cometadata/datacite-titles-descriptions-related-identifiers huggingface dataset:
DOI: 10.15156/bio/sh0935555.10fu
title: SH0935555.10FU

description: UNITE provides a unified way for delimiting, identifying, communicating, and working with DNA-based Species Hypotheses (SH). All fungal ITS sequences in the international nucleotide sequence databases are clustered to approximately the species level by applying a set of dynamic distance values (<0.5 - 3.0%). All species hypotheses are given a unique, stable name in the form of a DOI, and their taxonomic and ecological annotations are verified through distributed, web-based third-party annotation efforts. SHs are connected to a taxon name and its classification as far as possible (phylum, class, order, etc.) by taking into account identifications for all sequences in the SH. An automatically or manually designated sequence is chosen to represent each such SH. These sequences are released (https://unite.ut.ee/repository.php) for use by the scientific community in, for example, local sequence similarity searches and next-generation sequencing analysis pipelines. The system and the data are updated automatically as the number of public fungal ITS sequences grows.
DOI: 10.15156/bio/sh0935556.10fu
title: SH0935556.10FU

description: UNITE provides a unified way for delimiting, identifying, communicating, and working with DNA-based Species Hypotheses (SH). All fungal ITS sequences in the international nucleotide sequence databases are clustered to approximately the species level by applying a set of dynamic distance values (<0.5 - 3.0%). All species hypotheses are given a unique, stable name in the form of a DOI, and their taxonomic and ecological annotations are verified through distributed, web-based third-party annotation efforts. SHs are connected to a taxon name and its classification as far as possible (phylum, class, order, etc.) by taking into account identifications for all sequences in the SH. An automatically or manually designated sequence is chosen to represent each such SH. These sequences are released (https://unite.ut.ee/repository.php) for use by the scientific community in, for example, local sequence similarity searches and next-generation sequencing analysis pipelines. The system and the data are updated automatically as the number of public fungal ITS sequences grows.
DOI: 10.15468/dl.dsmggm
title: Occurrence Download

description: A dataset containing 8272 species occurrences available in GBIF matching the query:
{
 "and" : [
 "TaxonKey is Myotis brandtii (Eversmann, 1845)",
 "HasCoordinate is true",
 "Year is greater than or equal to 2011",
 "Year is less than or equal to 2024"
 ]
}

 The dataset includes 8272 records from 320 constituent datasets; see https://api.gbif.org/v1/occurrence/download/0099808-240626123714530/datasets/export for details.
 
Data from some individual datasets included in this download may be licensed under less restrictive terms.
DOI: 10.15468/dl.nh3umw
title: Occurrence Download

description: A dataset listing the 284 species recorded in GBIF matching the query:
{
 "and" : [
 "HasCoordinate is false",
 "OccurrenceStatus is Present",
 "TaxonKey is Stipa L.",
 "Year 1945-2025"
 ]
}

 The dataset's 284 records were derived from 233 constituent datasets; see https://api.gbif.org/v1/occurrence/download/0021500-250402121839773/datasets/export for details.
 
Data from some individual datasets included in this download may be licensed under less restrictive terms.
DOI: 10.15468/dl.uxc7px
title: Occurrence Download

description: A dataset listing the 296 species recorded in GBIF matching the query:
{
 "and" : [
 "HasCoordinate is true",
 "HasGeospatialIssue is false",
 "OccurrenceStatus is Present",
 "TaxonKey is Stipa L.",
 "Year 1945-2025"
 ]
}

 The dataset's 296 records were derived from 667 constituent datasets; see https://api.gbif.org/v1/occurrence/download/0021499-250402121839773/datasets/export for details.
 
Data from some individual datasets included in this download may be licensed under less restrictive terms.
DOI: 10.5281/zenodo.2652259
title: One-dimensional hydrodynamic solution data of wavelet-based adaptive finite volume and discontinuous Galerkin shallow water solvers

description: Raw data for a series of idealised, one-dimensional hydrodynamic test cases:


	dambreakwet (SWASHES 4.1.1)
	dambreakdry (SWASHES 4.1.2)
	dambreakmanning (SWASHES 4.1.3)
	dambreakupslope, dambreakdownslope (Kesserwani and Liang 2011)
	dambreakonehump (Ozmen-Cagatay and Kocaman 2011)
	lakeatrest (Kesserwani et al. 2018)
	parabolicbowlswashes (SWASHES 4.2.1)
	parabolicbowlliangmarche (Liang and Marche 2009)
	steadysubcritical (SWASHES 3.1.3)
	steadysupercritical (Haleem et al. 2015)
	steadytranscriticalshockless (SWASHES 4.1.4)
	steadytranscriticalshock (SWASHES 4.1.5) 


SWASHES refers to Delestre et al. 2013
DOI: 10.17632/fd8htt6785.1
title: Data for: Viscous sintering kinetics of biopolymer filaments extruded for 3D printing (Image Analysis)

description: Results of the image analysis during sintering sequences. Fusion bonding kinetics between two extruded filaments based on zein plasticized by 20w% glycerol (filament_diameter=2mm, each) at T=80°C, T=100°C, T=120°C, T=125°C, T=130°C and T=140°C (average values and standard deviations for 3 trials carried out at each temperature): - Evolution of the bonding angle, Theta [rad], between the two extruded filaments - Evolution of the convexity index, Iconvex [-], defined as the ratio between the area of the two filaments cross-section and the convex surface (the whole area including the two filaments cross-section and concavities between them). This ratio reaches a value of 1 if the fusion bonding leads to a perfect sintering of the two filaments, without residual concavity.
DOI: 10.17632/hz92442nhg.1
title: Data for: Viscous sintering kinetics of biopolymer filaments extruded for 3D printing (Dynamic Mechanical Analysis)

description: Results of Dynamic Mechanical Analysis -DMA- performed on extruded filament based on zein plasticized by 20w% glycerol (diameter_filament = 2 mm; lenght_filament=20mm). The mechanical active length between the two grips is 10 mm. The extrudate is characterized in tensile mode at 1Hz, with strain set at 0.1% and heating rate at 3°C/min. Values are presented for the storage modulus (E', [Pa]), the loss modulus (E'', [Pa]) and the damping factor (tan_delta=E''/E', [-]).
DOI: 10.5281/zenodo.2652197
title: Hydrodynamics-MariakerkeNovember2017

description: Hydrodynamics (ADCP) and suspended sediment concentrations (OBS) measured at Mariakerke in November 2017
DOI: 10.5281/zenodo.2652198
title: Hydrodynamics-MariakerkeNovember2017

description: Hydrodynamics (ADCP) and suspended sediment concentrations (OBS) measured at Mariakerke in November 2017
DOI: 10.17632/h92t6y3pkm.1
title: Data for: Predictive Livestock Early Warning System (PLEWS): Implications for animal production and animal/public health

description: Supplementary material_FCI_3month_average_contingency_final_jan_31_2017_pixel_ave_new This data is the forage condition indices on three monthly average for counties in Kenya.
DOI: 10.18716/nmrshiftdb2/60001972/chiuz_cdcl3
title: ChiuZ NMR dataset for (3R)-3,7-Dimethyl-1,6-octadien-3-ol; l-Linalool; Licareol in Chloroform-D1 (CDCl3)
DOI: 10.18716/nmrshiftdb2/60001972
title: NMR data for (3R)-3,7-Dimethyl-1,6-octadien-3-ol; l-Linalool; Licareol
DOI: 10.25606/surf.578c6039-140ee799
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (1024-035)

description: We present the results of the "Cosmogrid" cosmological N-body simulation suites based on the concordance LCDM model. The Cosmogrid simulation was performed in a 30 Mpc box with 2048³ particles. The mass of each particle is 1.28x10^5 Msun, which is sufficient to resolve ultra-faint dwarfs. We found that the halo mass function shows good agreement with the Sheth & Tormen fitting function down to ~10^7 Msun. We have analyzed the spherically averaged density profiles of the three most massive halos which are of galaxy group size and contain at least 170 million particles. The slopes of these density profiles become shallower than -1 at the inner most radius. We also find a clear correlation of halo concentration with mass. The mass dependence of the concentration parameter cannot be expressed by a single power law, however a simple model based on the Press-Schechter theory proposed by Navarro et al. gives reasonable agreement with this dependence. The spin parameter does not show a correlation with the halo mass. The probability distribution functions for both concentration and spin are well fitted by the log-normal distribution for halos with the masses larger than ~10^8 Msun. The subhalo abundance depends on the halo mass. Galaxy-sized halos have 50% more subhalos than ~10^11 Msun halos have. This is snapshot 035 of the 1024³ resolution collection.
DOI: 10.25606/surf.578c6039-773d1df7
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (1024-034)

description: We present the results of the "Cosmogrid" cosmological N-body simulation suites based on the concordance LCDM model. The Cosmogrid simulation was performed in a 30 Mpc box with 2048³ particles. The mass of each particle is 1.28x10^5 Msun, which is sufficient to resolve ultra-faint dwarfs. We found that the halo mass function shows good agreement with the Sheth & Tormen fitting function down to ~10^7 Msun. We have analyzed the spherically averaged density profiles of the three most massive halos which are of galaxy group size and contain at least 170 million particles. The slopes of these density profiles become shallower than -1 at the inner most radius. We also find a clear correlation of halo concentration with mass. The mass dependence of the concentration parameter cannot be expressed by a single power law, however a simple model based on the Press-Schechter theory proposed by Navarro et al. gives reasonable agreement with this dependence. The spin parameter does not show a correlation with the halo mass. The probability distribution functions for both concentration and spin are well fitted by the log-normal distribution for halos with the masses larger than ~10^8 Msun. The subhalo abundance depends on the halo mass. Galaxy-sized halos have 50% more subhalos than ~10^11 Msun halos have. This is snapshot 034 of the 1024³ resolution collection.
DOI: 10.18716/nmrshiftdb2/60000009
title: NMR data for Colchicin
DOI: 10.25606/surf.578c6039-03e0cfbf
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (2048-552)

description: We present the results of the "Cosmogrid" cosmological N-body simulation suites based on the concordance LCDM model. The Cosmogrid simulation was performed in a 30 Mpc box with 2048³ particles. The mass of each particle is 1.28x10^5 Msun, which is sufficient to resolve ultra-faint dwarfs. We found that the halo mass function shows good agreement with the Sheth & Tormen fitting function down to ~10^7 Msun. We have analyzed the spherically averaged density profiles of the three most massive halos which are of galaxy group size and contain at least 170 million particles. The slopes of these density profiles become shallower than -1 at the inner most radius. We also find a clear correlation of halo concentration with mass. The mass dependence of the concentration parameter cannot be expressed by a single power law, however a simple model based on the Press-Schechter theory proposed by Navarro et al. gives reasonable agreement with this dependence. The spin parameter does not show a correlation with the halo mass. The probability distribution functions for both concentration and spin are well fitted by the log-normal distribution for halos with the masses larger than ~10^8 Msun. The subhalo abundance depends on the halo mass. Galaxy-sized halos have 50% more subhalos than ~10^11 Msun halos have. This is snapshot 552 of the 2048³ resolution collection.
DOI: 10.25606/surf.578c6039-3b870c44
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (2048-547)

description: We present the results of the "Cosmogrid" cosmological N-body simulation suites based on the concordance LCDM model. The Cosmogrid simulation was performed in a 30 Mpc box with 2048³ particles. The mass of each particle is 1.28x10^5 Msun, which is sufficient to resolve ultra-faint dwarfs. We found that the halo mass function shows good agreement with the Sheth & Tormen fitting function down to ~10^7 Msun. We have analyzed the spherically averaged density profiles of the three most massive halos which are of galaxy group size and contain at least 170 million particles. The slopes of these density profiles become shallower than -1 at the inner most radius. We also find a clear correlation of halo concentration with mass. The mass dependence of the concentration parameter cannot be expressed by a single power law, however a simple model based on the Press-Schechter theory proposed by Navarro et al. gives reasonable agreement with this dependence. The spin parameter does not show a correlation with the halo mass. The probability distribution functions for both concentration and spin are well fitted by the log-normal distribution for halos with the masses larger than ~10^8 Msun. The subhalo abundance depends on the halo mass. Galaxy-sized halos have 50% more subhalos than ~10^11 Msun halos have. This is snapshot 547 of the 2048³ resolution collection.
DOI: 10.25606/surf.578c6039-5975dbc0
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (2048-544)

description: We present the results of the "Cosmogrid" cosmological N-body simulation suites based on the concordance LCDM model. The Cosmogrid simulation was performed in a 30 Mpc box with 2048³ particles. The mass of each particle is 1.28x10^5 Msun, which is sufficient to resolve ultra-faint dwarfs. We found that the halo mass function shows good agreement with the Sheth & Tormen fitting function down to ~10^7 Msun. We have analyzed the spherically averaged density profiles of the three most massive halos which are of galaxy group size and contain at least 170 million particles. The slopes of these density profiles become shallower than -1 at the inner most radius. We also find a clear correlation of halo concentration with mass. The mass dependence of the concentration parameter cannot be expressed by a single power law, however a simple model based on the Press-Schechter theory proposed by Navarro et al. gives reasonable agreement with this dependence. The spin parameter does not show a correlation with the halo mass. The probability distribution functions for both concentration and spin are well fitted by the log-normal distribution for halos with the masses larger than ~10^8 Msun. The subhalo abundance depends on the halo mass. Galaxy-sized halos have 50% more subhalos than ~10^11 Msun halos have. This is snapshot 544 of the 2048³ resolution collection.
DOI: 10.25606/surf.578c6039-6cad22e7
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (2048-584)

description: We present the results of the "Cosmogrid" cosmological N-body simulation suites based on the concordance LCDM model. The Cosmogrid simulation was performed in a 30 Mpc box with 2048³ particles. The mass of each particle is 1.28x10^5 Msun, which is sufficient to resolve ultra-faint dwarfs. We found that the halo mass function shows good agreement with the Sheth & Tormen fitting function down to ~10^7 Msun. We have analyzed the spherically averaged density profiles of the three most massive halos which are of galaxy group size and contain at least 170 million particles. The slopes of these density profiles become shallower than -1 at the inner most radius. We also find a clear correlation of halo concentration with mass. The mass dependence of the concentration parameter cannot be expressed by a single power law, however a simple model based on the Press-Schechter theory proposed by Navarro et al. gives reasonable agreement with this dependence. The spin parameter does not show a correlation with the halo mass. The probability distribution functions for both concentration and spin are well fitted by the log-normal distribution for halos with the masses larger than ~10^8 Msun. The subhalo abundance depends on the halo mass. Galaxy-sized halos have 50% more subhalos than ~10^11 Msun halos have. This is snapshot 584 of the 2048³ resolution collection.
DOI: 10.25606/surf.578c6039-aa86777e
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (2048-546)

description: We present the results of the "Cosmogrid" cosmological N-body simulation suites based on the concordance LCDM model. The Cosmogrid simulation was performed in a 30 Mpc box with 2048³ particles. The mass of each particle is 1.28x10^5 Msun, which is sufficient to resolve ultra-faint dwarfs. We found that the halo mass function shows good agreement with the Sheth & Tormen fitting function down to ~10^7 Msun. We have analyzed the spherically averaged density profiles of the three most massive halos which are of galaxy group size and contain at least 170 million particles. The slopes of these density profiles become shallower than -1 at the inner most radius. We also find a clear correlation of halo concentration with mass. The mass dependence of the concentration parameter cannot be expressed by a single power law, however a simple model based on the Press-Schechter theory proposed by Navarro et al. gives reasonable agreement with this dependence. The spin parameter does not show a correlation with the halo mass. The probability distribution functions for both concentration and spin are well fitted by the log-normal distribution for halos with the masses larger than ~10^8 Msun. The subhalo abundance depends on the halo mass. Galaxy-sized halos have 50% more subhalos than ~10^11 Msun halos have. This is snapshot 546 of the 2048³ resolution collection.
DOI: 10.25606/surf.578c6039-b2d36e36
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (2048-548)

description: We present the results of the "Cosmogrid" cosmological N-body simulation suites based on the concordance LCDM model. The Cosmogrid simulation was performed in a 30 Mpc box with 2048³ particles. The mass of each particle is 1.28x10^5 Msun, which is sufficient to resolve ultra-faint dwarfs. We found that the halo mass function shows good agreement with the Sheth & Tormen fitting function down to ~10^7 Msun. We have analyzed the spherically averaged density profiles of the three most massive halos which are of galaxy group size and contain at least 170 million particles. The slopes of these density profiles become shallower than -1 at the inner most radius. We also find a clear correlation of halo concentration with mass. The mass dependence of the concentration parameter cannot be expressed by a single power law, however a simple model based on the Press-Schechter theory proposed by Navarro et al. gives reasonable agreement with this dependence. The spin parameter does not show a correlation with the halo mass. The probability distribution functions for both concentration and spin are well fitted by the log-normal distribution for halos with the masses larger than ~10^8 Msun. The subhalo abundance depends on the halo mass. Galaxy-sized halos have 50% more subhalos than ~10^11 Msun halos have. This is snapshot 548 of the 2048³ resolution collection.
DOI: 10.25606/surf.578c6039-c04498d2
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (2048-549)

description: We present the results of the "Cosmogrid" cosmological N-body simulation suites based on the concordance LCDM model. The Cosmogrid simulation was performed in a 30 Mpc box with 2048³ particles. The mass of each particle is 1.28x10^5 Msun, which is sufficient to resolve ultra-faint dwarfs. We found that the halo mass function shows good agreement with the Sheth & Tormen fitting function down to ~10^7 Msun. We have analyzed the spherically averaged density profiles of the three most massive halos which are of galaxy group size and contain at least 170 million particles. The slopes of these density profiles become shallower than -1 at the inner most radius. We also find a clear correlation of halo concentration with mass. The mass dependence of the concentration parameter cannot be expressed by a single power law, however a simple model based on the Press-Schechter theory proposed by Navarro et al. gives reasonable agreement with this dependence. The spin parameter does not show a correlation with the halo mass. The probability distribution functions for both concentration and spin are well fitted by the log-normal distribution for halos with the masses larger than ~10^8 Msun. The subhalo abundance depends on the halo mass. Galaxy-sized halos have 50% more subhalos than ~10^11 Msun halos have. This is snapshot 549 of the 2048³ resolution collection.
DOI: 10.25606/surf.578c6039-c24d5659
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (2048-586)

description: We present the results of the "Cosmogrid" cosmological N-body simulation suites based on the concordance LCDM model. The Cosmogrid simulation was performed in a 30 Mpc box with 2048³ particles. The mass of each particle is 1.28x10^5 Msun, which is sufficient to resolve ultra-faint dwarfs. We found that the halo mass function shows good agreement with the Sheth & Tormen fitting function down to ~10^7 Msun. We have analyzed the spherically averaged density profiles of the three most massive halos which are of galaxy group size and contain at least 170 million particles. The slopes of these density profiles become shallower than -1 at the inner most radius. We also find a clear correlation of halo concentration with mass. The mass dependence of the concentration parameter cannot be expressed by a single power law, however a simple model based on the Press-Schechter theory proposed by Navarro et al. gives reasonable agreement with this dependence. The spin parameter does not show a correlation with the halo mass. The probability distribution functions for both concentration and spin are well fitted by the log-normal distribution for halos with the masses larger than ~10^8 Msun. The subhalo abundance depends on the halo mass. Galaxy-sized halos have 50% more subhalos than ~10^11 Msun halos have. This is snapshot 586 of the 2048³ resolution collection.
DOI: 10.25606/surf.578c6039-eced3e08
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (2048-587)

description: We present the results of the "Cosmogrid" cosmological N-body simulation suites based on the concordance LCDM model. The Cosmogrid simulation was performed in a 30 Mpc box with 2048³ particles. The mass of each particle is 1.28x10^5 Msun, which is sufficient to resolve ultra-faint dwarfs. We found that the halo mass function shows good agreement with the Sheth & Tormen fitting function down to ~10^7 Msun. We have analyzed the spherically averaged density profiles of the three most massive halos which are of galaxy group size and contain at least 170 million particles. The slopes of these density profiles become shallower than -1 at the inner most radius. We also find a clear correlation of halo concentration with mass. The mass dependence of the concentration parameter cannot be expressed by a single power law, however a simple model based on the Press-Schechter theory proposed by Navarro et al. gives reasonable agreement with this dependence. The spin parameter does not show a correlation with the halo mass. The probability distribution functions for both concentration and spin are well fitted by the log-normal distribution for halos with the masses larger than ~10^8 Msun. The subhalo abundance depends on the halo mass. Galaxy-sized halos have 50% more subhalos than ~10^11 Msun halos have. This is snapshot 587 of the 2048³ resolution collection.
DOI: 10.5281/zenodo.2652202
title: Hydrodynamics-MariakerkeApril2018

description: Hydrodynamics (ADCP) and suspended sediment concentrations (OBS) at Mariakerke in April 2018
DOI: 10.5281/zenodo.2652203
title: Hydrodynamics-MariakerkeApril2018

description: Hydrodynamics (ADCP) and suspended sediment concentrations (OBS) at Mariakerke in April 2018