cometadata/datacite-titles-descriptions-related-identifiers huggingface dataset:
DOI: 10.25909/5c416aaf948cf
title: Diagnostic test accuracy when screening for haliotid herpesvirus 1 (AbHV) in apparently healthy populations of Australian abalone Haliotis spp.

description: This code is the final latent class analysis used to estimate the diagnostic accuracy of 3 qPCR assays and histopathology for <i>Haliotid herpesvirus 1</i> (AbHV).
DOI: 10.25909/5c626a5e15979
title: Gruiformes PartitionFinder input and results

description: Input and results files from PartitionFinder analyses.
DOI: 10.25909/5c626a4965e4f
title: Gruiformes BEAST input

description: Input file from BEAST analyses.<br>
DOI: 10.25909/5c626947a23c2
title: Gruiformes MrBayes input

description: Input files from MrBayes analyses.<br>
DOI: 10.25909/5c6269d38a481
title: Gruiformes RAxML input

description: Input files for RAxML analysis.<br>
DOI: 10.25909/5c6269275bbaa
title: Gruiformes collapsed (merged) R1 and R2 sequencing reads

description: Collapsed (merged) Illumina R1 and R2 reads for <i>Aptornis defossor</i> (NMNZ S23033), <i>Aptornis otidiformis</i> (DM8046), <i>Aramus gaurauna</i> (USNM 614588), <i>Canirallus oculeus</i> (USNM 304071), <i>Psophia crepitans</i> (no voucher), and <i>Sarothrura rufa</i> (USNM 527273). Single-end reads for <i>Aptornis otidiformis</i> (CM AV.18536). Residual adapter sequences have been removed (using AdapterRemoval or Geneious).
DOI: 10.25909/5c654041d3849
title: Australian teachers' intent to leave teaching profession through logistic regression analysis

description: Staff in Australia's Schools (SiAS) 2010 is the second national survey of approximately 17,000 teachers and school leaders funded by the Australian Government, conducted by the Australian Council for Educational Research (ACER); the first being conducted in 2006-07. It collected data on a wide range of teacher characteristics and workforce issues including: demographic items, professional learning, qualification, future career intention, and career path. One of the major purposes of this national survey was to provide relevant data to inform teachers staffing issues and teacher workforce planning. (McKenzie, Rowley, et al., 2011). The data is self-reported and data quality generally regarded as good. The first aim of this project was to use logistic regression to estimate Australian teachers' Intent to permanently leave teaching profession prior to retirement. Another aim was to identify the factors (or independent variables) that could most accurately predict teachers' intention to leave.
DOI: 10.25909/5c762b57507ef
title: Supporting data for "Benefits of explicit treatment of zero flows in probabilistic hydrological modelling of ephemeral catchments" by McInerney et al. (2019)

description: This dataset contains results from the paper "Benefits of explicit treatment of zero flows in probabilistic hydrological modelling of ephemeral catchments" by McInerney et al, which is under review at Water Resources Research. <br>The folder "metrics" contains performance metrics for the catchments and residual error schemes considered in the case studies, including 1. The Continuous Ranked Probability Skill Score ('CRPSS.csv')2. The error in the proportion of zero flows ('ErrorPropZero.csv')3. The precision metric used in this study ('Precision.csv')4. The reliability metric used in this study ('Reliability.csv')5. The volumetric bias metric used in this study ('VolBias.csv')Also, the proportion of observed zero flows for each catchment is provided ('PropZero.csv').<br><br>
DOI: 10.25909/5c91790f7ff7f
title: Raw Data Report of Surveys

description: These data are the values of the correlation matrix of responses, the sort-values of each participants q-sort, factor analysis results, and free-text comments associated with most highly-ranked and lowest-ranked items.
DOI: 10.25909/5c917a2372b30
title: Full report of analysis output, plus summary of distinguishing statement

description: An excel spreadsheet that contains a clean copy of the Q-Assessor analysis output with separate tabs that contain the distinguishing statements of each factor. The distinguishing statements allow for interpretation of factor meanings.
DOI: 10.25909/5c917f5bc15f6
title: Coding and analysis records of transcribed interviews

description: These records reflect how the interview data was classified and coded using NVivo 12.
DOI: 10.5281/zenodo.17217914
title: The UAH Predictions of the Solar Wind and Magnetic Field at the Parker Solar Probe during Solar Encounter 25 (2025-09-17)

description: 1. Model

The MS-FLUKSS heliospheric MHD model is coupled with the WSA model (Kim et al. 2020), which used ADAPT-GONG input magnetograms, with the PFSS source surface height and the WSA outer boundary at 2.5 and 21.5 solar radii, respectively. The MHD model propagates the solar wind from 21.5 solar radii to 236 solar radii (1.1 AU) to fully enclose the PSP trajectory. Hence, field line tracing from PSP to the solar surface is performed through the MHD domain down to 21.5 solar radii instantaneously at approximately 1 hour cadence, where the origin of the field line on the photosphere is already known in the WSA model. See Badman et al. (2023) for details.

MS-FLUKSS: Multi-Scale Fluid-Kinetic Simulation Suite

MHD: Magnetohydrodynamic

WSA: Wang-Sheeley-Arge

ADAPT: Air Force Data Assimilative Photospheric flux Transport

GONG: Global Oscillation Network Group

PFSS: Potential Field Source Surface

PSP: Parker Solar Probe

 

2. Data

There are two sets of data files as described below:

(A) "PSP_AGONG_R000.dat" - "PSP_AGONG_R011.dat": MS-FLUKSS simulation results extracted along the PSP trajectory labeled by the input magnetogram (each of the 12 realizations of ADAPT-GONG) for the WSA model. 

Each data file consist of a header and 16 columns of numerical values in the following order:

(1) Time (fractional year)

(2) Heliocentric distance (AU)

(3) MS-FLUKSS longitude (rotated by ~180 degrees from inertial heliographic longitude in degrees)

(4) MS-FLUKSS latitude (same as heliographic latitude in degrees)

(5) Solar wind proton number density (cm^-3)

(6) Solar wind Vr (km/s)

(7) Solar wind Vphi (km/s)

(8) Solar wind Vtheta (km/s)

(9) Thermal pressure of solar wind and interstellar pickup ion mixture (picodyne/cm^2)

(10) Br (microgauss)

(11) Bphi (microgauss)

(12) Btheta (microgauss)

(13) Level set value for tracking the heliospheric current sheet

(14) Level set value for tracking the initial MS-FLUKSS longitude at the inner boundary

(15) Level set value for tracking the initial MS-FLUKSS latitude at the inner boundary

(16) Solar wind temperature.

 

(B) "UAH_psp_e25_20250917*_agongWSAmhd.csv": Carrington longitude and latitude of the predicted magnetic footpoint from 2025-09-17 to 2025-09-30.

 

Each data file consists of 4 columns of numeric values in the following order:

(1) Date (YYYY-MM-DD)

(2) Time (hh:mm:ss in UT)

(3) Carrington longitude (degree)

(4) Carrington latitude (degree)

 

3. Figures

There is one figure showing plots of predicted Br, Vr, density, and temperature at PSP: uah_psp_e25_20250917_agongWSAmhd.pdf.

A plot showing the footpoint prediction results projected onto the solar disk is available at the PSP science gateway, at https://psp-gateway.jhuapl.edu/website/SciencePlanning/MissionEvents/, under “Encounter 25”.
DOI: 10.5281/zenodo.17217872
title: The UAH Predictions of the Solar Wind and Magnetic Field at the Parker Solar Probe during Solar Encounter 25 (2025-09-16)

description: 1. Model

The MS-FLUKSS heliospheric MHD model is coupled with the WSA model (Kim et al. 2020), which used ADAPT-GONG input magnetograms, with the PFSS source surface height and the WSA outer boundary at 2.5 and 9 solar radii, respectively. The MHD model propagates the solar wind from 9 solar radii to 236 solar radii (1.1 AU) to fully enclose the PSP trajectory. Hence, field line tracing from PSP to the solar surface is performed through the MHD domain down to 9 solar radii instantaneously at approximately 1 hour cadence, where the origin of the field line on the photosphere is already known in the WSA model. See Badman et al. (2023) for details.

MS-FLUKSS: Multi-Scale Fluid-Kinetic Simulation Suite

MHD: Magnetohydrodynamic

WSA: Wang-Sheeley-Arge

ADAPT: Air Force Data Assimilative Photospheric flux Transport

GONG: Global Oscillation Network Group

PFSS: Potential Field Source Surface

PSP: Parker Solar Probe

 

2. Data

There are two sets of data files as described below:

(A) "PSP_AGONG_R000.dat" - "PSP_AGONG_R011.dat": MS-FLUKSS simulation results extracted along the PSP trajectory labeled by the input magnetogram (each of the 12 realizations of ADAPT-GONG) for the WSA model. 

Each data file consist of a header and 16 columns of numerical values in the following order:

(1) Time (fractional year)

(2) Heliocentric distance (AU)

(3) MS-FLUKSS longitude (rotated by ~180 degrees from inertial heliographic longitude in degrees)

(4) MS-FLUKSS latitude (same as heliographic latitude in degrees)

(5) Solar wind proton number density (cm^-3)

(6) Solar wind Vr (km/s)

(7) Solar wind Vphi (km/s)

(8) Solar wind Vtheta (km/s)

(9) Thermal pressure of solar wind and interstellar pickup ion mixture (picodyne/cm^2)

(10) Br (microgauss)

(11) Bphi (microgauss)

(12) Btheta (microgauss)

(13) Level set value for tracking the heliospheric current sheet

(14) Level set value for tracking the initial MS-FLUKSS longitude at the inner boundary

(15) Level set value for tracking the initial MS-FLUKSS latitude at the inner boundary

(16) Solar wind temperature.

 

(B) "UAH_psp_e25_20250916*_agongWSAmhd.csv": Carrington longitude and latitude of the predicted magnetic footpoint from 2025-09-16 to 2025-09-30.

 

Each data file consists of 4 columns of numeric values in the following order:

(1) Date (YYYY-MM-DD)

(2) Time (hh:mm:ss in UT)

(3) Carrington longitude (degree)

(4) Carrington latitude (degree)

 

3. Figures

There is one figure showing plots of predicted Br, Vr, density, and temperature at PSP: uah_psp_e25_20250916_agongWSAmhd.pdf.

A plot showing the footpoint prediction results projected onto the solar disk is available at the PSP science gateway, at https://psp-gateway.jhuapl.edu/website/SciencePlanning/MissionEvents/, under “Encounter 25”.
DOI: 10.5281/zenodo.17217873
title: The UAH Predictions of the Solar Wind and Magnetic Field at the Parker Solar Probe during Solar Encounter 25 (2025-09-16)

description: 1. Model

The MS-FLUKSS heliospheric MHD model is coupled with the WSA model (Kim et al. 2020), which used ADAPT-GONG input magnetograms, with the PFSS source surface height and the WSA outer boundary at 2.5 and 9 solar radii, respectively. The MHD model propagates the solar wind from 9 solar radii to 236 solar radii (1.1 AU) to fully enclose the PSP trajectory. Hence, field line tracing from PSP to the solar surface is performed through the MHD domain down to 9 solar radii instantaneously at approximately 1 hour cadence, where the origin of the field line on the photosphere is already known in the WSA model. See Badman et al. (2023) for details.

MS-FLUKSS: Multi-Scale Fluid-Kinetic Simulation Suite

MHD: Magnetohydrodynamic

WSA: Wang-Sheeley-Arge

ADAPT: Air Force Data Assimilative Photospheric flux Transport

GONG: Global Oscillation Network Group

PFSS: Potential Field Source Surface

PSP: Parker Solar Probe

 

2. Data

There are two sets of data files as described below:

(A) "PSP_AGONG_R000.dat" - "PSP_AGONG_R011.dat": MS-FLUKSS simulation results extracted along the PSP trajectory labeled by the input magnetogram (each of the 12 realizations of ADAPT-GONG) for the WSA model. 

Each data file consist of a header and 16 columns of numerical values in the following order:

(1) Time (fractional year)

(2) Heliocentric distance (AU)

(3) MS-FLUKSS longitude (rotated by ~180 degrees from inertial heliographic longitude in degrees)

(4) MS-FLUKSS latitude (same as heliographic latitude in degrees)

(5) Solar wind proton number density (cm^-3)

(6) Solar wind Vr (km/s)

(7) Solar wind Vphi (km/s)

(8) Solar wind Vtheta (km/s)

(9) Thermal pressure of solar wind and interstellar pickup ion mixture (picodyne/cm^2)

(10) Br (microgauss)

(11) Bphi (microgauss)

(12) Btheta (microgauss)

(13) Level set value for tracking the heliospheric current sheet

(14) Level set value for tracking the initial MS-FLUKSS longitude at the inner boundary

(15) Level set value for tracking the initial MS-FLUKSS latitude at the inner boundary

(16) Solar wind temperature.

 

(B) "UAH_psp_e25_20250916*_agongWSAmhd.csv": Carrington longitude and latitude of the predicted magnetic footpoint from 2025-09-16 to 2025-09-30.

 

Each data file consists of 4 columns of numeric values in the following order:

(1) Date (YYYY-MM-DD)

(2) Time (hh:mm:ss in UT)

(3) Carrington longitude (degree)

(4) Carrington latitude (degree)

 

3. Figures

There is one figure showing plots of predicted Br, Vr, density, and temperature at PSP: uah_psp_e25_20250916_agongWSAmhd.pdf.

A plot showing the footpoint prediction results projected onto the solar disk is available at the PSP science gateway, at https://psp-gateway.jhuapl.edu/website/SciencePlanning/MissionEvents/, under “Encounter 25”.
DOI: 10.5281/zenodo.17217913
title: The UAH Predictions of the Solar Wind and Magnetic Field at the Parker Solar Probe during Solar Encounter 25 (2025-09-17)

description: 1. Model

The MS-FLUKSS heliospheric MHD model is coupled with the WSA model (Kim et al. 2020), which used ADAPT-GONG input magnetograms, with the PFSS source surface height and the WSA outer boundary at 2.5 and 21.5 solar radii, respectively. The MHD model propagates the solar wind from 21.5 solar radii to 236 solar radii (1.1 AU) to fully enclose the PSP trajectory. Hence, field line tracing from PSP to the solar surface is performed through the MHD domain down to 21.5 solar radii instantaneously at approximately 1 hour cadence, where the origin of the field line on the photosphere is already known in the WSA model. See Badman et al. (2023) for details.

MS-FLUKSS: Multi-Scale Fluid-Kinetic Simulation Suite

MHD: Magnetohydrodynamic

WSA: Wang-Sheeley-Arge

ADAPT: Air Force Data Assimilative Photospheric flux Transport

GONG: Global Oscillation Network Group

PFSS: Potential Field Source Surface

PSP: Parker Solar Probe

 

2. Data

There are two sets of data files as described below:

(A) "PSP_AGONG_R000.dat" - "PSP_AGONG_R011.dat": MS-FLUKSS simulation results extracted along the PSP trajectory labeled by the input magnetogram (each of the 12 realizations of ADAPT-GONG) for the WSA model. 

Each data file consist of a header and 16 columns of numerical values in the following order:

(1) Time (fractional year)

(2) Heliocentric distance (AU)

(3) MS-FLUKSS longitude (rotated by ~180 degrees from inertial heliographic longitude in degrees)

(4) MS-FLUKSS latitude (same as heliographic latitude in degrees)

(5) Solar wind proton number density (cm^-3)

(6) Solar wind Vr (km/s)

(7) Solar wind Vphi (km/s)

(8) Solar wind Vtheta (km/s)

(9) Thermal pressure of solar wind and interstellar pickup ion mixture (picodyne/cm^2)

(10) Br (microgauss)

(11) Bphi (microgauss)

(12) Btheta (microgauss)

(13) Level set value for tracking the heliospheric current sheet

(14) Level set value for tracking the initial MS-FLUKSS longitude at the inner boundary

(15) Level set value for tracking the initial MS-FLUKSS latitude at the inner boundary

(16) Solar wind temperature.

 

(B) "UAH_psp_e25_20250917*_agongWSAmhd.csv": Carrington longitude and latitude of the predicted magnetic footpoint from 2025-09-17 to 2025-09-30.

 

Each data file consists of 4 columns of numeric values in the following order:

(1) Date (YYYY-MM-DD)

(2) Time (hh:mm:ss in UT)

(3) Carrington longitude (degree)

(4) Carrington latitude (degree)

 

3. Figures

There is one figure showing plots of predicted Br, Vr, density, and temperature at PSP: uah_psp_e25_20250917_agongWSAmhd.pdf.

A plot showing the footpoint prediction results projected onto the solar disk is available at the PSP science gateway, at https://psp-gateway.jhuapl.edu/website/SciencePlanning/MissionEvents/, under “Encounter 25”.
DOI: 10.25909/5c9589e08dfe3
title: Raspi Flat field Images - Camera 01

description: Various single flat field images taken with different integrated lenses using a Raspberry Pi V2 camera at 30°C.<br>The set contains 3669 flat field images per set in TIFF and JPEG format. Each image is approximattely16.2MB in size. Each JPEG image is 10.5MB. Each camera set is approximately 48GB in size.<br>Images are captured in JPEG format with Bayer 10-bit raw data appended to the end of the file. This is extracted using DCRAW. Full research methodology for obtaining these images can be read in DOI:10.1016/j.diin.2019.02.002<br><b>File structure:</b>Each compressed folder contains one camera's data. This is then segregated into subfolders which contains six folders representing each discrete lens used in the data collection process. This is combined with six pinhole lenses that were also used in the data collection process. Each of these folders is divided into a JPEG folder which contains the raw output of the sensor and a TIFF folder which contains the DCRAW converted images. The TIFF folder is then broken down into the images and a seperate folder called Fingerprint which contains the 50 images used to construct a reference pattern for the camera with that discrete lens.<br>The image is stored as a file name "BAYERYYYYMMDD-HHMMSS.tiff" where YYYY, MM, DD, HH, MM, SS represent standard ISO time stamp format.<br><b>Example Tree for Raspi01</b>/Raspi01.zip|-- Lens-01| |--JPEG| | |-- BAYER20170926-082159.jpg| | |-- BAYER20170926-082205.jpg| | | ...| | |-- BAYER20170926-084017.jpg| || |--TIFF| | | fingerprint| | | | -- BAYER20170926-083446.tiff| | | | -- BAYER20170926-083452.tiff| | | | ...| | | | -- BAYER20170926-084017.tiff| | || | |-- BAYER20170926-082159.tiff| | |-- BAYER20170926-082205.tiff| | | ...| | |-- BAYER20170926-083440.tiff||-- Lens-02|-- Lens-03<br>|-- Lens-04<br>|-- Lens-05<br>|-- Lens-06<br>|-- Pinhole-01<br>|-- Pinhole-02<br>|-- Pinhole-03<br>|-- Pinhole-04<br>|-- Pinhole-05<br>|<sub>--</sub> Pinhole-05
DOI: 10.25909/5c982265c4d37
title: Definitions and data for postoperative complications ERA Model.docx

description: This table provides data on the incidence of mortality and rare graft complications after endovascular aneurysm repair. It includes definitions of how the complications were combined for data modelling and provides additional information to be read along with the ERA Model interactive Excel spreadsheet
DOI: 10.25909/5c98a2188c0a1
title: Raspi Flat field Images - Camera 04

description: Various single flat field images taken with different integrated lenses using a Raspberry Pi V2 camera at 30°C.<br>The set contains 3669 flat field images per set in TIFF and JPEG format. Each image is approximattely16.2MB in size. Each JPEG image is 10.5MB. Each camera set is approximately 48GB in size.<br>Images are captured in JPEG format with Bayer 10-bit raw data appended to the end of the file. This is extracted using DCRAW. Full research methodology for obtaining these images can be read in DOI:10.1016/j.diin.2019.02.002<br><b>File structure:</b>Each compressed folder contains one camera's data. This is then segregated into subfolders which contains six folders representing each discrete lens used in the data collection process. This is combined with six pinhole lenses that were also used in the data collection process. Each of these folders is divided into a JPEG folder which contains the raw output of the sensor and a TIFF folder which contains the DCRAW converted images. The TIFF folder is then broken down into the images and a seperate folder called Fingerprint which contains the 50 images used to construct a reference pattern for the camera with that discrete lens.<br>The image is stored as a file name "BAYERYYYYMMDD-HHMMSS.tiff" where YYYY, MM, DD, HH, MM, SS represent standard ISO time stamp format.<br><b>Example Tree for Raspi01</b>/Raspi01.zip|-- Lens-01| |--JPEG| | |-- BAYER20170926-082159.jpg| | |-- BAYER20170926-082205.jpg| | | ...| | |-- BAYER20170926-084017.jpg| || |--TIFF| | | fingerprint| | | | -- BAYER20170926-083446.tiff| | | | -- BAYER20170926-083452.tiff| | | | ...| | | | -- BAYER20170926-084017.tiff| | || | |-- BAYER20170926-082159.tiff| | |-- BAYER20170926-082205.tiff| | | ...| | |-- BAYER20170926-083440.tiff||-- Lens-02|-- Lens-03<br>|-- Lens-04<br>|-- Lens-05<br>|-- Lens-06<br>|-- Pinhole-01<br>|-- Pinhole-02<br>|-- Pinhole-03<br>|-- Pinhole-04<br>|-- Pinhole-05<br>|<sub>--</sub> Pinhole-05
DOI: 10.25909/5c9a94e38f658
title: Raspi Flat field Images - Camera 02

description: Various single flat field images taken with different integrated lenses using a Raspberry Pi V2 camera at 30°C.<br>The set contains 3669 flat field images per set in TIFF and JPEG format. Each image is approximattely16.2MB in size. Each JPEG image is 10.5MB. Each camera set is approximately 48GB in size.<br>Images are captured in JPEG format with Bayer 10-bit raw data appended to the end of the file. This is extracted using DCRAW. Full research methodology for obtaining these images can be read in DOI:10.1016/j.diin.2019.02.002<br><b>File structure:</b>Each compressed folder contains one camera's data. This is then segregated into subfolders which contains six folders representing each discrete lens used in the data collection process. This is combined with six pinhole lenses that were also used in the data collection process. Each of these folders is divided into a JPEG folder which contains the raw output of the sensor and a TIFF folder which contains the DCRAW converted images. The TIFF folder is then broken down into the images and a seperate folder called Fingerprint which contains the 50 images used to construct a reference pattern for the camera with that discrete lens.<br>The image is stored as a file name "BAYERYYYYMMDD-HHMMSS.tiff" where YYYY, MM, DD, HH, MM, SS represent standard ISO time stamp format.<br><b>Example Tree for Raspi01</b>/Raspi01.zip|-- Lens-01| |--JPEG| | |-- BAYER20170926-082159.jpg| | |-- BAYER20170926-082205.jpg| | | ...| | |-- BAYER20170926-084017.jpg| || |--TIFF| | | fingerprint| | | | -- BAYER20170926-083446.tiff| | | | -- BAYER20170926-083452.tiff| | | | ...| | | | -- BAYER20170926-084017.tiff| | || | |-- BAYER20170926-082159.tiff| | |-- BAYER20170926-082205.tiff| | | ...| | |-- BAYER20170926-083440.tiff||-- Lens-02|-- Lens-03<br>|-- Lens-04<br>|-- Lens-05<br>|-- Lens-06<br>|-- Pinhole-01<br>|-- Pinhole-02<br>|-- Pinhole-03<br>|-- Pinhole-04<br>|-- Pinhole-05<br>|<sub>--</sub> Pinhole-05
DOI: 10.25909/5cb952bd0861c
title: Supplementary material from: Modelling the distribution of a wide-ranging invasive species using the sampling efforts of expert and citizen scientists.

description: 1- Results for the models calibrated with <i>Weigted Pts</i> pseudo-absences for the paper 'Modelling the distribution of a wide-ranging invasive species using the sampling efforts of expert and citizen scientists'.2- Final figure of the probability of distribution of rabbits in black and white.3- Final figure of the probability of distribution of rabbits in ASC format.<br>
DOI: 10.25909/5caaf18c3450d
title: Supporting Data - Naturally-diverse airborne environmental microbial exposures modulate the gut microbiome and may provide anxiolytic benefits in mice

description: Supporting data and code for the study "Naturally-diverse airborne environmental microbial exposures modulate the gut microbiome and may provide anxiolytic benefits in mice" by Craig Liddicoat, Harrison Sydnor, Christian Cando-Dumancela, Romy Dresken, Jiajun Liu, Nicholas J.C. Gellie, Jacob G. Mills, Jennifer Young, Laura Weyrich, Mark R. Hutchinson, Philip Weinstein, Martin F. Breed.<br>Refer to the Data description document for information on the contents of each file.