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As part of a NASA-funded study of diurnal thermal imaging at a Mars analog site, we conducted simultaneous oblique thermal imaging and in situ temperature measurements within two regions of interest on the Pisgah lava field, near Ludlow, California. Both regions of interest contained either cave or cave-like alcoves. Data released in this report was collected from 03/23/2010 to 03/25/2010. The experiment was conducted at Pisgah lava field, which is located about 175 miles northeast of Los Angeles on Bureau of Land Management lands. Consisting of Quaternary basaltic lava and a cinder cone superimposed on alluvial deposits and lacustrine sediments of Lavic Lake playa (Dibblee, 1966), the flow is approximately 21,000...
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From 2008 to 2012, the U.S. Geological Survey, in cooperation with the U.S. Army Corps of Engineers, Walla Walla District, developed an acoustic backscatter surrogate (model 1.0) for estimating real-time suspended-sediment concentration and loads at Clearwater River at Spalding, ID (USGS ID: 13342500) using a horizontally-mounted 3000kHz acoustic Doppler velocity meter (ADVM). This study is a continuation of the 2008 to 2012 acoustic backscatter surrogate study using samples collected since 2015 to validate the continued use of model 1.0. Sample data collected in 2015 to 2018 show a deviation from model 1.0 when backscatter data from the ADVM, after correction for acoustic losses, is greater than 65.7 decibels....
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CSV files containing measurements of ventifact feature and wind tail orientations, sand flux and wind modeling results.
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Almost all the pictures acquired by Mariner 10 that were used for mapping were obtained during the first encounter: those covering the southeast half of the quadrangle are incoming close-encounter images, and those covering the north-west corner are outoing close-encounter images. At the time the pictures were obtained, the terminator was at about long 7° to 8°, within the eastern part of the quadrangle. A large gap in coverage between in the incoming and outgoing images appears as a northeast-trending diagonal blank strip on the base map. A small part of this gap was filled in the southwestern part of the quadrangle by very poor second-encounter images.
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LiDAR scans were taken using a tripod mounted Riegl VZ-400 scanning LiDAR. The tripod was set up such that the scanner was between 1.5 and 2.5 m tall. The VZ-400 is a near infrared (1550 nm) scanner. Geometric control was achieved using a pair of Trimble RB GPS antennae, one mounted on the LiDAR scanner (rover) and the other setup as a base station. Before taking a LiDAR scan, the VZ-400 would use the GPSs to fix a real time kinematic (RTK) solution for the scanner’s location and then use that position (scan position) as a reference for LiDAR returns. Post processing was done using RIScan-Pro version 2 (scanner specific software). Also, in post-processing, overlapping areas of point clouds were merged and inaccuracies...
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The U.S. Geological Survey provides a wide range of scientific information to an even wider group of stakeholders. Understanding what capacities are needed and if and or where these capacities exist across the USGS landscape is critical in moving science to the next level of use, implementation, and visualization. The concept behind the groups organized to conduct and interpret the survey that collected these data took advantage of the USGS’s position as a science organization with expertise spanning a wide range of science disciplines, stakeholders, and responsibilities. A survey was conducted of USGS employees (Sep 20-Nov 20) to get a current sample of the capacities that exist across the USGS.
A point layer of sites known to be useful analogs for planetary science, such as impact craters, dunes, volcanoes, and other processes observed on bodies across the solar system.
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A polygon layer of regions of multiple planetary bodies beyond Earth that are covered by proposed or published planetary geologic maps published by the USGS.
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As part of a NASA-funded study of sediment flux rates at a Mars analog site, we installed a suite of instruments in a small dune field near Grand Falls, Arizona. Data released in this report were collected from 10/28/2013 to 11/04/2016. The Grand Falls (GF) dune field is located on the Navajo Nation. It lies ~70 km NE of Flagstaff, AZ, 2 km east of Grand Falls, and just north of the Little Colorado River (LCR). The dune field consists of barchans, smaller dunes, ripples, and bare, indurated interdune surfaces; all features commonly found on the Martian surface. We measured sediment flux using a Sensit saltation sensor and a set of three Big Spring Number Eight (BSNE) passive sediment samplers, at 20, 50, and 100...
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Grand Falls dune field (GFDF) is located on the Navajo Nation, ~70 km NE of Flagstaff, AZ. This active dune field displays a range of morphologies, including barchans, smaller dunes, and ripples, and is bimodal in composition. The felsic component is likely derived from the Little Colorado River, and the mafic component (basaltic grains) is locally sourced from nearby cinder cones [1]. GFDF is an excellent analog site for both active dunes on Mars and other planetary bodies that have dune-like features (e.g., Venus and Titan). We have set up a meteorological station within the dune field that records temperature, barometric pressure, relative humidity, wind direction, wind speed, solar radiation, and precipitation...
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The Mars Global Digital Dune Database provides a comprehensive and quantitative view of the geographic distribution of dune fields from 65° N to 65° S latitude. The database encompasses ~ 550 dune fields, covering ~ 70,000 km2, with an estimated total volume between 3,600 km3 and 13,400 km3. Over 2300 selected Thermal Emission Imaging System (THEMIS) infrared (IR), THEMIS visible (VIS) and Mars Orbiter Camera Narrow Angle (MOC NA) images were used to build the database and are included in the ArcMap and ArcReader versions of the database. An initial data set of THEMIS band 9 spectral range images covering orbits 816-9601 (spanning 02/2002 - 02/2004 and Ls = 0.085º-358.531º) and comprising more than 30,000 images...
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Dataset contains latitude, longitude and additional attribute information for mounds in the lowlands of Mars. This version of the database contains data for mounds in the southwestern Utopia Planitia region of the martian lowlands.
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Basic information about the planetary surface of the Kuiper quadrangle is provided by three sequences of high-quality photographs designated Mercury I, II, and II, obtained during the incoming phases of three encounters of the Mariner 10 spacecraft with Mercury. Mercury I includes 75 whole-frame photographs of the Kuiper quadrangle; Mercury II, 13 whole-frame photographs; and Mercury III, 70 quarter-frame photographs. The photographs include 19 stereopairs in the southern part of the quadrangle. The most distant of the photographs was taken at an altitude of 89,879 km, the closest at an altitude of 7,546 km. Resolution, therefore, varies widely but ranges from about 1.5 to 2.0 km over most of the area.
Data for Journal article: Relationship between explosive and effusive volcanism in the Montes Apenninus region of the Moon in JGR: Planets
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Mariner 10 photographic coverage was available for only the eastern two-thirds of the Tolstoj quadrangle. Image data from three Mariner 10 encounters with Mercury were used in mapping the quadrangle.
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Although ice in the Martian mid-latitudes is typically covered by a layer of dust or regolith, it is exposed in some locations by fresh impact craters or in erosional scarps. In both cases, the exposed ice is massive or excess ice with a low lithic content. We find that erosional scarps occur between 50–61 north and south latitude, and that they are concentrated in and near Milankovič crater in the northern hemisphere and southeast of the Hellas basin in the southern hemisphere. These may represent locations of particularly thick or clean bodies of ice. Pits created by retreat of the scarps represent sublimation-thermokarst landforms that evolve in a manner distinct from other ice-loss landforms on Mars. New impact...
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The Beethoven quadrangle is located in the equatorial region of Mercury, in the center of the imaged area. Most pictures of the quadrangle were obtained at high sun angles as the Mariner 10 spacecraft receded from the planet. Images in the northeastern part of the quadrangle are very poor to unusable. Another difficulty in mapping is the poor match in topographic bases between Beethvoen and adjacent quadrangles. Mismatches are especially common along the borders withthe Kuiper and Discovery quadrangles to the east and southeast.
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This map sheet is one of a series covering that part of the surface of Mercury that was illuminated during the Mariner 10 encounters. Planimetric control is provided by photogrammetric triangulation using Mariner 10 pictures (Davies and Batson, 1975). Discrepancies between images in the base mosaic and computed control-point positions appear to be less than 5 km. No attempt was made to resolve discrepancies in feature positions on this sheet and those on the Kuiper (H-6) quadrangle to the north and the Bach (H-15) quadrangle to the south. The latter sheets were controlled by an earlier, more preliminary net.
map background search result map search result map Geologic Map fo the Beethoven Quadrangle of Mercury Geologic Map of the Discovery Quadrangle of Mercury Geologic Map of the Kuiper Quadrangle of Mercury Geologic Map of the Victoria Quadrangle of Mercury Model Archive Summary for Suspended Sediment, Acoustic Sediment Surrogate Model 2.0, USGS gage number 13342500, Clearwater River at Spalding, Idaho Grand Falls, Arizona: Dune Field Sand Transport 2013 - 2016 Known Terrestrial Analog Sites for Planetary Science Oblique Thermal Imaging of the Pisgah Lava Field, California Acquired March 2010 Oblique Thermal Imaging of the Pisgah Lava Field, California Acquired March 2010 - Field B Oblique Thermal Imaging of the Pisgah Lava Field, California Acquired March 2010 - Station 7 USGS Earthmap Capacity Assessment Dataset NASA GIFT Iceland Highlands: 2015-2019 Baugur LiDAR USGS Database of Mounds in Southwest Utopia Planitia Mars Imagery, photogrammetry, and meteorological data from December 2021 to December 2022, Grand Falls Dune Field, Arizona Imagery, photogrammetry, and meteorological data from December 2021 to December 2022, Grand Falls Dune Field, Arizona Grand Falls, Arizona: Dune Field Sand Transport 2013 - 2016 Oblique Thermal Imaging of the Pisgah Lava Field, California Acquired March 2010 Oblique Thermal Imaging of the Pisgah Lava Field, California Acquired March 2010 - Field B Oblique Thermal Imaging of the Pisgah Lava Field, California Acquired March 2010 - Station 7 Model Archive Summary for Suspended Sediment, Acoustic Sediment Surrogate Model 2.0, USGS gage number 13342500, Clearwater River at Spalding, Idaho NASA GIFT Iceland Highlands: 2015-2019 Baugur LiDAR USGS Database of Mounds in Southwest Utopia Planitia Mars Geologic Map of the Kuiper Quadrangle of Mercury Geologic Map of the Discovery Quadrangle of Mercury Geologic Map of the Victoria Quadrangle of Mercury Geologic Map fo the Beethoven Quadrangle of Mercury USGS Earthmap Capacity Assessment Dataset Known Terrestrial Analog Sites for Planetary Science