The Dust Opacity of Star‐forming Galaxies

By D. Calzetti. 2001

686 citations recorded by the source corpus.

The presence of dust in galaxies removes one‐half or more of the stellar energy from the UV‐optical budget of the universe and has a profound impact on our understanding of how galaxies evolve. Measures of opacity in local galaxies are reviewed together with widely used theoretical and empirical methods for quantifying its effects. Existing evidence shows that the dust content of nearby galaxies depends not only on their morphology but also on their luminosity and activity level. A digression is devoted to starbursts in view of their potential relevance for measures of opacity in distant galaxies. Scarcity of coherent multiwavelength data sets hampers our ability to derive reliable obscuration estimates in intermediate‐ and high‐redshift galaxies. This, in turn, limits the reliability of inferred physical quantities, such as star formation rates, stellar population ages, galaxy luminosity functions, and others.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/bf24cc86dd312bf268bb3e75ec4ddf61b5eb59f0

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Citations in the corpus

The shapes of galaxies in the Sloan Digital Sky Survey (2008, background): “…of interstellar medium (ISM) in galaxies, and the relationship between optical and infrared emission from galaxies (for reviews, see Davies & Burstein 1995 and Calzetti 2001), and studies of the brightness of galaxies as a function of axial ratio should allow the effects of dust to be quantified.”
CAIRNS: The Cluster and Infall Region Nearby Survey. I. Redshifts and Mass Profiles (2003, methodology): “If this assumption is incorrect (Calzetti 2001), then Balmer decrements are necessary to obtain accurate SFR estimates.”
Galaxy And Mass Assembly (GAMA): Spectroscopic analysis (2013, methodology): “A Calzetti (2001) obscuration curve is used in estimating theobscuration corrections to the stellar continuum, and is applied throughout the GANDALF measurement process.”
Dusty, Radiation Pressure-Dominated Photoionization. II. Multiwavelength Emission Line Diagnostics for Narrow-Line Regions (2004, methodology): “As for the previous section, the Calzetti (2001) curve is used for reddening correction.”
Modeling the Pan-Spectral Energy Distribution of Starburst Galaxies. IV. The Controlling Parameters of the Starburst SED (2007, background): “12 and which provides a close approximation to the empirically-derived Calzetti extinction law for starburst galaxies (Calzetti 2001).”
On the Normalization of the Cosmic Star Formation History (2006, background): “Dust obscuration corrections The issue of dust corrections is complex and has been addressed by many authors (e.g., Buat et al. 2005; Bell 2003b; Buat et al. 2002; Calzetti 2001).”
Modeling the Panchromatic Spectral Energy Distributions of Galaxies (2013, background): “…which differs from extinction in two important respects: (1) light can be scattered both out of and into a given line of sight; (2) the geometrical distribution of dust with respect to the stars strongly affects the resulting SED (see Calzetti 2001, for an extensive discussion of these issues).”
Dust Attenuation Curves in the Local Universe: Demographics and New Laws for Star-forming Galaxies and High-redshift Analogs (2018, background): “…addition to absorption and scattering out of the line of sight, the scattering into the line of sight and the effects of dust/star distribution and viewing orientation (the “geometry”; see review by Calzetti 2001, also Charlot & Fall 2000; Conroy et al. 2010; Conroy 2013; Chevallard et al. 2013).”
CALIBRATING EXTINCTION-FREE STAR FORMATION RATE DIAGNOSTICS WITH 33 GHz FREE–FREE EMISSION IN NGC 6946 (2011, result): “It is also worth noting that the derived coefficient for scaling the IR luminosity given above is larger than that from empirical studies of starburst galaxies which report a coefficient closer to ∼0.6 (e.g., Meurer et al. 1999; Calzetti 2001).”
On the Evolution of Star-forming Galaxies (2004, methodology): “For continuum measurements (primarily UV wavelengths from 1500 to 2800 8) the starburst obscuration curve from Calzetti et al. (2000) is used (see also Calzetti 2001).”
The Romulus cosmological simulations: a physical approach to the formation, dynamics and accretion models of SMBHs (2016, background): “We then make the assumption that the dust is uniformly distributed in a sheet around the stars, which allows us to relate the dust extinction by a simple function of the dust optical depth (Calzetti 2001).”
Lyα Emission-Line Galaxies at z = 3.1 in the Extended Chandra Deep Field-South (2007, methodology): “However, according to the Calzetti (2001) extinction law, the effect of dust on the emission-line flux of a galaxy is much greater than that on the stellar continuum.”
DUST-CORRECTED STAR FORMATION RATES OF GALAXIES. II. COMBINATIONS OF ULTRAVIOLET AND INFRARED TRACERS (2011, methodology): “The ANUV/AHα ratio defined by our data is 1.52±0.56, coincident with the predicted value from Calzetti (2001)’s law within the error.”
LINE DERIVED INFRARED EXTINCTION TOWARD THE GALACTIC CENTER (2011, background): “A similar effect of very inhomogeneously distributed extinction in the case of galaxy integrated measurements (mixed case) is visible in the top left panel of Figure 2 in Calzetti (2001).”
INTERSTELLAR DUST GRAINS (2003, background): “From observations of the overall emission spectrum Calzetti (2001) infers the internal extinction by dust in starburst galaxies.”
The STAGES view of red spirals and dusty red galaxies: Mass-dependent quenching of star formation in cluster infall (2008, background): “Hence, UV-based estimates capture 1/3 of the SF in blue galaxies, consistent with a large body of literature (see Calzetti 2001, and references therein), but only 1/7.”
Far-infrared spectral energy distribution fitting for galaxies near and far (2012, background): “Although this gives rise to many free parameters in the models, the slew of broadband filters in the optical and nearinfrared make this detailed SED fitting possible, even with the effects of dust obscuration/attenuation taken into account (e.g. Calzetti et al. 1994; Calzetti 2001).”