Dust extinction of the stellar continua in starburst galaxies: The ultraviolet and optical extinction law

Calzetti, Daniela; Kinney, A. L.; Storchi‐Bergmann, Thaisa

doi:10.1086/174346

Cited by 1,543 publications

(2,420 citation statements)

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“…The Code Investigating GALaxy Emission (Cigale) was developed from an algorithm described in Burgarella et al (2005) and formally presented in Noll et al (2009). Cigale is based on model spectra generated in the optical/near-infrared by Maraston (2005) which account for thermally pulsating asymptotic giant branch (TP-AGB) stars, synthetic dust attenuation curves based on the modified laws presented in Calzetti et al (1994) and Calzetti (2001) and far-infrared SED templates from Dale & Helou (2002). In contrast, the Multi-wavelength Analysis of Galaxy Physical Properties, or Magphys code, is a modeling package described in da which empirically constrains the output of an SED from the ultraviolet through far-infrared using an energy balance argument.…”

Section: Direct Fir-only Methodsmentioning

confidence: 99%

Dusty star-forming galaxies at high redshift

2014

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Far-infrared and submillimeter wavelength surveys have now established the important role of dusty, star-forming galaxies (DSFGs) in the assembly of stellar mass and the evolution of massive galaxies in the Universe. The brightest of these galaxies have infrared luminosities in excess of 10 13 L with implied star-formation rates of thousands of solar masses per year. They represent the most intense starbursts in the Universe, yet many are completely optically obscured. Their easy detection at submm wavelengths is due to dust heated by ultraviolet radiation of newly forming stars. When summed up, all of the dusty, star-forming galaxies in the Universe produce an infrared radiation field that has an equal energy density as the direct starlight emission from all galaxies visible at ultraviolet and optical wavelengths. The bulk of this infrared extragalactic background light emanates from galaxies as diverse as gas-rich disks to mergers of intense starbursting galaxies. Major advances in far-infrared instrumentation in recent years, both spacebased and ground-based, has led to the detection of nearly a million DSFGs, yet our understanding of the underlying astrophysics that govern the start and end of the dusty starburst phase is still in nascent stage. This review is aimed at summarizing the current status of DSFG studies, focusing especially on the detailed characterization of the bestunderstood subset (submillimeter galaxies, who were summarized in the last review of this field over a decade ago, Blain et al. 2002), but also the selection and characterization of more recently discovered DSFG populations. We review DSFG population statistics, their physical properties including dust, gas and stellar contents, their environments, and current theoretical models related to the formation and evolution of these galaxies.

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Section: Direct Fir-only Methodsmentioning

confidence: 99%

Dusty star-forming galaxies at high redshift

2014

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“…In particular, two age-sensitive diagnostics, the color-color diagram UV−V versus V−I and the equivalent width of Hα, were combined to constrain the most likely age for each stellar cluster and, assuming a Salpeter IMF, to assign a mass (Figure 1; , Harris et al 2004. Hα/Hβ Large-and small-scale feedback in the Starburst centers of galaxies 379 ratio maps were used to correct photometry and fluxes for the effects of dust reddening (Calzetti, Kinney & Storchi-Bergmann 1994). The cluster ages were then re-mapped onto the galaxy images to derive the history of the cluster formation in each starburst.…”

Section: Charting the Young Stellar Populations In Starburstsmentioning

confidence: 99%

Large– and small–scale feedback in the Starburst centers of galaxies

Calzetti

2004

Proc. IAU

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Abstract. The interplay between stellar populations and gas in local starburst galaxies is analyzed using images from the Hubble Space Telescope to map the ages of the young stellar components and to isolate the contribution of shocks on spatial scales ranging from a few tens of pc to ∼1 kpc. The shocked gas represents a small fraction of the total ionized gas in these objects, yet it can have profound effects on the long-term evolution of the starburst, which may include the triggering of new star formation.

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“…The starburst galaxies has been extracted from the sample of 39 objects of Calzetti et al (1994), 3 Seyfert galaxies have been excluded. Complementary data such as FIR, Hα fluxes and Balmer decrements come from Calzetti et al (1995) .…”

Section: The Iue Sample Of Starburst Galaxiesmentioning

confidence: 99%

“…The IUE sample: the fluxes are corrected for the Galactic extinction following Calzetti et al (1994). The UV fluxes are taken in the bin 1863-1963Å from Kinney et al (1993. Other data come from Calzetti et al (1994Calzetti et al ( , 1995. The galaxies are sorted according to their diameter.…”

Section: The Extinction In the Hα Emission Linementioning

confidence: 99%

Star Formation and Dust Extinction in Nearby Star Forming and Starburst Galaxies

Buat

Boselli²,

Gavazzi³

et al. 2002

The Evolution of Galaxies

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Abstract. We study the star formation rate and dust extinction properties of a sample of nearby star forming galaxies as derived from Hα and UV (∼ 2000Å) observations and we compare them to those of a sample of starburst galaxies. The dust extinction in Hα is estimated from the Balmer decrement and the extinction in UV using the FIR to UV flux ratio or the attenuation law for starburst galaxies of Calzetti et al. (2000). The Hα and UV emissions are strongly correlated with a very low scatter for the star forming objects and with a much higher scatter for the starburst galaxies. The Hα to UV flux ratio is found larger by a factor ∼ 2 for the starburst galaxies. We compare both samples with a purely UV selected sample of galaxies and we conclude that the mean Hα and UV properties of nearby star forming galaxies are more representative of UV selected galaxies than starburst galaxies. We emphasize that the Hα to UV flux ratio is strongly dependent on the dust extinction: the positive correlation found between FHα/FUV and FFIR/FUV vanishes when the Hα and UV flux are corrected for dust extinction. The Hα to UV flux ratios converted into star formation rate and combined with the Balmer decrement measurements are tentatively used to estimate the dust extinction in UV.

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Dust extinction of the stellar continua in starburst galaxies: The ultraviolet and optical extinction law

Cited by 1,543 publications

References 0 publications

Dusty star-forming galaxies at high redshift

Dusty star-forming galaxies at high redshift

Large– and small–scale feedback in the Starburst centers of galaxies

Star Formation and Dust Extinction in Nearby Star Forming and Starburst Galaxies

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