Dust in the Galactic Environment

By D. Whittet. 2018

498 citations recorded by the source corpus.

Dust in the Galaxy: Our view from within. Abundances and depletions. Extinction and scattering. Polarization and grain alignment. Infrared absorption features. Continuum and line emission. Dust in stellar ejecta. Evolution of dust in the interstellar medium. The early phases of stellar evolution. Towards a unified model for interstellar dust. Appendices. References. Index.

Subfields: Astronomy and Astrophysics

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In Astronomy and Astrophysics

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Citations in the corpus

• Dust formation in early galaxies (2003, methodology): “It is generally accepted that dust is formed in the atmospheres of evolved stars and ejected via stellar winds with mass loss rates of up to 10−6M⊙yr −1 (Gehrz 1989; Whittet 1992) and contribute up to 0.3M⊙ of dust to the ISM in our Galaxy per year (Bode 1988).”
• The chemistry of multiply deuterated species in cold, dense interstellar cores (2004, background): “ISM: abundances – ISM: molecules – ISM: individual objects: ρ Oph D, L1544”
• Interstellar Extinction and Polarization in the Taurus Dark Clouds: The Optical Properties of Dust near the Diffuse/Dense Cloud Interface (2001, background): “5 in some regions of active star formation such as M42 (e.g., Whittet 1992 and references therein).”
• The SCUBA Local Universe Galaxy Survey — I. First measurements of the submillimetre luminosity and dust mass functions (2000, background): “Suggested sites of formation range from post-AGB stars to supernova remnants (Whittet 1992).”
• Infrared to millimetre photometry of ultra-luminous ir galaxies: new evidence favouring a 3-stage dust model (2001, methodology): “Thereby the following standard conversions are used: 0.1 M ·pc−2 ⇔ τV = 0.4 U. Klaas et al.: Ultra-luminous IR galaxies 835 (Whittet 1992), and τ100 µm = 0.006 · τV (Mathis et al. 1983).”
• SCUBA observations of galaxies with metallicity measurements: a new method for determining the relation between submillimetre luminosity and dust mass (2002, methodology): “The fraction of metals incorporated in dust in the interstellar medium can be estimated from UV spectroscopic observations of nearby stars, which show that a significant fraction of the metals that one would expect, from cosmic abun- dances, to be in the ISM are not there - they have been bound up i”
• The Spitzer/GLIMPSE Surveys: A New View of the Milky Way (2009, background): “By modeling the spectral energy distributions of the stars seen toward these clouds, it is possible to estimate their optical depths from which masses can be inferred (Whittet 1992), providing an important independent check on radio determinations.”
• Models for Interstellar Extinction in the Galaxy (2005, background): “A similar equation holds for E(B V ); the ratio between total and selective extinction is taken to be 3.05 (Whittet 1992).”