Find research datasets worth reusing
Search datasets from major research repositories and use ShareScore to quickly assess how well each record supports discovery, access, and reuse.
571
datasets available to search
ShareScore release 0.9.0
Dataset results
571 results for “Brightness”
SMAPVEX16 Manitoba PALS Brightness Temperature and Soil Moisture Data V001
This product contains data derived from permanent in situ soil stations and observations by the Passive Active L-band System (PALS) microwave aircraft instrument. The PALS instrument was mounted to a DC-3 aircraft, which flew six parallel flight lines at an altitude of 3000 m in order to map a 26 km x 48 km domain in Manitoba, Canada. Nine permanent soil stations were distributed throughout this same area. The soil characteristics included in this data set are volumetric soil moisture, vertically and horizontally polarized brightness temperature, effective soil temperature, effective vegetation temperature, vegetation water content, land cover classification, sand and clay fraction, and volumetric soil moisture uncertainty estimates.
CLASIC07 PALS Brightness Temperature Data V001
This data set contains brightness temperature data obtained by the Passive Active L-band System (PALS) microwave aircraft radiometer instrument as part of the Cloud and Land Surface Interaction Campaign 2007 (CLASIC07).
AMSR-E/AMSR2 Unified L3 Daily 12.5 km Brightness Temperatures, Sea Ice Concentration, Motion & Snow Depth Polar Grids V001
This data set reports average daily horizontally and vertically polarized brightness temperatures; sea ice concentrations; and snow depths over sea ice on 12.5 km resolution north and south polar stereographic grids. Ungridded sea ice motion data are also available for the Arctic. The data are derived from observations acquired by the Advanced Microwave Scanning Radiometer (AMSR) for EOS (AMSR-E) and AMSR2 instruments that have been spatially resampled by the Japan Aerospace Exploration Agency (JAXA) to unify the AMSR-E and AMSR2 missions. Brightness temperatures are available at 18.7 GHz, 23.8 GHz, 36.5 GHz and 89.0 GHz for ascending and descending orbits, and as a single daily average. Sea ice concentrations are generated with the Enhanced NASA Team (NT2) algorithm; a separate variable reports the daily sea ice concentration difference between the legacy AMSR Basic Bootstrap Algorithm (ABA) and the NT2.
SnowEx17 Radiometrics Surface-Based Radiometer Brightness Temperatures V001
This data set consists of surface-based radiometer (SBR) brightness temperatures of the snow surface and vegetation at Grand Mesa, CO, USA, acquired during NASA's 2017 SnowEx campaign. Four SBRs were deployed in the field and obtained measurements at 89, 37, 19, and 10.67 GHz in both vertical (V-pol) and horizontal (H-pol) polarizations. Data are available for 37 locations across Grand Mesa collected over five days in February, 2017. They include both 2-4 minute observations and 20 minute, continuous measurements during surface melt, with the latter designed to capture the brightness temperature increase caused by the presence of liquid water in the snow. This data set also contains snowfork measurements of snow wetness for 13 sites.
SMAP Enhanced L1C Radiometer Half-Orbit 9 km EASE-Grid Brightness Temperatures V004
This enhanced Level-1C (L1C) product contains calibrated and geolocated brightness temperatures acquired by the Soil Moisture Active Passive (SMAP) radiometer during 6:00 a.m. descending and 6:00 p.m. ascending half-orbit passes. This product is derived from SMAP Level-1B (L1B) interpolated antenna temperatures. Backus-Gilbert optimal interpolation techniques are used to extract enhanced information from SMAP antenna temperatures before they are converted to brightness temperatures. The resulting brightness temperatures are posted to an Earth-fixed, 9 km Equal-Area Scalable Earth Grid, Version 2.0 (EASE-Grid 2.0) in three projections: global cylindrical, Northern Hemisphere azimuthal, and Southern Hemisphere azimuthal.
AMPR BRIGHTNESS TEMPERATURE (TB) TOGA COARE V2
The Advanced Microwave Precipitation Radiometer (AMPR) data set was part of the atmospheric measurements collected during the intensive observation period of the Tropical Ocean Global Atmosphere-Coupled Ocean Atmosphere Response Experiment (TOGA COARE). AMPR brightness temperature data were collected at a combination of frequencies (10.7, 19.35, 37.1, and 85.5 GHz) and for the period Jan. 12, 1993 - Feb. 25, 1993. The TOGA COARE geographic domain pertinent to the AMPR data set was from the equator to 21 S latitude and 145 E - 161 E longitude.
AMPR TEFLUN-A BRIGHTNESS TEMPERATURE (TB) V1
The Advanced Microwave Precipitation Radiometer (AMPR) was deployed during the Texas-Florida Underflights (TEFLUN-A); the first of three TRMM ground validation missions. AMPR data were collected at four microwave frequencies (10.7, 19.35, 37.1 and 85.5 GHz) for the period of 15 April 1998 through 04 May 1998. The TEFLUN-A mission studied convection over sub-tropical land and ocean regions within the range of research-quality radar, lightning, radiosonde, and raingage sites in Florida and Texas.
XMM-Newton Bright Serendipitous Survey
We present here the XMM-Newton Bright Serendipitous Survey, composed of two flux-limited samples: the XMM-Newton Bright Source Sample (BSS, hereafter) and the XMM-Newton "Hard" Bright Source Sample (HBSS, hereafter). The selection criteria for these two sample, 0.5 - 4.5 keV count rate >= 0.01 ct/s (BSS) and 4.5 - 7.5 keV count rate >= 0.002 ct/s (HBSS), correspond to a flux limit of f<sub>X</sub> ~ 7 x 10<sup>-14</sup> erg/cm<sup>2</sup>/s in the 0.5 - 4.5 keV and 4.5 - 7.5 keV energy bands, respectively, for sources with power-law spectra with energy spectral indices between 0.7 and 0.8. This table contains the basic data on a complete sample of 400 X-ray sources (389 of them belong to the BSS, 67 to the HBSS, with 56 X-ray sources in common) derived from the analysis of 237 suitable XMM-Newton fields (211 for the HBSS). At the flux limit of the survey, it covers a survey area of 28.10 (25.17 for the HBSS) square degrees. The extragalactic number-flux relationships (in the 0.5 - 4.5 keV and in the 4.5 - 7.5 keV energy bands) are in good agreement with previous and new results making the authors confident in the correctness of the data selection and their analysis. This table was created by the HEASARC in October 2006 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/428/383">CDS Catalog J/A+A/428/383</a> (the merger of files table3.dat and table4.dat). This is a service provided by NASA HEASARC .
SMAP Enhanced L1C Radiometer Half-Orbit 9 km EASE-Grid Brightness Temperatures V004
This enhanced Level-1C (L1C) product contains calibrated and geolocated brightness temperatures acquired by the Soil Moisture Active Passive (SMAP) radiometer during 6:00 a.m. descending and 6:00 p.m. ascending half-orbit passes. This product is derived from SMAP Level-1B (L1B) interpolated antenna temperatures. Backus-Gilbert optimal interpolation techniques are used to extract enhanced information from SMAP antenna temperatures before they are converted to brightness temperatures. The resulting brightness temperatures are posted to an Earth-fixed, 9 km Equal-Area Scalable Earth Grid, Version 2.0 (EASE-Grid 2.0) in three projections: global cylindrical, Northern Hemisphere azimuthal, and Southern Hemisphere azimuthal.
SMAP L1B Radiometer Half-Orbit Time-Ordered Brightness Temperatures V006
This Level-1B (L1B) product provides calibrated estimates of time-ordered geolocated brightness temperatures measured by the Soil Moisture Active Passive (SMAP) passive microwave radiometer. SMAP L-band brightness temperatures are referenced to the Earth's surface with undesired and erroneous radiometric sources removed.
SMAPVEX16 Iowa PALS Brightness Temperature and Soil Moisture Data V001
This product contains data derived from permanent in situ soil stations and observations by the Passive Active L-band System (PALS) microwave aircraft instrument. The PALS instrument was mounted to a DC-3 aircraft, which flew six parallel flight lines at an altitude of 3000 m in order to map a study area in South Fork, Iowa, United States. A total of 20 soil stations were distributed throughout this same area. The soil characteristics included in this data set are volumetric soil moisture, vertically and horizontally polarized brightness temperature, effective soil temperature, effective vegetation temperature, vegetation water content, land cover classification, sand and clay fraction, and volumetric soil moisture uncertainty estimates.
Australia Telescope Low-Brightness Survey Source Catalog
The Australia Telescope Low-brightness Survey (ATLBS) regions have been mosaic imaged at a radio frequency of 1.4 GHz with 6 arcseconds angular resolution and 72 microJansky per beam (µJy/beam) rms noise. The images (centered at RA 00<sup>h</sup> 35<sup>m</sup> 00<sup>s</sup>, Dec -67<sup>o</sup> 00' 00" and RA 00<sup>h</sup> 59<sup>m</sup> 17<sup>s</sup>, Dec -67<sup>o</sup> 00' 00", J2000 epoch) cover 8.42 deg<sup>2</sup> sky area and have no artifacts or imaging errors above the image thermal noise. Multi-resolution radio and optical r-band images (made using the 4 m CTIO Blanco telescope) were used to recognize multi-component sources and prepare a source list of 1366 1.4-GHZ sources; the detection threshold was 0.38 mJy in a low-resolution radio image made with beam FWHM of 50 arcseconds. Radio source counts in the flux density range 0.4-8.7 mJy are estimated, with corrections applied for noise bias, effective area correction, and resolution bias. The resolution bias is mitigated using low-resolution radio images, while effects of source confusion are removed by using high-resolution images for identifying blended sources. Below 1 mJy the ATLBS counts are systematically lower than the previous estimates. Showing no evidence for an upturn down to 0.4 mJy, they do not require any changes in the radio source population down to the limit of the survey. The work suggests that automated image analysis for counts may be dependent on the ability of the imaging to reproduce connecting emission with low surface brightness and on the ability of the algorithm to recognize sources, which may require that source finding algorithms effectively work with multi-resolution and multi-wavelength data. The work underscores the importance of using source lists - as opposed to component lists - and correcting for the noise bias in order to precisely estimate counts close to the image noise and determine the upturn at sub-mJy flux density. This table was created by the HEASARC in April 2013 based on an electronic version of Table 2 from the reference paper that was obtained from the ApJ web site.. This is a service provided by NASA HEASARC .
MER2 Mini-TES Derived Brightness Temperature Data Bundle
This bundle contains brightness temperature data from the Mini-TES instrument on Mars Exploration Rover 2 (Spirit).
CASSINI SATURN UVIS SOLAR STELLAR BRIGHTNESS TIME SERIES 1.2
Photometric observations of stellar occultations by Saturnian rings, satellites, atmospheres, and Jovian atmosphere.
Single-cell RNA sequencing of tobacco Bright Yellow-2 cell line reveals heterogeneity in cell cycle phase
GEO Series GSE193131. Nicotiana tabacum. 8 samples. Type: Expression profiling by high throughput sequencing.
Optical spectra of Halpha-bright knots in Stephan's Quintet
<p>Optical spectra of Hα-bright knots in the intragroup medium of Stephan's Quintet, an interacting compact galaxy group featuring a string X-ray shock. Provided in HDF5 and FITS, the astronomical FITS file transfer format. </p>
Interchromophoric Interactions Determine the Maximum Brightness Density in DNA Origami Structures
<p>An ideal point light source is as small and as bright as possible. For fluorescent point light sources, homogeneity of the light sources is important as well as that the fluorescent units inside the light source maintain their photophysical properties, which is compromised by dye aggregation. Here we propose DNA origami as a rigid scaffold to arrange dye molecules in a dense pixel array with high control of stoichiometry and dye–dye interactions. In order to find the highest labeling density in a DNA origami structure without influencing dye photophysics, we alter the distance of two ATTO647N dyes in single base pair steps and probe the dye–dye interactions on the single-molecule level. For small distances strong quenching in terms of intensity and fluorescence lifetime is observed. With increasing distance, we observe reduced quenching and molecular dynamics. However, energy transfer processes in the weak coupling regime still have a significant impact and can lead to quenching by singlet-dark-state-annihilation. Our study fills a gap of studying the interactions of dyes relevant for superresolution microscopy with dense labeling and for single-molecule biophysics. Incorporating these findings in a 3D DNA origami object will pave the way to bright and homogeneous DNA origami nanobeads.</p>
A novel method to obtain three-dimensional urban surface temperature from ground-based thermography - Figure 10 median brightness temperatures
<p>Median brightness temperatures as shown in Figure 10 of Morrison et al. (2018) <em>A novel method to obtain three-dimensional urban surface temperature from ground-based thermography </em><a href="https://doi.org/10.1016/j.rse.2018.05.004">https://doi.org/10.1016/j.rse.2018.05.004</a></p> <p>Details on the files can be found below. Further details can be found in the linked paper and references. </p> <p><strong>Thermal infrared camera brightness temperature measurements</strong></p> <p><strong>02082014_COSMOTIRsunShade.csv:</strong><br> <strong>TIME</strong>: Local time. Timestep indicates end of 60 min aggregation interval using 1 min image samples.<br> <strong>class</strong>: sunlit (observed surface is in direct sun) or shaded (observed surface is in shade)<br> <strong>median_Tb_K</strong>: median brightness temperature across all images and image pixels for the given class and timestep (K)</p> <p><strong>02082014_COSMOTIRorientations.csv:</strong><br> <strong>TIME</strong>: Local time. Timestep indicates end of 60 min aggregation interval using 1 min image samples.<br> <strong>class</strong>: sunlit (observed surface is in direct sun) or shaded (observed surface is in shade) also stratified by surface orientation i.e. <sun_status>_<orientation><br> <strong>median_Tb_K</strong>: median brightness temperature across all images and image pixels for the given class and timestep (K) </p> <p><strong>002082014_COSMOTIRorientationsAndSunShade.csv:</strong><br> <strong>TIME</strong>: Local time. Timestep indicates end of 60 min aggregation interval using 1 min image samples.<br> <strong>class</strong>: sunlit (observed surface is in direct sun) or shaded (observed surface is in shade) also stratified by surface orientation i.e. <sun_status>_<orientation><br> <strong>median_Tb_K</strong>: median brightness temperature across all images and image pixels for the given class and timestep (K) </p> <p> </p> <p><strong>Supplementary standard meteorological and radiation measurements.</strong></p> <p><strong>MET_RAD_Morrisonetal_2018.csv</strong>:</p> <p><strong>TIME</strong>: Local time. 10 min end of average of 1 min samples.<br> <strong>press</strong>: Atmospheric pressure (hPa) (site: JMA Kumagaya AMeDAS)<br> <strong>Tair</strong>: Air temperature (degrees celsius) (site: JMA Kumagaya AMeDAS)<br> <strong>RH</strong>: Relative humidity (%) (site: JMA Kumagaya AMeDAS)<br> <strong>WS</strong>: Wind speed (m/s) (site: JMA Kumagaya AMeDAS)<br> <strong>SWdn_direct</strong>: Direct incoming shortwave radiation (W m-2) (site: COSMO, Eko MS-56)<br> <strong>SWdn</strong>: Hemispherical incoming shortwave radiation (W m-2) (site: COSMO, Eko MR-40)<br> <strong>SWup</strong>: Hemispherical outgoing shortwave radiation (W m-2) (site: COSMO, Eko MR-40)<br> <strong>LWdn</strong>: Hemispherical incoming longwave radiation (W m-2) (site: COSMO, Eko MR-40)<br> <strong>LWup</strong>: Hemispherical outgoing longwave radiation (W m-2) (site: COSMO, Eko MR-40)</p> <p> </p>
The phase-shifting effect of bright light exposure on circadian rhythmicity in the human transcriptome
GEO Series GSE122725. Homo sapiens. 141 samples. Type: Expression profiling by array.
VOYAGER 1&2 JUPITER BRIGHTNESS NORTH/SOUTH MAP SET V1.0
This data set contains Voyager 1 and 2 measurements of the brightness of Jupiter at H Lyman alpha and in the H2 Lyman and Werner bands shortward of H Lyman alpha. Pointing has been corrected by the C-Smithing process, and these data were derived from the pre-encounter North-South Map sequences. In this sequence, the UVS field of view was located near the central meridian of the planet. The field of view stepped slowly from north to south, and then rapidly repositioned to the north. These scans were repeated until all Jovian longitudes had been sampled. Coverage in longitude was not continuous in time. Rather, some longitude ranges were covered on the preceding or following rotation of Jupiter.
ScienceDex guides
Understand access before you commit
These curated guides explain access requirements, typical timelines, costs, and reuse considerations for widely used research datasets.
Allen Brain Atlas
Allen Brain Atlas is an Allen Institute collection of brain map atlases, datasets, APIs, and analysis tools covering mouse, human, and non-human primate brain resources.
Annotated Behaviour and Observability Dataset (ABODe)
ABODe is a University of Edinburgh DataShare dataset for behavior classification in group-housed mice using home-cage video, identities, bounding boxes, ground-plate positions, and annotator labels.
DANDI Archive for NWB datasets
DANDI is a BRAIN Initiative archive for publishing and sharing neurophysiology data, including electrophysiology, optophysiology, and behavioral data packaged as NWB and related standards.
International Brain Laboratory public data
The International Brain Laboratory public data releases expose standardized mouse decision-making experiments, including Neuropixels recordings, widefield calcium imaging, behavior, and session metadata accessed through the ONE API.
OpenNeuro
OpenNeuro is a free, open platform for sharing neuroimaging datasets, with public search, dataset pages, and download paths for web, S3, DataLad, and the OpenNeuro CLI.