The Dust Attenuation Law in Galaxies
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The Dust Attenuation Law in Galaxies. / Salim, Samir; Narayanan, Desika.
Annual Reviews. Vol. 58 CA, USA, 2020. p. 529-575 (Annual Review of Astronomy and Astrophysics, Vol. 58).Research output: Chapter in Book/Report/Conference proceeding › Book chapter › Research › peer-review
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TY - CHAP
T1 - The Dust Attenuation Law in Galaxies
AU - Salim, Samir
AU - Narayanan, Desika
PY - 2020/7/14
Y1 - 2020/7/14
N2 - Understanding the properties of dust attenuation curves in galaxies and the physical mechanisms that shape them are among the fundamental questions of extragalactic astrophysics, with great practical significance for deriving the physical properties of galaxies. Attenuation curves result from a combination of dust grain properties, dust content, and the spatial arrangement of dust and different populations of stars. In this review, we assess the state of the field, paying particular attention to extinction curves as the building blocks of attenuation laws. We introduce a quantitative framework to characterize extinction and attenuation curves, present a theoretical foundation for interpreting empirical results, overview an array of observational methods, and review observational results at low and high redshifts. Our main conclusions include the following:Attenuation curves exhibit a wide range of UV-through-optical slopes, from curves with shallow (Milky Way-like) slopes to those exceeding the slope of the Small Magellanic Cloud extinction curve.The slopes of the curves correlate strongly with the effective optical opacities, in the sense that galaxies with lower dust column density (lower visual attenuation) tend to have steeper slopes, whereas the galaxies with higher dust column density have shallower (grayer) slopes.Galaxies exhibit a range of 2175- Alpha UV bump strengths, including no bump, but, on average, are suppressed compared with the average MilkyWay extinction curve.Theoretical studies indicate that both the correlation between the slope and the dust column as well as variations in bump strength may result from geometric and radiative transfer effects.
AB - Understanding the properties of dust attenuation curves in galaxies and the physical mechanisms that shape them are among the fundamental questions of extragalactic astrophysics, with great practical significance for deriving the physical properties of galaxies. Attenuation curves result from a combination of dust grain properties, dust content, and the spatial arrangement of dust and different populations of stars. In this review, we assess the state of the field, paying particular attention to extinction curves as the building blocks of attenuation laws. We introduce a quantitative framework to characterize extinction and attenuation curves, present a theoretical foundation for interpreting empirical results, overview an array of observational methods, and review observational results at low and high redshifts. Our main conclusions include the following:Attenuation curves exhibit a wide range of UV-through-optical slopes, from curves with shallow (Milky Way-like) slopes to those exceeding the slope of the Small Magellanic Cloud extinction curve.The slopes of the curves correlate strongly with the effective optical opacities, in the sense that galaxies with lower dust column density (lower visual attenuation) tend to have steeper slopes, whereas the galaxies with higher dust column density have shallower (grayer) slopes.Galaxies exhibit a range of 2175- Alpha UV bump strengths, including no bump, but, on average, are suppressed compared with the average MilkyWay extinction curve.Theoretical studies indicate that both the correlation between the slope and the dust column as well as variations in bump strength may result from geometric and radiative transfer effects.
KW - ISM
KW - dust
KW - extinction
KW - simulations
KW - SED fitting
KW - galaxy evolution
KW - STAR-FORMING GALAXIES
KW - SPECTRAL ENERGY-DISTRIBUTIONS
KW - GRAIN-SIZE DISTRIBUTION
KW - LARGE-MAGELLANIC-CLOUD
KW - AROMATIC-HYDROCARBON EMISSION
KW - ULTRAVIOLET EXTINCTION CURVES
KW - ACTIVE GALACTIC NUCLEI
KW - IRX-BETA RELATION
KW - 1ST BILLION YEARS
KW - INTERSTELLAR DUST
U2 - 10.1146/annurev-astro-032620-021933
DO - 10.1146/annurev-astro-032620-021933
M3 - Book chapter
VL - 58
T3 - Annual Review of Astronomy and Astrophysics
SP - 529
EP - 575
BT - Annual Reviews
CY - CA, USA
ER -
ID: 253030027