cometadata/datacite-titles-descriptions-related-identifiers huggingface dataset:
DOI: 10.5517/ccdc.csd.cc14m564
title: CCDC 1061105: Experimental Crystal Structure Determination

description: Related Article: Sihem Yebedri, Oussama Nehar, Radia Mahboub, Thierry Roisnel, Leila Boukli-Hacene, Samira Louhibi|2019|J.Mol.Struct.|1193|45|doi:10.1016/j.molstruc.2019.05.020
description: An entry from the Cambridge Structural Database, the world’s repository for small molecule crystal structures. The entry contains experimental data from a crystal diffraction study. The deposited dataset for this entry is freely available from the CCDC and typically includes 3D coordinates, cell parameters, space group, experimental conditions and quality measures.
DOI: 10.5517/ccdc.csd.cc1n0zg3
title: CCDC 1520285: Experimental Crystal Structure Determination

description: Related Article: Rahma Jabbar, Francois Michaud, Slaheddine Kamoun|2019|Solid State Sciences|94|8|doi:10.1016/j.solidstatesciences.2019.04.012
description: An entry from the Cambridge Structural Database, the world’s repository for small molecule crystal structures. The entry contains experimental data from a crystal diffraction study. The deposited dataset for this entry is freely available from the CCDC and typically includes 3D coordinates, cell parameters, space group, experimental conditions and quality measures.
DOI: 10.5517/ccdc.csd.cc1nlvgk
title: CCDC 1537459: Experimental Crystal Structure Determination

description: Related Article: Abdulrahman I. Almansour, Raju Suresh Kumar, Natarajan Arumugam, Giulia Bianchini, J. Carlos Menéndez, Dhaifallah M. Al-thamili, Govindasami Periyasami, Mohammad Altaf|2019|Tetrahedron Lett.|60|1514|doi:10.1016/j.tetlet.2019.05.010
description: An entry from the Cambridge Structural Database, the world’s repository for small molecule crystal structures. The entry contains experimental data from a crystal diffraction study. The deposited dataset for this entry is freely available from the CCDC and typically includes 3D coordinates, cell parameters, space group, experimental conditions and quality measures.
DOI: 10.7910/dvn/iapq3x/hqsyke
title: Prepare BEST gridded data.do

description: Prepares best_gridded.dta
DOI: 10.7910/dvn/iapq3x/vhanlq
title: ged_data.tab

description: Contains data on violent events from the Georeferenced Event Data (GED) data, version 17.1.
DOI: 10.7910/dvn/iapq3x/arftuq
title: Prepare country data.do

description: Prepares countrydata.dta
DOI: 10.7910/dvn/iapq3x/rmdn1o
title: willmott_gridded.tab

description: Contains gridded monthly temperature data from the Terrestrial Air Temperature: 1900-2014 Gridded Monthly Time Series (V 4.01) (Willmott and Matsuura 2015).
DOI: 10.7910/dvn/iapq3x/v5oooa
title: stations_analysis.tab

description: Consists of station-month data covering stations in the Global Climate Observing System (GCOS) Surface Network (GSN) located SSA during the period 1973-2016. This file is used for tests on the effect of conflict on station loss in section 1.
DOI: 10.7910/dvn/iapq3x/wrgnvu
title: Prepare GED data.do

description: Prepares ged_data.dta
DOI: 10.7910/dvn/iapq3x/mpbh82
title: cru_ts_gridded.tab

description: Contains gridded monthly temperature data from the University of East Anglia’s Climatic Research Unit (CRU), version 3.25.
DOI: 10.7910/dvn/iapq3x/q1lkwh
title: country_analysis.tab

description: Consists of country-year level observations for countries in sub-Saharan Africa (SSA) in the period 1946-2016. This file is used for all tests on country-year level analysis, including tests on coverage in section 1, on bias and measurement error in section 2, and the relationship between temperature and conflict in section 3.
DOI: 10.7910/dvn/iapq3x/uya9g8
title: Run tests for ITE -- Conflict.do

description: Performs tests on the effect of temperature on civil conflict reported in section 3, particularly Figure 7 and A3.
DOI: 10.7910/dvn/iapq3x/qyq8py
title: Prepare Willmott gridded data.do

description: Prepares gsn_data.dta
DOI: 10.7910/dvn/iapq3x/xskhrq
title: Make BEST analysis data.do

description: Makes best_analysis.dta
DOI: 10.7910/dvn/iapq3x/yhjhm4
title: Run tests for ITE -- Bias.do

description: Performs tests on bias in the CRU data reported in section 2, particularly Figures 5 and A2.
DOI: 10.7910/dvn/iapq3x/hutpyf
title: cru_stations.tab

description: Contains station-year data on stations used in the CRU data set.
DOI: 10.7910/dvn/iapq3x/pd3fsd
title: Make GSN station analsysis data.do

description: Makes stations_analysis.dta
DOI: 10.7910/dvn/iapq3x/tcbss7
title: Prepare GSN data.do

description: :unav
DOI: 10.7910/dvn/iapq3x/uigthu
title: Run tests for ITE -- Station loss.do

description: Performs tests on station loss reported in section 1, particularly Table 2 and Figure A1 in the appendix.
DOI: 10.7910/dvn/iapq3x/f33jhk
title: Prepare BEST station data.do

description: Prepares best_stations.dta
DOI: 10.7910/dvn/iapq3x/pcelke
title: temperature_analysis.tab

description: Consists of grid-cell month level observations covering the land area of SSA at 0.5 degree resolution from 1946-2016. This file is used for tests on bias and measurement error in section 2.
DOI: 10.7910/dvn/iapq3x/v1ityb
title: Prepare CRU station data.do

description: Prepares cru_stations.dta
DOI: 10.7910/dvn/iapq3x/fvicxa
title: Run tests for ITE -- Measurement error.do

description: Performs tests on measurement error reported in section 2, particularly Figure 6 and Tables 3 and A1.
DOI: 10.7910/dvn/iapq3x/lhdzjm
title: gsn_data.tab

description: Contains station-month data on stations in the Global Climate Observing System (GCOS) Surface Network (GSN).
DOI: 10.7910/dvn/iapq3x/ohhonu
title: readme.txt

description: :unav
DOI: 10.7910/dvn/iapq3x/xgjxim
title: best_stations.tab

description: Contains station-month data on stations used in the BEST data set.
DOI: 10.7910/dvn/iapq3x/0cfcnt
title: Make temperature analysis data.do

description: Makes temperature_analysis.dta
DOI: 10.7910/dvn/iapq3x/aca8ob
title: countrydata.tab

description: Contains raw country-year data.
DOI: 10.7910/dvn/iapq3x/w9kdlt
title: ghcn_cams_gridded.tab

description: Contains gridded monthly temperature data from the Global Historical Climatology Network - Climate Anomaly Monitoring System (GHCN-CAMS) gridded 2m land temperature data.
DOI: 10.7910/dvn/iapq3x/fkhz8n
title: Run tests for ITE -- Coverage.do

description: Performs tests on variation in coverage at the country level reported in section 1, particularly the analysis around Figures 1-4 and Table 1.
DOI: 10.7910/dvn/iapq3x/vaagka
title: best_analysis.tab

description: Consists of grid-cell month level observations covering the land area of SSA at 1.0 degree resolution from 1946-2016. This file is used for tests on bias in section 2.
DOI: 10.7910/dvn/iapq3x/wkyy5v
title: Make country analysis data.do

description: Makes country_analysis.dta
DOI: 10.7910/dvn/iapq3x/chtbqm
title: best_gridded.tab

description: Contains gridded monthly temperature data from the Berkeley Earth surface temperature (BEST) project.
DOI: 10.7910/dvn/iapq3x/w2evxr
title: Prepare GHCN CAMS gridded data.do

description: Prepares ghcn_cams_gridded.dta
DOI: 10.7910/dvn/iapq3x/z8sa2m
title: Prepare CRU_TS gridded data.do

description: Prepares cru_ts_gridded.dta
DOI: 10.17632/65pgmz9rtn.1
title: Image-processing software for detecting particles moving in micro-pier structure driven by the contractions of cardiomyocyte bridge

description: This program (main.py, OpenCV, written by Python) provides the XY-position of particles in each frame of the original movie (255.m4v) and a movie with circles indicating the particle positions (255_result.mp4). For the analysis of particle displacement, we used the distribution of brightness around the target particle as a template, where the area of the particle in a movie image is brighter than the other area (255_result.txt). The detected XY-position of the template was determined as the XY-position of the particle in the frame.
DOI: 10.17632/pp5kx8bh7b.1
title: Image-processing software for detecting the edge of micro-pier structure driven by the contractions of cardiomyocyte bridge

description: This program (detectWall.py, OpenCV, written by Python) provides the X-position of the pier from the original movie (230.m4v) and a movie with detected lines indicating the pier edges (230_20190207191754_wall.mp4). For the analysis of pier displacement, we used the feature of pier in the movie data, where the area of pier in a movie image is brighter than the other area. First, the template of brightness corresponding to the pier and non-pier areas was prepared, and then, the template matching was performed in each frame of the movie (230_20190207191754.all.txt, 230_20190207191754.wall.txt). The detected X-position of the template was determined as the X-position of the pier in the frame.
DOI: 10.5281/zenodo.2747010
title: Database of Russian names, surnames and midnames for gender identification

description: Database of names, surnames and midnames across the Russian federation used as source to teach algorithms for gender identification by fullname.

Dataset prepared for MongoDB database. It has MongoDB dump and dump of tables as JSON lines files.

Used in gender identification and fullname parsing software https://github.com/datacoon/russiannames

Available under Creative Commons CC-BY SA by default.
DOI: 10.5281/zenodo.2747011
title: Database of Russian names, surnames and midnames for gender identification

description: Database of names, surnames and midnames across the Russian federation used as source to teach algorithms for gender identification by fullname.

Dataset prepared for MongoDB database. It has MongoDB dump and dump of tables as JSON lines files.

Used in gender identification and fullname parsing software https://github.com/datacoon/russiannames

Available under Creative Commons CC-BY SA by default.
DOI: 10.25606/surf.578c6039-90f06309
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (2048-702)

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 702 of the 2048³ resolution collection.
DOI: 10.25606/surf.578c6039-61e55226
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (2048-672)

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 672 of the 2048³ resolution collection.
DOI: 10.25606/surf.578c6039-d6efb2f3
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (2048-673)

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 673 of the 2048³ resolution collection.
DOI: 10.25606/surf.578c6039-f8b633ae
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (2048-704)

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 704 of the 2048³ resolution collection.
DOI: 10.25606/surf.578c6039-22f82549
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (2048-714)

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 714 of the 2048³ resolution collection.
DOI: 10.25606/surf.578c6039-37df8e4b
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (2048-715)

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 715 of the 2048³ resolution collection.
DOI: 10.25606/surf.578c6039-51ca025f
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (2048-719)

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 719 of the 2048³ resolution collection.
DOI: 10.25606/surf.578c6039-e901964e
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (2048-716)

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 716 of the 2048³ resolution collection.
DOI: 10.25606/surf.578c6039-07807172
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (2048-717)

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 717 of the 2048³ resolution collection.