A Quantitative Comparison of the Small Magellanic Cloud, Large Magellanic Cloud, and Milky Way Ultraviolet to Near-Infrared Extinction Curves

By K. Gordon, G. Clayton, K. Misselt, A. Landolt, Michael J. Wolff. 2003

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In Astronomy and Astrophysics

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SURVEYING THE AGENTS OF GALAXY EVOLUTION IN THE TIDALLY STRIPPED, LOW METALLICITY SMALL MAGELLANIC CLOUD (SAGE-SMC). I. OVERVIEW (2011, background): “In addition, the SMC is the only local galaxy which has the ultraviolet dust characteristics (lack of 2175 Å extinction bump, Gordon et al. 2003) of starburst galaxies in the local (Calzetti et al. 1994; Gordon et al. 1997) and high-redshift (2 < z < 4, Vijh et al. 2003) universe.”
THE MOSDEF SURVEY: MEASUREMENTS OF BALMER DECREMENTS AND THE DUST ATTENUATION CURVE AT REDSHIFTS z ∼ 1.4–2.6 (2015, background): “…and nearby galaxies have yielded detailed information on the shape of the dust extinction and attenuation curves, respectively, in the local Universe (e.g., Prevot et al. 1984; Cardelli et al. 1989; Pei 1992; Calzetti et al. 1994, 2000; Gordon et al. 2003; Johnson et al. 2007a; Wild et al. 2011).”
Empirical determination of the shape of dust attenuation curves in star-forming galaxies (2011, methodology): “We adopt the tabulated LMC and SMC-bar curves of Gordon et al. (2003), spline interpolating onto our wavelength points.”
Optical Star Formation Rate Indicators (2005, neutral): “Other reddening curves in this wavelength regime (e.g., for the Small Magellanic Cloud; Gordon et al. 2003) are very similar to the two curves plotted.”
Recovering galaxy star formation and metallicity histories from spectra using VESPA (2007, methodology): “Both methods make similar assumptions regarding stellar models, but MOPED uses a Large Magellanic Cloud (Gordon et al. 2003) dust extinction curve, and single screen modelling for all optical depths.”
Dust Attenuation Curves in the Local Universe: Demographics and New Laws for Star-forming Galaxies and High-redshift Analogs (2018, background): “…Small Magellanic Clouds (LMC and SMC) (Nandy et al. 1975, 1980; Rocca-Volmerange et al. 1981), from which the average total extinction curves currently in use for these galaxies have been derived (e.g., Seaton 1979; Cardelli et al. 1989; Fitzpatrick 1986; Prevot et al. 1984; Gordon et al. 2003).”
Non-standard grain properties, dark gas reservoir, and extended submillimeter excess, probed by Herschel in the Large Magellanic Cloud (2011, result): “Moreover, a significant excess of large grains would flatten the UV rise of the extinction curve, contradicting the observations of several lines of sight within the LMC (Gordon et al., 2003).”
PHYSICAL PROPERTIES AND GALACTIC DISTRIBUTION OF MOLECULAR CLOUDS IDENTIFIED IN THE GALACTIC RING SURVEY (2010, methodology): “…is therefore: Γpe = 4.86× 10−26G0(Rgal)e−5.4AV nH [ergs cm−3s−1] (16) In this equation, we assumed that CO was present for AV > 1 (Wolfire et al. 2010), and used the standard Milky Way extinction curve to relate A1000, the FUV extinction at 1000 Å, and AV (A1000 = 4-5 AV , see Gordon et al. 2003).”
The history of star-forming galaxies in the Sloan Digital Sky Survey (2007, methodology): “…attenuation, we have selected 1000 galaxies at random from the SFhq sample and fitted them with four other functions: the starburst attenuation law of Calzetti, Kinney & Storchi-Bergmann (1994), the SMC and LMC curves from Gordon et al. (2003) and the λ−0.7 law used by Kauffmann et al. (2003a).”
The GALEX Ultraviolet Atlas of Nearby Galaxies (2006, methodology): “Studies on the dust attenuation in galaxies based on either photometric or spectroscopic UV studies are numerous, including Calzetti et al. (1994), Heckman et al. (1995),Meurer et al. (1995, 1999), Buat&Xu (1996), Gordon et al. (2000, 2003), Buat et al. (2002), and Roussel et al. (2005).”
Re-evaluating old stellar populations (2018, methodology): “The Milky Way extinction law of Fitzpatrick (1999), modified in the near-infrared by Indebetouw et al. (2005) is shown in black, and that of Gordon et al. (2003) for the Large Magellanic Cloud in grey.”
PRIMUS: CONSTRAINTS ON STAR FORMATION QUENCHING AND GALAXY MERGING, AND THE EVOLUTION OF THE STELLAR MASS FUNCTION FROM z = 0–1 (2013, background): “The currently supported possibilities are the Calzetti et al. (2000) starburst galaxy attenuation curve, the Charlot & Fall (2000) attenuation law, the O’Donnell (1994) Milky Way extinction curve, the extinction curve of the Small Magellanic Cloud (Gordon et al. 2003), or no attenuation.”
The Behavior of the Aromatic Features in M101 H II Regions: Evidence for Dust Processing (2008, background): “…Cloud (Gordon & Clayton 1998), Large Magellanic Cloud (Misselt et al. 1999), and Milky Way (Clayton et al. 2000; Valencic et al. 2003) paint a consistent picture where the 2175 Å bump is depressed and the overall UV extinction increased in regions near massive star formation (Gordon et al. 2003).”
ON THE SOURCE OF THE DUST EXTINCTION IN TYPE Ia SUPERNOVAE AND THE DISCOVERY OF ANOMALOUSLY STRONG Na i ABSORPTION (2013, methodology): “When only color excesses are provided by these authors, visual extinctions were computed using the average RV values given by Gordon et al. (2003).”
The SEDs and host galaxies of the dustiest GRB afterglows (2011, background): “…the differences in extinction properties along different sight-lines through the diffuse ISM to giant molecular clouds in the Local Group (e.g., Gordon et al. 2003; Fitzpatrick 2004), and the geometrical differences between a single sight-line and an extended distribution of star-light and…”
The Magellanic Clouds Photomtric Survey: The Small Magellanic Cloud Stellar Catalog and Extinction Map (2001, methodology): “We adopt a standard Galactic extinction curve (Schild 1977), which is acceptable for the LMC over the optical wavelength region (see Gordon et al. (2003)).”
STRONG NEBULAR LINE RATIOS IN THE SPECTRA of z ∼ 2–3 STAR FORMING GALAXIES: FIRST RESULTS FROM KBSS-MOSFIRE (2014, background): “…E(B − V)cont to estimate the attenuation of the Hα emission line in magnitudes, A(Hα) = 2.52×2.27 E(B − V)cont = 5.72×E(B − V)cont (4) assuming Galactic extinction, or A(Hα) = 2.00×2.27 E(B − V)cont = 4.54×E(B − V)cont (5) for SMC extinction (Gordon et al. 2003) applied to the nebular emission.”
Analysis of galaxy spectral energy distributions from far-UV to far-IR with CIGALE: studying a SINGS test sample (2009, background): “Moreover, the typical width of the UV bump of these galaxies is only about 60% of those measured for characteristic Milky Way and LMC sightlines.”