cometadata/datacite-titles-descriptions-related-identifiers huggingface dataset:
DOI: 10.25606/surf.578c6039-0c8c9310
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (2048-747)

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 747 of the 2048³ resolution collection.
DOI: 10.25606/surf.578c6039-2d2e70f3
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (2048-749)

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 749 of the 2048³ resolution collection.
DOI: 10.25606/surf.578c6039-74a21cf5
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (2048-746)

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 746 of the 2048³ resolution collection.
DOI: 10.25606/surf.578c6039-a7b125da
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (2048-748)

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 748 of the 2048³ resolution collection.
DOI: 10.25919/5cc62f4369dd3
title: Parkes observations for project P991 semester 2019APRS_02

description: Finding radio pulsars orbiting near Sgr A* is a major goal of pulsar surveys with existing telescopes and future telescopes such as the Square Kilometer Array (SKA). The discovery of such pulsars will allow us to measure relativistic effects through timing of pulsars in tight orbits around Sgr A*, to characterise the distribution of dark matter near Sgr A*, to study the stellar population in the GC region and to probe the scattering region around Sgr A*. Although several surveys of the GC region have done, the Ultra-Wideband Low (UWL) receiver provides us a much wider frequency coverage with great sensitivity and therefore it is an excellent chance to revisit the GC region. At around 4GHz, a survey with UWL will achieve a sensitivity significantly higher than previous Parkes and Green Bank surveys, especially for pulsars with short spin periods and high dispersion measures.
DOI: 10.14469/hpc/5563
title: Co(II)-Tetraphenylporphyrin, -1 triplet, C2v, all-up isomer, optimized (Huckel) G=-3294.616684

description: Gaussian Calculation
DOI: 10.21227/102k-hy68
title: Bitcoin Scanner Data (2018)

description: Bitcoin is a decentralized digital currency that has gained significant attention and growth in recent years. Unlike traditional currencies, Bitcoin does not rely on a centralized authority to control the supply, distribution, and verification of the validity of transactions. Instead, Bitcoin relies on a peer-to- peer network of volunteers to distribute pending transactions and confirmed blocks, verify transactions, and to collectively implement a replicated ledger that everyone agrees on. This peer-to-peer (P2P) network is at the heart of Bitcoin and many other blockchain technologies. In this article, we present a comparative measurement study of nodes in the Bitcoin network. We measure and analyze how many so-called ‘volunteers’ are in Bitcoin P2P network by scanning the live Bitcoin network for 37 days in 2018, and compare them with data reported by prior work in 2013∼2016. Our work is motivated by the fact that Bitcoin has experienced explosive growth in terms of number of users, transactions, value, and interest over the recent couple years. Our investigation includes the IP addresses of Bitcoin nodes, size of the network, power-law in the geographic distribution, protocol and client versions, and network latencies, and show how today’s network is different from early days. In addition, based on the observations made from the measurement study, we propose a simple distance-based peer selection rule for improved connectivity and faster data propagation. Evaluation results show that our proposed light-weight and backward-compatible peer selection rule has potential to reduce data dissemination latency.
DOI: 10.21227/cg6f-0f59
title: Bitcoin Scanner Data (2018)

description: Bitcoin is a decentralized digital currency that has gained significant attention and growth in recent years. Unlike traditional currencies, Bitcoin does not rely on a centralized authority to control the supply, distribution, and verification of the validity of transactions. Instead, Bitcoin relies on a peer-to- peer network of volunteers to distribute pending transactions and confirmed blocks, verify transactions, and to collectively implement a replicated ledger that everyone agrees on. This peer-to-peer (P2P) network is at the heart of Bitcoin and many other blockchain technologies. In this article, we present a comparative measurement study of nodes in the Bitcoin network. We measure and analyze how many so-called ‘volunteers’ are in Bitcoin P2P network by scanning the live Bitcoin network for 37 days in 2018, and compare them with data reported by prior work in 2013∼2016. Our work is motivated by the fact that Bitcoin has experienced explosive growth in terms of number of users, transactions, value, and interest over the recent couple years. Our investigation includes the IP addresses of Bitcoin nodes, size of the network, power-law in the geographic distribution, protocol and client versions, and network latencies, and show how today’s network is different from early days. In addition, based on the observations made from the measurement study, we propose a simple distance-based peer selection rule for improved connectivity and faster data propagation. Evaluation results show that our proposed light-weight and backward-compatible peer selection rule has potential to reduce data dissemination latency.
DOI: 10.14272/rydygezrgperjg-ocozrvbesa-n.1
title: C20H11F3N2O4
title: InChI=1S/C20H11F3N2O4/c21-15-8-13(9-16(22)18(15)23)24-25-17-7-12(20(28)29)5-6-14(17)10-1-3-11(4-2-10)19(26)27/h1-9H,(H,26,27)(H,28,29)/b25-24+

description: This dataset contains experimental data from a sample (InChI=1S/C20H11F3N2O4/c21-15-8-13(9-16(22)18(15)23)24-25-17-7-12(20(28)29)5-6-14(17)10-1-3-11(4-2-10)19(26)27/h1-9H,(H,26,27)(H,28,29)/b25-24+).
      The datasets from the following experiments are available:
      
      1H NMR
      
      13C NMR
      
      Others
      
      Mass
      
      IR
      
      Others
DOI: 10.14272/rydygezrgperjg-ocozrvbesa-n/13cnmr
title: 13C NMR (, InChI=1S/C20H11F3N2O4/c21-15-8-13(9-16(22)18(15)23)24-25-17-7-12(20(28)29)5-6-14(17)10-1-3-11(4-2-10)19(26)27/h1-9H,(H,26,27)(H,28,29)/b25-24+)

description: dataset for 13C NMR
      
      13C NMR (125 MHz, DMSO-d6, ppm) δ = 167.1 (1C, CO2H), 166.4 (1C, CO2H), 151.5 (d, 2C, CF), 147.9 (1C, Cq), 143.9 (1C, Cq), 141.3 (1C, Cq), 137.5 (1C, Cq), 132.4 (1C, CH), 131.7 (1C, CH), 131.0 (2C, CH), 130.4 (1C, Cq), 129.6 (1C, Cq), 129.1 (1C, Cq), 128.9 (2C, CH), 116.6 (1C, CH), 108.0–107.9 (m, 2C, CH). This spectrum contains around 10% impurities due to inseparable isomer and side-product.
DOI: 10.14272/rydygezrgperjg-ocozrvbesa-n/1hnmr
title: 1H NMR (, InChI=1S/C20H11F3N2O4/c21-15-8-13(9-16(22)18(15)23)24-25-17-7-12(20(28)29)5-6-14(17)10-1-3-11(4-2-10)19(26)27/h1-9H,(H,26,27)(H,28,29)/b25-24+)

description: dataset for 1H NMR
      
      1H NMR (500 MHz, DMSO-d6, ppm) δ = 13.23 (b-s, 2H, CO2H), 8.24 (d, 1H, J = 1.5 Hz, CH), 8.17 (dd, 1H, J = 8.0 Hz, 1.5 Hz, CH), 8.05 (m, 2H, CH), 7.81 (d, 1H, J = 8.0 Hz, CH), 7.63 (m, 2H, CH), 7.49 (m, 2H, CH). This spectrum contains around 10% impurities due to inseparable isomer and side-product.
DOI: 10.14272/rydygezrgperjg-ocozrvbesa-n/ir
title: IR (, InChI=1S/C20H11F3N2O4/c21-15-8-13(9-16(22)18(15)23)24-25-17-7-12(20(28)29)5-6-14(17)10-1-3-11(4-2-10)19(26)27/h1-9H,(H,26,27)(H,28,29)/b25-24+)

description: dataset for IR
      
      IR (ATR, ṽ) = 2956, 1731, 1717, 1605, 1432, 1280, 1207, 1187, 1103 cm–1.
DOI: 10.14272/rydygezrgperjg-ocozrvbesa-n/mass
title: Mass (, InChI=1S/C20H11F3N2O4/c21-15-8-13(9-16(22)18(15)23)24-25-17-7-12(20(28)29)5-6-14(17)10-1-3-11(4-2-10)19(26)27/h1-9H,(H,26,27)(H,28,29)/b25-24+)

description: dataset for Mass
      
      EI (m/z, 70 eV, 220 °C): 400 (100) [M]+, 398 (29) [M–2H]+, 355 (47) [M–CO2H]+, 269 (27) [M–C6H2F3]+. HRMS–EI (m/z): [M]+ Calcd. for C20H11F3N2O4, 400.0671; Found. 400.0667.
DOI: 10.14272/rydygezrgperjg-ocozrvbesa-n/others
title: Others (, InChI=1S/C20H11F3N2O4/c21-15-8-13(9-16(22)18(15)23)24-25-17-7-12(20(28)29)5-6-14(17)10-1-3-11(4-2-10)19(26)27/h1-9H,(H,26,27)(H,28,29)/b25-24+)

description: dataset for Others
      
      19F NMR (470 MHz, DMSO-d6, ppm) δ = -132.87 (dd, 2F, J = 21.2 Hz, J = 8.0 Hz, CF), -155.89 (tt, 1F, J = 21.2 Hz, J = 6.6 Hz, CF). This spectrum shows signals at -126.84 and -130.89 ppm corresponding to the cis-isomer.
DOI: 10.14272/rydygezrgperjg-ocozrvbesa-n/others.1
title: Others (, InChI=1S/C20H11F3N2O4/c21-15-8-13(9-16(22)18(15)23)24-25-17-7-12(20(28)29)5-6-14(17)10-1-3-11(4-2-10)19(26)27/h1-9H,(H,26,27)(H,28,29)/b25-24+)

description: dataset for Others
      
      UV-VIS (CH2Cl2), λmax = 195, 273, 329 nm.
DOI: 10.25606/surf.578c6039-45c88b92
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (1024-095)

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 095 of the 1024³ resolution collection.
DOI: 10.25606/surf.578c6039-52605a11
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (1024-090)

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 090 of the 1024³ resolution collection.
DOI: 10.25606/surf.578c6039-dfc3be9e
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (1024-089)

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 089 of the 1024³ resolution collection.
DOI: 10.25606/surf.578c6039-ef775988
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (1024-009)

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 009 of the 1024³ resolution collection.
DOI: 10.25606/surf.578c6039-ff4f4b66
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (1024-094)

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 094 of the 1024³ resolution collection.
DOI: 10.25606/surf.578c6039-705c6818
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (1024-097)

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 097 of the 1024³ resolution collection.