHARAD instrument [13]. References. [1] R. Arvidson, et al. Mars exploration program 2007 phoenix landing site selection and characteristics. Journal of Geophysical Research-Planets, 113, JUN 19 2008. [2] M. Golombek, et al. Assessment of mars exploration rover landing site predictions. Nature, 436(7047):44-48, JUL 7 2005. [3] K. E. Herkenhoff, et al. Meter-scale morphology of the north polar region of mars. Science, 317(5845):1711-1715, SEP 21 2007. [4] A. B. Ivanov. Ten-Meter Scale Topography and Roughness of Mars Exploration Rovers Landing Sites and Martian Polar Regions. volume 34 of Lunar and Planetary Inst. Technical Report, pages 2084-+, Mar. 2003. [5] A. B. Ivanov and J. J. Lorre. Analysis of Mars Orbiter Camera Stereo Pairs. In Lunar and Planetary Institute Conference Abstracts, volume 33 of Lunar and Planetary Inst. Technical Report, pages 1845-+, Mar. 2002. [6] R. Jaumann, et al. The high-resolution stereo camera (HRSC) experiment on mars express: Instrument aspects and experiment conduct from interplanetary cruise through the nominal mission. Planetary and Space Science, 55(7-8):928-952, MAY 2007. [7] R. L. Kirk, et al. Ultrahigh resolution topographic mapping of mars with MRO HIRISE stereo images: Meter-scale slopes of candidate phoenix landing sites. Journal of Geophysical Research-Planets, 113, NOV 15 2008. [8] S. Lavoie, et al. Processing and analysis of mars pathfinder science data at the jet propulsion laboratory's science data processing systems section. Journal of Geophysical Research-Planets, 104(E4):8831-8852, APR 25 1999. [9] J. J. Lorre, et al. Recent developments at JPL in the application of image processing to astronomy. In D. L. Crawford, editor, Instrumentation in Astronomy III, volume 172 of Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, pages 394-402, 1979. [10] M. Malin, et al. Early views of the martian surface from the mars orbiter camera of mars global surveyor. Science, 279(5357):1681-1685, MAR 13 1998. [11] M. C. Malin,et al. Context camera investigation on board the mars reconnaissance orbiter. Journal of Geophysical Research-Planets, 112(E5), MAY 18 2007. [12] A. S. McEwen, et al.. Mars reconnaissance orbiter's high resolution imaging science experiment (HIRISE). Journal of Geophysical Research-Planets, 112(E5), MAY 17 2007. [13] A. Rossi, et al. Multi-spacecraft synergy with MEX HRSC and MRO SHARAD: Light-Toned Deposits in crater bulges. AGU Fall Meeting Abstracts, pages B1371+, Dec. 2008. [14] A. P. Rossi, et al. Stratigraphic architecture and structural control on sediment emplacement in Becquerel crater (Mars). volume 40. Lunar and Planetary Science Institute, 2009. [15] K. L. Tanaka,et al. North polar region of mars: Advances in stratigraphy, structure, and erosional modification, AUG 2008. Icarus. [16] USGS. Planetary image processing software: ISIS3. http://isis.astrogeology.usgs.gov/

Ten-Meter Scale Topography and Roughness of Mars Exploration Rovers Landing Sites and Martian Polar Regions

NASA Technical Reports Server (NTRS)

Ivanov, Anton B.

2003-01-01

The Mars Orbiter Camera (MOC) has been operating on board of the Mars Global Surveyor (MGS) spacecraft since 1998. It consists of three cameras - Red and Blue Wide Angle cameras (FOV=140 deg.) and Narrow Angle camera (FOV=0.44 deg.). The Wide Angle camera allows surface resolution down to 230 m/pixel and the Narrow Angle camera - down to 1.5 m/pixel. This work is a continuation of the project, which we have reported previously. Since then we have refined and improved our stereo correlation algorithm and have processed many more stereo pairs. We will discuss results of our stereo pair analysis located in the Mars Exploration rovers (MER) landing sites and address feasibility of recovering topography from stereo pairs (especially in the polar regions), taken during MGS 'Relay-16' mode.

Engineer's drawing of Skylab 4 Far Ultraviolet Electronographic camera

NASA Image and Video Library

1973-11-19

S73-36910 (November 1973) --- An engineer's drawing of the Skylab 4 Far Ultraviolet Electronographic camera (Experiment S201). Arrows point to various features and components of the camera. As the Comet Kohoutek streams through space at speeds of 100,000 miles per hour, the Skylab 4 crewmen will use the S201 UV camera to photograph features of the comet not visible from the Earth's surface. While the comet is some distance from the sun, the camera will be pointed through the scientific airlock in the wall of the Skylab space station Orbital Workshop (OWS). By using a movable mirror system built for the Ultraviolet Stellar Astronomy (S019) Experiment and rotating the space station, the S201 camera will be able to photograph the comet around the side of the space station. Photo credit: NASA

KSC-02pd1131

NASA Image and Video Library

2002-07-10

KENNEDY SPACE CENTER, FLA. -- Scott Minnick, with United Space Alliance, places a fiber-optic camera inside the flow line on Endeavour. Minnick wears a special viewing apparatus that sees where the camera is going. The inspection is the result of small cracks being discovered on the LH2 Main Propulsion System (MPS) flow liners in other orbiters. Endeavour is next scheduled to fly on mission STS-113.

KSC-02pd1128

NASA Image and Video Library

2002-07-10

KENNEDY SPACE CENTER, FLA. -- Scott Minnick, with United Space Alliance, places a fiber-optic camera inside the flow line on Endeavour. Minnick wears a special viewing apparatus that sees where the camera is going. The inspection is the result of small cracks being discovered on the LH2 Main Propulsion System (MPS) flow liners in other orbiters. Endeavour is next scheduled to fly on mission STS-113.

Selection of the InSight landing site

USGS Publications Warehouse

Golombek, M.; Kipp, D.; Warner, N.; Daubar, Ingrid J.; Fergason, Robin L.; Kirk, Randolph L.; Beyer, R.; Huertas, A.; Piqueux, Sylvain; Putzig, N.E.; Campbell, B.A.; Morgan, G. A.; Charalambous, C.; Pike, W. T.; Gwinner, K.; Calef, F.; Kass, D.; Mischna, M A; Ashley, J.; Bloom, C.; Wigton, N.; Hare, T.; Schwartz, C.; Gengl, H.; Redmond, L.; Trautman, M.; Sweeney, J.; Grima, C.; Smith, I. B.; Sklyanskiy, E.; Lisano, M.; Benardini, J.; Smrekar, S.E.; Lognonne, P.; Banerdt, W. B.

2017-01-01

The selection of the Discovery Program InSight landing site took over four years from initial identification of possible areas that met engineering constraints, to downselection via targeted data from orbiters (especially Mars Reconnaissance Orbiter (MRO) Context Camera (CTX) and High-Resolution Imaging Science Experiment (HiRISE) images), to selection and certification via sophisticated entry, descent and landing (EDL) simulations. Constraints on elevation (≤−2.5 km">≤−2.5 km≤−2.5 km for sufficient atmosphere to slow the lander), latitude (initially 15°S–5°N and later 3°N–5°N for solar power and thermal management of the spacecraft), ellipse size (130 km by 27 km from ballistic entry and descent), and a load bearing surface without thick deposits of dust, severely limited acceptable areas to western Elysium Planitia. Within this area, 16 prospective ellipses were identified, which lie ∼600 km north of the Mars Science Laboratory (MSL) rover. Mapping of terrains in rapidly acquired CTX images identified especially benign smooth terrain and led to the downselection to four northern ellipses. Acquisition of nearly continuous HiRISE, additional Thermal Emission Imaging System (THEMIS), and High Resolution Stereo Camera (HRSC) images, along with radar data confirmed that ellipse E9 met all landing site constraints: with slopes <15° at 84 m and 2 m length scales for radar tracking and touchdown stability, low rock abundance (<10 %) to avoid impact and spacecraft tip over, instrument deployment constraints, which included identical slope and rock abundance constraints, a radar reflective and load bearing surface, and a fragmented regolith ∼5 m thick for full penetration of the heat flow probe. Unlike other Mars landers, science objectives did not directly influence landing site selection.

Students' Target

NASA Technical Reports Server (NTRS)

2005-01-01

[figure removed for brevity, see original site] Context image for PIA03648 Ascraeus Mons

After examining numerous THEMIS images and using the JMars targeting software, eighth grade students from Charleston Middle School in Charleston, IL, selected the location of -8.37N and 276.66E for capture by the THEMIS visible camera during Mars Odyssey's sixth orbit of Mars on Nov. 22, 2005. The students are investigating relationships between channels, craters, and basins on Mars. The Charleston Middle School students participated in the Mars Student Imaging Project (MSIP) and submitted a proposal to use the THEMIS visible camera.

Image information: VIS instrument. Latitude 8.8S, Longitude 279.6E. 17 meter/pixel resolution.

Note: this THEMIS visual image has not been radiometrically nor geometrically calibrated for this preliminary release. An empirical correction has been performed to remove instrumental effects. A linear shift has been applied in the cross-track and down-track direction to approximate spacecraft and planetary motion. Fully calibrated and geometrically projected images will be released through the Planetary Data System in accordance with Project policies at a later time.

NASA's Jet Propulsion Laboratory manages the 2001 Mars Odyssey mission for NASA's Office of Space Science, Washington, D.C. The Thermal Emission Imaging System (THEMIS) was developed by Arizona State University, Tempe, in collaboration with Raytheon Santa Barbara Remote Sensing. The THEMIS investigation is led by Dr. Philip Christensen at Arizona State University. Lockheed Martin Astronautics, Denver, is the prime contractor for the Odyssey project, and developed and built the orbiter. Mission operations are conducted jointly from Lockheed Martin and from JPL, a division of the California Institute of Technology in Pasadena.

Medusae Fossae Formation

NASA Technical Reports Server (NTRS)

1998-01-01

An exotic terrain of wind-eroded ridges and residual smooth surfaces are seen in one of the highest resolution images ever taken of Mars from orbit. The Medusae Fossae formation is believed to be formed of the fragmental ejecta of huge explosive volcanic eruptions. When subjected to intense wind-blasting over hundreds of millions of years, this material erodes easily once the uppermost tougher crust is breached. In the Mars Orbiter Camera (MOC) image shown on the right, the crust, or cap rock, can be seen in the upper right part of the picture. The finely-spaced ridges are similar to features on Earth called yardangs, which are formed by intense winds plucking individual grains from, and by wind-driven sand blasting particles off, sedimentary deposits.

The MOC image was taken on October 30, 1997 at 11:05 AM PST, shortly after the Mars Global Surveyor spacecraft's 31st closest approach to Mars. The image covers an area 3.6 X 21.5 km (2.2 X 13.4 miles) at 3.6 m (12 feet) per picture element--craters only 11 m (36 feet, about the size of a swimming pool) across can be seen. The context image (left; the best Viking view of the area; VO 1 387S34) has a resolution of 240 m/pixel, or 67 times lower resolution than the MOC frame.

Malin Space Science Systems (MSSS) and the California Institute of Technology built the MOC using spare hardware from the Mars Observer mission. MSSS operates the camera from its facilities in San Diego, CA. The Jet Propulsion Laboratory's Mars Surveyor Operations Project operates the Mars Global Surveyor spacecraft with its industrial partner, Lockheed Martin Astronautics, from facilities in Pasadena, CA and Denver, CO.

Design, Development and Testing of the Miniature Autonomous Extravehicular Robotic Camera (Mini AERCam) Guidance, Navigation and Control System

NASA Technical Reports Server (NTRS)

Wagenknecht, J.; Fredrickson, S.; Manning, T.; Jones, B.

2003-01-01

Engineers at NASA Johnson Space Center have designed, developed, and tested a nanosatellite-class free-flyer intended for future external inspection and remote viewing of human spaceflight activities. The technology demonstration system, known as the Miniature Autonomous Extravehicular Robotic Camera (Mini AERCam), has been integrated into the approximate form and function of a flight system. The primary focus has been to develop a system capable of providing external views of the International Space Station. The Mini AERCam system is spherical-shaped and less than eight inches in diameter. It has a full suite of guidance, navigation, and control hardware and software, and is equipped with two digital video cameras and a high resolution still image camera. The vehicle is designed for either remotely piloted operations or supervised autonomous operations. Tests have been performed in both a six degree-of-freedom closed-loop orbital simulation and on an air-bearing table. The Mini AERCam system can also be used as a test platform for evaluating algorithms and relative navigation for autonomous proximity operations and docking around the Space Shuttle Orbiter or the ISS.

Orbiter Camera Payload System

NASA Technical Reports Server (NTRS)

1980-01-01

Components for an orbiting camera payload system (OCPS) include the large format camera (LFC), a gas supply assembly, and ground test, handling, and calibration hardware. The LFC, a high resolution large format photogrammetric camera for use in the cargo bay of the space transport system, is also adaptable to use on an RB-57 aircraft or on a free flyer satellite. Carrying 4000 feet of film, the LFC is usable over the visible to near IR, at V/h rates of from 11 to 41 milliradians per second, overlap of 10, 60, 70 or 80 percent and exposure times of from 4 to 32 milliseconds. With a 12 inch focal length it produces a 9 by 18 inch format (long dimension in line of flight) with full format low contrast resolution of 88 lines per millimeter (AWAR), full format distortion of less than 14 microns and a complement of 45 Reseau marks and 12 fiducial marks. Weight of the OCPS as supplied, fully loaded is 944 pounds and power dissipation is 273 watts average when in operation, 95 watts in standby. The LFC contains an internal exposure sensor, or will respond to external command. It is able to photograph starfields for inflight calibration upon command.

Cartography of the Luna-21 landing site and Lunokhod-2 traverse area based on Lunar Reconnaissance Orbiter Camera images and surface archive TV-panoramas

NASA Astrophysics Data System (ADS)

Karachevtseva, I. P.; Kozlova, N. A.; Kokhanov, A. A.; Zubarev, A. E.; Nadezhdina, I. E.; Patratiy, V. D.; Konopikhin, A. A.; Basilevsky, A. T.; Abdrakhimov, A. M.; Oberst, J.; Haase, I.; Jolliff, B. L.; Plescia, J. B.; Robinson, M. S.

2017-02-01

The Lunar Reconnaissance Orbiter Camera (LROC) system consists of a Wide Angle Camera (WAC) and Narrow Angle Camera (NAC). NAC images (∼0.5 to 1.7 m/pixel) reveal details of the Luna-21 landing site and Lunokhod-2 traverse area. We derived a Digital Elevation Model (DEM) and an orthomosaic for the study region using photogrammetric stereo processing techniques with NAC images. The DEM and mosaic allowed us to analyze the topography and morphology of the landing site area and to map the Lunokhod-2 rover route. The total range of topographic elevation along the traverse was found to be less than 144 m; and the rover encountered slopes of up to 20°. With the orthomosaic tied to the lunar reference frame, we derived coordinates of the Lunokhod-2 landing module and overnight stop points. We identified the exact rover route by following its tracks and determined its total length as 39.16 km, more than was estimated during the mission (37 km), which until recently was a distance record for planetary robotic rovers held for more than 40 years.

1. Context view includes Building 59 (second from left). Camera ...

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

1. Context view includes Building 59 (second from left). Camera is pointed ENE along Farragut Aveune. Buildings on left side of street are, from left: Building 856, Building 59 and Building 107. On right side of street they are, from right; Building 38, Building 452 and Building 460. - Puget Sound Naval Shipyard, Pattern Shop, Farragut Avenue, Bremerton, Kitsap County, WA

Progress in the Scandia Region Geologic Map of Mars

NASA Technical Reports Server (NTRS)

Tanaka, K. L.; Rodriguez, J. A. P.

2010-01-01

We are in the second year of a four year project to produce a geologic map of the Scandia region of Mars at 1:3,000,000 scale for publication in the USGS Scientific Investigations Map series. The primary objective of the map is to analyze and reconstruct the resurfacing history of this region in much greater detail than achieved by the previous northern plainswide mapping effort. This region includes (1) a broad swath of the Vastitas Borealis plains that includes various Scandia landforms and the Phoenix lander site; (2) part of the margin of the north polar plateau, Planum Boreum; and (3) the northern margin of the immense Alba Mons volcanic shield. We rely mostly on Mars Orbiter Laser Altimeter (MOLA) digital elevation models, Thermal Emission Imaging Spectrometer infrared and visual range, and Context Camera images for mapping and topographic analysis.

A Recent Cluster of Impacts

NASA Image and Video Library

2017-02-07

The dark spots in this enhanced-color infrared image are the recent impact craters that occurred in the Tharsis region between 2008 and 2014. These impact craters were first discovered by the Mars Context Camera (or CTX, also onboard the Mars Reconnaissance Orbiter) as a cluster of dark spots. The meteoroid that formed these craters must have broken up upon atmospheric entry and fragmented into two larger masses along with several smaller fragments, spawning at least twenty or so smaller impact craters. The dark halos around the resulting impact craters are a combination of the light-toned dust being cleared from the impact event and the deposition of the underlying dark toned materials as crater ejecta. The distribution and the pattern of the rayed ejecta suggests that the meteoroid most-likely struck from the south. http://photojournal.jpl.nasa.gov/catalog/PIA11176

Coordinates of anthropogenic features on the Moon

NASA Astrophysics Data System (ADS)

Wagner, R. V.; Nelson, D. M.; Plescia, J. B.; Robinson, M. S.; Speyerer, E. J.; Mazarico, E.

2017-02-01

High-resolution images from the Lunar Reconnaissance Orbiter Camera (LROC) Narrow Angle Camera (NAC) reveal the landing locations of recent and historic spacecraft and associated impact sites across the lunar surface. Using multiple images of each site acquired between 2009 and 2015, an improved Lunar Reconnaissance Orbiter (LRO) ephemeris, and a temperature-dependent camera orientation model, we derived accurate coordinates (<12 m) for each soft-landed spacecraft, rover, deployed scientific payload, and spacecraft impact crater that we have identified. Accurate coordinates enhance the scientific interpretations of data returned by the surface instruments and of returned samples of the Apollo and Luna sites. In addition, knowledge of the sizes and positions of craters formed as the result of impacting spacecraft provides key benchmarks into the relationship between energy and crater size, as well as calibration points for reanalyzing seismic measurements acquired during the Apollo program. We identified the impact craters for the three spacecraft that impacted the surface during the LRO mission by comparing before and after NAC images.

Background and imaging simulations for the hard X-ray camera of the MIRAX mission

NASA Astrophysics Data System (ADS)

Castro, M.; Braga, J.; Penacchioni, A.; D'Amico, F.; Sacahui, R.

2016-07-01

We report the results of detailed Monte Carlo simulations of the performance expected both at balloon altitudes and at the probable satellite orbit of a hard X-ray coded-aperture camera being developed for the Monitor e Imageador de RAios X (MIRAX) mission. Based on a thorough mass model of the instrument and detailed specifications of the spectra and angular dependence of the various relevant radiation fields at both the stratospheric and orbital environments, we have used the well-known package GEANT4 to simulate the instrumental background of the camera. We also show simulated images of source fields to be observed and calculated the detailed sensitivity of the instrument in both situations. The results reported here are especially important to researchers in this field considering that we provide important information, not easily found in the literature, on how to prepare input files and calculate crucial instrumental parameters to perform GEANT4 simulations for high-energy astrophysics space experiments.

Coordinates of Anthropogenic Features on the Moon

NASA Technical Reports Server (NTRS)

Wagner, R. V.; Nelson, D. M.; Plescia, J. B.; Robinson, M. S.; Speyerer , E. J.; Mazarico, E.

2016-01-01

High-resolution images from the Lunar Reconnaissance Orbiter Camera (LROC) Narrow Angle Camera (NAC) reveal the landing locations of recent and historic spacecraft and associated impact sites across the lunar surface. Using multiple images of each site acquired between 2009 and 2015, an improved Lunar Reconnaissance Orbiter (LRO) ephemeris, and a temperature-dependent camera orientation model, we derived accurate coordinates ( less than 12 meters) for each soft-landed spacecraft, rover, deployed scientific payload, and spacecraft impact crater that we have identified. Accurate coordinates enhance the scientific interpretations of data returned by the surface instruments and of returned samples of the Apollo and Luna sites. In addition, knowledge of the sizes and positions of craters formed as the result of impacting spacecraft provides key benchmarks into the relationship between energy and crater size, as well as calibration points for reanalyzing seismic measurements acquired during the Apollo program. We identified the impact craters for the three spacecraft that impacted the surface during the LRO mission by comparing before and after NAC images.

Apollo 8 crew shown during intravehicular activity during mission

NASA Technical Reports Server (NTRS)

1968-01-01

Astronaut Frank Borman, commander, is shown during intravehicular activity on the Apollo 8 lunar orbit mission. This still print was made from movie film taken by an on-board 16mm motion picture camera (56531); Astronaut William A. Anders, lunar module pilot, is shown during intravehicular activity on the Apollo 8 lunar orbit mission (56532); Astronaut James A. Lovell Jr., command module milot, is shown during intravehicular activity on the Apollo 8 lunar orbit mission (56533).

Variability of the symbiotic X-ray binary GX 1+4. Enhanced activity near periastron passage

NASA Astrophysics Data System (ADS)

Iłkiewicz, Krystian; Mikołajewska, Joanna; Monard, Berto

2017-05-01

Context. GX 1+4 belongs to a rare class of X-ray binaries with red giant donors, symbiotic X-ray binaries. It has a history of complicated variability on multiple timescales in the optical light and X-rays. The nature of this variability remains poorly understood. Aims: We aim to study variability of GX 1+4 on long timescale in X-ray and optical bands. Methods: We took X-ray observations from the INTEGRAL Soft Gamma-Ray Imager and RXTE All Sky Monitor. Optical observations were made with the INTEGRAL Optical Monitoring Camera. Results: The variability of GX 1+4 both in optical light and hard X-ray emission (>17 keV) is dominated by 50-70 d quasi-periodic changes. The amplitude of this variability is highest during the periastron passage, while during the potential neutron star eclipse the system is always at minimum. This confirms the 1161 d orbital period that has had been proposed for the system based on radial velocity curve. Neither the quasi-periodic variability or the orbital period are detected in soft X-ray emission (1.3-12.2 keV), where the binary shows no apparent periodicity.

Active Volcanic Eruptions on Io

NASA Technical Reports Server (NTRS)

1996-01-01

Six views of the volcanic plume named Prometheus, as seen against Io's disk and near the bright limb (edge) of the satellite by the SSI camera on the Galileo spacecraft during its second (G2) orbit of Jupiter. North is to the top of each frame. To the south-southeast of Prometheus is another bright spot that appears to be an active plume erupting from a feature named Culann Patera. Prometheus was active 17 years ago during both Voyager flybys, but no activity was detected by Voyager at Culann. Both of these plumes were seen to glow in the dark in an eclipse image acquired by the imaging camera during Galileo's first (G1) orbit, and hot spots at these locations were detected by Galileo's Near-Infrared Mapping Spectrometer.

The plumes are thought to be driven by heating sulfur dioxide in Io's subsurface into an expanding fluid or 'geyser'. The long-lived nature of these eruptions requires that a substantial supply of sulfur dioxide must be available in Io's subsurface, similar to groundwater. Sulfur dioxide gas condenses into small particles of 'snow' in the expanding plume, and the small particles scatter light and appear bright at short wavelengths. The images shown here were acquired through the shortest-wavelength filter (violet) of the Galileo camera. Prometheus is about 300 km wide and 75 km high and Culann is about 150 km wide and less than 50 km high. The images were acquired on September 4, 1996 at a range of 2,000,000 km (20 km/pixel resolution). Prometheus is named after the Greek fire god and Culann is named after the Celtic smith god.

The Jet Propulsion Laboratory, Pasadena, CA manages the Galileo mission for NASA's Office of Space Science, Washington, DC. JPL is an operating division of California Institute of Technology (Caltech).

This image and other images and data received from Galileo are posted on the World Wide Web, on the Galileo mission home page at URL http://galileo.jpl.nasa.gov. Background information and educational context for the images can be found at URL http://www.jpl.nasa.gov/galileo/sepo

SKYLAB (SL)-4 - CREW TRAINING (ORBITAL WORKSTATION [OWS]) - JSC

NASA Image and Video Library

1973-08-22

S73-32848 (10 Sept. 1973) --- Scientist-astronaut Edward G. Gibson, science pilot for the third manned Skylab mission (Skylab 4), reads the markings on a magazine of 400 feet of film for the 16mm Data Acquisition Camera (DAC), during a training exercise in the Orbital Workshop (OWS) trainer at Johnson Space Center. Photo credit: NASA

Magnetospheric Multiscale Mission Micrometeoroid/Orbital Debris Impacts

NASA Technical Reports Server (NTRS)

Williams, Trevor; Sedlak, Joseph; Shulman, Seth

2017-01-01

The MMS spacecraft are highly instrumented (accelerometers, star cameras, Sun sensors, science experiments for plasmas etc.). This presentation will discuss how data from these systems has allowed two micrometeoroid/orbital debris events to be studied: the Feb. 2, 2016 impact with an MMS4 shunt resistor, and the June 12, 2016 impact with an MMS4 wire boom.

Space telescope low scattered light camera - A model

NASA Technical Reports Server (NTRS)

Breckinridge, J. B.; Kuper, T. G.; Shack, R. V.

1982-01-01

A design approach for a camera to be used with the space telescope is given. Camera optics relay the system pupil onto an annular Gaussian ring apodizing mask to control scattered light. One and two dimensional models of ripple on the primary mirror were calculated. Scattered light calculations using ripple amplitudes between wavelength/20 wavelength/200 with spatial correlations of the ripple across the primary mirror between 0.2 and 2.0 centimeters indicate that the detection of an object a billion times fainter than a bright source in the field is possible. Detection of a Jovian type planet in orbit about alpha Centauri with a camera on the space telescope may be possible.

Hubble Space Telescope photographed by Electronic Still Camera

NASA Image and Video Library

1993-12-04

S61-E-008 (4 Dec 1993) --- This view of the Earth-orbiting Hubble Space Telescope (HST) was photographed with an Electronic Still Camera (ESC), and down linked to ground controllers soon afterward. This view was taken during rendezvous operations. Endeavour's crew captured the HST on December 4, 1993 in order to service the telescope. Over a period of five days, four of the crew members will work in alternating pairs outside Endeavour's shirt sleeve environment. Electronic still photography is a relatively new technology which provides the means for a handheld camera to electronically capture and digitize an image with resolution approaching film quality. The electronic still camera has flown as an experiment on several other shuttle missions.

Apollo 8 Mission image

NASA Image and Video Library

1968-12-21

Apollo 8,Moon, Latitude 15 degrees South,Longitude 170 degrees West. Camera Tilt Mode: High Oblique. Direction: Southeast. Sun Angle 17 degrees. Original Film Magazine was labeled E. Camera Data: 70mm Hasselblad; F-Stop: F-5.6; Shutter Speed: 1/250 second. Film Type: Kodak SO-3400 Black and White,ASA 40. Other Photographic Coverage: Lunar Orbiter 1 (LO I) S-3. Flight Date: December 21-27,1968.

The Kaguya Mission Overview

NASA Astrophysics Data System (ADS)

Kato, Manabu; Sasaki, Susumu; Takizawa, Yoshisada

2010-07-01

The Japanese lunar orbiter Kaguya (SELENE) was successfully launched by an H2A rocket on September 14, 2007. On October 4, 2007, after passing through a phasing orbit 2.5 times around the Earth, Kaguya was inserted into a large elliptical orbit circling the Moon. After the apolune altitude was lowered, Kaguya reached its nominal 100 km circular polar observation orbit on October 19. During the process of realizing the nominal orbit, two subsatellites Okina (Rstar) and Ouna (Vstar) were released into elliptical orbits with 2400 km and 800 km apolune, respectively; both elliptical orbits had 100 km perilunes. After the functionality of bus system was verified, four radar antennas and a magnetometer boom were extended, and a plasma imager was deployed. Acquisition of scientific data was carried out for 10 months of nominal mission that began in mid-December 2007. During the 8-month extended mission, magnetic fields and gamma-rays from lower orbits were measured; in addition to this, low-altitude observations were carried out using a Terrain Camera, a Multiband Imager, and an HDTV camera. New data pertaining to an intense magnetic anomaly and GRS data with higher spatial resolution were acquired to study magnetism and the elemental distribution of the Moon. After some orbital maneuvers were performed by using the saved fuel, the Kaguya spacecraft finally impacted on the southeast part of the Moon. The Kaguya team has archived the initial science data, and since November 2, 2009, the data has been made available to public, and can be accessed at the Kaguya homepage of JAXA. The team continues to also study and publish initial results in international journals. Science purposes of the mission and onboard instruments including initial science results are described in this overview.

From a Million Miles Away, NASA Camera Shows Moon Crossing Face of Earth

NASA Image and Video Library

2015-08-05

This animation still image shows the far side of the moon, illuminated by the sun, as it crosses between the DISCOVR spacecraft's Earth Polychromatic Imaging Camera (EPIC) camera and telescope, and the Earth - one million miles away. Credits: NASA/NOAA A NASA camera aboard the Deep Space Climate Observatory (DSCOVR) satellite captured a unique view of the moon as it moved in front of the sunlit side of Earth last month. The series of test images shows the fully illuminated “dark side” of the moon that is never visible from Earth. The images were captured by NASA’s Earth Polychromatic Imaging Camera (EPIC), a four megapixel CCD camera and telescope on the DSCOVR satellite orbiting 1 million miles from Earth. From its position between the sun and Earth, DSCOVR conducts its primary mission of real-time solar wind monitoring for the National Oceanic and Atmospheric Administration (NOAA).

IMAX camera in payload bay

NASA Image and Video Library

1995-12-20

STS074-361-035 (12-20 Nov 1995) --- This medium close-up view centers on the IMAX Cargo Bay Camera (ICBC) and its associated IMAX Camera Container Equipment (ICCE) at its position in the cargo bay of the Earth-orbiting Space Shuttle Atlantis. With its own ?space suit? or protective covering to protect it from the rigors of space, this version of the IMAX was able to record scenes not accessible with the in-cabin cameras. For docking and undocking activities involving Russia?s Mir Space Station and the Space Shuttle Atlantis, the camera joined a variety of in-cabin camera hardware in recording the historical events. IMAX?s secondary objectives were to film Earth views. The IMAX project is a collaboration between NASA, the Smithsonian Institution?s National Air and Space Museum (NASM), IMAX Systems Corporation, and the Lockheed Corporation to document significant space activities and promote NASA?s educational goals using the IMAX film medium.

STS-56 ESC Earth observation of New York City at night

NASA Technical Reports Server (NTRS)

1993-01-01

STS-56 electronic still camera (ESC) Earth observation image shows New York City at night as recorded on the 64th orbit of Discovery, Orbiter Vehicle (OV) 103. The image was recorded with an image intensifier on the Hand-held, Earth-oriented, Real-time, Cooperative, User-friendly, Location-targeting and Environmental System (HERCULES). HERCULES is a device that makes it simple for shuttle crewmembers to take pictures of Earth as they merely point a modified 35mm camera and shoot any interesting feature, whose latitude and longitude are automatically determined in real-time. Center coordinates on this image are 40.665 degrees north latitude and 74.048 degrees west longitude. (1/60 second exposure). Digital file name is ESC04034.IMG.

STS-56 ESC Earth observation of New Zealand (South Island)

NASA Technical Reports Server (NTRS)

1993-01-01

STS-56 electronic still camera (ESC) Earth observation image shows New Zealand (South Island) as recorded on the 45th orbit of Discovery, Orbiter Vehicle (OV) 103. Westport is easily delineated in the image, which was recorded by the Hand-held, Earth-oriented, Real-time, Cooperative, User-friendly, Location-targeting and Environmental System (HERCULES). HERCULES is a device that makes it simple for shuttle crewmembers to take pictures of Earth as they merely point a modified 35mm camera and shoot any interesting feature, whose latitude and longitude are automatically determined in real-time. Center coordinates are 41.836 degrees south latitude and 171.641 degrees east longitude. (300mm lens, no filter). Digital file name is ESC07007.IMG.

High-resolution topomapping of candidate MER landing sites with Mars Orbiter Camera narrow-angle images

USGS Publications Warehouse

Kirk, R.L.; Howington-Kraus, E.; Redding, B.; Galuszka, D.; Hare, T.M.; Archinal, B.A.; Soderblom, L.A.; Barrett, J.M.

2003-01-01

We analyzed narrow-angle Mars Orbiter Camera (MOC-NA) images to produce high-resolution digital elevation models (DEMs) in order to provide topographic and slope information needed to assess the safety of candidate landing sites for the Mars Exploration Rovers (MER) and to assess the accuracy of our results by a variety of tests. The mapping techniques developed also support geoscientific studies and can be used with all present and planned Mars-orbiting scanner cameras. Photogrammetric analysis of MOC stereopairs yields DEMs with 3-pixel (typically 10 m) horizontal resolution, vertical precision consistent with ???0.22 pixel matching errors (typically a few meters), and slope errors of 1-3??. These DEMs are controlled to the Mars Orbiter Laser Altimeter (MOLA) global data set and consistent with it at the limits of resolution. Photoclinometry yields DEMs with single-pixel (typically ???3 m) horizontal resolution and submeter vertical precision. Where the surface albedo is uniform, the dominant error is 10-20% relative uncertainty in the amplitude of topography and slopes after "calibrating" photoclinometry against a stereo DEM to account for the influence of atmospheric haze. We mapped portions of seven candidate MER sites and the Mars Pathfinder site. Safety of the final four sites (Elysium, Gusev, Isidis, and Meridiani) was assessed by mission engineers by simulating landings on our DEMs of "hazard units" mapped in the sites, with results weighted by the probability of landing on those units; summary slope statistics show that most hazard units are smooth, with only small areas of etched terrain in Gusev crater posing a slope hazard.

International Space Station (ISS)

NASA Image and Video Library

2001-09-16

The setting sun and the thin blue airglow line at Earth's horizon was captured by the International Space Station's (ISS) Expedition Three crewmembers with a digital camera. Some of the Station's components are silhouetted in the foreground. The crew was launched aboard the Space Shuttle Orbiter Discovery STS-105 mission, on August 10, 2001, replacing the Expedition Two crew. After marning the orbiting ISS for 128 consecutive days, the three returned to Earth on December 17, 2001, aboard the STS-108 mission Space Shuttle Orbiter Endeavour.

Skylab 3 crewmen shown eating in Orbital Workshop wardroom

NASA Image and Video Library

1973-08-01

S73-31705 (1 Aug. 1973) --- The three Skylab 3 crewmen are shown eating in the Orbital Workshop (OWS) wardroom of the Skylab space station in Earth orbit, in this photographic reproduction taken from a television transmission made by a color TV camera aboard the OWS. Astronaut Alan L. Bean (right), commander, illustrates eating under zero-gravity conditions upsidedown. The two other crewmen are scientist-astronaut Owen K. Garriott (left), science pilot; and astronaut Jack R. Lousma, pilot. Photo credit: NASA

Acidalia and Chryse Plains, Mars

NASA Image and Video Library

2000-06-14

Somewhere down there sits the Mars Pathfinder lander and Sojourner rover. This Mars Global Surveyor Mars Orbiter Camera view of the red planet shows the region that includes Ares Vallis and the Chryse Plains upon which both Mars Pathfinder and the Viking 1 landed in 1997 and 1976, respectively. Acidalia Planitia is the dark surface that dominates the center left. The Pathfinder site is immediately south of Acidalia, just left of center in this view. Also shown--the north polar cap is at the top, and Arabia Terra and Sinus Meridiani are to the right. The bluish-white features are clouds. This is a color composite of 9 red and 9 blue image strips taken by the Mars Global Surveyor Mars Orbiter Camera on 9 successive orbits from pole-to-pole during the calibration phase of the mission in March 1999. The color is computer-enhanced and is not shown as it would actually appear to the human eye. http://photojournal.jpl.nasa.gov/catalog/PIA02000

KSC-04pd1672

NASA Image and Video Library

2004-08-23

KENNEDY SPACE CENTER, FLA. - The Remote Manipulator System (RMS), also known as the Canadian robotic arm, for the orbiter Discovery has arrived at KSC’s Vehicle Assembly Building Lab. Seen on the left end is the shoulder pitch joint. The wrist and shoulder joints on the RMS allow the basic structure of the arm to maneuver similar to a human arm. The RMS is used to deploy and retrieve payloads, provide a mobile extension ladder or foot restraints for crew members during extravehicular activities; and to aid the flight crew members in viewing surfaces of the orbiter or payloads through a television camera on the RMS. The arm is also serving as the base for the new Orbiter Boom Sensor System (OBSS), one of the safety measures for Return to Flight, equipping the Shuttle with cameras and laser systems to inspect the Shuttle’s Thermal Protection System while in space. Discovery is scheduled for a launch planning window of March 2005 on mission STS-114.

Development of Camera Model and Geometric Calibration/validation of Xsat IRIS Imagery

NASA Astrophysics Data System (ADS)

Kwoh, L. K.; Huang, X.; Tan, W. J.

2012-07-01

XSAT, launched on 20 April 2011, is the first micro-satellite designed and built in Singapore. It orbits the Earth at altitude of 822 km in a sun synchronous orbit. The satellite carries a multispectral camera IRIS with three spectral bands - 0.52~0.60 mm for Green, 0.63~0.69 mm for Red and 0.76~0.89 mm for NIR at 12 m resolution. In the design of IRIS camera, the three bands were acquired by three lines of CCDs (NIR, Red and Green). These CCDs were physically separated in the focal plane and their first pixels not absolutely aligned. The micro-satellite platform was also not stable enough to allow for co-registration of the 3 bands with simple linear transformation. In the camera model developed, this platform stability was compensated with 3rd to 4th order polynomials for the satellite's roll, pitch and yaw attitude angles. With the camera model, the camera parameters such as the band to band separations, the alignment of the CCDs relative to each other, as well as the focal length of the camera can be validated or calibrated. The results of calibration with more than 20 images showed that the band to band along-track separation agreed well with the pre-flight values provided by the vendor (0.093° and 0.046° for the NIR vs red and for green vs red CCDs respectively). The cross-track alignments were 0.05 pixel and 5.9 pixel for the NIR vs red and green vs red CCDs respectively. The focal length was found to be shorter by about 0.8%. This was attributed to the lower operating temperature which XSAT is currently operating. With the calibrated parameters and the camera model, a geometric level 1 multispectral image with RPCs can be generated and if required, orthorectified imagery can also be produced.

QuadCam - A Quadruple Polarimetric Camera for Space Situational Awareness

NASA Astrophysics Data System (ADS)

Skuljan, J.

A specialised quadruple polarimetric camera for space situational awareness, QuadCam, has been built at the Defence Technology Agency (DTA), New Zealand, as part of collaboration with the Defence Science and Technology Laboratory (Dstl), United Kingdom. The design was based on a similar system originally developed at Dstl, with some significant modifications for improved performance. The system is made up of four identical CCD cameras looking in the same direction, but in a different plane of polarisation at 0, 45, 90 and 135 degrees with respect to the reference plane. A standard set of Stokes parameters can be derived from the four images in order to describe the state of polarisation of an object captured in the field of view. The modified design of the DTA QuadCam makes use of four small Raspberry Pi computers, so that each camera is controlled by its own computer in order to speed up the readout process and ensure that the four individual frames are taken simultaneously (to within 100-200 microseconds). In addition, a new firmware was requested from the camera manufacturer so that an output signal is generated to indicate the state of the camera shutter. A specialised GPS unit (also developed at DTA) is then used to monitor the shutter signals from the four cameras and record the actual time of exposure to an accuracy of about 100 microseconds. This makes the system well suited for the observation of fast-moving objects in the low Earth orbit (LEO). The QuadCam is currently mounted on a Paramount MEII robotic telescope mount at the newly built DTA space situational awareness observatory located on Whangaparaoa Peninsula near Auckland, New Zealand. The system will be used for tracking satellites in low Earth orbit and geostationary belt as well. The performance of the camera has been evaluated and a series of test images have been collected in order to derive the polarimetric signatures for selected satellites.

The Terrain of Margaritifer Chaos

NASA Technical Reports Server (NTRS)

1999-01-01

The jumbled and broken terrain in the picture on the left is known as chaotic terrain. Chaotic terrain was first observed in Mariner 6 and 7 images of Mars more than 30 years ago, and is thought to result from collapse after material--perhaps water or ice--was removed from the subsurface by events such as the formation of giant flood channels. The region shown here is named 'Margaritifer Chaos'. The left picture is a Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) red wide angle camera context frame that covers an area 115 km (71 miles) across. The small white box is centered at 10.3oS, 21.4oW and indicates the location of the high-resolution view on the right. The high resolution view (right) covers a small portion of the Margaritifer Chaos at 1.8 meters (6 feet) per pixel. The area shown is 3 km (1.9 miles) across. Uplands are lumpy with small bright outcrops of bedrock. Lowlands or valleys in the chaotic terrain have floors covered by light-toned windblown d rifts. This image is typical of the very highest-resolution views of the equatorial latitudes of Mars. Both pictures are illuminated from the left/upper left, north is toward the top.

The Nimbus 4 data catalog. Volume 3: Data orbits 1124-1956, 1 July - 31 August 1970

NASA Technical Reports Server (NTRS)

1971-01-01

The Nimbus 4 satellite catalog for the period of 1 July through 31 August, 1970 is presented. The subjects discussed are: (1) summary of operations, (2) orbital elements and daily sensors on table, (3) image dissector camera system montages, and (4) temperature-humidity infrared radiometer montages. Data are presented as tables and photographs.

GEMINI-TITAN (GT)-9 TEST - ASTRONAUT BEAN, ALAN - KSC

NASA Image and Video Library

1973-08-14

S73-31973 (August 1973) --- Scientist-astronaut Owen K. Garriott, Skylab 3 science pilot, looks at a map of Earth at the food table in the ward room of the Orbital Workshop (OWS). In this photographic reproduction taken from a television transmission made by a color TV camera aboard the Skylab space station cluster in Earth orbit. Photo credit: NASA

Magnificent Mars 10 Years of Mars Reconnaissance Orbiter

NASA Image and Video Library

2016-03-09

NASA's Mars Reconnaissance Orbiter has clocked more than a decade of service at the Red Planet and has yielded scientific discoveries and magnificent views of a distant world. Video uses spacecraft animation and stills set to music. These images taken by MRO's HiRISE camera are not in true color because they include infrared information in order to be optimized for geological science.

SKYLAB (SL)-2 - TELEVISION (INFLIGHT)

NASA Image and Video Library

1973-05-27

S73-26776 (26 May 1973) --- An interior view of the Orbital Workshop of the Skylab 1 space station cluster in Earth orbit can be seen in this reproduction taken from a color television transmission made by a TV camera aboard the space station. Astronaut Charles Conrad Jr., Skylab 2 commander, is floating up through the hatch. Food lockers are in the foreground. Photo credit: NASA

Lytro camera technology: theory, algorithms, performance analysis

NASA Astrophysics Data System (ADS)

Georgiev, Todor; Yu, Zhan; Lumsdaine, Andrew; Goma, Sergio

2013-03-01

The Lytro camera is the first implementation of a plenoptic camera for the consumer market. We consider it a successful example of the miniaturization aided by the increase in computational power characterizing mobile computational photography. The plenoptic camera approach to radiance capture uses a microlens array as an imaging system focused on the focal plane of the main camera lens. This paper analyzes the performance of Lytro camera from a system level perspective, considering the Lytro camera as a black box, and uses our interpretation of Lytro image data saved by the camera. We present our findings based on our interpretation of Lytro camera file structure, image calibration and image rendering; in this context, artifacts and final image resolution are discussed.

Orbital-science investigation: Part C: photogrammetry of Apollo 15 photography

USGS Publications Warehouse

Wu, Sherman S.C.; Schafer, Francis J.; Jordan, Raymond; Nakata, Gary M.; Derick, James L.

1972-01-01

Mapping of large areas of the Moon by photogrammetric methods was not seriously considered until the Apollo 15 mission. In this mission, a mapping camera system and a 61-cm optical-bar high-resolution panoramic camera, as well as a laser altimeter, were used. The mapping camera system comprises a 7.6-cm metric terrain camera and a 7.6-cm stellar camera mounted in a fixed angular relationship (an angle of 96° between the two camera axes). The metric camera has a glass focal-plane plate with reseau grids. The ground-resolution capability from an altitude of 110 km is approximately 20 m. Because of the auxiliary stellar camera and the laser altimeter, the resulting metric photography can be used not only for medium- and small-scale cartographic or topographic maps, but it also can provide a basis for establishing a lunar geodetic network. The optical-bar panoramic camera has a 135- to 180-line resolution, which is approximately 1 to 2 m of ground resolution from an altitude of 110 km. Very large scale specialized topographic maps for supporting geologic studies of lunar-surface features can be produced from the stereoscopic coverage provided by this camera.

NICMOS status and plans

NASA Technical Reports Server (NTRS)

Thompson, Rodger I.

1997-01-01

Near Infrared Camera and Multi-Object Spectrometer (NICMOS) has been in orbit for about 8 months. This is a report on its current status and future plans. Also included are some comments on particular aspects of data analysis concerning dark subtraction, shading, and removal of cosmic rays. At present NICMOS provides excellent images of high scientific content. Most of the observations utilize cameras 1 and 2 which are in excellent focus. Camera 3 is not yet within the range of the focus adjustment mechanism, but its current images are still quite excellent. In this paper we will present the status of various aspects of the NICMOS instrument.

MRO's High Resolution Imaging Science Experiment (HiRISE): Polar Science Expectations

NASA Technical Reports Server (NTRS)

McEwen, A.; Herkenhoff, K.; Hansen, C.; Bridges, N.; Delamere, W. A.; Eliason, E.; Grant, J.; Gulick, V.; Keszthelyi, L.; Kirk, R.

2003-01-01

The Mars Reconnaissance Orbiter (MRO) is expected to launch in August 2005, arrive at Mars in March 2006, and begin the primary science phase in November 2006. MRO will carry a suite of remote-sensing instruments and is designed to routinely point off-nadir to precisely target locations on Mars for high-resolution observations. The mission will have a much higher data return than any previous planetary mission, with 34 Tbits of returned data expected in the first Mars year in the mapping orbit (255 x 320 km). The HiRISE camera features a 0.5 m telescope, 12 m focal length, and 14 CCDs. We expect to acquire approximately 10,000 observations in the primary science phase (approximately 1 Mars year), including approximately 2,000 images for 1,000 stereo targets. Each observation will be accompanied by a approximately 6 m/pixel image over a 30 x 45 km region acquired by MRO s context imager. Many HiRISE images will be full resolution in the center portion of the swath width and binned (typically 4x4) on the sides. This provides two levels of context, so we step out from 0.3 m/pixel to 1.2 m/pixel to 6 m/pixel (at 300 km altitude). We expect to cover approximately 1% of Mars at better than 1.2 m/pixel, approximately 0.1% at 0.3 m/pixel, approximately 0.1% in 3 colors, and approximately 0.05% in stereo. Our major challenge is to find the dey contacts, exposures and type morphologies to observe.

STS-28 Columbia, OV-102, MS Brown uses ARRIFLEX camera on aft flight deck

NASA Image and Video Library

1989-08-13

STS028-17-033 (August 1989) --- Astronaut Mark N. Brown, STS-28 mission specialist, pauses from a session of motion-picture photography conducted through one of the aft windows on the flight deck of the Earth-orbiting Space Shuttle Columbia. He is using an Arriflex camera. The horizon of the blue and white appearing Earth and its airglow are visible in the background.

Acapulco, Mexico taken with electronic still camera

NASA Image and Video Library

1995-10-29

STS073-E-5275 (3 Nov. 1995) --- Resort City of Acapulco appears in this north-looking view, photographed from the Earth-orbiting space shuttle Columbia with the Electronic Still Camera (ESC). The airport lies on a narrow neck of land between the sea and a large coastal lagoon. This mission marks the first time NASA has released in mid-flight electronically-downlinked color images that feature geographic subject matter.

The Atlases of Vesta derived from Dawn Framing Camera images

NASA Astrophysics Data System (ADS)

Roatsch, T.; Kersten, E.; Matz, K.; Preusker, F.; Scholten, F.; Jaumann, R.; Raymond, C. A.; Russell, C. T.

2013-12-01

The Dawn Framing Camera acquired during its two HAMO (High Altitude Mapping Orbit) phases in 2011 and 2012 about 6,000 clear filter images with a resolution of about 60 m/pixel. We combined these images in a global ortho-rectified mosaic of Vesta (60 m/pixel resolution). Only very small areas near the northern pole were still in darkness and are missing in the mosaic. The Dawn Framing Camera also acquired about 10,000 high-resolution clear filter images (about 20 m/pixel) of Vesta during its Low Altitude Mapping Orbit (LAMO). Unfortunately, the northern part of Vesta was still in darkness during this phase, good illumination (incidence angle < 70°) was only available for 66.8 % of the surface [1]. We used the LAMO images to calculate another global mosaic of Vesta, this time with 20 m/pixel resolution. Both global mosaics were used to produce atlases of Vesta: a HAMO atlas with 15 tiles at a scale of 1:500,000 and a LAMO atlas with 30 tiles at a scale between 1:200,000 and 1:225,180. The nomenclature used in these atlases is based on names and places historically associated with the Roman goddess Vesta, and is compliant with the rules of the IAU. 65 names for geological features were already approved by the IAU, 39 additional names are currently under review. Selected examples of both atlases will be shown in this presentation. Reference: [1]Roatsch, Th., etal., High-resolution Vesta Low Altitude Mapping Orbit Atlas derived from Dawn Framing Camera images. Planetary and Space Science (2013), http://dx.doi.org/10.1016/j.pss.2013.06.024i

The Effect of Camera Angle and Image Size on Source Credibility and Interpersonal Attraction.

ERIC Educational Resources Information Center

McCain, Thomas A.; Wakshlag, Jacob J.

The purpose of this study was to examine the effects of two nonverbal visual variables (camera angle and image size) on variables developed in a nonmediated context (source credibility and interpersonal attraction). Camera angle and image size were manipulated in eight video taped television newscasts which were subsequently presented to eight…

An ordinary camera in an extraordinary location: Outreach with the Mars Webcam

NASA Astrophysics Data System (ADS)

Ormston, T.; Denis, M.; Scuka, D.; Griebel, H.

2011-09-01

The European Space Agency's Mars Express mission was launched in 2003 and was Europe's first mission to Mars. On-board was a small camera designed to provide ‘visual telemetry’ of the separation of the Beagle-2 lander. After achieving its goal it was shut down while the primary science mission of Mars Express got underway. In 2007 this camera was reactivated by the flight control team of Mars Express for the purpose of providing public education and outreach—turning it into the ‘Mars Webcam’.The camera is a small, 640×480 pixel colour CMOS camera with a wide-angle 30°×40° field of view. This makes it very similar in almost every way to the average home PC webcam. The major difference is that this webcam is not in an average location but is instead in orbit around Mars. On a strict basis of non-interference with the primary science activities, the camera is turned on to provide unique wide-angle views of the planet below.A highly automated process ensures that the observations are scheduled on the spacecraft and then uploaded to the internet as rapidly as possible. There is no intermediate stage, so that visitors to the Mars Webcam blog serve as ‘citizen scientists’. Full raw datasets and processing instructions are provided along with a mechanism to allow visitors to comment on the blog. Members of the public are encouraged to use this in either a personal or an educational context and work with the images. We then take their excellent work and showcase it back on the blog. We even apply techniques developed by them to improve the data and webcam experience for others.The accessibility and simplicity of the images also makes the data ideal for educational use, especially as educational projects can then be showcased on the site as inspiration for others. The oft-neglected target audience of space enthusiasts is also important as this allows them to participate as part of an interplanetary instrument team.This paper will cover the history of the project and the technical background behind using the camera and linking the results to an accessible blog format. It will also cover the outreach successes of the project, some of the contributions from the Mars Webcam community, opportunities to use and work with the Mars Webcam and plans for future uses of the camera.

SKYLAB (SL)-3 - TELEVISION

NASA Image and Video Library

1973-09-29

S73-34619 (28 July 1973) --- A composite of four frames taken from 16mm movie camera footage showing an overhead view of the Skylab space station cluster in Earth orbit. The Maurer motion picture camera scenes were being filmed during the Skylab 3 Command/Service Module's (CSM) first "fly around" inspection of the space station. Close comparison of the four frames reveals movement of the improvised parasol solar shield over the Orbital Workshop (OWS). The "flapping" of the sun shade was caused from the exhaust of the reaction control subsystem (RCS) thrusters of the Skylab 3 CSM. The one remaining solar array system wing on the OWS is in the lower left background. The solar panel in the lower left foreground is on the Apollo Telescope Mount (ATM). Photo credit: NASA

Astronauts Sullivan and Leestma perform in-space simulation of refueling

NASA Image and Video Library

1984-10-14

S84-43432 (11 Oct. 1984) --- Appearing small in the center background of this image, astronauts Kathryn D. Sullivan, left, and David C. Leestma, both 41-G mission specialists, perform an in-space simulation of refueling another spacecraft in orbit. Their station on the space shuttle Challenger is the orbital refueling system (ORS), positioned on the mission peculiar support structure (MPR ESS). The Large Format Camera (LFC) is left of the two mission specialists. In the left foreground is the antenna for the shuttle imaging radar (SIR-B) system onboard. The Canadian-built remote manipulator system (RMS) is positioned to allow close-up recording capability of the busy scene. A 50mm lens on a 70mm camera was used to photograph this scene. Photo credit: NASA

Mars Global Surveyor: 7 Years in Orbit!

NASA Technical Reports Server (NTRS)

2004-01-01

12 September 2004 Today, 12 September 2004, the Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) team celebrates 7 Earth years orbiting Mars. MGS first reached the red planet and performed its critical orbit insertion burn on 12 September 1997. Over the past 7 years, MOC has returned over 170,000 images; its narrow angle camera has covered about 4.5% of the surface, and its wide angle cameras have viewed 100% of the planet nearly everyday.

At this time, MOC is not acquiring data because Mars is on the other side of the Sun relative to Earth. This period, known as Solar Conjunction, occurs about once every 26 months. During Solar Conjunction, no radio communications from spacecraft that are orbiting or have landed on Mars can be received. MOC was turned off on 7 September and is expected to resume operations on 25 September 2004, when Mars re-emerges from behind the Sun.

The rotating color image of Mars shown here was compiled from MOC red and blue wide angle daily global images acquired exactly 1 Mars year ago on 26 October 2002 (Ls 86.4o). In other words, Mars today (12 September 2004) should look about the same as the view provided here. Presently, Mars is in very late northern spring, and the north polar cap has retreated almost to its summer configuration. Water ice clouds form each afternoon at this time of year over the large volcanoes in the Tharsis and Elysium regions. A discontinuous belt of clouds forms over the martian equator; it is most prominent north of the Valles Marineris trough system. In the southern hemisphere, it is late autumn and the giant Hellas Basin floor is nearly white with seasonal frost cover. The south polar cap is not visible, it is enveloped in seasonal darkness. The northern summer and southern winter seasons will begin on 20 September 2004.

Thermal Effects on Camera Focal Length in Messenger Star Calibration and Orbital Imaging

NASA Astrophysics Data System (ADS)

Burmeister, S.; Elgner, S.; Preusker, F.; Stark, A.; Oberst, J.

2018-04-01

We analyse images taken by the MErcury Surface, Space ENviorment, GEochemistry, and Ranging (MESSENGER) spacecraft for the camera's thermal response in the harsh thermal environment near Mercury. Specifically, we study thermally induced variations in focal length of the Mercury Dual Imaging System (MDIS). Within the several hundreds of images of star fields, the Wide Angle Camera (WAC) typically captures up to 250 stars in one frame of the panchromatic channel. We measure star positions and relate these to the known star coordinates taken from the Tycho-2 catalogue. We solve for camera pointing, the focal length parameter and two non-symmetrical distortion parameters for each image. Using data from the temperature sensors on the camera focal plane we model a linear focal length function in the form of f(T) = A0 + A1 T. Next, we use images from MESSENGER's orbital mapping mission. We deal with large image blocks, typically used for the production of a high-resolution digital terrain models (DTM). We analyzed images from the combined quadrangles H03 and H07, a selected region, covered by approx. 10,600 images, in which we identified about 83,900 tiepoints. Using bundle block adjustments, we solved for the unknown coordinates of the control points, the pointing of the camera - as well as the camera's focal length. We then fit the above linear function with respect to the focal plane temperature. As a result, we find a complex response of the camera to thermal conditions of the spacecraft. To first order, we see a linear increase by approx. 0.0107 mm per degree temperature for the Narrow-Angle Camera (NAC). This is in agreement with the observed thermal response seen in images of the panchromatic channel of the WAC. Unfortunately, further comparisons of results from the two methods, both of which use different portions of the available image data, are limited. If leaving uncorrected, these effects may pose significant difficulties in the photogrammetric analysis, specifically these may be responsible for erroneous longwavelength trends in topographic models.

Attempt to the detection of small wildfire by the uncooled micro bolometer camera onboard 50 kg class satellite

NASA Astrophysics Data System (ADS)

Fukuhara, T.; Kouyama, T.; Kato, S.; Nakamura, R.

2016-12-01

University International Formation Mission (UNIFORM) in Japan started in 2011 is an ambitious project that specialized to surveillance of small wildfire to contribute to provide fire information for initial suppression. Final aim of the mission is to construct a constellation with several 50 kg class satellites for frequent and exclusive observation. The uncooled micro-bolometer camera with 640 x 480 pixels based on commercial products has been newly developed for the first satellite. It has been successfully launched on 24 May 2014 and injected to the Sun-Synchronous orbit at local time of 12:00 with altitude of 628 km. The camera has been detected considerable hotspots not only wildfire but also volcanoes. Brightness temperature observed on orbit has been verified and scale of observed wildfire has been roughly presumed; the smallest wildfire ever detected has flame zone less than 2 x 103 m2. It is one tenth of initial requirement estimated in design process; our camera has enough ability to discover small wildfire and to provide beneficial information for fire control with low cost and quick fabrication; it would contribute to practical utility especially in developing nations. A next camera is available for new wildfire mission with satellite constellation; it has already developed for flight. Pixel arrays increasing to 1024 x 768, spatial resolution becomes fine to detect smaller wildfire whereas the swath of image is kept. This camera would be applied to the future planetary mission for Mars and Asteroid explore, too. When it observes planetary surface, thermal inertia can be estimated from continuous observation. When it observes atmosphere, cloud-top altitude can be estimated from horizontal temperature distribution.

Retrieving Atmospheric Dust Loading on Mars Using Engineering Cameras and MSL's Mars Hand Lens Imager (MAHLI)

NASA Astrophysics Data System (ADS)

Wolfe, C. A.; Lemmon, M. T.

2015-12-01

Dust in the Martian atmosphere influences energy deposition, dynamics, and the viability of solar powered exploration vehicles. The Viking, Pathfinder, Spirit, Opportunity, Phoenix, and Curiosity landers and rovers each included the ability to image the Sun with a science camera equipped with a neutral density filter. Direct images of the Sun not only provide the ability to measure extinction by dust and ice in the atmosphere, but also provide a variety of constraints on the Martian dust and water cycles. These observations have been used to characterize dust storms, to provide ground truth sites for orbiter-based global measurements of dust loading, and to help monitor solar panel performance. In the cost-constrained environment of Mars exploration, future missions may omit such cameras, as the solar-powered InSight mission has. We seek to provide a robust capability of determining atmospheric opacity from sky images taken with cameras that have not been designed for solar imaging, such as the engineering cameras onboard Opportunity and the Mars Hand Lens Imager (MAHLI) on Curiosity. Our investigation focuses primarily on the accuracy of a method that determines optical depth values using scattering models that implement the ratio of sky radiance measurements at different elevation angles, but at the same scattering angle. Operational use requires the ability to retrieve optical depth on a timescale useful to mission planning, and with an accuracy and precision sufficient to support both mission planning and validating orbital measurements. We will present a simulation-based assessment of imaging strategies and their error budgets, as well as a validation based on the comparison of direct extinction measurements from archival Navcam, Hazcam, and MAHLI camera data.

Olympus Mons in Color

NASA Technical Reports Server (NTRS)

1997-01-01

Sections of MOC images P024_01 and P024_02, shown here in color composite form, were acquired with the low resolution red and blue wide angle cameras over a 5 minute period starting when Mars Global Surveyor was at its closest point to the planet at the beginning of its 24th orbit (around 4:00 AM PDT on October 20, 1997). To make this image, a third component (green) was synthesized from the red and blue images. During the imaging period, the camera was pointed straight down towards the martian surface, 176 km (109 miles) below the spacecraft. During the time it took to acquire the image, the spacecraft rose to an altitude of 310 km (193 miles). Owing to data camera scanning rate and data volume constraints, the image was acquired at a resolution of roughly 1 km (0.609 mile) per pixel. The image shown here covers an area from 12o to 26o N latitude and 126o N to 138o W longitude. The image is oriented with north to the top.

As has been noted in other MOC releases, Olympus Mons is the largest of the major Tharsis volcanoes, rising 25 km (15.5 miles) and stretching over nearly 550 km (340 miles) east-west. The summit caldera, a composite of as many as seven roughly circular collapse depressions, is 66 by 83 km (41 by 52 miles) across. Also seen in this image are water-ice clouds that accumulate around and above the volcano during the late afternoon (at the time the image was acquired, the summit was at 5:30 PM local solar time). To understand the value of orbital observations, compare this image with the two taken during approach (PIA00929 and PIA00936), that are representative of the best resolution from Earth.

Through Monday, October 28, the MOC had acquired a total of 132 images, most of which were at low sun elevation angles. Of these images, 74 were taken with the high resolution narrow angle camera and 58 with the low resolution wide angle cameras. Twenty-eight narrow angle and 24 wide angle images were taken after the suspension of aerobraking. These images, including the one shown above, are among the best returned so far.

Launched on November 7, 1996, Mars Global Surveyor entered Mars orbit on Thursday, September 11, 1997. The original mission plan called for using friction with the planet's atmosphere to reduce the orbital energy, leading to a two-year mapping mission from close, circular orbit (beginning in March 1998). Owing to difficulties with one of the two solar panels, aerobraking was suspended in mid-October and is scheduled to resume in mid-November. Many of the original objectives of the mission, and in particular those of the camera, are likely to be accomplished as the mission progresses.

Malin Space Science Systems and the California Institute of Technology built the MOC using spare hardware from the Mars Observer mission. MSSS operates the camera from its facilities in San Diego, CA. The Jet Propulsion Laboratory's Mars Surveyor Operations Project operates the Mars Global Surveyor spacecraft with its industrial partner, Lockheed Martin Astronautics, from facilities in Pasadena, CA and Denver, CO.

STS-61 Space Shuttle mission report

NASA Technical Reports Server (NTRS)

Fricke, Robert W., Jr.

1994-01-01

The STS-61 Space Shuttle Program Mission Report summarizes the Hubble Space Telescope (HST) servicing mission as well as the Orbiter, External Tank (ET), Solid Rocket Booster (SRB), Redesigned Solid Rocket Motor (RSRM), and the Space Shuttle main engine (SSME) systems performance during the fifty-ninth flight of the Space Shuttle Program and fifth flight of the Orbiter vehicle Endeavour (OV-105). In addition to the Orbiter, the flight vehicle consisted of an ET designated as ET-60; three SSME's which were designated as serial numbers 2019, 2033, and 2017 in positions 1, 2, and 3, respectively; and two SRB's which were designated BI-063. The RSRM's that were installed in each SRB were designated as 360L023A (lightweight) for the left SRB, and 360L023B (lightweight) for the right SRB. This STS-61 Space Shuttle Program Mission Report fulfills the Space Shuttle Program requirement as documented in NSTS 07700, Volume 8, Appendix E. That document requires that each major organizational element supporting the Program report the results of its hardware evaluation and mission performance plus identify all related in-flight anomalies. The primary objective of the STS-61 mission was to perform the first on-orbit servicing of the Hubble Space Telescope. The servicing tasks included the installation of new solar arrays, replacement of the Wide Field/Planetary Camera I (WF/PC I) with WF/PC II, replacement of the High Speed Photometer (HSP) with the Corrective Optics Space Telescope Axial Replacement (COSTAR), replacement of rate sensing units (RSU's) and electronic control units (ECU's), installation of new magnetic sensing systems and fuse plugs, and the repair of the Goddard High Resolution Spectrometer (GHRS). Secondary objectives were to perform the requirements of the IMAX Cargo Bay Camera (ICBC), the IMAX Camera, and the Air Force Maui Optical Site (AMOS) Calibration Test.

Co-registration of Laser Altimeter Tracks with Digital Terrain Models and Applications in Planetary Science

NASA Technical Reports Server (NTRS)

Glaeser, P.; Haase, I.; Oberst, J.; Neumann, G. A.

2013-01-01

We have derived algorithms and techniques to precisely co-register laser altimeter profiles with gridded Digital Terrain Models (DTMs), typically derived from stereo images. The algorithm consists of an initial grid search followed by a least-squares matching and yields the translation parameters at sub-pixel level needed to align the DTM and the laser profiles in 3D space. This software tool was primarily developed and tested for co-registration of laser profiles from the Lunar Orbiter Laser Altimeter (LOLA) with DTMs derived from the Lunar Reconnaissance Orbiter (LRO) Narrow Angle Camera (NAC) stereo images. Data sets can be co-registered with positional accuracy between 0.13 m and several meters depending on the pixel resolution and amount of laser shots, where rough surfaces typically result in more accurate co-registrations. Residual heights of the data sets are as small as 0.18 m. The software can be used to identify instrument misalignment, orbit errors, pointing jitter, or problems associated with reference frames being used. Also, assessments of DTM effective resolutions can be obtained. From the correct position between the two data sets, comparisons of surface morphology and roughness can be made at laser footprint- or DTM pixel-level. The precise co-registration allows us to carry out joint analysis of the data sets and ultimately to derive merged high-quality data products. Examples of matching other planetary data sets, like LOLA with LRO Wide Angle Camera (WAC) DTMs or Mars Orbiter Laser Altimeter (MOLA) with stereo models from the High Resolution Stereo Camera (HRSC) as well as Mercury Laser Altimeter (MLA) with Mercury Dual Imaging System (MDIS) are shown to demonstrate the broad science applications of the software tool.

Astronaut Jack Lousma looks at map of Earth in ward room of Skylab cluster

NASA Image and Video Library

1973-08-01

S73-34193 (1 Aug. 1973) --- Astronaut Jack R. Lousma, Skylab 3 pilot, looks at a map of Earth at the food table in the ward room of the Orbital Workshop (OWS). In this photographic reproduction taken from a television transmission made by a color TV camera aboard the Skylab space station cluster in Earth orbit. Photo credit: NASA

The Nimbus 4 data catalog. Volume 8: Data orbits 5206-10,120, 1 May 1971 - 30 April 1972

NASA Technical Reports Server (NTRS)

1972-01-01

Data from various instruments onboard the Nimbus 4 are presented, including the image dissector camera system, the temperature-humidity infrared radiometer, infrared interferometer spectrometer, and monitor of ultraviolet solar energy experiments. This data was collected from 1 May 1971 to 30 Apr. 1972. Orbital elements and daily sensor data are presented in tabular form.

Accurate Mars Express orbits to improve the determination of the mass and ephemeris of the Martian moons

NASA Astrophysics Data System (ADS)

Rosenblatt, P.; Lainey, V.; Le Maistre, S.; Marty, J. C.; Dehant, V.; Pätzold, M.; Van Hoolst, T.; Häusler, B.

2008-05-01

The determination of the ephemeris of the Martian moons has benefited from observations of their plane-of-sky positions derived from images taken by cameras onboard spacecraft orbiting Mars. Images obtained by the Super Resolution Camera (SRC) onboard Mars Express (MEX) have been used to derive moon positions relative to Mars on the basis of a fit of a complete dynamical model of their motion around Mars. Since, these positions are computed from the relative position of the spacecraft when the images are taken, those positions need to be known as accurately as possible. An accurate MEX orbit is obtained by fitting two years of tracking data of the Mars Express Radio Science (MaRS) experiment onboard MEX. The average accuracy of the orbits has been estimated to be around 20-25 m. From these orbits, we have re-derived the positions of Phobos and Deimos at the epoch of the SRC observations and compared them with the positions derived by using the MEX orbits provided by the ESOC navigation team. After fit of the orbital model of Phobos and Deimos, the gain in precision in the Phobos position is roughly 30 m, corresponding to the estimated gain of accuracy of the MEX orbits. A new solution of the GM of the Martian moons has also been obtained from the accurate MEX orbits, which is consistent with previous solutions and, for Phobos, is more precise than the solution from the Mars Global Surveyor (MGS) and Mars Odyssey (ODY) tracking data. It will be further improved with data from MEX-Phobos closer encounters (at a distance less than 300 km). This study also demonstrates the advantage of combining observations of the moon positions from a spacecraft and from the Earth to assess the real accuracy of the spacecraft orbit. In turn, the natural satellite ephemerides can be improved and participate to a better knowledge of the origin and evolution of the Martian moons.

Investigation of the influence of spatial degrees of freedom on thermal infrared measurement

NASA Astrophysics Data System (ADS)

Fleuret, Julien R.; Yousefi, Bardia; Lei, Lei; Djupkep Dizeu, Frank Billy; Zhang, Hai; Sfarra, Stefano; Ouellet, Denis; Maldague, Xavier P. V.

2017-05-01

Long Wavelength Infrared (LWIR) cameras can provide a representation of a part of the light spectrum that is sensitive to temperature. These cameras also named Thermal Infrared (TIR) cameras are powerful tools to detect features that cannot be seen by other imaging technologies. For instance they enable defect detection in material, fever and anxiety in mammals and many other features for numerous applications. However, the accuracy of thermal cameras can be affected by many parameters; the most critical involves the relative position of the camera with respect to the object of interest. Several models have been proposed in order to minimize the influence of some of the parameters but they are mostly related to specific applications. Because such models are based on some prior informations related to context, their applicability to other contexts cannot be easily assessed. The few models remaining are mostly associated with a specific device. In this paper the authors studied the influence of the camera position on the measurement accuracy. Modeling of the position of the camera from the object of interest depends on many parameters. In order to propose a study which is as accurate as possible, the position of the camera will be represented as a five dimensions model. The aim of this study is to investigate and attempt to introduce a model which is as independent from the device as possible.

Machine vision for real time orbital operations

NASA Technical Reports Server (NTRS)

Vinz, Frank L.

1988-01-01

Machine vision for automation and robotic operation of Space Station era systems has the potential for increasing the efficiency of orbital servicing, repair, assembly and docking tasks. A machine vision research project is described in which a TV camera is used for inputing visual data to a computer so that image processing may be achieved for real time control of these orbital operations. A technique has resulted from this research which reduces computer memory requirements and greatly increases typical computational speed such that it has the potential for development into a real time orbital machine vision system. This technique is called AI BOSS (Analysis of Images by Box Scan and Syntax).

MS Musgrave conducts CFES experiment on middeck

NASA Image and Video Library

1983-04-09

STS006-03-381 (4-9 April 1983) --- Astronaut F. Story Musgrave, STS-6 mission specialist, monitors the activity of a sample in the continuous flow electrophoresis system (CFES) aboard the Earth-orbiting space shuttle Challenger. Dr. Musgrave is in the middeck area of the spacecraft. He has mounted a 35mm camera to record the activity through the window of the experiment. This frame was also photographed with a 35mm camera. Photo credit: NASA

Indirectly Funded Research and Exploratory Development at the Applied Physics Laboratory, Fiscal Year 1978.

DTIC Science & Technology

1979-12-01

used to reduce costs ). The orbital data from the prototype ion composi- tion telescope will not only be of great scientific interest -pro- viding for...active device whose transfer function may be almost arbitrarily defined, and cost and production trends permit contemplation of networks containing...developing solid-state television camera systems based on CCD imagers. RICA hopes to produce a $500 color camera for consumer use. Fairchild and Texas

Earth observation

NASA Image and Video Library

2014-09-04

ISS040-E-129950 (4 Sept. 2014) --- In this photograph. taken by one of the Expedition 40 crew members aboard the Earth-orbiting International Space Station, the orange spot located in the very center is the sun, which appears to be sitting on Earth's limb. At far right, a small bright spot is believed to be a reflection from somewhere in the camera system or something on the orbital outpost. When the photographed was exposed, the orbital outpost was flying at an altutude of 226 nautical miles above a point near French Polynesia in the Pacific Ocean.

Astronaut Owen Garriott trims hair of Astronaut Alan Bean

NASA Image and Video Library

1973-08-19

SL3-108-1292 (19 Aug. 1973) --- Scientist-astronaut Owen K. Garriott, Skylab 3 science pilot, trims the hair of astronaut Alan L. Bean, commander, in this onboard photograph from the Skylab Orbital Workshop (OWS) in Earth orbit. Astronaut Jack R. Lousma, pilot, took this picture with a 35mm Nikon camera. Bean holds a vacuum hose to gather in loose hair. The crew of the second manned Skylab flight went on to successfully complete 59 days aboard the Skylab space station cluster in Earth orbit. Photo credit: NASA

Geographic Information Systems and Martian Data: Compatibility and Analysis

NASA Technical Reports Server (NTRS)

Jones, Jennifer L.

2005-01-01

Planning future landed Mars missions depends on accurate, informed data. This research has created and used spatially referenced instrument data from NASA missions such as the Thermal Emission Imaging System (THEMIS) on the Mars Odyssey Orbiter and the Mars Orbital Camera (MOC) on the Mars Global Surveyor (MGS) Orbiter. Creating spatially referenced data enables its use in Geographic Information Systems (GIS) such as ArcGIS. It has then been possible to integrate this spatially referenced data with global base maps and build and populate location based databases that are easy to access.

Beats: Video Monitors and Cameras.

ERIC Educational Resources Information Center

Worth, Frazier

1996-01-01

Presents a method to teach the concept of beats as a generalized phenomenon rather than teaching it only in the context of sound. Involves using a video camera to film a computer terminal, 16-mm projector, or TV monitor. (JRH)

Payload canister transporter in VPF clean room

NASA Technical Reports Server (NTRS)

1984-01-01

Payload canister transporter in Vertical Processing Facility (VPF) Clean Room loaded with Earth Radiation Budget Satellite (ERBS), Large Format Camera (LFC) and Orbital Refueling System (ORS) for STS-41G mission.

Mars Orbiter Camera Views the 'Face on Mars' - Best View from Viking

NASA Technical Reports Server (NTRS)

1998-01-01

Shortly after midnight Sunday morning (5 April 1998 12:39 AM PST), the Mars Orbiter Camera (MOC) on the Mars Global Surveyor (MGS) spacecraft successfully acquired a high resolution image of the 'Face on Mars' feature in the Cydonia region. The image was transmitted to Earth on Sunday, and retrieved from the mission computer data base Monday morning (6 April 1998). The image was processed at the Malin Space Science Systems (MSSS) facility 9:15 AM and the raw image immediately transferred to the Jet Propulsion Laboratory (JPL) for release to the Internet. The images shown here were subsequently processed at MSSS.

The picture was acquired 375 seconds after the spacecraft's 220th close approach to Mars. At that time, the 'Face', located at approximately 40.8o N, 9.6o W, was 275 miles (444 km) from the spacecraft. The 'morning' sun was 25o above the horizon. The picture has a resolution of 14.1 feet (4.3 meters) per pixel, making it ten times higher resolution than the best previous image of the feature, which was taken by the Viking Mission in the mid-1970's. The full image covers an area 2.7 miles (4.4 km) wide and 25.7 miles (41.5 km) long.

This Viking Orbiter image is one of the best Viking pictures of the area Cydonia where the 'Face' is located. Marked on the image are the 'footprint' of the high resolution (narrow angle) Mars Orbiter Camera image and the area seen in enlarged views (dashed box). See PIA01440-1442 for these images in raw and processed form.

Malin Space Science Systems and the California Institute of Technology built the MOC using spare hardware from the Mars Observer mission. MSSS operates the camera from its facilities in San Diego, CA. The Jet Propulsion Laboratory's Mars Surveyor Operations Project operates the Mars Global Surveyor spacecraft with its industrial partner, Lockheed Martin Astronautics, from facilities in Pasadena, CA and Denver, CO.

Machine Vision for Relative Spacecraft Navigation During Approach to Docking

NASA Technical Reports Server (NTRS)

Chien, Chiun-Hong; Baker, Kenneth

2011-01-01

This paper describes a machine vision system for relative spacecraft navigation during the terminal phase of approach to docking that: 1) matches high contrast image features of the target vehicle, as seen by a camera that is bore-sighted to the docking adapter on the chase vehicle, to the corresponding features in a 3d model of the docking adapter on the target vehicle and 2) is robust to on-orbit lighting. An implementation is provided for the case of the Space Shuttle Orbiter docking to the International Space Station (ISS) with quantitative test results using a full scale, medium fidelity mock-up of the ISS docking adapter mounted on a 6-DOF motion platform at the NASA Marshall Spaceflight Center Flight Robotics Laboratory and qualitative test results using recorded video from the Orbiter Docking System Camera (ODSC) during multiple orbiter to ISS docking missions. The Natural Feature Image Registration (NFIR) system consists of two modules: 1) Tracking which tracks the target object from image to image and estimates the position and orientation (pose) of the docking camera relative to the target object and 2) Acquisition which recognizes the target object if it is in the docking camera Field-of-View and provides an approximate pose that is used to initialize tracking. Detected image edges are matched to the 3d model edges whose predicted location, based on the pose estimate and its first time derivative from the previous frame, is closest to the detected edge1 . Mismatches are eliminated using a rigid motion constraint. The remaining 2d image to 3d model matches are used to make a least squares estimate of the change in relative pose from the previous image to the current image. The changes in position and in attitude are used as data for two Kalman filters whose outputs are smoothed estimate of position and velocity plus attitude and attitude rate that are then used to predict the location of the 3d model features in the next image.

Calibration of the Lunar Reconnaissance Orbiter Camera

NASA Astrophysics Data System (ADS)

Tschimmel, M.; Robinson, M. S.; Humm, D. C.; Denevi, B. W.; Lawrence, S. J.; Brylow, S.; Ravine, M.; Ghaemi, T.

2008-12-01

The Lunar Reconnaissance Orbiter Camera (LROC) onboard the NASA Lunar Reconnaissance Orbiter (LRO) spacecraft consists of three cameras: the Wide-Angle Camera (WAC) and two identical Narrow Angle Cameras (NAC-L, NAC-R). The WAC is push-frame imager with 5 visible wavelength filters (415 to 680 nm) at a spatial resolution of 100 m/pixel and 2 UV filters (315 and 360 nm) with a resolution of 400 m/pixel. In addition to the multicolor imaging the WAC can operate in monochrome mode to provide a global large- incidence angle basemap and a time-lapse movie of the illumination conditions at both poles. The WAC has a highly linear response, a read noise of 72 e- and a full well capacity of 47,200 e-. The signal-to-noise ratio in each band is 140 in the worst case. There are no out-of-band leaks and the spectral response of each filter is well characterized. Each NAC is a monochrome pushbroom scanner, providing images with a resolution of 50 cm/pixel from a 50-km orbit. A single NAC image has a swath width of 2.5 km and a length of up to 26 km. The NACs are mounted to acquire side-by-side imaging for a combined swath width of 5 km. The NAC is designed to fully characterize future human and robotic landing sites in terms of topography and hazard risks. The North and South poles will be mapped on a 1-meter-scale poleward of 85.5° latitude. Stereo coverage can be provided by pointing the NACs off-nadir. The NACs are also highly linear. Read noise is 71 e- for NAC-L and 74 e- for NAC-R and the full well capacity is 248,500 e- for NAC-L and 262,500 e- for NAC- R. The focal lengths are 699.6 mm for NAC-L and 701.6 mm for NAC-R; the system MTF is 28% for NAC-L and 26% for NAC-R. The signal-to-noise ratio is at least 46 (terminator scene) and can be higher than 200 (high sun scene). Both NACs exhibit a straylight feature, which is caused by out-of-field sources and is of a magnitude of 1-3%. However, as this feature is well understood it can be greatly reduced during ground processing. All three cameras were calibrated in the laboratory under ambient conditions. Future thermal vacuum tests will characterize critical behaviors across the full range of lunar operating temperatures. In-flight tests will check for changes in response after launch and provide key data for meeting the requirements of 1% relative and 10% absolute radiometric calibration.

Hypervelocity impact studies using a rotating mirror framing laser shadowgraph camera

NASA Technical Reports Server (NTRS)

Parker, Vance C.; Crews, Jeanne Lee

1988-01-01

The need to study the effects of the impact of micrometeorites and orbital debris on various space-based systems has brought together the technologies of several companies and individuals in order to provide a successful instrumentation package. A light gas gun was employed to accelerate small projectiles to speeds in excess of 7 km/sec. Their impact on various targets is being studied with the help of a specially designed continuous-access rotating-mirror framing camera. The camera provides 80 frames of data at up to 1 x 10 to the 6th frames/sec with exposure times of 20 nsec.

Optical registration of spaceborne low light remote sensing camera

NASA Astrophysics Data System (ADS)

Li, Chong-yang; Hao, Yan-hui; Xu, Peng-mei; Wang, Dong-jie; Ma, Li-na; Zhao, Ying-long

2018-02-01

For the high precision requirement of spaceborne low light remote sensing camera optical registration, optical registration of dual channel for CCD and EMCCD is achieved by the high magnification optical registration system. System integration optical registration and accuracy of optical registration scheme for spaceborne low light remote sensing camera with short focal depth and wide field of view is proposed in this paper. It also includes analysis of parallel misalignment of CCD and accuracy of optical registration. Actual registration results show that imaging clearly, MTF and accuracy of optical registration meet requirements, it provide important guarantee to get high quality image data in orbit.

An Overview of the HST Advanced Camera for Surveys' On-orbit Performance

NASA Astrophysics Data System (ADS)

Hartig, G. F.; Ford, H. C.; Illingworth, G. D.; Clampin, M.; Bohlin, R. C.; Cox, C.; Krist, J.; Sparks, W. B.; De Marchi, G.; Martel, A. R.; McCann, W. J.; Meurer, G. R.; Sirianni, M.; Tsvetanov, Z.; Bartko, F.; Lindler, D. J.

2002-05-01

The Advanced Camera for Surveys (ACS) was installed in the HST on 7 March 2002 during the fourth servicing mission to the observatory, and is now beginning science operations. The ACS provides HST observers with a considerably more sensitive, higher-resolution camera with wider field and polarimetric, coronagraphic, low-resolution spectrographic and solar-blind FUV capabilities. We review selected results of the early verification and calibration program, comparing the achieved performance with the advertised specifications. Emphasis is placed on the optical characteristics of the camera, including image quality, throughput, geometric distortion and stray-light performance. More detailed analyses of various aspects of the ACS performance are presented in other papers at this meeting. This work was supported by a NASA contract and a NASA grant.

Testing of the Apollo 15 Metric Camera System.

NASA Technical Reports Server (NTRS)

Helmering, R. J.; Alspaugh, D. H.

1972-01-01

Description of tests conducted (1) to assess the quality of Apollo 15 Metric Camera System data and (2) to develop production procedures for total block reduction. Three strips of metric photography over the Hadley Rille area were selected for the tests. These photographs were utilized in a series of evaluation tests culminating in an orbitally constrained block triangulation solution. Results show that film deformations up to 25 and 5 microns are present in the mapping and stellar materials, respectively. Stellar reductions can provide mapping camera orientations with an accuracy that is consistent with the accuracies of other parameters in the triangulation solutions. Pointing accuracies of 4 to 10 microns can be expected for the mapping camera materials, depending on variations in resolution caused by changing sun angle conditions.

First NAC Image Obtained in Mercury Orbit

NASA Image and Video Library

2017-12-08

NASA image acquired: March 29, 2011 This is the first image of Mercury taken from orbit with MESSENGER’s Narrow Angle Camera (NAC). MESSENGER’s camera system, the Mercury Dual Imaging System (MDIS), has two cameras: the Narrow Angle Camera and the Wide Angle Camera (WAC). Comparison of this image with MESSENGER’s first WAC image of the same region shows the substantial difference between the fields of view of the two cameras. At 1.5°, the field of view of the NAC is seven times smaller than the 10.5° field of view of the WAC. This image was taken using MDIS’s pivot. MDIS is mounted on a pivoting platform and is the only instrument in MESSENGER’s payload capable of movement independent of the spacecraft. The other instruments are fixed in place, and most point down the spacecraft’s boresight at all times, relying solely on the guidance and control system for pointing. The 90° range of motion of the pivot gives MDIS a much-needed extra degree of freedom, allowing MDIS to image the planet’s surface at times when spacecraft geometry would normally prevent it from doing so. The pivot also gives MDIS additional imaging opportunities by allowing it to view more of the surface than that at which the boresight-aligned instruments are pointed at any given time. On March 17, 2011 (March 18, 2011, UTC), MESSENGER became the first spacecraft ever to orbit the planet Mercury. The mission is currently in the commissioning phase, during which spacecraft and instrument performance are verified through a series of specially designed checkout activities. In the course of the one-year primary mission, the spacecraft's seven scientific instruments and radio science investigation will unravel the history and evolution of the Solar System's innermost planet. Visit the Why Mercury? section of this website to learn more about the science questions that the MESSENGER mission has set out to answer. Credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington NASA Goddard Space Flight Center enables NASA’s mission through four scientific endeavors: Earth Science, Heliophysics, Solar System Exploration, and Astrophysics. Goddard plays a leading role in NASA’s accomplishments by contributing compelling scientific knowledge to advance the Agency’s mission. Follow us on Twitter Join us on Facebook

Real-time full-motion color Flash lidar for target detection and identification

NASA Astrophysics Data System (ADS)

Nelson, Roy; Coppock, Eric; Craig, Rex; Craner, Jeremy; Nicks, Dennis; von Niederhausern, Kurt

2015-05-01

Greatly improved understanding of areas and objects of interest can be gained when real time, full-motion Flash LiDAR is fused with inertial navigation data and multi-spectral context imagery. On its own, full-motion Flash LiDAR provides the opportunity to exploit the z dimension for improved intelligence vs. 2-D full-motion video (FMV). The intelligence value of this data is enhanced when it is combined with inertial navigation data to produce an extended, georegistered data set suitable for a variety of analysis. Further, when fused with multispectral context imagery the typical point cloud now becomes a rich 3-D scene which is intuitively obvious to the user and allows rapid cognitive analysis with little or no training. Ball Aerospace has developed and demonstrated a real-time, full-motion LIDAR system that fuses context imagery (VIS to MWIR demonstrated) and inertial navigation data in real time, and can stream these information-rich geolocated/fused 3-D scenes from an airborne platform. In addition, since the higher-resolution context camera is boresighted and frame synchronized to the LiDAR camera and the LiDAR camera is an array sensor, techniques have been developed to rapidly interpolate the LIDAR pixel values creating a point cloud that has the same resolution as the context camera, effectively creating a high definition (HD) LiDAR image. This paper presents a design overview of the Ball TotalSight™ LIDAR system along with typical results over urban and rural areas collected from both rotary and fixed-wing aircraft. We conclude with a discussion of future work.

Study of the detail content of Apollo orbital photography

NASA Technical Reports Server (NTRS)

Kinzly, R. E.

1972-01-01

The results achieved during a study of the Detail Content of Apollo Orbital Photography are reported. The effect of residual motion smear or image reproduction processes upon the detail content of lunar surface imagery obtained from the orbiting command module are assessed. Data and conclusions obtained from the Apollo 8, 12, 14 and 15 missions are included. For the Apollo 8, 12 and 14 missions, the bracket-mounted Hasselblad camera had no mechanism internal to the camera for motion compensation. If the motion of the command module were left totally uncompensated, these photographs would exhibit a ground smear varying from 12 to 27 meters depending upon the focal length of the lens and the exposure time. During the photographic sequences motion compensation was attempted by firing the attitude control system of the spacecraft at a rate to compensate for the motion relative to the lunar surface. The residual smear occurring in selected frames of imagery was assessed using edge analyses methods to obtain and achieved modulation transfer function (MTF) which was compared to a baseline MTF.

September epsilon Perseid cluster as a result of orbital fragmentation

NASA Astrophysics Data System (ADS)

Koten, P.; Čapek, D.; Spurný, P.; Vaubaillon, J.; Popek, M.; Shrbený, L.

2017-04-01

Context. A bright fireball was observed above the Czech Republic on September 9, 2016, at 23:06:59 UT. Moreover, the video cameras at two different stations recorded eight fainter meteors flying on parallel atmospheric trajectories within less than 2 s. All the meteors belong to the September epsilon Perseid meteor shower. The measured proximity of all meteors during a very low activity meteor shower suggests that a cluster of meteors was observed. Aims: The goal of the paper is first to determine whether this event was a random occurrence or a real meteor cluster and second, if it was a cluster, to determine the epoch and at what distance from the Earth the separation of the particles occurred. Methods: The atmospheric trajectories of the observed meteors, masses, and relative distances of individual particles were determined using a double-station observation. According to the distances and masses of the particles, the most probable distance and time of fragmentation is determined. Results: The observed group of meteors is interpreted as the result of the orbital fragmentation of a bigger meteoroid. The fragmentation happened no earlier than 2 or 3 days before the encounter with the Earth at a distance smaller than 0.08 AU from the Earth.

Astronaut Alan Bean reads data from book while holding teleprinter tape

NASA Technical Reports Server (NTRS)

1973-01-01

Astronaut Alan L. Bean, Skylab 3 commander, reads data from book in his right hand while holding teleprinter tape in his left hand, in the ward room of the Skylab space station's Orbital Workshop (OWS) crew quarters. This photograph was taken with a 35mm Nikon camera held by one of Bean's fellow crewmen during the 56.5 day second manned Skylab mission in Earth orbit.

A New Lunar Digital Elevation Model from the Lunar Orbiter Laser Altimeter and SELENE Terrain Camera

NASA Technical Reports Server (NTRS)

Barker, M. K.; Mazarico, E.; Neumann, G. A.; Zuber, M. T.; Haruyama, J.; Smith, D. E.

2015-01-01

We present an improved lunar digital elevation model (DEM) covering latitudes within +/-60 deg, at a horizontal resolution of 512 pixels per degree ( approx.60 m at the equator) and a typical vertical accuracy approx.3 to 4 m. This DEM is constructed from approx.4.5 ×10(exp 9) geodetically-accurate topographic heights from the Lunar Orbiter Laser Altimeter (LOLA) onboard the Lunar Reconnaissance Orbiter, to which we co-registered 43,200 stereo-derived DEMs (each 1 deg×1 deg) from the SELENE Terrain Camera (TC) ( approx.10(exp 10) pixels total). After co-registration, approximately 90% of the TC DEMs show root-mean-square vertical residuals with the LOLA data of < 5 m compared to approx.50% prior to co-registration. We use the co-registered TC data to estimate and correct orbital and pointing geolocation errors from the LOLA altimetric profiles (typically amounting to < 10 m horizontally and < 1 m vertically). By combining both co-registered datasets, we obtain a near-global DEM with high geodetic accuracy, and without the need for surface interpolation. We evaluate the resulting LOLA + TC merged DEM (designated as "SLDEM2015") with particular attention to quantifying seams and crossover errors.

JMISR INteractive eXplorer

NASA Technical Reports Server (NTRS)

Nelson, David L.; Diner, David J.; Thompson, Charles K.; Hall, Jeffrey R.; Rheingans, Brian E.; Garay, Michael J.; Mazzoni, Dominic

2010-01-01

MISR (Multi-angle Imaging SpectroRadiometer) INteractive eXplorer (MINX) is an interactive visualization program that allows a user to digitize smoke, dust, or volcanic plumes in MISR multiangle images, and automatically retrieve height and wind profiles associated with those plumes. This innovation can perform 9-camera animations of MISR level-1 radiance images to study the 3D relationships of clouds and plumes. MINX also enables archiving MISR aerosol properties and Moderate Resolution Imaging Spectroradiometer (MODIS) fire radiative power along with the heights and winds. It can correct geometric misregistration between cameras by correlating off-nadir camera scenes with corresponding nadir scenes and then warping the images to minimize the misregistration offsets. Plots of BRF (bidirectional reflectance factor) vs. camera angle for points clicked in an image can be displayed. Users get rapid access to map views of MISR path and orbit locations and overflight dates, and past or future orbits can be identified that pass over a specified location at a specified time. Single-camera, level-1 radiance data at 1,100- or 275- meter resolution can be quickly displayed in color using a browse option. This software determines the heights and motion vectors of features above the terrain with greater precision and coverage than previous methods, based on an algorithm that takes wind direction into consideration. Human interpreters can precisely identify plumes and their extent, and wind direction. Overposting of MODIS thermal anomaly data aids in the identification of smoke plumes. The software has been used to preserve graphical and textural versions of the digitized data in a Web-based database.

Mars Daily Global Image from April 1999

NASA Image and Video Library

2000-09-08

Twelve orbits a day provide NASA Mars Global Surveyor MOC wide angle cameras a global napshot of weather patterns across the planet. Here, bluish-white water ice clouds hang above the Tharsis volcanoes.

Dunes in Brashear

NASA Image and Video Library

2006-01-08

This Mars Global Surveyor MGS Mars Orbiter Camera MOC image shows a field of dark sand dunes on the northwestern floor of Brashear Crater. The dunes formed largely from winds that blew from the southeast lower right

Mountainous Crater Rim on Mars

NASA Image and Video Library

2013-10-17

This is a screen shot from a high-definition simulated movie of Mojave Crater on Mars, based on images taken by the High Resolution Imaging Science Experiment HiRISE camera on NASA Mars Reconnaissance Orbiter.

Study of magnetic perturbations on SEC vidicon tubes. [large space telescope

NASA Technical Reports Server (NTRS)

Long, D. C.; Zucchino, P.; Lowrance, J.

1973-01-01

A laboratory measurements program was conducted to determine the tolerances that must be imposed to achieve optimum performance from SEC-vidicon data sensors in the LST mission. These measurements along with other data were used to formulate recommendations regarding the necessary telemetry and remote control for the television data sensors when in orbit. The study encompassed the following tasks: (1) Conducted laboratory measurements of the perturbations which an external magnetic field produces on a magnetically focused, SEC-vidicon. Evaluated shielding approaches. (2) Experimentally evaluated the effects produced on overall performance by variations of the tube electrode potentials, and the focus, deflection and alignment fields. (3) Recommended the extent of ground control of camera parameters and camera parameter telemetry required for optimizing the performance of the television system in orbit. The experimental data are summarized in a set of graphs.

``High energy Electron exPeriment (HEP)'' onboard the ERG satellite

NASA Astrophysics Data System (ADS)

Mitani, T.; Takashima, T.; Kasahara, S.; Miyake, W.; Hirahara, M.

2017-12-01

The Exploration of energization and Radiation in Geospace (ERG) satellite was successfully launched on December 20, 2016, and now explores how relativistic electrons in the radiation belts are generated during space storms. "High energy Electron exPeriment (HEP)" onboard the ERG satellite observes 70 keV - 2 MeV electrons and provides three-dimensional velocity distribution of electrons every spacecraft spin period. Electrons are observed by two types of camera designs, HEP-L and HEP-H, with regard to geometrical factor and energy range. HEP-L observes 0.1 - 1 MeV electrons and its geometrical factor (G-factor) is 10-3 cm2 str, and HEP-H observes 0.7 - 2 MeV and G-factor is 10-2 cm2 str. HEP-L and HEP-H each consist of three pin-hole type cameras, and each camera consist of mechanical collimator, stacked silicon semiconductor detectors and readout ASICs. HEP-H has larger opening angle of the collimator and more silicon detectors to observe higher energy electrons than HEP-L. The initial checkout in orbit was carried out in February 2017 and it was confirmed that there was no performance degradation by comparing the results of the initial checkout in orbit and the prelaunch function tests. Since late March, HEP has carried out normal observation. HEP observed losses and recovery of the outer radiation belt electrons several times up to now. In this presentation we introduce the HEP instrument design, prelaunch tests results and report the initial results in orbit.

Precise Trajectory Reconstruction of CE-3 Hovering Stage By Landing Camera Images

NASA Astrophysics Data System (ADS)

Yan, W.; Liu, J.; Li, C.; Ren, X.; Mu, L.; Gao, X.; Zeng, X.

2014-12-01

Chang'E-3 (CE-3) is part of the second phase of the Chinese Lunar Exploration Program, incorporating a lander and China's first lunar rover. It was landed on 14 December, 2013 successfully. Hovering and obstacle avoidance stages are essential for CE-3 safety soft landing so that precise spacecraft trajectory in these stages are of great significance to verify orbital control strategy, to optimize orbital design, to accurately determine the landing site of CE-3, and to analyze the geological background of the landing site. Because the time consumption of these stages is just 25s, it is difficult to present spacecraft's subtle movement by Measurement and Control System or by radio observations. Under this background, the trajectory reconstruction based on landing camera images can be used to obtain the trajectory of CE-3 because of its technical advantages such as unaffecting by lunar gravity field spacecraft kinetic model, high resolution, high frame rate, and so on. In this paper, the trajectory of CE-3 before and after entering hovering stage was reconstructed by landing camera images from frame 3092 to frame 3180, which lasted about 9s, under Single Image Space Resection (SISR). The results show that CE-3's subtle changes during hovering stage can be emerged by the reconstructed trajectory. The horizontal accuracy of spacecraft position was up to 1.4m while vertical accuracy was up to 0.76m. The results can be used for orbital control strategy analysis and some other application fields.

The ET as it falls away from the orbiter after separation on STS-121

NASA Image and Video Library

2006-07-04

S121-E-05006 (4 July 2006) --- This picture of the STS-121 external tank was taken with a digital still camera by an astronaut only seconds after separation from the Space Shuttle Discovery on launch day. Engineers, managers and flight controllers have carefully studied this image and other frames from this series as well as a number of pictures showing the falling ET as photographed from umbilical well cameras.

The ET as it falls away from the orbiter after separation on STS-121

NASA Image and Video Library

2006-07-04

STS121-E-05011 (4 July 2006)-- This picture of the STS-121 external tank was taken with a digital still camera by an astronaut only seconds after separation from the Space Shuttle Discovery on launch day. Engineers, managers and flight controllers have carefully studied this image and other frames from this series as well as a number of pictures showing the falling ET as photographed from umbilical well cameras.

The ET as it falls away from the orbiter after separation on STS-121

NASA Image and Video Library

2006-07-04

STS121-E-05008 (4 July 2006)-- This picture of the STS-121 external tank was taken with a digital still camera by an astronaut only seconds after separation from the Space Shuttle Discovery on launch day. Engineers, managers and flight controllers have carefully studied this image and other frames from this series as well as a number of pictures showing the falling ET as photographed from umbilical well cameras.

Sellers and Fossum on the end of the OBSS during EVA1 on STS-121 / Expedition 13 joint operations

NASA Image and Video Library

2006-07-08

STS121-323-011 (8 July 2006) --- Astronauts Piers J. Sellers and Michael E. Fossum, STS-121 mission specialists, work in tandem on Space Shuttle Discovery's Remote Manipulator System/Orbiter Boom Sensor System (RMS/OBSS) during the mission's first scheduled session of extravehicular activity (EVA). Also visible on the OBSS are the Laser Dynamic Range Imager (LDRI), Intensified Television Camera (ITVC) and Laser Camera System (LCS).

KSC-02pd1130

NASA Image and Video Library

2002-07-10

KENNEDY SPACE CENTER, FLA. -- With the engines removed from Endeavour, the flow line can be inspected. On the right, Gerry Kathka, with United Space Alliance, hands part of a fiber-optic camera system to Scott Minnick, left. Minnick wears a special viewing apparatus that sees where the camera is going. The inspection is the result of small cracks being discovered on the LH2 Main Propulsion System (MPS) flow liners in other orbiters. Endeavour is next scheduled to fly on mission STS-113.

Background simulations of the wide-field coded-mask camera for X-/Gamma-ray of the French-Chinese mission SVOM

NASA Astrophysics Data System (ADS)

Godet, Olivier; Barret, Didier; Paul, Jacques; Sizun, Patrick; Mandrou, Pierre; Cordier, Bertrand

SVOM (Space Variable Object Monitor) is a French-Chinese mission dedicated to the study of high-redshift GRBs, which is expected to be launched in 2012. The anti-Sun pointing strategy of SVOM along with a strong and integrated ground segment consisting of two wide-field robotic telescopes covering the near-IR and optical will optimise the ground-based GRB follow-ups by the largest telescopes and thus the measurements of spectroscopic redshifts. The central instrument of the science payload will be an innovative wide-field coded-mask camera for X- /Gamma-rays (4-250 keV) responsible for triggering and localising GRBs with an accuracy better than 10 arc-minutes. Such an instrument will be background-dominated so it is essential to estimate the background level expected once in orbit during the early phase of the instrument design in order to ensure good science performance. We present our Monte-Carlo simulator enabling us to compute the background spectrum taking into account the mass model of the camera and the main components of the space environment encountered in orbit by the satellite. From that computation, we show that the current design of the camera CXG will be more sensitive to high-redshift GRBs than the Swift-BAT thanks to its low-energy threshold of 4 keV.

A low cost automatic detection and ranging system for space surveillance in the medium Earth orbit region and beyond.

PubMed

Danescu, Radu; Ciurte, Anca; Turcu, Vlad

2014-02-11

The space around the Earth is filled with man-made objects, which orbit the planet at altitudes ranging from hundreds to tens of thousands of kilometers. Keeping an eye on all objects in Earth's orbit, useful and not useful, operational or not, is known as Space Surveillance. Due to cost considerations, the space surveillance solutions beyond the Low Earth Orbit region are mainly based on optical instruments. This paper presents a solution for real-time automatic detection and ranging of space objects of altitudes ranging from below the Medium Earth Orbit up to 40,000 km, based on two low cost observation systems built using commercial cameras and marginally professional telescopes, placed 37 km apart, operating as a large baseline stereovision system. The telescopes are pointed towards any visible region of the sky, and the system is able to automatically calibrate the orientation parameters using automatic matching of reference stars from an online catalog, with a very high tolerance for the initial guess of the sky region and camera orientation. The difference between the left and right image of a synchronized stereo pair is used for automatic detection of the satellite pixels, using an original difference computation algorithm that is capable of high sensitivity and a low false positive rate. The use of stereovision provides a strong means of removing false positives, and avoids the need for prior knowledge of the orbits observed, the system being able to detect at the same time all types of objects that fall within the measurement range and are visible on the image.

VizieR Online Data Catalog: Astrometric monitoring of ultracool dwarf binaries (Dupuy+, 2017)

NASA Astrophysics Data System (ADS)

Dupuy, T. J.; Liu, M. C.

2017-09-01

In Table 1 we list all 33 binaries in our Keck+CFHT astrometric monitoring sample, along with three other binaries that have published orbit and parallax measurements. We began obtaining resolved Keck AO astrometry in 2007-2008, and we combined our new astrometry with available data in the literature or public archives (e.g., HST and Gemini) to refine our orbital period estimates and thereby our prioritization for Keck observations. We present here new Keck/NIRC2 AO imaging and non-redundant aperture-masking observations, in addition to a re-analysis of our own previously published data and publicly available archival data for our sample binaries. Table 2 gives our measured astrometry and flux ratios for all Keck AO data used in our orbital analysis spanning 2003 Apr 15 to 2016 May 13. In total there are 339 distinct measurements (unique bandpass and epoch for a given target), where 302 of these are direct imaging and 37 are non-redundant aperture masking. Eight of the imaging measurements are from six unpublished archival data sets. See section 3.1.1 for further details. In addition to our Keck AO monitoring, we also obtained data for three T dwarf binaries over a three-year HST program using the Advanced Camera for Surveys (ACS) Wide Field Camera (WFC) in the F814W bandpass. See section 3.1.2 for further details. Many of our sample binaries have HST imaging data in the public archive. We have re-analyzed the available archival data coming from the WFPC2 Planetary Camera (WFPC2-PC1), ACS High Resolution Channel (ACS-HRC), and NICMOS Camera 1 (NICMOS-NIC1). See section 3.1.3 for further details. We present here an updated analysis of our data from the Hawaii Infrared Parallax Program that uses the CFHT facility infrared camera WIRCam. Our observing strategy and custom astrometry pipeline are described in detail in Dupuy & Liu (2012, J/ApJS/201/19). See section 3.2 for further explanations. (10 data files).

Massive stereo-based DTM production for Mars on cloud computers

NASA Astrophysics Data System (ADS)

Tao, Y.; Muller, J.-P.; Sidiropoulos, P.; Xiong, Si-Ting; Putri, A. R. D.; Walter, S. H. G.; Veitch-Michaelis, J.; Yershov, V.

2018-05-01

Digital Terrain Model (DTM) creation is essential to improving our understanding of the formation processes of the Martian surface. Although there have been previous demonstrations of open-source or commercial planetary 3D reconstruction software, planetary scientists are still struggling with creating good quality DTMs that meet their science needs, especially when there is a requirement to produce a large number of high quality DTMs using "free" software. In this paper, we describe a new open source system to overcome many of these obstacles by demonstrating results in the context of issues found from experience with several planetary DTM pipelines. We introduce a new fully automated multi-resolution DTM processing chain for NASA Mars Reconnaissance Orbiter (MRO) Context Camera (CTX) and High Resolution Imaging Science Experiment (HiRISE) stereo processing, called the Co-registration Ames Stereo Pipeline (ASP) Gotcha Optimised (CASP-GO), based on the open source NASA ASP. CASP-GO employs tie-point based multi-resolution image co-registration, and Gotcha sub-pixel refinement and densification. CASP-GO pipeline is used to produce planet-wide CTX and HiRISE DTMs that guarantee global geo-referencing compliance with respect to High Resolution Stereo Colour imaging (HRSC), and thence to the Mars Orbiter Laser Altimeter (MOLA); providing refined stereo matching completeness and accuracy. All software and good quality products introduced in this paper are being made open-source to the planetary science community through collaboration with NASA Ames, United States Geological Survey (USGS) and the Jet Propulsion Laboratory (JPL), Advanced Multi-Mission Operations System (AMMOS) Planetary Data System (PDS) Pipeline Service (APPS-PDS4), as well as browseable and visualisable through the iMars web based Geographic Information System (webGIS) system.

Dark Flows in Newton Crater Extending During Summer Six-Image Sequence

NASA Image and Video Library

2011-08-04

This image comes from observations of Newton crater by the HiRISE camera onboard NASA Mars Reconnaissance Orbiter where features appear and incrementally grow during warm seasons and fade in cold seasons.

Mars Odyssey Seen by Mars Global Surveyor

NASA Image and Video Library

2005-05-19

This view is an enlargement of an image of NASA Mars Odyssey spacecraft taken by the Mars Orbiter Camera aboard NASA Mars Global Surveyor while the two spacecraft were about 90 kilometers 56 miles apart.

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

High-Resolution Global Geologic Map of Ceres from NASA Dawn Mission

NASA Astrophysics Data System (ADS)

Williams, D. A.; Buczkowski, D. L.; Crown, D. A.; Frigeri, A.; Hughson, K.; Kneissl, T.; Krohn, K.; Mest, S. C.; Pasckert, J. H.; Platz, T.; Ruesch, O.; Schulzeck, F.; Scully, J. E. C.; Sizemore, H. G.; Nass, A.; Jaumann, R.; Raymond, C. A.; Russell, C. T.

2018-06-01

This presentation will discuss the completed 1:4,000,000 global geologic map of dwarf planet Ceres derived from Dawn Framing Camera Low Altitude Mapping Orbit (LAMo) images, combining 15 quadrangle maps.

A Rover Journey Begins

NASA Image and Video Library

2012-09-06

Tracks from the first drives of NASA Curiosity rover are visible in this image captured by the High-Resolution Imaging Science Experiment HiRISE camera on NASA Mars Reconnaissance Orbiter. The rover is seen where the tracks end.

Large, Fresh Crater Surrounded by Smaller Craters

NASA Image and Video Library

2014-05-22

The largest crater associated with a March 2012 impact on Mars has many smaller craters around it, revealed in this image from the High Resolution Imaging Science Experiment HiRISE camera on NASA Mars Reconnaissance Orbiter.

Flank vents and graben as indicators of Late Amazonian volcanotectonic activity on Olympus Mons

NASA Astrophysics Data System (ADS)

Peters, S. I.; Christensen, P. R.

2017-03-01

Previous studies have focused on large-scale features on Olympus Mons, such as its flank terraces, the summit caldera complex, and the basal escarpment and aureole deposits. Here we identify and characterize previously unrecognized and unmapped small scale features to help further understand the volcanotectonic evolution of this enormous volcano. Using Context Camera, High Resolution Imaging Science Experiment, Thermal Emission Imaging System, High Resolution Stereo Camera Digital Terrain Model, and Mars Orbiter Laser Altimeter data, we identified and characterized the morphology and distribution of 60 flank vents and 84 grabens on Olympus Mons. We find that effusive eruptions have dominated volcanic activity on Olympus Mons in the Late Amazonian. Explosive eruptions were rare, implying volatile-poor magmas and/or a lack of magma-water interactions during the Late Amazonian. The distribution of flank vents suggests dike propagation of hundreds of kilometers and shallow magma storage. Small grabens, not previously observed in lower-resolution data, occur primarily on the lower flanks of Olympus Mons and indicate late-stage extensional tectonism. Based on superposition relationships, we have concluded two stages of development for Olympus Mons during the Late Amazonian: (1) primarily effusive resurfacing and formation of flank vents followed by (2) waning effusive volcanism and graben formation and/or reactivation. This developmental sequence resembles that proposed for Ascraeus Mons and other large Martian shields, suggesting a similar geologic evolution for these volcanoes.

KSC-05PD-0587

NASA Technical Reports Server (NTRS)

2005-01-01

KENNEDY SPACE CENTER, FLA. In the Orbiter Processing Facility bay 1 at NASAs Kennedy Space Center, a worker rolls the plastic cover removed from the Orbital Boom Sensor System (OBSS), at right, which will be installed in the payload bay of Atlantis. The 50- foot-long OBSS attaches to the Remote Manipulator System, or Shuttle robotic arm, and is one of the new safety measures for Return to Flight, equipping the orbiter with cameras and laser systems to inspect the Shuttles Thermal Protection System while in space. The Return to Flight mission STS-121 has a launch window of July 12 - July 31, 2005.

KSC-05PD-0175

NASA Technical Reports Server (NTRS)

2005-01-01

KENNEDY SPACE CENTER, FLA. In the Orbiter Processing Facility bay 3, workers oversee the lowering of the Orbiter Boom Sensor System (OBSS) on the starboard side of Discoverys payload bay. At lower right is the Remote Manipulator System (RMS), or Shuttle robotic arm. The 50-foot-long OBSS attaches to the RMS, and is one of the new safety measures for Return to Flight, equipping the orbiter with cameras and laser systems to inspect the Shuttles Thermal Protection System while in space. The Return to Flight mission, STS-114, has a launch window of May 12 to June 3, 2005.

Apollo 8 Mission image,Target of Opportunity (T/O) 10

NASA Image and Video Library

1968-12-21

Apollo 8,Moon,Target of Opportunity (T/O) 10, Various targets. Latitude 18 degrees South,Longitude 163.50 degrees West. Camera Tilt Mode: High Oblique. Direction: South. Sun Angle 12 degrees. Original Film Magazine was labeled E. Camera Data: 70mm Hasselblad; F-Stop: F-5.6; Shutter Speed: 1/250 second. Film Type: Kodak SO-3400 Black and White,ASA 40. Other Photographic Coverage: Lunar Orbiter 1 (LO I) S-3. Flight Date: December 21-27,1968.

View of Jack Lousma's hands using silverware to gather food at food station

NASA Technical Reports Server (NTRS)

1973-01-01

A close-up view of Skylab 3 pilot Jack Lousma's hands using a silverware utensil to gather food at the food station, in this photographic reproduction taken from a television transmission made by a color TV camera aboard the Skylab space station in Earth orbit. Astronaut Alan L. Bean, commander, had just zoomed the TV camera in for this closeup of the food tray following a series of wide shots of Lousma at the food station.

HTV-4 Re-entry camera 1 card 1.

NASA Image and Video Library

2013-09-07

ISS036-E-041384 (7 Sept. 2013) --- A stationary camera onboard the International Space Station took this picture of the Japanese HTV-4 cargo spacecraft as it entered Earth’s atmosphere on Sept. 7, subsequently burning up. HTV-4 was launched by Japan's Aerospace Exploration Agency (JAXA) on Aug. 4 of this year in order to bring up supplies for the astronauts and cosmonauts onboard the station, and after spending a month docked to the orbital outpost, it was released on Sept. 4.

Expedition One CDR Shepherd with IMAX camera

NASA Image and Video Library

2001-02-11

STS98-E-5164 (11 February 2001) --- Astronaut William M. (Bill) Shepherd documents activity onboard the newly attached Destiny laboratory using an IMAX motion picture camera. The crews of Atlantis and the International Space Station on February 11 opened the Destiny laboratory and spent the first full day of what are planned to be years of work ahead inside the orbiting science and command center. Shepherd opened the Destiny hatch, and he and Shuttle commander Kenneth D. Cockrell ventured inside at 8:38 a.m. (CST). Members of both crews went to work quickly inside the new module, activating air systems, fire extinguishers, alarm systems, computers and internal communications. The crew also continued equipment transfers from the shuttle to the station and filmed several scenes onboard the station using an IMAX camera. This scene was recorded with a digital still camera.

HST High Gain Antennae photographed by Electronic Still Camera

NASA Image and Video Library

1993-12-04

S61-E-009 (4 Dec 1993) --- This view of one of two High Gain Antennae (HGA) on the Hubble Space Telescope (HST) was photographed with an Electronic Still Camera (ESC). The scene was down linked to ground controllers soon after the Space Shuttle Endeavour caught up to the orbiting telescope 320 miles above Earth. Shown here before grapple, the HST was captured on December 4, 1993 in order to service the telescope. Over a period of five days, four of the seven STS-61 crew members will work in alternating pairs outside Endeavour's shirt sleeve environment. Electronic still photography is a relatively new technology which provides the means for a handheld camera to electronically capture and digitize an image with resolution approaching film quality. The electronic still camera has flown as an experiment on several other shuttle missions.

Effects on Training Using Illumination in Virtual Environments

NASA Technical Reports Server (NTRS)

Maida, James C.; Novak, M. S. Jennifer; Mueller, Kristian

1999-01-01

Camera based tasks are commonly performed during orbital operations, and orbital lighting conditions, such as high contrast shadowing and glare, are a factor in performance. Computer based training using virtual environments is a common tool used to make and keep CTW members proficient. If computer based training included some of these harsh lighting conditions, would the crew increase their proficiency? The project goal was to determine whether computer based training increases proficiency if one trains for a camera based task using computer generated virtual environments with enhanced lighting conditions such as shadows and glare rather than color shaded computer images normally used in simulators. Previous experiments were conducted using a two degree of freedom docking system. Test subjects had to align a boresight camera using a hand controller with one axis of rotation and one axis of rotation. Two sets of subjects were trained on two computer simulations using computer generated virtual environments, one with lighting, and one without. Results revealed that when subjects were constrained by time and accuracy, those who trained with simulated lighting conditions performed significantly better than those who did not. To reinforce these results for speed and accuracy, the task complexity was increased.

NASA Shuttle Lightning Research: Observations of Nocturnal Thunderstorms and Lightning Displays as Seen During Recent Space Shuttle Missions

NASA Technical Reports Server (NTRS)

Vaughan, Otha H., Jr.

1994-01-01

A number of interesting lightning events have been observed using the low light level TV camera of the space shuttle during nighttime observations of thunderstorms near the limb of the Earth. Some of the vertical type lightning events that have been observed will be presented. Using TV cameras for observing lightning near the Earth's limb allows one to determine the location of the lightning and other characteristics by using the star field data and the shuttle's orbital position to reconstruct the geometry of the scene being viewed by the shuttle's TV cameras which are located in the payload bay of the shuttle.

KSC-01pp1802

NASA Image and Video Library

2001-12-01

KENNEDY SPACE CENTER, Fla. - STS-109 Mission Specialist Richard Lennehan (left) and Payload Commander John Grunsfeld get a feel for tools and equipment that will be used on the mission. The crew is at KSC to take part in Crew Equipment Interface Test activities that include familiarization with the orbiter and equipment. The goal of the mission is to service the HST, replacing Solar Array 2 with Solar Array 3, replacing the Power Control Unit, removing the Faint Object Camera and installing the Advanced Camera for Surveys, installing the Near Infrared Camera and Multi-Object Spectrometer (NICMOS) Cooling System, and installing New Outer Blanket Layer insulation on bays 5 through 8. Mission STS-109 is scheduled for launch Feb. 14, 2002

Orbit determination based on meteor observations using numerical integration of equations of motion

NASA Astrophysics Data System (ADS)

Dmitriev, V.; Lupovka, V.; Gritsevich, M.

2014-07-01

We review the definitions and approaches to orbital-characteristics analysis applied to photographic or video ground-based observations of meteors. A number of camera networks dedicated to meteors registration were established all over the word, including USA, Canada, Central Europe, Australia, Spain, Finland and Poland. Many of these networks are currently operational. The meteor observations are conducted from different locations hosting the network stations. Each station is equipped with at least one camera for continuous monitoring of the firmament (except possible weather restrictions). For registered multi-station meteors, it is possible to accurately determine the direction and absolute value for the meteor velocity and thus obtain the topocentric radiant. Based on topocentric radiant one further determines the heliocentric meteor orbit. We aim to reduce total uncertainty in our orbit-determination technique, keeping it even less than the accuracy of observations. The additional corrections for the zenith attraction are widely in use and are implemented, for example, here [1]. We propose a technique for meteor-orbit determination with higher accuracy. We transform the topocentric radiant in inertial (J2000) coordinate system using the model recommended by IAU [2]. The main difference if compared to the existing orbit-determination techniques is integration of ordinary differential equations of motion instead of addition correction in visible velocity for zenith attraction. The attraction of the central body (the Sun), the perturbations by Earth, Moon and other planets of the Solar System, the Earth's flattening (important in the initial moment of integration, i.e. at the moment when a meteoroid enters the atmosphere), atmospheric drag may be optionally included in the equations. In addition, reverse integration of the same equations can be performed to analyze orbital evolution preceding to meteoroid's collision with Earth. To demonstrate the developed technique, we provide calculated orbits for several cases, including well-known meteorite-producing fireballs. A comparison of our estimates with previously published ones is also provided.

Candidate Landing Site for the Mars Science Laboratory: Vernal Crater, S.W. ARabia Terra

NASA Technical Reports Server (NTRS)

Paris, K. N.; Allen, C. C.; Oehler, D. Z.

2007-01-01

In the fall of 2009, the Mars Science Laboratory (MSL) will be launched to Mars. The purpose of this mission is to assess biologic potential and geology and to investigate planetary processes of relevance to past habitability. MSL will be able to provide visual, chemical, radiation, and environmental data with its suite of instruments [1]. In order to be selected for the MSL landing site, certain engineering requirements must be met [1] and the area should contain geologic features suggestive of past habitability, so that the overriding science goal of the mission will be attained. There are a total of 33 proposed landing sites as of the first MSL Landing Site Workshop held in Pasadena, CA from May 31st to June 2nd, 2006 [1]. There will be an opportunity to gather high resolution visual and hyperspectral data on all proposed landing sites from the now-orbiting Mars Reconnaissance Orbiter (MRO) which entered martian orbit and began its main science phase in November of 2006 [2]. The data being gathered are from: the high resolution imaging science experiment (HiRISE), the context (CTX) camera and the compact reconnaissance imaging spectrometer (CRISM) onboard the spacecraft. The footprints of these instruments are centered on a single point, and each proposer must submit these coordinates, along with the coordinates of the proposed landing ellipse. Data from these instruments, along with new MOC images and THEMIS mosaics, will be used to enhance our understanding of the geologic and engineering parameters of each site.

The NASA Fireball Network

NASA Technical Reports Server (NTRS)

Cooke, William J.

2013-01-01

In the summer of 2008, the NASA Meteoroid Environments Office (MEO) began to establish a video fireball network, based on the following objectives: (1) determine the speed distribution of cm size meteoroids, (2) determine the major sources of cm size meteoroids (showers/sporadic sources), (3) characterize meteor showers (numbers, magnitudes, trajectories, orbits), (4) determine the size at which showers dominate the meteor flux, (5) discriminate between re-entering space debris and meteors, and 6) locate meteorite falls. In order to achieve the above with the limited resources available to the MEO, it was necessary that the network function almost fully autonomously, with very little required from humans in the areas of upkeep or analysis. With this in mind, the camera design and, most importantly, the ASGARD meteor detection software were adopted from the University of Western Ontario's Southern Ontario Meteor Network (SOMN), as NASA has a cooperative agreement with Western's Meteor Physics Group. 15 cameras have been built, and the network now consists of 8 operational cameras, with at least 4 more slated for deployment in calendar year 2013. The goal is to have 15 systems, distributed in two or more groups east of automatic analysis; every morning, this server also automatically generates an email and a web page (http://fireballs.ndc.nasa.gov) containing an automated analysis of the previous night's events. This analysis provides the following for each meteor: UTC date and time, speed, start and end locations (longitude, latitude, altitude), radiant, shower identification, light curve (meteor absolute magnitude as a function of time), photometric mass, orbital elements, and Tisserand parameter. Radiant/orbital plots and various histograms (number versus speed, time, etc) are also produced. After more than four years of operation, over 5,000 multi-station fireballs have been observed, 3 of which potentially dropped meteorites. A database containing data on all these events, including the videos and calibration information, has been developed and is being modified to include data from the SOMN and other camera networks.

Context-based handover of persons in crowd and riot scenarios

NASA Astrophysics Data System (ADS)

Metzler, Jürgen

2015-02-01

In order to control riots in crowds, it is helpful to get ringleaders under control and pull them out of the crowd if one has become an offender. A great support to achieve these tasks is the capability of observing the crowd and ringleaders automatically by using cameras. It also allows a better conservation of evidence in riot control. A ringleader who has become an offender should be tracked across and recognized by several cameras, regardless of whether overlapping camera's fields of view exist or not. We propose a context-based approach for handover of persons between different camera fields of view. This approach can be applied for overlapping as well as for non-overlapping fields of view, so that a fast and accurate identification of individual persons in camera networks is feasible. Within the scope of this paper, the approach is applied to a handover of persons between single images without having any temporal information. It is particularly developed for semiautomatic video editing and a handover of persons between cameras in order to improve conservation of evidence. The approach has been developed on a dataset collected during a Crowd and Riot Control (CRC) training of the German armed forces. It consists of three different levels of escalation. First, the crowd started with a peaceful demonstration. Later, there were violent protests, and third, the riot escalated and offenders bumped into the chain of guards. One result of the work is a reliable context-based method for person re-identification between single images of different camera fields of view in crowd and riot scenarios. Furthermore, a qualitative assessment shows that the use of contextual information can support this task additionally. It can decrease the needed time for handover and the number of confusions which supports the conservation of evidence in crowd and riot scenarios.

Mars Odyssey Seen by Mars Global Surveyor 3-D

NASA Image and Video Library

2005-05-19

This stereoscopic picture of NASA Mars Odyssey spacecraft was created from two views of that spacecraft taken by the Mars Orbiter Camera on NASA Mars Global Surveyor. 3D glasses are necessary to view this image.

Reflecting on Icy Rhea

NASA Image and Video Library

2009-11-03

Bright sunlight on Rhea shows off the cratered surface of Saturn second largest moon in this image captured by NASA Cassini Orbiter. The image was taken in visible light with the Cassini spacecraft narrow-angle camera on Sept. 21, 2009.

Warm-Season Flows on Slope in Horowitz Crater Nine-Image Sequence

NASA Image and Video Library

2011-08-04

This image comes from observations of Horowitz crater by the HiRISE camera onboard NASA Mars Reconnaissance Orbiter. The features that extend down the slope during warm seasons are called recurring slope lineae.

Caught in Action: Avalanches on North Polar Scarps

NASA Image and Video Library

2008-03-03

Amazingly, this image has captured at least four Martian avalanches, or debris falls, in action. It was taken on February 19, 2008, by the High Resolution Imaging Science Experiment HiRISE camera on NASA Mars Reconnaissance Orbiter.

Dark Spots

NASA Technical Reports Server (NTRS)

2006-01-01

Dark spots (left) and 'fans' appear to scribble dusty hieroglyphics on top of the Martian south polar cap in two high-resolution Mars Global Surveyor, Mars Orbiter Camera images taken in southern spring. Each image is about 3-kilometers wide (2-miles).

Ripple Trap

NASA Image and Video Library

2006-04-03

This Mars Global Surveyor MGS Mars Orbiter Camera MOC image shows the margin of a lava flow on a cratered plain in the Athabasca Vallis region of Mars. Remarkably, the cratered plain in this scene is essentially free of bright, windblown ripples

Phoenix Lander Amid Disappearing Spring Ice

NASA Image and Video Library

2010-01-11

NASA Phoenix Mars Lander, its backshell and heatshield visible within this enhanced-color image of the Phoenix landing site taken on Jan. 6, 2010 by the High Resolution Imaging Science Experiment HiRISE camera on NASA Mars Reconnaissance Orbiter.

Phobos from 6,800 Kilometers Color

NASA Image and Video Library

2008-04-09

The High Resolution Imaging Science Experiment HiRISE camera on NASA Mars Reconnaissance Orbiter took two images of the larger of Mars two moons, Phobos, within 10 minutes of each other on March 23, 2008. This is the first.

Zooming in on Landing Site

NASA Image and Video Library

2008-05-24

This animation zooms in on the area on Mars where NASA Phoenix Mars Lander will touchdown on May 25, 2008. The image was taken by the High Resolution Imaging Science Experiment HiRISE camera on NASA Mars Reconnaissance Orbiter.

End effector on orbiter's RMS arm

NASA Image and Video Library

2001-03-13

STS102-E-5201 (13 March 2001) --- A view of the interior of the end effector apparatus on the end of the Canadian-built remote manipulator system (RMS) arm. The photograph was taken with a digital still camera.

Mars Odyssey Observes Deimos

NASA Image and Video Library

2018-02-22

Colors in this image of the Martian moon Deimos indicate a range of surface temperatures detected by observing the moon on February 15, 2018, with the Thermal Emission Imaging System (THEMIS) camera on NASA's Mars Odyssey orbiter. The left edge of the small moon is in darkness, and the right edge in sunlight. Temperature information was derived from thermal-infrared imaging such as the grayscale image shown smaller at lower left with the moon in the same orientation. The color-coding merges information from THEMIS observations made in 10 thermal-infrared wavelength bands. This was the first observation of Deimos by Mars Odyssey; the spacecraft first imaged Mars' other moon, Phobos, on September 29, 2017. Researchers have been using THEMIS to examine Mars since early 2002, but the maneuver turning the orbiter around to point the camera at Phobos was developed only recently. https://photojournal.jpl.nasa.gov/catalog/PIA22250

Mars Odyssey Observes Phobos

NASA Image and Video Library

2018-02-22

Colors in this image of the Martian moon Phobos indicate a range of surface temperatures detected by observing the moon on February 15, 2018, with the Thermal Emission Imaging System (THEMIS) camera on NASA's Mars Odyssey orbiter. The left edge of the small moon is in darkness, and the right edge in sunlight. Phobos has an oblong shape with average diameter of about 14 miles (22 kilometers). Temperature information was derived from thermal-infrared imaging such as the grayscale image shown smaller at lower left with the moon in the same orientation. The color-coding merges information from THEMIS observations made in 10 thermal-infrared wavelength bands. This was the second observation of Phobos by Mars Odyssey; the first was on September 29, 2017. Researchers have been using THEMIS to examine Mars since early 2002, but the maneuver turning the orbiter around to point the camera at Phobos was developed only recently. https://photojournal.jpl.nasa.gov/catalog/PIA22249

Initiation of a lightning search using the lightning and airglow camera onboard the Venus orbiter Akatsuki

NASA Astrophysics Data System (ADS)

Takahashi, Yukihiro; Sato, Mitsuteru; Imai, Masataka; Lorenz, Ralph; Yair, Yoav; Aplin, Karen; Fischer, Georg; Nakamura, Masato; Ishii, Nobuaki; Abe, Takumi; Satoh, Takehiko; Imamura, Takeshi; Hirose, Chikako; Suzuki, Makoto; Hashimoto, George L.; Hirata, Naru; Yamazaki, Atsushi; Sato, Takao M.; Yamada, Manabu; Murakami, Shin-ya; Yamamoto, Yukio; Fukuhara, Tetsuya; Ogohara, Kazunori; Ando, Hiroki; Sugiyama, Ko-ichiro; Kashimura, Hiroki; Ohtsuki, Shoko

2018-05-01

The existence of lightning discharges in the Venus atmosphere has been controversial for more than 30 years, with many positive and negative reports published. The lightning and airglow camera (LAC) onboard the Venus orbiter, Akatsuki, was designed to observe the light curve of possible flashes at a sufficiently high sampling rate to discriminate lightning from other sources and can thereby perform a more definitive search for optical emissions. Akatsuki arrived at Venus during December 2016, 5 years following its launch. The initial operations of LAC through November 2016 have included a progressive increase in the high voltage applied to the avalanche photodiode detector. LAC began lightning survey observations in December 2016. It was confirmed that the operational high voltage was achieved and that the triggering system functions correctly. LAC lightning search observations are planned to continue for several years.

KENNEDY SPACE CENTER, FLA. - In the Payload Hazardous Servicing Facility at KSC, installation is under way of the Mars Orbiter Camera (MOC) on the Mars Global Surveyor spacecraft. The MOC is one of a suite of six scientific instruments that will gather data about Martian topography, mineral distribution and weather during a two-year period. The Mars Global Surveyor is slated for launch aboard a Delta II expendable launch vehicle on Nov. 6, the beginning of a 20-day launch period.

NASA Image and Video Library

1996-08-19

KENNEDY SPACE CENTER, FLA. - In the Payload Hazardous Servicing Facility at KSC, installation is under way of the Mars Orbiter Camera (MOC) on the Mars Global Surveyor spacecraft. The MOC is one of a suite of six scientific instruments that will gather data about Martian topography, mineral distribution and weather during a two-year period. The Mars Global Surveyor is slated for launch aboard a Delta II expendable launch vehicle on Nov. 6, the beginning of a 20-day launch period.

International Ultraviolet Explorer observations of the peculiar variable spectrum of the eclipsing binary R Arae

NASA Technical Reports Server (NTRS)

Mccluskey, G. E.; Kondo, Y.

1983-01-01

The eclipsing binary system R Arae = HD 149730 is a relatively bright southern system with an orbital period of about 4.4 days. It is a single-lined spectroscopic binary. The spectral class of the primary component is B9 Vp. The system was included in a study of mass flow and evolution in close binary systems using the International Ultraviolet Explorer satellite (IUE). Four spectra in the wavelength range from 1150 to 1900 A were obtained with the far-ultraviolet SWP camera, and six spectra in the range from 1900 to 3200 range were obtained with the mid-ultraviolet LWR camera. The close binary R Arae exhibits very unusual ultraviolet spectra. It appears that no other close binary system, observed with any of the orbiting satellites, shows outside-eclipse ultraviolet continuum flux variations of this nature.

Spirit's Travels During its First 238 Martian Days

NASA Technical Reports Server (NTRS)

2004-01-01

This map shows the complete traverse of NASA's Mars Exploration Rover Spirit through the rover's 238th martian day, or sol (Sept. 3, 2004). This was shortly before the rover stopped driving for about two weeks while Mars was nearly behind the Sun from Earth's perspective. The background image consists of frames from the Mars Orbiter Camera on NASA's Mars Global Surveyor orbiter. Inset images along the route are from Spirit's navigation camera. From its landing site, Spirit drove up to the rim of 'Bonneville' crater on the far left and to the north rim of 'Missoula' crater. Then it commenced a long drive across the plains, deviating to avoid large hollows. Upon arrival at the base of the 'Columbia Hills,' Spirit drove north for a short distance before beginning its ascent onto the 'West Spur,' where it is currently located. The scale bar at lower left is 500 meters (1,640 feet). North is up.

KENNEDY SPACE CENTER, FLA. -- NASA Deputy Associate Administrator for Space Station and Shuttle Programs Michael Kostelnik (left) discusses some of the working parts inside the nose of Shuttle Discovery in Orbiter Processing Facility Bay 3 with a United Space Alliance (USA) technician (back to camera). NASA and USA Space Shuttle program management are participating in a leadership workday. The day is intended to provide management with an in-depth, hands-on look at Shuttle processing activities at KSC.

NASA Image and Video Library

2003-12-19

KENNEDY SPACE CENTER, FLA. -- NASA Deputy Associate Administrator for Space Station and Shuttle Programs Michael Kostelnik (left) discusses some of the working parts inside the nose of Shuttle Discovery in Orbiter Processing Facility Bay 3 with a United Space Alliance (USA) technician (back to camera). NASA and USA Space Shuttle program management are participating in a leadership workday. The day is intended to provide management with an in-depth, hands-on look at Shuttle processing activities at KSC.

Report of the facility definition team spacelab UV-Optical Telescope Facility

NASA Technical Reports Server (NTRS)

1975-01-01

Scientific requirements for the Spacelab Ultraviolet-Optical Telescope (SUOT) facility are presented. Specific programs involving high angular resolution imagery over wide fields, far ultraviolet spectroscopy, precisely calibrated spectrophotometry and spectropolarimetry over a wide wavelength range, and planetary studies, including high resolution synoptic imagery, are recommended. Specifications for the mounting configuration, instruments for the mounting configuration, instrument mounting system, optical parameters, and the pointing and stabilization system are presented. Concepts for the focal plane instruments are defined. The functional requirements of the direct imaging camera, far ultraviolet spectrograph, and the precisely calibrated spectrophotometer are detailed, and the planetary camera concept is outlined. Operational concepts described in detail are: the makeup and functions of shuttle payload crew, extravehicular activity requirements, telescope control and data management, payload operations control room, orbital constraints, and orbital interfaces (stabilization, maneuvering requirements and attitude control, contamination, utilities, and payload weight considerations).

High-resolution Ceres Low Altitude Mapping Orbit Atlas derived from Dawn Framing Camera images

NASA Astrophysics Data System (ADS)

Roatsch, Th.; Kersten, E.; Matz, K.-D.; Preusker, F.; Scholten, F.; Jaumann, R.; Raymond, C. A.; Russell, C. T.

2017-06-01

The Dawn spacecraft Framing Camera (FC) acquired over 31,300 clear filter images of Ceres with a resolution of about 35 m/pxl during the eleven cycles in the Low Altitude Mapping Orbit (LAMO) phase between December 16 2015 and August 8 2016. We ortho-rectified the images from the first four cycles and produced a global, high-resolution, uncontrolled photomosaic of Ceres. This global mosaic is the basis for a high-resolution Ceres atlas that consists of 62 tiles mapped at a scale of 1:250,000. The nomenclature used in this atlas was proposed by the Dawn team and was approved by the International Astronomical Union (IAU). The full atlas is available to the public through the Dawn Geographical Information System (GIS) web page [http://dawngis.dlr.de/atlas] and will become available through the NASA Planetary Data System (PDS) (http://pdssbn.astro.umd.edu/).

VUV testing of science cameras at MSFC: QE measurement of the CLASP flight cameras

NASA Astrophysics Data System (ADS)

Champey, P.; Kobayashi, K.; Winebarger, A.; Cirtain, J.; Hyde, D.; Robertson, B.; Beabout, B.; Beabout, D.; Stewart, M.

2015-08-01

The NASA Marshall Space Flight Center (MSFC) has developed a science camera suitable for sub-orbital missions for observations in the UV, EUV and soft X-ray. Six cameras were built and tested for the Chromospheric Lyman-Alpha Spectro-Polarimeter (CLASP), a joint MSFC, National Astronomical Observatory of Japan (NAOJ), Instituto de Astrofisica de Canarias (IAC) and Institut D'Astrophysique Spatiale (IAS) sounding rocket mission. The CLASP camera design includes a frame-transfer e2v CCD57-10 512 × 512 detector, dual channel analog readout and an internally mounted cold block. At the flight CCD temperature of -20C, the CLASP cameras exceeded the low-noise performance requirements (<= 25 e- read noise and <= 10 e- /sec/pixel dark current), in addition to maintaining a stable gain of ≍ 2.0 e-/DN. The e2v CCD57-10 detectors were coated with Lumogen-E to improve quantum efficiency (QE) at the Lyman- wavelength. A vacuum ultra-violet (VUV) monochromator and a NIST calibrated photodiode were employed to measure the QE of each camera. Three flight cameras and one engineering camera were tested in a high-vacuum chamber, which was configured to operate several tests intended to verify the QE, gain, read noise and dark current of the CCD. We present and discuss the QE measurements performed on the CLASP cameras. We also discuss the high-vacuum system outfitted for testing of UV, EUV and X-ray science cameras at MSFC.

A Low Cost Automatic Detection and Ranging System for Space Surveillance in the Medium Earth Orbit Region and Beyond

PubMed Central

Danescu, Radu; Ciurte, Anca; Turcu, Vlad

2014-01-01

The space around the Earth is filled with man-made objects, which orbit the planet at altitudes ranging from hundreds to tens of thousands of kilometers. Keeping an eye on all objects in Earth's orbit, useful and not useful, operational or not, is known as Space Surveillance. Due to cost considerations, the space surveillance solutions beyond the Low Earth Orbit region are mainly based on optical instruments. This paper presents a solution for real-time automatic detection and ranging of space objects of altitudes ranging from below the Medium Earth Orbit up to 40,000 km, based on two low cost observation systems built using commercial cameras and marginally professional telescopes, placed 37 km apart, operating as a large baseline stereovision system. The telescopes are pointed towards any visible region of the sky, and the system is able to automatically calibrate the orientation parameters using automatic matching of reference stars from an online catalog, with a very high tolerance for the initial guess of the sky region and camera orientation. The difference between the left and right image of a synchronized stereo pair is used for automatic detection of the satellite pixels, using an original difference computation algorithm that is capable of high sensitivity and a low false positive rate. The use of stereovision provides a strong means of removing false positives, and avoids the need for prior knowledge of the orbits observed, the system being able to detect at the same time all types of objects that fall within the measurement range and are visible on the image. PMID:24521941

MRO Context Camera (CTX) Investigation Primary Mission Results

NASA Astrophysics Data System (ADS)

Edgett, K. S.; Malin, M. C.; Science; Operations Teams, M.

2008-12-01

The Mars Reconnaissance Orbiter (MRO) Context Camera (CTX) acquires panchromatic images of Mars at ~6 m/pixel; the majority cover areas 30 km wide by 43 to 313 km long. As of 31 August 2008, 36% of Mars was imaged at 6 m/pixel and 10.8% was covered more than once. Areas imaged multiple times include stereopairs and locations covered repeatedly to monitor dust-raising events, seasonal frost patterns, or landforms and albedo features known or anticipated to change. CTX provides context for data acquired by other MRO science instruments, as well. Using our knowledge of imaging performance as a function of seasonal atmospheric, frost, and insolation conditions from the 4 Mars-year Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) investigation, we undertook several time-dependent campaigns to create 6 m/pixel mosaics of regions such as Hellas Planitia, the south polar residual cap (covered in spring and in summer), and the north polar region. In addition, we obtained 6 m/pixel mosaics of the Valles Marineris, Sinus Meridiani, Marte Valles, Athabasca Valles, portions of the northern plains, fretted terrain and chaotic terrain, large volcanoes, yardang-forming materials in Amazonis and Aeolis, the small volcanoes and platy flows south of Cerberus, and many other regions. We monitored thousands of mid-latitude gullies, and we used our MOC experience to target dust-raising events that repeat every year at the same locations. Retreat of cliffs formed in layers of CO2 ice in the south polar cap was observed for the 5th southern summer since 1999. Dozens of new impact craters and crater clusters were observed; all formed since 1999 and some formed during the MRO Primary Mission. We routinely re-targeted the new impact sites to see how they change and alert other MRO instrument teams so they could observe them. CTX images of the cratered highlands emphasize the view that the upper crust of Mars is layered with interbedded filled and buried valleys, fluvial channels, and impact craters ranging in diameter from meters to hundreds of kilometers. CTX observations reiterate a critical MOC result regarding small, sub-kilometer diameter craters: the substrates most resistant to erosion retain the most small craters (and the boulders produced by the impacts). CTX images provide many examples in which a younger, harder substrate (e.g., a lava flow) is more heavily cratered (with < 1 km diameter craters) than subjacent, older rock units. One example occurs in the form of lava flows located immediately west of Meridiani Planum; similar flows underlie the hematite-bearing, plains- forming rock in nearby Miyamoto Crater. Northern Meridiani also exhibits exhumed, low-order streams (of the scale of hillslope rills and creeks); these were filled, buried, lithified, and later returned to the surface by erosion-some of them in inverted form. Terrain immediately west of Juventae Chasma exhibits similar inverted streams and rills that were first documented by MOC and provide key evidence for rainfall and hillslope runoff. CTX data show that there are many hundreds of inverted fluvial channels, of a variety of sizes, all over the planet, especially in Arabia Terra, Solis Planum, and Thaumasia. We also used CTX to map a small, unnamed outflow channel system west of Bond Crater, and we have been documenting all of the small Martian volcanoes, typically < 30 km across, including those occurring in the Labyrinthus Noctis. CTX data are widely available, as they are archived with the NASA Planetary Data System on a rolling basis every 6 months.

Research on target tracking algorithm based on spatio-temporal context

NASA Astrophysics Data System (ADS)

Li, Baiping; Xu, Sanmei; Kang, Hongjuan

2017-07-01

In this paper, a novel target tracking algorithm based on spatio-temporal context is proposed. During the tracking process, the camera shaking or occlusion may lead to the failure of tracking. The proposed algorithm can solve this problem effectively. The method use the spatio-temporal context algorithm as the main research object. We get the first frame's target region via mouse. Then the spatio-temporal context algorithm is used to get the tracking targets of the sequence of frames. During this process a similarity measure function based on perceptual hash algorithm is used to judge the tracking results. If tracking failed, reset the initial value of Mean Shift algorithm for the subsequent target tracking. Experiment results show that the proposed algorithm can achieve real-time and stable tracking when camera shaking or target occlusion.

Space Shuttle Projects

NASA Image and Video Library

2001-08-01

This is the insignia of the STS-109 Space Shuttle mission. Carrying a crew of seven, the Space Shuttle Orbiter Columbia was launched with goals of maintenance and upgrades to the Hubble Space Telescope (HST). The Marshall Space Flight Center had the responsibility for the design, development, and construction of the HST, which is the most complex and sensitive optical telescope ever made, to study the cosmos from a low-Earth orbit. The HST detects objects 25 times fainter than the dimmest objects seen from Earth and provides astronomers with an observable universe 250 times larger than is visible from ground-based telescopes, perhaps as far away as 14 billion light-years. The HST views galaxies, stars, planets, comets, possibly other solar systems, and even unusual phenomena such as quasars, with 10 times the clarity of ground-based telescopes. During the STS-109 mission, the telescope was captured and secured on a work stand in Columbia's payload bay using Columbia's robotic arm where four members of the crew performed five spacewalks completing system upgrades to the HST. Included in those upgrades were: The replacement of the solar array panels; replacement of the power control unit (PCU); replacement of the Faint Object Camera (FOC) with a new advanced camera for Surveys (ACS); and installation of the experimental cooling system for the Hubble's Near-Infrared Camera and Multi-object Spectrometer (NICMOS), which had been dormant since January 1999 when it original coolant ran out. Lasting 10 days, 22 hours, and 11 minutes, the STS-109 mission was the 27th flight of the Orbiter Columbia and the 108th flight overall in NASA's Space Shuttle Program.

Limb clouds and dust on Mars from VMC-Mars Express images

NASA Astrophysics Data System (ADS)

Sanchez-Lavega, Agustin; Chen, Hao Chen; Ordoñez-Etxeberria, Iñaki; Hueso, Ricardo; Cardesin, Alejandro; Titov, Dima; Wood, Simon

2016-10-01

We have used the large image database generated by the Visual Monitoring Camera (VMC) onboard Mars Express to first search and then study, the properties of projected features (dust and water clouds) on the planet limb. VMC is a small camera serving since 2007 for public education and outreach (Ormston et al., 2011). The camera consists of a CMOS sensor with a Bayer filter mosaic providing color images in the wavelength range 400-900 nm. Since the observations were performed in an opportunistic mode (nor planned on a science base) the captured events occurred in a random mode. In total 17 limb features were observed in the period spanning from April 2007 to August 2015. Their extent at limb varies from about 100 km for the smaller ones to 2,000 km for the major ones. They showed a rich morphology consisting in series of patchy elements with a uniform top layer located at altitudes ranging from 30 to 85 km. The features are mostly concentrated between latitudes 45 deg North and South covering most longitudes although a greater concentration occurs around -90 to +90 deg. from the reference meridian (i.e. longitude 0 degrees, East or West). Most events in the southern hemisphere occurred for orbital longitudes 0-90 degrees (autumnal season) and in the north for orbital longitudes 330-360 (winter season). We present a detailed study of two of these events, one corresponding to a dust storm observed also with the MARCI instrument onboard Mars Reconnaissance Orbiter, and a second one corresponding to a water cloud.

Astronaut Alan Bean reads data from book while holding teleprinter tape

NASA Image and Video Library

1973-08-08

SL3-111-1514 (July-September 1973) --- Astronaut Alan L. Bean, Skylab 3 commander, reads data from book in his right hand while holding teleprinter tape in his left hand, in the ward room of the Skylab space station's Orbital Workshop (OWS) crew quarters. This photograph was taken with a 35mm Nikon camera held by one of Bean's fellow crewmen during the 56.5 day second manned Skylab mission in Earth orbit. Photo credit: NASA

Liftoff of shuttle Challenger and mission STS 51-B

NASA Technical Reports Server (NTRS)

1985-01-01

Liftoff of shuttle Challenger and mission STS 51-B. The shuttle orbiter, its external tank and one of the solid rocket boosters (SRB) are still visible as it leaves the pad. This photo was taken from across the water over the top of a grove of trees (051); Photo taken from camera on the launch complex, showing the orbiter just clearing the tower (052); Side view of the liftoff as the SRBs begin to fire (053).

Back-to-Back Martian Dust Storms

NASA Image and Video Library

2017-03-09

This frame from a movie clip of hundreds of images from NASA's Mars Reconnaissance Orbiter shows a global map of Mars with atmospheric changes from Feb. 18, 2017 through March 6, 2017, a period when two regional-scale dust storms appeared. It combines hundreds of images from the Mars Color Imager (MARCI) camera on NASA's Mars Reconnaissance Orbiter. The date for each map in the series is given at upper left. Dust storms appear as pale tan. In the opening frames, one appears left of center, near the top (north) of the map, then grows in size as it moves south, eventually spreading to about half the width of the map after reaching the southern hemisphere. As the dust from that first storm becomes more diffuse in the south, another storm appears near the center of the map in the final frames. In viewing the movie, it helps to understand some of the artifacts produced by the nature of MARCI images when seen in animation. MARCI acquires images in swaths from pole-to-pole during the dayside portion of each orbit. The camera can cover the entire planet in just over 12 orbits, and takes about one day to accumulate this coverage. The individual swaths for each day are assembled into a false-color, map-projected mosaic for the day. Equally spaced blurry areas that run from south-to-north result from the high off-nadir viewing geometry in those parts of each swath, a product of the spacecraft's low orbit. Portions with sharper-looking details are the central part of an image, viewing more directly downward through less atmosphere than the obliquely viewed portions. MARCI has a 180-degree field of view, and Mars fills about 78 percent of that field of view when the camera is pointed down at the planet. However, the Mars Reconnaissance Orbiter often is pointed to one side or the other off its orbital track in order to acquire targeted observations by other imaging systems on the spacecraft. When such rolls exceed about 20 degrees, gaps occur in the mosaic of MARCI swaths. Other dark gaps appear where data are missing. It isn't easy to see the actual dust motion in the atmosphere in these images, owing to the apparent motion of these artifacts. However, by concentrating on specific surface features (craters, prominent ice deposits, etc.) and looking for the tan clouds of dust, it is possible to see where the storms start and how they grow, move and eventually dissipate. Movies are available at http://photojournal.jpl.nasa.gov/catalog/PIA21484

STS-31 Space Shuttle mission report

NASA Technical Reports Server (NTRS)

Camp, David W.; Germany, D. M.; Nicholson, Leonard S.

1990-01-01

The STS-31 Space Shuttle Program Mission Report contains a summary of the vehicle subsystem activities on this thirty-fifth flight of the Space Shuttle and the tenth flight of the Orbiter Vehicle Discovery (OV-103). In addition to the Discovery vehicle, the flight vehicle consisted of an External Tank (ET) (designated as ET-34/LWT-27), three Space Shuttle main engines (SSME's) (serial numbers 2011, 2031, and 2107), and two Solid Rocket Booster (SRB) (designated as BI-037). The primary objective of the mission was to place the Hubble Space Telescope (HST) into a 330 nmi. circular orbit having an inclination of 28.45 degrees. The secondary objectives were to perform all operations necessary to support the requirements of the Protein Crystal Growth (PCG), Investigations into Polymer Membrane Processing (IPMP), Radiation Monitoring Equipment (RME), Ascent Particle Monitor (APM), IMAX Cargo Bay Camera (ICBC), Air Force Maui Optical Site Calibration Test (AMOS), IMAX Crew Compartment Camera, and Ion Arc payloads. In addition, 12 development test objectives (DTO's) and 10 detailed supplementary objectives (DSO's) were assigned to the flight. The sequence of events for this mission is shown. The significant problems that occurred in the Space Shuttle Orbiter subsystems during the mission are summarized, and the official problem tracking list is presented. In addition, each of the Space Shuttle Orbiter problems is cited in the subsystem discussion.

4 Vesta in Color: High Resolution Mapping from Dawn Framing Camera Images

NASA Technical Reports Server (NTRS)

Reddy, V.; LeCorre, L.; Nathues, A.; Sierks, H.; Christensen, U.; Hoffmann, M.; Schroeder, S. E.; Vincent, J. B.; McSween, H. Y.; Denevi, B. W.;

Students Target

NASA Image and Video Library

2005-12-19

Using the JMars targeting software, eighth grade students from Charleston Middle School in Charleston, IL, selected the location of -8.37N and 276.66E for capture by the THEMIS visible camera during Mars Odyssey sixth orbit of Mars on Nov. 22, 2005

Diffuse Winter Lighting of the Chasma Boreale Scarp

NASA Image and Video Library

2013-08-08

Sunlight was just starting to reach the high Northern latitudes in late winter when NASA Mars Reconnaissance Orbiter HiRISE camera captured this image of part of the steep scarps around portions of the North Polar layered deposits.

Gidzenko in Service Module with laptop computers

NASA Image and Video Library

2001-03-30

ISS-01-E-5070 (December 2000) --- Astronaut Yuri P. Gidzenko, Expedition One Soyuz commander, works with computers in the Zvezda or Service Module aboard the Earth-orbiting International Space Station (ISS). The picture was taken with a digital still camera.

Europa Active Surface

NASA Image and Video Library

1997-09-07

On June 27, 1996, during Galileo first orbit around Jupiter, a newly discovered impact crater could be seen just right of the center of this image of Jupiter moon Europa returned by NASA Galileo spacecraft camera. http://photojournal.jpl.nasa.gov/catalog/PIA00294

Could This Be the Mars Soviet 3 Lander?

NASA Image and Video Library

2013-04-11

This set of images shows what might be hardware from the Soviet Union 1971 Mars 3 lander, seen in a pair of images from the High Resolution Imaging Science Experiment HiRISE camera on NASA Mars Reconnaissance Orbiter.

Which Came First, the Yardang or the Platy Flow?

NASA Image and Video Library

2014-02-13

One of the great strengths of the HiRISE camera onboard NASA Mars Reconnaissance Orbiter is that its high resolution can help resolve interesting questions. Here, is the platy flow material younger than the yardang-forming material?

The HRSC Experiment on Mars Express: First Imaging Results from the Commissioning Phase

NASA Astrophysics Data System (ADS)

Oberst, J.; Neukum, G.; Hoffmann, H.; Jaumann, R.; Hauber, E.; Albertz, J.; McCord, T. B.; Markiewicz, W. J.

2004-12-01

The ESA Mars Express spacecraft was launched from Baikonur on June 2, 2003, entered Mars orbit on December 25, 2003, and reached the nominal mapping orbit on January 28, 2004. Observing conditions were favorable early on for the HRSC (High Resolution Stereo Camera), designed for the mapping of the Martian surface in 3-D. The HRSC is a pushbroom scanner with 9 CCD line detectors mounted in parallel and perpendicular to the direction of flight on the focal plane. The camera can obtain images at high resolution (10 m/pix), in triple stereo (20 m/pix), in four colors, and at five different phase angles near-simultaneously. An additional Super-Resolution Channel (SRC) yields nested-in images at 2.3 m/pix for detailed photogeologic studies. Even for nominal spacecraft trajectory and camera pointing data from the commissioning phase, solid stereo image reconstructions are feasible. More yet, the three-line stereo data allow us to identify and correct errors in navigation data. We find that > 99% of the stereo rays intersect within a sphere of radius < 20m after orbit and pointing data correction. From the HRSC images we have produced Digital Terrain Models (DTMs) with pixel sizes of 200 m, some of them better. HRSC stereo models and data obtained by the MOLA (Mars Orbiting Laser Altimeter) show good qualitative agreement. Differences in absolute elevations are within 50 m, but may reach several 100 m in lateral positioning (mostly in the spacecraft along-track direction). After correction of these offsets, the HRSC topographic data conveniently fill the gaps between the MOLA tracks and reveal hitherto unrecognized morphologic detail. At the time of writing, the HRSC has covered approx. 22.5 million square kilometers of the Martian surface. In addition, data from 5 Phobos flybys from May through August 2004 were obtained. The HRSC is beginning to make major contributions to geoscience, atmospheric science, photogrammetry, and cartography of Mars (papers submitted to Nature).

Imaging experiment: The Viking Mars orbiter

USGS Publications Warehouse

Carr, M.H.; Baum, W.A.; Briggs, G.A.; Masursky, H.; Wise, D.W.; Montgomery, D.R.

1972-01-01

The general objectives of the Imaging Experiment on the Viking Orbiter are to aid the selection of Viking Lander sites, to map and monitor the chosen sites during lander operations, to aid in the selection of future landing sites, and to extend our knowledge of the planet. The imaging system consists of two identical vidicon cameras each attached to a 1026 mm T/8 telescope giving approximately 1?? square field of view. From an altitude of 1500 km the picture elements will be approximately 24m apart. The vidicon is coupled with an image intensifier which provides increased sensitivity and permits electronic shuttering and image motion compensation. A vidicon readout time of 2.24 sec enables pictures to be taken in rapid sequence for contiguous coverage at high resolution. The camera differs from those previously flown to Mars by providing contiguous coverage at high resolution on a single orbital pass, by having sufficient sensitivity to use narrow band color filters at maximum resolution, and by having response in the ultraviolet. These capabilities will be utelized to supplement lander observations and to extend our knowledge particularly of volcanic, erosional, and atmospheric phenomena on Mars. ?? 1972.

French Meteor Network for High Precision Orbits of Meteoroids

NASA Technical Reports Server (NTRS)

Atreya, P.; Vaubaillon, J.; Colas, F.; Bouley, S.; Gaillard, B.; Sauli, I.; Kwon, M. K.

2011-01-01

There is a lack of precise meteoroids orbit from video observations as most of the meteor stations use off-the-shelf CCD cameras. Few meteoroids orbit with precise semi-major axis are available using film photographic method. Precise orbits are necessary to compute the dust flux in the Earth s vicinity, and to estimate the ejection time of the meteoroids accurately by comparing them with the theoretical evolution model. We investigate the use of large CCD sensors to observe multi-station meteors and to compute precise orbit of these meteoroids. An ideal spatial and temporal resolution to get an accuracy to those similar of photographic plates are discussed. Various problems faced due to the use of large CCD, such as increasing the spatial and the temporal resolution at the same time and computational problems in finding the meteor position are illustrated.

Observations of the Perseids 2013 using SPOSH cameras

NASA Astrophysics Data System (ADS)

Margonis, A.; Elgner, S.; Christou, A.; Oberst, J.; Flohrer, J.

2013-09-01

Earth is constantly bombard by debris, most of which disintegrates in the upper atmosphere. The collision of a dust particle, having a mass of approximately 1g or larger, with the Earth's atmosphere results into a visible streak of light in the night sky, called meteor. Comets produce new meteoroids each time they come close to the Sun due to sublimation processes. These fresh particles are moving around the Sun in orbits similar to their parent comet forming meteoroid streams. For this reason, the intersection of Earth's orbital path with different comets, gives rise to anumber of meteor showers throughout the year. The Perseids are one of the most prominent annual meteor showers occurring every summer, having its origin in Halley-type comet 109P/Swift-Tuttle. The dense core of this stream passes Earth's orbit on the 12th of August when more than 100 meteors per hour can been seen by a single observer under ideal conditions. The Technical University of Berlin (TUB) and the German Aerospace Center (DLR) together with the Armagh observatory organize meteor campaigns every summer observing the activity of the Perseids meteor shower. The observations are carried out using the Smart Panoramic Optical Sensor Head (SPOSH) camera system [2] which has been developed by DLR and Jena-Optronik GmbH under an ESA/ESTEC contract. The camera was designed to image faint, short-lived phenomena on dark planetary hemispheres. The camera is equipped with a highly sensitive back-illuminated CCD chip having a pixel resolution of 1024x1024. The custom-made fish-eye lens offers a 120°x120° field-of-view (168° over the diagonal) making the monitoring of nearly the whole night sky possible (Fig. 1). This year the observations will take place between 3rd and 10th of August to cover the meteor activity of the Perseids just before their maximum. The SPOSH cameras will be deployed at two remote sites located in high altitudes in the Greek Peloponnese peninsula. The baseline of ∼50km between the two observing stations ensures a large overlapping area of the cameras' field of views allowing the triangulation of approximately every meteor captured by the two observing systems. The acquired data will be reduced using dedicated software developed at TUB and DLR. Assuming a successful campaign, statistics, trajectories and photometric properties of the processed double-station meteors will be presented at the conference. Furthermore, a first order statistical analysis of the meteors processed during the 2012 and the new 2013 campaigns will be presented [1].

Thermal Design of the Instrument for the Transiting Exoplanet Survey Satellite

NASA Technical Reports Server (NTRS)

Allen, Gregory D.

2016-01-01

TESS observatory is a two year NASA Explorer mission which will use a set of four cameras to discover exoplanets. It will be placed in a high-earth orbit with a period of 13.7 days and will be unaffected by temperature disturbances caused by environmental heating from the Earth. The cameras use their stray-light baffles to passively cool the cameras and in turn the CCD's in order to maintain operational temperatures. The design has been well thought out and analyzed to maximize temperature stability. The analysis shows that the design keeps the cameras and their components within their temperature ranges which will help make it a successful mission. It will also meet its survival requirement of sustaining exposure to a five hour eclipse. Official validation and verification planning is underway and will be performed as the system is built up. It is slated for launch in 2017.

MS Lucid places samples in the TEHOF aboard the Spektr module

NASA Image and Video Library

1997-03-26

STS079-S-082 (16-26 Sept. 1996) --- Cosmonaut guest researcher Shannon W. Lucid and Valeri G. Korzun, her Mir-22 commander, are pictured on the Spektr Module aboard Russia's Earth-orbiting Mir Space Station. Korzun was the third of four commanders that Lucid served with during her record-setting 188 consecutive days in space. Later, Lucid returned to Earth with her fourth commander-astronaut William F. Readdy-and five other NASA astronauts to complete the STS-79 mission. During the STS-79 mission, the crew used an IMAX camera to document activities aboard the space shuttle Atlantis and the various Mir modules. A hand-held version of the 65mm camera system accompanied the STS-79 crew into space in Atlantis' crew cabin. NASA has flown IMAX camera systems on many Shuttle missions, including a special cargo bay camera's coverage of other recent Shuttle-Mir rendezvous and/or docking missions.

Observations of the Perseids 2012 using SPOSH cameras

NASA Astrophysics Data System (ADS)

Margonis, A.; Flohrer, J.; Christou, A.; Elgner, S.; Oberst, J.

2012-09-01

The Perseids are one of the most prominent annual meteor showers occurring every summer when the stream of dust particles, originating from Halley-type comet 109P/Swift-Tuttle, intersects the orbital path of the Earth. The dense core of this stream passes Earth's orbit on the 12th of August producing the maximum number of meteors. The Technical University of Berlin (TUB) and the German Aerospace Center (DLR) organize observing campaigns every summer monitoring the Perseids activity. The observations are carried out using the Smart Panoramic Optical Sensor Head (SPOSH) camera system [0]. The SPOSH camera has been developed by DLR and Jena-Optronik GmbH under an ESA/ESTEC contract and it is designed to image faint, short-lived phenomena on dark planetary hemispheres. The camera features a highly sensitive backilluminated 1024x1024 CCD chip and a high dynamic range of 14 bits. The custom-made fish-eye lens offers a 120°x120° field-of-view (168° over the diagonal). Figure 1: A meteor captured by the SPOSH cameras simultaneously during the last 2011 observing campaign in Greece. The horizon including surrounding mountains can be seen in the image corners as a result of the large FOV of the camera. The observations will be made on the Greek Peloponnese peninsula monitoring the post-peak activity of the Perseids during a one-week period around the August New Moon (14th to 21st). Two SPOSH cameras will be deployed in two remote sites in high altitudes for the triangulation of meteor trajectories captured at both stations simultaneously. The observations during this time interval will give us the possibility to study the poorly-observed postmaximum branch of the Perseid stream and compare the results with datasets from previous campaigns which covered different periods of this long-lived meteor shower. The acquired data will be processed using dedicated software for meteor data reduction developed at TUB and DLR. Assuming a successful campaign, statistics, trajectories and photometric properties of the processed double-station meteors will be presented at the conference. Furthermore, a first order statistical analysis of the meteors processed during the 2011 and the new 2012 campaigns will be presented [0].

Digital Video Cameras for Brainstorming and Outlining: The Process and Potential

ERIC Educational Resources Information Center

Unger, John A.; Scullion, Vicki A.

2013-01-01

This "Voices from the Field" paper presents methods and participant-exemplar data for integrating digital video cameras into the writing process across postsecondary literacy contexts. The methods and participant data are part of an ongoing action-based research project systematically designed to bring research and theory into practice…

CLOSE BINARIES WITH INFRARED EXCESS: DESTROYERS OF WORLDS?

DOE Office of Scientific and Technical Information (OSTI.GOV)

Matranga, M.; Drake, J. J.; Kashyap, V. L.

2010-09-10

We present the results of a Spitzer photometric investigation into the IR excesses of close binary systems. In a sample of 10 objects, excesses in Infrared Array Camera and MIPS24 bands implying the presence of warm dust are found for 3. For two objects, we do not find excesses reported in earlier IRAS studies. We discuss the results in the context of the scenario suggested by Rhee and co-workers, in which warm dust is continuously created by destructive collisions between planetary bodies. A simple numerical model for the steady-state distribution of dust in one IR excess system shows a centralmore » clearing of radius 0.22 AU caused by dynamical perturbations from the binary star. This is consistent with the size of the central clearing derived from the Spitzer spectral energy distribution. We conclude that close binaries could be efficient 'destroyers of worlds' and lead to destabilization of the orbits of their planetary progeny by magnetically driven angular momentum loss and secular shrinkage of the binary separation.« less

Influence of Fault-Controlled Topography on Fluvio-Deltaic Sedimentary Systems in Eberswalde Crater, Mars

NASA Technical Reports Server (NTRS)

Rice, Melissa S.; Gupta, Sanjeev; Bell, James F., III; Warner, Nicholas H.

2011-01-01

Eberswalde crater was selected as a candidate landing site for the Mars Science Laboratory (MSL) mission based on the presence of a fan-shaped sedimentary deposit interpreted as a delta. We have identified and mapped five other candidate fluvio -deltaic systems in the crater, using images and digital terrain models (DTMs) derived from the Mars Reconnaissance Orbiter (MRO) High Resolution Imaging Science Experiment (HiRISE) and Context Camera (CTX). All of these systems consist of the same three stratigraphic units: (1) an upper layered unit, conformable with (2) a subpolygonally fractured unit, unconformably overlying (3) a pitted unit. We have also mapped a system of NNE-trending scarps interpreted as dip-slip faults that pre-date the fluvial -lacustrine deposits. The post-impact regional faulting may have generated the large-scale topography within the crater, which consists of a Western Basin, an Eastern Basin, and a central high. This topography subsequently provided depositional sinks for sediment entering the crater and controlled the geomorphic pattern of delta development.

The New Hard X-ray Mission

NASA Astrophysics Data System (ADS)

Pareschi, Giovanni; Tagliaferri, Gianpiero; Argan, Andrea; Bellazzini, Ronaldo; Catalano, Osvaldo; Costa, Enrico; Cusumano, Giancarlo; Fiore, Fabrizio; Fiorini, Carlo; Malaguti, Giuseppe; Matt, Giorgio; Mereghetti, Sandro; Micela, Giuseppina; Perola, Giuseppe Cesare; Villa, Gabriele

2010-07-01

The Italian New Hard X-ray Mission (NHXM) is an evolution of the HEXIT-Sat concept, extending up to 80 keV the fine imaging capability today available only at E<10 keV, with the further addition of photoelectric imaging polarimetry. NHXM consists of four identical mirrors, with a 10 m focal length, achieved after launch by means of a deployable structure. Three of the four telescopes will have at their focus three identical spectro-imaging cameras, while a X-ray imaging polarimeter will be placed at the focus of the fourth. In order to ensure a low and stable background, NHXM will be place on a low Earth equatorial orbit. NHXM will provide a real breakthrough on a number of hot astrophysical issues, broadly falling under two main topics: i) censing the black holes in the Universe and probing the physics of accretion in the most diverse conditions; ii) investigating the particle acceleration mechanisms at work in different contexts, and the effects of radiative transfer in highly magnetized plasmas and strong gravitational fields.

The Evolution of Gully Features in Acidalia Planitia

NASA Image and Video Library

2017-10-23

This observation image from NASA's Mars Reconnaisance Orbiter (MRO) captures details regarding the evolution of gully features observed in a crater in Acidalia Planitia. A Context Camera image provides context for these gullies showing an approximately 7-kilometer diameter crater in which we see that the gullies occur exclusively on the northern wall. This is unlike most of the observed gully sites in the northern Martian hemisphere, which typically have gullies on their pole-facing slopes. Another unique observation of this set of gullies is that they start mid-way down the crater's wall rather than cutting directly into the upper crater wall or rim. The younger, more recently active fans are generally rougher than the older, smoother fans that are located near the base of the slope. Consistent with this interpretation, are a number of observed superposition and cross-cutting relationships. The rougher fans are always superimposed over the older, smoother ones. Discontinuous fractures are observed to cross-cut only older features, while the most recently active portions of the gullies, in this case the channels or fans, are not cut by the fractures, but in some cases even superimpose them. This suggests that the fractures formed prior to the last phase of gully activity. https://photojournal.jpl.nasa.gov/catalog/PIA22054

A complex of meteorite-forming bodies (the Innisfree - Ridgedale family).

NASA Astrophysics Data System (ADS)

Shestaka, I. S.

1994-12-01

For the first time a swarm of meteorite-forming bodies was identified. Yearly this swarm's orbit approaches the Earth's orbit in early February. This swarm contains the Innisfree and Ridgedale fireballs, 9 small meteoric swarms, several asteroids and 12 fireballs photographed by the cameras of the Prairie Network and Canadian Meteorite Observation and Discovery Project. The discovery of this complex, intensive bombardments of the Moon's surface recorded by means of seismographs left on the Moon, the analysis of the time distributions of meteorite falls on the Earth and other established facts confirm the existence of swarms of meteorite-forming bodies which are crossing the Earth's orbit.

Photogrammetric application of viking orbital photography

USGS Publications Warehouse

Wu, S.S.C.; Elassal, A.A.; Jordan, R.; Schafer, F.J.

1982-01-01

Special techniques are described for the photogrammetric compilation of topographic maps and profiles from stereoscopic photographs taken by the two Viking Orbiter spacecraft. These techniques were developed because the extremely narrow field of view of the Viking cameras precludes compilation by conventional photogrammetric methods. The techniques adjust for internal consistency the Supplementary Experiment Data Record (SEDR-the record of spacecraft orientation when photographs were taken) and the computation of geometric orientation parameters of the stereo models. A series of contour maps of Mars is being compiled by these new methods using a wide variety of Viking Orbiter photographs, to provide the planetary research community with topographic information. ?? 1982.

SL3-108-01288

NASA Image and Video Library

1973-07-01

SL3-108-1288 (July-Sept. 1973) --- Astronaut Owen K. Garriott, science pilot of the Skylab 3 mission, is stationed at the Apollo Telescope Mount (ATM) console in the Multiple Docking Adapter (MDA) of the Skylab space station in Earth orbit. This picture was taken with a handheld 35mm Nikon camera. Astronauts Garriott, Alan L. Bean and Jack R. Lousma remained with the Skylab space station cluster in orbit for 59 days conducting numerous medical, scientific and technological experiments. In orbit the MDA functions as a major experiment control center for solar observations. From this console the astronauts actively control the ATM solar physics telescopes. Photo credit: NASA

VUV Testing of Science Cameras at MSFC: QE Measurement of the CLASP Flight Cameras

NASA Technical Reports Server (NTRS)

Champey, Patrick; Kobayashi, Ken; Winebarger, Amy; Cirtain, Jonathan; Hyde, David; Robertson, Bryan; Beabout, Brent; Beabout, Dyana; Stewart, Mike

2015-01-01

The NASA Marshall Space Flight Center (MSFC) has developed a science camera suitable for sub-orbital missions for observations in the UV, EUV and soft X-ray. Six cameras were built and tested for the Chromospheric Lyman-Alpha Spectro-Polarimeter (CLASP), a joint National Astronomical Observatory of Japan (NAOJ) and MSFC sounding rocket mission. The CLASP camera design includes a frame-transfer e2v CCD57-10 512x512 detector, dual channel analog readout electronics and an internally mounted cold block. At the flight operating temperature of -20 C, the CLASP cameras achieved the low-noise performance requirements (less than or equal to 25 e- read noise and greater than or equal to 10 e-/sec/pix dark current), in addition to maintaining a stable gain of approximately equal to 2.0 e-/DN. The e2v CCD57-10 detectors were coated with Lumogen-E to improve quantum efficiency (QE) at the Lyman- wavelength. A vacuum ultra-violet (VUV) monochromator and a NIST calibrated photodiode were employed to measure the QE of each camera. Four flight-like cameras were tested in a high-vacuum chamber, which was configured to operate several tests intended to verify the QE, gain, read noise, dark current and residual non-linearity of the CCD. We present and discuss the QE measurements performed on the CLASP cameras. We also discuss the high-vacuum system outfitted for testing of UV and EUV science cameras at MSFC.

The use of a wearable camera to capture and categorise the environmental and social context of self-identified eating episodes.

PubMed

Gemming, Luke; Doherty, Aiden; Utter, Jennifer; Shields, Emma; Ni Mhurchu, Cliona

2015-09-01

Research investigating the influence of the environmental and social factors on eating behaviours in free-living settings is limited. This study investigates the utility of using wearable camera images to assess the context of eating episodes. Adult participants (N = 40) wore a SenseCam wearable camera for 4 days (including 1 familiarisation day) over a 15-day period in free-living conditions, and had their diet assessed using three image-assisted multiple-pass 24-hour dietary recalls. The images of participants' eating episodes were analysed and annotated according to their environmental and social contexts; including eating location, external environment (indoor/outdoor), physical position, social interaction, and viewing media screens. Data for 107 days were used, with a total of 742 eating episodes considered for annotation. Twenty nine per cent (214/742) of the episodes could not be categorised due to absent images (12%, n = 85), dark/blurry images (8%, n = 58), camera not worn (7%, n = 54) and for mixed reasons (2%, n = 17). Most eating episodes were at home (59%) and indoors (91%). Meals at food retailers were 24.8 minutes longer (95% CI: 13.4 to 36.2) and were higher in energy (mean difference = 1196 kJ 95% CI: 242, 2149) than at home. Most episodes were seated at tables (27%) or sofas (26%), but eating standing (19%) or at desks (18%) were common. Social interaction was evident for 45% of episodes and media screens were viewed during 55% of episodes. Meals at home watching television were 3.1 minutes longer (95% CI: -0.6 to 6.7) and higher in energy intake than when no screen was viewed (543 kJ 95% CI: -32 to 1120). The environmental and social context that surrounds eating and dietary behaviours can be assessed using wearable camera images. Copyright © 2015 Elsevier Ltd. All rights reserved.

Evidence for Recent Liquid Water on Mars: Seepage Sites in 'Aerobraking Crater' Revisited

NASA Technical Reports Server (NTRS)

2000-01-01

(A) [figure removed for brevity, see original site] (B) [figure removed for brevity, see original site] (C) (D) You will need 3D glasses to view this anaglyph

The first clue that there might be places on Mars where liquid groundwater seeps out onto the surface came from a picture taken by the Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) during the pre-mapping Orbit Insertion Phase of the mission. The picture, shown in (A)above, was taken at the end of December 1997 while the spacecraft was still in the midst of aerobraking maneuvers to put it into the circular orbit needed for the Mapping Phase of the project. The Aerobraking 1 image, AB1-07707, showed dark, v-shaped scars on the western wall of a 50 kilometer-(31 mile)-diameter impact crater in southern Noachis Terra at 65oS, 15oW (see B, above, for context). The v-shaped features taper downslope to form narrow, somewhat curved channels. The relationship seen here was interpreted by MOC scientists to be similar to seepage landforms on Earth that form where springs emerge on a slope and water runs downhill.

Once MGS achieved its Mapping Orbit in March 1999, the MOC was in a better position to take pictures of 10 times higher resolution than the Aerobraking AB1-07707 image. The opportunity to take a new picture of the proposed 'seepage' sites on the wall of the crater in southern Noachis finally arose in January 2000. The result is MOC image M11-00530, shown above in (top) and (C). This new close-up shows that the darkly-shaped scars host many small channels of only a few meters (yards) across. These small channels run downslope and coalesce at the apex (or point) of each 'v'. Amid the small channels are many large boulders, some of them the size of houses, that have eroded out of the crater wall. A 3-D view created using the AB1 and M11 images is shown in (D). The stereo picture (red-blue '3D' glasses required) emphasizes the presence of small channels and valleys, and shows that these valleys start almost at the very top of the v-shaped dark areas.

The context picture in (B) is a mosaic of Viking 2 orbiter images 497B47 and 497B48 acquired December 28, 1977. The Aerobraking MGS MOC image, AB1-07707, is shown overlain on the Viking context image; it was taken 20 years later on December 29, 1997. The smaller white box in the context picture shows the location of MOC Mapping Phase image M11-00530, roughly 2 years later on January 4, 2000. North is 'up' in pictures (A) and (B), and to the lower right in (top), (C), and (D). Sunlight illuminates (A) from the upper left, (B) from the upper right, and (top) and (C) from the upper right. The top image in (top) is the aerobraking image, AB1-07707, with a white box indicating the location of the lower image, M11-00530, and the stereo pair in (D). The white box on the left in (C) shows the location of the close-up on the right in (C).

STS-26 MS Nelson on fixed based (FB) shuttle mission simulator (SMS) middeck

NASA Technical Reports Server (NTRS)

1988-01-01

STS-26 Discovery, Orbiter Vehicle (OV) 103, Mission Specialist (MS) George D. Nelson trains on the middeck of the fixed based (FB) shuttle mission simulator (SMS). Nelson, wearing communications assembly headset, adjusts camera mounting bracket.

What Juno will see at Jupiter South Pole Simulation

NASA Image and Video Library

2011-08-03

This simulated view of the south pole of Jupiter illustrates the unique perspective of NASA Juno mission. Juno polar orbit will allow its camera, called JunoCam, to image Jupiter clouds from a vantage point never accessed by other spacecraft.

Light-Toned Bedrock Along Cracks as Evidence of Fluid Alteration

NASA Image and Video Library

2007-02-15

This enhanced-color image from the HiRISE camera on NASA Mars Reconnaissance Orbiter shows a landscape of sand dunes and buttes among a background of light-toned bands and dark-toned bands in the Candor Chasma region

Simulated Flyover of Mars Canyon Map Animation

NASA Image and Video Library

2014-12-12

This frame from an animation simulates a flyover of a portion of a Martian canyon detailed in a geological map produced by the U.S. Geological Survey and based on observations by the HiRISE camera on NASA Mars Reconnaissance Orbiter.

Calibration Image of Earth by Mars Color Imager

NASA Image and Video Library

2005-08-22

Three days after the Mars Reconnaissance Orbiter Aug. 12, 2005, launch, the NASA spacecraft was pointed toward Earth and the Mars Color Imager camera was powered up to acquire a suite of color and ultraviolet images of Earth and the Moon.

Calibration View of Earth and the Moon by Mars Color Imager

NASA Image and Video Library

2005-08-22

Three days after the Mars Reconnaissance Orbiter Aug. 12, 2005, launch, the spacecraft was pointed toward Earth and the Mars Color Imager camera was powered up to acquire a suite of images of Earth and the Moon.

Recent Aqueous Environments in Impact Craters and the Astrobiological Exploration of Mars

NASA Technical Reports Server (NTRS)

Cabrol, N. A.; Wynn-Williams, D. D.; Crawford, D. A.; Grin, E. A.

2001-01-01

Three cases of recent aqueous environments are surveyed at Mars Orbiting Camera (MOC) high-resolution in the E-Gorgonum, Newton and Hale craters and their astrobiological implications assessed. Additional information is contained in the original extended abstract.

Horowitz checks flight notes at the commander's station

NASA Image and Video Library

2001-08-10

STS105-E-5002 (10 August 2001) --- Astronaut Scott J. Horowitz, STS-105 commander, checks flight notes at the commander's station on the flight deck of the Earth-orbiting Space Shuttle Discovery. The image was recorded with a digital still camera.

Horowitz checks flight notes at the commander's station

NASA Image and Video Library

2001-08-10

STS105-E-5001 (10 August 2001) --- Astronaut Scott J. Horowitz, STS-105 commander, checks flight notes at the commander's station on the flight deck of the Earth-orbiting Space Shuttle Discovery. The image was recorded with a digital still camera.

Full-Frame Reference for Test Photo of Moon

NASA Image and Video Library

2005-09-10

This pair of views shows how little of the full image frame was taken up by the Moon in test images taken Sept. 8, 2005, by the High Resolution Imaging Science Experiment HiRISE camera on NASA Mars Reconnaissance Orbiter.

Skylab (SL)-3 - Astronaut Jack R. Lousma - Utensils

NASA Image and Video Library

1973-09-19

S73-34198 (1 Aug. 1973) --- A close-up view of the hands of astronaut Jack R. Lousma, Skylab 3 pilot, using a silverware utensil to gather food at the food station, in this photographic reproduction taken from a television transmission made by a color TV camera aboard the Skylab space station in Earth orbit. Astronaut Alan L. Bean, commander, had just zoomed the TV camera in for this close-up of the food tray following a series of wide shots of Lousma at the food station. Photo credit: NASA

VizieR Online Data Catalog: Hubble Tarantula Treasury Project (HTTP). III. (Sabbi+, 2016)

NASA Astrophysics Data System (ADS)

Sabbi, E.; Lennon, D. J.; Anderson, J.; Cignoni, M.; van der Marel, R. P.; Zaritsky, D.; de Marchi, G.; Panagia, N.; Gouliermis, D. A.; Grebel, E. K.; Gallagher, J. S., III; Smith, L. J.; Sana, H.; Aloisi, A.; Tosi, M.; Evans, C. J.; Arab, H.; Boyer, M.; de Mink, S. E.; Gordon, K.; Koekemoer, A. M.; Larsen, S. S.; Ryon, J. E.; Zeidler, P.

2016-02-01

Hubble Tarantula Treasury Project (HTTP; HST 12939, PI Elena Sabbi + HST 12499, PI Danny Lennon) was awarded 60 orbits of HST time in cycle 20 to survey the entire Tarantula Nebula (30 Doradus), using both the UVIS and the IR channels of the Wide Field Camera 3 (WFC3), and, in parallel, the Wide Field Channel (WFC) of the Advanced Camera for Surveys (ACS). See log of the observations (from 2011 Oct 03 to 2013 Sep 17) in table 1. (2 data files).

Earth Observation taken during the 41G mission

NASA Image and Video Library

2009-06-25

41G-120-056 (October 1984) --- Parts of Israel, Lebanon, Palestine, Syria and Jordan and part of the Mediterranean Sea are seen in this nearly-vertical, large format camera's view from the Earth-orbiting Space Shuttle Challenger. The Sea of Galilee is at center frame and the Dead Sea at bottom center. The frame's center coordinates are 32.5 degrees north latitude and 35.5 degrees east longitude. A Linhof camera, using 4" x 5" film, was used to expose the frame through one of the windows on Challenger's aft flight deck.

View of Arabella, one of the two Skylab 3 spiders used in experiment

NASA Technical Reports Server (NTRS)

1973-01-01

A close-up view of Arabella, one of the two Skylab 3 common cross spiders 'Araneus diadematus,' and the web it had spun in the zero gravity of space aboard the Skylab space station cluster in Earth orbit. This is a photographic reproduction made from a color television transmission aboard Skylab. Arabella and Anita, were housed in an enclosure onto which a motion picture camera and a still camera were attached to record the spiders' attempts to build a web in the weightless environment.

Two bright fireballs over Great Britain

NASA Astrophysics Data System (ADS)

Koukal, Jakub; Káčerek, Richard

2018-02-01

On November 24, 2017 shortly before midnight and on November 25, 2017 shortly before sunrise, two very bright fireballs lit up the sky over the United Kingdom. The UKMON (United Kingdom Meteor Observation Network) cameras and onboard cameras in the automobiles recorded their flight. The fireballs paths in the Earth's atmosphere were calculated, as well as the orbits of bodies in the Solar System. The flight of both bodies, the absolute magnitude of which approached the brightness of the full Moon, was also observed by numerous random observers from the public in Great Britain, Ireland and France.

RME 1323 and DTO 671 during second EVA of STS-87

NASA Image and Video Library

1997-12-03

STS087-752-035 (19 November – 5 December 1997) --- This out-the-window view shows the Autonomous Extravehicular Activity Robotic Camera Sprint (AERCam Sprint) free-flying in the vicinity of the cargo bay of the Earth-orbiting Space Shuttle Columbia. The AERCam Sprint is a prototype free-flying television camera that could be used for remote inspections of the exterior of the International Space Station (ISS). This view, backdropped over southern Madagascar, was taken during this flight's second Extravehicular Activity (EVA), on December 3, 1997.

RME 1323 and DTO 671 during second EVA of STS-87

NASA Image and Video Library

1997-12-03

STS087-752-034 (19 November - 5 December 1997) --- This out-the-window view shows the Autonomous Extravehicular Activity Robotic Camera Sprint (AERCam Sprint) free-flying in the vicinity of the cargo bay of the Earth-orbiting Space Shuttle Columbia. The AERCam Sprint is a prototype free-flying television camera that could be used for remote inspections of the exterior of the International Space Station (ISS). This view, backdropped over southern Madagascar, was taken during this flight's second extravehicular activity (EVA), on December 3, 1997.

3D for the people: multi-camera motion capture in the field with consumer-grade cameras and open source software

PubMed Central

Evangelista, Dennis J.; Ray, Dylan D.; Hedrick, Tyson L.

2016-01-01

ABSTRACT Ecological, behavioral and biomechanical studies often need to quantify animal movement and behavior in three dimensions. In laboratory studies, a common tool to accomplish these measurements is the use of multiple, calibrated high-speed cameras. Until very recently, the complexity, weight and cost of such cameras have made their deployment in field situations risky; furthermore, such cameras are not affordable to many researchers. Here, we show how inexpensive, consumer-grade cameras can adequately accomplish these measurements both within the laboratory and in the field. Combined with our methods and open source software, the availability of inexpensive, portable and rugged cameras will open up new areas of biological study by providing precise 3D tracking and quantification of animal and human movement to researchers in a wide variety of field and laboratory contexts. PMID:27444791

The Nimbus 4 data catalog. Volume 5: 1 November - 31 December 1970, data orbits 2776-3594

NASA Technical Reports Server (NTRS)

1971-01-01

A catalog of data acquired from the Nimbus 4 meteorological satellite is presented. The volume covers the period 1 November through 31 December 1970. The Nimbus 4 catalog presents the type of data available, anomalies in the data, and geographic location and time of the data. The subjects discussed are: (1) summary of operations, (2) orbital elements and daily sensors on table, (3) image dissector camera system montages, and (4) temperature-humidity infrared radiometer montages.

Astronaut Alan Bean flies the Astronaut Maneuvering Equipment

NASA Image and Video Library

1973-08-27

SL3-107-1215 (27 Aug. 1973) --- Astronaut Alan L. Bean, Skylab 3 commander, flies the M509 Astronaut Maneuvering Equipment in the forward dome area of the Orbital Workshop (OWS) on the space station cluster in Earth orbit. One of his fellow crewmen took this photograph with a 35mm Nikon camera. Bean is strapped into the back mounted, hand-controlled Automatically Stabilized Maneuvering Unit (ASMU). The dome area is about 22 feet in diameter and 19 feet from top to bottom. Photo credit: NASA

Skylab 2 astronauts seen in wardroom of crew quarters of Skylab 1 station

NASA Technical Reports Server (NTRS)

1973-01-01

Two of the three Skylab 2 astronauts are seen in the wardroom of the crew quarters of the Orbital Workshop of the Skylab 1 space station cluster in Earth orbit in this reproduction taken from a color television transmission made by a TV camera aboard the space station. They are preparing to eat a meal. Astronaut Charles Conrad Jr., commander, is in the right foreground. In the background is scientist-astronaut Joseph P. Kerwin, science pilot.

Polar Landforms

NASA Technical Reports Server (NTRS)

2005-01-01

10 August 2005 This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows eroded remnants of carbon dioxide ice in the south polar residual cap of Mars. The scarps that outline each small mesa have retreated about 3 meters (10 feet) per Mars year since MGS began orbiting the red planet in 1997.

Location near: 87.0oS, 31.9oW Image width: width: 3 km (1.9 mi) Illumination from: upper left Season: Southern Spring

Astronaut Charles Conrad poses in shower facility in crew quarters

NASA Technical Reports Server (NTRS)

1973-01-01

Astronaut Charles Conrad Jr., Skylab 2 commander, smiles for the camera after a hot bath in the shower facility in the crew quarters of the Orbital Workshop of the Skylab 2 space station cluster in Earth orbit. In deploying the shower facility the shower curtain is pulled up from the floor and attached to the ceiling. The water comes through a push-button shower head attached to a flexible hose. Water is drawn off by a vacuum system.

ASTRONAUT KERWIN, JOSEPH P. - EXTRAVEHICULAR ACTIVITY (EVA) - SKYLAB (SL)-2

NASA Image and Video Library

1973-06-01

S73-27562 (June 1973) --- Scientist-astronaut Joseph P. Kerwin, Skylab 2 science pilot, performs extravehicular activity (EVA) at the Skylab 1 and 2 space station cluster in Earth orbit, as seen in this reproduction taken from a color television transmission made by a TV camera aboard the station. Kerwin is just outside the Airlock Module. Kerwin assisted astronaut Charles Conrad Jr., Skylab 2 commander, during the successful EVA attempt to free the stuck solar array system wing on the Orbital Workshop. Photo credit: NASA

View of the HST berthed to the Shuttle Atlantis

NASA Image and Video Library

2009-05-13

S125-E-007257 (14 May 2009) --- A wide view of the Hubble Space Telescope, locked down in the cargo bay of the Earth-orbiting Space Shuttle Atlantis, which will be site of a great deal of hands-on servicing over the next five days. The Canadian-built remote manipulator system arm (right), with its video cameras documenting activity in the shuttle's cargo bay all week, was instrumental in grappling and subsequently capturing the giant orbital observatory for the final servicing mission.

Rover Team Decides: Safety First

NASA Technical Reports Server (NTRS)

2006-01-01

NASA's Mars Exploration Rover Spirit recorded this view while approaching the northwestern edge of 'Home Plate,' a circular plateau-like area of bright, layered outcrop material roughly 80 meters (260 feet) in diameter. The images combined into this mosaic were taken by Spirit's navigation camera during the rover's 746th, 748th and 750th Martian days, or sols (Feb. 7, 9 and 11, 2006).

With Martian winter closing in, engineers and scientists working with NASA's Mars Exploration Rover Spirit decided to play it safe for the time being rather than attempt to visit the far side of Home Plate in search of rock layers that might show evidence of a past watery environment. This feature has been one of the major milestones of the mission. Though it's conceivable that rock layers might be exposed on the opposite side, sunlight is diminishing on the rover's solar panels and team members chose not to travel in a counterclockwise direction that would take the rover to the west and south slopes of the plateau. Slopes in that direction are hidden from view and team members chose, following a long, thorough discussion, to have the rover travel clockwise and remain on north-facing slopes rather than risk sending the rover deeper into unknown terrain.

In addition to studying numerous images from Spirit's cameras, team members studied three-dimensional models created with images from the Mars Orbiter Camera on NASA's Mars Globel Surveyor orbiter. The models showed a valley on the southern side of Home Plate, the slopes of which might cause the rover's solar panels to lose power for unknown lengths of time. In addition, images from Spirit's cameras showed a nearby, talus-covered section of slope on the west side of Home Plate, rather than exposed rock layers scientists eventually hope to investigate.

Home Plate has been on the rover's potential itinerary since the early days of the mission, when it stood out in images taken by the Mars Orbiter Camera shortly after the rover landed on Mars. Spirit arrived at Home Plate after traveling 4 miles (6.4 kilometers) across the plains of Gusev Crater, up the slopes of 'West Spur' and 'Husband Hill,' and down again. Scientists are studying the origin of the layering in the outcrop using the Athena science instruments on the rover's arm.

Photogrammetric Processing of Planetary Linear Pushbroom Images Based on Approximate Orthophotos

NASA Astrophysics Data System (ADS)

Geng, X.; Xu, Q.; Xing, S.; Hou, Y. F.; Lan, C. Z.; Zhang, J. J.

2018-04-01

It is still a great challenging task to efficiently produce planetary mapping products from orbital remote sensing images. There are many disadvantages in photogrammetric processing of planetary stereo images, such as lacking ground control information and informative features. Among which, image matching is the most difficult job in planetary photogrammetry. This paper designs a photogrammetric processing framework for planetary remote sensing images based on approximate orthophotos. Both tie points extraction for bundle adjustment and dense image matching for generating digital terrain model (DTM) are performed on approximate orthophotos. Since most of planetary remote sensing images are acquired by linear scanner cameras, we mainly deal with linear pushbroom images. In order to improve the computational efficiency of orthophotos generation and coordinates transformation, a fast back-projection algorithm of linear pushbroom images is introduced. Moreover, an iteratively refined DTM and orthophotos scheme was adopted in the DTM generation process, which is helpful to reduce search space of image matching and improve matching accuracy of conjugate points. With the advantages of approximate orthophotos, the matching results of planetary remote sensing images can be greatly improved. We tested the proposed approach with Mars Express (MEX) High Resolution Stereo Camera (HRSC) and Lunar Reconnaissance Orbiter (LRO) Narrow Angle Camera (NAC) images. The preliminary experimental results demonstrate the feasibility of the proposed approach.

SELMA: a mission to study lunar environment and surface interaction

NASA Astrophysics Data System (ADS)

Barabash, Stas; Futaana, Yoshifumi

2017-04-01

SELMA (Surface, Environment, and Lunar Magnetic Anomalies) proposed for the ESA M5 mission opportunity is a mission to study how the Moon environment and surface interact. SELMA addresses four overarching science questions: (1) What is the origin of water on the Moon? (2) How do the "volatile cycles" on the Moon work? (3) How do the lunar mini-magnetospheres work? (4) What is the influence of dust on the lunar environment and surface? SELMA uses a unique combination of remote sensing via UV, IR, and energetic neutral atoms and local measurements of plasma, fields, waves, exospheric gasses, and dust. It will also conduct an impact experiment to investigate volatile content in the soil of the permanently shadowed area of the Shakleton crater. SELMA carries an impact probe to sound the Reiner-Gamma mini-magnetosphere and its interaction with the lunar regolith from the SELMA orbit down to the surface. The SELMA science objectives include: - Establish the role of the solar wind and exosphere in the formation of the water bearing materials; - Determine the water content in the regolith of the permanently shadowed region and its isotope composition; - Establish variability, sources and sinks of the lunar exosphere and its relations to impact events; - Investigate a mini-magnetosphere interaction with the solar wind; - Investigate the long-term effects of mini-magnetospheres on the local surface; - Investigate how the impact events affect the lunar dust environments; - Investigate how the plasma effects result in lofting the lunar dust; SELMA is a flexible and short (15 months) mission including the following elements SELMA orbiter, SELMA Impact Probe for Magnetic Anomalies (SIP-MA), passive Impactor, and Relaying CubeSat (RCS). SELMA is placed on quasi-frozen polar orbit 30 km x 200 km with the pericenter over the South Pole. Approximately 9 months after the launch SELMA releases SIP-MA to sound the Reiner-Gamma magnetic anomaly with very high time resolution <0.5 s to investigate small-scale structure of the respective mini-magnetosphere. At the end of the mission the passive impactor impacts the permanently shadowed region of the Shakleton crater >10 sec before SELMA and SELMA orbiter flies through the resulted plume to perform high resolution mass spectroscopy of the released volatiles. The data are downlinked to ground and RCS. RCS stays on orbit for 2 more hours to downlink the complete data set. SELMA orbiter payload include: Remote sensing instruments - Infrared and visible spectrometer with spectral range 400 - 3600 nm; - Wide angle and transient phenomena camera to detect meteoroid impact (>100 g) - Moon UV imaging spectrometer with spectral range 115 - 315 nm - ENA telescope with an angular resolution < 10 ̊ In-situ instruments - Lunar ion spectrometer M/ΔM > 80 - Lunar scattered proton and negative ion experiment: - Lunar electron spectrometer - Moon magnetometer - Plasma wave instrument - Lunar dust detector: M>10-15 kg - Lunar exospheric mass spectrometer: M/ΔM > 1000 SIP-MA payload includes: - Waves and electric field instrument - Impact probe ions and electrons spectrometer - Impact probe magnetometer - Context camera Passive 10 kg copper spherical impactor

Spacecraft camera image registration

NASA Technical Reports Server (NTRS)

Kamel, Ahmed A. (Inventor); Graul, Donald W. (Inventor); Chan, Fred N. T. (Inventor); Gamble, Donald W. (Inventor)

1987-01-01

A system for achieving spacecraft camera (1, 2) image registration comprises a portion external to the spacecraft and an image motion compensation system (IMCS) portion onboard the spacecraft. Within the IMCS, a computer (38) calculates an image registration compensation signal (60) which is sent to the scan control loops (84, 88, 94, 98) of the onboard cameras (1, 2). At the location external to the spacecraft, the long-term orbital and attitude perturbations on the spacecraft are modeled. Coefficients (K, A) from this model are periodically sent to the onboard computer (38) by means of a command unit (39). The coefficients (K, A) take into account observations of stars and landmarks made by the spacecraft cameras (1, 2) themselves. The computer (38) takes as inputs the updated coefficients (K, A) plus synchronization information indicating the mirror position (AZ, EL) of each of the spacecraft cameras (1, 2), operating mode, and starting and stopping status of the scan lines generated by these cameras (1, 2), and generates in response thereto the image registration compensation signal (60). The sources of periodic thermal errors on the spacecraft are discussed. The system is checked by calculating measurement residuals, the difference between the landmark and star locations predicted at the external location and the landmark and star locations as measured by the spacecraft cameras (1, 2).

Development of an Extra-vehicular (EVA) Infrared (IR) Camera Inspection System

NASA Technical Reports Server (NTRS)

Gazarik, Michael; Johnson, Dave; Kist, Ed; Novak, Frank; Antill, Charles; Haakenson, David; Howell, Patricia; Pandolf, John; Jenkins, Rusty; Yates, Rusty

2006-01-01

Designed to fulfill a critical inspection need for the Space Shuttle Program, the EVA IR Camera System can detect crack and subsurface defects in the Reinforced Carbon-Carbon (RCC) sections of the Space Shuttle s Thermal Protection System (TPS). The EVA IR Camera performs this detection by taking advantage of the natural thermal gradients induced in the RCC by solar flux and thermal emission from the Earth. This instrument is a compact, low-mass, low-power solution (1.2cm3, 1.5kg, 5.0W) for TPS inspection that exceeds existing requirements for feature detection. Taking advantage of ground-based IR thermography techniques, the EVA IR Camera System provides the Space Shuttle program with a solution that can be accommodated by the existing inspection system. The EVA IR Camera System augments the visible and laser inspection systems and finds cracks and subsurface damage that is not measurable by the other sensors, and thus fills a critical gap in the Space Shuttle s inspection needs. This paper discusses the on-orbit RCC inspection measurement concept and requirements, and then presents a detailed description of the EVA IR Camera System design.

Radiometric stability of the Multi-angle Imaging SpectroRadiometer (MISR) following 15 years on-orbit

NASA Astrophysics Data System (ADS)

Bruegge, Carol J.; Val, Sebastian; Diner, David J.; Jovanovic, Veljko; Gray, Ellyn; Di Girolamo, Larry; Zhao, Guangyu

2014-09-01

The Multi-angle Imaging SpectroRadiometer (MISR) has successfully operated on the EOS/ Terra spacecraft since 1999. It consists of nine cameras pointing from nadir to 70.5° view angle with four spectral channels per camera. Specifications call for a radiometric uncertainty of 3% absolute and 1% relative to the other cameras. To accomplish this, MISR utilizes an on-board calibrator (OBC) to measure camera response changes. Once every two months the two Spectralon panels are deployed to direct solar-light into the cameras. Six photodiode sets measure the illumination level that are compared to MISR raw digital numbers, thus determining the radiometric gain coefficients used in Level 1 data processing. Although panel stability is not required, there has been little detectable change in panel reflectance, attributed to careful preflight handling techniques. The cameras themselves have degraded in radiometric response by 10% since launch, but calibration updates using the detector-based scheme has compensated for these drifts and allowed the radiance products to meet accuracy requirements. Validation using Sahara desert observations show that there has been a drift of ~1% in the reported nadir-view radiance over a decade, common to all spectral bands.

Autonomous Path Planning for On-Orbit Servicing Vehicles

NASA Astrophysics Data System (ADS)

McInnes, C. R.

On-orbit servicing has long been considered as a means of reducing mission costs. While automated on-orbit servicing of satellites in LEO and GEO has yet to be realised, the International Space Station (ISS) will require servicing in a number of forms for re-supply, external visual inspection and maintenance. This paper will discuss a unified approach to path planning for such servicing vehicles using artificial potential field methods. In particular, path constrained rendezvous and docking of the ESA Automated Transfer Vehicle (ATV) at the ISS will be investigated as will mission and path planning tools for the Daimler-Chrysler Aerospace ISS Inspector free-flying camera. Future applications for free-flying microcameras and co-operative control between multiple free-flyers for on-orbit assembly will also be considered.

Liquid Water on the Surface of Mars Today: Present Gully Activity Observed by the Mars Reconnaissance Orbiter (MRO) and Mars Global Surveyor (MGS) and Direction for Future Missions

NASA Astrophysics Data System (ADS)

Harrison, T. N.; Malin, M. C.; Edgett, K. S.

2009-12-01

Eight new flows in martian mid-latitude gullies have been found using the MRO Context Camera and MGS Mars Orbiter Camera. Each formed during 1999-2009. Using MRO HiRISE images, we find that the morphology and inferred emplacement behavior of these features is consistent with those of debris flows fluidized by a liquid medium and not by dry, granular flows. Evidence comes from the patterns of flow around obstacles, ponding in and subsequent overtopping of topographic depressions, and super-elevation of deposits on channel banks where the channels change direction, attributes consistent with a liquid but not with fluid-like granular flow. Additional evidence includes anastomoses in distal reaches and lobate terminations. Of the 8 flows, 3 have formation dates constrained to within a single Mars year (although not the same year); these 3 formed during autumn to early spring, demonstrating that summer warming is not participating in creating the liquid (i.e., that would melt snow or ice). The new gully deposits indicate that some gullies are currently active, suggesting that Mars has liquid water today and it occasionally appears on the planet’s surface. NASA’s Mars Exploration Program has focused on the “follow the water” theme and is now shifting toward “habitability” and life detection. Places where liquid water comes to the Martian surface today warrant detailed investigation. Martian astrobiology involves the search for evidence of extinct and extant life. Discovery of ancient sedimentary rocks shifted emphasis from the Viking-era pursuit of present-day microbial life to MSL’s focus on habitable environments. Recent descriptions of contemporary methane production have renewed interest in searching for extant life. Missions to locations of potential present day life, whether indicated by methane or liquid water, must deal with the associated planetary protection issues (they are “special regions”). More information about such locations is critical. Present mission planning is focused on methane (a 2016 trace gas orbiter), while the on-going gully activity is not being subjected to the same level of examination. Active gully locations might represent the optimum landing site for the much-discussed astrobiology rover mission (2018), provided additional information can be developed (i.e., the occurrence and recurrence rates and locations, and further evidence of the role of water). Long-term orbital monitoring at high resolution plus lander deployment from orbit after activity is detected are key gully mission objectives, as are the development of vehicles that can negotiate steep slopes and instruments that can detect sub-surface ice and/or water. As an added benefit, rather than learning only about a specific landing site, the knowledge gained from a single landed mission at a gullied site would be applicable to thousands of other locations on Mars.

100 New Impact Crater Sites Found on Mars

NASA Astrophysics Data System (ADS)

Kennedy, M. R.; Malin, M. C.

2009-12-01

Recent observations constrain the formation of 100 new impact sites on Mars over the past decade; 19 of these were found using the Mars Global Surveyor Mars Orbiter Camera (MOC), and the other 81 have been identified since 2006 using the Mars Reconnaissance Orbiter Context Camera (CTX). Every 6 meter/pixel CTX image is examined upon receipt and, where they overlap images of 0.3-240 m/pixel scale acquired by the same or other Mars-orbiting spacecraft, we look for features that may have changed. New impact sites are initially identified by the presence of a new dark spot or cluster of dark spots in a CTX image. Such spots may be new impact craters, or result from the effect of impact blasts on the dusty surface. In some (generally rare) cases, the crater is sufficiently large to be resolved in the CTX image. In most cases, however, the crater(s) cannot be seen. These are tentatively designated as “candidate” new impact sites, and the CTX team then creates an opportunity for the MRO spacecraft to point its cameras off-nadir and requests that the High Resolution Imaging Science Experiment (HiRISE) team obtain an image of ~0.3 m/pixel to confirm whether a crater or crater cluster is present. It is clear even from cursory examination that the CTX observations are areographically biased to dusty, higher albedo areas on Mars. All but 3 of the 100 new impact sites occur on surfaces with Lambert albedo values in excess of 23.5%. Our initial study of MOC images greatly benefited from the initial global observations made in one month in 1999, creating a baseline date from which we could start counting new craters. The global coverage by MRO Mars Color Imager is more than a factor of 4 poorer in resolution than the MOC Wide Angle camera and does not offer the opportunity for global analysis. Instead, we must rely on partial global coverage and global coverage that has taken years to accumulate; thus we can only treat impact rates statistically. We subdivide the total data set of 100 sites into 3 sets of observations: the original 19 MOC observations found in a survey of 15% of the planet, craters found only in CTX repeat coverage of 7% of Mars, and the remaining 69 craters found in a data set covering 40% of the planet. Using the mean interval between the latest observation preceding the impact and the first observation showing the impact for these groups of craters, we determine that the cratering rate is roughly 8 ± 6 x 10-7 craters/km2/yr for craters greater than ~1 m diameter. The cratering rate on Mars is sufficiently high to warrant consideration both for scientific studies and as a hazard to future exploration. Impacts are sufficiently frequent to act as seismic sources for studies of shallow crustal structure, if a seismic network is sufficiently dispersed and long-lived. Impacts large enough to provide information about deep interior structure are rare but probably occur on a decadal timescale. As recently noted in Science, new craters can be used to probe the distribution of subsurface ice and to provide samples from shallow depths that otherwise require meter-scale drilling systems. There is a finite probability that visitors to Mars for more than a month or two will hear or feel the effects of a nearby impact.

Activities of JAXA's Innovative Technology Center on Space Debris Observation

NASA Astrophysics Data System (ADS)

Yanagisawa, T.; Kurosaki, H.; Nakajima, A.

The innovative technology research center of JAXA is developing observational technologies for GEO objects in order to cope with the space debris problem. The center had constructed the optical observational facility for space debris at Mt. Nyukasa, Nagano in 2006. As observational equipments such as CCD cameras and telescopes were set up, the normal observation started. In this paper, the detail of the facilities and its activities are introduced. The observational facility contains two telescopes and two CCD cameras. The apertures of the telescopes are 35cm and 25 cm, respectively. One CCD camera in which 2K2K chip is installed can observe a sky region of 1.3 times 1.3-degree using the 35cm telescope. The other CCD camera that contains two 4K2K chips has an ability to observe 2.6 times 2.6-degree's region with the 25cm telescope. One of our main objectives is to detect faint GEO objects that are not catalogued. Generally, the detection limit of GEO object is determined by the aperture of the telescope. However, by improving image processing techniques, the limit may become low. We are developing some image processing methods that use many CCD frames to detect faint objects. We are trying to use FPGA (Field Programmable Gate Array) system to reduce analyzing time. By applying these methods to the data taken by a large telescope, the detection limit will be significantly lowered. The orbital determination of detected GEO debris is one of the important things to do. Especially, the narrow field view of an optical telescope hinders us from re-detection of the GEO debris for the orbital determination. Long observation time is required for one GEO object for the orbital determination that is inefficient. An effective observation strategy should be considered. We are testing one observation method invented by Umehara that observes one inertia position in the space. By observing one inertia position for two nights, a GEO object that passed through the position in the first night must pass through the position in the second night. The rough orbit is determined from two nights' data. The test observation showed that this method was able to detect many GEO objects and determined their orbits by three nights' observations. We also joined the campaign observations of IADC(Inter-Agency Space Debris Coordination Committee). By analyzing the observed data with the method that we developed, 88 catalogued and 38 un-catalogued objects were detected. The magnitude of the faintest object detected in this campaign observation was 18.5. The object is un-detectable by human inspection.

New Mars Camera's First Image of Mars from Mapping Orbit (Full Frame)

NASA Technical Reports Server (NTRS)

2006-01-01

The high resolution camera on NASA's Mars Reconnaissance Orbiter captured its first image of Mars in the mapping orbit, demonstrating the full resolution capability, on Sept. 29, 2006. The High Resolution Imaging Science Experiment (HiRISE) acquired this first image at 8:16 AM (Pacific Time). With the spacecraft at an altitude of 280 kilometers (174 miles), the image scale is 25 centimeters per pixel (10 inches per pixel). If a person were located on this part of Mars, he or she would just barely be visible in this image.

The image covers a small portion of the floor of Ius Chasma, one branch of the giant Valles Marineris system of canyons. The image illustrates a variety of processes that have shaped the Martian surface. There are bedrock exposures of layered materials, which could be sedimentary rocks deposited in water or from the air. Some of the bedrock has been faulted and folded, perhaps the result of large-scale forces in the crust or from a giant landslide. The image resolves rocks as small as small as 90 centimeters (3 feet) in diameter. It includes many dunes or ridges of windblown sand.

This image (TRA_000823_1720) was taken by the High Resolution Imaging Science Experiment camera onboard the Mars Reconnaissance Orbiter spacecraft on Sept. 29, 2006. Shown here is the full image, centered at minus 7.8 degrees latitude, 279.5 degrees east longitude. The image is oriented such that north is to the top. The range to the target site was 297 kilometers (185.6 miles). At this distance the image scale is 25 centimeters (10 inches) per pixel (with one-by-one binning) so objects about 75 centimeters (30 inches) across are resolved. The image was taken at a local Mars time of 3:30 PM and the scene is illuminated from the west with a solar incidence angle of 59.7 degrees, thus the sun was about 30.3 degrees above the horizon. The season on Mars is northern winter, southern summer.

[Photojournal note: Due to the large sizes of the high-resolution TIFF and JPEG files, some systems may experience extremely slow downlink time while viewing or downloading these images; some systems may be incapable of handling the download entirely.]

NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The HiRISE camera was built by Ball Aerospace & Technologies Corporation, Boulder, Colo., and is operated by the University of Arizona, Tucson.

Empty STS-114 orbiter Discovery Payload bay

NASA Image and Video Library

2005-07-29

ISS011-E-11340 (29 July 2005) --- A "fish-eye" lens on a digital still camera was used to record this image of the Space Shuttle Discovery from the International Space Station, to which it is docked for several days of joint activities.

Orbital motions of bubbles in an acoustic field

NASA Astrophysics Data System (ADS)

Shirota, Minori; Yamashita, Ko; Inamura, Takao

2012-09-01

This experimental study aims to clarify the mechanism of orbital motion of two oscillating bubbles in an acoustic field. Trajectory of the orbital motion on the wall of a spherical levitator was observed using a high-speed video camera. Because of a good repeatability in volume oscillation of bubbles, we were also able to observe the radial motion driven at 24 kHz by stroboscopic like imaging technique. The orbital motions of bubbles raging from 0.13 to 0.18 mm were examined with different forcing amplitude and in different viscous oils. As a result, we found that pairs of bubbles revolve along an elliptic orbit around the center of mass of the bubbles. We also found that the two bubbles perform anti-phase radial oscillation. Although this radial oscillation should result in a repulsive secondary Bjerknes force, the bubbles kept a constant separate distance of about 1 mm, which indicates the existence of centripetal primary Bjerknes force.

1. Context view shows approach of access road to summit, ...

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

1. Context view shows approach of access road to summit, communication towers and NW corner of lookout tower at center right. Camera is pointed SE. - Chelan Butte Lookout, Summit of Chelan Butte, Chelan, Chelan County, WA

1. Context view showing Bunker 103 on right and road ...

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

1. Context view showing Bunker 103 on right and road leading south to Bunker 104. Camera pointed SW. - Puget Sound Naval Shipyard, Munitions Storage Bunker, Naval Ammunitions Depot, North of Campbell Trail, Bremerton, Kitsap County, WA

'Inca City' is Part of a Circular Feature

NASA Technical Reports Server (NTRS)

2002-01-01

MGS MOC Release No. MOC2-319, 8 August 2002 [figure removed for brevity, see original site] 'Inca City' is the informal name given by Mariner 9 scientists in 1972 to a set of intersecting, rectilinear ridges that are located among the layered materials of the south polar region of Mars. Their origin has never been understood; most investigators thought they might be sand dunes, either modern dunes or, more likely, dunes that were buried, hardened, then exhumed. Others considered them to be dikes formed by injection of molten rock (magma) or soft sediment into subsurface cracks that subsequently hardened and then were exposed at the surface by wind erosion. The Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) has provided new information about the 'Inca City' ridges, though the camera's images still do not solve the mystery. The new information comes in the form of a MOC red wide angle context frame taken in mid-southern spring, shown above left and above right. The original Mariner 9 view of the ridges is seen at the center. The MOC image shows that the 'Inca City' ridges, located at 82oS, 67oW, are part of a larger circular structure that is about 86 km (53 mi) across. It is possible that this pattern reflects an origin related to an ancient, eroded meteor impact crater that was filled-in, buried, then partially exhumed. In this case, the ridges might be the remains of filled-in fractures in the bedrock into which the crater formed, or filled-in cracks within the material that filled the crater. Or both explanations could be wrong. While the new MOC image shows that 'Inca City' has a larger context as part of a circular form, it does not reveal the exact origin of these striking and unusual martian landforms.

"Inca City" is Part of a Circular Feature

NASA Image and Video Library

2002-08-07

MGS MOC Release No. MOC2-319, 8 August 2002. "Inca City" is the informal name given by Mariner 9 scientists in 1972 to a set of intersecting, rectilinear ridges that are located among the layered materials of the south polar region of Mars. Their origin has never been understood; most investigators thought they might be sand dunes, either modern dunes or, more likely, dunes that were buried, hardened, then exhumed. Others considered them to be dikes formed by injection of molten rock (magma) or soft sediment into subsurface cracks that subsequently hardened and then were exposed at the surface by wind erosion. The Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) has provided new information about the "Inca City" ridges, though the camera's images still do not solve the mystery. The new information comes in the form of a MOC red wide angle context frame taken in mid-southern spring, shown above left and above right. The original Mariner 9 view of the ridges is seen at the center. The MOC image shows that the "Inca City" ridges, located at 82°S, 67°W, are part of a larger circular structure that is about 86 km (53 mi) across. It is possible that this pattern reflects an origin related to an ancient, eroded meteor impact crater that was filled-in, buried, then partially exhumed. In this case, the ridges might be the remains of filled-in fractures in the bedrock into which the crater formed, or filled-in cracks within the material that filled the crater. Or both explanations could be wrong. While the new MOC image shows that "Inca City" has a larger context as part of a circular form, it does not reveal the exact origin of these striking and unusual martian landforms. http://photojournal.jpl.nasa.gov/catalog/PIA03918

Characterization of Orbital Debris Photometric Properties Derived from Laboratory-Based Measurements

NASA Technical Reports Server (NTRS)

Cowardin, H.; Abercromby, K.; Barker, E.; Seitzer, P.; Schildknecht, T.

2010-01-01

To better characterize and model optical data acquired from ground-based telescopes, the Optical Measurements Center (OMC) at NASA/JSC attempts to emulate illumination conditions seen in space using equipment and techniques that parallel telescopic observations and source-target-sensor orientations. The OMC uses a 75 Watt Xenon arc lamp as a solar simulator, an SBIG CCD camera with standard Johnson/Bessel filters, and a robotic arm to simulate an object's position and rotation. The laboratory uses known shapes, materials suspected to be consistent with the orbital debris population, and three phase angles to best match the lighting conditions of the telescope based data. The fourteen objects studied in the laboratory are fragments or materials acquired through ground-tests of scaled-model satellites/rocket bodies as well as material samples in more/less "flight-ready" condition. All fragments were measured at 10 increments in a full 360 rotation at 6 , 36 , and 60 phase angles. This paper will investigate published color photometric data for a series of orbital debris targets and compare it to the empirical photometric measurements generated in the OMC. Using the data acquired over specific rotational angles through different filters (B, V, R, I), a color index is acquired (B-R, R-I). Using these values and their associated lightcurves, this laboratory data is compared to observational data obtained on the 1 m telescope of the Astronomical Institute of the University of Bern (AUIB), the 0.9 m operated by the Small- and Medium-Aperture Research Telescope System (SMARTS) Consortium and the Curtis-Schmidt 0.6 m Michigan Orbital Debris Space Debris Telescope both located at Cerro Tololo Inter-American Observatory (CTIO). An empirical based optical characterization model will be presented to provide preliminary correlations between laboratory based and telescope-based data in the context of classification of GEO debris objects.

LROC Stereo Observations

NASA Astrophysics Data System (ADS)

Beyer, Ross A.; Archinal, B.; Li, R.; Mattson, S.; Moratto, Z.; McEwen, A.; Oberst, J.; Robinson, M.

2009-09-01

The Lunar Reconnaissance Orbiter Camera (LROC) will obtain two types of multiple overlapping coverage to derive terrain models of the lunar surface. LROC has two Narrow Angle Cameras (NACs), working jointly to provide a wider (in the cross-track direction) field of view, as well as a Wide Angle Camera (WAC). LRO's orbit precesses, and the same target can be viewed at different solar azimuth and incidence angles providing the opportunity to acquire `photometric stereo' in addition to traditional `geometric stereo' data. Geometric stereo refers to images acquired by LROC with two observations at different times. They must have different emission angles to provide a stereo convergence angle such that the resultant images have enough parallax for a reasonable stereo solution. The lighting at the target must not be radically different. If shadows move substantially between observations, it is very difficult to correlate the images. The majority of NAC geometric stereo will be acquired with one nadir and one off-pointed image (20 degree roll). Alternatively, pairs can be obtained with two spacecraft rolls (one to the left and one to the right) providing a stereo convergence angle up to 40 degrees. Overlapping WAC images from adjacent orbits can be used to generate topography of near-global coverage at kilometer-scale effective spatial resolution. Photometric stereo refers to multiple-look observations of the same target under different lighting conditions. LROC will acquire at least three (ideally five) observations of a target. These observations should have near identical emission angles, but with varying solar azimuth and incidence angles. These types of images can be processed via various methods to derive single pixel resolution topography and surface albedo. The LROC team will produce some topographic models, but stereo data collection is focused on acquiring the highest quality data so that such models can be generated later.

Modeling Floods in Athabasca Valles, Mars, Using CTX Stereo Topography

NASA Astrophysics Data System (ADS)

Dundas, C. M.; Keszthelyi, L. P.; Denlinger, R. P.; Thomas, O. H.; Galuszka, D.; Hare, T. M.; Kirk, R. L.; Howington-Kraus, E.; Rosiek, M.

2012-12-01

Among the most remarkable landforms on Mars are the outflow channels, which suggest the occurrence of catastrophic water floods in the past. Athabasca Valles has long been thought to be the youngest of these channels [1-2], although it has recently become clear that the young crater age applies to a coating lava flow [3]. Simulations with a 2.5-dimensional flood model have provided insight into the details of flood dynamics but have also demonstrated that the Digital Elevation Model (DEM) from the Mars Orbiter Laser Altimeter (MOLA) Mission Experiment Gridded Data Records includes significant artifacts at this latitude at the scales relevant for flood modeling [4]. In order to obtain improved topography, we processed stereo images from the Context Camera (CTX) of the Mars Reconnaissance Orbiter (MRO) using methods developed for producing topographic models of the Moon with images from the Lunar Reconnaissance Orbiter Camera, a derivative of the CTX camera. Some work on flood modeling with CTX stereo has been published by [5], but we will present several advances, including corrections to the published CTX optical distortion model and improved methods to combine the stereo and MOLA data. The limitations of current methods are the accuracy of control to MOLA and the level of error introduced when the MRO spacecraft is not in a high-stability mode during stereo imaging, leading to jitter impacting the derived topography. Construction of a mosaic of multiple stereo pairs, controlled to MOLA, allows us to consider flow through the cluster of streamlined islands in the upper part of the channel [6], including what is suggested to be the best example of flood-formed subaqueous dunes on Mars [7]. We will present results from running a flood model [4, 8] through the high-resolution (100 m/post) DEM covering the streamlined islands and subaqueous dunes, using results from a lower-resolution model as a guide to the inflow. By considering a range of flow levels below estimated peak flow, we can examine the flow behavior at the site of the apparent subaqueous dunes and, in particular, assess whether the flow in this area is uniquely conducive to the formation of such bedforms [e.g., 9]. [1] Berman D. C. and Hartmann W. K. (2002) Icarus 159, 1-17. [2] Burr D. M. et al. (2002) Icarus 159, 53-73. [3] Jaeger W. L. et al. (2010) Icarus 205, 230-243. [4] Keszthelyi L. P. et al. (2007) GRL 34, L21206. [5] McIntyre et al. (2012) JGR 117, E03009. [6] Burr D. (2005) Geomorphology 69, 242-252. [7] Burr D. M. et al. (2004) Icarus 171, 68-83. [8] Denlinger R. P. and O'Connell D. R. H. (2008) J. Hyd. Eng. 134, 1590-1602. [9] Kleinhans M. G. (2005) JGR 110, E12003.

Image Mosaicking Approach for a Double-Camera System in the GaoFen2 Optical Remote Sensing Satellite Based on the Big Virtual Camera.

PubMed

Cheng, Yufeng; Jin, Shuying; Wang, Mi; Zhu, Ying; Dong, Zhipeng

2017-06-20

The linear array push broom imaging mode is widely used for high resolution optical satellites (HROS). Using double-cameras attached by a high-rigidity support along with push broom imaging is one method to enlarge the field of view while ensuring high resolution. High accuracy image mosaicking is the key factor of the geometrical quality of complete stitched satellite imagery. This paper proposes a high accuracy image mosaicking approach based on the big virtual camera (BVC) in the double-camera system on the GaoFen2 optical remote sensing satellite (GF2). A big virtual camera can be built according to the rigorous imaging model of a single camera; then, each single image strip obtained by each TDI-CCD detector can be re-projected to the virtual detector of the big virtual camera coordinate system using forward-projection and backward-projection to obtain the corresponding single virtual image. After an on-orbit calibration and relative orientation, the complete final virtual image can be obtained by stitching the single virtual images together based on their coordinate information on the big virtual detector image plane. The paper subtly uses the concept of the big virtual camera to obtain a stitched image and the corresponding high accuracy rational function model (RFM) for concurrent post processing. Experiments verified that the proposed method can achieve seamless mosaicking while maintaining the geometric accuracy.

Photography in Dermatologic Surgery: Selection of an Appropriate Camera Type for a Particular Clinical Application.

PubMed

Chen, Brian R; Poon, Emily; Alam, Murad

2017-08-01

Photographs are an essential tool for the documentation and sharing of findings in dermatologic surgery, and various camera types are available. To evaluate the currently available camera types in view of the special functional needs of procedural dermatologists. Mobile phone, point and shoot, digital single-lens reflex (DSLR), digital medium format, and 3-dimensional cameras were compared in terms of their usefulness for dermatologic surgeons. For each camera type, the image quality, as well as the other practical benefits and limitations, were evaluated with reference to a set of ideal camera characteristics. Based on these assessments, recommendations were made regarding the specific clinical circumstances in which each camera type would likely be most useful. Mobile photography may be adequate when ease of use, availability, and accessibility are prioritized. Point and shoot cameras and DSLR cameras provide sufficient resolution for a range of clinical circumstances, while providing the added benefit of portability. Digital medium format cameras offer the highest image quality, with accurate color rendition and greater color depth. Three-dimensional imaging may be optimal for the definition of skin contour. The selection of an optimal camera depends on the context in which it will be used.

The GMT-Consortium Large Earth Finder (G-CLEF): an optical Echelle spectrograph for the Giant Magellan Telescope (GMT)

NASA Astrophysics Data System (ADS)

Szentgyorgyi, Andrew; Baldwin, Daniel; Barnes, Stuart; Bean, Jacob; Ben-Ami, Sagi; Brennan, Patricia; Budynkiewicz, Jamie; Chun, Moo-Young; Conroy, Charlie; Crane, Jeffrey D.; Epps, Harland; Evans, Ian; Evans, Janet; Foster, Jeff; Frebel, Anna; Gauron, Thomas; Guzmán, Dani; Hare, Tyson; Jang, Bi-Ho; Jang, Jeong-Gyun; Jordan, Andres; Kim, Jihun; Kim, Kang-Miin; Mendes de Oliveira, Claudia Mendes; Lopez-Morales, Mercedes; McCracken, Kenneth; McMuldroch, Stuart; Miller, Joseph; Mueller, Mark; Oh, Jae Sok; Onyuksel, Cem; Ordway, Mark; Park, Byeong-Gon; Park, Chan; Park, Sung-Joon; Paxson, Charles; Phillips, David; Plummer, David; Podgorski, William; Seifahrt, Andreas; Stark, Daniel; Steiner, Joao; Uomoto, Alan; Walsworth, Ronald; Yu, Young-Sam

2016-08-01

The GMT-Consortium Large Earth Finder (G-CLEF) will be a cross-dispersed, optical band echelle spectrograph to be delivered as the first light scientific instrument for the Giant Magellan Telescope (GMT) in 2022. G-CLEF is vacuum enclosed and fiber-fed to enable precision radial velocity (PRV) measurements, especially for the detection and characterization of low-mass exoplanets orbiting solar-type stars. The passband of G-CLEF is broad, extending from 3500Å to 9500Å. This passband provides good sensitivity at blue wavelengths for stellar abundance studies and deep red response for observations of high-redshift phenomena. The design of G-CLEF incorporates several novel technical innovations. We give an overview of the innovative features of the current design. G-CLEF will be the first PRV spectrograph to have a composite optical bench so as to exploit that material's extremely low coefficient of thermal expansion, high in-plane thermal conductivity and high stiffness-to-mass ratio. The spectrograph camera subsystem is divided into a red and a blue channel, split by a dichroic, so there are two independent refractive spectrograph cameras. The control system software is being developed in model-driven software context that has been adopted globally by the GMT. G-CLEF has been conceived and designed within a strict systems engineering framework. As a part of this process, we have developed a analytical toolset to assess the predicted performance of G-CLEF as it has evolved through design phases.

Space Shuttle orbit determination using empirical force modeling of attitude maneuvers for the German MOMS-02/D2 mission

NASA Technical Reports Server (NTRS)

Vonbraun, C.; Reigber, Christoph

1994-01-01

In the spring of 1993, the MOMS-02 (modular Optoelectronic Multispectral Scanner) camera, as part of the second German Spacelab mission aboard STS-55, successfully took digital threefold stereo images of the surface of the Earth. While the mission is experimental in nature, its primary goals are to produce high quality maps and three-dimensional digital terrain models of the Earth's surface. Considerable improvement in the quality of the terrain model can be attained if information about the position and attitude of the camera is included during the adjustment of the image data. One of the primary sources of error in the Shuttle's position is due to the significant attitude maneuvers conducted during the course of the mission. Various arcs, using actual Tracking and Data Relay Satellite (TDRSS) Doppler data of STS-55, were processed to determine how effectively empirical force modeling could be used to solve for the radial, transverse, and normal components of the orbit perturbations caused by these routine maneuvers. Results are presented in terms of overlap-orbit differences in the three components. Comparisons of these differences, before and after the maneuvers are estimated, show that the quality of an orbit can be greatly enhanced with this technique, even if several maneuvers are present. Finally, a discussion is made of some of the difficulties encountered with this approach, and some ideas for future studies are presented.

Temperature Gradient on Martian Moon Phobos

NASA Image and Video Library

2017-10-04

This image combines two products from the first pointing at the Martian moon Phobos by the Thermal Emission Imaging System (THEMIS) camera on NASA's Mars Odyssey orbiter, on Sept. 29, 2017. Surface-temperature information from observation in thermal-infrared wavelengths is overlaid on a more detailed image from a visible-light observation. The left edge of the small moon was in darkness, and the right edge in morning sunlight. Phobos has an oblong shape with average diameter of about 14 miles (22 kilometers). The distance to Phobos from Odyssey during the observation was about 3,424 miles (5,511 kilometers). Researchers will analyze the surface-temperature information from this observation and possible future THEMIS observations to learn how quickly the surface warms after sunup or cools after sundown. That could provide information about surface materials, because larger rocks heat or cool more slowly than smaller particles do. The thermal information in this image is from merging observations made in four thermal-infrared wavelength bands, centered from 11.04 microns to 14.88 microns. Researchers have been using THEMIS to examine Mars since early 2002, but the maneuver turning the orbiter around to point the camera at Phobos was developed only recently. Odyssey orbits Mars at an altitude of about 250 miles (400 kilometers), much closer to the planet than to Phobos, which orbits about 3,700 miles (6,000 kilometers) above the surface of Mars. https://photojournal.jpl.nasa.gov/catalog/PIA22057

A New Method for Wide-field Near-IR Imaging with the Hubble Space Telescope

NASA Astrophysics Data System (ADS)

Momcheva, Ivelina G.; van Dokkum, Pieter G.; van der Wel, Arjen; Brammer, Gabriel B.; MacKenty, John; Nelson, Erica J.; Leja, Joel; Muzzin, Adam; Franx, Marijn

2017-01-01

We present a new technique for wide and shallow observations using the near-infrared channel of Wide Field Camera 3 (WFC3) on the Hubble Space Telescope (HST). Wide-field near-IR surveys with HST are generally inefficient, as guide star acquisitions make it impractical to observe more than one pointing per orbit. This limitation can be circumvented by guiding with gyros alone, which is possible as long as the telescope has three functional gyros. The method presented here allows us to observe mosaics of eight independent WFC3-IR pointings in a single orbit by utilizing the fact that HST drifts by only a very small amount in the 25 s between non-destructive reads of unguided exposures. By shifting the reads and treating them as independent exposures the full resolution of WFC3 can be restored. We use this “drift and shift” (DASH) method in the Cycle 23 COSMOS-DASH program, which will obtain 456 WFC3 H 160 pointings in 57 orbits, covering an area of 0.6 degree in the COSMOS field down to H 160 = 25. When completed, the program will more than triple the area of extra-galactic survey fields covered by near-IR imaging at HST resolution. We demonstrate the viability of the method with the first four orbits (32 pointings) of this program. We show that the resolution of the WFC3 camera is preserved, and that structural parameters of galaxies are consistent with those measured in guided observations.

Experimental Comparison of Knife-Edge and Multi-Parallel Slit Collimators for Prompt Gamma Imaging of Proton Pencil Beams.

PubMed

Smeets, Julien; Roellinghoff, Frauke; Janssens, Guillaume; Perali, Irene; Celani, Andrea; Fiorini, Carlo; Freud, Nicolas; Testa, Etienne; Prieels, Damien

2016-01-01

More and more camera concepts are being investigated to try and seize the opportunity of instantaneous range verification of proton therapy treatments offered by prompt gammas emitted along the proton tracks. Focusing on one-dimensional imaging with a passive collimator, the present study experimentally compared in combination with the first, clinically compatible, dedicated camera device the performances of instances of the two main options: a knife-edge slit (KES) and a multi-parallel slit (MPS) design. These two options were experimentally assessed in this specific context as they were previously demonstrated through analytical and numerical studies to allow similar performances in terms of Bragg peak retrieval precision and spatial resolution in a general context. Both collimators were prototyped according to the conclusions of Monte Carlo optimization studies under constraints of equal weight (40 mm tungsten alloy equivalent thickness) and of the specificities of the camera device under consideration (in particular 4 mm segmentation along beam axis and no time-of-flight discrimination, both of which less favorable to the MPS performance than to the KES one). Acquisitions of proton pencil beams of 100, 160, and 230 MeV in a PMMA target revealed that, in order to reach a given level of statistical precision on Bragg peak depth retrieval, the KES collimator requires only half the dose the present MPS collimator needs, making the KES collimator a preferred option for a compact camera device aimed at imaging only the Bragg peak position. On the other hand, the present MPS collimator proves more effective at retrieving the entrance of the beam in the target in the context of an extended camera device aimed at imaging the whole proton track within the patient.

Autonomous Vision Navigation for Spacecraft in Lunar Orbit

NASA Astrophysics Data System (ADS)

Bader, Nolan A.

NASA aims to achieve unprecedented navigational reliability for the first manned lunar mission of the Orion spacecraft in 2023. A technique for accomplishing this is to integrate autonomous feature tracking as an added means of improving position and velocity estimation. In this thesis, a template matching algorithm and optical sensor are tested onboard three simulated lunar trajectories using linear covariance techniques under various conditions. A preliminary characterization of the camera gives insight into its ability to determine azimuth and elevation angles to points on the surface of the Moon. A navigation performance analysis shows that an optical camera sensor can aid in decreasing position and velocity errors, particularly in a loss of communication scenario. Furthermore, it is found that camera quality and computational capability are driving factors affecting the performance of such a system.

A math model for high velocity sensoring with a focal plane shuttered camera.

NASA Technical Reports Server (NTRS)

Morgan, P.

1971-01-01

A new mathematical model is presented which describes the image produced by a focal plane shutter-equipped camera. The model is based upon the well-known collinearity condition equations and incorporates both the translational and rotational motion of the camera during the exposure interval. The first differentials of the model with respect to exposure interval, delta t, yield the general matrix expressions for image velocities which may be simplified to known cases. The exposure interval, delta t, may be replaced under certain circumstances with a function incorporating blind velocity and image position if desired. The model is tested using simulated Lunar Orbiter data and found to be computationally stable as well as providing excellent results, provided that some external information is available on the velocity parameters.

STS-51 Discovery launch

NASA Image and Video Library

1993-09-12

STS051-S-108 (12 Sept. 1993) --- The Space Shuttle Discovery soars toward a nine-day stay in Earth-orbit to support the mission. Launch occurred at 7:45 a.m. (EDT) September 12, 1993. Note the diamond shock effect coming from the thrust of the three main engines. Onboard the shuttle were astronauts Frank L. Culbertson, Jr., William F. Readdy, Daniel W. Bursch, James H. Newman and Carl E. Walz, along with a number of payloads. The payloads included the Advanced Communications Technology Satellite (ACTS) with its Transfer Orbit Stage (TOS), the Orbiting Retrievable Far and Extreme Ultraviolet Spectrometer (ORFEUS) and its Shuttle Pallet Satellite (SPAS) carrier. This photograph was taken with a 35mm camera.

KSC-08pd1959

NASA Image and Video Library

2008-07-11

CAPE CANAVERAL, Fla. – In the Orbiter Processing Facility at NASA's Kennedy Space Center, STS-125 Mission Specialists Mike Massimino (left) and Michael Good (right) check out the orbiter boom sensor system and the attached camera in space shuttle Atlantis' payload bay. Equipment familiarization is part of the crew equipment interface test, which provides hands-on experience with hardware and equipment for the mission. Atlantis is targeted to launch Oct. 8 on the STS-125 mission to service the Hubble Space Telescope. The mission crew will perform history-making, on-orbit “surgery” on two important science instruments aboard the telescope. After capturing the telescope, two teams of spacewalking astronauts will perform the repairs during five planned spacewalks. Photo credit: NASA/Kim Shiflett

STS-31 MS Sullivan and Pilot Bolden monitor SE 82-16 Ion Arc on OV-103 middeck

NASA Technical Reports Server (NTRS)

1990-01-01

STS-31 Mission Specialist (MS) Kathryn D. Sullivan monitors and advises ground controllers of the activity inside the Student Experiment (SE) 82-16, Ion arc - studies of the effects of microgravity and a magnetic field on an electric arc, mounted in front of the middeck lockers aboard Discovery, Orbiter Vehicle (OV) 103. Pilot Charles F. Bolden uses a video camera and an ARRIFLEX motion picture camera to record the activity inside the special chamber. A sign in front of the experiment reads 'SSIP 82-16 Greg's Experiment Happy Graduation from STS-31.' SSIP stands for Shuttle Student Involvement Program. Gregory S. Peterson who developed the experiment (Greg's Experiment) is a student at Utah State University and monitored the experiment's operation from JSC's Mission Control Center (MCC) during the flight. Decals displayed in the background on the orbiter galley represent the Hubble Space Telescope (HST), the United States (U.S.) Naval Reserve, Navy Oceanographers, U.S. Navy, and Univer

Impacts on the Hubble Space Telescope Wide Field and Planetary Camera 2: Microanalysis and Recognition of Micrometeoroid Compositions

NASA Technical Reports Server (NTRS)

Kearsley, A. T.; Ross, D. K.; Anz-Meador, P.; Liou, J. C.; Opiela, J.; Grime, G. W.; Webb, R. P.; Jeynes, C.; Palitsin, V. V.; Colaux, J. L.;

STS-109 Flight Day 3 Highlights

NASA Technical Reports Server (NTRS)

2002-01-01

This footage from the third day of the STS-109 mission to service the Hubble Space Telescope (HST) begins with the grappling of the HST by the robotic arm of the Columbia Orbiter, operated by Mission Specialist Nancy Currie. During the grappling, numerous angles deliver close-up images of the telescope which appears to be in good shape despite many years in orbit around the Earth. Following the positioning of the HST on its berthing platform in the Shuttle bay, the robotic arm is used to perform an external survey of the telescope. Some cursory details are given about different equipment which will be installed on the HST including a replacement cooling system for the Near Infrared Camera Multi-Object Spectrometer (NICMOS) and the Advanced Camera for Surveys. Following the survey, there is footage of the retraction of both of the telescope's two flexible solar arrays, which was successful. These arrays will be replaced by rigid solar arrays with decreased surface area and increased performance.

VizieR Online Data Catalog: HST FGS-1r parallaxes for 8 metal-poor stars (Chaboyer+, 2017)

NASA Astrophysics Data System (ADS)

Chaboyer, B.; McArthur, B. E.; O'Malley, E.; Benedict, G. F.; Feiden, G. A.; Harrison, T. E.; McWilliam, A.; Nelan, E. P.; Patterson, R. J.; Sarajedini, A.

2017-08-01

Each program star was observed with the HST Advanced Camera for Surveys-Wide Field Camera (ACS/WFC) in the F606W and F814W filters. The CTE-corrected ACS/WFC images for the program stars were retrieved from MAST. These instrumental magnitudes were corrected for exposure time, matched to form colors, and calibrated to the VEGAMag and ground-based VI systems using the Sirianni+ (2005PASP..117.1049S) photometric transformations. Ground based photometry for all of our program stars were obtained using the New Mexico State University (NMSU) 1m telescope, the MDM 1.3m telescope, and the SMARTS 0.9m telescope. See appendix A1 for further details. We used HST FGS-1r, a two-axis interferometer, to make the astrometric observations. Eighty-nine orbits of HST astrometric observations were made between 2008 December and 2013 June. Every orbit contained several observations of the target and surrounding reference stars. (4 data files).

Analysis of GRACE Range-rate Residuals with Emphasis on Reprocessed Star-Camera Datasets

NASA Astrophysics Data System (ADS)

Goswami, S.; Flury, J.; Naeimi, M.; Bandikova, T.; Guerr, T. M.; Klinger, B.

2015-12-01

Since March 2002 the two GRACE satellites orbit the Earth at rela-tively low altitude. Determination of the gravity field of the Earth including itstemporal variations from the satellites' orbits and the inter-satellite measure-ments is the goal of the mission. Yet, the time-variable gravity signal has notbeen fully exploited. This can be seen better in the computed post-fit range-rateresiduals. The errors reflected in the range-rate residuals are due to the differ-ent sources as systematic errors, mismodelling errors and tone errors. Here, weanalyse the effect of three different star-camera data sets on the post-fit range-rate residuals. On the one hand, we consider the available attitude data andon other hand we take the two different data sets which has been reprocessedat Institute of Geodesy, Hannover and Institute of Theoretical Geodesy andSatellite Geodesy, TU Graz Austria respectively. Then the differences in therange-rate residuals computed from different attitude dataset are analyzed inthis study. Details will be given and results will be discussed.

The Kaguya Mission: Science Achievements and Data Release

NASA Astrophysics Data System (ADS)

Kato, Manabu; Sasaki, Susumu; Takizawa, Yoshisada

2010-05-01

Lunar orbiter Kaguya (SELENE) has impacted the Moon on July 10, 2009. The Kaguya mission has completed to observe the whole Moon for total twenty months; checkout term of three months, nominal one of ten months, and the extension of seven months. In the extended mission before the impact the measurements of magnetic field and gamma-ray from lower orbits have been perrformed successfully in addition to low altitude observation by Terraine Camera, Multiband Imager, and HDTV Camera. New data of intense magnetic anomaly and GRS data with higher spacial resolution has been acquired to study elemental distribution and magnetism of the Moon. New information and insights have been brought to lunar sciences in topography, gra-vimetry, geology, mineralogy, lithology, plasma physics. On November 1, 2009 the Kaguya team has released science data to the public as an international promise. The archive data can be accessed through Kaguya homepage of JAXA. Image gallary and 3D GIS system have been also put on view from the same homepage.

Lunar Satellite Snaps Image of Earth

NASA Image and Video Library

2014-05-07

This image, captured Feb. 1, 2014, shows a colorized view of Earth from the moon-based perspective of NASA's Lunar Reconnaissance Orbiter. Credit: NASA/Goddard/Arizona State University -- NASA's Lunar Reconnaissance Orbiter (LRO) experiences 12 "earthrises" every day, however LROC (short for LRO Camera) is almost always busy imaging the lunar surface so only rarely does an opportunity arise such that LROC can capture a view of Earth. On Feb. 1, 2014, LRO pitched forward while approaching the moon's north pole allowing the LROC Wide Angle Camera to capture Earth rising above Rozhdestvenskiy crater (112 miles, or 180 km, in diameter). Read more: go.nasa.gov/1oqMlgu NASA image use policy. NASA Goddard Space Flight Center enables NASA’s mission through four scientific endeavors: Earth Science, Heliophysics, Solar System Exploration, and Astrophysics. Goddard plays a leading role in NASA’s accomplishments by contributing compelling scientific knowledge to advance the Agency’s mission. Follow us on Twitter Like us on Facebook Find us on Instagram

A Physical Model-based Correction for Charge Traps in the Hubble Space Telescope ’s Wide Field Camera 3 Near-IR Detector and Its Applications to Transiting Exoplanets and Brown Dwarfs

DOE Office of Scientific and Technical Information (OSTI.GOV)

Zhou, Yifan; Apai, Dániel; Schneider, Glenn

The Hubble Space Telescope Wide Field Camera 3 (WFC3) near-IR channel is extensively used in time-resolved observations, especially for transiting exoplanet spectroscopy as well as brown dwarf and directly imaged exoplanet rotational phase mapping. The ramp effect is the dominant source of systematics in the WFC3 for time-resolved observations, which limits its photometric precision. Current mitigation strategies are based on empirical fits and require additional orbits to help the telescope reach a thermal equilibrium . We show that the ramp-effect profiles can be explained and corrected with high fidelity using charge trapping theories. We also present a model for this processmore » that can be used to predict and to correct charge trap systematics. Our model is based on a very small number of parameters that are intrinsic to the detector. We find that these parameters are very stable between the different data sets, and we provide best-fit values. Our model is tested with more than 120 orbits (∼40 visits) of WFC3 observations and is proved to be able to provide near photon noise limited corrections for observations made with both staring and scanning modes of transiting exoplanets as well as for starting-mode observations of brown dwarfs. After our model correction, the light curve of the first orbit in each visit has the same photometric precision as subsequent orbits, so data from the first orbit no longer need to be discarded. Near-IR arrays with the same physical characteristics (e.g., JWST/NIRCam ) may also benefit from the extension of this model if similar systematic profiles are observed.« less

A Physical Model-based Correction for Charge Traps in the Hubble Space Telescope’s Wide Field Camera 3 Near-IR Detector and Its Applications to Transiting Exoplanets and Brown Dwarfs

NASA Astrophysics Data System (ADS)

Zhou, Yifan; Apai, Dániel; Lew, Ben W. P.; Schneider, Glenn

2017-06-01

The Hubble Space Telescope Wide Field Camera 3 (WFC3) near-IR channel is extensively used in time-resolved observations, especially for transiting exoplanet spectroscopy as well as brown dwarf and directly imaged exoplanet rotational phase mapping. The ramp effect is the dominant source of systematics in the WFC3 for time-resolved observations, which limits its photometric precision. Current mitigation strategies are based on empirical fits and require additional orbits to help the telescope reach a thermal equilibrium. We show that the ramp-effect profiles can be explained and corrected with high fidelity using charge trapping theories. We also present a model for this process that can be used to predict and to correct charge trap systematics. Our model is based on a very small number of parameters that are intrinsic to the detector. We find that these parameters are very stable between the different data sets, and we provide best-fit values. Our model is tested with more than 120 orbits (∼40 visits) of WFC3 observations and is proved to be able to provide near photon noise limited corrections for observations made with both staring and scanning modes of transiting exoplanets as well as for starting-mode observations of brown dwarfs. After our model correction, the light curve of the first orbit in each visit has the same photometric precision as subsequent orbits, so data from the first orbit no longer need to be discarded. Near-IR arrays with the same physical characteristics (e.g., JWST/NIRCam) may also benefit from the extension of this model if similar systematic profiles are observed.

Improved Space Object Orbit Determination Using CMOS Detectors

NASA Astrophysics Data System (ADS)

Schildknecht, T.; Peltonen, J.; Sännti, T.; Silha, J.; Flohrer, T.

2014-09-01

CMOS-sensors, or in general Active Pixel Sensors (APS), are rapidly replacing CCDs in the consumer camera market. Due to significant technological advances during the past years these devices start to compete with CCDs also for demanding scientific imaging applications, in particular in the astronomy community. CMOS detectors offer a series of inherent advantages compared to CCDs, due to the structure of their basic pixel cells, which each contains their own amplifier and readout electronics. The most prominent advantages for space object observations are the extremely fast and flexible readout capabilities, feasibility for electronic shuttering and precise epoch registration, and the potential to perform image processing operations on-chip and in real-time. The major challenges and design drivers for ground-based and space-based optical observation strategies have been analyzed. CMOS detector characteristics were critically evaluated and compared with the established CCD technology, especially with respect to the above mentioned observations. Similarly, the desirable on-chip processing functionalities which would further enhance the object detection and image segmentation were identified. Finally, we simulated several observation scenarios for ground- and space-based sensor by assuming different observation and sensor properties. We will introduce the analyzed end-to-end simulations of the ground- and space-based strategies in order to investigate the orbit determination accuracy and its sensitivity which may result from different values for the frame-rate, pixel scale, astrometric and epoch registration accuracies. Two cases were simulated, a survey using a ground-based sensor to observe objects in LEO for surveillance applications, and a statistical survey with a space-based sensor orbiting in LEO observing small-size debris in LEO. The ground-based LEO survey uses a dynamical fence close to the Earth shadow a few hours after sunset. For the space-based scenario a sensor in a sun-synchronous LEO orbit, always pointing in the anti-sun direction to achieve optimum illumination conditions for small LEO debris, was simulated. For the space-based scenario the simulations showed a 20 130 % improvement of the accuracy of all orbital parameters when varying the frame rate from 1/3 fps, which is the fastest rate for a typical CCD detector, to 50 fps, which represents the highest rate of scientific CMOS cameras. Changing the epoch registration accuracy from a typical 20.0 ms for a mechanical shutter to 0.025 ms, the theoretical value for the electronic shutter of a CMOS camera, improved the orbit accuracy by 4 to 190 %. The ground-based scenario also benefit from the specific CMOS characteristics, but to a lesser extent.

Martian Mystery: Do Some Materials Flow Uphill?

NASA Technical Reports Server (NTRS)

1999-01-01

Some of the geological features of Mars defy conventional, or simple, explanations. A recent example is on the wall of a 72 kilometer-wide (45 mile-wide) impact crater in Promethei Terra. The crater (above left) is located at 39oS, 247oW. Its inner walls appear in low-resolution images to be deeply gullied.

A high resolution Mars Orbiter Camera (MOC) image shows that each gully on the crater's inner wall contains a tongue of material that appears to have flowed (to best see this, click on the icon above right and examine the full image). Ridges and grooves that converge toward the center of each gully and show a pronounced curvature are oriented in a manner that seems to suggest that material has flowed from the top toward the bottom of the picture. This pattern is not unlike pouring pancake batter into a pan... the viscous fluid will form a steep, lobate margin and spread outward across the pan. The ridges and grooves seen in the image are also more reminiscent of the movement of material out and away from a place of confinement, as opposed to the types of features seen when they flow into a more confined area. Mud and lava-flows, and even some glaciers, for the most part behave in this manner. From these observations, and based solely on the appearance, one might conclude that the features formed by moving from the top of the image towards the bottom.

But this is not the case! The material cannot have flowed from the top towards the bottom of the area seen in the high resolution image (above, right), because the crater floor (which is the lowest area in the image) is at the top of the picture. The location and correct orientation of the high resolution image is shown by a white box in the context frame on the left. Since gravity pulls the material in the gullies downhill not uphill the pattern of ridges and grooves found on these gully-filling materials is puzzling. An explanation may lie in the nature of the material (e.g., how viscous was the pancake batter-like material?) and how rapidly it moved, but for now this remains an unexplained martian phenomenon.

The context image (above, left) was taken by the MOC red wide angle camera at the same time that the MOC narrow angle camera obtained the high resolution view (above, right). Context images such as this provide a simple way to determine the location of each new high resolution view of the planet. Both images are illuminated from the upper left. The high resolution image covers an area 3 km (1.9 mi) across.

Malin Space Science Systems and the California Institute of Technology built the MOC using spare hardware from the Mars Observer mission. MSSS operates the camera from its facilities in San Diego, CA. The Jet Propulsion Laboratory's Mars Surveyor Operations Project operates the Mars Global Surveyor spacecraft with its industrial partner, Lockheed Martin Astronautics, from facilities in Pasadena, CA and Denver, CO.

Hellas as a Possible Site of Ancient Ice-Covered Lakes on Mars

NASA Technical Reports Server (NTRS)

Moore, Jeffrey M.; Wilhelms, Don E.; DeVincenzi, Donald (Technical Monitor)

2002-01-01

Based on topographic, morphologic, and stratigraphic evidence, we propose that ancient water-laid sediment is the dominant component of deposits within Hellas Planitia, Mars. Multiply layered sediment is manifested by alternating benches and scarps visible in Mars Orbiting Camera narrow-angle (MOC NA) images. Viking Orbiter camera and MOC NA images were used to map contacts and stratigraphically order the different materials units within Hellas. Mar's Orbiting Laser Altimeter (MOLA) data reveal that the contacts of these sedimentary units, as well as a number of scarps or other abrupt changes in landscape texture, trace contours of constant elevation for thousands of km, and in one case all around the basin. Channels, consensually interpreted to be cut by water, lead into the basin. MOLA results indicate that the area encompassed by greater Hellas' highest closed contour is nearly one-fifth that of the entire northern plains, making the Hellas 'drainage' area much larger than previously reported. If lakes formed under climatic conditions similar to the modern Martian climate, they would develop thick ice carapaces, then the lakes would eventually sublimate away. Two units within Hellas exhibit a reticulate or honeycomb pattern we speculate are impressions made by lake-lowered ice blocks grounding into initially soft mud.

Hellas as a possible site of ancient ice-covered lakes on Mars

USGS Publications Warehouse

Moore, Johnnie N.; Wilhelms, D.E.

2001-01-01

Based on topographic, morphologic, and stratigraphic evidence, we propose that ancient water-laid sediment is the dominant component of deposits within Hellas Planitia, Mars. Multiple-layered sediment is manifested by alternating benches and scarps visible in Mars orbiting camera narrow-angle (MOC NA) images. Viking Orbiter camera and MOC NA images were used to map contacts and stratigraphically order the different materials units within Hellas. Mars orbiting laser altimeter (MOLA) data reveal that the contacts of these sedimentary units, as well as a number of scarps or other abrupt changes in landscape texture, trace contours of constant elevation for thousands of km, and in one case all around the basin. Channels, consensually interpreted to be cut by water, lead into the basin. MOLA results indicate that the area encompassed by greater Hellas' highest closed contour is nearly one-fifth that of the entire northern plains, making the Hellas "drainage" area much larger than previously reported. If lakes formed under climatic conditions similar to the modern Martian climate, they would develop thick ice carapaces, then the lakes would eventually sublimate away. Two units within Hellas exhibit a reticulate or honeycomb pattern, which we speculate are impressions made by lake-lowered ice blocks grounding into initially soft mud.

It's a Bird, It's a Plane, It's a... Spacecraft?

NASA Technical Reports Server (NTRS)

2004-01-01

Observing the sky with the green filter of it panoramic camera, the Mars Exploration Rover Spirit came across a surprise: a streak across the sky. The streak, seen in the middle of this mosaic of images taken by the navigation and panoramic cameras, was probably the brightest object in the sky at the time. Scientists theorize that the mystery line could be either a meteorite or one of seven out-of-commission spacecraft still orbiting Mars. Because the object appeared to move 4 degrees of an arc in 15 seconds it is probably not the Russian probes Mars 2, Mars 3, Mars 5, or Phobos 2; or the American probes Mariner 9 or Viking 1. That leaves Viking 2, which has a polar orbit that would fit with the north-south orientation of the streak. In addition, only Viking 1 and 2 were left in orbits that could produce motion as fast as that seen by Spirit. Said Mark Lemmon, a rover team member from Texas A&M University, Texas, 'Is this the first image of a meteor on Mars, or an image of a spacecraft sent from another world during the dawn of our robotic space exploration program? We may never know, but we are still looking for clues'.

The inset shows only the panoramic image of the streak.

Lunar Reconnaissance Orbiter Data Enable Science and Terrain Analysis of Potential Landing Sites in South Pole-Aitken Basin

NASA Astrophysics Data System (ADS)

Jolliff, B. L.

2017-12-01

Exploring the South Pole-Aitken basin (SPA), one of the key unsampled geologic terranes on the Moon, is a high priority for Solar System science. As the largest and oldest recognizable impact basin on the Moon, it anchors the heavy bombardment chronology. It is thus a key target for sample return to better understand the impact flux in the Solar System between formation of the Moon and 3.9 Ga when Imbrium, one of the last of the great lunar impact basins, formed. Exploration of SPA has implications for understanding early habitable environments on the terrestrial planets. Global mineralogical and compositional data exist from the Clementine UV-VIS camera, the Lunar Prospector Gamma Ray Spectrometer, the Moon Mineralogy Mapper (M3) on Chandrayaan-1, the Chang'E-1 Imaging Interferometer, the spectral suite on SELENE, and the Lunar Reconnaissance Orbiter Cameras (LROC) Wide Angle Camera (WAC) and Diviner thermal radiometer. Integration of data sets enables synergistic assessment of geology and distribution of units across multiple spatial scales. Mineralogical assessment using hyperspectral data indicates spatial relationships with mineralogical signatures, e.g., central peaks of complex craters, consistent with inferred SPA basin structure and melt differentiation (Moriarty & Pieters, 2015, JGR-P 118). Delineation of mare, cryptomare, and nonmare surfaces is key to interpreting compositional mixing in the formation of SPA regolith to interpret remotely sensed data, and for scientific assessment of landing sites. LROC Narrow Angle Camera (NAC) images show the location and distribution of >0.5 m boulders and fresh craters that constitute the main threats to automated landers and thus provide critical information for landing site assessment and planning. NAC images suitable for geometric stereo derivation and digital terrain models so derived, controlled with Lunar Orbiter Laser Altimeter (LOLA) data, and oblique NAC images made with large slews of the spacecraft, are crucial to both scientific and landing-site assessments. These images, however, require favorable illumination and significant spacecraft resources. Thus they make up only a small percentage of all of the images taken. It is essential for future exploration to support LRO continued operation for these critical datasets.

Orbital revolution of a pair of bubbles in an acoustic field

NASA Astrophysics Data System (ADS)

Shirota, Minori; Yamashita, Kou; Inamura, Takao

2011-11-01

This experimental study aims to clarify the mechanism of orbital motion of two oscillating bubbles in an acoustic field. Trajectory of the orbital motion was observed using a high-speed video camera. Because of a good repeatability in volume oscillation of bubbles, we were also able to observe the radial motion driven at 24 kHz by stroboscopic like imaging; the cyclic bubble oscillation was appeared to slow down by capturing images at the framing rate close to the forcing frequency. The orbital motions of bubbles raging from 0.13 to 0.18 mm were examined with different forcing amplitude and in different viscous oils. As a result, we found that pairs of bubbles revolve along a circular orbit around the center of mass of the orbiting two bubbles. We also found that the two bubbles perform anti-phase radial oscillation. Although this radial oscillation should result in a repulsive secondary Bjerknes force, the bubbles kept a constant separate distance of about 1 mm, which indicates the existence of centripetal primary Bjerknes force. The angular velocity of orbital revolution increases linearly with the increase in Bjerknes force.

The PanCam Instrument for the ExoMars Rover

PubMed Central

Coates, A.J.; Jaumann, R.; Griffiths, A.D.; Leff, C.E.; Schmitz, N.; Josset, J.-L.; Paar, G.; Gunn, M.; Hauber, E.; Cousins, C.R.; Cross, R.E.; Grindrod, P.; Bridges, J.C.; Balme, M.; Gupta, S.; Crawford, I.A.; Irwin, P.; Stabbins, R.; Tirsch, D.; Vago, J.L.; Theodorou, T.; Caballo-Perucha, M.; Osinski, G.R.

2017-01-01

Abstract The scientific objectives of the ExoMars rover are designed to answer several key questions in the search for life on Mars. In particular, the unique subsurface drill will address some of these, such as the possible existence and stability of subsurface organics. PanCam will establish the surface geological and morphological context for the mission, working in collaboration with other context instruments. Here, we describe the PanCam scientific objectives in geology, atmospheric science, and 3-D vision. We discuss the design of PanCam, which includes a stereo pair of Wide Angle Cameras (WACs), each of which has an 11-position filter wheel and a High Resolution Camera (HRC) for high-resolution investigations of rock texture at a distance. The cameras and electronics are housed in an optical bench that provides the mechanical interface to the rover mast and a planetary protection barrier. The electronic interface is via the PanCam Interface Unit (PIU), and power conditioning is via a DC-DC converter. PanCam also includes a calibration target mounted on the rover deck for radiometric calibration, fiducial markers for geometric calibration, and a rover inspection mirror. Key Words: Mars—ExoMars—Instrumentation—Geology—Atmosphere—Exobiology—Context. Astrobiology 17, 511–541.

Combining color and shape information for illumination-viewpoint invariant object recognition.

PubMed

Diplaros, Aristeidis; Gevers, Theo; Patras, Ioannis

2006-01-01

In this paper, we propose a new scheme that merges color- and shape-invariant information for object recognition. To obtain robustness against photometric changes, color-invariant derivatives are computed first. Color invariance is an important aspect of any object recognition scheme, as color changes considerably with the variation in illumination, object pose, and camera viewpoint. These color invariant derivatives are then used to obtain similarity invariant shape descriptors. Shape invariance is equally important as, under a change in camera viewpoint and object pose, the shape of a rigid object undergoes a perspective projection on the image plane. Then, the color and shape invariants are combined in a multidimensional color-shape context which is subsequently used as an index. As the indexing scheme makes use of a color-shape invariant context, it provides a high-discriminative information cue robust against varying imaging conditions. The matching function of the color-shape context allows for fast recognition, even in the presence of object occlusion and cluttering. From the experimental results, it is shown that the method recognizes rigid objects with high accuracy in 3-D complex scenes and is robust against changing illumination, camera viewpoint, object pose, and noise.

'Berries' Here, There, Everywhere

NASA Technical Reports Server (NTRS)

2004-01-01

This approximate true-color image suggests that the plains beyond the small crater where the Mars Exploration Rover Opportunity now sits are littered with the same dark grey material found inside the crater in the form of spherules or 'blueberries.' Because Mars orbiters have observed the iron-bearing mineral hematite across these plains, scientists hypothesize that the blueberries are also made up of this mineral. This image was taken by the rover's panoramic camera on the 17th martian day, or sol, of its mission. Data from the camera's red, green and blue filters were combined to create this image.

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.

View of Astronaut Owen Garriott taking video of two Skylab spiders experiment

NASA Technical Reports Server (NTRS)

1973-01-01

View of Scientist-Astronaut Owen K. Garriott, Skylab 3 science pilot, taking TV footage of Arabella and Anita, the two Skylab 3 common cross spiders 'aranous diadematus,' aboard the Skylab space station cluster in Earth orbit. During the 59 day Skylab 3 mission the two spiders Arabella and Anita, were housed in an enclosure onto which a motion picture and still camera were attached to record the spiders' attempts to build a web in the weightless environment. Note the automatic data acquisition camera (DAC) about 3.5 feet to Garriott's right (about waist level).

Micrometeoroid Impacts on the Hubble Space Telescope Wide Field and Planetary Camera 2: Larger Particles

NASA Technical Reports Server (NTRS)

Kearsley, A. T.; Grime, G. W.; Webb, R. P.; Jeynes, C.; Palitsin, V.; Colaux, J. L.; Ross, D. K.; Anz-Meador, P.; Liou, J. C.; Opiela, J.;

Mapping Sequence performed during the STS-117 R-Bar Pitch Maneuver

NASA Image and Video Library

2007-06-10

ISS015-E-11320 (10 June 2007) --- This is one of a series of images, photographed with a digital still camera using an 800mm focal length, featuring the different areas of the Space Shuttle Atlantis as it approached the International Space Station and performed a back-flip to accommodate close scrutiny by eyeballs and cameras. This image shows part of Atlantis' cabin and its docking system, which a short time later was involved in linking up with the orbital outpost. Distance from the station and shuttle at this time was approximately 600 feet.

Astronaut John Young in shadow of Lunar Module behind ultraviolet camera

NASA Image and Video Library

1972-04-22

AS16-114-18439 (22 April 1972) --- Astronaut Charles M. Duke Jr., lunar module pilot, stands in the shadow of the Lunar Module (LM) behind the ultraviolet (UV) camera which is in operation. This photograph was taken by astronaut John W. Young, commander, during the mission's second extravehicular activity (EVA). The UV camera's gold surface is designed to maintain the correct temperature. The astronauts set the prescribed angles of azimuth and elevation (here 14 degrees for photography of the large Magellanic Cloud) and pointed the camera. Over 180 photographs and spectra in far-ultraviolet light were obtained showing clouds of hydrogen and other gases and several thousand stars. The United States flag and Lunar Roving Vehicle (LRV) are in the left background. While astronauts Young and Duke descended in the Apollo 16 Lunar Module (LM) "Orion" to explore the Descartes highlands landing site on the moon, astronaut Thomas K. Mattingly II, command module pilot, remained with the Command and Service Modules (CSM) "Casper" in lunar orbit.

Astronaut Charles M. Duke, Jr., in shadow of Lunar Module behind ultraviolet camera

NASA Technical Reports Server (NTRS)

1972-01-01

Astronaut Charles M. Duke, Jr., lunar module pilot, stands in the shadow of the Lunar Module (LM) behind the ultraviolet (UV) camera which is in operation. This photograph was taken by astronaut John W. Young, mission commander, during the mission's second extravehicular activity (EVA-2). The UV camera's gold surface is designed to maintain the correct temperature. The astronauts set the prescribed angles of azimuth and elevation (here 14 degrees for photography of the large Magellanic Cloud) and pointed the camera. Over 180 photographs and spectra in far-ultraviolet light were obtained showing clouds of hydrogen and other gases and several thousand stars. The United States flag and Lunar Roving Vehicle (LRV) are in the left background. While astronauts Young and Duke descended in the Apollo 16 Lunar Module (lm) 'Orion' to explore the Descartes highlands landing site on the Moon, astronaut Thomas K. Mattingly II, command module pilot, remained with the Command and Service Modules (csm) 'Casper' in lunar orbit.

MS Lucid and Blaha with MGBX aboard the Mir space station Priroda module

NASA Image and Video Library

1997-03-26

STS079-S-092 (16-26 Sept. 1996) --- Astronauts Shannon W. Lucid and John E. Blaha work at a microgravity glove box on the Priroda Module aboard Russia's Mir Space Station complex. Blaha, who flew into Earth-orbit with the STS-79 crew, and Lucid are the first participants in a series of ongoing exchanges of NASA astronauts serving time as cosmonaut guest researchers onboard Mir. Lucid went on to spend a total of 188 days in space before returning to Earth with the STS-79 crew. During the STS-79 mission, the crew used an IMAX camera to document activities aboard the Space Shuttle Atlantis and the various Mir modules, with the cooperation of the Russian Space Agency (RSA). A hand-held version of the 65mm camera system accompanied the STS-79 crew into space in Atlantis' crew cabin. NASA has flown IMAX camera systems on many Shuttle missions, including a special cargo bay camera's coverage of other recent Shuttle-Mir rendezvous and/or docking missions.

Runco and Thomas show off trays of food on the middeck

NASA Image and Video Library

1996-05-26

S77-E-5120 (26 May 1996) --- Astronauts Mario Runco, Jr. and Andrew S. W. Thomas, both mission specialists, pose for photo while in the middeck of the Earth-orbiting Space Shuttle Endeavour. The scene was recorded with an Electronic Still Camera (ESC).

KSC-PL62-76872

NASA Image and Video Library

1962-02-23

CAPE CANAVERAL, Fla. -- President John F. Kennedy honors John H. Glenn Jr. during welcome back ceremonies at Patrick Air Force Base and Cape Canaveral in Florida after his historic three-orbit mission aboard Friendship 7. Vice President Lyndon B. Johnson looks on, with his back to the camera. Photo credit: NASA

Brightness Rhythm of Mars Flyby Comet Is Clue to Rotation Rate

NASA Image and Video Library

2014-11-07

This graph shows changes in apparent brightness of comet C/2013 A1 Siding Spring as it approached and receded from Mars, as seen by the HiRISE camera on NASA Mars Reconnaissance Orbiter. The pattern suggests the comet rotates once every eight hours.

MS Dunbar exercises on an ergometer

NASA Image and Video Library

1998-03-03

S89-E-5202 (25 Jan 1998) --- This Electronic Still Camera (ESC) image shows mission specialist, Bonnie J. Dunbar, payload commander, working out on the bicycle ergometer onboard the Earth-orbiting Space Shuttle Endeavour. This ESC view was taken on January 25, 1998, at 18:36:52 GMT.

Cloud formation over Western Atlantic Ocean north of South America

NASA Image and Video Library

1962-10-03

S62-06606 (3 Oct. 1962) --- Cloud formation over Western Atlantic Ocean north of South America taken during the fourth orbit pass of the Mercury-Atlas 8 (MA-8) mission by astronaut Walter M. Schirra Jr. with a hand-held camera. Photo credit: NASA

Controlled photomosaic map of Europa Je 15 M CMN

USGS Publications Warehouse

,

2002-01-01

This sheet is one in a series of maps of the Galilean satellites of Jupiter at a nominal scale of 1:15,000,000. This series is based on data from the Galileo Orbiter Solid-State Imaging (SSI) camera and the Voyager 1 and 2 spacecraft.

Convolutional Neural Network-Based Shadow Detection in Images Using Visible Light Camera Sensor.

PubMed

Kim, Dong Seop; Arsalan, Muhammad; Park, Kang Ryoung

2018-03-23

Recent developments in intelligence surveillance camera systems have enabled more research on the detection, tracking, and recognition of humans. Such systems typically use visible light cameras and images, in which shadows make it difficult to detect and recognize the exact human area. Near-infrared (NIR) light cameras and thermal cameras are used to mitigate this problem. However, such instruments require a separate NIR illuminator, or are prohibitively expensive. Existing research on shadow detection in images captured by visible light cameras have utilized object and shadow color features for detection. Unfortunately, various environmental factors such as illumination change and brightness of background cause detection to be a difficult task. To overcome this problem, we propose a convolutional neural network-based shadow detection method. Experimental results with a database built from various outdoor surveillance camera environments, and from the context-aware vision using image-based active recognition (CAVIAR) open database, show that our method outperforms previous works.

Convolutional Neural Network-Based Shadow Detection in Images Using Visible Light Camera Sensor

PubMed Central

Kim, Dong Seop; Arsalan, Muhammad; Park, Kang Ryoung

2018-01-01

Recent developments in intelligence surveillance camera systems have enabled more research on the detection, tracking, and recognition of humans. Such systems typically use visible light cameras and images, in which shadows make it difficult to detect and recognize the exact human area. Near-infrared (NIR) light cameras and thermal cameras are used to mitigate this problem. However, such instruments require a separate NIR illuminator, or are prohibitively expensive. Existing research on shadow detection in images captured by visible light cameras have utilized object and shadow color features for detection. Unfortunately, various environmental factors such as illumination change and brightness of background cause detection to be a difficult task. To overcome this problem, we propose a convolutional neural network-based shadow detection method. Experimental results with a database built from various outdoor surveillance camera environments, and from the context-aware vision using image-based active recognition (CAVIAR) open database, show that our method outperforms previous works. PMID:29570690

Calibration Image of Earth by Mars Color Imager

NASA Technical Reports Server (NTRS)

2005-01-01

Three days after the Mars Reconnaissance Orbiter's Aug. 12, 2005, launch, the NASA spacecraft was pointed toward Earth and the Mars Color Imager camera was powered up to acquire a suite of color and ultraviolet images of Earth and the Moon. When it gets to Mars, the Mars Color Imager's main objective will be to obtain daily global color and ultraviolet images of the planet to observe martian meteorology by documenting the occurrence of dust storms, clouds, and ozone. This camera will also observe how the martian surface changes over time, including changes in frost patterns and surface brightness caused by dust storms and dust devils.

The purpose of acquiring an image of Earth and the Moon just three days after launch was to help the Mars Color Imager science team obtain a measure, in space, of the instrument's sensitivity, as well as to check that no contamination occurred on the camera during launch. Prior to launch, the team determined that, three days out from Earth, the planet would only be about 4.77 pixels across, and the Moon would be less than one pixel in size, as seen from the Mars Color Imager's wide-angle perspective. If the team waited any longer than three days to test the camera's performance in space, Earth would be too small to obtain meaningful results.

The images were acquired by turning Mars Reconnaissance Orbiter toward Earth, then slewing the spacecraft so that the Earth and Moon would pass before each of the five color and two ultraviolet filters of the Mars Color Imager. The distance to Earth was about 1,170,000 kilometers (about 727,000 miles).

This image shows a color composite view of Mars Color Imager's image of Earth. As expected, it covers only five pixels. This color view has been enlarged five times. The Sun was illuminating our planet from the left, thus only one quarter of Earth is seen from this perspective. North America was in daylight and facing toward the camera at the time the picture was taken; the data from the camera were being transmitted in real time to the Deep Space Network antennas in Goldstone, California.

jsc2003e15407

NASA Image and Video Library

2000-01-09

JSC2003-E-15407 (9 Jan. 1990) --- A 35mm still camera located in the umbilical well of the Space Shuttle Columbia took this photograph of the external fuel tank (ET) after it was dropped from the launch stack as the shuttle headed for Earth-orbit on Jan. 9, 1990 for the STS-32 mission. Several large divots are visible near the forward ET/orbiter bipod and smaller divots are visible on the H2 tank acreage. The vertical streak and the horizontal bands were the results of repairs done prior to launch.

Launch of space shuttle Challenger on the 41-C mission

NASA Image and Video Library

1984-04-06

41C-3029 (6 April 1984) --- The space shuttle Challenger and its five-member astronaut crew leave the launch pad at the Kennedy Space Center to begin a six-day stay in space. Astronaut John W. Young, a veteran of two shuttle missions and six spaceflights overall, recorded the image with a handheld 70mm camera from the shuttle training aircraft which he was using to monitor environmental conditions around Florida. This is the eighth mission on which Young photographed one of NASA's orbiter vehicles beginning its orbital stay. Photo credit: NASA

Surveying the earth from 20,000 miles

USGS Publications Warehouse

Colvocoresses, A.P.

1970-01-01

Current space programs aimed at monitoring the earth's resources concentrate on the lower orbital altitudes of 100 to 500 nautical miles. An earth synchronous (geo-stationary) orbit is 19,400 n. mi. above the earth. A powerful telephoto camera at such a location can monitor and record many time-variant phenomena far more effectively than instruments at lower altitudes. The geo-stationary systems characteristics and problem areas related to optics and telemetry are outlined and detailed, and on-going programs are discussed as they relate to the geo-stationary system.

Survey view of damage to the STS-117 OMS Pod taken by an Expedition 15 Crewmember

NASA Image and Video Library

2007-06-13

ISS015E11804 (13 June 2007) --- A digital still camera recorded this image of a gap caused by an uplifted area on the thermal blanket protecting Atlantis' portside orbital maneuvering system (OMS) pod. The STS-117 Mission Management Team (MMT) has decided the best course of action to take in regard to the uplifted thermal blanket on the post side Orbital Maneuvering System Pod was to add the repair task on EVA 3 with astronauts Jim Reilly and John (Danny) Olivas.

GEMINI-TITAN (GT)-3 - EARTH- SKY VIEW

NASA Image and Video Library

1965-03-23

S65-18740 (23 March 1965) --- Astronaut John W. Young took this picture during the second orbit of the Gemini-Titan 3 three-orbit mission as the spacecraft "Molly Brown" passed over Northern Mexico at an altitude of 90 miles. The light-brown circular area at the lower right is the Sonoran Desert. The lower portion of the picture is Mexico, and the upper part is California. Young used a hand-held modified 70mm Hasselblad camera with color film. The lens setting was 250th of a second at f/11.

KSC-04PD-0805

NASA Technical Reports Server (NTRS)

2004-01-01

KENNEDY SPACE CENTER, FLA. -- On a tour of the Orbiter Processing Facility, Florida Gov. Jeb Bush (back to camera in white shirt) learns about work being done on the orbiter Endeavour (background). Accompanying him is U.S. Mint Director Henrietta Holsman Fore (at right of Bush). The tour followed the launching ceremony at the KSC Visitor Complex for the new Florida quarter issued by the U.S. Mint. The ceremony was emceed by Center Director Jim Kennedy and included remarks by NASA Administrator Sean OKeefe, Bush, Fore and Deputy Secretary of the Treasury Samuel W. Bodman.

KSC-04pd0805

NASA Image and Video Library

2004-04-07

KENNEDY SPACE CENTER, FLA. -- On a tour of the Orbiter Processing Facility, Florida Gov. Jeb Bush (back to camera in white shirt) learns about work being done on the orbiter Endeavour (background). Accompanying him is U.S. Mint Director Henrietta Holsman Fore (at right of Bush). The tour followed the launching ceremony at the KSC Visitor Complex for the new Florida quarter issued by the U.S. Mint. The ceremony was emceed by Center Director Jim Kennedy and included remarks by NASA Administrator Sean O’Keefe, Bush, Fore and Deputy Secretary of the Treasury Samuel W. Bodman.

Astronaut Jack Lousma seen outside Skylab space station during EVA

NASA Image and Video Library

1973-08-06

S73-31976 (5 Aug. 1973) --- Astronaut Jack R. Lousma, Skylab 3 pilot, is seen outside the Skylab space station in Earth orbit during the Aug. 5, 1973 Skylab 3 extravehicular activity (EVA) in this photographic reproduction taken from a television transmission made by a color TV camera aboard the space station. Scientist-astronaut Owen K. Garriott, Skylab 3 science pilot, participated in the EVA with Lousma. During the EVA the two crewmen deployed the twin pole solar shield to help shade the Orbital Workshop. Photo credit: NASA

STS-48 Pilot Reightler on OV-103's aft flight deck poses for ESC photo

NASA Technical Reports Server (NTRS)

1991-01-01

STS-48 Pilot Kenneth S. Reightler, Jr, positioned under overhead window W8, poses for an electronic still camera (ESC) photo on the aft flight deck of the earth-orbiting Discovery, Orbiter Vehicle (OV) 103. Crewmembers were testing the ESC as part of Development Test Objective (DTO) 648, Electronic Still Photography. The digital image was stored on a removable hard disk or small optical disk, and could be converted to a format suitable for downlink transmission. The ESC is making its initial appearance on this Space Shuttle mission.

Astronaut Alan Bean flies the Astronaut Maneuvering Equipment in the OWS

NASA Technical Reports Server (NTRS)

1973-01-01

Astronaut Alan L. Bean, Skylab 3 commander, flies the M509 Astronaut Maneuvering Equipment, as seen in this photographic reproduction taken from a television transmission made by a color television camera in the Orbital Workshop (OWS) of the Skylab space station in Earth orbit. Bean is strapped into the back-mounted, hand-controlled Automatically stabilized Maneuvering Unit (ASMU). The M509 exercise was in the forward dome area of the OWS. THe dome area is about 22 feet in diameter and 19 feet form top to bottom.

IPL Processing of the Viking Orbiter Images of Mars

NASA Technical Reports Server (NTRS)

Ruiz, R. M.; Elliott, D. A.; Yagi, G. M.; Pomphrey, R. B.; Power, M. A.; Farrell, W., Jr.; Lorre, J. J.; Benton, W. D.; Dewar, R. E.; Cullen, L. E.

1977-01-01

The Viking orbiter cameras returned over 9000 images of Mars during the 6-month nominal mission. Digital image processing was required to produce products suitable for quantitative and qualitative scientific interpretation. Processing included the production of surface elevation data using computer stereophotogrammetric techniques, crater classification based on geomorphological characteristics, and the generation of color products using multiple black-and-white images recorded through spectral filters. The Image Processing Laboratory of the Jet Propulsion Laboratory was responsible for the design, development, and application of the software required to produce these 'second-order' products.

Coprates Chasma

NASA Technical Reports Server (NTRS)

1998-01-01

Mars Orbiter Camera (MOC) image of a 10 km by 12 km area of Coprates Chasma (14.7 degrees S, 55.8 degrees W), a ridge with a flat upper surface in the center of Coprates Chasma, which is part of the 6000-km-long Valles Marineris. Rock layers are visible just below the ridge. The gray scale (4.8 m/pixel) MOC image was combined with a Viking Orbiter color view of the same area. The faults of a graben offset beds on the slope to the left.

Figure caption from Science Magazine

Candid views of the STS-81 and Mir 22 crews on the orbiter's middeck

NASA Image and Video Library

1997-01-16

STS081-E-05498 (16 Jan. 1997) --- Supplies and equipment transfer are the topic of the day, as the Space Shuttle Atlantis and Russia's Mir Space Station respective commanders have a discussion aboard the Orbiter. Left to right are cosmonauts Valeri G. Korzun and Aleksandr Y. Kaleri, Mir-22 commander and flight engineer respectively; along with astronaut Michael A. Baker, mission commander. The photograph was recorded with an Electronic Still Camera (ESC) and later was downlinked to flight controllers in Houston, Texas.

Forward end (+XA side) of the PMA-2 prior to mating to the Orbiter Docking System (ODS).

NASA Image and Video Library

1998-12-05

STS088-335-017 (5 Dec. 1998) --- One of the STS-88 astronauts aimed a 35mm camera through Endeavour's aft flight deck windows to record this Dec. 5 image of the Unity connecting module as it was being unberthed in the cargo bay. The berthing and mating process constituted the first link in a long chain of events that led up to the eventual deployment in Earth orbit of the connected Unity and Zarya modules later in the 11-day mission. Photo credit: NASA

KSC-04PD-1680

NASA Technical Reports Server (NTRS)

2004-01-01

KENNEDY SPACE CENTER, FLA. In the Orbiter Processing Facility, workers help guide the nose cap (right) toward the orbiter Atlantis for installation. The nose cap was removed from the vehicle in May and sent back to the vendor for thorough Non- Destructive Engineering evaluation and recoating. Thermography was also performed to check for internal flaws. This procedure uses high intensity light to heat areas that are immediately scanned with an infrared camera. White Thermal Protection System blankets were reinstalled on the nose cap before installation. Processing continues on Atlantis for its future mission to the International Space Station.

KSC-04PD-1681

NASA Technical Reports Server (NTRS)

2004-01-01

KENNEDY SPACE CENTER, FLA. In the Orbiter Processing Facility, workers help install the nose cap (right) onto the orbiter Atlantis. The nose cap was removed from the vehicle in May and sent back to the vendor for thorough Non-Destructive Engineering evaluation and recoating. Thermography was also performed to check for internal flaws. This procedure uses high intensity light to heat areas that are immediately scanned with an infrared camera. White Thermal Protection System blankets were reinstalled on the nose cap before installation. Processing continues on Atlantis for its future mission to the International Space Station.

Skylab beverage container filled with orange juice held by Astronaut Conrad

NASA Technical Reports Server (NTRS)

1973-01-01

An accordian-style beverage dispenser filled with orange juice is held by Astronaut Charles Conrad Jr., Skylab 2 commander, in this close-up view which is a reproduction taken from a color television transmission made by a TV camera aboard the Skylab 1 and 2 space station cluster in Earth orbit. Conrad (head and face not in view) is seated at the wardroom table in the crew quarters of the Orbital Workshop. The dispenser contained beverage crystals, and Conrad has just added the prescribed amount of water to make the orange drink.

Solar Conjunction Ends: Nirgal Vallis

NASA Technical Reports Server (NTRS)

2004-01-01

28 September 2004 For the past several weeks, Mars was on the other side of the Sun relative to Earth. During this period, known as solar conjunction, radio communication with spacecraft orbiting and roving on Mars was limited. As is always done during solar conjunction, on 7 September 2004, the Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) was turned off. On Saturday, 25 September 2004, the MOC team gathered at Malin Space Science Systems to command the instrument to turn back on again. After a successful turn-on, MOC acquired its first narrow angle camera image, shown here, on orbit 24808 (24,808th orbit since the start of the Mapping phase of the MGS mission in March 1999).

The 25 September image shows a portion of Nirgal Vallis, an ancient valley system in the Mare Erythraeum region of Mars. The valley floor is covered by large, ripple-like bedforms created by wind. This early southern winter image is located near 27.4oS, 42.9oW, and covers an area approximately 3 km (1.9 mi) across. Sunlight illuminates the scene from the upper left.

This was the 4th solar conjunction period that MGS and MOC have been through since the spacecraft reached the red planet in September 1997. The four solar conjunction periods, where MOC was turned off, were:

First solar conjunction: 29 April - 1 June 1998 Second solar conjunction: 22 June - 12 July 2000 Third solar conjunction: 1 August - 18 August 2002 Fourth solar conjunction: 7 September - 25 September 2004.

In late October, MGS MOC will mark the start of its fourth Mars year since the beginning of the Mapping Phase of the mission in March 1999. MGS and MOC have already been orbiting Mars for more than 4 Mars years, including the pre-Mapping aerobrake and science phasing orbit insertion periods.