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| Draine & Lee | |
|---|---|
| Name | Draine & Lee |
| Fields | Astrophysics; Interstellar medium; Dust physics |
| Notable works | "Optical properties of interstellar graphite and silicate grains" |
| Institutions | Princeton University; Harvard University; University of Chicago |
Draine & Lee
Draine & Lee are the eponymous authors of a seminal 1984 paper on interstellar dust whose models influenced studies at Harvard University, Princeton University, University of Chicago, California Institute of Technology, Massachusetts Institute of Technology and observatories such as Palomar Observatory, Kitt Peak National Observatory, Mount Wilson Observatory, European Southern Observatory and Arecibo Observatory. Their work entered the canon alongside contributions from researchers affiliated with NASA, ESA, National Science Foundation, Institute for Advanced Study and was cited in contexts involving instruments like the Hubble Space Telescope, Spitzer Space Telescope, Infrared Astronomical Satellite, Very Large Array and Submillimeter Array.
The Draine & Lee model emerged from collaborations among scientists in the environments of Princeton University, Harvard University, University of Chicago, University of Cambridge, University of Oxford, Columbia University, Yale University, Cornell University, University of California, Berkeley, California Institute of Technology and research centers including Bell Labs, Los Alamos National Laboratory, Lawrence Berkeley National Laboratory, Argonne National Laboratory and Jet Propulsion Laboratory. Influences included prior work by researchers at Max Planck Institute for Astronomy, Institut d'Astrophysique de Paris, Royal Observatory, Greenwich, Royal Astronomical Society, Society of Photo-Optical Instrumentation Engineers and scholars connected to the National Academy of Sciences, Royal Society, American Astronomical Society and American Physical Society. Historical context invoked studies of interstellar extinction from groups led by figures associated with Cambridge Observatory, Lick Observatory, Green Bank Observatory and projects like the Palomar Sky Survey and the Two Micron All-Sky Survey.
The model characterized optical constants for grain materials drawing on laboratory and theoretical traditions from Bell Labs, Brookhaven National Laboratory, Argonne National Laboratory and universities such as MIT, Stanford University, University of Illinois Urbana-Champaign, University of Michigan, University of Colorado Boulder and Northwestern University. It specified size distributions and compositions including graphite and silicate components consonant with results from groups at University of Arizona, Rice University, University of Minnesota, Pennsylvania State University, University of Maryland, University of Toronto, McGill University, University of British Columbia and Australian National University. The treatment paralleled dielectric and Mie-scattering computations used in literature from Max Planck Society, Royal Institute of Technology (KTH), ETH Zurich, Technical University of Munich and Seoul National University, and interfaced with observational extinction curves measured by teams at Mount Stromlo Observatory, Anglo-Australian Observatory, South African Astronomical Observatory and Cerro Tololo Inter-American Observatory.
Their calculations used Mie theory and effective medium approximations similar to methods employed by researchers at Los Alamos National Laboratory, Princeton Plasma Physics Laboratory, Sandia National Laboratories, Rutherford Appleton Laboratory, CERN, Fermi National Accelerator Laboratory and computing resources typified by IBM and Cray Research. The computational pipeline echoed algorithms developed at Bell Labs Research, AT&T Bell Laboratories, RAND Corporation, University of California, Santa Cruz, University of Pennsylvania, University of Texas at Austin and University of Washington. Cross-disciplinary techniques linked to spectroscopy and materials studies at National Institute of Standards and Technology, Materials Research Laboratory (MRL), Fraunhofer Society and Tokyo Institute of Technology.
Key outputs included tabulated absorption and scattering efficiencies that influenced analyses at Space Telescope Science Institute, Max Planck Institute for Astrophysics, Institute of Astronomy, Cambridge, Harvard-Smithsonian Center for Astrophysics, Kavli Institute for Cosmology, University of California, Santa Cruz, University of California, Los Angeles, University of Edinburgh and University of Sydney. The model underpinned extinction-correction methods used in research on Milky Way structure, Local Group, Andromeda Galaxy, Small Magellanic Cloud, Large Magellanic Cloud and star-forming regions like Orion Nebula, Taurus Molecular Cloud, Perseus Molecular Cloud, Eagle Nebula and Horsehead Nebula. Its influence extended to cosmological and galactic studies by teams at European Southern Observatory, Space Science Institute, Canadian Space Agency, Australian Space Agency, Indian Space Research Organisation and collaborations with CERN astrophysics groups.
Observational assessments used data from facilities such as Hubble Space Telescope, Spitzer, James Webb Space Telescope, Chandra X-ray Observatory, XMM-Newton, GALEX, WISE, Planck (spacecraft), IRAS and ground arrays like Atacama Large Millimeter Array, Very Large Array, Keck Observatory, Subaru Telescope, Gemini Observatory and Gran Telescopio Canarias. Applications appeared in studies of interstellar polarization by teams at Max Planck Institute for Radio Astronomy, Instituto de Astrofísica de Canarias, National Astronomical Observatory of Japan, Korea Astronomy and Space Science Institute and groups linked to the SETI Institute. The model informed observational pipelines and surveys including the Sloan Digital Sky Survey, Dark Energy Survey, Gaia mission, Large Synoptic Survey Telescope (Vera C. Rubin Observatory), Pan-STARRS and the Herschel Space Observatory.
Later refinements and alternatives were proposed by investigators at University of Arizona, University of Massachusetts Amherst, University of Heidelberg, Max Planck Institute for Astronomy, Cardiff University, Leiden University, University of Copenhagen, Nanjing University, Peking University, Tsinghua University, University of Tokyo, Kyoto University, Osaka University, Space Research Institute (IKI), Istituto Nazionale di Astrofisica, Observatoire de Paris and other institutions. Successor models incorporated PAHs, composite grains, porous aggregates and updated optical constants influenced by laboratories at Argonne, Brookhaven, NIST, SLAC National Accelerator Laboratory and industrial partners including DuPont and 3M. These revisions were integrated into analysis tools developed by teams at Astropy Project, NASA Exoplanet Science Institute, European Space Agency Science and community software from IPAC and various university research groups.