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

Takeuchi, Tsutomu T.; Buat, V.; Iglésias-Páramo, J.; Boselli, A.; Burgarella, D.

doi:10.1051/0004-6361:20042189

Cited by 74 publications

(106 citation statements)

References 34 publications

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“…The discrepancy could either be explained by a larger PAH emission in distant ULIRGs or instead by the hot dust heated by a buried AGN. We note however, that part of this discrepancy could be due to uncertain local SEDs templates (Takeuchi et al 2005;Buat et al 2009). In Fig.…”

Section: Resultsmentioning

confidence: 75%

Herschelunveils a puzzling uniformity of distant dusty galaxies

Elbaz¹,

Hwang²,

Magnelli

et al. 2010

A&A

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The Herschel Space Observatory enables us to accurately measure the bolometric output of starburst galaxies and active galactic nuclei (AGN) by directly sampling the peak of their far-infrared (IR) emission. Here we examine whether the spectral energy distribution (SED) and dust temperature of galaxies have strongly evolved over the last 80% of the age of the Universe. We discuss possible consequences for the determination of starformation rates (SFR) and any evidence for a major change in their star-formation properties. We use Herschel deep extragalactic surveys from 100 to 500 μm to compute total IR luminosities in galaxies down to the faintest levels, using PACS and SPIRE in the GOODS-North field (PEP and HerMES key programs). An extension to fainter luminosities is done by stacking images on 24 μm prior positions. We show that measurements in the SPIRE bands can be used below the statistical confusion limit if information at higher spatial resolution is used, e.g. at 24 μm, to identify "isolated" galaxies whose flux is not boosted by bright neighbors. Below z ∼ 1.5, mid-IR extrapolations are correct for star-forming galaxies with a dispersion of only 40% (0.15 dex), therefore similar to z ∼ 0 galaxies, over three decades in luminosity below the regime of ultra-luminous IR galaxies (ULIRGs, L IR ≥ 10 12 L ). This narrow distribution is puzzling when considering the range of physical processes that could have affected the SED of these galaxies. Extrapolations from only one of the 160 μm, 250 μm or 350 μm bands alone tend to overestimate the total IR luminosity. This may be explained by the lack of far-IR constraints around and above ∼150 μm (rest-frame) before Herschel on those templates. We also note that the dust temperature of luminous IR galaxies (LIRGs, L IR ≥ 10 11 L ) around z ∼ 1 is mildly colder by 10-15% than their local analogs and up to 20% for ULIRGs at z ∼ 1.6 (using a single modified blackbody-fit to the peak far-IR emission with an emissivity index of β = 1.5). Above z = 1.5, distant galaxies are found to exhibit a substantially larger mid-over far-IR ratio, which could either result from stronger broad emission lines or warm dust continuum heated by a hidden AGN. Two thirds of the AGNs identified in the field with a measured redshift exhibit the same behavior as purely star-forming galaxies. Hence a large fraction of AGNs harbor coeval star formation at very high SFR and in conditions similar to purely star-forming galaxies.

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Section: Resultsmentioning

confidence: 75%

Herschelunveils a puzzling uniformity of distant dusty galaxies

Elbaz¹,

Hwang²,

Magnelli

et al. 2010

A&A

Self Cite

193

150

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“…To check the consistency of our approach, we compared our results with those of Takeuchi et al (2005), Sajina et al (2005), Caputi et al (2007), and Bavouzet et al (2008), in particular. In their work, Caputi et al provide an empirical calibration of the conversion from νL ν (8 μm) to the bolometric IR luminosity (L IR bol ), based on a sample of Spitzer-selected galaxies, while Takeuchi et al (2005) and Sajina et al (2005) obtain a relation between νL ν (24 μm) and L IR bol .…”

Section: Total Infrared Bolometric Luminosities and Lfmentioning

confidence: 97%

“…In their work, Caputi et al provide an empirical calibration of the conversion from νL ν (8 μm) to the bolometric IR luminosity (L IR bol ), based on a sample of Spitzer-selected galaxies, while Takeuchi et al (2005) and Sajina et al (2005) obtain a relation between νL ν (24 μm) and L IR bol . Bavouzet et al (2008) elaborate on the latter by including into the analysis, data at 8, 24, 70 and 160 μm, mostly from Spitzer, for their sample sources.…”

Section: Total Infrared Bolometric Luminosities and Lfmentioning

confidence: 99%

Mid- and far-infrared luminosity functions and galaxy evolution from multiwavelengthSpitzerobservations up toz ~ 2.5

Rodighiero¹,

Vaccari²,

Franceschini³

et al. 2010

A&A

156

145

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Context. Studies of the infrared (IR) emission of cosmic sources have proven essential to constraining the evolutionary history of cosmic star formation and the gravitational accretion of nuclear black holes, because many of these events occur inside heavily dustextinguished environments. Aims. The Spitzer Space Telescope has provided a large amount of data to constrain the nature and cosmological evolution of infrared source populations. In the present paper we exploit a large homogeneous dataset to derive a self-consistent picture of IR emission based on the time-dependent λ eff = 24, 15, 12, and 8 μm monochromatic and bolometric IR luminosity functions (LF) over the full 0 < z < 2.5 redshift range. Methods. Our present analysis is based on a combination of data from deep Spitzer surveys of the VIMOS VLT Deep Survey (VVDS-SWIRE) and GOODS fields. To our limiting flux of S 24 = 400 μJy, our sample derived from VVDS-SWIRE includes 1494 sources, and 666 and 904 sources brighter than S 24 = 80 μJy are catalogued in GOODS-S and GOODS-N, respectively, for a total area of ∼0.9 square degrees. Apart from a few galaxies, we obtain reliable optical identifications and redshifts for all these sources, providing a rich and robust dataset for our luminosity function determination. The final combined reliable sample includes 3029 sources, the fraction with photometric redshifts being 72% over all redshifts and almost all galaxies at z > 1.5. Based on the multiwavelength information available in these areas, we constrain the LFs at 8, 12, 15, and 24 μm. We also infer the total IR luminosities from our best-fit model of the observed SEDs of each source, and use this to derive the bolometric (8−1000 μm) LF and comoving volume emissivity to z ∼ 2.5. Results. In the redshift interval 0 < z < 1, the bolometric IR luminosity density evolves as (1 + z) 3.8±0.4 . Although it is more uncertain at higher-z, our results show a flattening in the IR luminosity density at z > 1. The mean redshift of the peak in the source number density shifts with luminosity: the brightest IR galaxies appear to form stars at earlier cosmic times (z > 1.5), while star formation in the less luminous galaxies continues until more recent epochs (z ∼ 1 for L IR < 10 11 L ), in overall agreement with similar analyses in the literature. Conclusions. Our results are indicative of a rapid increase in the galaxy IR comoving volume emissivity up to z ∼ 1 and a constant average emissivity at z > 1. We also appear to measure a difference in the evolutionary rate of the source number densities as a function of luminosity, which is consistent with the downsizing evolutionary patterns reported for other samples of cosmic sources.

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“…The extrapolation from the mid-infrared (MIR) emission to the total IR emission is known to be quite difficult but, to z = 1, we still observe a wavelength range also observed in the nearby universe by either IRAS or ISO. As a consequence, several calibrations and IR SED templates were proposed in the literature based on observations of nearby galaxies by IRAS and/or ISO (e.g., Chary & Elbaz 2001;Dale & Helou 2002;Takeuchi et al 2005a). The Spitzer observations have illustrated the large variety of IR spectral energy distributions in nearby galaxies (Dale et al 2005;Rieke et al 2008).…”

Section: Estimating the Ir Luminositiesmentioning

confidence: 99%

“…We also consider the calibrations of Takeuchi et al (2005a) (hereafter TBI05) based on a statistical analysis of all the galaxies observed in the four bands of IRAS in the Point Source Catalog (Saunders et al 2000). The relation obtained by TBI05 at λ = 12 μm for local galaxies (i.e., when we observe a galaxy at λ obs , its emitted wavelength λ em corresponds to 12 μm at z = 1) is slightly modified to take into account a slight non-linearity for the most luminous objects,…”

Section: Estimating the Ir Luminositiesmentioning

confidence: 99%

The infrared emission of ultraviolet-selected galaxies fromz= 0 toz= 1

Buat

Takeuchi²,

Burgarella

et al. 2009

A&A

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Aims. We want to study the IR (>8 μm) emission of galaxies selected on the basis of their rest-frame UV light in a very homogeneous way (wavelength and luminosity) from z = 0 to z = 1. We compare their UV and IR rest-frame emission to study the evolution in dust attenuation with z as well as to check if a UV selection is capable of tracking all star formation. This UV selection will also be compared to a sample of Lyman break galaxies selected at z 1. Methods. We select galaxies in UV (1500-1800 Å) rest-frame at z = 0, z = 0.6-0.8, z = 0.8-1.2, and with as Lyman break galaxies at z = 0.9-1.3, the samples are compiled to sample the same range of luminosity at any redshift. The UV rest-frame data come from GALEX for z < 1 and the U-band of the EIS survey (at z = 1). The UV data are combined with the IRAS 60 μm observations at z = 0 and the Spitzer data at 24 μm for z > 0 sources. The evolution in the IR and UV luminosities with z is analysed for individual galaxies as well as in terms of luminosity functions. Results. The L IR /L UV ratio is used to measure dust attenuation. This ratio does not seem to evolve significantly with z for the bulk of our sample galaxies, but some trends are found for both galaxies with a strong dust attenuation and UV luminous sources: galaxies with L IR /L UV > 10 are more frequent at z > 0 than at z = 0, and the largest values of L IR /L UV are found for UV faint objects; in contrast, the most luminous galaxies of our samples (L UV > 2 × 10 10 L ), detected at z = 1, exhibit a lower dust attenuation than fainter ones. The value of L IR /L UV increases with the K rest-frame luminosity of the galaxies at all redshifts considered and shows a residual anticorrelation with L UV . The most massive and UV luminous galaxies exhibit quite high specific star formation rates. Lyman break galaxies exhibit systematically lower dust attenuation than UV-selected galaxies of same luminosity, but similar specific star formation rates. The analysis of the UV + IR luminosity functions leads to the conclusion that up to z = 1, most of the star formation activity of UV-selected galaxies is emitted in IR. Although we are able to infer information about all the star formation from our UV selection at z = 0.7, at z = 1 we miss a large fraction of galaxies more luminous than 10 11 L . The effect is found to be larger for Lyman break galaxies.

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

Cited by 74 publications

References 34 publications

Herschelunveils a puzzling uniformity of distant dusty galaxies

Herschelunveils a puzzling uniformity of distant dusty galaxies

Mid- and far-infrared luminosity functions and galaxy evolution from multiwavelengthSpitzerobservations up toz ~ 2.5

The infrared emission of ultraviolet-selected galaxies fromz= 0 toz= 1

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