cometadata/datacite-titles-descriptions-related-identifiers huggingface dataset:
DOI: 10.15468/dl.x6466z
title: Occurrence Download

description: A dataset containing 29 species occurrences available in GBIF matching the query:
{
 "and" : [
 "CoordinateUncertaintyInMeters 0.0-1000.0",
 "Geometry POLYGON((-6.25617 41.0851,27.48128 41.0851,27.48128 72.26782,-6.25617 72.26782,-6.25617 41.0851))",
 "HasCoordinate is true",
 "HasGeospatialIssue is false",
 "TaxonKey is Arabis sudetica"
 ]
}

 The dataset includes 29 records from 7 constituent datasets; see https://api.gbif.org/v1/occurrence/download/0063218-251120083545085/datasets/export for details.
 
Data from some individual datasets included in this download may be licensed under less restrictive terms.
DOI: 10.25574/29826
title: Chandra X-ray Observatory ObsId 29826

description: Chandra Observations of a Source-Rich region in NGC 891
DOI: 10.5281/zenodo.18015534
title: Spontaneous Raman data (514 nm) for "Raman Spectral Analysis in the CHx-Stretching Region as a Guiding Beacon for Non-Targeted, Disruption-Free Monitoring of Germination and Biofilm Formation in the Green Seaweed Ulva"

description: The dataset contains exported raw and processed spontaneous Raman spectroscopy data acquired with a WITec Alpha300 system (514 nm excitation). The measurements correspond to the study by:

C. Schultz, D. Zopf, A. Holzinger, A. Silge, T. Meyer-Zedler, M. Schmitt, T. Wichard, J. Popp, ChemPhysChem 2024, 25, e202400173. https://doi.org/10.1002/cphc.202400173

The zip-file is structured as follows:





0_axenic – Exported raw and processed Raman data from axenic cultures of Ulva mutabilis




1_MS2 – Exported raw and processed Raman data from cocultures of Ulva mutabilis with MS2 bacteria




2_MS6 – Exported raw and processed Raman data from cocultures of Ulva mutabilis with MS6 bacteria




3_MS6MS2 – Exported raw and processed Raman data from tripartite cultures of Ulva mutabilis with MS2 and MS6 bacteria




4_Processing_scripts – Python scripts used for data processing and figure generation. Script A requires pre–wavenumber-corrected data (AAP correction and x-axis harmonization/interpolation), identified by the suffix _Rcorr in the filename. These corrected data are included in the dataset.




5_main_manuscript_figures – Collection of figures from the main manuscript
DOI: 10.5281/zenodo.18015535
title: Spontaneous Raman data (514 nm) for "Raman Spectral Analysis in the CHx-Stretching Region as a Guiding Beacon for Non-Targeted, Disruption-Free Monitoring of Germination and Biofilm Formation in the Green Seaweed Ulva"

description: The dataset contains exported raw and processed spontaneous Raman spectroscopy data acquired with a WITec Alpha300 system (514 nm excitation). The measurements correspond to the study by:

C. Schultz, D. Zopf, A. Holzinger, A. Silge, T. Meyer-Zedler, M. Schmitt, T. Wichard, J. Popp, ChemPhysChem 2024, 25, e202400173. https://doi.org/10.1002/cphc.202400173

The zip-file is structured as follows:





0_axenic – Exported raw and processed Raman data from axenic cultures of Ulva mutabilis




1_MS2 – Exported raw and processed Raman data from cocultures of Ulva mutabilis with MS2 bacteria




2_MS6 – Exported raw and processed Raman data from cocultures of Ulva mutabilis with MS6 bacteria




3_MS6MS2 – Exported raw and processed Raman data from tripartite cultures of Ulva mutabilis with MS2 and MS6 bacteria




4_Processing_scripts – Python scripts used for data processing and figure generation. Script A requires pre–wavenumber-corrected data (AAP correction and x-axis harmonization/interpolation), identified by the suffix _Rcorr in the filename. These corrected data are included in the dataset.




5_main_manuscript_figures – Collection of figures from the main manuscript
DOI: 10.48322/hwg4-hw39
title: ICON Extreme Ultraviolet Spectrograph Images 
title: EUV Images

description: This describes the data produce for ICON EUV Daytime O+ (DP 2.6), which is in NetCDF4 format. These files are named ICON_L2-6_EUV_YYYY-MM-DD_vXXrZZ.NC, where YYYY-MM-DD is the year month day and VXX shows the version number and rZZ shows the revision number of this file.  Each individual file nominally contains 1 day (24 hours) of data. The L2 EUV Daytime files are produced from the L1 EUV files, and their primary data product is the O+ profile derived from a retrieval that is detailed in a paper: https://doi.org/10.1007/s11214-017-0385-1. In addition, many other parameters and geophysical data products are included in the file.  The data are identified in one of 3 var_types: data – which contains the primary data product; support data – which contains parameters used in the retrieval such as geometry etc. that may also be useful in any analysis of this data; and ignore_data – which are recorded for debugging purposes and should not be used for publication without detailed discussion with the ICON team. The dimensions of the data also indicate its type.  For example, anything with epoch as a dimension means there is 1 value corresponding to each instrument exposure. Anything with dimension Input_data corresponds to the input data, passed from Level 1.  Anything with a dimension of model refers to the forward model parameters used as part of the inversion. Anything with dimension altitude corresponds to the altitude grid used for the inverted parameters.
DOI: 10.48322/w3qs-ed95
title: ICON The Far Ultra Violet Imaging Spectrograph Dayside Images 
title: FUV Dayside Images

description: The FUV instrument takes 2D images of the Earth’s horizon in the Far ultraviolet. The imager is pointing approximately 90 degrees to the spacecraft motion, similar to looking out of the side window of a car as it drives down the road. Onboard electronics read the image 8 times per second and perform Time Delay Integration (TDI) to remove the motion-blur from the images. A turret is used to steer the field of view of the instrument left to right to ensure it always looks along the magnetic meridian (towards the magnetic pole).
	  
	  This describes the data product for ICON FUV Daytime O/N2 (DP 2.4). The ratio of oxygen to nitrogen in the thermosphere is obtained from the two channels of ICON FUV instrument data in, through an inversion process described in https://doi.org/10.1007/s11214-018-0477-6.  The L2 FUV Daytime files are produced from the L1 FUV files.
DOI: 10.48322/4vx2-1c67
title: ICON The Far Ultra Violet Imaging Spectrograph Nightside Images 
title: FUV Nightside Images

description: The FUV instrument takes 2D images of the Earth’s horizon in the Far ultraviolet. The imager is pointing approximately 90 degrees to the spacecraft motion, similar to looking out of the side window of a car as it drives down the road. Onboard electronics read the image 8 times per second and perform Time Delay Integration (TDI) to remove the motion-blur from the images. A turret is used to steer the field of view of the instrument left to right to ensure it always looks along the magnetic meridian (towards the magnetic pole).
DOI: 10.48322/bwjz-nk36
title: ICON The Far Ultra Violet Imaging Spectrograph Day Limb Images
title: FUV Day Limb Images

description: The FUV instrument takes 2D images of the Earth’s horizon in the Far ultraviolet. 
	  The imager is pointing approximately 90 degrees to the spacecraft motion, similar to looking out 
	  of the side window of a car as it drives down the road. Onboard electronics read the CCD detectors 8 times per
	  second and collect the data into radiance profiles every 12 seconds. The calibrated level 1 radiances
	  and Level 1 ancillary spacecraft data are combined in a limb retrieval to produce the level 2.4 O/N2 limb product.
DOI: 10.48322/2mv5-xy46
title: ICON Ion Velocity Meter (IVM) A Data
title: IVM A Data

description: The IVM consists of two planar thermal ion sensors, a retarding potential analyzer (RPA) and an ion drift meter (IDM).
DOI: 10.48322/07nf-qa27
title: ICON Michelson Interferometer for Global High-resolution Thermospheric Imaging viewing direction A
title: MIGHTI A LOS Green

description: 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.
DOI: 10.48322/1dta-a634
title: ICON Ion Velocity Meter (IVM) B Data
title: IVM B Data

description: The IVM consists of two planar thermal ion sensors, a retarding potential analyzer (RPA) and an ion drift meter (IDM).
DOI: 10.48322/mjdw-td24
title: ICON Michelson Interferometer for Global High-resolution Thermospheric Imaging viewing direction A
title: MIGHTI A LOS Red

description: 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.
DOI: 10.48322/d0qk-qc73
title: ICON Michelson Interferometer for Global High-resolution Thermospheric Imaging Viewing Direction A Temperature
title: MIGHTI A Temperature

description: 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.
DOI: 10.48322/s7j9-kn77
title: ICON Michelson Interferometer for Global High-resolution Thermospheric Imaging viewing direction B
title: MIGHTI B LOS Green

description: 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.
DOI: 10.48322/4fvv-ka29
title: ICON Michelson Interferometer for Global High-resolution Thermospheric Imaging viewing direction B
title: MIGHTI B LOS Red

description: 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.
DOI: 10.48322/vtce-7y29
title: ICON Michelson Interferometer for Global High-resolution Thermospheric Imaging Wind Vectors Green
title: MIGHTI Wind Vectors Green

description: 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.
DOI: 10.48322/zrhc-pb76
title: ICON Michelson Interferometer for Global High-resolution Thermospheric Imaging Viewing Direction B Temperature
title: MIGHTI B Temperature

description: 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.
DOI: 10.48322/pyfw-zv85
title: ICON Michelson Interferometer for Global High-resolution Thermospheric Imaging Wind Vectors Red
title: MIGHTI Wind Vectors Red

description: 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.
DOI: 10.48322/v9pw-wd37
title: GPS Deduced ROTI Index, Standard Deviation of the Rate of Change of the Total Electron Content (TEC), World Maps and Movies, 15 min Data

description: The ROTI Index is the Standard Deviation of the Rate of Change of the Total Electron Content, TEC, during a 15 min Interval. The TEC Values are measured between a Global Positioning Satellite, GPS, and Ground Receiver Station.
DOI: 10.48322/xsb1-nc45
title: IMAGE Extreme UltraViolet (EUV) Imager, Modified Data 2 (M2), 10 min Data

description: The IMAGE extreme ultraviolet (EUV) imager detects resonantly scattered solar EUV photons with a wavelength of 30.4 nm that have been resonantly scattered by singly ionized helium (Sandel et al., 2000). The sizeable database of IMAGE global snapshots from the extreme ultraviolet (EUV) imager provides revolutionary observations of spatial and temporal plasma distributions throughout the plasmasphere. In this study, the IMAGE EUV data have been mapped to the equator using the approach detailed in Gallagher et al. (2005). IMAGE EUV data have been used to create an automated method that locates and extracts the plasmapause. The plasmapause extraction technique searches a set range of possible plasmasphere densities for a maximum gradient in order to identify the magnetic local time, MLT, dependent plasmapause position as a function of time. This description has been adapted from text appearing in Katus et al. (2015).
DOI: 10.48322/gnrm-pd86
title: IMAGE Predicted Orbital Data

description: IMAGE Predicted Orbit Data, GSE and GSM Coordinates
DOI: 10.48322/awms-1e38
title: IMAGE RPI Monthly Electron Density Values

description: The electron density values listed in this file are derived from the IMAGE Radio Plasma Imager (B.W. Reinisch, PI) data using an automatic fitting program written by Phillip Webb with manual correction. The electron number densities were produced using an automated procedure (with manual correction when necessary) which attempted to self-consistently fit an enhancement in the IMAGE RPI Dynamic Spectra to either 1) the Upper Hybrid Resonance band, 2) the Z-mode or 3) the continuum edge. The automatic algorithm works by rules determined by comparison of the active and passive RPI data [Benson et al., GRL, vol. 31, L20803, doi:10.1029/2004GL020847, 2004]. The manual data points are not from frequencies chosen freely by a human. Rather the human specifies that the computer should search for a peak or continuum edge in a certain frequency region. Thus even the manual points are determined, in part, by the automatic algorithms. Of course that does not guarantee that the data points are right, but it does eliminate some human bias.
DOI: 10.48322/tqpm-9804
title: IMAGE RPI Dynamic Spectrogram data in CDF at NASA CDAWeb
title: IM_K1_RPI

description: RPI passive wave measurement capturing voltage spectral density of the radio emissions in space as a function of frequency, typically between 3 and 1009 kHz. This operating frequency range was selected by the RPI team to provide optimal temporal resolution of the wave observations. Commonly used in the analysis of noise generators, spectral density is a frequency-dependent characteristic that describes how much power is generated by the emission source in a 1 Hz bandwidth. The original description of emissions was done in terms of thermal noise measurements, though the same approach also applies to non-thermal emissions such as AKR. CDF_DS_PT5M stores calibrated data from all three RPI antennas X, Y, and Z individually and a combined X+Y antenna channel. The data are presented as the Voltage Spectral Density (VSD), which is the root of power spectral density, measured in [V/root-Hz] units. Note that conversion of antenna voltage to electric field strength depends on the effective length of the receive antenna, and such conversion is not performed here. (See spase://SMWG/Instrument/IMAGE/RPI for a time history of the lengths of the three mutually orthogonal RPI dipole antennas.) RPI is capable of detecting input radio emissions above its noise floor of 5 nV/root-Hz, which is determined by the internal white noise of the RPI antenna pre-amplifiers. The VSD in RPI spectrogram data is presented in dB relative to 1 V/root-Hz (logarithmic scale), units of dB(V/root-Hz). The RPI instrument noise floor is 5 nV/root-Hz = -166 dB(V/root-Hz) at the receiver input. Software suggested by the science team for CDF file visualization: (1) Plotting tool at the CDAWeb portal, (2) For analysis beyond static image inspection, including color scale optimization, zooming, text export, alternative data representations in physical units, detailed frequency and time information, overlaid model fpe and fce graphs, and EPS quality figures, use BinBrowser software at UML, http://ulcar.uml.edu/rpi.html