cometadata/datacite-titles-descriptions-related-identifiers huggingface dataset:
DOI: 10.25345/c5k03x
title: MassIVE MSV000083490 - GNPS - Abagyan's lab bioactive compounds screening
title: GNPS - Abagyan's lab bioactive compounds screening
DOI: 10.25919/5c7626b4ca092
title: Parkes observations for project P986 semester 2018OCTS_06

description: Pulsar survey is one of the top priorities of the Square Kilometer Arrays (SKA). The discovery of pulsars in relativistic binaries, pulsars in binary with black holes and pulsars in the Galactic Center (GC) will improve our understanding of gravity theories, physics of black holes and stellar population and environment in the GC region. However, conventional periodic searches for pulsars are only sensitive to strictly periodic signals with low duty cycles. Although various methods have been developed to search for pulsars in these extreme systems, it is still very challenging and computationally expensive. 

One of the solutions is to find pulsar candidates in radio continuum surveys and then carry out targeted searches (e.g. Frail et al 2017). This technique allows a search over the full field of view while avoiding the need for expensive pixel-by-pixel high time resolution searches. We propose to observe 32 compact, steep spectrum candidates selected from NVSS and TGSS surveys using the Ultra-Wideband Low (UWL) receiver. The frequency coverage (as low as 700MHz) and low system temperature (~20K) of UWL will enable us to carry out a sensitive search of steep spectrum sources.
DOI: 10.17632/64p3sh9s68.1
title: Data for: Relationship between auditory pathway fractional anisotropy and audibility in patients with cerebellopontine angle tumors on diffusion tensor imaging

description: Data for tables 1 and 2, figures 2 to 4
DOI: 10.5281/zenodo.2578729
title: RAGE Summative Ecosystem Evaluation

description: <strong>General description: </strong>Data from the system evaluation of the Social Network Mediator integration into the RAGE Ecosystem Portal

<strong>Topic</strong><br>
ACM CSS 2012: ACM CSS 2012: Human-centered computing - Human computer interaction (HCI) - User studies, Usability testing

<strong>Name entitites</strong><br>
Organizational information: Graz University of Technology, Forschungsinstitut für Telekommunikation und Kooperation<br>
Geographical information: Europe

Time information: May-June 2018

<strong>Types</strong>: Excel file

<strong>RAGCS target group:</strong> target groups - supply side - research institutions; industry participants

<strong>Evaluation dimensions</strong><br>
Evaluation object: features and functions of the Social Networking Platforms and Groupware Platforms along with the Visual Interactive Asset Map integrated into the RAGE Ecosystem portal<br>
Evaluation variables: usefulness, usability, quality of the user interface, quality of the tutorial, demographics, added value and other features

<strong>Instruments:</strong> USE questionnaire (usefulness, satisfaction, ease of use; Lund, 2001); items adopted from the System Usability Scale - SUS (Brooke, 1996); items adapted from Thielsch & Stegemöller (2012); questionnaire items defined for the purpose of the evaluation

<strong>Relationships</strong>: D8.4 - Second RAGE Evaluation Report<br>
Related datasets: 10.5281/zenodo.1209192, 10.5281/zenodo.1209198.
DOI: 10.5281/zenodo.2578728
title: RAGE Summative Ecosystem Evaluation

description: <strong>General description: </strong>Data from the system evaluation of the Social Network Mediator integration into the RAGE Ecosystem Portal

<strong>Topic</strong><br>
ACM CSS 2012: ACM CSS 2012: Human-centered computing - Human computer interaction (HCI) - User studies, Usability testing

<strong>Name entitites</strong><br>
Organizational information: Graz University of Technology, Forschungsinstitut für Telekommunikation und Kooperation<br>
Geographical information: Europe

Time information: May-June 2018

<strong>Types</strong>: Excel file

<strong>RAGCS target group:</strong> target groups - supply side - research institutions; industry participants

<strong>Evaluation dimensions</strong><br>
Evaluation object: features and functions of the Social Networking Platforms and Groupware Platforms along with the Visual Interactive Asset Map integrated into the RAGE Ecosystem portal<br>
Evaluation variables: usefulness, usability, quality of the user interface, quality of the tutorial, demographics, added value and other features

<strong>Instruments:</strong> USE questionnaire (usefulness, satisfaction, ease of use; Lund, 2001); items adopted from the System Usability Scale - SUS (Brooke, 1996); items adapted from Thielsch & Stegemöller (2012); questionnaire items defined for the purpose of the evaluation

<strong>Relationships</strong>: D8.4 - Second RAGE Evaluation Report<br>
Related datasets: 10.5281/zenodo.1209192, 10.5281/zenodo.1209198.
DOI: 10.5281/zenodo.1493510
title: Underlying data for "Metabolism of remimazolam in primary human hepatocytes during continuous long-term infusion in a 3D bioreactor system"

description: The dataset supports the manuscript "Metabolism of remimazolam in primary human hepatocytes during continuous long-term infusion in a 3D bioreactor system" published in the journal "Drug design, development and therapy" in 2019
DOI: 10.25606/surf.578c6039-d9eff2de
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (1024-021)

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 021 of the 1024³ resolution collection.
DOI: 10.25606/surf.578c6039-84bc2e7a
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (2048-042)

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 042 of the 2048³ resolution collection.
DOI: 10.25606/surf.578c6039-91201631
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (1024-023)

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 023 of the 1024³ resolution collection.
DOI: 10.25606/surf.578c6039-e27ef58e
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (2048-045)

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 045 of the 2048³ resolution collection.
DOI: 10.25606/surf.578c6039-221d9123
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (1024-016)

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 016 of the 1024³ resolution collection.
DOI: 10.25606/surf.578c6039-620547ce
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (2048-043)

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 043 of the 2048³ resolution collection.
DOI: 10.25606/surf.578c6039-7cdedf3c
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (2048-044)

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 044 of the 2048³ resolution collection.
DOI: 10.25606/surf.578c6039-920992cd
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (2048-035)

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 2048³ resolution collection.
DOI: 10.5281/zenodo.2578950
title: LexiRumah v2.1.2

description: A lexical database of languages of the Lesser Sunda Islands and their suggested relations. Available through an online-interface on https://lexirumah.model-ling.eu


	Minor bugfixes
	Provide Lexibank interface
description: Funding:
Reconstructing the past through languages of the present: the Lesser Sunda Islands
Netherlands Organisation for Scientific Research (The Hague)
GRANT_NUMBER: 277-70-012
URL: https://www.nwo.nl/en/research-and-results/research-projects/i/91/22391.html
DOI: 10.25606/surf.578c6039-17307d78
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (2048-041)

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 041 of the 2048³ resolution collection.
DOI: 10.25606/surf.578c6039-26e4202d
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (2048-040)

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 040 of the 2048³ resolution collection.
DOI: 10.25606/surf.578c6039-30200d9a
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (2048-036)

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 036 of the 2048³ resolution collection.
DOI: 10.25606/surf.578c6039-5fd5f305
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (2048-038)

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 038 of the 2048³ resolution collection.