cometadata/datacite-titles-descriptions-related-identifiers huggingface dataset:
DOI: 10.5281/zenodo.3470389
title: Surface nuclear magnetic resonance survey in Lexington, NE 29 March 2010

description: This is a surface nuclear magnetic resonance dataset collected on 29 March 2010 in Lexington NE, USA. <strong>Instrument</strong>: Vista Clara, GMR <strong>Static magnetic field</strong>: 53,761 nT <strong>B field Inclination</strong>: 68.0 (NOAA derived) <strong>B field declination:</strong> 0 (the transmitter loop is aligned along magnetic north within compass accuracy) <strong>Transmitter loop type</strong>: 100 m square loop <strong>Pulse type</strong>: FID, 40 ms <strong>Transmitter channel:</strong> Ch. 1 <strong>Reference Channels: </strong>Ch. 2 and Ch. 3 <strong>Conductivity mode</strong>l: TEM derived Top (m) Bottom (m) Thickness (m) Resistivity (Ohm m) Layer 1 0.00 15.49 15.49 16.91 Layer 2 15.49 43.67 28.18 24.06 Layer 3 43.67 inf inf 33.23 The dataset had 18 stacks, but stack 1 is corrupted and not included.
description: {"references": ["Irons, T.P., Hobza, C.M., Steele, G.V., Abraham, J.D., Cannia, J.C., Woodward, D.D., 2012, Quantification of aquifer properties with surface nuclear magnetic resonance in the Platte River valley, central Nebraska, using a novel inversion method: U.S. Geological Survey Scientific Investigations Report 2012\u20135189, 50 p."]}
DOI: 10.5281/zenodo.3470390
title: Surface nuclear magnetic resonance survey in Lexington, NE 29 March 2010

description: This is a surface nuclear magnetic resonance dataset collected on 29 March 2010 in Lexington NE, USA. <strong>Instrument</strong>: Vista Clara, GMR <strong>Static magnetic field</strong>: 53,761 nT <strong>B field Inclination</strong>: 68.0 (NOAA derived) <strong>B field declination:</strong> 0 (the transmitter loop is aligned along magnetic north within compass accuracy) <strong>Transmitter loop type</strong>: 100 m square loop <strong>Pulse type</strong>: FID, 40 ms <strong>Transmitter channel:</strong> Ch. 1 <strong>Reference Channels: </strong>Ch. 2 and Ch. 3 <strong>Conductivity mode</strong>l: TEM derived Thickness Resistivity (Ohm m) Layer 1 15.49 16.91 Layer 2 28.18 24.06 Layer 3 inf 33.23 The dataset had 18 stacks, but stack 1 is corrupted and not included.
description: {"references": ["Irons, T.P., Hobza, C.M., Steele, G.V., Abraham, J.D., Cannia, J.C., Woodward, D.D., 2012, Quantification of aquifer properties with surface nuclear magnetic resonance in the Platte River valley, central Nebraska, using a novel inversion method: U.S. Geological Survey Scientific Investigations Report 2012\u20135189, 50 p."]}
DOI: 10.25606/surf.578c6039-4ed82588
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (2048-525)

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 525 of the 2048³ resolution collection.
DOI: 10.25606/surf.578c6039-65fdfe40
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (2048-734)

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 734 of the 2048³ resolution collection.
DOI: 10.5281/zenodo.3457537
title: Supplementary Data for Massively Parallel Implicit Equal-Weights Particle Filter for Ocean Drift Trajectory Forecasting

description: This data repository is provided as a supplement to the paper *Massively Parallel Implicit Equal-Weights Particle Filter for Ocean Drift Trajectory Forecasting* written by Håvard Heitlo Holm, Martin Lilleeng Sætra and Peter Jan van Leeuwen. It contains the complete datasets (initial conditions and results of the ensemble simulations) obtained from the experiments presented therein. This data set is generated by, and can be further post-processed and visualized by, the code published as *metno/gpu-ocean: Supplementary Software for Massively Parallel Implicit Equal-Weights Particle Filter for Ocean Drift Trajectory Forecasting* by Håvard Heitlo Holm, Martin Lilleeng Sætra and André Rigland Brodtkorb (DOI 10.5281/zenodo.3458291).
description: HHH and MLS thanks the Research Council of Norway for funding the GPU Ocean project, with grant number 250935. PJvL thanks the European Research Council for funding the CUNDA grant 694509 under the European Union's Horizon 2020 research and innovation programme. Some of the computations were performed on resources provided by UNINETT Sigma2 -- the National Infrastructure for High Performance Computing and Data Storage in Norway under project number nn9550k.
DOI: 10.25606/surf.578c6039-1d2ddfd8
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (2048-558)

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 558 of the 2048³ resolution collection.
DOI: 10.25606/surf.578c6039-87666b61
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (2048-156)

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 156 of the 2048³ resolution collection.
DOI: 10.5281/zenodo.3457538
title: Supplementary Data for Massively Parallel Implicit Equal-Weights Particle Filter for Ocean Drift Trajectory Forecasting

description: This data repository is provided as a supplement to the paper *Massively Parallel Implicit Equal-Weights Particle Filter for Ocean Drift Trajectory Forecasting* written by Håvard Heitlo Holm, Martin Lilleeng Sætra and Peter Jan van Leeuwen. It contains the complete datasets (initial conditions and results of the ensemble simulations) obtained from the experiments presented therein. This data set is generated by, and can be further post-processed and visualized by, the code published as *metno/gpu-ocean: Supplementary Software for Massively Parallel Implicit Equal-Weights Particle Filter for Ocean Drift Trajectory Forecasting* by Håvard Heitlo Holm, Martin Lilleeng Sætra and André Rigland Brodtkorb (DOI 10.5281/zenodo.3458291).
description: HHH and MLS thanks the Research Council of Norway for funding the GPU Ocean project, with grant number 250935. PJvL thanks the European Research Council for funding the CUNDA grant 694509 under the European Union's Horizon 2020 research and innovation programme. Some of the computations were performed on resources provided by UNINETT Sigma2 -- the National Infrastructure for High Performance Computing and Data Storage in Norway under project number nn9550k.
DOI: 10.25606/surf.578c6039-7b49728b
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (2048-503)

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 503 of the 2048³ resolution collection.
DOI: 10.25606/surf.578c6039-81d49007
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (2048-751)

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 751 of the 2048³ resolution collection.
DOI: 10.25606/surf.578c6039-aba78562
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (2048-599)

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 599 of the 2048³ resolution collection.
DOI: 10.25606/surf.578c6039-60e0a19c
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (2048-650)

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 650 of the 2048³ resolution collection.
DOI: 10.25606/surf.578c6039-da3a2977
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (2048-541)

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 541 of the 2048³ resolution collection.
DOI: 10.5519/qd.hk502zos
title: Query on the Natural History Museum Data Portal (data.nhm.ac.uk) (31 records)
DOI: 10.5519/qd.mx6f5k8r
title: Query on the Natural History Museum Data Portal (data.nhm.ac.uk) (3061 records)
DOI: 10.14457/cu.the.2010.1156
title: Social-economic impact of R3 road on Thailand, Lao PDR and Yunnan province (PRC) with focus on Lao PDR

description: This study focused on studying the social-economic impacts from the R3 road on Lao PDR; particularly, on Bokeo Province and Luang Namtha Province. There were two levels in this research. First, the study on Bokeo and Luang Namtha provincial social-economic development which focused on three sectors: trade, investment, and agriculture. It provided a wider view on economic development of the two provinces. Second, the study was on the social-economic impacts on local communities adjacent to the R3 road. Twelve villages along the R3 road were studied in this research. In Huaysai District, Bokeo Province, there were five villages; and in Namtha District, Luang Namtha province, seven villages were studied on social-economic impacts of the R3 road. The research findings showed that the R3 road contributed to economic development on Thailand, Lao PDR and Yunnan Province, People’s Republic of China. The explicit evidences were the volume of trade among three parties has increased sharply since the completion of the R3 road in February 2008. The trans-border trade between Thailand and China increased more than two times from 2008 to 2009; thanks to the R3 road. Moreover, the R3 road provides better transportation, markets, economic opportunities, education, accessibility to healthcare services, and other services to Lao ethnic people along the road. However, the findings from case studies showed that the R3 road created negative social impacts to villagers in two aspects. First, the R3 road physical impacts such as land compensation, drainage system, road accidents, and the increase of land prices. Second, the impacts were from developments on the R3 road area; mainly, the investments. Therefore, this study revealed social-economic impacts of R3 and gave suggestions for problems on Lao PDR.
DOI: 10.14457/cu.the.2010.1157
title: The evolution of architectural style of mosques in Bangkok (1782-2010)

description: The main purpose of the thesis is to study the evolution of architectural style of mosques in Bangkok during 1782-2010. A number of local and foreign factors have influenced the architectural style of mosques in Bangkok including ethnic groups, identity, the urbanization of Bangkok, development of construction materials, architectural style from the foreign countries in particular Islamic countries and European countries. The architectural style of mosques in Bangkok can be according to the evolution of the architectural technique and social development process into three periods. Such periods are: 1. The Mosques during the Early Rattanakosin Period (1782-1855). During this period, there were many mosques were built by the vernacular architecture such as wood and bamboo following the tropical climate and Thai traditional architecture. Some prominent mosques were merely constructed by the brick which were similar to the Buddhist monastery in order to represent the mosque as the sacred place for worshipping Allah as well. 2. The Mosque during the Modernization Period (1855-1932). According to the colonialism and the Bowring Treaty, there were many Muslim from the colonial nations migrated to Siam. This and a technological development in terms of transportation, material and construction have resulted in the fact that mosques were built in various styles. Such styles are: the applied Thai style, the European style, the style of West Asia and the colonial nation style. 3. The Mosques in Bangkok during the Contemporary Period (1932- 2010).During this time, there are various styles according to social, architectural development and function. Some mosques are mostly renovated from the old ones. They have been used for additional functions including being the Islamic center and the head office of the Islamic Affair administration. However, many mosques were designed by the West-Asia architectural style which is dominated by dome and minarat.