Scattering Properties of Carbonaceous-Silicate Dust Mixtures

The results provided here are described by Draine (2003a), "Scattering by Interstellar Dust Grains. I. Optical and Ultraviolet" Ap.J. 598:1017-1025.
The grain size distributions are from Weingartner & Draine (2001), "Dust Grain Size Distributions and Extinction in the Milky Way, LMC, and SMC", Ap.J. 548:296-309

• Average Milky Way dust with R_V=3.1 and C/H = 56 ppm in PAHs.
  Scattering phase function:
  • 12 wavelengths from 8930 A to 1820 A
  • 12 wavelengths from 1700 A to 600 A
  • 12 wavelengths from 9000 A to 10.2 micron
  Polarization as a function of scattering angle:
  • 12 wavelengths from 8930 A to 1820 A
  • 12 wavelengths from 1700 A to 600 A
  • 12 wavelengths from 9000 A to 10.2 micron

• LMC average dust with R_V=2.6 and C/H = 20 ppm in PAHs.
  Scattering phase function:
  • 12 wavelengths from 8930 A to 1820 A
  • 12 wavelengths from 1700 A to 600 A
  • 12 wavelengths from 9000 A to 10.2 micron
  Polarization as a function of scattering angle:
  • 12 wavelengths from 8930 A to 1820 A
  • 12 wavelengths from 1700 A to 600 A
  • 12 wavelengths from 9000 A to 10.2 micron

• SMC Bar dust with R_V=2.87 and no PAHs:
  Scattering phase function:
  • 12 wavelengths from 8930 A to 1820 A
  • 12 wavelengths from 1700 A to 600 A
  • 12 wavelengths from 9000 A to 10.2 micron
  Polarization as a function of scattering angle:
  • 12 wavelengths from 8930 A to 1820 A
  • 12 wavelengths from 1700 A to 600 A
  • 12 wavelengths from 9000 A to 10.2 micron

If there are particular scattering properties that would be of interest to you but which are not provided here, send email to <draine@astro.princeton.edu>. The URL of this page is http://www.astro.princeton.edu/~draine/dust/scat.html

> Back to Interstellar Dust page.

> Back to Bruce Draine's home page