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At least 73 records · Page 4Linked to original sources
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↗
USGS1981

Thermal inertia mapping of Mars from 60°S to 60°N

Twenty-micrometer brightness temperatures are used to derive the thermal inertia for 81% of the Martian surface between latitudes ±60°. These data were acquired by the two Viking Infrared Thermal Mappers in 1977 and 1978 following the two global dust storms of 1977. The spatial resolution used is 2° in latitude by 2° in longitude and the total range in derived inertia is . The distribution of thermal inertia is strongly bimodal with all values of thermal inertia less than being associated with three disjoint bright regions mostly in the northern hemisphere. Sufficient dust is raised in global storms to provide fine material adequate to produce these low-inertia areas but the specific deposition mechanism has not been defined. At the low resolution used, no complete exposures of clean rock were found. There is some tendency for darker material to be associated with higher thermal inertia, although the trend is far from one to one. The distribution of high- and low-inertia areas is sufficiently nonrandom to produce a variation in whole-disk brightness temperature with central meridian longitude. This variation and the change in surface kinetic temperature associated with dust storms are factors in establishing the whole-disk brightness temperature at radio and infrared wavelengths and will be important for those who use Mars as a calibration source.

Icarus↗
USGS2001

Copper, cadmium, and zinc concentrations in juvenile Chinook salmon and selected fish-forage organisms (aquatic insects) in the upper Sacramento River, California

This study assessed the downstream extent andseverity of copper (Cu), cadmium (Cd), and zinc (Zn)contamination from acid mine drainage on juvenile chinook salmon( Oncorhynchus tshawytscha ) and aquatic insects over aroughly 270-km reach of the Sacramento River below KeswickReservoir. During April–May 1998, salmon were collected fromfour sites in the river and from a fish hatchery that receiveswater from Battle Creek. Salmon from river sites were examinedfor gut contents to document their consumption of variousinvertebrate taxa, whereas salmon from river sites and thehatchery were used for metal determinations. Midge(Chironomidae) and caddisfly (Trichoptera) larvae and mayfly(Ephemeroptera) nymphs were collected for metal determinationsduring April–June from river sites and from Battle and Buttecreeks. The fish hatchery and Battle and Butte creeks served asreference sites because they had no history of receiving minedrainage. Salmon consumed mostly midge larvae and pupae (44.0%,damp-dry biomass), caddisfly larvae (18.9%), Cladocera (5.8%),and mayfly nymphs (5.7%). These results demonstrated thatinsects selected for metal determinations were important as fishforage. Dry-weight concentrations of Cu, Cd, and Zn weregenerally far higher in salmon and insects from the river thanfrom reference sites. Within the river, high metalconcentrations persisted as far downstream as South Meridian (thelowermost sampling site). Maximum concentrations of Cd (30.7 μg g -1 ) and Zn (1230 μg g -1 ),but not Cu (87.4 μg g -1 ), in insects exceeded amounts that other investigators reported as toxic when fed for prolonged periods to juvenile salmonids.

California↗
USGS2010

Time-averaged paleomagnetic field at the equator: Complete data and results from the Galapagos Islands, Ecuador

We present here the complete paleomagnetic laboratory results from a collection of approximately 1500 oriented cores from all 16 of the Galapagos Islands, Ecuador, collected by Allan Cox in 1964–1965 but nearly all previously unpublished. The islands are located in the eastern Pacific Ocean within 1.4° of latitude from the equator and range in age from historically erupted to 3 Ma, mostly determined by published K-Ar and 3He isotopic dating. The number of sites collected on each island ranges from 1 to 28, for a total of 186. After combining duplicate site mean directions, 149 are used for an overall mean direction and 8 represent excursions and one reversal path. Divided by geomagnetic polarity chron, 110 site means are Brunhes or Jaramillo (normal polarity), 27 are Matuyama (reversed polarity), and 12 are Gauss (both polarities). We have completed the magnetic cleaning that was commenced in the late 1960s. Secondary (mostly viscous) magnetizations were nearly all removed by alternating field demagnetization at 10 mT. We have used the so-called blanket cleaning method, generally at 10 mT. All sites were in basalt flows and gave good paleomagnetic results; none was rejected in toto, and only a few core specimens were magnetically unsatisfactory. Nearly all sites had eight independently oriented cores, and within-site angular standard deviations of directions range from 1° to 8°. We used both Fisher and Bingham statistics to analyze the data and found that many of the direction populations are strongly elongate along the paleomagnetic meridian, while the corresponding virtual pole (VGP) populations are essentially circularly distributed. The paleomagnetic poles, calculated as the means of VGPs, are as follows: Brunhes and Jaramillo, north latitude = 86.9°, east longitude = 245.1°, and 95% confidence radius A 95 = 1.9°; Matuyama, latitude = 87.2°, longitude = 158.2°, and A 95 = 3.8°; Gauss, latitude = 83.0°, longitude = 204.7°, and A 95 = 7.0°. These paleomagnetic poles do not differ significantly from one another, but the Brunhes and Jaramillo combined pole is significantly near-sided with respect to the Galapagos, as is the overall mean pole, which is at latitude = 87.1° and longitude = 227.6°, with A 95 = 1.7°. Omitting the excursion and reversal path data, the overall angular standard deviation of VGPs is 11.7° with lower and upper 95% confidence limits of 10.8° and 12.7°, respectively, in good agreement with previously published values for near-equatorial sampling latitudes.

Galapagos Islands↗
USGS2011

An empirical model of the quiet daily geomagnetic field variation

An empirical model of the quiet daily geomagnetic field variation has been constructed based on geomagnetic data obtained from 21 stations along the 210 Magnetic Meridian of the Circum‐pan Pacific Magnetometer Network (CPMN) from 1996 to 2007. Using the least squares fitting method for geomagnetically quiet days ( Kp ≤ 2+), the quiet daily geomagnetic field variation at each station was described as a function of solar activity SA , day of year DOY , lunar age LA , and local time LT . After interpolation in latitude, the model can describe solar‐activity dependence and seasonal dependence of solar quiet daily variations (S) and lunar quiet daily variations (L). We performed a spherical harmonic analysis (SHA) on these S and L variations to examine average characteristics of the equivalent external current systems. We found three particularly noteworthy results. First, the total current intensity of the S current system is largely controlled by solar activity while its focus position is not significantly affected by solar activity. Second, we found that seasonal variations of the S current intensity exhibit north‐south asymmetry; the current intensity of the northern vortex shows a prominent annual variation while the southern vortex shows a clear semi‐annual variation as well as annual variation. Thirdly, we found that the total intensity of the L current system changes depending on solar activity and season; seasonal variations of the L current intensity show an enhancement during the December solstice, independent of the level of solar activity.

Journal of Geophysical Research A: Space Physics↗
USGS2007

Mapping raster imagery to the interrupted Goode Homolosine projection

Because of the increasing emphasis on global monitoring, processing remotely-sensed raster image data onto global map projections has become an important issue. One class of map projections, interrupted equal-area projections, is especially useful for this purpose. The use of the Interrupted Goode Homolosine map projection for the Global Land Advanced Very High Resolution Radiometer (AVHRR) 1 km project and the AVHRR Pathfinder project has produced a map that is both attractive to the viewer and useful for data analysis. This interrupted, composite, equal-area map projection uses the Sinusoidal projection for low latitudes and the Mollweide projection for high latitudes and is broken into 12 regions, each with its own central meridian. This combination of projections helps to preserve the shape of the land masses and results in a map that has less distortion than an uninterrupted global map. The use of the interrupted projection also simplifies the processing and management of larger data sets, because the data can be processed either separately in the component projections that make up the interrupted projection or directly onto the interrupted projection.

International Journal of Remote Sensing↗
USGS2007

Climate factor for small-basin flood frequency

A climate factor, CT, (T = 2-, 25-, and 100-year recurrence intervals) that delineates regional trends in small-basin flood frequency was derived using data from 71 long-term rainfall record sites. Values of CT at these sites were developed by a regression analysis that related rainfall-runoff model estimates of T-year floods to a sample set of 50 model calibrations. CT was regionalized via kriging to develop maps depicting its geographic variation for a large part of the United States east of the 105th meridian. Kriged estimates of CT and basin-runoff characteristics were used to compute regionalized T-year floods for 200 small drainage basins. Observed T-year flood estimates also were developed for these sites. Regionalized floods are shown to account for a large percentage of the variability in observed flood estimates with coefficients of determination ranging from 0.89 for 2-year floods to 0.82 for 100-year floods. The relative importance of the factors comprising regionalized flood estimates is evaluated in terms of scale (size of drainage area), basin-runoff characteristics (rainfall-runoff model parameters), and climate (CT).

Water Resources Bulletin↗
USGS1962

Correlation of the Carrizo Sand in Arkansas and adjacent states

The Carrizo Sand (Eocene), the basal unit of the Claiborne Group, can be recognized in the subsurface throughout much of southeastern Arkansas and is correlated with the Carrizo Sand of Louisiana and the Meridian Sand Member of the Tallahatta Formation of Mississippi. The term Carrizo Sand is appropriate for use in Arkansas , as the stratigraphic terminology most workers apply to the Claiborne Group in Arkansas conforms with the terminology of Louisiana. A surface exposure of the Carrizo Sand in Arkansas is lithologically identical with described exposures of the Carrizo in northwestern Louisiana.

Arkansas, Louisiana, Mississippi, Tennessee↗
USGS1942

Reconnaissance survey of the Roberts Mountains, Nevada

The Roberts Mountains region, central Nevada, provides an excellent section of Paleozoic rocks ranging from Upper Cambrian to Permian. Major low-angle thrusting is indicated by deformed Ordovician strata resting on Paleozoics of varying age. Overlying a thick breccia zone, the upper thrust plate consists of sandstones, andesitic flows and tuffs, black shales, and bedded cherts (Vinini formation). Ordovician age of the Vinini is established on the basis of graptolite faunules. A belt of Lower to Middle Ordovician graptolitic facies similar to the Vinini formation crosses the Great Basin west of Roberts Mountains. Deposits of roughly the same age in the Roberts Mountains meridian and eastward are dominantly limestone, carrying distinct faunas. Axial planes of overturned folds in the thrust plate dip west, a further indication that the upper thrust plate moved from west to east. Minimum horizontal displacement is 16 miles. The date of thrusting is uncertain, but presumably was later Cretaceous or early Tertiary. Following thrusting, an alaskite stock and rhyolite porphyry plugs were intruded; lava flows and tuffs covered the area in part. Thrust plate and cover of volcanics have been broken into normal fault blocks. The post-thrusting igneous rocks, like volcanic rocks of Utah and New Mexico, are characterized by high potash content.

Nevada↗
USGS2021

Earthquake magnitudes from dynamic strain

Dynamic strains have never played a role in determining local earthquake magnitudes, which are routinely set by displacement waveforms from seismic instrumentation (e.g., M L ⁠ ). We present a magnitude scale for local earthquakes based on broadband dynamic strain waveforms. This scale is derived from the peak root‐mean‐squared strains ( ⁠ A ⁠ ) in 4589 records of dynamic strain associated with 365 crustal earthquakes and 77 borehole strainmeters along the Pacific‐North American plate boundary on the west coast of the United States and Canada. In this data set, catalog moment magnitudes range from 3.5≤ M w ≤ 7.2 ⁠ , and hypocentral distances range from 6≤ R ≤500 km . The 1D representation of geometrical spreading and attenuation of A common to all strain data is log A 0 ( R )=−0.00072R−1.45log(R) . After correcting for instrument gain, site terms, and event terms, the magnitude scale, M DS =log A −log A 0 ( R )−log(3×10−9) ⁠ , scales as ≈0.92 M w with a residual standard deviation of 0.19. This close association with M w holds for events east of the −124° meridian; west of this boundary, however, a constant correction of 0.41 is needed to adjust for additional along‐path attenuation effects. As a check on the accuracy of this magnitude scale, we apply it to dynamic strain records from three strainmeters located in the near field of the 2019 M 6.4 and 7.1 Ridgecrest earthquakes. Results from these six records are in agreement to within 0.5 magnitude units, and five out of six records are in agreement to within 0.34 units.

California, Oregon, Washington↗