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In parts, the rover was tracked through VLBI observations, which enabled path reconstruction (Salzberg, 1973). For this, we determined lateral offset values (in image line and sample) in the overlapping orthoimages, which were then manually corrected for. The astronauts' traverse path and stations (extracted from the historic traverse map) within Taurus‐Littrow Valley were superimposed onto an LROC NAC orthomosaic (M104318871L/R) for approximate positioning purposes.

It is a young impact crater, 106 m in diameter, and was chosen in order to study more recent cratering events. In contrast to utilizing fully assembled 360° panoramas, as reported in Haase et al. (, Controlled orthomap of Traverse Station 4. After a 13‐min drive they arrived at Station 1 (Apollo 17 Mission Evaluation Team, 1973). The PanCam Instrument for the ExoMars Rover. EPs and the geophones constitute the Apollo 17 Geophysical Station (Kovach et al., 1973). Additional pictures were taken to illustrate deployment of the ALSEP and for other operational purposes [Batson et al., 1981]. We used two different online sources to obtain astronaut imagery. They are listed in the order of layering, the first image being displayed in its full east‐west extent on the top and the image listed last being displayed on the bottom layer partially covered by overlying images.

We adopted this differentiation and only slightly corrected the course of the traverse at the sites, where the crew had deployed EPs from the rover.
Therefore, single frames were used to measure relative angles within that area. [7] The WAC instantaneous field‐of‐view (IFOV) is 5.15 arcmin for the VIS optics. Processes in Geophysics, Atmospheric

The position of the astronaut while recording the ‘Station 1 Pan’ (northwest of Steno Crater) is pinpointed by the origin of the least squares adjusted network of North azimuth angles (plotted on a 0.5 m/pxl LROC NAC orthoimage (M113758461R)). Additionally, prominent surface features such as large boulders, crater rims, and astronaut equipment, e.g. The underlying programming platform of the DLR stereo‐processing pipeline is the Video Image Communication and Retrieval (VICAR) Image Processing System (National Aeronautics and Space Administration, 2018). (a) To approximately level frame AS17‐133‐20296 horizontally it was rotated before measuring angular directions to reference features located within Victory Crater (horizontal directions are represented by white lines). Astrophysical Observatory. Using two metric Hasselblad cameras (see section 2.2), they recorded single frames, stereo pairs, and series of overlapping photographs to form panoramas. Armstrong became the first person to step onto the lunar surface six hours and 39 minutes later on July 21 at 02:56 UTC; Aldrin joined him 19 minutes later. He then moved northward and recorded a second panorama standing right in the middle of the ALSEP instrument suite near the C/S. One of the Apollo 17 surface cameras (S/N 1023), which was primarily used for color imagery taken by E. Cernan, was calibrated in preparation of the Apollo 16 mission (Malhotra, 1972). Both images were orthorectified using an adapted version of the DTM, which was horizontally shifted to reasonably match the image's projection geometry in order to minimize pixel displacement caused by faulty terrain.

Learn more. The DTM ranges from 30.425°E to 30.910°E in longitude and from 18.762°N to 21.143°N in latitude, including parts of the North, East, and South Massifs. The average speed driven by astronaut Cernan was 6 km/hr (average of all traverses, neglecting short stops).

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To apply a weighted least squares adjustment we assigned standard deviations to the angular measurements (±0.4°) and the orthoimage coordinates (±1 m).

Planets, Magnetospheric A minimum of four observed directions DCF set up an overdetermined, nonlinear equation system, which is solved after linearization using a first‐order Taylor series approximation. The crew gathered samples and performed photography at this site.

To facilitate the identification and positioning procedure, heights were represented by colors and contour lines to clearly display the local topography. Look for … See, Journal of Advances The frames are AS17‐140‐21483 to AS17‐140‐21509, and the standard deviation of the mean panorama position is ±0.5 m. Station 7 is located 490 m east of Station 6, on the lower slope of the North Massif just above the break in slope between the Massif and the valley floor (Figure 18). If you do not receive an email within 10 minutes, your email address may not be registered,

A typical LROC NAC stereo‐image set is acquired by two sensors (NAC‐L and NAC‐R) from two different orbits and thus consists of four images. The distances between the astronaut/camera and the craters range from 153 m (c7) to 429 m (c5).

Our results were integrated into a new LROC NAC-based Apollo 17 Traverse Map and also used to generate a series of large-scale maps of all nine traverse stations and of the ALSEP area. Landing Site Coordinates 0.67408° N latitude, 23.47297° E longitude Apollo 12 — Oceanus Procellarum Lunar Landing Time 01:54:35 a.m. EST, November 19, 1969 Landing Site Coordinates 3.01239° S latitude, 23.42157° W longitude . The area is located on a 13.6 degree slope (24.2%) and covered with boulders, which had rolled down from higher on the Massif. (a) Panorama sites and the Lunar Roving Vehicle (LRV) position were determined by angular network adjustments. A gift to the National Air and Space Museum is a gift to the nation, the world, and the future. Profile of the EVA 3 traverse path.

For each panorama site we resampled the original 0.5 m/pixel LROC NAC orthomosaic and map‐projected it to a local stereographic projection, defining the center at the approximate position of the astronaut during image acquisition. Geolocations of the Explosive Packages of the active seismic sounding experiment Lunar Seismic Profiling Experiment (LSPE). This allowed us to derive angles from the panorama. Isabel Haase, Marita Wählisch, Philipp Gläser, Jürgen Oberst, Mark Robinson, Research output: Contribution to journal › Article. During a 1‐month period in August 2011, the orbit of LRO was lowered to approach the lunar surface as close as 22 km. Recently, the Apollo 17 seismic data were closely reviewed by different geophysicists groups (Heffels et al., 2017; Sollberger et al., 2016). However, under favorable conditions, this proved to be a just as adequate method, provided that a crater's shape or extent is unambiguously discernable in the astronaut image. The frames are AS17‐147‐22569 to AS17‐147‐22588.

Boulder 1, for example, is laying right at the break of slope, and Boulder 2 rests about 6 m above the valley on the Massif's 14.9 degree slope (26.6%; see Figure 11). (or is it just me...), Smithsonian Privacy

These images not only provide unique close‐up views of the lunar surface but also allow making angular measurements, which can be used to derive positions, feature sizes, directions, and distances. We acknowledge the NASA LRO Missions Operations Team at Goddard Space Flight Center and thank the LROC Science Operations Team at Arizona State University for constant expert support and amicable collaboration.

Previously, we reported on our cartographic study of the Apollo 17 landing site, in which we derived astronaut and feature positions by analyzing Apollo surface panoramas in combination with LROC NAC orthoimages (Haase et al., 2012). We generated a controlled DTM of the Taurus‐Littrow Valley with a raster grid of 1.5 m and a controlled orthomosaic at 0.5 m/pixel scale. To further correct the DTMs for the vertical effects of errors in the exterior orientation, we determined mean offsets in elevation where adjacent DTMs overlap.

Until now, however, our knowledge of the coordinates of sampling sites and instrument locations relies on estimates from surface images and astronaut descriptions.
For example, a comparison of the coordinates of the Lunar Module (LM) derived from the traverse map to the ones given by Davies and Colvin [2000] reveals an error of 59 arcsec in latitude and 48 arcsec in longitude. Visually fitting the network of angles to the GLD100 model provided a first, 100‐m‐scale approximation for the location of traverse station 1 (see Figure 3). VLBI observations on radio transmission from the five ALSEPs, monitored between 1972 and 1974, resulted in relative coordinates with uncertainties of about 10 m horizontally and about 30 m vertically [King et al., 1976]. The vertical resolution is 0.1 m, and elevations are related to a sphere with a radius of 1737.4 km. [37] Standing between the Geophone Rock and the Geophone 3 instrument (part of the seismic sounding experiment), the first color panorama ‘Geo 3 Pan’ was taken at about 03:33 UTC (120:40 GET) consisting of frames AS17‐147‐22544 to ‐22562 [Wolfe et al., 1981]. [20] This study concentrates on full 360° Hasselblad panoramas, which were routinely recorded at each of the traverse stations and at the ALSEP area.

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