Spectral Energy Distributions of Dusty Galaxies

Takagi, Toshinobu; Vansevičius, Vladas; Arimoto, N.

doi:10.1093/pasj/55.2.385

Cited by 56 publications

(75 citation statements)

References 104 publications

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“…When discussing these models, it's important to keep in mind that the accuracy or applicability of these models cannot be tested with data since it simply does not exist in enough detail to disentangle effects of geometry, distribution, optical depth, etc. It's also important to note that many have done work in this area, particularly modeling radiative transfer in local starburst populations to generate SEDs (Efstathiou & Rowan-Robinson, 1995;Efstathiou et al, 2000;Efstathiou & Siebenmorgen, 2009;Nenkova et al, 2002;Dullemond & van Bemmel, 2005;Piovan et al, 2006;Nenkova et al, 2008;Takagi et al, 2003;Fritz et al, 2006;Hönig et al, 2006;Schartmann et al, 2008), but here we try to focus on the techniques which have been most commonly employed for SED fitting of high-z dusty starbursts 11 . Silva et al (1998) developed the Grasil code to model galaxy emission by explicitly accounting for dust absorption and emission from the ultraviolet through to the far-infrared.…”

Section: Employing Dust Radiative Transfer Models and Empirical Templmentioning

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: Employing Dust Radiative Transfer Models and Empirical Templmentioning

confidence: 99%

Dusty star-forming galaxies at high redshift

2014

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“…Such studies play a crucial role in constructing and verifying IR galaxy evolution models (e.g., Granato et al 2000;Franceschini et al 2001;Takeuchi et al 2001a,b;Takagi et al 2003).…”

Section: Introductionmentioning

confidence: 99%

Mid-infrared luminosity as an indicator of the total infrared luminosity of galaxies

Takeuchi

Buat

Iglésias-Páramo

et al. 2005

A&A

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Abstract. The infrared (IR) emission plays a crucial role in understanding the star formation in galaxies hidden by dust. We first examined four estimators of the IR luminosity of galaxies, L FIR (Helou et al. 1988 (Sanders & Mirabel 1996) by using the observed SEDs of wellknown galaxies. We found that L IR provides excellent estimates of the total IR luminosity for a variety of galaxy SEDs. The performance of L TIR2 was also found to be very good. Using L IR , we then statistically analyzed the IRAS PSCz galaxy sample (Saunders et al. 2000) and found useful formulae relating the MIR monochromatic luminosities [L(12 µm) and L(25 µm)] and L IR . For this purpose we constructed a subsample of 1420 galaxies with all four IRAS band (12, 25, 60, and 100 µm) flux densities. We found linear relations between L IR and MIR luminosities, L(12 µm) and L(25 µm). The prediction error with a 95% confidence level is a factor of 4-5. Hence, these formulae are useful for the estimation of the total IR luminosity only from 12 µm or 25 µm observations. We further tried to make an "interpolation" formula for galaxies at 0 < z < 1. For this purpose we construct the formula of the relation between 15-µm luminosity and the total IR luminosity. We conclude that the 15-µm formula can be used as an estimator of the total IR luminosity from 24 µm observation of galaxies at z 0.6.

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“…Even if the duration of this obscured period is short, because SNe explosions and stellar-wind energy injection sweep away the gas soon after the onset of star formation, its effect on the light emitted by these young stars cannot be neglected. Excluding old ellipticals, in which star formation stopped at relatively early epochs, for all morphological types the impact of young dusty populations on the galaxy SED has to be considered (see Takagi et al 2003;Piovan et al 2006a;Siebenmorgen & Krügel 2007, for more details about young SEDs); (ii) low-and intermediate-mass stars in the asymptotic giant branch (AGB) phase may form an outer dust-rich shell of material obscuring and reprocessing the radiation emitted by the star underneath (see Bressan et al 1998;Piovan et al 2003;Marigo et al 2008, for the relation between dusty shells around AGB stars and SSPs); (iii) finally, because of the contribution of metal-rich material by supernovae and stellar winds, the ISM acquires over the years a dust-rich diffuse component capable of absorbing/re-emitting radiation (see . It has been successfully employed to reproduce the SEDs of the active central regions of star-forming galaxies from the UV to the far-IR by varying some basic parameters.…”

Section: Theory Versus Observations: a Possible Interpretationmentioning

confidence: 99%

GALEXUV properties of the polar ring galaxy MCG-05-07-001 and the shell galaxies NGC 1210 and NGC 5329

Marino

Iodice²,

Tantalo

et al. 2009

A&A

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Context. Systems of shells and polar rings in early-type galaxies are considered "bona fide" tracers of mass accretion and/or mergers. Their high frequency in low density environments suggests that these processes could drive the evolution of at least a fraction of the early-type galaxy population. Aims. We investigate the star formation histories of this type of galaxies. Their UV emission is important for testing whether these galaxies host ongoing or recent star formation and how this formation varies across the galaxy. Methods. We used far-and near-ultraviolet, optical, near-infrared images, neutral hydrogen HI maps, and line-strength indices to investigate the nuclear and outer regions of these galaxies as well as the regions where fine structures are present. Results. The GALEX near UV (NUV) and far UV (FUV) images of MCG-05-07-001 and NGC 1210 show complex tidal tails and debris structures. The far UV morphology of both galaxies appears so different from the optical morphology that the early-type classification may not apply. In both GALEX bands, the polar ring of MCG-05-07-001 is the dominant feature, whereas an extended tidal tail dominates the FUV bands of NGC 1210. In MCG-05-07-001 and NGC 1210, there is a strong correlation between structures detected in the FUV and NUV bands and in HI. In contrast, NGC 5329 does not show evidence of shells in the GALEX bands. We try to constrain the age of the accretion episode or merger that produced the shells and polar rings with the aid of composite stellar populations that take the presence of dust into account. The presence of HI in both MCG-05-07-001 and NGC 1210 argues in favour of wet mergers. Models suggest the presence of very young stellar populations in MCG-05-07-001: the observations could be explained in the framework of a conspicuous burst of star formation that occurred ≤1 Gyr ago and involved a large fraction of the galaxy mass. Our models suggest that also the nuclei of NGC 1210 and NGC 5329 could have been rejuvenated by an accretion episode about 2-4 Gyr ago.

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Spectral Energy Distributions of Dusty Galaxies

Cited by 56 publications

References 104 publications

Dusty star-forming galaxies at high redshift

Dusty star-forming galaxies at high redshift

Mid-infrared luminosity as an indicator of the total infrared luminosity of galaxies

GALEXUV properties of the polar ring galaxy MCG-05-07-001 and the shell galaxies NGC 1210 and NGC 5329

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