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| Bohlin, Dickinson, and Calzetti | |
|---|---|
| Name | Bohlin, Dickinson, and Calzetti |
| Occupation | Astronomers, Astrophysicists |
| Fields | astronomy, astrophysics, interstellar medium |
| Notable works | "Interstellar extinction curves", "UV attenuation laws" |
Bohlin, Dickinson, and Calzetti
Bohlin, Dickinson, and Calzetti are widely cited contributors whose combined work underpins modern understanding of ultraviolet and optical extinction and attenuation by dust in the Milky Way, Magellanic Clouds, and external galaxies such as those in the Hubble Deep Field. Their studies connect measurements from observatories like the International Ultraviolet Explorer, the Hubble Space Telescope, and the Galaxy Evolution Explorer to models used by researchers at institutions including the Space Telescope Science Institute and the Max Planck Institute for Astronomy.
The three researchers emerged from scientific milieus around flagship facilities and programs: one collaborator with the International Ultraviolet Explorer and the Copernicus era, one associated with calibration efforts at the Space Telescope Science Institute, and one active in multiwavelength surveys coordinated with the Sloan Digital Sky Survey and the Spitzer Space Telescope. Their networks include collaborations with leading figures and groups at Harvard–Smithsonian Center for Astrophysics, the European Southern Observatory, the National Radio Astronomy Observatory, and the California Institute of Technology. Coauthors and users of their results span investigators from the University of Cambridge, Princeton University, Massachusetts Institute of Technology, University of California, Berkeley, and the Max Planck Society, while data products informed analysis pipelines used by teams on the Keck Observatory, Very Large Telescope, and Atacama Large Millimeter/submillimeter Array.
Collectively, the trio produced foundational papers and empirical parametrizations used as reference standards across the astronomy literature. Their outputs are frequently cited alongside canonical resources from authors such as Cardelli, Clayton, and Mathis, Fitzpatrick, and Draine; their UV-to-optical attenuation law is implemented in synthesis codes maintained by groups at Yale University and Geneva Observatory. Major works have been incorporated in the calibration suites for the Hubble Space Telescope photometric systems and used to interpret spectra from instruments on Keck Observatory and the Very Large Telescope. Their models provide inputs to spectral energy distribution fitting tools developed at institutions like MPIA and University of Oxford, and are compared with reddening curves derived for systems observed by the Sloan Digital Sky Survey and the Hubble Ultra Deep Field.
Their methodology integrates ultraviolet spectrophotometry, optical photometry, and infrared constraints drawn from missions including IRAS, Spitzer Space Telescope, and Herschel Space Observatory. They employed standard stars calibrated through networks at the Landolt Standard Stars program and cross-checked results with spectrophotometric atlases used by the Space Telescope Science Institute. Data reduction pipelines referenced tools developed at CERN and analysis environments common at NASA Ames Research Center and Jet Propulsion Laboratory. Samples included sightlines in the Milky Way, regions in the Large Magellanic Cloud, the Small Magellanic Cloud, and galaxies cataloged in the Hubble Deep Field and the Great Observatories Origins Deep Survey. Statistical approaches brought their results into dialogue with Bayesian techniques used at Columbia University and frequentist analyses practiced by groups at University of Chicago.
The combined findings have shaped how researchers interpret reddening and attenuation across environments from local star-forming regions to high-redshift systems observed by Hubble Space Telescope programs and planned surveys with the James Webb Space Telescope. Their empirical attenuation law is routinely compared with theoretical dust models by Draine and with empirical curves from studies of the Magellanic Clouds and the Milky Way by teams at ESO and the Royal Astronomical Society. Observational campaigns at facilities like ALMA and VLA use their calibrations when estimating dust-corrected star formation rates, while cosmological surveys at Subaru Telescope and Keck Observatory incorporate their prescriptions into photometric redshift and stellar population modeling pipelines run at Stanford University and University College London.
Their prescriptions for ultraviolet attenuation and optical extinction underpin conversions from observed luminosity to intrinsic star formation indicators used in work by research groups at Caltech, Max Planck Institute for Astrophysics, University of Cambridge, and Princeton University. Studies of main-sequence star formation, mass–metallicity relations, and quenching processes in surveys such as the CANDELS program and the COSMOS survey apply their attenuation corrections when deriving stellar masses and specific star formation rates. Interpretations of rest-frame UV slopes for high-redshift galaxies discovered with the Hubble Space Telescope and anticipated with the James Webb Space Telescope depend on these laws, and they inform radiative transfer models developed at the Jet Propulsion Laboratory and the Leiden Observatory.
Authors and groups at University of Arizona, University of Toronto, University of Edinburgh, and ETH Zurich have noted limitations when applying a single attenuation curve across heterogeneous sightlines, prompting extensions that incorporate geometry, scattering, and grain composition variations explored by Draine, Zubko, and others. Subsequent work from teams at ESO, Max Planck Institute for Astronomy, Imperial College London, and University of California, Santa Cruz has developed spatially resolved attenuation maps and radiative transfer simulations that refine or replace simple prescriptions in regimes influenced by active galactic nuclei found in catalogs from Chandra X-ray Observatory and XMM-Newton. These developments have led to hybrid approaches used by consortia running the Euclid and Roman Space Telescope projects that combine empirical laws with model grids from the Padova and Bruzual & Charlot stellar population synthesis families.