Dust Absorption and the Cosmic Ultraviolet Flux Density

Massarotti, M.; Iovino, A.; Buzzoni, A.

doi:10.1086/323787

Cited by 29 publications

(40 citation statements)

References 28 publications

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“…All the UV data reported in the figure are not extinction-corrected, with the only exception of the three points measured by Massarotti et al (2001). Our predictions indicate a peak in the total UV LD corresponding to the redshift of galaxy formation and a monotonically decreasing trend down to z ¼ 0, with a particularly strong evolution between z ¼ 1 and 0.…”

Section: Evolution Of the Galaxy Luminosity Densitymentioning

confidence: 74%

“…The UV luminosity density is dominated by the light emitted by young and massive stars; thus it provides an estimate of the cosmic SFR density. Relevant observations of galaxies in the UV are typically performed at 1500 Å (Madau et al 1996(Madau et al , 1998bSteidel et al 1999;Massarotti, Iovino, & Buzzoni 2001Å (Treyer et al 1998, and 2800 Å (Lilly et al 1996;Sawicki et al 1997;Connolly et al 1997;Cowie et al 1999). Other ways to assess star formation include observations of nebular emission lines such as H (Gallego et al 1995;Gronwall 1998;Tresse & Maddox 1998;Glazebrook et al 1999) and O ii (Hammer et al 1997).…”

Section: Observed Star Formation Rate Densitymentioning

confidence: 99%

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The Cosmic Evolution of the Galaxy Luminosity Density

Calura

Matteuccí

2003

ApJ

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We reconstruct the history of the cosmic star formation in the universe by means of detailed chemical evolution models for galaxies of different morphological types. We consider a picture of coeval noninteracting evolving galaxies in which elliptical galaxies experience intense and rapid starbursts within the first gigayears after their formation and spiral and irregular galaxies continue to form stars at lower rates up to the present time. Such models allow one to follow in detail the evolution of the metallicity of the gas from which the stars are formed. We normalize the galaxy population to the B-band luminosity function observed in the local universe and study the redshift evolution of the luminosity densities in the B, U, I, and K bands, calculating galaxy colors and evolutionary corrections by means of a detailed synthetic stellar population model. Our predictions indicate that the decline of the galaxy luminosity density between redshift 1 and 0 observed in the U, B, and I bands is caused mainly by star-forming spiral galaxies that slowly exhaust their gas reservoirs. Elliptical galaxies have dominated the total luminosity density in all optical bands at early epochs, when all their stars formed by means of rapid and very intense starbursts. Irregular galaxies bring a negligible contribution to the total luminosity density in any band at any time. We study the cosmic missingmetal crisis and conclude that it could be even more serious than what has been assessed by previous authors, if the bulk of the metals were produced in dust-obscured starbursts associated with the early spheroid formation. The most plausible site for the missing metals could be the warm gas in galaxy groups and protoclusters, in which the metals could have been ejected through galactic winds following intense starbursts. Finally, we predict the evolution of the cosmic star formation and supernova II and Ia rates and obtain the best fit to the observations, assuming a Salpeter initial mass function. All our results indicate that the bulk of the stellar mass in most galaxies were already in place at early epochs, and we predict a peak in the global star formation rate at high redshift because of elliptical galaxies.

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Section: Evolution Of the Galaxy Luminosity Densitymentioning

confidence: 74%

Section: Observed Star Formation Rate Densitymentioning

confidence: 99%

The Cosmic Evolution of the Galaxy Luminosity Density

Calura

Matteuccí

2003

ApJ

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“…The presence of dust in starburst galaxies at high redshift has been confirmed by analyzing galaxy colors with the SED fitting method (see Massarotti et al 2001b, and references therein). Meurer et al (1999) adopted an entirely empirical approach based on the correlation between color reddening, dust absorption and far infrared flux for local starburst galaxies (supposed to be also valid at high redshifts).…”

Section: Comparison Between Z Spec and Z Photmentioning

confidence: 94%

New insights on the accuracy of photometric redshift measurements

Massarotti

Iovino²,

Buzzoni³

et al. 2001

A&A

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Abstract. We use the deepest and most complete redshift catalog currently available (the Hubble Deep Field (HDF) North supplemented by new HDF South redshift data) to minimize residuals between photometric and spectroscopic redshift estimates. The good agreement at zspec < 1.5 shows that model libraries provide a good description of the galaxy population. At zspec ≥ 2.0, the systematic shift between photometric and spectroscopic redshifts decreases when the modeling of the absorption by the interstellar and intergalactic media is refined. As a result, in the entire redshift range z ∈ [0, 6], residuals between photometric and spectroscopic redshifts are roughly halved. For objects fainter than the spectroscopic limit, the main source of uncertainty in photometric redshifts is related to photometric errors, and can be assessed with Monte Carlo simulations.

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“…small f and large ) (e.g. Heckman et al 1998;Meurer et al 1999;Massarotti et al 2001) or perhaps a small extinction (e.g. H01).…”

Section: Application To the Cosmic Sfhmentioning

confidence: 99%

Star formation rate in galaxies from UV, IR, and Hαestimators

Hirashita¹,

Buat²,

Inoue³

2003

A&A

157

193

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Abstract. Infrared (IR) luminosity of galaxies originating from dust thermal emission can be used as an indicator of the star formation rate (SFR). Inoue et al. (2000, IHK) have derived a formula for the conversion from dust IR luminosity to SFR by using the following three quantities: the fraction of Lyman continuum luminosity absorbed by gas ( f ), the fraction of UV luminosity absorbed by dust ( ), and the fraction of dust heating from old ( > ∼ 10 8 yr) stellar populations (η). We develop a method to estimate those three quantities based on the idea that the various way of SFR estimates from ultraviolet (UV) luminosity (2000 Å luminosity), Hα luminosity, and dust IR luminosity should return the same SFR. After applying our method to samples of galaxies, the following results are obtained in our framework. First, our method is applied to a sample of starforming galaxies, finding that f ∼ 0.6, ∼ 0.5, and η ∼ 0.4 as representative values. Next, we apply the method to a starburst sample, which shows larger extinction than the star-forming galaxy sample. With the aid of f , , and η, we are able to estimate reliable SFRs from UV and/or IR luminosities. Moreover, the Hα luminosity, if the Hα extinction is corrected by using the Balmer decrement, is suitable for a statistical analysis of SFR, because the same correction factor for the Lyman continuum extinction (i.e. 1/ f ) is applicable to both normal and starburst galaxies over all the range of SFR. The metallicity dependence of f and is also tested: Only the latter proves to have a correlation with metallicity. As an extension of our result, the local (z = 0) comoving density of SFR can be estimated with our dust extinction corrections. We show that all UV, Hα, and IR comoving luminosity densities at z = 0 give a consistent SFR per comoving volume (∼3 × 10 −2 h M yr −1 Mpc −3 ). Useful formulae for SFR estimate are listed.

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Dust Absorption and the Cosmic Ultraviolet Flux Density

Cited by 29 publications

References 28 publications

The Cosmic Evolution of the Galaxy Luminosity Density

The Cosmic Evolution of the Galaxy Luminosity Density

New insights on the accuracy of photometric redshift measurements

Star formation rate in galaxies from UV, IR, and Hαestimators

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