cometadata/datacite-titles-descriptions-related-identifiers huggingface dataset:
DOI: 10.7910/dvn/hjgj2a/tkcxat
title: 20190809114853150_wifi_33_185_004_g6_LGM-G600L.tab

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DOI: 10.7910/dvn/hjgj2a/xgh54j
title: 20190809142027276_wifi_33_181_020_g6_LGM-G600L.tab

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DOI: 10.7910/dvn/hjgj2a/xws2al
title: 20190809132001830_wifi_33_175_003_chanseok2_SM-G950N.tab

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DOI: 10.7910/dvn/hjgj2a/ykslur
title: 20190809134504589_wifi_33_175_007_g6_LGM-G600L.tab

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DOI: 10.7910/dvn/hjgj2a/2oinds
title: 20190809145001864_wifi_33_191_001_g6_LGM-G600L.tab

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DOI: 10.7910/dvn/hjgj2a/d08dlw
title: 20190809120753589_wifi_33_188_012_g6_LGM-G600L.tab

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DOI: 10.7910/dvn/hjgj2a/ee0vqe
title: 20190809114817256_wifi_33_185_002_g6_LGM-G600L.tab

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DOI: 10.7910/dvn/hjgj2a/h7jpwt
title: 20190809133459365_wifi_33_178_013_chanseok2_SM-G950N.tab

description: :unav
DOI: 10.7910/dvn/hjgj2a/hsiqbp
title: 20190809112053403_wifi_33_179_006_g6_LGM-G600L.tab

description: :unav
DOI: 10.7910/dvn/hjgj2a/icnmoe
title: 20190809120737294_wifi_33_188_011_g6_LGM-G600L.tab

description: :unav
DOI: 10.7910/dvn/hjgj2a/nqskuj
title: 20190809114111814_wifi_33_182_009_g6_LGM-G600L.tab

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DOI: 10.7910/dvn/hjgj2a/o75prw
title: 20190809110522367_wifi_33_177_002_g6_LGM-G600L.tab

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DOI: 10.7910/dvn/hjgj2a/tszlpz
title: 20190809134309874_wifi_33_180_009_chanseok2_SM-G950N.tab

description: :unav
DOI: 10.7910/dvn/dqgtmp/ycyiq4
title: sheepFattening_irrigatedFodder.xls

description: :unav
DOI: 10.7910/dvn/hjgj2a/3m0w4w
title: 20190809105339338_wifi_33_175_009_chanseok_SM-G950N.tab

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DOI: 10.7910/dvn/hjgj2a/5mf7nc
title: 20190809143250467_wifi_33_185_016_g6_LGM-G600L.tab

description: :unav
DOI: 10.7910/dvn/hjgj2a/ajtys1
title: 20190809113034030_wifi_33_181_015_chanseok_SM-G950N.tab

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DOI: 10.7910/dvn/hjgj2a/d3rawr
title: 20190809142506611_wifi_33_182_013_g6_LGM-G600L.tab

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DOI: 10.7910/dvn/hjgj2a/ltwmcu
title: 20190809135545336_wifi_33_182_018_chanseok2_SM-G950N.tab

description: :unav
DOI: 10.7910/dvn/hjgj2a/pigvwv
title: 20190809140052671_wifi_33_185_012_chanseok2_SM-G950N.tab

description: :unav
DOI: 10.7910/dvn/hjgj2a/t6uv8b
title: 20190809134431335_wifi_33_180_015_chanseok2_SM-G950N.tab

description: :unav
DOI: 10.7910/dvn/hjgj2a/uhwxma
title: 20190809135621924_wifi_33_177_012_g6_LGM-G600L.tab

description: :unav
DOI: 10.7910/dvn/hjgj2a/wfxpvt
title: 20190809143531557_wifi_33_186_006_g6_LGM-G600L.tab

description: :unav
DOI: 10.25606/surf.578c6039-480efcbb
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (2048-735)

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 735 of the 2048³ resolution collection.
DOI: 10.5281/zenodo.3463579
title: Model output: CICE experiments with varying floe and wave physics

description: Model output from CICE experiments with varying floe size distribution and wave physics See manuscript below for further details: Roach, L., C. Bitz, C. Horvat, and S. Dean (2019), Advances in modelling interactions between sea ice and ocean surface waves. Journal of Advances in Modeling Earth Systems (in review)
DOI: 10.5281/zenodo.3463580
title: Model output: CICE experiments with varying floe and wave physics

description: Model output from CICE experiments with varying floe size distribution and wave physics See manuscript below for further details: Roach, L., C. Bitz, C. Horvat, and S. Dean (2019), Advances in modelling interactions between sea ice and ocean surface waves. Journal of Advances in Modeling Earth Systems (in review)
DOI: 10.5281/zenodo.3463686
title: mTagBFP2-expressing vectors for electroporation of marine protists

description: Plasmid maps and genbank sequence files for the plasmids used for electroporation of model organism <em>Nannochloropsis oceanica</em> and environmental samples following the protocol Matute et al. EMS initiative from Gordon and Betty Moore foundation.
DOI: 10.7910/dvn/hjgj2a/1ns1lj
title: 20190809110519202_wifi_33_177_017_chanseok_SM-G950N.tab

description: :unav
DOI: 10.7910/dvn/hjgj2a/fgh2qt
title: 20190809114345485_wifi_33_182_017_g6_LGM-G600L.tab

description: :unav
DOI: 10.7910/dvn/hjgj2a/lid4mw
title: 20190809135204481_wifi_33_176_011_g6_LGM-G600L.tab

description: :unav
DOI: 10.7910/dvn/hjgj2a/rq71kg
title: 20190809120503099_wifi_33_190_005_chanseok_SM-G950N.tab

description: :unav
DOI: 10.7910/dvn/hjgj2a/tpswdv
title: 20190809140617864_wifi_33_179_005_g6_LGM-G600L.tab

description: :unav
DOI: 10.7910/dvn/hjgj2a/wgsjcc
title: 20190809111758815_wifi_33_179_012_chanseok_SM-G950N.tab

description: :unav
DOI: 10.7910/dvn/hjgj2a/xsswp8
title: 20190809105214965_wifi_33_175_005_chanseok_SM-G950N.tab

description: :unav
DOI: 10.7910/dvn/hjgj2a/za1r8q
title: 20190809142930468_wifi_33_185_003_g6_LGM-G600L.tab

description: :unav
DOI: 10.7910/dvn/hjgj2a/zwjslg
title: 20190809115757390_wifi_33_186_011_g6_LGM-G600L.tab

description: :unav
DOI: 10.7910/dvn/hjgj2a/1gbd2n
title: 20190809141901122_wifi_33_181_015_g6_LGM-G600L.tab

description: :unav
DOI: 10.7910/dvn/hjgj2a/3hrvwi
title: 20190809105251272_wifi_33_175_002_g6_LGM-G600L.tab

description: :unav
DOI: 10.7910/dvn/hjgj2a/7ubbna
title: 20190809112540931_wifi_33_180_020_chanseok_SM-G950N.tab

description: :unav
DOI: 10.7910/dvn/hjgj2a/aonhrk
title: 20190809112602439_wifi_33_180_007_g6_LGM-G600L.tab

description: :unav
DOI: 10.7910/dvn/hjgj2a/b1by8a
title: 20190809141203576_wifi_33_188_008_chanseok2_SM-G950N.tab

description: :unav
DOI: 10.7910/dvn/hjgj2a/fy6ucl
title: 20190809132656973_wifi_33_176_013_chanseok2_SM-G950N.tab

description: :unav
DOI: 10.7910/dvn/hjgj2a/h9khnw
title: 20190809141214638_wifi_33_180_011_g6_LGM-G600L.tab

description: :unav
DOI: 10.7910/dvn/hjgj2a/mdrzkj
title: 20190809111258219_wifi_33_183_002_chanseok_SM-G950N.tab

description: :unav
DOI: 10.7910/dvn/hjgj2a/rnsthr
title: 20190809135915699_wifi_33_185_005_chanseok2_SM-G950N.tab

description: :unav
DOI: 10.25919/5d8e5fa6d4b85
title: Parkes observations for project P985 semester 2019APRS_08

description: We propose to use the ultra-wide-bandwidth, low frequency receiver installed at the Parkes telescope in order to quantify the broad-band intermittency time scale, polarization, quasi-periodicities, and mode changing of a newly discovered pulsar, PSR J1926-0653. The pulsar is unique in its emission properties. It has multiple pulse components, that change with time (both mode- changing and sub-pulse drifting phenomena are evident). The pulsar exhibits nulls in which a few individual pulses seem to be missing. It also exhibits longer-scale (hour-scale) intermittency behaviour in which the emission switches off for long periods of time. The pulse flux densities often, but not always, seem to exhibit quasi-periodic variations. Clearly this pulsar may hold the key to many different emission phenomena and we request time on Parkes, FAST and ATCA to parameterise the pulsar and its emission properties in detail.
DOI: 10.7910/dvn/hjgj2a/fug5qw
title: 20190809140105349_wifi_33_185_013_chanseok2_SM-G950N.tab

description: :unav
DOI: 10.7910/dvn/hjgj2a/ip6zn6
title: 20190809141342440_wifi_33_180_017_g6_LGM-G600L.tab

description: :unav
DOI: 10.7910/dvn/hjgj2a/knjmsr
title: 20190809140632244_wifi_33_179_006_g6_LGM-G600L.tab

description: :unav
DOI: 10.7910/dvn/hjgj2a/lxh9l4
title: 20190809132530799_wifi_33_176_007_chanseok2_SM-G950N.tab

description: :unav
DOI: 10.7910/dvn/hjgj2a/mkougm
title: 20190809115516017_wifi_33_186_003_g6_LGM-G600L.tab

description: :unav
DOI: 10.7910/dvn/hjgj2a/mxonll
title: 20190809120446018_wifi_33_188_002_g6_LGM-G600L.tab

description: :unav
DOI: 10.7910/dvn/hjgj2a/onsw8n
title: 20190809133740820_wifi_33_179_001_chanseok2_SM-G950N.tab

description: :unav
DOI: 10.7910/dvn/hjgj2a/pslwq3
title: 20190809140925982_wifi_33_187_013_chanseok2_SM-G950N.tab

description: :unav
DOI: 10.25606/surf.578c6039-cc794818
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (2048-201)

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 201 of the 2048³ resolution collection.
DOI: 10.5281/zenodo.3463693
title: mTagBFP2-expressing vectors for electroporation of marine protists

description: Plasmid maps and genbank sequence files for the plasmids used for electroporation of model organism <em>Nannochloropsis oceanica</em> and environmental samples following the protocol Matute et al. EMS initiative from Gordon and Betty Moore foundation.
DOI: 10.5281/zenodo.3463694
title: mTagBFP2-expressing vectors for electroporation of marine protists

description: Plasmid maps and genbank sequence files for the plasmids used for electroporation of model organism <em>Nannochloropsis oceanica</em> and environmental samples following the protocol Matute et al. EMS initiative from Gordon and Betty Moore foundation.
DOI: 10.7910/dvn/hjgj2a/16ofof
title: 20190809143910248_wifi_33_187_006_g6_LGM-G600L.tab

description: :unav
DOI: 10.7910/dvn/hjgj2a/17piba
title: 20190809133634648_wifi_33_183_003_chanseok2_SM-G950N.tab

description: :unav
DOI: 10.7910/dvn/hjgj2a/9t1fgs
title: 20190809141134496_wifi_33_180_009_g6_LGM-G600L.tab

description: :unav
DOI: 10.7910/dvn/hjgj2a/9uqlxo
title: 20190809115747094_wifi_33_188_007_chanseok_SM-G950N.tab

description: :unav
DOI: 10.7910/dvn/hjgj2a/flljx2
title: 20190809111510231_wifi_33_178_013_g6_LGM-G600L.tab

description: :unav
DOI: 10.7910/dvn/hjgj2a/omo4yi
title: 20190809133303942_wifi_33_178_005_chanseok2_SM-G950N.tab

description: :unav
DOI: 10.7910/dvn/hjgj2a/osdfza
title: 20190809134343277_wifi_33_175_002_g6_LGM-G600L.tab

description: :unav
DOI: 10.7910/dvn/hjgj2a/uacsqg
title: 20190809114720022_wifi_33_184_004_g6_LGM-G600L.tab

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DOI: 10.7910/dvn/hjgj2a/ulrn1g
title: 20190809133401948_wifi_33_178_009_chanseok2_SM-G950N.tab

description: :unav
DOI: 10.7910/dvn/hjgj2a/zu0uxy
title: 20190809114816539_wifi_33_186_005_chanseok_SM-G950N.tab

description: :unav
DOI: 10.25606/surf.578c6039-28ac7709
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (2048-192)

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 192 of the 2048³ resolution collection.
DOI: 10.25919/5d8eb5f472fbb
title: Parkes observations for project P958 semester 2019APRS_91

description: Fast radio bursts (FRBs) continue to raise more questions than they answer. Until a few months ago, only one burst – the only one known to repeat - had been localized to a bright radio nebula (either a young supernova remnant or pulsar wind nebulae) in a distant dwarf galaxy. Over the last year searches with the Australian Square Kilometre Array Pathfinder (ASKAP) have detected 28 bursts, two of which have been localised to host galaxies at redshifts &gt; 0.3. These bursts and their hosts are very unlike the repeater, suggesting there may be a dichotomy in the population. Over the next six months we expect to detect another 12 FRBs, which will also have sub-arcsecond localisations. Here we propose to search this population for repeats. Our comprehensive sample and a dense monitoring campaign of well localised bursts, at a fluence limit more than 60 times lower than that of their detections, will either confirm the presence of additional repeating FRBs or the uniqueness of FRB 121102 amongst the population.
DOI: 10.7910/dvn/hjgj2a/1g0kh0
title: 20190809134821901_wifi_33_181_008_chanseok2_SM-G950N.tab

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DOI: 10.7910/dvn/hjgj2a/8w73hz
title: 20190809111520238_wifi_33_179_002_chanseok_SM-G950N.tab

description: :unav
DOI: 10.7910/dvn/hjgj2a/db9pvn
title: 20190809135957455_wifi_33_185_008_chanseok2_SM-G950N.tab

description: :unav
DOI: 10.7910/dvn/hjgj2a/hnueig
title: 20190809112309002_wifi_33_180_010_chanseok_SM-G950N.tab

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DOI: 10.7910/dvn/hjgj2a/ledguw
title: 20190809110449184_wifi_33_177_015_chanseok_SM-G950N.tab

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DOI: 10.7910/dvn/hjgj2a/lus3h4
title: 20190809113152982_wifi_33_181_003_g6_LGM-G600L.tab

description: :unav
DOI: 10.7910/dvn/hjgj2a/mz4ngv
title: 20190809113849836_wifi_33_182_001_g6_LGM-G600L.tab

description: :unav
DOI: 10.7910/dvn/hjgj2a/tnpeku
title: 20190809112838632_wifi_33_180_016_g6_LGM-G600L.tab

description: :unav
DOI: 10.7910/dvn/hjgj2a/2wgray
title: 20190809111117490_wifi_33_178_001_g6_LGM-G600L.tab

description: :unav
DOI: 10.7910/dvn/hjgj2a/3l4dyh
title: 20190809140112255_wifi_33_178_009_g6_LGM-G600L.tab

description: :unav
DOI: 10.7910/dvn/hjgj2a/8boykx
title: 20190809134008248_wifi_33_179_012_chanseok2_SM-G950N.tab

description: :unav
DOI: 10.7910/dvn/hjgj2a/geuypp
title: 20190809120603510_wifi_33_188_006_g6_LGM-G600L.tab

description: :unav
DOI: 10.7910/dvn/hjgj2a/hxutsh
title: 20190809144828091_wifi_33_190_002_g6_LGM-G600L.tab

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DOI: 10.7910/dvn/hjgj2a/ppqxol
title: 20190809105639563_wifi_33_175_019_chanseok_SM-G950N.tab

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DOI: 10.7910/dvn/hjgj2a/t8mwhq
title: 20190809143925003_wifi_33_187_007_g6_LGM-G600L.tab

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DOI: 10.7910/dvn/hjgj2a/u5wyhv
title: 20190809112524300_wifi_33_180_005_g6_LGM-G600L.tab

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DOI: 10.7910/dvn/hjgj2a/wngoyv
title: 20190809113638939_wifi_33_182_015_chanseok_SM-G950N.tab

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DOI: 10.7910/dvn/hjgj2a/z9mwky
title: 20190809141817371_wifi_33_181_012_g6_LGM-G600L.tab

description: :unav
DOI: 10.25606/surf.578c6039-548af13b
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (2048-062)

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 062 of the 2048³ resolution collection.
DOI: 10.25606/surf.578c6039-edce4c11
title: The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos (2048-671)

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 671 of the 2048³ resolution collection.
DOI: 10.7910/dvn/hjgj2a/0rcpeb
title: 20190809113443708_wifi_33_182_007_chanseok_SM-G950N.tab

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DOI: 10.7910/dvn/hjgj2a/apr3y3
title: 20190809134538057_wifi_33_175_009_g6_LGM-G600L.tab

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DOI: 10.7910/dvn/hjgj2a/jbmgnh
title: 20190809113135111_wifi_33_181_002_g6_LGM-G600L.tab

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DOI: 10.7910/dvn/hjgj2a/lbghtb
title: 20190809133106084_wifi_33_177_018_chanseok2_SM-G950N.tab

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DOI: 10.7910/dvn/hjgj2a/nwe2ay
title: 20190809113002061_wifi_33_181_013_chanseok_SM-G950N.tab

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DOI: 10.7910/dvn/hjgj2a/qutlym
title: 20190809134230389_wifi_33_180_006_chanseok2_SM-G950N.tab

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DOI: 10.7910/dvn/hjgj2a/uthgtc
title: 20190809132311376_wifi_33_175_017_chanseok2_SM-G950N.tab

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DOI: 10.7910/dvn/hjgj2a/x18ty1
title: 20190809135738512_wifi_33_184_003_chanseok2_SM-G950N.tab

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DOI: 10.7910/dvn/hjgj2a/2d7ajn
title: 20190809110633581_wifi_33_177_022_chanseok_SM-G950N.tab

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DOI: 10.7910/dvn/hjgj2a/9awbhr
title: 20190809135518347_wifi_33_182_016_chanseok2_SM-G950N.tab

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DOI: 10.7910/dvn/hjgj2a/lgqpwu
title: 20190809115636402_wifi_33_186_007_g6_LGM-G600L.tab

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DOI: 10.7910/dvn/hjgj2a/ovllxx
title: 20190809132517273_wifi_33_176_006_chanseok2_SM-G950N.tab

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DOI: 10.7910/dvn/hjgj2a/q5fihi
title: 20190809112713925_wifi_33_180_011_g6_LGM-G600L.tab

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DOI: 10.7910/dvn/hjgj2a/s1qkpq
title: 20190809141253159_wifi_33_188_012_chanseok2_SM-G950N.tab

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DOI: 10.7910/dvn/hjgj2a/tzdjd1
title: 20190809115336654_wifi_33_187_009_chanseok_SM-G950N.tab

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DOI: 10.7910/dvn/hjgj2a/vkfncf
title: 20190809144632835_wifi_33_189_004_g6_LGM-G600L.tab

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DOI: 10.7910/dvn/hjgj2a/0fc4pr
title: 20190809114505678_wifi_33_185_015_chanseok_SM-G950N.tab

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DOI: 10.7910/dvn/hjgj2a/bmnje2
title: 20190809140142171_wifi_33_178_011_g6_LGM-G600L.tab

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DOI: 10.7910/dvn/hjgj2a/cdzzbp
title: 20190809115010794_wifi_33_186_011_chanseok_SM-G950N.tab

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DOI: 10.7910/dvn/hjgj2a/ncpap7
title: 20190809113729365_wifi_33_182_018_chanseok_SM-G950N.tab

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DOI: 10.7910/dvn/hjgj2a/njuhka
title: 20190809113651322_wifi_33_181_019_g6_LGM-G600L.tab

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DOI: 10.7910/dvn/hjgj2a/tuaddx
title: 20190809115716124_wifi_33_188_005_chanseok_SM-G950N.tab

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DOI: 10.7910/dvn/hjgj2a/v5xndw
title: 20190809114025508_wifi_33_184_004_chanseok_SM-G950N.tab

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DOI: 10.7910/dvn/hjgj2a/y7rupq
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DOI: 10.7910/dvn/m7dsbq
title: ASPIRES South Africa RCT Final Analysis Dataset

description: FHI 360 conducted a full factorial randomized controlled trial (RCT) to determine the effects of the financial capabilities and HIV prevention education interventions on the prevalence of sexually transmitted infections (STIs) among adolescents. The objectives of the RCT were to assess whether integrating an economic strengthening intervention with an HIV prevention education intervention improved economic and health outcomes more than either intervention alone, and to estimate the resources required at the program level to support the ES and HIV prevention education interventions.Data were collected through Audio Computer-Assisted Self-Interviews (ACASI) with participants and STI and pregnancy testing of urine samples at three time points: baseline, endline 1 (immediately after the end of the intervention), and endline 2 (9 months after endline 1). This dataset contains the baseline and endline survey and STI data.
DOI: 10.7910/dvn/m7dsbq/bj1skj
title: Analysis_deid.tab

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DOI: 10.7910/dvn/m7dsbq/n4ob64
title: Analysis_Specs_12_27_2018.tab

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DOI: 10.7910/dvn/3xtvih/ep5kq9
title: Endline1_Specs_08_16_2018.xlsx

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DOI: 10.7910/dvn/3xtvih/gbcwen
title: Endline1_analysis_deid.tab

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DOI: 10.7910/dvn/3xtvih/nrlv05
title: Endline2_Specs_08_16_2018.xlsx

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