Dust Grain-Size Distributions and Extinction in the Milky Way, Large Magellanic Cloud, and Small Magellanic Cloud

By J. Weingartner, B. Draine. 2001

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In Astronomy and Astrophysics

Citations in the corpus

Physical Processes in the Interstellar Medium (2014, methodology): “A more recent treatment by Weingartner & Draine (2001b) gives similar values for for small ψ, but predicts a more rapid fall-off in and Γpe with increasing ψ for ψ > 104.”
Mid-Infrared Spectra of Classical AGNs Observed with the Spitzer Space Telescope (2005, background): “This apparent emission begins to rise at ∼ 7.5µm , which is where the silicate opacity spectra of Weingartner and Draine (2001) and Li and Draine (2001) predict silicate emission should first appear, and which is consistent with the observed beginning of the silicate emission profile in the two…”
RESOLVED IMAGES OF LARGE CAVITIES IN PROTOPLANETARY TRANSITION DISKS (2011, methodology): “For the sake of homogeneity, we assume dust grains with mineral abundances as in the interstellar medium (ISM) (see Weingartner & Draine 2001), despite some evidence in individual cases for different compositions.”
A general model for the CO–H2 conversion factor in galaxies with applications to the star formation law (2011, methodology): “We use the Weingartner & Draine (2001) dust grain model (with R = 3.15) as updated by Draine & Li (2007).”
Dust properties of protoplanetary disks in the Taurus-Auriga star forming region from millimeter wavelengths (2009, methodology): “…spherical grains made of astronomical silicates, carbonaceous materials and water ice (optical constants for the individual components from Weingartner & Draine 2001, Zubko et al. 1996, Warren 1984 respectively) adopting fractional abundances used by Pollack et al. (1994) (see caption of…”
CRYSTALLINE SILICATES AND DUST PROCESSING IN THE PROTOPLANETARY DISKS OF THE TAURUS YOUNG CLUSTER (2007, methodology): “In these models, we include only small (radius 0.25 μm) dust grains with interstellar-like opacity (Weingartner & Draine 2001) in the upper disk layers, taken to be that above a tenth of the local gas-pressure scale height.”
TRANSITIONAL DISKS AS SIGNPOSTS OF YOUNG, MULTIPLANET SYSTEMS (2011, methodology): “We use a standard Milky Way dust composition of 20% carbon and 80% small (sub-µm) circumstellar silicates (Weingartner & Draine 2001; Li & Draine 2001; Draine et al. 2007).”
Cool outflows in galaxies and their implications (2020, background): “The dust scattering cross-section and its phase function (angular dependence) may be decomposed into two functions (Weingartner and Draine 2001; Draine 2003): ( dσs”
Forming the cores of giant planets from the radial pebble flux in protoplanetary discs (2014, background): “ISM grains are predominantly about 0.1−1 µm in size (Weingartner & Draine 2001), which would result in ξ ≈ 10.”
Evidence for a Population of High-Redshift Submillimeter Galaxies from Interferometric Imaging (2007, background): “For redshifts of z ∼> 3, assuming the Weingartner & Draine (2001) Milky Way dust opacity, dust temperature Td = 45 − 70 K, and a flat ΛCDM cosmology, we find that the observed 345 GHz (rest–frame > 1380 GHz) flux of our objects (F890µm ≈ 10 mJy) implies dust masses of order 0.6 − 3 × 109 M⊙ at the…”
HERSCHEL FAR-INFRARED AND SUBMILLIMETER PHOTOMETRY FOR THE KINGFISH SAMPLE OF NEARBY GALAXIES (2011, methodology): “Draine & Li (2007) use the size distributions of Weingartner & Draine (2001) for dust in the diffuse Milky Way, except for adjustment of the parameters that characterize the PAH size distribution.”
H$_2$ formation on interstellar dust grains: the viewpoints of theory, experiments, models and observations (2017, background): “is responsible for the observed power-law size-distribution in the diffuse ISM (Jones et al., 1996; Weingartner and Draine, 2001; Clayton et al., 2003).”
Dust Masses, PAH Abundances, and Starlight Intensities in the SINGS Galaxy Sample (2007, background): “The ionized fraction i(NC) (a function of the number NC of carbon atoms in the PAH) will depend primarily on the ratio U ffiffiffiffiffi Te p /ne, where ne and Te are the electron density and temperature (Bakes & Tielens 1994; Weingartner & Draine 2001b).”
PROTOPLANETARY DISK STRUCTURES IN OPHIUCHUS (2009, methodology): “Opacities for this grain population were computed with a Mie scattering code, assuming the silicate and graphite abundances determined for dust grains in the interstellar medium by Draine & Lee (1984) and their updated optical properties as calculated by Weingartner & Draine (2001).”
INTERSTELLAR DUST GRAINS (2003, methodology): “The extinction and scattering cross sections per H nucleon, calculated for the Weingartner & Draine (2001a) grain model, are shown in Figs.”
INTERSTELLAR EXTINCTION LAW TOWARD THE GALACTIC CENTER III: J, H, KS BANDS IN THE 2MASS AND THE MKO SYSTEMS, AND 3.6, 4.5, 5.8, 8.0 μm IN THE SPITZER/IRAC SYSTEM (2009, background): “…shows positive deviation from the power law as the wavelength increases to > 3 μm as we see above, and (2) a number of dust grain models (e.g., Weingartner & Draine 2001; Dwek 2004; Voshchinnikov et al. 2006) predict such positive deviation, it is possible that the power index changes in the…”
Dusty Star Forming Galaxies at High Redshift (2014, background): “…(PAHs) are a fewÅ-diameter heavymolecules containing hundreds of carbon atomswhich exist in coldmolecular clouds (Leger and Puget, 1984; Allamandola et al., 1985) andwhen irradiated by young stars, emit spectral line features at discrete wavelengths from ≈3–19 µm (Weingartner and Draine, 2001).”
Planck 2013 results. XI. All-sky model of thermal dust emission (2013, background): “Second, the grain size A11, page 5 of 37 A11, page 6 of 37 distribution (Mathis et al. 1977; Weingartner & Draine 2001) is important; exposed to the same ISRF, bigger grains have a lower equilibrium temperature than smaller ones.”