cometadata/datacite-titles-descriptions-related-identifiers huggingface dataset:
DOI: 10.3535/059-mr1-5rc
title: Arrhenatherum elatius (L.) P.Beauv. ex J.Presl & C.Presl

description: Digital Specimen for the physical specimen hosted at Finnish Museum of Natural History.
DOI: 10.3535/059-mvg-0sh
title: Triglochin palustris L.

description: Digital Specimen for the physical specimen hosted at Finnish Museum of Natural History.
DOI: 10.48322/8p6g-5v25
title: FAST high resolution data

description: High resolution data obtained by various instruments in the auroral region are available from UCB. They include electric and magnetic AC and DC fields data, energetic particle data, plasma waves and plasma data.
DOI: 10.48322/w0p5-5f22
title: FAST DCF Key Parameters

description: This data set provides the 5-second (spin-averaged) FAST survey electric and magnetic field (Delta B) data within the low altitude auroral arc region. The three-axis searchcoil magnetometer (the AC magnetometer) provides measurement of structures and waves corresponding to ELF and VLF frequencies.  Magnetic field power spectral densities are obtained between 10 Hz and 4 kHz on two axes, and from the third one that is sampled up to 2 MHz, the magnetic component of auroral kilometric radiation (AKR).  Once the auroral electron precipitation is detected, survey data will shift from a slow to a fast survey mode at rates of 32 to 2048 samples per second.  Slow survey data has ~0.06 s resolution, and fast survey, typically has ~0.5 ms resolution. There is a frequency-dependent sensitivity between 10^-8 and 10^-10 nT^2/Hz. Electric field power spectral densities are also provided for the same frequency ranges.
DOI: 10.3535/059-xya-p7t
title: Juncus compressus Jacq.

description: Digital Specimen for the physical specimen hosted at Finnish Museum of Natural History.
DOI: 10.3535/059-y6n-1q5
title: Atriplex patula L.

description: Digital Specimen for the physical specimen hosted at Finnish Museum of Natural History.
DOI: 10.48322/38pk-xy58
title: Galileo Plasma Wave Sensors (PWS) Summary Electric Field Dataset
title: GO JUPITER PWS RESAMP SUMMARY SPECTRUM ANALYZER 60S V1.0

description: This data set includes 1-minute averages of the electric and magnetic wave spectra obtained during the period that the Galileo plasma wave receiver was operated during the Jupiter orbital mission (prime, GEM and GMM). The parameter provided for the electric field spectrum is the electric field spectral density in units of V**2/m**2/Hz. The magnetic field spectrum is provided in units of magnetic field spectral density, nT**2/Hz. The spectral information is averaged and binned into 49 logarithmically-spaced channels from about 6 Hz to 5.6 MHz for the electric measurements and 34 channels from about 6 Hz to 75 kHz for the magnetic. Note that these 'channels' do not generally correspond to the 158 specific channels described in the instrument description document. The reduction in spectral resolution for this data set was performed in order to make the set more conducive to use as a browse data set. The sources of this browse data set are the High Frequency Receiver, Sweep Frequency Receiver, and Spectrum Analyzer which make up the Low Rate Science portion of the PWS.
DOI: 10.48322/gqda-tv68
title: Galileo Plasma Wave Sensors (PWS) Summary Magnetic Field Dataset
title: GO JUPITER PWS RESAMP SUMMARY SPECTRUM ANALYZER 60S V1.0

description: This data set includes 1-minute averages of the electric and magnetic wave spectra obtained during the period that the Galileo plasma wave receiver was operated during the Jupiter orbital mission (prime, GEM and GMM). The parameter provided for the electric field spectrum is the electric field spectral density in units of V**2/m**2/Hz. The magnetic field spectrum is provided in units of magnetic field spectral density, nT**2/Hz. The spectral information is averaged and binned into 49 logarithmically-spaced channels from about 6 Hz to 5.6 MHz for the electric measurements and 34 channels from about 6 Hz to 75 kHz for the magnetic. Note that these 'channels' do not generally correspond to the 158 specific channels described in the instrument description document. The reduction in spectral resolution for this data set was performed in order to make the set more conducive to use as a browse data set. The sources of this browse data set are the High Frequency Receiver, Sweep Frequency Receiver, and Spectrum Analyzer which make up the Low Rate Science portion of the PWS.
DOI: 10.3535/059-yhg-gf6
title: Psammophiliella muralis (L.) Ikonn.

description: Digital Specimen for the physical specimen hosted at Finnish Museum of Natural History.
DOI: 10.3535/05a-391-p7t
title: Spinulum annotinum (L.) A. Haines

description: Digital Specimen for the physical specimen hosted at Finnish Museum of Natural History.
DOI: 10.48322/c5d6-br40
title: Gold Level 1C Day Disk data

description: The Level 1C Day Disk data is sampled on a uniform angular grid of 0.2° in both Longitude and Latitude. The data is resampled as follows:
		* About 4 scan mirror positions to fill the 0.2° L1C bin.
		* Image displacement per scan mirror step: 0.0494°
		* Narrow slit width: 0.075°
		* Use center of L1B and L1C bins to resample (nearest neighbor) GOLD Public Science Data Products Guide (1.0) 26
		* Spectral data is combined within a L1C bin WITHOUT doing any wavelength alignment
		for each L1B sample
		* 92 bins E-W
		* 104 bins N-S
DOI: 10.48322/xbhc-5n57
title: Gold Level 1C German Space Agency Disk data

description: The Level 1C German Space Agency Disk data is sampled on a uniform angular grid of 0.2° in both Longitude and Latitude. The data is resampled as follows:
		* About 4 scan mirror positions to fill the 0.2° L1C bin.
		* Image displacement per scan mirror step: 0.0494°
		* Narrow slit width: 0.075°
		* Use center of L1B and L1C bins to resample (nearest neighbor) GOLD Public Science Data Products Guide (1.0) 26
		* Spectral data is combined within a L1C bin WITHOUT doing any wavelength alignment
		for each L1B sample
		* 92 bins E-W
		* 104 bins N-S
DOI: 10.3535/05a-9ws-0xl
title: Luzula sudetica (Willd.) Schult.

description: Digital Specimen for the physical specimen hosted at Finnish Museum of Natural History.
DOI: 10.48322/2abb-5978
title: Gold Level 1C Limb data

description: The Level 1C limb data is sampled on a uniform angular grid  Latitude. 
	  The data is resampled as follows:
		* About 4 scan mirror positions to fill the 0.2° L1C bin.
		* Narrow slit width: 0.075°
		* Use center of L1B and L1C bins to resample (nearest neighbor) GOLD Public Science Data Products Guide (1.0) 26
		* Spectral data is combined within a L1C bin WITHOUT doing any wavelength alignment
		for each L1B sample
		* 30 bins Altitude
		* 32 bins N-S
DOI: 10.3535/05a-d63-hr3
title: Ranunculus flammula subsp. flammula

description: Digital Specimen for the physical specimen hosted at Finnish Museum of Natural History.
DOI: 10.3535/05a-f18-7w8
title: Carex oederi var. oederi

description: Digital Specimen for the physical specimen hosted at Finnish Museum of Natural History.
DOI: 10.48322/gj9t-v633
title: GOLD Level L2 Molecular Oxygen Density Profile

description: O2 is derived from measurements of stellar occultation in the Shumann Runge continuum. 
	  As the star rises or sets relative to the satellite position the stellar spectrum is measured across 
	  the GOLD spectral bandpass, from 132 to 162 nm. Geolocation of the OCC L1B data provides the 
	  line-of-sight tangent altitude vs. time during the occultation. This results in a 2-dimensional 
	  map of the stellar signal, in counts or calibrated geophysical units (irradiance), vs. wavelength 
	  and tangent altitude. A sample of this image is represented in the top left panel of the OCC L1D 
	  image in Figure 3-22.
	  
      The measured counts profile is then normalized by the unattenuated, exo-atmospheric spectrum, yielding 
	  the slant path transmission profile vs. wavelength at the native L1C spectral sampling of 0.12 nm. 
	  The defining characteristic of the atmospheric transmission is that it is completely independent of 
	  instrument calibration or absolute accuracy. The full transmission spectrum is binned into a small 
	  number of 2-nm spectral channels for use in the retrievals. These retrieval channels are chosen to 
	  span the spectral dependence of the O2 absorption cross-section in order to maximize the O2 retrieval 
	  altitude range (approximately 120-240 km). In the Version 1 O2DEN data set two spectral channels 
	  are used, centered at 142- and 159-nm.
      
	  Since stars rise or set at approximately 3 km/sec, as observed from orbit, the 100-msec occultation 
	  cadence results in a measurement of extremely high (sub-km) vertical resolution. The data are binned 
	  to enhance signal-to-noise, producing an effective vertical resolution of 10 km or less, which is 
	  sufficient to easily resolve the scale height of the O2 thermospheric profile.
      
	  The algorithm uses an optimal estimation routine, which provide a complete error analysis and 
	  retrieval diagnostics such as averaging kernels and information content. A data vector constructed 
	  from the multiple spectral channels of slant path transmission is used to derive the atmospheric 
	  state vector – O2 density vs. geometric altitude – via a nonlinear, iterative inversion. The retrieved 
	  O2 density profile is reported on a fixed altitude grid with 5-km spacing. The valid altitude range 
	  varies for each event, but generally ranges from ~120 – 240.
DOI: 10.48322/q9qk-h486
title: Gold Level 1C Day Disk data

description: The Level 1C NI1 data is sampled on a uniform angular grid of 0.15° in both Longitude and Latitude. The data is resampled as follows:
		* About 4 scan mirror positions to fill the 0.15° L1C bin.
		* Use center of L1B and L1C bins to resample (nearest neighbor) GOLD Public Science Data Products Guide (1.0) 26
		* Spectral data is combined within a L1C bin WITHOUT doing any wavelength alignment
		for each L1B sample
		* 51 bins E-W
		* 100 bins N-S
DOI: 10.3535/05a-ht1-1h8
title: Festuca ovina L.

description: Digital Specimen for the physical specimen hosted at Finnish Museum of Natural History.
DOI: 10.3535/05a-tjb-nk9
title: Hammarbya paludosa (L.) Kuntze

description: Digital Specimen for the physical specimen hosted at Finnish Museum of Natural History.
DOI: 10.48322/509j-gm79
title: Helios 2 hourly merged magnetic field and plasma data

description: This is an hourly resolution, merged magnetic field and plasma data set created at NSSDC for COHOWeb. Magnetic field vectors and plasma flow direction angles are given in RTN coordinates. Spacecraft position data are given in Heliographic inertial (HGI coordinates).
DOI: 10.48322/zwyq-g988
title: Gold Level L2 Solar EUV proxy

description: The GOLD solar irradiance proxy (QEUV) is a proxy for the integrated solar EUV 
	  irradiance below 45 nm, which can be derived directly from far ultraviolet (FUV) radiance 
	  measurements. QEUV is a dayside disk data product, derived from the GOLD DAY measurement mode.
	  
	  Algorithm heritage
	  The disk QEUV retrieval algorithm was originally developed for use with GUVI and SSUSI images 
	  (Strickland et al., [1995]).  The GOLD implementation of this algorithm takes advantage of GOLD’s 
	  ability to transmit the full spectrum to maximize the signal-to-noise ratio and eliminate atomic 
	  emission lines that contaminate the N2 LBH bands (e.g., N I 149.3 nm). This algorithm has been 
	  extensively documented and applied (e.g., Strickland et al. [2004]; Evans et al., [1995]). The 
	  associated GOLD Level 2 data product is called QEUV.
	  
	  References
	  -Evans, J. S., D. J. Strickland and R. E. Huffman (1995), Satellite remote sensing of thermospheric 
	   O/N2 and solar EUV: 2. Data analysis, J. Geophys. Res., Vol. 100, NO. A7, pages 12,227-12,233.
      -Strickland, D. J., J. S. Evans, and L. J. Paxton (1995), Satellite remote sensing of thermospheric  
	   O/N2 and solar EUV: 1. Theory, J. Geophys. Res., 110, A7, pages 12,217-12,226.
      -Strickland, D. J., J. L. Lean, R. R. Meier, A. B. Christensen, L. J. Paxton, D. Morrison, J. D. 
	   Craven, R. L. Walterscheid, D. L. Judge, and D. R. McMullin, (2004), Solar EUV irradiance variability 
	   derived from terrestrial far ultraviolet dayglow observations, Vol. 31, L03801, doi:10.1029/2003GL018415.
DOI: 10.3535/059-meg-rdv
title: Dryopteris filix-mas (L.) Schott

description: Digital Specimen for the physical specimen hosted at Finnish Museum of Natural History.
DOI: 10.3535/05a-w6g-p9s
title: Matteuccia struthiopteris (L.) Tod.

description: Digital Specimen for the physical specimen hosted at Finnish Museum of Natural History.
DOI: 10.48322/2pmw-ee13
title: Gold Level L2 Peak Electron Density

description: The GOLD night disk scan (NI1) measurements are used to derive the peak electron density (NMAX, electrons/cm3) on the disk. GOLD performs NI1 scans in both hemispheres from 17:00 to 21:00 hours spacecraft local time each night. NMAX is retrieved on a 2D rectangular (latitude vs. longitude) grid of fixed dimensions for each scan. However, the actual latitude and longitude values in the grid vary from scan to scan as the NI1 sequence utilizes a pattern of short (15 minute) localized scans that progress from east to west across the disk throughout the sequence.
DOI: 10.48322/eh54-2h31
title: Helios 2 E6 (Kunow) Hourly Particle Fluxes in CDF Format

description: particle-flux>Merged proton, electron and alpha particle fluxes. Helios-A and Helios-B Spacecraft were a Pair of Deep Space Probes developed by the Federal Republic of Germany, FRG, in a Cooperative Program with NASA. The Purpose of the Mission was to make pioneering Measurements of the Interplanetary Medium from the Vicinity of the Earth Orbit to 0.3 AU. The Objective of Experiment, E6, was to study High-Energy, Charged, Cosmic Ray Particles of Solar, Planetary, and Galactic Origin in Interplanetary Space. Protons and Alpha Particles with Energies >1.3 MeV/n, and electrons >3.3 MeV were measured within Interplanetary Space over the Range from 0.3 to 1.0 A.U. The Instrument, a Particle Telescope with 55° Field of View, consisted of five Semiconductor Detectors, one Sapphire Cherenkov Counter, and one Scintillation Counter, all enclosed by an Anticoincidence Cylinder. The Telescope was calibrated prior to Launch using Radioactive Sources, Particle Acceletors, and Ground-Level Muons. It measured Protons and Alpha particles in six Channels, 1.3 to 3.3, 3.3 to 13, 13 to 27, 27 to 37, 37 to 45, and >45 MeV/n, and Electrons in five Energy Channels, 0.3 to 0.8, 0.8 to 2, 2 to 3, 3 to 4, and >4 MeV. For more Detail See pages 253-257 of Raumfahrtforschung, Volume 19, Number 5, 1975. The Helios-A Cosmic Ray '.dat' and Helios-B Cosmic Ray '.dat' files contains hourly averaged Fluxes of Electrons, Protons and Alpha Particles in the MeV Ranges. The Files were written in ASCII-Codes. Each Record contains 10 hourly Averages. The Differential Fluxes, (m^2 s sr MeV)^-1, Cover, in several Bands, the Energy Range 0.3 to 2.0 MeV for Electrons, 4.0 to 51 MeV for Protons, and 2.0 to 48 MeV for Alpha Particles. Also provided are the Integral Fluxes of Alphas above 48 MeV, and Protons above 51 MeV. For some of the Energy Channels, the Standard Deviations of the Averages are also provided. Each File is preceded by a Header Record, providing the Start and Stop Times of the Data in the File. The Acronyms for the Rate Channels are composed of a Letter and an Indication of the Energy Range in MeV/n for Protons and Alpha Particles, respectively and MeV for Electrons. The counting Rates are given as (m^2 s sr MeV/n)^-1 except for the Integral Channels P>51 and A>48, which are given as (m^2 s sr)^-1. Note: 1. Negative Rates, -0.99999E+04, indicate Missing or Invalid Data. 2. The Energy Boundaries for the Electron Channels 0.2 to 0.8 and 0.8 to 2 are only rough Estimates.
DOI: 10.48322/ybkm-rz28
title: Gold Level L2 Molecular Oxygen Density Profile

description: O2 is derived from measurements of stellar occultation in the Shumann Runge continuum. 
	  As the star rises or sets relative to the satellite position the stellar spectrum is measured across 
	  the GOLD spectral bandpass, from 132 to 162 nm. Geolocation of the OCC L1B data provides the 
	  line-of-sight tangent altitude vs. time during the occultation. This results in a 2-dimensional 
	  map of the stellar signal, in counts or calibrated geophysical units (irradiance), vs. wavelength 
	  and tangent altitude. A sample of this image is represented in the top left panel of the OCC L1D 
	  image in Figure 3-22.
	  
      The measured counts profile is then normalized by the unattenuated, exo-atmospheric spectrum, yielding 
	  the slant path transmission profile vs. wavelength at the native L1C spectral sampling of 0.12 nm. 
	  The defining characteristic of the atmospheric transmission is that it is completely independent of 
	  instrument calibration or absolute accuracy. The full transmission spectrum is binned into a small 
	  number of 2-nm spectral channels for use in the retrievals. These retrieval channels are chosen to 
	  span the spectral dependence of the O2 absorption cross-section in order to maximize the O2 retrieval 
	  altitude range (approximately 120-240 km). In the Version 1 O2DEN data set two spectral channels 
	  are used, centered at 142- and 159-nm.
      
	  Since stars rise or set at approximately 3 km/sec, as observed from orbit, the 100-msec occultation 
	  cadence results in a measurement of extremely high (sub-km) vertical resolution. The data are binned 
	  to enhance signal-to-noise, producing an effective vertical resolution of 10 km or less, which is 
	  sufficient to easily resolve the scale height of the O2 thermospheric profile.
      
	  The algorithm uses an optimal estimation routine, which provide a complete error analysis and 
	  retrieval diagnostics such as averaging kernels and information content. A data vector constructed 
	  from the multiple spectral channels of slant path transmission is used to derive the atmospheric 
	  state vector – O2 density vs. geometric altitude – via a nonlinear, iterative inversion. The retrieved 
	  O2 density profile is reported on a fixed altitude grid with 5-km spacing. The valid altitude range 
	  varies for each event, but generally ranges from ~120 – 240.
DOI: 10.48322/f67k-v705
title: Gold Level 1C Occultation data

description: The Level 1C Dayside Disk Images are interrupted via stored instrument commands when 
	  target stars suitable for occultation measurements approach either limb. 
	  To perform the occultation measurement, the slit mechanism inserts the 1 degree wide occultation (OCC) 
	  slit at the spectrometer focal plane, and the scan mirrors slew the Field of View to the star. 
	  The mirror is centered at a 225 km tangent point altitude. Occultations require 6 minutes to 
	  execute (30 seconds to configure the instrument, 30 seconds for uncertainty in timing and pointing, 
	  4 minutes for the actual occultation, 30 seconds for uncertainty in timing and pointing, and 30 
	  seconds to return to HR slit). Once the occultation is complete, the HR slit is inserted, the scan 
	  mirror returns to its departure point in the original mapping observation, and Dayside Disk Image is 
	  resumed. By choice GOLD is limited to performing ~10 occultations a day for most of the year, 
	  reducing the dayside mapping duty cycle by ~5%.
DOI: 10.48322/qjyq-y358
title: Interball Tail definitive orbital data

description: Definitive Interball Tail satellite and subsatellite (Interball-1 and Magion-4) orbital data: Spacecraft position, velocity, and status flags.
DOI: 10.48322/c0xs-k906
title: Interball Tail energetic particle 2-min Key Parameters

description: Interball Tail energetic proton (22-28 keV, 1-3 MeV) and electron (21-26, 76-95, 150-500 keV) fluxes from DOK-2 and SKA-2 sensors, 2-min key parameters
DOI: 10.48322/z1rp-x549
title: Interball Tail Radio Emission 2-min Key Parameters

description: This set of Interball Tail Probe radio emission flux was measured in 2-min intervals in the 100, 252, 500 kHz frequencies, with the width of each channel at about 10 kHz. Loop antenna with 1.5 m2 area was used.
DOI: 10.3535/05a-zf3-9ec
title: Arabidopsis arenosa (L.) Lawalrée

description: Digital Specimen for the physical specimen hosted at Finnish Museum of Natural History.
DOI: 10.48322/7g0e-ax29
title: IMAGE Radio Plasma Imager (RPI) Plasmagram Full Resolution Binary Data

description: RPI plasmagram full resolution data (received signal strength in the frequency-range frame), uncalibrated. Presented as instrument packets wrapped in the standard CCSDS headers. Description of the RPI instrument-level data model can be found at http://ulcar.uml.edu/RPI/RPITelemetryDataFormat_V2.8.pdf. Data are viewed/calibrated/edited by BinBrowser software, see http://ulcar.uml.edu/rpi.html for download and users' guide. RPI plasmagrams are visualized by plotting images in which received signal strength (color scale) is a function of echo delay (range in vertical scale) and radio-sounder frequency (horizontal scale) of the radar pulses. Echoes from important magnetospheric structures, such as the magnetopause and the plasmapause, appear as traces on plasmagrams. Plasmagram traces are intermixed with vertical signatures corresponding to the locally excited plasma resonances and various natural emissions propagating in space.
DOI: 10.48322/dt0h-xw03
title: IMAGE Housekeeping Data via CDAWeb

description: This set of housekeeping data from the IMAGE mission comes from the Central Interface Data Processor (CIDP) and the interface with the Spacecraft/System Control Unit (SCU).   The CIDP provides the following major functions for the Observatory:
(1) Instrument data acquisition, processing, and compression.
(2) Stored command processing.
(3) Command receipt (from the SCU), processing, storage (if a delayed command),
and transfer to the instruments.
(4) Time/attitude synchronization with the spacecraftÕs Attitude Determination
and Control system for generation of the nadir and sun pulse signals sent to
the instruments.
(5) Deckplate thermal control.
(6) Additional EEPROM storage for instrument software or tables.
(7) Power switching and current limiting.

The SCU provides the following major functions for the Observatory: 
(1) Ground command receipt, processing, storage (for delayed command execution)
and relay to the CIDP.
(2) Telemetry data formatting and downlink
(3) Spacecraft attitude determination and control.
(4) Spacecraft thermal control.
(5) Spacecraft power management.
(6) Spacecraft housekeeping data acquisition, formatting, and storage.
(7) Management of the Mass Memory Module.
(8) Management of the engineering and high speed telemetry downlink.
(9) Safe/hold management of the Observatory.

Products include:
  
IM_HK_ADS: Image Attitude Determination System Housekeeping
IM_HK_AST: Image Autonomous Star Tracker Housekeeping 
IM_HK_COM: Image Communication Systems Housekeeping 
IM_HK_FSW: Image Flight Software Housekeeping 
IM_HK_PWR: Image Power Systems Housekeeping
IM_HK_TML: Image Thermal Housekeeping
DOI: 10.3535/05a-zkb-n64
title: Cerastium glutinosum Fr.

description: Digital Specimen for the physical specimen hosted at Finnish Museum of Natural History.
DOI: 10.3535/05b-302-fav
title: Dryopteris carthusiana (Vill.) H. P. Fuchs

description: Digital Specimen for the physical specimen hosted at Finnish Museum of Natural History.
DOI: 10.48322/n8h3-d525
title: IMP 8 Cosmic Ray Nuclear Composition (CRNC) hourly energetic alpha particle fluxes

description: This data set contains hourly, spin-averaged
fluxes of alpha particles from the IMP8 Cosmic Ray Nuclear Composition
experiment of U. Chicago and UNH.  There are fluxes of alpha particles
in 9 energy bins from 10.90-12.89 to 84.32-94.81 MeV/n.  These fluxes
were generated at GSFC/SPDF from count rates accessible from
UNH.
DOI: 10.3535/05b-an9-f5p
title: Neottia ovata (L.) Hartm.

description: Digital Specimen for the physical specimen hosted at Finnish Museum of Natural History.
DOI: 10.3535/05b-bfh-0c0
title: Eriophorum latifolium Hoppe

description: Digital Specimen for the physical specimen hosted at Finnish Museum of Natural History.