cometadata/datacite-titles-descriptions-related-identifiers huggingface dataset:
DOI: 10.14457/cu.the.1993.374
title: ความรู้ ทัศนคติ และการปฏิบัติตนเกี่ยวกับโรคเอดส์ ของผู้บริหารสถานศึกษาและครูอนามัยโรงเรียนประถมศึกษา สังกัดสำนักงานคณะกรรมการการประถมศึกษาแห่งชาติ เขตการศึกษา 8 /
DOI: 10.15121/1234401
title: Fluid rare earth element anlayses from wells RN-12 and RN-19, Reykjanes, Iceland

description: Results for fluid rare earth elment analyses from Reykjanes wells RN-12 and RN-19. The data have not been corrected for flashing. Samples preconcetrated using chelating resin with IDA functional group (InertSep ME-1). Analyzed using and Element magnetic sctor ICP-MS.
DOI: 10.6073/pasta/de9a12d52ee7d61ff99c00e326b8a6fa
title: Fuel Loading in Simulated Hurricane Experiment at Harvard Forest since 1993
DOI: 10.15121/1234402
title: Silica Precipitation and Lithium Sorption

description: This file contains silica precipitation and lithium sorption data from the project. The silica removal data is corrected from the previous submission. The previous submission did not take into account the limit of detection of the ICP-MS procedure.
DOI: 10.15121/1234403
title: Compilation of Rare Earth Element Analyses from US Geothermal Fields and Mid Ocean Ridge Hydrothermal Vents

description: Compilation of rare earth element and associated major and minor dissolved constituent analytical data for USA geothermal fields and global seafloor hydrothermal vents. Data is in original units. Reference to and use of this data should be attributed to the original authors and publications according to the provisions outlined therein.
DOI: 10.15121/1234404
title: Raft River Geothermal Field Well Head Brine Sample

description: Raw data and data workup of assay for real-world brine sample. Brine sample was taken at the well head.
DOI: 10.15121/1234405
title: Column Sorption Uptake and Regeneration Study; Rare Earth Element Sorbent Uptake and Sorbent Stripping

description: Study of rare earth element (REE) uptake from geothermal brine simulant by column loading, metal recovery through stripping, and regeneration of column for re-loading. Simulated brine testing.
DOI: 10.5255/ukda-sn-7860-1
title: Community Mental Health Service User Survey, 2015
DOI: 10.14457/kmutt.the.2004.198
title: การศึกษาแนวทางการจัดการกากสีในอู่เคาะพ่นสีรถยนต์ /
DOI: 10.14457/kmutt.the.2006.162
title: การศึกษาแนวทางการจัดหาวัตถุดิบ และน้ำมันเชื้อเพลิงที่เป็นมิตรกับสิ่งแวดล้อม เพื่อใช้ในภาคอุตสาหกรรม /
DOI: 10.14457/kmutt.the.2008.224
title: การศึกษาแนวทางการจัดการระบบผลิตไฟฟ้าแบบผสมผสานพลังงานแสงอาทิตย์ กับพลังน้ำขนาดเล็กแบบยั่งยืน สำหรับการบริการสาธารณะในชุมชนชนบท : กรณีศึกษาหมู่บ้านปิตุคี อำเภออมก๋อย จังหวัดเชียงใหม่ /
DOI: 10.14457/kmutt.the.2009.246
title: การศึกษาแนวทางการจัดการทรัพยากรปูแสมโดยชุมชนมีส่วนร่วม : กรณีศึกษาพื้นที่บริเวณปากแม่น้ำบางตะบูน /
DOI: 10.14457/kmutt.the.2009.247
title: การศึกษาแนวทางการจัดการด้านคุณภาพงานก่อสร้างของบริษัทที่ปรึกษาควบคุมงาน /
DOI: 10.6073/pasta/1a619680f1b57c1b4d21867fe9fb1487
title: Core Site Phenology Study from the Chihuahaun Desert Grassland and Shrubland at the Sevilleta National Wildlife Refuge, New Mexico (2000-present )
DOI: 10.6073/pasta/bc5413d8595e692b813c0041ca6cebd6
title: Ant Functional Diversity in Temperate Zone Forests: A Comparison with Neotropical Ants
DOI: 10.7931/j29884x3
title: Indices of possum abundance and browse at forest sites in New Zealand
DOI: 10.14457/ubu.res.2006.3
title: การศึกษาศักยภาพการจัดการท่องเที่ยวเชิงนิเวศ อย่างมีส่วนร่วมของชุมชนในเขตพื้นที่รอยต่อเทศบาลนครอุบลราชธานี กับเทศบาลเมืองวารินชำราบ จังหวัดอุบลราชธานี : กรณีศึกษา ชุมชนดอนงิ้ว และชุมชนกุดเป่ง [หมู่ 16] /
DOI: 10.14457/ubu.res.2006.5
title: การศึกษาการทำความเย็นและความร้อน โดยใช้แผงเก็บสะสมพลังงาน /
DOI: 10.14457/ubu.res.2006.10
title: การเตรียมวัสดุเทอร์โมอิเล็กตริกจากเถ้าแกลบ /
DOI: 10.14457/ubu.res.2006.7
title: การผลิตและวิเคราะห์ก๊าซผลิตภัณฑ์จากฟางข้าว โดยใช้เตาผลิตก๊าซชนิดไหลลง /
DOI: 10.14457/ubu.res.2006.8
title: ฤทธิ์ของน้ำมันหอมระเหยจากขมิ้น ในการยับยั้งกระบวนการออกซิเดชันของ Plasma lipids และ LDL (Low Density Lipoprotein) /
DOI: 10.14457/ubu.res.2006.9
title: การจำลองการเคลื่อนที่ของวัตถุในแนวดิ่ง ภายใต้แรงโน้มถ่วง /
DOI: 10.25606/surf.578c6039-2f867325
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (2048-583)

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 583 of the 2048³ resolution collection.
DOI: 10.25606/surf.578c6039-968ecbcb
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (2048-576)

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 576 of the 2048³ resolution collection.
DOI: 10.25606/surf.578c6039-e969d56b
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (2048-580)

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 580 of the 2048³ resolution collection.
DOI: 10.25606/surf.578c6039-34e4740a
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (2048-574)

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 574 of the 2048³ resolution collection.
DOI: 10.25606/surf.578c6039-4b015693
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (2048-578)

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 578 of the 2048³ resolution collection.
DOI: 10.25606/surf.578c6039-5690d363
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (2048-579)

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 579 of the 2048³ resolution collection.
DOI: 10.25606/surf.578c6039-98c3a3fb
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (2048-582)

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 582 of the 2048³ resolution collection.
DOI: 10.25606/surf.578c6039-b28d86a0
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (2048-581)

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 581 of the 2048³ resolution collection.
DOI: 10.17632/gbx8p43nrr.1
title: Data for: Metabolomic Stability of Exercise-Induced Sweat

description: Sweat was collected from the forearms of male participants. Sweat was aliquoted and frozen after 0, 30, 60, and 90 minutes at either room temperature or body temperature. Samples were lyophilized to dryness, reconstituted, and run by HILIC-MS. Data was acquired on a Q Exactive HF using polarity switching at 15,000 resolution.
DOI: 10.5519/qd.snjlf9wc
title: Query on the Natural History Museum Data Portal (data.nhm.ac.uk) (5 records)
DOI: 10.14272/lvgohacwpddeka-ztrvsjdysa-n/chmo0000470
title: mass spectrometry (MS) ()
title: InChI=1S/C50H32F6N4O4/c1-3-63-49(61)27-9-5-25(6-10-27)43-35-13-17-39(57-35)45(29-21-31(51)47(55)32(52)22-29)41-19-15-37(59-41)44(26-7-11-28(12-8-26)50(62)64-4-2)38-16-20-42(60-38)46(40-18-14-36(43)58-40)30-23-33(53)48(56)34(54)24-30/h5-24,57,60H,3-4H2,1-2H3/b43-35-,43-36-,44-37-,44-38-,45-39-,45-41-,46-40-,46-42-

description: dataset for mass spectrometry (MS) MS (FAB, 3-NBA): m/z (%) = 866.2 (78) [M]+, 867.2 (100) [M + H]+, 868.2 (50) [M + H]+.
DOI: 10.14272/lvgohacwpddeka-ztrvsjdysa-n/chmo0000593
title: 1H nuclear magnetic resonance spectroscopy (1H NMR) ()
title: InChI=1S/C50H32F6N4O4/c1-3-63-49(61)27-9-5-25(6-10-27)43-35-13-17-39(57-35)45(29-21-31(51)47(55)32(52)22-29)41-19-15-37(59-41)44(26-7-11-28(12-8-26)50(62)64-4-2)38-16-20-42(60-38)46(40-18-14-36(43)58-40)30-23-33(53)48(56)34(54)24-30/h5-24,57,60H,3-4H2,1-2H3/b43-35-,43-36-,44-37-,44-38-,45-39-,45-41-,46-40-,46-42-

description: dataset for 1H nuclear magnetic resonance spectroscopy (1H NMR) 1H NMR (400 MHz, CDCl3, ppm) δ = –2.91 (bs, 2H, NH), 1.57 (t, J = 7.1 Hz, 6H, CH3), 4.60 (q, J = 7.1 Hz, 4H, CH2), 7.80–7.91 (m, 4H, CHCF), 8.30 (d, J = 8.2 Hz, 4H, HPh), 8.48 (d, J = 8.3 Hz, 4H, HPh), 8.79–8.93 (m, 8H, HPyr).
DOI: 10.5519/qd.u1ay3i52
title: Query on the Natural History Museum Data Portal (data.nhm.ac.uk) (1 records)
DOI: 10.14272/lvgohacwpddeka-ztrvsjdysa-n.1
title: C50H32F6N4O4
title: InChI=1S/C50H32F6N4O4/c1-3-63-49(61)27-9-5-25(6-10-27)43-35-13-17-39(57-35)45(29-21-31(51)47(55)32(52)22-29)41-19-15-37(59-41)44(26-7-11-28(12-8-26)50(62)64-4-2)38-16-20-42(60-38)46(40-18-14-36(43)58-40)30-23-33(53)48(56)34(54)24-30/h5-24,57,60H,3-4H2,1-2H3/b43-35-,43-36-,44-37-,44-38-,45-39-,45-41-,46-40-,46-42-

description: This dataset contains experimental data from a sample (InChI=1S/C50H32F6N4O4/c1-3-63-49(61)27-9-5-25(6-10-27)43-35-13-17-39(57-35)45(29-21-31(51)47(55)32(52)22-29)41-19-15-37(59-41)44(26-7-11-28(12-8-26)50(62)64-4-2)38-16-20-42(60-38)46(40-18-14-36(43)58-40)30-23-33(53)48(56)34(54)24-30/h5-24,57,60H,3-4H2,1-2H3/b43-35-,43-36-,44-37-,44-38-,45-39-,45-41-,46-40-,46-42-). The datasets from the following experiments are available: 1H nuclear magnetic resonance spectroscopy (1H NMR) 13C nuclear magnetic resonance spectroscopy (13C NMR) infrared absorption spectroscopy (IR) mass spectrometry (MS) mass spectrometry (MS)
DOI: 10.14272/lvgohacwpddeka-ztrvsjdysa-n/chmo0000470.1
title: mass spectrometry (MS) ()
title: InChI=1S/C50H32F6N4O4/c1-3-63-49(61)27-9-5-25(6-10-27)43-35-13-17-39(57-35)45(29-21-31(51)47(55)32(52)22-29)41-19-15-37(59-41)44(26-7-11-28(12-8-26)50(62)64-4-2)38-16-20-42(60-38)46(40-18-14-36(43)58-40)30-23-33(53)48(56)34(54)24-30/h5-24,57,60H,3-4H2,1-2H3/b43-35-,43-36-,44-37-,44-38-,45-39-,45-41-,46-40-,46-42-

description: dataset for mass spectrometry (MS) HRMS (C50H33O4N4F6): calcd 867.2401, found 867.2403.
DOI: 10.14272/lvgohacwpddeka-ztrvsjdysa-n/chmo0000595
title: 13C nuclear magnetic resonance spectroscopy (13C NMR) ()
title: InChI=1S/C50H32F6N4O4/c1-3-63-49(61)27-9-5-25(6-10-27)43-35-13-17-39(57-35)45(29-21-31(51)47(55)32(52)22-29)41-19-15-37(59-41)44(26-7-11-28(12-8-26)50(62)64-4-2)38-16-20-42(60-38)46(40-18-14-36(43)58-40)30-23-33(53)48(56)34(54)24-30/h5-24,57,60H,3-4H2,1-2H3/b43-35-,43-36-,44-37-,44-38-,45-39-,45-41-,46-40-,46-42-

description: dataset for 13C nuclear magnetic resonance spectroscopy (13C NMR) 13C NMR (100 MHz, CDCl3): d (ppm) = 14.7 (+, 2C, CH3), 61.6 (–, 2C, CH2), 117.1 (Cq), 118.8 (m, CHCF), 120.0 (Cq), 128.2 (+), 130.5 (Cq), 134.6 (+), 137.8 (m, CCHCF), 140.3 (dt, J = 254.0, 15.3 Hz, CFpara), 146.3 (Cq), 149.8 (ddd, J = 252.8, 9.8, 4.1 Hz, CFmeta), 166.8 (Cq, COO), (residual 35 Cs distributed on listed signals).
DOI: 10.14272/lvgohacwpddeka-ztrvsjdysa-n/chmo0000630
title: infrared absorption spectroscopy (IR) ()
title: InChI=1S/C50H32F6N4O4/c1-3-63-49(61)27-9-5-25(6-10-27)43-35-13-17-39(57-35)45(29-21-31(51)47(55)32(52)22-29)41-19-15-37(59-41)44(26-7-11-28(12-8-26)50(62)64-4-2)38-16-20-42(60-38)46(40-18-14-36(43)58-40)30-23-33(53)48(56)34(54)24-30/h5-24,57,60H,3-4H2,1-2H3/b43-35-,43-36-,44-37-,44-38-,45-39-,45-41-,46-40-,46-42-

description: dataset for infrared absorption spectroscopy (IR) IR (ATR, ṽ) = 3302 (vw), 3070 (vw), 1707 (m), 1607 (w), 1525 (w), 1475 (w), 1423 (w), 1401 (w), 1365 (w), 1307 (vw), 1271 (m), 1237 (w), 1176 (w), 1108 (w), 1040 (m), 1022 (w), 973 (w), 928 (w), 869 (w), 849 (vw), 805 (m), 762 (w), 732 (w), 717 (w), 636 (vw), 561 (vw), 541 (w), 408 (vw) cm–1.
DOI: 10.14272/nrdqbpjlnqdpcn-bopyevhasa-n.1
title: C50H30Br8N4O4
title: InChI=1S/C50H30Br8N4O4/c1-3-65-49(63)27-19-15-25(16-20-27)31-45-37(55)33(51)41(59-45)29(23-11-7-5-8-12-23)43-35(53)39(57)47(61-43)32(26-17-21-28(22-18-26)50(64)66-4-2)48-40(58)36(54)44(62-48)30(24-13-9-6-10-14-24)42-34(52)38(56)46(31)60-42/h5-22,59,62H,3-4H2,1-2H3/b41-29-,42-30-,43-29-,44-30-,45-31-,46-31-,47-32-,48-32-

description: This dataset contains experimental data from a sample (InChI=1S/C50H30Br8N4O4/c1-3-65-49(63)27-19-15-25(16-20-27)31-45-37(55)33(51)41(59-45)29(23-11-7-5-8-12-23)43-35(53)39(57)47(61-43)32(26-17-21-28(22-18-26)50(64)66-4-2)48-40(58)36(54)44(62-48)30(24-13-9-6-10-14-24)42-34(52)38(56)46(31)60-42/h5-22,59,62H,3-4H2,1-2H3/b41-29-,42-30-,43-29-,44-30-,45-31-,46-31-,47-32-,48-32-). The datasets from the following experiments are available: 1H nuclear magnetic resonance spectroscopy (1H NMR) 13C nuclear magnetic resonance spectroscopy (13C NMR) infrared absorption spectroscopy (IR) mass spectrometry (MS)
DOI: 10.14272/nrdqbpjlnqdpcn-bopyevhasa-n/chmo0000470
title: mass spectrometry (MS) ()
title: InChI=1S/C50H30Br8N4O4/c1-3-65-49(63)27-19-15-25(16-20-27)31-45-37(55)33(51)41(59-45)29(23-11-7-5-8-12-23)43-35(53)39(57)47(61-43)32(26-17-21-28(22-18-26)50(64)66-4-2)48-40(58)36(54)44(62-48)30(24-13-9-6-10-14-24)42-34(52)38(56)46(31)60-42/h5-22,59,62H,3-4H2,1-2H3/b41-29-,42-30-,43-29-,44-30-,45-31-,46-31-,47-32-,48-32-

description: dataset for mass spectrometry (MS) MS (FAB, 3-NBA): m/z (%) = 1390.3 (100) [M(79Br481Br4) + H]+ (Fitting isotope pattern for eight bromines).
DOI: 10.14272/nrdqbpjlnqdpcn-bopyevhasa-n/chmo0000593
title: 1H nuclear magnetic resonance spectroscopy (1H NMR) ()
title: InChI=1S/C50H30Br8N4O4/c1-3-65-49(63)27-19-15-25(16-20-27)31-45-37(55)33(51)41(59-45)29(23-11-7-5-8-12-23)43-35(53)39(57)47(61-43)32(26-17-21-28(22-18-26)50(64)66-4-2)48-40(58)36(54)44(62-48)30(24-13-9-6-10-14-24)42-34(52)38(56)46(31)60-42/h5-22,59,62H,3-4H2,1-2H3/b41-29-,42-30-,43-29-,44-30-,45-31-,46-31-,47-32-,48-32-

description: dataset for 1H nuclear magnetic resonance spectroscopy (1H NMR) 1H NMR (400 MHz, CDCl3, ppm) δ = –1.56 (bs, 2H, NH), 1.55 (t, J = 7.1 Hz, 6H, CH3), 4.55 (q, J = 7.1 Hz, 4H, CH2), 7.72–7.90 (m, 6H, HPh), 8.17–8.25 (m, 4H, HPh), 8.31 (d, J = 8.3 Hz, 4H, HPh), 8.45 (d, J = 8.3 Hz, 4H, HPh).
DOI: 10.14272/nrdqbpjlnqdpcn-bopyevhasa-n/chmo0000595
title: 13C nuclear magnetic resonance spectroscopy (13C NMR) ()
title: InChI=1S/C50H30Br8N4O4/c1-3-65-49(63)27-19-15-25(16-20-27)31-45-37(55)33(51)41(59-45)29(23-11-7-5-8-12-23)43-35(53)39(57)47(61-43)32(26-17-21-28(22-18-26)50(64)66-4-2)48-40(58)36(54)44(62-48)30(24-13-9-6-10-14-24)42-34(52)38(56)46(31)60-42/h5-22,59,62H,3-4H2,1-2H3/b41-29-,42-30-,43-29-,44-30-,45-31-,46-31-,47-32-,48-32-

description: dataset for 13C nuclear magnetic resonance spectroscopy (13C NMR) 13C NMR (100 MHz, CDCl3, ppm) δ = 14.6 (+, CH3), 61.6 (–, CH2), 119.6 (Cq), 121.4 (Cq), 128.6 (+), 129.5 (+), 130.1 (+), 131.5 (Cq), 136.9 (+), 137.1 (Cq), 141.2 (Cq), 166.9 (Cq, COO), (residual 38 Cs distributed on listed signals).