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opencc-by-4.0Aug 2023View details →

ACCESS-AM2 dust fields 2015-2019

The ACCESS-AM2 (Australian Community Climate and Earth-System Simulator - Atmospheric Model Version 2) data used in Weis et al. (2024), Nature Geoscience, <a href="https://doi.org/10.1038/s41586-024-07366-4">https://doi.org/10.1038/s41586-024-07366-4</a> The data set includes:  <ul> <li>Dust mass mixing ratios at surface</li> <li>Dry and wet deposition fluxes </li> <li>Dust optical depth </li> <li>10m U and V wind components </li> </ul>

opencc-by-4.0Jan 2024View details →

Figure 1 in Fauna and distribution of house dust mites in two northern districts of Kerala, India

Figure 1. The distribution of mite Dermatophagoides pteronyssinus in rural and urban areas of Malappuram and Kozhikkode districts.

opencc-by-4.0Apr 2024View details →

Data for "Improved constraints on hematite refractive index for estimating climatic effects of dust aerosols"

This repository contains calculated/simulated data on the imaginary part of the complex refractive index, single scattering albedo, and/or optical depth for dust aerosols in the visible band or at the wavelength of 550 nm. For detailed information on (1) the acquisition and utilization of this data, (2) comprehensive configurations for model simulations, (3) the principal findings, and (4) the methodology employed to achieve these findings, please refer to the article authored by Li, Mahowald et al. (2024; Commun. Earth Environ). Other datasets, including the code and laboratory observations presented in the paper, can be found elsewhere (refer to the Data and Code Availability sections of the paper). For any clarification regarding the data and code, inquiries related to the publication, or potential collaboration, please contact Longlei Li (<a href="mailto:ll859@cornell.edu">ll859@cornell.edu</a>) or Natalie M. Mahowald (<a href="mailto:mahowald@cornell.edu">mahowald@cornell.edu</a>).

Dust extinction curves: Ferrara (1999) original resolution

These datasets are based on the models described in <a href="https://ui.adsabs.harvard.edu/abs/2018RNAAS...2..188B">Benson (2018)</a>, and are intended to closely match the models run by <a href="http://adsabs.harvard.edu/abs/1999ApJS..123..437F">Ferrara et al. (1999)</a> - they use the same dust grain properties and galactic geometry. Additionally, they are tabulated at the same inclinations, optical depths, wavelengths, and morphologies as in <a href="http://adsabs.harvard.edu/abs/1999ApJS..123..437F">Ferrara et al. (1999)</a>. Dust Properties Dust grain albedos, scattering asymmetries, and opacities to extinction are taken from <a href="http://adsabs.harvard.edu/abs/1997ApJ...487..625G">Gordon et al. (1997)</a>, for either their Milky Way, “MW”, or Small Magellanic Cloud, “SMC”, models (as encoded in each file name), and assume Henyey-Greenstein scattering.   Stellar Geometry Galactic disks follow exponential profiles in both radial and vertical directions, with the vertical scale height equal to 0.0875 times the radial scale length. Spheroids follow spherical <a href="http://adsabs.harvard.edu/abs/1983MNRAS.202..995J">Jaffe (1983)</a> profiles. Note that spheroid radii in this work are listed as the scale radius, rs, while <a href="http://adsabs.harvard.edu/abs/1999ApJS..123..437F">Ferrara et al. (1999)</a> listed the corresponding effective radius, re=rs/1.16. Dust Geometry Dust is distributed in the disk, and follows exponential profiles in both radial and vertical directions. The vertical scale height is set to a multiple, hz, of the stellar disk scale height. The value of hz is encoded in each file name.

Dust extinction curves: KMH94 R_V=5.5 model

This dataset is based on the models described in <a href="https://ui.adsabs.harvard.edu/abs/2018RNAAS...2..188B">Benson (2018)</a>. Dust Properties Dust grain properties are taken from <a href="http://adsabs.harvard.edu/abs/1994ApJ...422..164K">Kim, Martin, and Hendry (1994)</a>, specifically their model with with RV=3.1 and a full scattering calculation. Stellar Geometry Galactic disks follow exponential profiles in the radial direction, and sech2 distributions in the vertical direction. The vertical scale height is set to a multiple, hd, of the stellar disk scale length, and its value is encoded in each file name. Spheroids follow spherical <a href="http://adsabs.harvard.edu/abs/1990ApJ...356..359H">Hernquist (1990)</a> profiles. Dust Geometry Dust is distributed in the disk, and follows exponential profiles in both radial and vertical directions. The vertical scale height is set to a multiple, hz, of the stellar disk scale length, and its value is encoded in each file name.

Dust extinction curves: KMH94 HG R_V=5.5 model

This dataset is based on the models described in <a href="https://ui.adsabs.harvard.edu/abs/2018RNAAS...2..188B">Benson (2018)</a>. Dust Properties Dust grain properties are taken from <a href="http://adsabs.harvard.edu/abs/1994ApJ...422..164K">Kim, Martin, and Hendry (1994)</a>, specifically their model with with RV=3.1 and Henyey-Greenstein scattering. Stellar Geometry Galactic disks follow exponential profiles in the radial direction, and sech2 distributions in the vertical direction. The vertical scale height is set to a multiple, hd, of the stellar disk scale length, and its value is encoded in each file name. Spheroids follow spherical <a href="http://adsabs.harvard.edu/abs/1990ApJ...356..359H">Hernquist (1990)</a> profiles. Dust Geometry Dust is distributed in the disk, and follows exponential profiles in both radial and vertical directions. The vertical scale height is set to a multiple, hz, of the stellar disk scale length, and its value is encoded in each file name.

Dust extinction curves: Grasil-like

These datasets are based on the models described in <a href="https://ui.adsabs.harvard.edu/abs/2018RNAAS...2..188B">Benson (2018)</a>, and are intended to mimic the geometries used by <a href="https://adlibitum.oats.inaf.it/silva/grasil/grasil.html">Grasil</a>. Dust Properties Dust grain properties are taken from <a href="http://adsabs.harvard.edu/abs/2003ARA%26A..41..241D">Draine (2003)</a> - specifically their model with either RV=3.1 or RV=5.5 as encoded in the file name with prefix dustD03. Stellar Geometry Galactic disks follow exponential profiles in both radial and vertical directions, with the vertical scale height equal to 0.1 or 0.5 times the radial scale length as encoded in the file name with prefix hzStars. Note that spheroid radii in this work are listed as the scale radius, rs, while <a href="http://adsabs.harvard.edu/abs/1999ApJS..123..437F">Ferrara et al. (1999)</a> listed the corresponding effective radius, re=rs/1.16. Dust Geometry Dust is distributed in the disk, and follows exponential profiles in both radial and vertical directions. The vertical scale height is set to a multiple, hz, of the stellar disk scale height. The value of hz is encoded in each file name with prefix hzDust.

Dust extinction curves: Draine R_V=5.5 model

This dataset is based on the models described in <a href="https://ui.adsabs.harvard.edu/abs/2018RNAAS...2..188B">Benson (2018)</a>. Dust Properties Dust grain properties are taken from <a href="http://adsabs.harvard.edu/abs/2003ARA%26A..41..241D">Draine (2003)</a> - specifically their model with RV=5.5. Stellar Geometry Galactic disks follow exponential profiles in the radial direction, and sech2 distributions in the vertical direction. The vertical scale height is set to a multiple, hd, of the stellar disk scale length, and its value is encoded in each file name. Spheroids follow spherical <a href="http://adsabs.harvard.edu/abs/1990ApJ...356..359H">Hernquist (1990)</a> profiles. Dust Geometry Dust is distributed in the disk, and follows exponential profiles in both radial and vertical directions. The vertical scale height is set to a multiple, hz, of the stellar disk scale length, and its value is encoded in each file name.

Dust extinction curves: Draine R_V=3.1 model

This dataset is based on the models described in <a href="https://ui.adsabs.harvard.edu/abs/2018RNAAS...2..188B">Benson (2018)</a>. Dust Properties Dust grain properties are taken from <a href="http://adsabs.harvard.edu/abs/2003ARA%26A..41..241D">Draine (2003)</a> - specifically their model with RV=3.1. Stellar Geometry Galactic disks follow exponential profiles in the radial direction, and sech2 distributions in the vertical direction. The vertical scale height is set to a multiple, hd, of the stellar disk scale length, and its value is encoded in each file name. Spheroids follow spherical <a href="http://adsabs.harvard.edu/abs/1990ApJ...356..359H">Hernquist (1990)</a> profiles. Dust Geometry Dust is distributed in the disk, and follows exponential profiles in both radial and vertical directions. The vertical scale height is set to a multiple, hz, of the stellar disk scale length, and its value is encoded in each file name.

Dust extinction curves: Draine R_V=4.0 model

This dataset is based on the models described in <a href="https://ui.adsabs.harvard.edu/abs/2018RNAAS...2..188B">Benson (2018)</a>. Dust Properties Dust grain properties are taken from <a href="http://adsabs.harvard.edu/abs/2003ARA%26A..41..241D">Draine (2003)</a> - specifically their model with RV=4.0. Stellar Geometry Galactic disks follow exponential profiles in the radial direction, and sech2 distributions in the vertical direction. The vertical scale height is set to a multiple, hd, of the stellar disk scale length, and its value is encoded in each file name. Spheroids follow spherical <a href="http://adsabs.harvard.edu/abs/1990ApJ...356..359H">Hernquist (1990)</a> profiles. Dust Geometry Dust is distributed in the disk, and follows exponential profiles in both radial and vertical directions. The vertical scale height is set to a multiple, hz, of the stellar disk scale length, and its value is encoded in each file name.

Dust extinction curves: Ferrara (1999) high resolution

These datasets are based on the models described in <a href="https://ui.adsabs.harvard.edu/abs/2018RNAAS...2..188B">Benson (2018)</a>, and are intended to closely match the models run by <a href="http://adsabs.harvard.edu/abs/1999ApJS..123..437F">Ferrara et al. (1999)</a> - they use the same dust grain properties and galactic geometry. However, they are tabulated using a much higher resolution grid of inclinations, optical depths, wavelengths, and morphologies than in <a href="http://adsabs.harvard.edu/abs/1999ApJS..123..437F">Ferrara et al. (1999)</a>. Dust Properties Dust grain albedos, scattering asymmetries, and opacities to extinction are taken from <a href="http://adsabs.harvard.edu/abs/1997ApJ...487..625G">Gordon et al. (1997)</a>, for either their Milky Way, “MW”, or Small Magellanic Cloud, “SMC”, models (as encoded in each file name), and assume Henyey-Greenstein scattering.   Stellar Geometry Galactic disks follow exponential profiles in both radial and vertical directions, with the vertical scale height equal to 0.0875 times the radial scale length. Spheroids follow spherical <a href="http://adsabs.harvard.edu/abs/1983MNRAS.202..995J">Jaffe (1983)</a> profiles. Note that spheroid radii in this work are listed as the scale radius, rs, while <a href="http://adsabs.harvard.edu/abs/1999ApJS..123..437F">Ferrara et al. (1999)</a> listed the corresponding effective radius, re=rs/1.16. Dust Geometry Dust is distributed in the disk, and follows exponential profiles in both radial and vertical directions. The vertical scale height is set to a multiple, hz, of the stellar disk scale height. The value of hz is encoded in each file name.

Data Supplement for ApJ Paper: Stumbling over planetary building blocks: AU Microscopii as an exampleof the challenge of retrieving debris-disk dust properties

Computational data set underlying a manuscript analyzing visible to near infrared wavelength Hubble-STIS spectrographic coronagraph observations of the AU Microscopii debis disk. To interpret this multi-wavelength data set, we calculated light scattering properties of three different debris disk dust grain shape models: spheres, porous spheres, and more realistic irregular agglomerated debris particles. Calculations of scattering efficiency and phase function were done over a range of dust grain sizes and material refractive indices. This bundle contains three .hdf table files. Each table file contains a size parameter array (1D), complex refractive index array (1D), scattering efficiency array (1D), and scattering phase function array (2D). The 1st dimension of each array is the same size. The 2nd dimension of the scattering phase function is 60, the number of scattering angles calculated at an angular resolution of 3 degrees.

opencc-by-4.0Feb 2022View details →

Dataset for Bate (2022): Dust coagulation during the early stages of star formation: molecular cloud collapse and first hydrostatic core evolution

This data set contains 12 smoothed particle hydrodynamics (SPH) dump files that were used to produce some of the figures in the journal paper: Bate, Matthew. R., 2022, Monthly Notices of the Royal Astronomical Society, accepted 13 May 2022 Each of the SPH dump files is from a different calculation of the early stages of star formation: the gravitational collapse of a molecular cloud core, including dust coagulation.  Each SPH dump file gives the state of the SPH calculation when the maximum temperature reached 1500 K, except for the beta=0.05 cases which give the state when the maximum hydrogen number density reaches 10^{14} cm^{-3}.  The calculations were each performed using 3 million SPH particles and differed by their initial rotation rate, which was parameterised by beta=0, 0.0025, 0.005, 0.01, 0.02, and 0.05 (the magnitude of the ratio of the rotational and gravitational potential energies).  Dump files from calculations that include and exclude envelope turbulence are provided (both are used for Figure B1).  The dump files associated with each calculation are: beta=0:      B1M0123 (does not include envelope turbulence) beta=0.0025: B1M2123 (does not include envelope turbulence) beta=0.005:  B1M5123 (does not include envelope turbulence) beta=0.01:   B1M1128 (does not include envelope turbulence) beta=0.02:   B1M2126 (does not include envelope turbulence) beta=0.05:   B1M5109_b05_NoEnvTurb (does not include envelope turbulence) beta=0.0:    B1M0123_b0_EnvTurb beta=0.0025: B1M2177_b0025_EnvTurb beta=0.005:  B1M5209_b005_EnvTurb beta=0.01:   B1M1219_b01_EnvTurb beta=0.02:   B1M2221_b02_EnvTurb beta=0.05:   B1M5321_b05_EnvTurb The SPH dump files are Fortran binary files written in big endian format and generated by the sphNG code (Benz 1990; Bate 1995; Bate & Keto 2015). They can be read, visualised, and manipulated using the free, publicly available SPLASH visualisation code (which reads sphNG dump files), written by Daniel J. Price, that can be downloaded from:  http://users.monash.edu.au/~dprice/splash/  The SPLASH configuration files used to produce Figs. 10,11,12,and B1 in Bate (2022) are included with this dataset in a gzipped tar file.

opencc-by-4.0Jul 2022View details →

Engineering Dust Coma Model (EDCM) for ESA's Comet Interceptor mission to a dynamically new comet

This data-set contains all results from the Engineering Dust Coma Model (EDCM) for ESA's Comet Interceptor (CI) mission to a dynamically new comet. A full description of the model behind the data can be found in the peer-reviewed paper Marschall, Zakharov et al. (2022), <a href="https://doi.org/10.1051/0004-6361/202243648">https://doi.org/10.1051/0004-6361/202243648</a>. Please cite this data-set and the paper when using the data. Contemporary numerical models of dusty-gas coma are used to obtain spatial distribution of dust for a given set of parameters. By varying parameters within a range of possible values we obtain an ensemble of possible dust distributions. Then, this ensemble is statistically evaluated in order to define the most probable cases and hence reduce the dispersion. This ensemble can be used to estimate not only the likely dust abundance along e.g. a fly-by trajectory of a spacecraft but also quantify the associated uncertainty. The dust environment assessment for the case when the target comet is not known beforehand (or when its parameters are known with large uncertainty) is critical for spacecraft safety and planning. The EDCM provides an assessment of dust environment for the CI mission.

Figure 3 in Species identification and seasonal prevalence of house dust mites in Assiut City, Egypt: A descriptive study in an urban area

Figure 3. Dermatophagoides farinae adult female (SEM photo) – a. Dorsal view shows sce (external scapular seta) is much longer than sci (internal scapular seta); b. Ventral view shows the genital system of the female; c. Lateral views shows the finely striated body and prodorsal shield; d. Hysterostoma region and anal opening; e. Epigynium and genital opening; f. Ventral view of the gnathostoma.

Figure 2 in Species identification and seasonal prevalence of house dust mites in Assiut City, Egypt: A descriptive study in an urban area

Figure 2. Dermatophagoides farinae (adult male) – a. Habitus (100×) before being cleared in Hoyer's medium and the enlarged 1st and 3rd pairs of legs are noted; b. Fused apodemes I (arrow) while apodemes II (arrow head) and apodemes III (curved arrow) are not fused (200×); c. Anal plate (arrow), post anal seta 2 (ps2) (curved arrow) (400×).

Figure 1 in Species identification and seasonal prevalence of house dust mites in Assiut City, Egypt: A descriptive study in an urban area

Figure 1. Dermatophagoides farinae (adult female) – a. Habitus (before being cleared) (10×); b. Habitus (after being cleared in Hoyer's medium) (x100); c. Distal solenidion on tarsus I (arrow head), terminal spinous process (curved arrow) and tarsus II with the two distal solenidia (arrow) (200×); d. Magnified tarsus II with distal solenidia (arrow head) and two small spinous tubercles (long arrow) (400×); e. The low-arched epigynium (arrow) and the faint transverse striations above it (arrow head); f. Bursa copulatrix (arrow), its external opening and sclerotized part (arrow head).

Figure 4 in Species identification and seasonal prevalence of house dust mites in Assiut City, Egypt: A descriptive study in an urban area

Figure 4. Dermatophagoides farinae adult male (SEM photo) – a. Ventral view showing the enlarged first pair of legs. B. The aedeagus; c. The anal plate containing the anal suckers.

opencc-zeroApr 2024View details →

dryad40/100

Concentrations of the rare earth elements (REE) and Thorium-232 (232Th) in glacial dust from the northern Gulf of Alaska region

Concentrations of the rare earth elements (REE) and Thorium-232 (232Th) are presented for filtered air (dust) samples collected from the northern Gulf of Alaska region, including from Middleton Island (AK)(59.4214 N, 146.3493 W) and the Copper River delta (60.4324 N, 145.0954 W). Size-fractionated samples were collected in November 2019, using a Tisch Volumetric Flow Controlled (VFC) high volume sampler (Tisch Environmental, TE-5170V- BL) outfitted with a Cascade impactor. The six size fractions collected ranged from <0.49 micrometers (um) to >7.2 um in diameter. This sampler technology is discussed in greater detail in Morton et al, 2013. Samples were filtered with acid-washed Whatman 41 (W41) cellulose fiber filters. Additional bulk dust samples were collected in October 2012, using a Thermo Partisol Plus 2025 using Teflon filters. Samples were fully digested using concentrated nitric and hydrofluoric acids, following the approach of Morton et al, 2013. Samples were analyzed using a Thermofisher iCAP inductively coupled plasma mass spectrometer (ICP-MS) in KED mode, with He as a collision cell gas, adapted from the approach of Trommetter et al (2020). Concentrations were determined from standard curves using a REE ICP-MS standard from High-Purity Standards (that also contained 232Th). Three internal standards (Ge, In, and Bi) were added to both samples and standards, to correct for short-term variability in the instrument response and to evaluate stability of mass response during the ICP-MS run. Concentration estimates for the REE and 232Th were blank-corrected using full-process blanks that included filters deployed during times when there was no known dust deposition. Most of the full-process blank concentrations were 100 times or more smaller than the concentrations of our lowest standard (with the exception of Ce, the concentration of which was ~seven times smaller than our lowest standard. This means that our blank concentrations were very low but also not quantified extremely accurately. Our best estimates are that the full-process blanks, including filters, ranged from 0.02 picograms per square centimeter (pg cm-2) for Eu, Tb, and Ho, to 2 pg cm-2 for Ce. These blank concentrations were in all cases 40 times or more smaller than our lowest REE sample concentration for the <0.49 um size fraction with the smallest amount of dust, and ~3 orders of magnitude smaller than the signal of the largest samples. The REE data are also presented in a double-normalized format that first normalizes to concentrations of Post Archean Australian Shale and then normalizes to the mean REE concentration. The normalization approach is slightly modified from that of Serno et al, 2014.