Starburst and cirrus models for submillimeter galaxies

Efstathiou, A.; Siebenmorgen, R.

doi:10.1051/0004-6361/200811205

Cited by 59 publications

(67 citation statements)

References 67 publications

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“…The 850 µm flux density weighted mean of our sample of FeLoBALs is F s = 1.14 ± 0.58 mJy. By applying the Kennicutt SFR-L IR conversion (Kennicutt 1998) and assuming a variety of dust templates (Chary & Elbaz 2001;Efstathiou & Siebenmorgen 2009) this value corresponds to a SFR of ∼150-240 M yr −1 . This result suggests that FeLoBAL QSOs are forming new stars at similar rates of both BAL and non-BAL quasars (∼10 2 M yr −1 ; Cao Orjales et al 2012), and not at the prodigious rates typical of luminous starburst galaxies, such as SMGs, which are characterized by SFRs ≥ 500 M yr −1 (e.g.…”

Section: Discussionmentioning

confidence: 99%

“…Each template varies both in metallicity (Z = 0.08, 0.2 and 0.5) and stellar age (25 Myr, 100 Myr, 290 Myr, 640 Myr, 900 Myr, 1.4 Gyr, 2.5 Gyr, 5 Gyr, 6 Gyr, 12 Gyr). For the AGN and starburst components, we rely on a set of templates by Efstathiou & Rowan-Robinson (1999) and Efstathiou & Siebenmorgen (2009). AGN emission varies with viewing angle and the model assumes a smooth torus whose density and thickness are, respectively, inversely and directly proportional to the distance from the nucleus (the use of smooth torus models may represent a caveat since recent studies provided observational evidence in support of a clumpy morphology, e.g.…”

Section: Sed Fitsmentioning

confidence: 99%

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A SCUBA-2 survey of FeLoBAL QSOs. Are FeLoBALs in a ‘transition phase’ between ULIRGs and QSOs?

Violino¹,

Coppin²,

Stevens³

et al. 2016

Mon. Not. R. Astron. Soc.

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It is thought that a class of broad absorption line (BAL) QSOs, characterised by Fe absorption features in their UV spectra (called 'FeLoBALs'), could mark a transition stage between the end of an obscured starburst event and a youthful QSO beginning to shed its dust cocoon, where Fe has been injected into the interstellar medium by the starburst. To test this hypothesis we have undertaken deep SCUBA-2 850 µm observations of a sample of 17 FeLoBAL QSOs with 0.89 z 2.78 and -23.31 M B -28.50 to directly detect an excess in the thermal emission of the dust which would probe enhanced star-formation activity. We find that FeLoBALs are not luminous sources in the submillimetre, none of them are individually detected at 850 µm, nor as a population through stacking (F s = 1.14 ± 0.58 mJy). Statistical and survival analyses reveal that FeLoBALs have sub-mm properties consistent with BAL and non-BAL QSOs with matched redshifts and magnitudes. An SED fitting analysis shows that the FIR emission is dominated by AGN activity, and a starburst component is required only in 6/17 sources of our sample; moreover the integrated total luminosity of 16/17 sources is L 10 12 L , high enough to classify FeLoBALs as infrared luminous.In conclusion, we do not find any evidence in support of FeLoBAL QSOs being a transition population between a ULIRG and an unobscured QSO; in particular, FeLoBALs are not characterized by a cold starburst which would support this hypothesis.

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Section: Discussionmentioning

confidence: 99%

Section: Sed Fitsmentioning

confidence: 99%

A SCUBA-2 survey of FeLoBAL QSOs. Are FeLoBALs in a ‘transition phase’ between ULIRGs and QSOs?

Violino¹,

Coppin²,

Stevens³

et al. 2016

Mon. Not. R. Astron. Soc.

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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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“…Recently, De Looze et al (2014) extended the applicability of the "decoding technique" to the modelling of a resolved nearby face-on galaxy. Other approaches to the "decoding observed panchromatic SEDs" include the radiative transfer models of Rowan-Robinson & Crawford (1989), , Silva et al (1998), Efstathiou & Rowan-Robinson (2003), Rowan-Robinson et al (2005), Piovan et al (2006), Efstathiou & Siebenmorgen (2009) The second approach (called "encoding predicted physical quantities" by PT10) consists of the application of dust radiative transfer codes to galaxy models obtained through numerical simulations of galaxy formation and evolution. In contrast to the decoding approach, in this case the stellar and dust distributions are derived from first principles.…”

Section: Introductionmentioning

confidence: 99%

Predicting the stellar and non-equilibrium dust emission spectra of high-resolution simulated galaxies with dart-ray

Natale¹,

Popescu²,

Tuffs³

et al. 2015

Monthly Notices of the Royal Astronomical Society

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We describe the calculation of the stochastically heated dust emission using the 3D ray-tracing dust radiative transfer code DART-Ray, which is designed to solve the dust radiative transfer problem for galaxies with arbitrary geometries. In order to reduce the time required to derive the non-equilibrium dust emission spectra from each volume element within a model, we implemented an adaptive SED library approach, which we tested for the case of axisymmetric galaxy geometries. To show the capabilities of the code, we applied DART-Ray to a highresolution N-body+SPH galaxy simulation to predict the appearance of the simulated galaxy at a set of wavelengths from the UV to the sub-mm. We analyse the results to determine the effect of dust on the observed radial and vertical profiles of the stellar emission as well as on the attenuation and scattering of light from the constituent stellar populations. We also quantify the proportion of dust re-radiated stellar light powered by young and old stellar populations, both bolometrically and as a function of infrared wavelength.

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Starburst and cirrus models for submillimeter galaxies

Cited by 59 publications

References 67 publications

A SCUBA-2 survey of FeLoBAL QSOs. Are FeLoBALs in a ‘transition phase’ between ULIRGs and QSOs?

A SCUBA-2 survey of FeLoBAL QSOs. Are FeLoBALs in a ‘transition phase’ between ULIRGs and QSOs?

Dusty star-forming galaxies at high redshift

Predicting the stellar and non-equilibrium dust emission spectra of high-resolution simulated galaxies with dart-ray

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