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.
50
datasets available to search
ShareScore release 0.9.0
Dataset results
50 results for “Interferometer”
TIMED TIMED Doppler Interferometer (TIDI) Zonal and Meridional Winds at 60-180 km, Version 0307, 82.28 s Data
The TIMED Doppler Interferometer, TIDI, instrument is a Fabry-Perot interferometer designed to measure zonal and meridional winds in the mesosphere and lower thermosphere. This TIMED TIDI data product contains neutral gas doppler temperature estimates and vector wind velocities estimated from line of sight inverted wind profiles based on rotational line measurements of molecular Oxygen, O₂, (0,0) by using the TIDI P9 763.78 nm filter. This Level 3 data set of wind vectors contains that are mapped onto fixed angle-along-the-track grids. Vertical resolution is ~2 km at the lower altitudes and 25 km at the thermosphere, with an accuracy that approaches approximately 3 m/sec. Each profile is annotated with ancillary data including profile position and processing status. * TIMED Rules of the Road * ----------------------- Users of TIMED data are asked to respect the following guidelines: * 1) Mission scientific and model results are open to all. * 2) Users should contact the principal investigator, PI, or designated team member of an instrument or modeling group early in an analysis project to discuss the appropriate use of instrument data or model results. This applies to TIMED mission team members, guest investigators, and other members of the scientific community or general public. * 3) Users that wish to publish the results derived from TIMED data should normally offer co-authorship to the PI or his/her designated team member. Co-authorship may be declined. Appropriate acknowledgement to institutions, personnel, and funding agencies should be given. * 4) Users should heed the caveats of investigators as to the interpretation and limitations of data or model results. Investigators supplying data or models may insist that such caveats be published, even if co-authorship is declined. Data and model version numbers should also be specified. * 5) Pre-prints of publications and conference abstracts should be widely distributed to interested parties within the mission and related projects. TIMED TIDI data are available from the following access URLs but the linked data are not stored by using the Common Data Format, CDF. Note that this SPASE Numerical Description only describes the MESSENGER Magnetometer data stored in Common Data Files. +------------------------------------------------------------------------------------------------+ Data Source Data Access URL ------------------------------------------------------------------------------------------------ University of Michigan ftp://tidi.engin.umich.edu/tidi/ High Altitude Observatory, HAO http://download.hao.ucar.edu/archive/tidi/plots/winds/zonave/ +------------------------------------------------------------------------------------------------+
ICON Michelson Interferometer for Global High-resolution Thermospheric Imaging viewing direction B
The MIGHTI instrument measures the horizontal wind speed and direction (the wind vector). Each MIGHTI unit measures the wind along its line of sight. MIGHTI uses two perpendicular fields of view nominally pointing 45 degrees and 135 degrees in azimuth from the spacecraft velocity (MIGHTI A and MIGHTI B). Combining data from both units, this 90 degrees separation between their views allows the wind vector to be determined. For the wind measurements MIGHTI observes the Doppler shift of the atomic oxygen red and green lines at 630.0 nm and 557.7 nm wavelength. The wavelength shift is measured using field-widened, temperature compensated Doppler Asymmetric Spatial Heterodyne (DASH) spectrometers, employing low order échelle gratings operating at two different orders for the different atmospheric lines. The temperature measurement is accomplished by a multichannel photometric measurement of the spectral shape of the molecular oxygen A-band around 762 nm wavelength. For each field of view, the signals of the two oxygen lines and the A-band are detected on different regions of a single, cooled, frame transfer charge coupled device (CCD) detector. On-board calibration sources are used to periodically quantify thermal drifts, simultaneously with observing the atmosphere.
ICON Michelson Interferometer for Global High-resolution Thermospheric Imaging viewing direction B
The MIGHTI instrument measures the horizontal wind speed and direction (the wind vector). Each MIGHTI unit measures the wind along its line of sight. MIGHTI uses two perpendicular fields of view nominally pointing 45 degrees and 135 degrees in azimuth from the spacecraft velocity (MIGHTI A and MIGHTI B). Combining data from both units, this 90 degrees separation between their views allows the wind vector to be determined. For the wind measurements MIGHTI observes the Doppler shift of the atomic oxygen red and green lines at 630.0 nm and 557.7 nm wavelength. The wavelength shift is measured using field-widened, temperature compensated Doppler Asymmetric Spatial Heterodyne (DASH) spectrometers, employing low order échelle gratings operating at two different orders for the different atmospheric lines. The temperature measurement is accomplished by a multichannel photometric measurement of the spectral shape of the molecular oxygen A-band around 762 nm wavelength. For each field of view, the signals of the two oxygen lines and the A-band are detected on different regions of a single, cooled, frame transfer charge coupled device (CCD) detector. On-board calibration sources are used to periodically quantify thermal drifts, simultaneously with observing the atmosphere.
ICON Michelson Interferometer for Global High-resolution Thermospheric Imaging Wind Vectors Green
The MIGHTI instrument measures the horizontal wind speed and direction (the wind vector). Each MIGHTI unit measures the wind along its line of sight. MIGHTI uses two perpendicular fields of view nominally pointing 45 degrees and 135 degrees in azimuth from the spacecraft velocity (MIGHTI A and MIGHTI B). Combining data from both units, this 90 degrees separation between their views allows the wind vector to be determined. For the wind measurements MIGHTI observes the Doppler shift of the atomic oxygen red and green lines at 630.0 nm and 557.7 nm wavelength. The wavelength shift is measured using field-widened, temperature compensated Doppler Asymmetric Spatial Heterodyne (DASH) spectrometers, employing low order échelle gratings operating at two different orders for the different atmospheric lines. The temperature measurement is accomplished by a multichannel photometric measurement of the spectral shape of the molecular oxygen A-band around 762 nm wavelength. For each field of view, the signals of the two oxygen lines and the A-band are detected on different regions of a single, cooled, frame transfer charge coupled device (CCD) detector. On-board calibration sources are used to periodically quantify thermal drifts, simultaneously with observing the atmosphere.
ICON Michelson Interferometer for Global High-resolution Thermospheric Imaging viewing direction A
The MIGHTI instrument measures the horizontal wind speed and direction (the wind vector). Each MIGHTI unit measures the wind along its line of sight. MIGHTI uses two perpendicular fields of view nominally pointing 45 degrees and 135 degrees in azimuth from the spacecraft velocity (MIGHTI A and MIGHTI B). Combining data from both units, this 90 degrees separation between their views allows the wind vector to be determined. For the wind measurements MIGHTI observes the Doppler shift of the atomic oxygen red and green lines at 630.0 nm and 557.7 nm wavelength. The wavelength shift is measured using field-widened, temperature compensated Doppler Asymmetric Spatial Heterodyne (DASH) spectrometers, employing low order échelle gratings operating at two different orders for the different atmospheric lines. The temperature measurement is accomplished by a multichannel photometric measurement of the spectral shape of the molecular oxygen A-band around 762 nm wavelength. For each field of view, the signals of the two oxygen lines and the A-band are detected on different regions of a single, cooled, frame transfer charge coupled device (CCD) detector. On-board calibration sources are used to periodically quantify thermal drifts, simultaneously with observing the atmosphere.
ICON Michelson Interferometer for Global High-resolution Thermospheric Imaging viewing direction A
The MIGHTI instrument measures the horizontal wind speed and direction (the wind vector). Each MIGHTI unit measures the wind along its line of sight. MIGHTI uses two perpendicular fields of view nominally pointing 45 degrees and 135 degrees in azimuth from the spacecraft velocity (MIGHTI A and MIGHTI B). Combining data from both units, this 90 degrees separation between their views allows the wind vector to be determined. For the wind measurements MIGHTI observes the Doppler shift of the atomic oxygen red and green lines at 630.0 nm and 557.7 nm wavelength. The wavelength shift is measured using field-widened, temperature compensated Doppler Asymmetric Spatial Heterodyne (DASH) spectrometers, employing low order échelle gratings operating at two different orders for the different atmospheric lines. The temperature measurement is accomplished by a multichannel photometric measurement of the spectral shape of the molecular oxygen A-band around 762 nm wavelength. For each field of view, the signals of the two oxygen lines and the A-band are detected on different regions of a single, cooled, frame transfer charge coupled device (CCD) detector. On-board calibration sources are used to periodically quantify thermal drifts, simultaneously with observing the atmosphere.
IRAM Plateau de Bure Interferometer Observation Log
This table contains the IRAM Plateau de Bure Interferometer observation log. The Institut de Radio Astronomie Millimetrique (IRAM) was founded in 1979 and is operated as a French-German-Spanish collaboration. Its partner institutes are the CNRS (Centre National de la Recherche Scientifique, France), the MPG (Max Planck Gesellschaft, Germany), and the IGN (Instituto Geografico Nacional, Spain). The principal activity of IRAM is the study of cold matter (molecular gas and dust) in the solar system, in our Galaxy, and out to cosmological distances, in order to determine its composition, density, mass, temperature, and kinematics. IRAM operates two observatories at millimeter wavelengths which are open to the international astronomical community: the 30-m single-dish telescope on Pico Veleta (2850 m), Spain, and the six-antenna interferometer on the Plateau de Bure (2550 m) in France. Both sites are at high altitude to reduce the absorption by water vapor. The observatories are supported by the IRAM offices and laboratories in Granada and Grenoble. The observation log included here concerns the Plateau de Bure Interferometer (PdBI) and summarizes the observations made there between December 1, 1990, and March 31, 2017, inclusive. No observations were done by the PdBI during the periods 1999-Sep-30 to 2000-Dec-03 and 2006-Sep-25 to 2007-Jan-18 (installation of the new receiver), notice. The observation log for the 30-m telescope is available as the HEASARC database table <a href="/W3Browse/ground-based/iram30mlog.html">IRAM30MLOG</a>, and the observation log for NOEMA (the NOrthern Extended Millimeter Array), the successor to the Plateau de Bure observatory, is available as the HEASARC database table <a href="/W3Browse/ground-based/iramnoelog.html">IRAMNOELOG</a>. For more information on IRAM, see <a href="http://www.iram-institute.org/">the IRAM home page</a>. This table was originally ingested by the HEASARC in November 2005. It is based on the CDS table B/iram/, files pdbi.dat and pdbi_pi.dat. It was last updated in July 2019, based on an updated version of these tables which were also obtained from the CDS. This is a service provided by NASA HEASARC .
ICON Michelson Interferometer for Global High-resolution Thermospheric Imaging Wind Vectors Red
The MIGHTI instrument measures the horizontal wind speed and direction (the wind vector). Each MIGHTI unit measures the wind along its line of sight. MIGHTI uses two perpendicular fields of view nominally pointing 45 degrees and 135 degrees in azimuth from the spacecraft velocity (MIGHTI A and MIGHTI B). Combining data from both units, this 90 degrees separation between their views allows the wind vector to be determined. For the wind measurements MIGHTI observes the Doppler shift of the atomic oxygen red and green lines at 630.0 nm and 557.7 nm wavelength. The wavelength shift is measured using field-widened, temperature compensated Doppler Asymmetric Spatial Heterodyne (DASH) spectrometers, employing low order échelle gratings operating at two different orders for the different atmospheric lines. The temperature measurement is accomplished by a multichannel photometric measurement of the spectral shape of the molecular oxygen A-band around 762 nm wavelength. For each field of view, the signals of the two oxygen lines and the A-band are detected on different regions of a single, cooled, frame transfer charge coupled device (CCD) detector. On-board calibration sources are used to periodically quantify thermal drifts, simultaneously with observing the atmosphere.
ICON Michelson Interferometer for Global High-resolution Thermospheric Imaging Viewing Direction B Temperature
MIGHTI samples the O2 A band spectral region at five different wavelengths in order to both measure the shape of the band and to specify a background radiance that is subtracted from the signal. The wavelengths of the filter passbands are selected to maximize the sensitivity to lower thermospheric temperature variations. The temperature measurement is accomplished by a multichannel photometric measurement of the spectral shape of the molecular oxygen A-band around 762 nm wavelength. For each field of view, the signals of the two oxygen lines and the A-band are detected on different regions of a single, cooled, frame transfer charge coupled device (CCD) detector. Two filter channels sample either end of the band to define a background (754.1 nm and 780.1 nm) and three more sample its shape (760.0 nm, 762.8 nm and 765.2 nm). Using three filters that sample the band shape allows the simultaneous retrieval of the atmospheric temperature and common shifts in the center wavelengths of the pass bands due to thermal drifts of the filters. On-board calibration sources are used to periodically quantify thermal drifts, simultaneously with observing the atmosphere.
DE 2 Fabry-Perot Interferometer (FPI), Thermospheric Neutral Gas Density, Meridional Wind, and Temperature, 8-sec data
The Fabry-Perot Interferometer, FPI, was a High-Resolution Remote Sensing Instrument designed to measure the Thermospheric Temperature, Meridional Wind, and Density of the following Metastable Atoms: Atomic Oxygen, Singlet S and D, and the 2P State of Ionic Atomic Oxygen. The FPI performed a Wavelength Analysis on the Light detected from the Thermospheric Emission Features by spatially scanning the Interference Fringe Plane with a Multichannel Array Detector. The Wavelength Analysis characterized the Doppler Line Profile of the emitting Species. A Sequential Altitude Scan performed by a Commandable Horizon Scan Mirror provided a Cross-Sectional View of the Thermodynamic and Dynamic State of the Thermosphere below the DE 2 Orbit. The Information obtained from this Investigation was used to Study the Dynamic Response of the Thermosphere to the Energy Sources caused by Magnetospheric Electric Fields and the Absorption of Solar Ultraviolet Light in the Thermosphere. The Instrument was based on the Visible Airglow Experiment, VAE, used in the AE Program. The Addition of a Scanning Mirror, the Fabry-Perot Etalon, an Image Plane Detector, and a Calibration Lamp were the Principal Differences. Interference Filters isolated Lines at 5577, 6300, 7320, 5896, and 5200, in Angstroms. The FPI had a Field of View of 0.53°, Half-Cone Angle. More Details are found in P. B. Hays et al., Space Sci. Instrum., 5(4), 395, 1981. From February 16, 1982 to September 11, 1982 the DE Satellite was inverted and the FPI measured Galactic Emissions. NOTE: Animations of DE2-FPI Science Products have been created as Daily Summary Files. The Animations contain Binned Averages displayed as a Color Code against a Geographic Background. The Bin Sizes are 7.5° Latitude and 24.0° Longitude. The Longitude Bin corresponds to the approximate Separation of adjacent Orbits, assuming that DE2 completed 15 Orbits per Day. The Animations are divided by Day, 06-18 LST, and Night, 18-06 LST, where LST is Local Standard Time. All Summary File Information and Animations employ Spacecraft Orbital Attitude Data. Users should note 1, that the DE2-FPI Experiment acquired Airglow Spectra by imaging the Terrestrial Limb below and ahead of the Spacecraft at an approximate Tangent Altitude of 250 km, 2, All Airglow Spectra were acquired while the DE2 Spacecraft orbited in it's Normal Configuration, which corresponded to Calendar Months August to February in 1981 to 1982 and n 1982 to 1983; 3, The Orbital Inclination of DE2 was 90° implying that DE2-FPI always viewed Ahead along the Meridian; 4, And that DE2 flew in an Elliptical Orbit with Perigee of 305 km and Apogee of 1300 km at Launch ans the Attitude of DE2 for each FPI Measurement is included with each reduced Data Point permitting Users to determine the Tangent Latitude corresponding to the 250 km Terrestrial Airglow Limb. The three GIF Animations are: 1. FPI_brightness.gif, which documents the OI, 630.0 nm,, Column Brightness in Units of log10 Rayleighs. Note different Scales for Day and Night. 2. FPI_temperature.gif, which documents the Neutral Thermosphere Temperature in Units of °Kelvin. 3. FPI_wind.gif, which documents the Line of Sight Neutral Wind Component in Units of m/s. The Wind Direction is positive when the Wind blows away from the approaching Spacecraft.
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.