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USGS1999

The Universal Transverse Mercator (UTM) grid

The most convenient way to identify points on the curved surface of the Earth is with a system of reference lines called parallels of latitude and meridians of longitude. On some maps, the meridians and parallels appear as straight lines. On most modern maps, however, the meridians and parallels appear as curved lines. These differences sre due to the mathematical treatment required to portray a curved surface on a flat surface so that important properties of the map (such as distance and areal accuracy) are shown with minimum distortion. The system used to portray a portion of the round Earth on a flat surface is called a map projection.

Fact Sheet↗

USGS2005

Technical review of the status of Northern Goshawks in the western United States

The U.S. Fish and Wildlife Service (FWS) was petitioned in 1997 to consider listing Northern Goshawks (Accipiter gentilis atricapillus) under the Endangered Species Act of 1973, west of the 100th meridian of the contiguous United States. In their 12-mo finding issued in June 1998, the FWS determined that listing this population as threatened or endangered was not warranted and based that decision on review existing population and habitat information. Because the status of goshawks in the western U.S. continues to be contentious and the FWS finding has been challenged, the Raptor Research Foundation, Inc. and The Wildlife Society jointly formed a committee to review information regarding the status of the goshawk population in the contiguous U.S. west of the 100th meridian. The committee was requested to: (1) determine if there is evidence of a population trend in goshawks in the western U.S., excluding Alaska; (2) determine if there is evidence that goshawks nesting in the eastern and western U.S. represent distinctive, genetically unique populations; and (3) evaluate evidence for goshawk-habitat relations, including any association with large, mostly-unbroken tracts of old growth and mature forests. Based on existing information, the committee concluded: (1) existing data are not adequate to assess population trend in goshawks west of the 100th meridian; (2) existing analyses of phylogeography have not provided evidence of genetic differences among recognized (atricapillus, laingi) or putative (apache) subspecies, and the genetic distinctness of atricapillus goshawks in western and eastern North America is not known; and (3) at present, assessing the status of goshawks solely using distribution of late-successional forests is not appropriate, based on the current understanding of goshawk-habitat relations, although goshawks clearly use and often select late-successional forests for nesting and foraging. We provide recommendations on information needs to assess status and population trend of goshawks in the western U.S. ?? 2005 The Raptor Research Foundation, Inc.

Journal of Raptor Research↗

USGS1988

Search for volatiles on icy satellites: I. Europa

New reflectance spectra have been obtained for both the leading and trailing sides of Europa, using the Cooled Grating Array Spectrometer (CGAS) of the NASA Infrared Telescope Facility (IRTF). The spectra are of higher precision than any yet obtained. Spectra of Europa's trailing side (central meridian longitude ≈300°) obtained in 1985 show two weak absorptions near 2.2 and 2.3 μm. Both of these features as well as others are seen in spectra obtained by R. N. Clark, R. B. Singer, P. D. Owensby, and F.P. Fanale (1980a, Bull. Amer. Astron. Soc. 12, 713–714) at similar central meridian longitude. Data obtained with an improved detector array in 1986, however, do not show the absorptions seen in the 1980 and 1985 spectra. It is not clear why the newest data do not show the apparent absorptions seen in previous years, but the suggestion is that either the 1980 and 1985 data are spurious or that the material responsible for the weak absorptions is no longer detectable. Analysis of the 1980 and 1985 data did not reveal any obvious source of systematic error capable of introducing spurious features, but we are skeptical of any explanation that cites transient deposition, movement, and/or destruction of material on Europa's trailing side to account for the nondetection of the features in the 1986 data. If the weak absorptions seen in the 1980 and 1985 data are real, they can be interpreted as indicating the transient spectroscopic presence of a molecular component on Europa's trailing side different from the water ice that is known to be the dominant surface constituent. Further monitoring is required to determine if the apparent absorptions are real.

Icarus↗

USGS2012

Strain accumulation across the Denali fault in the Delta River canyon, Alaska

Deformation along the Denali fault in the Delta River canyon was determined from geodetic surveys in 1941/1942, 1970, 1975, and 1979. The data were best for the 1975–1979 interval; in that period the average strain accumulation was essentially pure right lateral shear at a rate of 0.6 ± 0.1 μrad/a (a is years) (engineering shear) across a vertical plane striking N87°E. The plane of maximum shear is rotated about 30° counterclockwise from the local strike of the Denali fault but closely coincides with the strike of a major linear segment of the fault that begins 50 km farther west. The deformation between 1941/1942 and 1970 is consistent with a similar rate of strain accumulation if one removes the coseismic strain step contributed by the 1964 Alaska earthquake. The 1970–1975 deformation is poorly defined owing to uncertainties in the 1970 survey, but the strain accumulation during that period is certainly much less than during the 1975–1979 interval. The 1975–1979 strain accumulation is interpreted by means of a dislocation model which suggests that the Denali fault in the vicinity of the Delta River Canyon behaves as a leaky transform fault (i.e., a source of spreading as well as lateral slip). The block south of the Denali fault appears to be moving westward (parallel to the strike of the Denali fault west of the 147th meridian) at the rate of about 20 mm/a relative to the North American plate. Because the linear segment of the Denali fault east of the 147th meridian (along which the geodetic network is located) strikes N63°W, accommodation of the westward motion of the southern block requires some spreading within the fault zone as well as right lateral slip on the fault.

Journal of Geophysical Research Solid Earth↗

USGS2012

Curie temperature isotherm analysis and tectonic implications of aeromagnetic data from Nevada

Estimates of the depth to the Curie temperature isotherm in Nevada are in accordance with other regional geologic and geophysical information and together can be explained in the context of present-day tectonism. A method to estimate the depth extent of magnetic sources from the statistical properties of magnetic anomalies was applied to a statewide compilation of aeromagnetic data from Nevada. Basal depths of magnetic sources show no apparent correlation with the so-called magnetic quiet zone, which trends northerly through the eastern part of the state, or with basin-and-range topography. However, certain correlations with published heat flow measurements are apparent and suggest that undulations in basal depth of magnetic sources are related in part to undulations in the Curie temperature isotherm. For example, an area of shallow basal depth (<10 km) near Battle Mountain corresponds to an area of exceptionally high conductive heat flow and indicates a shallow depth to the Curie temperature isotherm in this region. A narrow zone of shallow basal depth extends south from the Battle Mountain area along the 118°W meridian to at least latitude 38°N, which also is a zone of historic surface offsets and high-magnitude earthquakes. The correspondence along the 118° meridian of shallow basal depth, high heat flow, high lower crustal seismic velocities, attenuated P and S wave arrivals, historic faulting, and large earthquakes suggests that they each are related to an active north trending spreading zone in this part of the Basin and Range province.

Journal of Geophysical Research Solid Earth↗

USGS2014

Geographic coincidence of richness, mass, conservation value, and response to climate of U.S. land birds

Distributional patterns across the United States of five avian community breeding-season characteristics—community biomass, richness, constituent species' vulnerability to extirpation, percentage of constituent species' global abundance present in the community (conservation index, CI), and the community's position along the ecological gradient underlying species composition (principal curve ordination score, PC)—were described, their covariation was analyzed, and projected effects of climate change on the characteristics and their covariation were modeled. Higher values of biomass, richness, and CI were generally preferred from a conservation perspective. However, higher values of these characteristics often did not coincide geographically; thus regions of the United States would differ in their value for conservation depending on which characteristic was chosen for setting conservation priorities. For instance, correlation patterns between characteristics differed among Landscape Conservation Cooperatives. Among the five characteristics, community richness and the ecological gradient underlying community composition (PC) had the highest correlations with longitude, with richness declining from east to west across the contiguous United States. The ecological gradient underlying composition exhibited a demarcation near the 100th meridian, separating the contiguous United States grossly into two similar-sized avian ecological provinces. The combined score (CS), a measure of species' threat of decline or extirpation, exhibited the strongest latitudinal pattern, declining from south to north. Over &sim;75% of the lower United States, projected changes in June temperature and precipitation to year 2080 were associated with decreased averaged values of richness, biomass, and CI, implying decreased conservation value for birds. The two ecological provinces demarcated near the 100th meridian diverged from each other, with projected changes in June temperatures and precipitation from the year 2000 to 2080 suggesting increased ecological dissimilarity between the eastern and western halves of the lower United States with changing climate. Anticipated climate-related changes in the five characteristics by 2080 were more weakly correlated with latitude or longitude then the responses themselves, indicating less distinct geographic patterns of characteristic change than in the characteristics themselves. Climate changes projected for 2080 included geographic shifts in avian biomass, CS, and PC values, a moderate overall decline in CI, and general decline in species richness per site.

Ecological Applications↗

USGS1906

Zinc and lead deposits of the Upper Mississippi Valley

The zinc and lead mines of the upper Mississippi Valley are in the southwest portion of Wisconsin and in adjacent parts of Illinois mid Iowa. The boundaries of the region are in part indefinite, since sporadic occurrences of the minerals are found outside the mining region proper. It is usual to define the area as including Grant, Lafayette, and Iowa counties in Wisconsin, Jo Daviess County in Illinois, and an irregular narrow belt of territory in Clayton and Dubuque counties paralleling the Mississippi River in Iowa. In this report a slightly smaller area is discussed, the region being limited on the east by the meridian of 90° west longitude. East of this meridian there are a few scattered prospects, hut comparatively little mining has been done in recent years in the area beyond the boundary indicated, so that it is sufficiently accurate for present purposes.

Illinois, Iowa, Wisconsin↗

USGS2004

Topographic Map of the West Candor Chasma Region of Mars, MTM 500k -05/282E OMKT

This map, compiled photogrammetrically from Viking Orbiter stereo image pairs, is part of a series of topographic maps of areas of special scientific interest on Mars. The figure of Mars used for the computation of the map projection is an oblate spheroid (flattening of 1/176.875) with an equatorial radius of 3396.0 km and a polar radius of 3376.8 km. The datum (the 0-km contour line) for elevations is defined as the equipotential surface (gravitational plus rotational) whose average value at the equator is equal to the mean radius as determined by Mars Orbiter Laser Altimeter. The projection is part of a Mars Transverse Mercator (MTM) system with 20? wide zones. For the area covered by this map sheet the central meridian is at 290? E. (70? W.). The scale factor at the central meridian of the zone containing this quadrangle is 0.9960 relative to a nominal scale of 1:500,000. Longitude increases to the east and latitude is planetocentric as allowed by IAU/IAG standards and in accordance with current NASA and USGS standards. A secondary grid (printed in red) has been added to the map as a reference to the west longitude/planetographic latitude system that is also allowed by IAU/IAG standards and has been used for previous Mars maps.

IMAP↗

USGS2004

Topographic map of the Tithonium Chasma Region of Mars, MTM 500k -05/277E OMKT

This map, compiled photogrammetrically from Viking Orbiter stereo image pairs, is part of a series of topographic maps of areas of special scientific interest on Mars. The figure of Mars used for the computation of the map projection is an oblate spheroid (flattening of 1/176.875) with an equatorial radius of 3396.0 km and a polar radius of 3376.8 km. The datum (the 0-km contour line) for elevations is defined as the equipotential surface (gravitational plus rotational) whose average value at the equator is equal to the mean radius as determined by Mars Orbiter Laser Altimeter. The projection is part of a Mars Transverse Mercator (MTM) system with 20? wide zones. For the area covered by this map sheet the central meridian is at 270? E. (70? W.). The scale factor at the central meridian of the zone containing this quadrangle is 0.9960 relative to a nominal scale of 1:500,000. Longitude increases to the east and latitude is planetocentric as allowed by IAU/IAG standards and in accordance with current NASA and USGS standards. A secondary grid (printed in red) has been added to the map as a reference to the west longitude/planetographic latitude system that is also allowed by IAU/IAG standards and has been used for previous Mars maps.

IMAP↗

USGS2004

Topographic Map of the Ophir and Central Candor Chasmata Region of Mars MTM 500k -05/287E OMKT

IMAP↗

USGS1904

Forest conditions in the San Francisco Mountains Forest Reserve, Arizona

On April 12, 1902, President Roosevelt issued a proclamation "for the purpose of consolidating into one reserve the lands heretofore embraced in the San Francisco Mountains Forest Reserves and of including therein the other adjacent lands within Francisco Mountains Forest Reserve, and is described by metes and bound as follows: ''Beginning at the northwest corner of township twenty-two (22) north, range one (1) east, Gila and Salt River meridian, Arizona; thence southerly along the said meridian, allowing for the proper offset on the fifth (5th) standard parallel north, to the southwest corner of Township nineteen (19) south, range one (1) east; thence easterly along the surveyed and unsurveyed township line to the point for the northwest corner of township eighteen (18) north, range four (4) east; thence southerly along the unsurveyed range line to its intersection with the fourth (4th) standard' parallel north; thence easterly along said parallel to the point for the northwest corner of township sixteen (16) north, range five (5) east; thence southerly to the point for the southwest corner of said township; then easterly to the point for the northwest corne1· of township fifteen (15) north, range six (6) east; thence southerly to the point for the southwest corner of section eighteen (18), said township; thence easterly along the unsurveyed section line to the point for the northwest corner of section nineteen (19), township fifteen (15) north, range seven (7) east; thence southerly to the southwest corner of said section; thence easterly along the unsurveyed section lines to the southwest corner of section nineteen (19), township fifteen (15) north, range nine (9) east; thence northerly to the northwest corner of said section; thence easterly along the section line to the southeast corner of section thirteen (13), said township; thence northerly to the northeast corner of section twelve (12), said township; thence easterly along the section lines to the southeast corner of section one (1), township fifteen (15) north, range eleven (11) east; thence northerly along the range line to its intersection with the fourth (4th) standard parallel north; thence westerly along said parallel to the southeast corner of township seventeen (17) north, range eleven (11) east; thence northerly along the surveyed and unsurveyed range line to the point for the northeast corner of township eighteen (18) north, range eleven (11) east; thence westerly to the southeast corner of township nineteen (19) north, range ten (10) east; thence northerly along the range line to its intersection with the fifth (5th) standard parallel north; thence westerly along said parallel to the point for the southeast corner of township twenty-one (21) north, range nine (9) east; thence northerly along the unsurveyed range line, allowing for the proper offset on the sixth (6th) standard parallel north, to the point for the northeast cornet· of township twenty-five (25) north, range nine (9) east; thence westerly along the surveyed and unsurveyed township line to the point for the northwest corner of township twenty-five (25) north, range three (3) east; thence southerly along the surveyed and unsurveyed range line, allowing for the proper offset on the sixth (6th) standard parallel north, to the northeast corner of township twenty-two (22) north, range two (2) east; thence westerly along the township line to the northwest corner of township twenty-two (22) north, range one (1) east, to the place of beginning."

Arizona↗

USGS1904

Forest conditions in the Absaroka division of the Yellowstone Forest Reserve, Montana and the Livingston and Big Timber quadrangles

The tract of land here designated the Absaroka division of the Yellowstone Forest Reserve was originally the Absaroka Forest Reserve. By proclamation of January 29, 1903, this reserve was merged with the Teton and the Yellowstone forest reserves, the whole taking the name of the Yellowstone Forest Reserve. The western, northern, and eastern boundaries, as then established and as applicable to the Absaroka division, are as follows: "Beginning at the point where the range line between ranges nine (9) and ten (10) east, principal meridian, Montana, intersects the northern boundary of the Yellowstone National Park; thence northerly along said surveyed and unsurveyed range line, allowing for the proper offset on the first (1st) standard parallel south, to the southwest corner of section eighteen (18), township four (4) south, range ten (10) east; thence easterly to the southeast corner of said section; thence northerly to the northeast corner of section six (6); said township: thence easterly to the southeast corner of section thirty-two (32), township three (3) south, range ten (10) east; thence northerly to the northeast corner of section five (5), said township; thence easterly along the township line to the northeast corner of township three (3) south, range eleven (11) east; thence southerly to the southeast corner of said township; thence easterly along the surveyed and unsurveyed township line to the point for the south- west corner of township three (3) south, range fourteen (14) east; thence northerly along the surveyed and unsurveyed range line to the northwest corner of township two (2) south, range fourteen (14) east; thence easterly to the northeast corner of said township; thence southerly to the point for the southeast corner of said township; thence easterly to the point for the northeast corner of township three (3) south, range fifteen (15) east; thence southerly to the point for the southeast corner of said township; thence easterly along the surveyed and unsurveyed township line to the northwest corner of township four (4) south, range eighteen (18) east; thence southerly along the range line to its intersection with the first (1st) standard parallel south; thence easterly along said parallel to the northeast corner of township six (6) south, range eighteen (18) east; thence southerly along the surveyed and unsurveyed range line to the southwest corner of township seven (7) south, range nineteen (19) east; thence easterly to the northwest comer of township eight (8) south, range twenty (20) east; thence southerly to the southwest corner of said township; thence easterly to the southeast corner of said township; thence southerly along the range line to its intersection with the boundary line between the States of Montana and Wyoming." The southern boundary of the area discussed is west from the point where the eastern boundary of the reserve intersects the Montana- Wyoming line to the southeast corner of township 9 north, range 14 east; thence along the northern boundary line of the Yellowstone National Park to the point where said boundary line of the park intersects the range line between ranges 9 and 10 east, principal meridian. The total area, as above delineated, includes 1,334,400 acres.

Montana↗

USGS1905

Forest conditions in the Gila River Forest Reserve, New Mexico

The Gila River Forest Reserve was established by proclamation of President McKinley on March 2, 1899. The following is a statement of the boundaries as laid down in the proclamation: "Beginning at a point on the boundary line between New Mexico and Arizona, where it is intersected by the north line of township five (5) south, range twenty-one (21) west, New Mexico principle meridian, New Mexico; thence easterly along the township line to the northeast corner of township five (5) south, range sixteen (16) west; thence southerly along the range line between ranges fifteen (15) and sixteen (16) west, to the southeast corner of township eight (8) south, range sixteen (16) west; thence easterly along the township line to the northeast corner of township nine (9) south, range fifteen (15) west; thence southerly along the range line to the southeast corner of said township; thence easterly along the township line to the northeast corner of township ten (10) south, range ten (10) west; thence southerly along the first guide meridian west, between ranges nine (9) and ten (10) west, to its intersection with the third (3rd) standard parallel south, between townships fifteen (15) and sixteen (16) south; thence westerly along the said third (3rd) standard parallel south to the southwest corner of township fifteen (15) south, range sixteen (16) west; thence northerly along the range line to the northwest corner of said township; thence westerly along the township line to the northeast corner of township fifteen (15) south, range nineteen (19) west; thence southerly along the range line to its intersection with the third (3d) standard parallel south; thence westerly along the third (3rd) standard parallel south to its intersection with the boundary line between New Mexico and Arizona; thence northerly along said boundary line to the point where it intersects the north line of township five (5) south, range twenty-one (21) west, the place of beginning."

New Mexico↗

USGS2015

Image mosaic and topographic map of the moon

Sheet 1: This image mosaic is based on data from the Lunar Reconnaissance Orbiter Wide Angle Camera (WAC; Robinson and others, 2010), an instrument on the National Aeronautics and Space Administration (NASA) Lunar Reconnaissance Orbiter (LRO) spacecraft (Tooley and others, 2010). The equatorial WAC images were orthorectified onto the Global Lunar Digital Terrain Mosaic (GLD100, WAC-derived 100 m/pixel digital elevation model; Scholten and others, 2012 ) while the polar images were orthorectified onto the lunar LOLA polar digital elevation models (Neumann and others, 2010). The Mercator projection is used between latitudes ±57°, with a central meridian at 0° longitude and latitude equal to the nominal scale at 0°. The Polar Stereographic projection is used for the regions north of the +55° parallel and south of the –55° parallel, with a central meridian set for both at 0° and a latitude of true scale at +90° and -90°, respectively. All named features greater than 85 km in diameter or length were included unless they were not visible on the map. Some selected well-known features less than 85 km in size were also included. For listed references, please open the full PDF. Sheet 2: This map is based on data from the Lunar Orbiter Laser Altimeter (LOLA; Smith and others, 2010), an instrument on the National Aeronautics and Space Administration (NASA) Lunar Reconnaissance Orbiter (LRO) spacecraft (Tooley and others, 2010). The image used for the base of this map represents more than 6.5 billion measurements gathered between July 2009 and July 2013, adjusted for consistency in the coordinate system described below, and then converted to lunar radii (Mazarico and others, 2012). For the Mercator portion, these measurements were converted into a digital elevation model (DEM) with a resolution of 0.015625 degrees per pixel, or 64 pixels per degree. In projection, the pixels are 473.8 m in size at the equator. For the polar portion, the LOLA elevation points were used to create a DEM at 240 meters per pixel. A shaded relief map was generated from each DEM with a sun angle of 45° from horizontal, and a sun azimuth of 270°, as measured clockwise from north with no vertical exaggeration. The DEM values were then mapped to a global color look-up table, with each color representing a range of 1 km of elevation. For this map sheet, only larger feature names are shown. For references listed above, please open the full PDF.

Scientific Investigations Map↗

USGS2014

Estimating the spatial distribution of wintering little brown bat populations in the eastern United States

Depicting the spatial distribution of wildlife species is an important first step in developing management and conservation programs for particular species. Accurate representation of a species distribution is important for predicting the effects of climate change, land-use change, management activities, disease, and other landscape-level processes on wildlife populations. We developed models to estimate the spatial distribution of little brown bat ( Myotis lucifugus ) wintering populations in the United States east of the 100th meridian, based on known hibernacula locations. From this data, we developed several scenarios of wintering population counts per county that incorporated uncertainty in the spatial distribution of the hibernacula as well as uncertainty in the size of the current little brown bat population. We assessed the variability in our results resulting from effects of uncertainty. Despite considerable uncertainty in the known locations of overwintering little brown bats in the eastern United States, we believe that models accurately depicting the effects of the uncertainty are useful for making management decisions as these models are a coherent organization of the best available information.

Ecology and Evolution↗

USGS1980

Report of the IAU Working Group on Cartographic Coordinates and Rotational Elements of the Planets and Satellites

This paper is the entire report of the IAU Working Group on Cartographic Coordinates and Rotational Elements of the Planets and Satellites, including three annexes. Tables give the recemmended values for the directions of the north poles of rotation and the prime meridians of the planets and satellites. Reference surfaces for mapping these bodies are described. The annexes discuss the guiding principles, given in the body of the report, present explanatory notes, and provide a bibliography of the rotational elements and reference surfaces of the planets and satellites, definitions, and algebraic expressions of relevant parameters. ?? 1980 D. Reidel Publishing Co.

Celestial Mechanics↗

USGS2007

Report of the IAU/IAG Working Group on cartographic coordinates and rotational elements: 2006

Every three years the IAU/IAG Working Group on Cartographic Coordinates and Rotational Elements revises tables giving the directions of the poles of rotation and the prime meridians of the planets, satellites, minor planets, and comets. This report introduces improved values for the pole and rotation rate of Pluto, Charon, and Phoebe, the pole of Jupiter, the sizes and shapes of Saturn satellites and Charon, and the poles, rotation rates, and sizes of some minor planets and comets. A high precision realization for the pole and rotation rate of the Moon is provided. The expression for the Sun's rotation has been changed to be consistent with the planets and to account for light travel time ?? 2007 Springer Science+Business Media B.V.

Celestial Mechanics and Dynamical Astronomy↗

USGS2010

Report of the IAU Working Group on cartographic coordinates and rotational elements: 2009

Every three years the IAU Working Group on Cartographic Coordinates and Rotational Elements revises tables giving the directions of the poles of rotation and the prime meridians of the planets, satellites, minor planets, and comets. This report takes into account the IAU Working Group for Planetary System Nomenclature (WGPSN) and the IAU Committee on Small Body Nomenclature (CSBN) definition of dwarf planets, introduces improved values for the pole and rotation rate of Mercury, returns the rotation rate of Jupiter to a previous value, introduces improved values for the rotation of five satellites of Saturn, and adds the equatorial radius of the Sun for comparison. It also adds or updates size and shape information for the Earth, Mars’ satellites Deimos and Phobos, the four Galilean satellites of Jupiter, and 22 satellites of Saturn. Pole, rotation, and size information has been added for the asteroids (21) Lutetia, (511) Davida, and (2867) Šteins. Pole and rotation information has been added for (2) Pallas and (21) Lutetia. Pole and rotation and mean radius information has been added for (1) Ceres. Pole information has been updated for (4) Vesta. The high precision realization for the pole and rotation rate of the Moon is updated. Alternative orientation models for Mars, Jupiter, and Saturn are noted. The Working Group also reaffirms that once an observable feature at a defined longitude is chosen, a longitude definition origin should not change except under unusual circumstances. It is also noted that alternative coordinate systems may exist for various (e.g. dynamical) purposes, but specific cartographic coordinate system information continues to be recommended for each body. The Working Group elaborates on its purpose, and also announces its plans to occasionally provide limited updates to its recommendations via its website, in order to address community needs for some updates more often than every 3 years. Brief recommendations are also made to the general planetary community regarding the need for controlled products, and improved or consensus rotation models for Mars, Jupiter, and Saturn.

Celestial Mechanics and Dynamical Astronomy↗