cometadata/datacite-titles-descriptions-related-identifiers huggingface dataset:
DOI: 10.5281/zenodo.3468616
title: WWV Centennial Recording of WWV 5 MHz from Western PA, U.S.A.- NA0B

description: Festival of Frequency Measurement 1 October 2019 UTC Date 20191001 Beacon Frequency: 5.000.000 Station Name: NA0B Latitud: 40.30.950 N Longitud: 79 55.353 W Grid: FN00am City: O'Hara Township, PA SF=69, A=12, K=1 at the end of measurament Equipment: Flexradio FLEX-6000M with GPS module, 24 hours warm up SW: fldigi 4.1.08 Released publicly under Creative Commons: YES
description: Start time of .csv file: 23:47:59 20190930 Antenna: EFHW-80 mounted in slope configuration from about 30' to about 70' Receiver Type: SDR FLEX-6000M Frequency Reference type: 10 Mhz GPS disciplined oscillator Frequency Measurement technique: Fldigi frequency analysis mode. No need to adjust ppm.
DOI: 10.5281/zenodo.3468617
title: WWV Centennial Recording of WWV 5 MHz from Western PA, U.S.A.- NA0B

description: Festival of Frequency Measurement 1 October 2019 UTC Date 20191001 Beacon Frequency: 5.000.000 Station Name: NA0B Latitud: 40.30.950 N Longitud: 79 55.353 W Grid: FN00am City: O'Hara Township, PA SF=69, A=12, K=1 at the end of measurament Equipment: Flexradio FLEX-6000M with GPS module, 24 hours warm up SW: fldigi 4.1.08 Released publicly under Creative Commons: YES
description: Start time of .csv file: 23:47:59 20190930 Antenna: EFHW-80 mounted in slope configuration from about 30' to about 70' Receiver Type: SDR FLEX-6000M Frequency Reference type: 10 Mhz GPS disciplined oscillator Frequency Measurement technique: Fldigi frequency analysis mode. No need to adjust ppm.
DOI: 10.25606/surf.578c6039-744ea7b5
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (2048-190)

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 190 of the 2048³ resolution collection.
DOI: 10.25606/surf.578c6039-b61b1cd2
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (2048-534)

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 534 of the 2048³ resolution collection.
DOI: 10.5281/zenodo.3463589
title: A Convolutional Neural Network classifier identifies tree species in mixed-conifer forest from hyperspectral imagery

description: Digital Publication of the training data polygons and hyperspectral imagery used in the manuscript "A Convolutional Neural Network classifier identifies tree species in mixed-conifer forest from hyperspectral imagery". Code is available in a Jupyter Notebook and can be found here: https://github.com/jonathanventura/canopy National Ecological Observatory Network. 2018. Provisional data downloaded from http://data.neonscience.org on 22 June 2018. Battelle, Boulder, CO, USA
description: Data to replicate the experiment is available for download in two zipped files: "NEON_D17_TEAK_DP1QA_20170627_181333_RGB_Reflectance.zip" (Imagery) "CNN_LABELS_2019.zip" (Training Label Shapefiles) * Note: The imagery is 5.5 gb (zipped). All code used to run the analysis is located in a repository here: https://github.com/jonathanventura/canopy The only flightline you will need to repeat our results is called "NEON_D17_TEAK_DP1_20170627_181333". If you download your own NEON data, the raw HDF 5 files can be converted to a geotiff using R code found here: http://neonscience.github.io/neon-data-institute-2016//R/open-NEON-hdf5-functions/ Contact the National Ecological Observatory Network (NEON) to download the comparable imagery data files for all sites and collections: https://data.neonscience.org/home.
DOI: 10.5281/zenodo.3468535
title: weecology/PortalData 1.132.0

description: Official Repo of the Portal Project Data
DOI: 10.5281/zenodo.3463701
title: ai-matrix SSD_Tensorflow

description: Large files in ai-matrix.
DOI: 10.5281/zenodo.3463702
title: ai-matrix SSD_Tensorflow

description: Large files in ai-matrix.
DOI: 10.5281/zenodo.3463705
title: ai-matrix SegLink

description: Large files in ai-matrix.
DOI: 10.5281/zenodo.3463699
title: ai-matrix NMT

description: Large files in ai-matrix.
DOI: 10.5281/zenodo.3467427
title: Chronicle of Nature - Phenology of Mammals of FSE Zapovednoe Podlemorye

description: Mammals Phenology dataset compiled in the context of Chronicle of Nature program in FSE Zapovednoe Podlemorye (Russian Federation) consisting of 126 records collected during 72 years between 1940 and 2014.
description: This dataset export was created by EarthCape software platform version 18.3.1.17814
DOI: 10.5281/zenodo.3467428
title: Chronicle of Nature - Phenology of Mammals of FSE Zapovednoe Podlemorye

description: Mammals Phenology dataset compiled in the context of Chronicle of Nature program in FSE Zapovednoe Podlemorye (Russian Federation) consisting of 126 records collected during 72 years between 1940 and 2014.
description: This dataset export was created by EarthCape software platform version 18.3.1.17814
DOI: 10.15468/fwhwbp
title: Description of the Adult Male of Stylops advarians Pierce (Strepsiptera: Stylopidae)

description: This dataset contains the digitized treatments in Plazi based on the original journal article Balzer, Zachary S., Davis, Arthur R. (2019): Description of the Adult Male of Stylops advarians Pierce (Strepsiptera: Stylopidae). Zootaxa 4674 (4): 496-500, DOI: https://doi.org/10.11646/zootaxa.4674.4.9
DOI: 10.25606/surf.578c6039-5585f8ec
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (2048-649)

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 649 of the 2048³ resolution collection.
DOI: 10.15468/ysroyw
title: Description of a new Central African earthworm, Petroscolex centenarius gen et sp. nov. (Crassiclitellata, Eudrilidae), celebrating the 100 th birthday of Pietro Omodeo

description: This dataset contains the digitized treatments in Plazi based on the original journal article Csuzdi, Csaba, Rota, Emilia, Szederjesi, Tímea, Sherlock, Emma, Brown, George G., Chang, Chih-Han, Cosin, Dario Diaz, Fragoso, Carlos, Jamieson, Barrie G. M., Hong, Yong, James, Samuel W., Paoletti, Maurizio G., Pavlícek, Tomás, Plisko, Danuta, Pop, Victor V., Shen, Huei-Ping (2019): Description of a new Central African earthworm, Petroscolex centenarius gen et sp. nov. (Crassiclitellata, Eudrilidae), celebrating the 100 th birthday of Pietro Omodeo. Zootaxa 4674 (5): 501-508, DOI: 10.11646/zootaxa.4674.5.1
DOI: 10.5281/zenodo.3468634
title: A GVC-type CGE Model

description: This dataset is created from WIOD dataset. (See http://www.wiod.org/home) The WIOD table of the year 2014 is aggregated into four regions ,the US, China, the European Union (EU28), and the rest of the world (ROW). Industries are aggregated into eighteen classifications according to ISIC Rev4 scheme. See aggregating.gms for details. .gdx files are aggregated MRIO table stored in GAMS and ready to run. The .txt file provide the calculation details of sliced value-added.
description: {"references": ["Timmer, M. P., Dietzenbacher, E., Los, B., Stehrer, R. and de Vries, G. J. (2015), \"An Illustrated User Guide to the World Input\u2013Output Database: the Case of Global Automotive Production\", Review of International Economics., 23: 575\u2013605", "E. Dietzenbacher, B. Los, R. Stehrer, M.P. Timmer and G.J. de Vries (2013), \"The Construction of World Input-Output Tables in the WIOD Project\", Economic Systems Research, 25, 71-98."]}
DOI: 10.5281/zenodo.3468635
title: A GVC-type CGE Model

description: This dataset is created from WIOD dataset. (See http://www.wiod.org/home) The WIOD table of the year 2014 is aggregated into four regions ,the US, China, the European Union (EU28), and the rest of the world (ROW). Industries are aggregated into eighteen classifications according to ISIC Rev4 scheme. See aggregating.gms for details. .gdx files are aggregated MRIO table stored in GAMS and ready to run. The .txt file provide the calculation details of sliced value-added.
description: {"references": ["Timmer, M. P., Dietzenbacher, E., Los, B., Stehrer, R. and de Vries, G. J. (2015), \"An Illustrated User Guide to the World Input\u2013Output Database: the Case of Global Automotive Production\", Review of International Economics., 23: 575\u2013605", "E. Dietzenbacher, B. Los, R. Stehrer, M.P. Timmer and G.J. de Vries (2013), \"The Construction of World Input-Output Tables in the WIOD Project\", Economic Systems Research, 25, 71-98."]}
DOI: 10.5281/zenodo.3468763
title: Festival of Frequency Measurement 1 October 2019 for WWV 5 MHz - Toby Haynes VE7CNF

description: Festival of Frequency Measurement 1 October 2019 for WWV 5 MHz Toby Haynes VE7CNF<br> Location: 49.266918N 122.900887W Grid CN89ng Burnaby, BC, Canada<br> Start Time: 2019 Sept 30 at 23:58 UTC<br> End time: 2019 Oct 2 at 00:02 UTC<br> Antenna: "Inverted L" vertical with ICOM AH-4 auto tuner, 50 ft high, 70 ft horizontal top wire.<br> Receiver: ICOM IC-7410 with internal TCXO reference and internal USB sound card chip with separate clock crystal.<br> Receiver in USB mode with carrier frequency 4998.5 kHz to give a 1500 Hz audio tone for the WWV 5 MHz carrier.<br> Measurement: 1500 Hz tone frequency estimated using program FLDigi v4.1.08 in frequency analysis mode. There was a drop in the WWV 5 MHz signal level around 15:00 UTC, after which the reduced SNR caused more variation in the FLDigi frequency measurements. Frequency calibration: Before and after the data set, the receiver frequency error was determined by using the receiver and FLDigi to measure a reference 5 MHz sine wave from a Rigol DG1032 function generator with external 10 MHz GPS-disciplined frequency reference (Trimble).<br> The "VE7CNF raw_2019-09-30-1810 UTC.csv" file includes the reference measurements and the data set. The two reference signal measurements were:<br> Receiver frequency error +0.066 Hz averaged for 1 minute starting 2019 Sept 30 at 18:10:25 UTC <br> Receiver frequency error +0.028 Hz averaged for 1 minute starting 2019 Oct 2 at 00:03:10 UTC Receiver frequency error at each time during the data set was then estimated, assuming that the error changed linearly over time betwen the two reference measurements. The estimated receiver frequency errors were applied to correct the data set in "VE7CNF CN89ng 5 MHz_2019-09-30-2358 UTC.csv." The measured WWV 5 MHz frequency error vs time is graphed in "VE7CNF_WWV5MHz_2019-10-01UTC.JPG," with a moving 1-minute average applied to the frequency error. The frequency dropped around 01:30 (local sunset was 01:51 UTC) and increased around 14:00 (local sunrise was 14:13 UTC).<br> <br>
DOI: 10.5281/zenodo.3468764
title: Festival of Frequency Measurement 1 October 2019 for WWV 5 MHz - Toby Haynes VE7CNF

description: Festival of Frequency Measurement 1 October 2019 for WWV 5 MHz Toby Haynes VE7CNF<br> Location: 49.266918N 122.900887W Grid CN89ng Burnaby, BC, Canada<br> Start Time: 2019 Sept 30 at 23:58 UTC<br> End time: 2019 Oct 2 at 00:02 UTC<br> Antenna: "Inverted L" vertical with ICOM AH-4 auto tuner, 50 ft high, 70 ft horizontal top wire.<br> Receiver: ICOM IC-7410 with internal TCXO reference and internal USB sound card chip with separate clock crystal.<br> Receiver in USB mode with carrier frequency 4998.5 kHz to give a 1500 Hz audio tone for the WWV 5 MHz carrier.<br> Measurement: 1500 Hz tone frequency estimated using program FLDigi v4.1.08 in frequency analysis mode. There was a drop in the WWV 5 MHz signal level around 15:00 UTC, after which the reduced SNR caused more variation in the FLDigi frequency measurements. Frequency calibration: Before and after the data set, the receiver frequency error was determined by using the receiver and FLDigi to measure a reference 5 MHz sine wave from a Rigol DG1032 function generator with external 10 MHz GPS-disciplined frequency reference (Trimble).<br> The "VE7CNF raw_2019-09-30-1810 UTC.csv" file includes the reference measurements and the data set. The two reference signal measurements were:<br> Receiver frequency error +0.066 Hz averaged for 1 minute starting 2019 Sept 30 at 18:10:25 UTC <br> Receiver frequency error +0.028 Hz averaged for 1 minute starting 2019 Oct 2 at 00:03:10 UTC Receiver frequency error at each time during the data set was then estimated, assuming that the error changed linearly over time betwen the two reference measurements. The estimated receiver frequency errors were applied to correct the data set in "VE7CNF CN89ng 5 MHz_2019-09-30-2358 UTC.csv." The measured WWV 5 MHz frequency error vs time is graphed in "VE7CNF_WWV5MHz_2019-10-01UTC.JPG," with a moving 1-minute average applied to the frequency error. The frequency dropped around 01:30 (local sunset was 01:51 UTC) and increased around 14:00 (local sunrise was 14:13 UTC).<br> <br>
DOI: 10.15468/mtyii6
title: Description of a new species of Willemia (Collembola: Hypogastruridae) from Panama with key to Willemia species occurring in the Americas

description: This dataset contains the digitized treatments in Plazi based on the original journal article García-Gómez, Arturo, Palacios-Vargas, José G. (2019): Description of a new species of Willemia (Collembola: Hypogastruridae) from Panama with key to Willemia species occurring in the Americas. Zootaxa 4674 (5): 564-570, DOI: https://doi.org/10.11646/zootaxa.4674.5.5
DOI: 10.25606/surf.578c6039-57eab9a0
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (2048-620)

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 620 of the 2048³ resolution collection.
DOI: 10.5281/zenodo.3468636
title: Festival of Frequency Measurement 1 October 2019 WB4HIR

description: Festival of Frequency Measurement 1 October 2019 Rodger Adams, WB4HIR WWV 5 MHZ Start time 21:02:38 UTC Sept. 30 2019 Stop time 1:27:03 UTC Oct. 2 2019 Antenna, attic mount, 70 ft balanced doublet Kenwood TS-590s receiver with TCXO FLDIGI in analysis mode, Receiver tuned to 4.999 USB mode Lat 35.08N Long 80.83W Alt 619 ft above MSL EM95OB Charlotte, NC
DOI: 10.5281/zenodo.3468637
title: Festival of Frequency Measurement 1 October 2019 WB4HIR

description: Festival of Frequency Measurement 1 October 2019 Rodger Adams, WB4HIR WWV 5 MHZ Start time 21:02:38 UTC Sept. 30 2019 Stop time 1:27:03 UTC Oct. 2 2019 Antenna, attic mount, 70 ft balanced doublet Kenwood TS-590s receiver with TCXO FLDIGI in analysis mode, Receiver tuned to 4.999 USB mode Lat 35.08N Long 80.83W Alt 619 ft above MSL EM95OB Charlotte, NC
DOI: 10.5281/zenodo.3468723
title: Festival of Frequency Measurement dataset - WV5L 34.10 -84.46 5 MHz Oct 1 2019

description: Festival of Frequency Measurement Submission event: WWV Centenial UTC Date: 01 Oct 2019 (starting 30 Sep 2300z, ending 2 Oct 0100z) beacon frequency: 5 MHz station name: WV5L, operated by Vance Loen lat long: 34.10 -84.46 city: Woodstock state: Georgia US difficulties: poor propagation Oct 01 from about 1600 to 2000 UTC between Ft. Collins and Woodstock equipment: Icom IC-7610 with Leo Bodnar GPSDO, antenna 96-foot dipole with ladder line (ZS6BKW design) tuning technique: receiver was tuned to 4999.00 KHz, upper sideband, 2.1KHz bandwidth, preamp off, AGC mid, 1 KHz detected audio captured from internal sound card, calibrated and logged by FLDIGI 4.1.08. propagation path: sky wave, about 1215 miles/1955 Km
DOI: 10.5281/zenodo.3468724
title: Festival of Frequency Measurement dataset - WV5L 34.10 -84.46 5 MHz Oct 1 2019

description: Festival of Frequency Measurement Submission event: WWV Centenial UTC Date: 01 Oct 2019 (starting 30 Sep 2300z, ending 2 Oct 0100z) beacon frequency: 5 MHz station name: WV5L, operated by Vance Loen lat long: 34.10 -84.46 city: Woodstock state: Georgia US difficulties: poor propagation Oct 01 from about 1600 to 2000 UTC between Ft. Collins and Woodstock equipment: Icom IC-7610 with Leo Bodnar GPSDO, antenna 96-foot dipole with ladder line (ZS6BKW design) tuning technique: receiver was tuned to 4999.00 KHz, upper sideband, 2.1KHz bandwidth, preamp off, AGC mid, 1 KHz detected audio captured from internal sound card, calibrated and logged by FLDIGI 4.1.08. propagation path: sky wave, about 1215 miles/1955 Km
DOI: 10.25606/surf.578c6039-083e7bb3
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (2048-454)

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 454 of the 2048³ resolution collection.
DOI: 10.5281/zenodo.3468632
title: Festival of Frequency Measurement 1 October 2019

description: Festival of Frequency Measurement 1 October 2019 Event: WWV Centennial UTC Date: 20191001 Beacon frequency: 05.000 000 Name and Callsign: Jimmy Herrera XE3I (X-Ray Eco Three India) Latitude: 21.1742 N Long: -86.8465 W Grid: EL61nc City: Cancun, Quintana Roo - Mexico Difficulties had: No Antenna type: Rotative Dipole (40 mts.) Antenna pointing direction (if applicable): North - South Receiver type: Kenwood TS-590S Frequency reference type: 04.999.00 USB Frequency measurement technique: Fldigi ver 3.23.21 Soapbox: Very interesting experiment.<br> <br> Released publicly under Creative Commons: Yes Open Source: Yes Creative Commons Attribution 4.0: Yes
DOI: 10.5281/zenodo.3468633
title: Festival of Frequency Measurement 1 October 2019

description: Festival of Frequency Measurement 1 October 2019 Event: WWV Centennial UTC Date: 20191001 Beacon frequency: 05.000 000 Name and Callsign: Jimmy Herrera XE3I (X-Ray Eco Three India) Latitude: 21.1742 N Long: -86.8465 W Grid: EL61nc City: Cancun, Quintana Roo - Mexico Difficulties had: No Antenna type: Rotative Dipole (40 mts.) Antenna pointing direction (if applicable): North - South Receiver type: Kenwood TS-590S Frequency reference type: 04.999.00 USB Frequency measurement technique: Fldigi ver 3.23.21 Soapbox: Very interesting experiment.<br> <br> Released publicly under Creative Commons: Yes Open Source: Yes Creative Commons Attribution 4.0: Yes