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12 results for “Extinction curves”
Dust extinction curves: Ferrara (1999) original resolution
<p>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>.</p> <p><strong>Dust Properties</strong></p> <p>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.</p> <p> </p> <p><strong>Stellar Geometry</strong></p> <p>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, <em>r</em><sub>s</sub>, while <a href="http://adsabs.harvard.edu/abs/1999ApJS..123..437F">Ferrara et al. (1999)</a> listed the corresponding effective radius, <em>r</em><sub>e</sub>=<em>r</em><sub>s</sub>/1.16.</p> <p><strong>Dust Geometry</strong></p> <p>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, <em>h</em><sub>z</sub>, of the stellar disk scale height. The value of <em>h</em><sub>z</sub> is encoded in each file name.</p>
Dust extinction curves: KMH94 R_V=5.5 model
<p>This dataset is based on the models described in <a href="https://ui.adsabs.harvard.edu/abs/2018RNAAS...2..188B">Benson (2018)</a>.</p> <p><strong>Dust Properties</strong></p> <p>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 R<sub>V</sub>=3.1 and a full scattering calculation.</p> <p><strong>Stellar Geometry</strong></p> <p>Galactic disks follow exponential profiles in the radial direction, and sech<sup>2</sup> distributions in the vertical direction. The vertical scale height is set to a multiple, <em>h</em><sub>d</sub>, 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.</p> <p><strong>Dust Geometry</strong></p> <p>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, <em>h</em><sub>z</sub>, of the stellar disk scale length, and its value is encoded in each file name.</p>
Dust extinction curves: KMH94 HG R_V=5.5 model
<p>This dataset is based on the models described in <a href="https://ui.adsabs.harvard.edu/abs/2018RNAAS...2..188B">Benson (2018)</a>.</p> <p><strong>Dust Properties</strong></p> <p>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 R<sub>V</sub>=3.1 and Henyey-Greenstein scattering.</p> <p><strong>Stellar Geometry</strong></p> <p>Galactic disks follow exponential profiles in the radial direction, and sech<sup>2</sup> distributions in the vertical direction. The vertical scale height is set to a multiple, <em>h</em><sub>d</sub>, 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.</p> <p><strong>Dust Geometry</strong></p> <p>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, <em>h</em><sub>z</sub>, of the stellar disk scale length, and its value is encoded in each file name.</p>
Dust extinction curves: Grasil-like
<p>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>.</p> <p><strong>Dust Properties</strong></p> <p>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 R<sub>V</sub>=3.1 or R<sub>V</sub>=5.5 as encoded in the file name with prefix dustD03.</p> <p><strong>Stellar Geometry</strong></p> <p>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, <em>r</em><sub>s</sub>, while <a href="http://adsabs.harvard.edu/abs/1999ApJS..123..437F">Ferrara et al. (1999)</a> listed the corresponding effective radius, <em>r</em><sub>e</sub>=<em>r</em><sub>s</sub>/1.16.</p> <p><strong>Dust Geometry</strong></p> <p>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, <em>h</em><sub>z</sub>, of the stellar disk scale height. The value of <em>h</em><sub>z</sub> is encoded in each file name with prefix hzDust.</p>
Dust extinction curves: Draine R_V=5.5 model
<p>This dataset is based on the models described in <a href="https://ui.adsabs.harvard.edu/abs/2018RNAAS...2..188B">Benson (2018)</a>.</p> <p><strong>Dust Properties</strong></p> <p>Dust grain properties are taken from <a href="http://adsabs.harvard.edu/abs/2003ARA%26A..41..241D">Draine (2003)</a> - specifically their model with R<sub>V</sub>=5.5.</p> <p><strong>Stellar Geometry</strong></p> <p>Galactic disks follow exponential profiles in the radial direction, and sech<sup>2</sup> distributions in the vertical direction. The vertical scale height is set to a multiple, <em>h</em><sub>d</sub>, 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.</p> <p><strong>Dust Geometry</strong></p> <p>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, <em>h</em><sub>z</sub>, of the stellar disk scale length, and its value is encoded in each file name.</p>
Dust extinction curves: Draine R_V=3.1 model
<p>This dataset is based on the models described in <a href="https://ui.adsabs.harvard.edu/abs/2018RNAAS...2..188B">Benson (2018)</a>.</p> <p><strong>Dust Properties</strong></p> <p>Dust grain properties are taken from <a href="http://adsabs.harvard.edu/abs/2003ARA%26A..41..241D">Draine (2003)</a> - specifically their model with R<sub>V</sub>=3.1.</p> <p><strong>Stellar Geometry</strong></p> <p>Galactic disks follow exponential profiles in the radial direction, and sech<sup>2</sup> distributions in the vertical direction. The vertical scale height is set to a multiple, <em>h</em><sub>d</sub>, 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.</p> <p><strong>Dust Geometry</strong></p> <p>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, <em>h</em><sub>z</sub>, of the stellar disk scale length, and its value is encoded in each file name.</p> <p> </p>
Dust extinction curves: Draine R_V=4.0 model
<p>This dataset is based on the models described in <a href="https://ui.adsabs.harvard.edu/abs/2018RNAAS...2..188B">Benson (2018)</a>.</p> <p><strong>Dust Properties</strong></p> <p>Dust grain properties are taken from <a href="http://adsabs.harvard.edu/abs/2003ARA%26A..41..241D">Draine (2003)</a> - specifically their model with R<sub>V</sub>=4.0.</p> <p><strong>Stellar Geometry</strong></p> <p>Galactic disks follow exponential profiles in the radial direction, and sech<sup>2</sup> distributions in the vertical direction. The vertical scale height is set to a multiple, <em>h</em><sub>d</sub>, 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.</p> <p><strong>Dust Geometry</strong></p> <p>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, <em>h</em><sub>z</sub>, of the stellar disk scale length, and its value is encoded in each file name.</p>
Dust extinction curves: Ferrara (1999) high resolution
<p>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>.</p> <p><strong>Dust Properties</strong></p> <p>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.</p> <p> </p> <p><strong>Stellar Geometry</strong></p> <p>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, <em>r</em><sub>s</sub>, while <a href="http://adsabs.harvard.edu/abs/1999ApJS..123..437F">Ferrara et al. (1999)</a> listed the corresponding effective radius, <em>r</em><sub>e</sub>=<em>r</em><sub>s</sub>/1.16.</p> <p><strong>Dust Geometry</strong></p> <p>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, <em>h</em><sub>z</sub>, of the stellar disk scale height. The value of <em>h</em><sub>z</sub> is encoded in each file name.</p>
A compendium of extinction curves for simple galactic geometries
<p>This is a tabulation of dust extinction curves for simple galactic geometries computed using the Hyperion radiative transfer package. Full details of the calculations and the file structure can be found <a href="https://drive.google.com/open?id=1iJomvqPjdcI9pjlpnovtx4_GpGGMVZB9">here</a>.</p>
Unveiling the Milky Way dust extinction curve in 3D
<p>We measure the extinction curves of 220 million stars with Gaia XP spectra and near-infrared photometry from 2MASS and WISE. We use a data-driven model that is developed from <a href="https://ui.adsabs.harvard.edu/abs/2023MNRAS.524.1855Z/abstract">Zhang et al. 2023</a>, with variable extinction curves, to determine stellar parameters and extinction curves simultaneously. For full details of our method, see our corresponding paper*.</p> <p>Here, we provide the resulting catalog of stellar parameters, our trained stellar model, and a few Python scripts that demonstrate how to interact with the catalog and model.</p> <p>See the <code>README.md</code> for more information.</p> <p>* Link of the paper will be posted here once available.</p> <p>Update on 05.04.2024: Uploaded the reference table <code>xi_Rv_ext_curve.h5</code>, which was missing. Updated the script <code>plot_ext_curve.py</code> for a larger range of R(V) .</p> <p>Update on 17.05.2024: Uploaded preliminary maps in <code>Rv_map_new.h5</code>; Uploaded the script <code>example_query.py</code> for examples of querying the map, as well as code for generating sky-view and birds'-eye view pictures. </p>
SpeX NIR spectra and extinction curves
<p><strong>SpeX near-infrared spectra and measured extinction curves for a sample of Milky Way sightlines.</strong></p> <ul> <li><em>SpeX_spectra.zip</em> contains the SpeX near-infrared spectra of 15 comparison and 25 reddened O/B type Milky Way stars, that were used to measure extinction curves.</li> <li><em>Data_files.zip</em> contains the data files of the stars in the format required by the code.</li> <li><em>Ext_curves.zip</em> contains 15 measured extinction curves and the measured average diffuse Milky Way extinction curve.</li> </ul> <p>See our paper Decleir et al. (ApJ, submitted) for a detailed discussion of our method and results.</p> <p>See the associated <a href="https://github.com/mdecleir/spex_nir_extinction/tree/v1.0.0">spex_nir_extinction GitHub repository</a> (<a href="https://zenodo.org/record/5806703#.YdYhrS-cY2I">Decleir et al. 2021</a>) for the code, Tables and Figures.</p> <p>This version (2.0) is an update from the first version (1.0), and is associated with the revised version of the paper. Changes include:</p> <ul> <li>updated uncertainties for R(V) in the headers of the extinction curve fits files.</li> <li>addition of 1/R(V) in the headers of the extinction curve fits files.</li> <li>addition of comments in the data files about the references and quality of the photometry </li> </ul>
Data for "The Dust Extinction Curve: Beyond R(V)"
<p>24 million dust extinction curves, detemined from Gaia XP spectra, as described in <a href="https://ui.adsabs.harvard.edu/abs/2024arXiv241022537G/abstract">Green, Zhang & Zhang (2025)</a>.</p> <p>We represent the extinction curves using a set of 16 basis vectors. For each star, there are 16 coefficients, which can be used to reconstruct the extinction curves. After loading <code>A_zp</code> and <code>G_subspace</code> from the file <code>G_subspace.json</code>, and <code>coeffs</code> from the file <code>coeffs.h5</code>, the extinction curves can be reconstructed using:</p> <p> <code>A = A_zp + np.sum(coeffs[None,:] * G_subspace[:,:], axis=1)</code></p> <p>The output <code>A</code> will have shape (star, wavelength). The wavelengths at which <code>A</code> is sampled are stored in the field <code>wavelengths_nm</code> (in nanometers), in <code>G_subspace.json</code>.</p> <p>The covariance matrix of the coefficients for each star is stored in the files <code>coeffs_cov_?.h5</code>. We store the diagonals and the upper triangles of the covariances separately. They can be reconstructed using the function <code>reconstruct_symm_matrices</code> from <code>symm_matrix_utils.py</code>:</p> <p> <code>from symm_matrix_utils.py import reconstruct_symm_matrices</code><br> <code>cov = reconstruct_symm_matrices(cov_diag, cov_triu_wo_diag)</code></p> <p>Additionally, we store the inverse covariance matrices in the files <code>coeffs_icov_?.h5</code>, in the same manner as the covariance matrices.</p> <p>The file <code>source_info.h5</code> contains a few useful Gaia fields and parameter estimates (with corresponding uncertainties) from <a href="https://ui.adsabs.harvard.edu/abs/2024arXiv240714594Z/abstract">Zhang & Green (2025)</a>.</p> <p>The file <code>feature_EW.h5</code> contains the equivalent widths (in nanometers) of the VBS and the 770 and 850 nm extinction features.</p> <p>Every file contains the Gaia DR3 <code>source_id</code> of every star, labeled <code>gdr3_source_id</code>.</p>
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