A global map of gamma ray counting rates binned on twenty-degree quasi-equal-area pixels is provided. The map was determined from a time series of net counting rates for the 7.6 MeV gamma ray peak produced by neutron capture with Fe within Ceres' regolith. The data were acquired by Dawn's Gamma Ray and Neutron Detector (GRaND) while in low altitude mapping orbit, about 385 km from Ceres' surface (about 0.8 body radii altitude). Prior to mapping, the time series counting data were subjected to corrections for variations in the flux of galactic cosmic rays and measurement geometry, as described by PRETTYMANETAL2017.

These multiple scanning experiment image can be used to construct multi-scale multi component digital rock.

URL: https://geoscience.data.qld.gov.au/dataset/mr002949

The Ray series map was compiled in 2018 at 1:100 000 as part of the Mineral Occurrence 1:100 000 Compilation series to provide an interpretation of known mineral occurrence information. The map product is available to all government agencies, industry and the public for reference and is located within the Ray (7645) 1:100 000 map area.

Displays the coverage of publicly available digital gamma-ray spectrometric data. The map legend is coloured according to the line spacing of the survey with broader line spacings (lower resolution …Show full descriptionDisplays the coverage of publicly available digital gamma-ray spectrometric data. The map legend is coloured according to the line spacing of the survey with broader line spacings (lower resolution surveys) displayed in lighter shades of blue and coral. Closer line spacings (higher resolution surveys are displayed in red, dark blue and purple.

URL: https://geoscience.data.qld.gov.au/dataset/mr002328

The Ray series map was compiled in 2018 at 1:100 000 as part of the Geological 1:100 000 Compilation series to provide an interpretation of known surface geology information. The map product is available to all government agencies, industry and the public for reference and is located within the Ray (7645) 1:100 000 map area.

Field data including geological map with sample locations, sample description, thin section images, Electron Backscatter Diffraction (EBSD) and Energy Dispersive X-ray Spectrometry (EDS) data. Field work and targeted sampling took place, in May 2023, around the exceptional field exposure of an interpreted Slow Earthquake zone in Col d’Amoss, New Caledonia. This data has come into existence through research funded by the NERC Grant NE/X012778/1 Exploring the geological signature of Slow Earthquakes through legacy experiments and field analysis.

Fossils, including those that occasionally preserve decay-prone soft-tissues, are mostly made of minerals. Accessing their chemical composition provides unique insight into their past biology and/or the mechanisms by which they preserve, leading to a series of developments in chemical and elemental imaging. However, the mineral composition of fossils, particularly where soft-tissues are preserved, is often only inferred indirectly from elemental data, while X-ray diffraction that specifically provides phase identification received little attention. Here, we show the use of synchrotron radiation to generate not only X-ray fluorescence elemental maps of a fossil, but also mineralogical maps in transmission geometry using a two-dimensional area detector placed behind the fossil. This innovative approach was applied to millimetre-thick cross-sections prepared through three-dimensionally preserved fossils, as well as to compressed fossils. It identifies and maps mineral phases and their distribution at the microscale over centimetre-sized areas, benefitting from the elemental information collected synchronously, and further informs on texture (preferential orientation), crystallites size and local strain. Probing such crystallographic information is instrumental in defining mineralization sequences, reconstructing the fossilization environment and constraining preservation biases. Similarly, this approach could potentially provide new knowledge on other (bio)mineralization processes in environmental sciences. We also illustrate that mineralogical contrasts between fossil tissues and/or the encasing sedimentary matrix can be used to visualize hidden anatomies in fossils.

Methods Data were collected at the DiffAbs beamline of the SOLEIL Synchrotron source (France). Synchronous synchrotron rapid scanning X-ray fluorescence and diffraction mapping (SRS-XRFD) was performed using an incident X-ray beam of 16.2 or 18 keV, monochromatised using a Si(111) double-crystal monochromator, with a beam size diameter reduced down to 50 or 100 µm using platinum pinholes, or focused down to ~10 µm using Kirkpatrick-Baez mirrors. XRF was collected using a 4-element silicon drift detector (SDD, Vortex ME4, Hitachi High-Technologies Science America, Inc., total active area: 170 mm2) oriented at 90° to the incident beam, in the horizontal plane. XRD was collected in transmission geometry using a 2D hybrid pixel detector (XPAD S140, 240×560 pixels of 130 µm each), placed behind the sample at a distance of typically 200–300 mm such to intercept diffraction rings over an angular range of ~7° in scattering angle (2θ). Two-dimensional scanning was done by moving laterally the fossils in a plane rotated around the vertical axis by 20° to the primary beam (i.e., incident angle), to limit X-ray beam footprint on the sample but also such that the sample exhibits its surface to the SDD detector (no shadowing of the reflected XRD signal, figure 1a). Mapping over the entire fossils at a 35–100 µm lateral resolution was performed on the fly using the FLYSCAN platform. A full XRF spectrum and one or several XRD images were collected at each pixel.

The present dataset includes 6 types of data:

(1) Synchrotron X-Ray Fluorescence elemental maps

Methods: All elemental distributions presented in the paper correspond to integrated intensities around emission lines of elements of interest (XRF peaks), represented using linear (expect figure 1b, logarithmic) grey or color scales that go from dark to light, respectively for low to high intensities.

Data: figure1b_AsPb-map_DATA_XRF.txt; figure1b_Mn-map_DATA_XRF.txt; figure1b_Zn-map_DATA_XRF.txt; figure1b_stackRGB_DATA_XRF.tif; figure2b_Ca-map_DATA_XRF.txt; figure2b_Fe-map_DATA_XRF.txt; figure2b_Y-map_DATA_XRF.txt; figure2b_stackRGB_DATA_XRF.tif; figure5f_Y-map_DATA_XRF.txt

(2) Synchrotron X-Ray Diffraction detector images

Methods: A few XPAD detector images are shown in the paper, either simply after flat correction (figure 1c) or after conversion to (2θ-Ѱ) coordinates (figure 2e). These images are represented using logarithmic color scales that go from dark to light, respectively for low to high intensities.

Data: figure1c_left_DATA_XRD.txt; figure1c_right_DATA_XRD.txt; figure2e_DATA_XRD.xlsx

(3) Diffractograms

Methods: XPAD detector images were processed (azimuthal data regrouping along y direction) to extract their respective diffractograms (Intensity vs. 2θ profiles). Phase identification and 2θ calibration were performed using powder XRD diffractograms obtained on fragments of the sedimentary matrix (and of the fossil when possible) using the Match! software (Crystal Impact) making use of the International Centre for Diffraction Data (ICDD)- PDF 2015 database. Additional peaks in the XRD maps could then be identified using Match/ICDD database, as well as from the elemental information provided by the XRF data.

Data: figure1d_DATA_XRD.xlsx; figure2f_DATA_XRD.xlsx

(4) Synchrotron X-Ray Diffraction mineral maps

Methods: During XPAD detector images processing 4D datasets (x, y, 2θ, intensity) were also generated, and then particular XRD contrast maps. Phase identification and 2θ calibration is discussed above. All phase distributions presented in the paper correspond to integrated intensities of XRD peaks of interest, represented using linear grey or color scales that go from dark to light, respectively for low to high intensities.

Data: figure1e_left_DATA_XRD.txt; figure1e_center_DATA_XRD.txt; figure1e_right_DATA_XRD.txt; figure2c_A211-map_DATA_XRD.txt; figure2c_C006-map_DATA_XRD.txt; figure2c_Q101-map_DATA_XRD.txt; figure2c_stackRGB_DATA_XRD.tif; figure2d_C012-map_DATA_XRD.txt; figure2d_C113-map_DATA_XRD.txt; figure2d_C202-map_DATA_XRD.txt; figure2d_stackRGB_DATA_XRD.tif; figure4a_17p97-map_DATA_XRD.txt; figure4a_25p09-map_DATA_XRD.txt; figure4a_26p01-map_DATA_XRD.txt; figure4a_stackRGB_DATA_XRD.tif; figure4b_22p51-map_DATA_XRD.txt; figure4b_26p97-map_DATA_XRD.txt; figure4b_27p63-map_DATA_XRD.txt; figure4b_stackRGB_DATA_XRD.tif; figure5b_FAp002-map-head_DATA_XRD.txt; figure5b_FAp211-map-head_DATA_XRD.txt; figure5b_phyll-map-head_DATA_XRD.txt; figure5b_stackRGB-head_DATA_XRD.tif; figure5b_FAp002-map-tail_DATA_XRD.txt; figure5b_FAp211-map-tail_DATA_XRD.txt; figure5b_phyll-map-tail_DATA_XRD.txt; figure5b_stackRGB-tail_DATA_XRD.tif; figure5c_FAp002-map-cropped_DATA_XRD.txt; figure5e_FAp002-map_DATA_XRD.txt

(5) Crystallite sizes

Methods: By Gaussian fitting the 2θ profile of XRD peaks attributed to different crystalline phases, corresponding crystallite sizes were extracted (for each pixel of the maps) by converting their full width at half maximum (FWHM) using Scherrer’s formula. It was assumed that only the crystallite size is contributing to the broadening, and an instrument resolution function measured as ~0.035° (amounting several 10 %, and up to 50 % of the measured peak FWHM) was also taken into account for FWHM deconvolution. Crystallite size distributions are represented in the paper using linear color scales that go from dark to light, respectively for low to high intensities.

Data: figure2g_A211-crystSize-map_DATA_XRD.txt; figure2g_C006-crystSize-map_DATA_XRD.txt; figure2g_Q101-crystSize-map_DATA_XRD:txt; figure2g_stackRGB_DATA_XRD.tif

(6) Local texture measurements

Methods: In order to confirm some microstructure results obtained using the local probe XRD approach, supplementary local texture measurements were performed. This was done by scanning it in azimuth (Φ, rotation around the sample surface normal) and elevation (Ѱ, rotation around the projection of the impinging X-ray beam on the sample surface), while recording, at each position, the X-ray scattered signal. The resulting intensity is represented in a map, in polar coordinates (azimuth angle and elevation, e.g. figures 3f–h). In this way, when one or several crystallites are oriented such that the Bragg law is fulfilled for the particular inter-reticular distance probed (or the particular Bragg angle 2θ), high signal is found in the particular corresponding regions of the polar map, allowing: i) to retrieve the particular orientation of the grains (j, y), and ii) to possibly quantify the volume ratio of that particular orientation, compared to other orientations on the map. Rapid texture measurements were performed using the XPAD area detector. The sample was illuminated by the impinging X-ray beam (of size ~ 150 × 150 µm2 in this case) and the azimuth (Φ) and elevation (Ѱ) angles were scanned, the first one continuously. An image was recorded in each point, then texture maps for various 2θ angles (i.e. volumes) were reconstructed. Then, a similar dataset was recorded at the next vertical position on the sample. Local texture measurements are represented in the paper using logarithmic color scales that go from dark to light, respectively for low to high intensities.

Data: Figure3b-d_DATA_XRD.xlsx; figure3f_left_DATA_XRD.txt; figure3f_right_DATA_XRD.txt; figure3g_left_DATA_XRD.txt; figure3g_right_DATA_XRD.txt; figure3h_left_DATA_XRD.txt; figure3h_right_DATA_XRD.txt

The gammaA geo-referenced airborne gamma-ray image of the study area at nominal scale 1:250,000, produced for the Thai Department of Mineral Resources (Kenting Earth Science International limited (KESIL), 1982; Wisedsind et al., 1994) was acquired. The AGRI data was collected at the beginning of the winter season in November 1985 by aircraft with flight line spacing of 2 km, terrain clearance of 400 m and a flight line direction west to east, flown at a constant height above the ground of 400 ft (MTC). The production of radiation and ternary radiation maps of Thailand were produced using IAEA method (Angsuwathana and Chotikanatis, 1997; IAEA, 2003), which resulted in an image with 400 x 400 m pixels. The gamma-ray spectrometer, developed by KESIL, contained 12 crystals in a 50.34 litre Harshaw NaI (Tl) crystal scintillator and recorded gamma-rays in 256 channels. The measured energy spectrum ranges from 0 to 3 MeV (wavelengths between 0.03 x 10-4 to 4.13 x 10-4 nanometres). The sensor measures the natural radiation from decay series of potassium (K), thorium (Th) and uranium (U) in the upper 45 cm of the Earth’s surface. The following energy windows were used to measure the total count (TC) and three radioelements: TC = 0.40-2.82 Mev., K = 1.36-1.56 Mev., U = 1.66-1.86 Mev., and Th = 2.42-2.82Mev. Potassium is measured directly from the decay of 40K and is expressed as a percentage. Thorium and Uranium are inferred from daughter elements associated with distinctive isotopic emissions from 208Tl and 214Bi in their respective decay chains and are expressed in equivalent parts per million and coded as eU and eTh. A complication is that 214Bi is also a decay product of radon gas, 222Rn, itself a decay product of radium, 226Ra. Radon concentration is highly dependent on soil moisture, being practically absent near the surface in dry soil and abundant in saturated soil (Grasty, 1997). Another complication is that the signals for 40K and 208Tl (i.e., eU) are attenuated in wet soil; this has been used to map soil moisture in homogeneous soil materials using K/eTh ratios (Carroll 1981). Atmospheric Rd is also affected by changes in air density due to temperature and pressure, thus data acquired in cool high-pressure conditions may have up to 30% enhanced Rd compared to warm low-pressure, thereby distorting the eU signal (IAEA, 2003). For these reasons the eU signal is considered less reliable than those for K and eTh.-ray imagery Date: 2019-06-20 Date Submitted: 2020-04-15

This archived Paleoclimatology Study is available from the NOAA National Centers for Environmental Information (NCEI), under the World Data Service (WDS) for Paleoclimatology. The associated NCEI study type is Climate Reconstruction. The data include parameters of climate reconstructions with a geographic location of Global. The time period coverage is from 18000 to 18000 in calendar years before present (BP). See metadata information for parameter and study location details. Please cite this study when using the data.

Our Phase I study demonstrated that muons, the long-range charged component of GCR showers, can penetrate SSBs on the order of a km in diameter or less, providing information on their interior structure. Muons produced in Earth’s atmosphere have been applied to image the interior of large objects, such as the Great Pyramids and volcanos. In Phase I, we found that the production of muons in the solid surfaces of airless bodies is much smaller than in Earth’s atmosphere. Nevertheless, the flux of transmitted muons is sufficient to detect inclusions within an asteroid or comet in a reasonable period of time, ranging from hours to weeks, depending on the size of the SSB and the density contrast, position and size of the inclusion. The intrinsic spatial resolution of muon radiography (“muography”) is on the scale of a few meters. The spatial resolution that can be achieved in practice depends on signal intensity and integration time, the angular resolution of the muon tracker (hodoscope) and details of data reduction and analysis methodology.

Our Phase II project will continue to assess remaining unknowns for the application of muography to determining the interior structure of SSBs, assess risks for implementation, and provide a roadmap for development of SSB muography beyond the NIAC program. To achieve our objectives, we will work on four interrelated tasks:

• Signal and background characterization: Characterize the production and transmission of muons and secondary particle backgrounds made by cosmic ray showers in SSBs;
• Imaging studies: Develop methods to determine the density structure of SSB interiors and near-surface features from radiographic and tomographic data;
• Instrument design: Using simulations and bench-top laboratory experiments, investigate specific concepts for the design of compact hodoscopes that can be deployed on a spacecraft or in situ;
• Synthesis: Determine the range of applicability of the concept, identify the steps needed for maturation of the concept, and explore concepts for a pilot muography mission.

Successful implementation of SSB muography requires a thorough understanding of muon production and transmission as well as sources of background. Phase I demonstrated that muon production is sensitive to the density of the top-most meter of the regolith. Thus, unknown variations in regolith density may obscure interior structure. Limb imaging of muons and the use of radar data to remotely map near-surface density will be explored as possible ways to mitigate variations in muon production. A compact, inexpensive system that could be deployed on a spacecraft or in situ appears to be feasible and warrants further study. A successful design must be capable of separately measuring the transmitted muon signal from the primary GCRs and secondary particles that scatter into the field-of-view of the hodoscope. This can be accomplished, for example, using Cherenkov radiators to reject lower energy scattered particles and to determine particle direction. Concepts for imaging systems identified in Phase I will be scrutinized.

Phase II will be carried out by a multidisciplinary project team with broad experience in cosmic ray physics, remote sensing, meteoritics and planetary science. While the development of muography for SSBs is risky, the potential benefits are significant. There are presently no established methods to directly characterize the interior structure and macroporosity of an asteroid or comet. Muography could provide a direct and cost-effective means of probing the interior density structure.

Two datasets were uploaded. Run numbers #r0101~#r0112 were collected from self-seeded XFEL mode. Run numbers #r0079~#r0090 were collected from SASE mode. The run number is shown in the file name as "ue_191027_SFX_runnumber-c00.cxi.".

Legacy product - no abstract available Legacy product - no abstract available

This data set provides tables of net counting rates of Fe gamma rays at 7.6 MeV measured by the BGO detector of Dawn's Gamma Ray and Neutron Detector acquired at the low altitude mapping orbit. The counting rates were normalized for variations of live time, solid angle of Vesta, and galactic cosmic ray intensity. They were also corrected for variations of neutron number density derived from thermal and epithermal neutron observations by GRaND (PRETTYMANETAL2013). The table contains the original Fe counting rates reported by YAMASHITAETAL2013.

The ODY MARS GAMMA RAY SPECTROMETER 5 ELEMENTS data set consists of a set of maps and underlying data products originally released to the public in March 2006. They contain data that was collected by the 2001 Mars Odyssey Gamma-ray Spectrometer between June 4, 2002 and April 3, 2005. These data are highly processed, and represent the fully corrected, CO2 frost free elemental concentrations. Data for all non-radioactive species have been masked to exclude polar regions where we currently cannot adequately deal with dilution by the large amounts of water ice.

The earth is continually bombarded by high-energy cosmic ray particles, and the worldwide average exposure to cosmic rays represents about 13% of the total annual effective dose received by the population. Therefore, assessment of cosmic ray exposure at the ground level is of great interest to better understand population exposure to ionizing radiation. This paper presents and describes the European Annual Cosmic-Ray Dose Map at 1 km resolution (Main Map). The Main Map displays the annual effective dose that a person may receive from cosmic rays at the ground level, which ranges from 301 to 3955 μSv. Moreover, thanks to the availability of population data, the annual cosmic-ray collective dose has been evaluated and population-weighted average annual effective dose (per capita) due to cosmic ray has been estimated for each European country considered in this study. The accuracy of the present study has been confirmed by comparing our results with those obtained using other models.

A global map of the concentration of iron within the regolith of asteroid 1 Ceres on twenty-degree quasi-equal-area pixels is provided. Iron concentrations were determined from gamma ray counting data acquired by Dawn's Gamma Ray and Neutron Detector (GRaND) in a low altitude mapping orbit, about 385 km from Ceres' surface (about 0.8 body radii altitude). The concentrations are representative of Ceres's bulk regolith to depths up to a few decimeters with a spatial resolution of about 600-km full-width-at-half-maximum of arc length on the surface. The methods used to determine iron concentration are described by PRETTYMANETAL2017.

The following data sets were collected to support the potential uses of opensource data in the context of digital humanities and heritage sciences.

This proposed experiment is conducted by the UCL Institute for Sustainable Heritage in collaboration with the Centre for Digital Humanities. Imaging methods including Photography, Multispectral Imaging, Hyperspectral Imaging and Xray Fluorescence Mapping have been collected along with the complete readout metadata of the instrumentation.

We hope that you find the data helpful, and we welcome you to use the data in any way you wish, for all and any analysis development purposes. For us to build upon this research, we ask that in return you would be willing to share in some regard your experiences in using open-source data, using our data, successes and issues.

If you would be willing to engage with us in this endeavor, please feel free to contact us so that we may be able to follow up with you.

Other Data sets available Here

E: molly.fort.21@ucl.ac.uk

Object Paradata;

Postcard – c. Early 1900's

Language – Eng.

Materials – colour print on card, metallic leafing.

Front transcription -

‘Greetings’

‘May your Birthday bring you Peace & perfect Happiness, Golden hopes & Love of Friends, And every Happiness this world can send.’

Object Dimensions – 138mm X 88mm

The postcard is an item of ephemera donated to the UCLDH Digitisation Suite by Prof Melissa Terras, for teaching and training purposes in 2015.

This folder contains:

X-ray fluorescence imaging map collected from a Bruker M4+ Tornado Micro-XRF System

Postcardmap1.bcf - Bruker composite file containing full fluorescence spectral and mapping data with some other information. Can be read by Bruker software or using freely dowloadable Hyperspy.

EDX.hdf5 - full fluorescence spectral and mapping data in open format, created and readable via. Hyperspy.

Postcard_data.txt - metadata saved in ASCII format by Bruker system.

postcardmap1_*.png - individual png images of mapped elements, listed in filename.

All nuclide maps that were generated in the paper "Abundance and distribution of radioelements in lunar terranes: Results of Chang’E-1 gamma ray spectrometer data".Citation:J. Chen et al., Abundance and distribution of radioelements in lunar terranes: Results of Chang'E-1 gamma ray spectrometer data. Advances in Space Research 57, 919–927 (2016).

Abstract ======== This data set consists of the MESSENGER XRS reduced data record observations, also known as RDRs, which are derived from the calibrated data records, CDRs. Each XRS observation results in four X-ray spectra. When an X-ray interacts with one of the four detectors, a charge or voltage pulse is generated. This signal is converted into one of 2^8 (256) channels, which are correlated to energy. Over a commanded integration time period a histogram of counts as a function of energy (channel number) is recorded. The EDRs are the number of events in each channel of the four detectors accumulated over the integration period. Channels above or below the useful energy range of the detectors are not transmitted. The result is three 244-channel GPC histograms and one 231-channel solar monitor histogram, each of which is designated as a single X-ray spectrum. Each observation is calibrated and processed into the CDR data set and then further processed to produce a map of elemental ratios, the maps of which compose the RDR data set.

This layer shows data collected mainly by the Geochemical Baseline Survey of the Environment (G-BASE) programme. Geochemical data are available for soil samples for the Humber-Trent and East Anglia atlas areas (see the Geochemical atlas areas layer). Samples for East Midlands and part of Southeast England have been collected and are currently either undergoing analysis or data conditioning. More than twenty urban areas have also been sampled and top soil analyses are available for these urban areas (Belfast, Cardiff, Corby, Coventry, Derby, Doncaster, Glasgow, Hull, Ipswich, Leicester, Lincoln, Manchester, Mansfield, Northampton, Nottingham, Peterborough, Scunthorpe, Sheffield, Swansea, Stoke, Telford, Wolverhampton and York). Regional samples are collected at an average density of one site per 2 square kilometres, urban sampling is at a density of 4 samples per square kilometre. Top soil samples are collected at a depth of 5 - 20cm. It is sieved through a 2mm mesh and milled to less than 150 microns. The data include analyses for some or all of the following elements by XRFS: Mg, P, K, Ca, Ti, Mn, Fe, V, Cr, Co, Ba, Ni, Cu, Zn, Ga, As, Se, Rb, Sr, Y, Zr, Nb, Mo, Pb, Bi, Th, U, Ag, Cd, Sn, Sb, Cs, La, Ce, Ge, Sc, Se, Br, Hf, Ta, W, Tl, Te and I. Loss on Ignition (LOI) and pH (in a slurry of 0.01 M CaCl2 ) is now routinely determined on 50% of regional and all urban samples.