Optically Faint Counterparts to the<i>Infrared Space Observatory</i>FIRBACK 170 Micron Population: Discovery of Cold, Luminous Galaxies at High Redshift

Chapman, Scott; Smail, Ian; Ivison, R. J.; Hélou, G.; Dale, Daniel A.; Lagache, G.

doi:10.1086/340552

Cited by 65 publications

(98 citation statements)

References 34 publications

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“…Then it still has H − K s > 0.5, but K s − LW2 becomes lower, because the PAH features move out of (2MASS13371721+0904430 at z = 0.3) has a remarkably high F100/F60 (=5.5) indicating a large amount of cool dust despite the ultra-luminous IR emission. A similar cool ULIRG has been found at z = 0.45 by Chapman et al (2002) in the ISO-FIRBACK survey.…”

Section: Far-infrared Propertiessupporting

confidence: 76%

Polycyclic aromatic hydrocarbon selected galaxies

Haas

Leipski

Siebenmorgen

et al. 2009

A&A

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Context. This is the fourth in a series of papers based on the ISOCAM Parallel Survey at 6.7 μm. While the first three papers have been devoted to active galactic nuclei (AGN), here we report on emission-line galaxies without AGN signatures in their optical spectra. Aims. Polycyclic aromatic hydrocarbon (PAH) emission has been found in both starbursts and modestly starforming galaxies, but the relation between starforming activity and PAH luminosity is still a matter of debate. The different correlation degrees could be caused by the variety of optical and far-infrared sample selection criteria. In order to obtain a census of the typical properties of PAH emitting galaxies, we here study moderately distant galaxies which have been selected by their PAH emission. Methods. Combining the ISOCAM Parallel Survey at 6.7 μm with 2MASS we have colour-selected a sample of 120 candidates for strong PAH emission. We obtained optical and mid-infrared spectra of 75 and 19 sources, respectively, and analysed IRASADDSCANs and available Spitzer 3.6-160 μm photometry. Results. The Spitzer mid-infrared spectra exhibit clear PAH features and corroborate that our photometric selection criteria trace the PAH emission of galaxies fairly well. The optical spectra show emission lines, at median redshift z ∼ 0.1, as well as H δ and Ca II absorption, indicating ongoing starformation as well as post-starbursts. The mid-and far-infrared spectral energy distributions (SEDs) provide evidence for a broad range of far-infrared (FIR) luminosities (10 9 L −2 × 10 12 L ), but in general the dust is colder (T < ∼ 25 K, β = 2) than for starburst galaxies like M 82 (T ≈ 40 K). For most galaxies the monocromatic luminosity (ν · L ν ) peaks at about equal height at optical, 6.7 μm (PAH) and FIR wavelengths. In about 15% of the sources the FIR luminosity exceeds the optical and PAH energy output by about a factor 5-10 despite the cool dust temperature; in these galaxies a large dust mass of 10 8 -10 9 M is inferred. Conclusions. At moderate distance (z ∼ 0.1), PAH selected galaxies turn out to be a quite heterogeneous population of dust-rich, partly infrared-luminous galaxies but mostly cool with a range of post-starburst signatures and starforming activity which appears to be rather modest relative to the entire gas content (derived from the dust mass and assuming a standard gas/dust ratio). Our results on PAH selected galaxies question the often expressed interpretation that the majority of high redshift galaxies detected in 15 and 24 μm surveys are dominated by powerful ongoing starbursts with high starforming efficiency.

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Section: Far-infrared Propertiessupporting

confidence: 76%

Polycyclic aromatic hydrocarbon selected galaxies

Haas

Leipski

Siebenmorgen

et al. 2009

A&A

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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: 83%

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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“…A third possibility would be that the infrared SEDs of galaxies evolve as a function of redshift (see e.g. Chapman et al 2002).…”

Section: Counts Inversionmentioning

confidence: 99%

Cosmic star-formation history from a non-parametric inversion of infrared galaxy counts

Borgne

Elbaz²,

Ocvirk

2009

A&A

102

123

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Aims. This paper aims at providing new conservative constraints on the cosmic star-formation (SF) history from the empirical modeling of recent observations in the mid and far infrared. Methods. We present a new empirical method based on a non-parametric inversion technique. It primarily uses multi-wavelength galaxy counts in the infrared and sub-mm (15, 24, 70, 160, 850 μm), and it does not require any redshift information. This inversion can be considered as a "blind" search for all possible evolutions and shapes of the infrared luminosity function of galaxies, from which the evolution of the star-formation rate density (SFRD) and its uncertainties are derived. The cosmic infrared background (CIRB) measurements are used a posteriori to tighten the range of solutions. The inversion relies only on two hypotheses: (1) the luminosity function remains smooth both in redshift and luminosity; (2) a set of infrared spectral energy distributions (SEDs) of galaxies must be assumed, with a dependency on the total luminosity alone. Results. The range of SF histories recovered at low redshift is well-constrained and consistent with direct measurements from various redshift surveys. Redshift distributions are recovered without any input into the redshifts of the sources making the counts. A peak of the SFRD at z 2 is preferred, although higher redshifts are not excluded. We also demonstrate that galaxy counts at 160 μm present an excess around 20 mJy that is not consistent with counts at other wavelengths under the hypotheses cited above. Finally, we find good consistency between the observed evolution of the stellar mass density and the prediction from our model of SF history. Conclusions. Multi-wavelength counts and CIRB (both projected observations) alone, interpreted with a luminosity-dependent library of SEDs, contain enough information to recover the cosmic evolution of the infrared luminosity function of galaxies, and therefore the evolution of the SFRD, with quantifiable errors. Moreover, the inability of the inversion to model perfectly and simultaneously the multi-wavelength infrared counts implies either (i) the existence of a sub-population of colder galaxies; (ii) a larger dispersion of dust temperatures among local galaxies than expected; (iii) a redshift evolution of the infrared SED of galaxies.

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Optically Faint Counterparts to theInfrared Space ObservatoryFIRBACK 170 Micron Population: Discovery of Cold, Luminous Galaxies at High Redshift

Cited by 65 publications

References 34 publications

Polycyclic aromatic hydrocarbon selected galaxies

Polycyclic aromatic hydrocarbon selected galaxies

Population synthesis modelling of luminous infrared galaxies at intermediate redshift

Cosmic star-formation history from a non-parametric inversion of infrared galaxy counts

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