The Canada‐UK Deep Submillimeter Survey: First Submillimeter Images, the Source Counts, and Resolution of the Background

Eales, Stephen Anthony; Lilly, S. J.; Gear, Walter Kieran; Dunne, L.; Bond, J. R.; Hammer, F.; Fèvre, O. Le; Crampton, D.

doi:10.1086/307069

Cited by 363 publications

(419 citation statements)

References 27 publications

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“…The fraction of cold galaxies can contribute to the number counts up to 50% at 170 μm. At moderate and high redshift, the possible importance of cold, luminous galaxies has also been pointed out by Eales et al (1999) and Chapman et al (2002). We use the fluxes ratio f 24 μm / f 70 μm (corresponding to the highest wavelengths in our sample) to estimate the dust temperature.…”

Section: Discussionmentioning

confidence: 85%

Population synthesis modelling of luminous infrared galaxies at intermediate redshift

Giovannoli

Buat

Noll

et al. 2010

A&A

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Context. Luminous InfraRed Galaxies (LIRGs) are particularly important for studying the build-up of the stellar mass from z = 1 to z = 0, and for determining physical properties of these objects at redshift 0.7. LIRGs are now identified as playing a major role in galaxy evolution from z = 1 to 0. The global star formation rate (SFR) at z ∼ 0.7 is mainly produced by LIRGs. Aims. We perform a multiwavelength study of an LIRGs sample in the Extended Chandra Deep Field South at z = 0.7, selected at 24 μm by MIPS onboard Spitzer Space Telescope and detected in 17 filters. Data go from the near-ultraviolet to the mid-infrared. This multiwavelength dataset allows us to place strong constraints on the spectral energy distributions (SEDs) of galaxies, and thus to efficiently derive physical parameters such as the SFR, the total infrared luminosity, attenuation parameters, and star formation history. We distinguish a subsample of galaxies detected at 70 μm, which we compare to the rest of the sample to investigate the relative importance of this wavelength in determining of the physical parameters. An important part of this work is elaboration of a mock catalogue that allows us to have a reliability criterion for the derived parameters. Methods. We studied LIRGs by means of the SED-fitting code CIGALE. At first, this code creates synthetic spectra from the Maraston stellar population models. The stellar population spectra are attenuated by using a synthetic Calzetti-based attenuation law before adding the dust emission as given by the infrared SED library. The originality of CIGALE is that it allows us to perform consistent fits of the dust-affected ultaviolet-to-infrared wavelength range. This technique appears to be a very powerful tool in the case where we can have access to a dataset that is well-sampled over a wide range of wavelengths. Results. We are able to derive a star formation history and to estimate the fraction of infrared luminosity reprocessed by an active galactic nucleus. We study the dust temperatures of our galaxies detected at 70 μm and find them colder than predicted by models. We also study the relation between the SFR and the stellar mass and do not find a tight correlation between either of them, but instead a flat distribution and a large scatter, which is interpreted in terms of variations in star formation history.

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Section: Discussionmentioning

confidence: 85%

Population synthesis modelling of luminous infrared galaxies at intermediate redshift

Giovannoli

Buat

Noll

et al. 2010

A&A

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“…The current model ties the dust temperature of a source to its luminosity as observed locally for the IRAS 1.2 Jy sample galaxies, whereby a galaxy with a FIR luminosity of 10 12 L has T d ¼ 35 K and dust emissivity ¼ 1:6, as described in Dale & Helou (2002). In addition, the 60=100 m color distribution observed locally is adopted in the FIR luminosity function, resulting in a tail of cold, luminous galaxies, which are preferentially selected with SCUBA at 850 m (e.g., Blain et al 1999b;Eales et al 1999;Chapman et al 2003a). As expected (see also the discussion in C02), the best-fitting peak evolution redshift must be lower if a population of luminous colder sources exists at high redshifts.…”

Section: Fittinggthe Multiwavv Elengg Th Counts and Backgg Roundsmentioning

confidence: 99%

Modeling the Evolution of Infrared Luminous Galaxies: The Influence of the Luminosity‐Temperature Distribution

Lewis

Chapman

Hélou

2005

ApJ

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The evolution of the luminous infrared galaxy population is explored using a pure luminosity evolution model that incorporates the locally observed luminosity-temperature distribution for IRAS galaxies. Pure luminosity evolution models in a fixed ÃCDM cosmology are fitted to submillimeter and infrared counts and backgrounds. We find that the differences between the locally determined bivariate model and the single-variable luminosity function ( LF) do not manifest themselves in the observed counts but rather are primarily apparent in the dust temperatures of sources in flux-limited surveys. Statistically significant differences in the redshift distributions are also observed. The bivariate model is used to predict the counts, redshifts, and temperature distributions of galaxies detectable by the Spitzer Space Telescope. The best-fitting model is compared to the high-redshift submillimeter galaxy population, revealing a median redshift for the total submillimeter population of z ¼ 1:8 þ0:9 À0:4 , in good agreement with recent spectroscopic studies of submillimeter galaxies. The temperature distribution for the submillimeter galaxies is modeled to predict the radio/submillimeter indices of the submillimeter galaxies, revealing that submillimeter galaxies exhibit a broader spread in spectral energy distributions than seen in the local IRAS galaxies.

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“…Following their detection in the first deep submm and mm surveys (e.g., Smail et al 1997;Hughes et al 1998;Eales et al 1999;Bertoldi et al 2000), much has been learned about the dusty high-redshift sources selected at such wavelengths. Although many studies have argued that these sources are likely ancestors of local ellipticals (e.g., Scott et al 2002;Dunne et al 2003) little progress in verifying this assertion has been made since.…”

Section: Introductionmentioning

confidence: 99%

Herschel-ATLAS: Evolution of the 250 µm luminosity function out to z=0.5

Dye

Dunne

Eales

et al. 2010

A&A

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We have determined the luminosity function of 250 μm-selected galaxies detected in the ∼14 deg 2 science demonstration region of the Herschel-ATLAS project out to a redshift of z = 0.5. Our findings very clearly show that the luminosity function evolves steadily out to this redshift. By selecting a sub-group of sources within a fixed luminosity interval where incompleteness effects are minimal, we have measured a smooth increase in the comoving 250 μm luminosity density out to z = 0.2 where it is 3.6 +1.4 −0.9 times higher than the local value.

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The Canada‐UK Deep Submillimeter Survey: First Submillimeter Images, the Source Counts, and Resolution of the Background

Cited by 363 publications

References 27 publications

Population synthesis modelling of luminous infrared galaxies at intermediate redshift

Population synthesis modelling of luminous infrared galaxies at intermediate redshift

Modeling the Evolution of Infrared Luminous Galaxies: The Influence of the Luminosity‐Temperature Distribution

Herschel-ATLAS: Evolution of the 250 µm luminosity function out to z=0.5

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