Dust in Starburst Galaxies

Gordon, K. D.; Calzetti, Daniela; Witt, A. N.

doi:10.1086/304654

Cited by 219 publications

(355 citation statements)

References 54 publications

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“…However, we also For comparison, the Calzetti law is also indicated by a dotted green line. It has been shown that the Calzetti law is the result of the attenuation by a medium with an SMC-type dust (Gordon et al 1997;Inoue 2005). We can recover this result using Eq.…”

Section: Attenuation Curvessupporting

confidence: 53%

The extinction law at high redshift and its implications

Gallerani

Maiolino

Juárez

et al. 2010

A&A

152

171

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We analyze the optical-near infrared spectra of 33 quasars with redshifts 3.9 ≤ z ≤ 6.4 to investigate the properties of dust extinction at these cosmic epochs. The SMC extinction curve has been shown to reproduce the dust reddening of most quasars at z < 2.2; we investigate whether this curve also provides a good description of dust extinction at higher redshifts. We fit the observed spectra with synthetic absorbed quasar templates obtained by varying the intrinsic slope (α λ ), the absolute extinction (A 3000 ), and by using a grid of empirical and theoretical extinction curves. We find that seven quasars in our sample are affected by substantial extinction (A 3000 ≥ 0.8), and characterized by very steep intrinsic slopes (α λ ≤ −2.3). All of the individual quasars require extinction curve deviating from that of the SMC, with a tendency to flatten at λ ≤ 2000 Å (in the rest frame of the source). However, due to the uncertainties in the individual extinction curves the SMC is still (marginally) consistent with the data in most cases. We obtain a mean extinction curve at z > 4, both by performing a simultaneous fit of all quasars and by averaging the extinction curves inferred for individual quasars. In the case of broad absorption line quasars (which are generally more absorbed by dust and possibly in a younger evolutionary stage), the mean extinction curve deviates from the SMC at a confidence level ≥95%. The difference between extinction curves in quasars at z > 4 and in quasars at lower redshift is indicative of either a different dust production mechanism at high redshift, or a different mechanism for processing dust into the ISM. We suggest that the same transitions may also apply to normal, star-forming galaxies at z > 4. In particular, the observed change in the average spectral slope of galaxies at z > 4 may be partially ascribed to a variation in the extinction curve, rather than a lower dust content at high redshift. In this scenario, the extinction curve inferred at z > 4 would imply a cosmic star-formation corrected for dust attenuation a factor of ∼2 higher than estimated in the past.

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Section: Attenuation Curvessupporting

confidence: 53%

The extinction law at high redshift and its implications

Gallerani

Maiolino

Juárez

et al. 2010

A&A

152

171

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“…This clumpy geometry is also chosen since it has been shown to reproduce both the observable continuum properties of starburst galaxies and the Calzetti attenuation law (Gordon et al 1997;Witt & Gordon 2000;Vijh et al 2003). Finally, this also allows us to make a detailed investigation into the continuity of the extensive grid of radiation transfer models by Schaerer et al (2011).…”

Section: D Geometries Model Parameters and Model Outputmentioning

confidence: 99%

Lymanαline and continuum radiative transfer in a clumpy interstellar medium

Duval

Schaerer

Östlin

et al. 2014

A&A

108

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Aims. Studying the effects of an inhomogeneous interstellar medium (ISM) on the strength and the shape of the Lyman alpha (Lyα) line in starburst galaxies. Methods. Using our 3D Monte Carlo Lyα radiation transfer code, we study the radiative transfer of Lyα, UV and optical continuum photons in homogeneous and clumpy shells of neutral hydrogen and dust surrounding a central source. Our simulations predict the Lyα and continuum escape fraction, the Lyα equivalent width EW(Lyα), and the Lyα line profile, and their dependence on the geometry of the gas distribution and the main input physical parameters. Results. The ISM clumpiness is found to have a strong impact on the Lyα line radiative transfer, entailing a strong dependence of the emergent features of the Lyα line (escape fraction, EW(Lyα)) on the ISM morphology. Although a clumpy and dusty ISM appears more transparent to radiation (both line and continuum) compared to an equivalent homogeneous ISM of equal dust optical depth, we find that the Lyα photons are, in general, still more attenuated than UV continuum radiation. As a consequence, the observed equivalent width of the Lyα line (EW obs (Lyα)) is lower than the intrinsic one (EWint(Lyα)) for nearly all clumpy ISM configurations considered. There are, however, special conditions under which Lyα photons escape more easily than the continuum, resulting in an enhanced EW obs (Lyα). The requirement for this to happen is that the ISM is almost static (galactic outflows ≤ 200 km s −1 ), extremely clumpy (with density contrasts > 10 7 in HI between clumps and the interclump medium), and very dusty (E(B-V) > 0.30). When these conditions are fulfilled the emergent Lyα line profile generally shows no velocity shift and little asymmetry. Otherwise the Lyα line profile is very similar to that expected for homogeneous media. Conclusions. Given the asymmetry and velocity shifts generally observed in star-forming galaxies with Lyα emission, we therefore conclude that clumping is unlikely to significantly enhance their relative Lyα/UV transmission.

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“…We consider these possibilities in Paper II. Mathis et al 1977 andWhite 1979. b Values from Gordon et al 1997.…”

Section: Ultraviolet Faintnessmentioning

confidence: 99%

“…Finally, the scattering geometry is constrained by a wealth of observations. Interstellar polarization and reddening (e.g., Breger 1986Breger , 1987, atomic and molecular line absorption (Federman 1982;Bohlin et al 1983;White 1984;White et al 2001), radio line emission (Gordon & Arny 1984;Federman & Wilson 1984;Bally & White 1986), and far-infrared (FIR) thermal emission (Castelaz, Sellgren, & Werner 1987;White & Bally 1993) indicate a low level of interstellar matter across most of the cluster but more on the western side, perhaps with some optically thick dust southwest of the star 23 Tau (Merope). Enough material is probably in front of the major stars to dominate the scattered light budget for forward-scattering grains, but some of the densest gas and dust may lie behind or among the stars on the west side of the cluster.…”

Section: Introductionmentioning

confidence: 99%

The Pleiades Reflection Nebula. I. Ultraviolet, Optical, and Far‐Infrared Imaging Photometry

Gibson

Nordsieck²

2003

ApJ

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We present new wide-field optical and ultraviolet images of the Pleiades reflection nebula that allow a more thorough evaluation of the dust scattering than any prior data set. Vacuum-UV images were taken at 1650 and 2200 Å during the first flight of the Wide-Field Imaging Survey Polarimeter (WISP), a sounding rocketborne telescope. WISP captured the brighter parts of the nebula at both wavelengths, with 3 sensitivities of 22.5 and 23.4 UV mag arcsec À2 , respectively. The 5=0 Â 1=7 WISP field was also mapped at 4400 Å with a mosaic of 40 Burrell Schmidt CCD frames using a broadband B J filter. The Schmidt mosaic shows extensive and intricate nebulosity down to a 5 sensitivity limit of 27.6 B mag arcsec À2 , including features undetected by photographic surveys. We explore the intensity and color behavior of the nebula in our UV and optical images and far-infrared IRAS data. We find that the photometric structure near bright stars is more complex than previous studies have implied, but general trends are still apparent. The color gradients around the stars are caused by phase function effects rather than internal reddening. The greater concentration of scattered light versus thermal emission indicates that most of the observed scattering is from foreground dust. A somewhat greater concentration of UV versus optical light suggests grain scattering is more forward-directed at shorter wavelengths. The UV nebula is much fainter than expected from the stellar photometry and interstellar reddening. Explaining this UV faintness requires either more reddening than is measured or significant alterations to current dust property estimates.

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Dust in Starburst Galaxies

Cited by 219 publications

References 54 publications

The extinction law at high redshift and its implications

The extinction law at high redshift and its implications

Lymanαline and continuum radiative transfer in a clumpy interstellar medium

The Pleiades Reflection Nebula. I. Ultraviolet, Optical, and Far‐Infrared Imaging Photometry

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