The cosmic far-infrared background buildup since redshift 2 at 70 and 160 microns in the COSMOS and GOODS fields

Jauzac, Mathilde; Dole, H.; Floc’h, E. Le; Aussel, H.; Caputi, K.; Ilbert, O.; Salvato, M.; Bavouzet, N.; Beelen, A.; Béthermin, M.; Kneib, Jean-Paul; Lagache, G.; Puget, J.

doi:10.1051/0004-6361/201015432

Cited by 34 publications

(49 citation statements)

References 73 publications

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“…The best-fit parameters as well as their uncertainties and degeneracies were obtained using a Monte Carlo Markov chain (MCMC) Metropolis-Hastings algorithm. The model adjusted on deep counts and monochromatic LFs at key wavelengths also reproduces recent very discriminating observations well, such as the Jauzac et al (2011) measured redshift distribution of the CIB.…”

Section: Resultssupporting

confidence: 63%

Planckearly results. XVIII. The power spectrum of cosmic infrared background anisotropies

Ade¹,

Aghanim²,

Arnaud³

et al. 2011

A&A

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185

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Using Planck maps of six regions of low Galactic dust emission with a total area of about 140 deg 2 , we determine the angular power spectra of cosmic infrared background (CIB) anisotropies from multipole = 200 to = 2000 at 217, 353, 545 and 857 GHz. We use 21-cm observations of Hi as a tracer of thermal dust emission to reduce the already low level of Galactic dust emission and use the 143 GHz Planck maps in these fields to clean out cosmic microwave background anisotropies. Both of these cleaning processes are necessary to avoid significant contamination of the CIB signal. We measure correlated CIB structure across frequencies. As expected, the correlation decreases with increasing frequency separation, because the contribution of high-redshift galaxies to CIB anisotropies increases with wavelengths. We find no significant difference between the frequency spectrum of the CIB anisotropies and the CIB mean, with ΔI/I = 15% from 217 to 857 GHz. In terms of clustering properties, the Planck data alone rule out the linear scale-and redshift-independent bias model. Non-linear corrections are significant. Consequently, we develop an alternative model that couples a dusty galaxy, parametric evolution model with a simple halo-model approach. It provides an excellent fit to the measured anisotropy angular power spectra and suggests that a different halo occupation distribution is required at each frequency, which is consistent with our expectation that each frequency is dominated by contributions from different redshifts. In our best-fit model, half of the anisotropy power at = 2000 comes from redshifts z < 0.8 at 857 GHz and z < 1.5 at 545 GHz, while about 90% come from redshifts z > 2 at 353 and 217 GHz, respectively.

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Section: Resultssupporting

confidence: 63%

Planckearly results. XVIII. The power spectrum of cosmic infrared background anisotropies

Ade¹,

Aghanim²,

Arnaud³

et al. 2011

A&A

Self Cite

185

View full text Add to dashboard Cite

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“…Note that to help aid the comparison, error bars include systematics due to calibration and beam uncertainties. They are: BLAST data from Viero et al (2009;brown crosses) and Hajian et al (2012;lavender diamonds) 24 μm selected sources; Jauzac et al 2011), and we also find an uncharacteristically large β (discussed further in Section 6.3).…”

Section: Comparison To Published Modelsmentioning

confidence: 56%

HerMES: COSMIC INFRARED BACKGROUND ANISOTROPIES AND THE CLUSTERING OF DUSTY STAR-FORMING GALAXIES

Viero

Wang

Zemcov

et al. 2013

ApJ

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We present measurements of the auto-and cross-frequency power spectra of the cosmic infrared background (CIB) at 250, 350, and 500 μm (1200, 860, and 600 GHz) from observations totaling ∼70 deg 2 made with the SPIRE instrument aboard the Herschel Space Observatory. We measure a fractional anisotropy δI /I = 14% ± 4%, detecting signatures arising from the clustering of dusty star-forming galaxies in both the linear (2-halo) and nonlinear (1-halo) regimes; and that the transition from the 2-to 1-halo terms, below which power originates predominantly from multiple galaxies within dark matter halos, occurs at k θ ∼ 0.10-0.12 arcmin −1 ( ∼ 2160-2380), from 250 to 500 μm. New to this paper is clear evidence of a dependence of the Poisson and 1-halo power on the flux-cut level of masked sources-suggesting that some fraction of the more luminous sources occupy more massive halos as satellites, or are possibly close pairs. We measure the cross-correlation power spectra between bands, finding that bands which are farthest apart are the least correlated, as well as hints of a reduction in the correlation between bands when resolved sources are more aggressively masked. In the second part of the paper, we attempt to interpret the measurements in the framework of the halo model. With the aim of fitting simultaneously with one model the power spectra, number counts, and absolute CIB level in all bands, we find that this is achievable by invoking a luminosity-mass relationship, such that the luminosity-to-mass ratio peaks at a particular halo mass scale and declines toward lower and higher mass halos. Our best-fit model finds that the halo mass which is most efficient at hosting star formation in the redshift range of peak star-forming activity, z ∼ 1-3, is log(M peak /M ) ∼ 12.1 ± 0.5, and that the minimum halo mass to host infrared galaxies is log(M min /M ) ∼ 10.1 ± 0.6.

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“…In this case their hosts exhibit much redder colors than those allowed by the "IRAC peaker" selection, which would contribute to lowering its efficiency. However, the AGN contribution to the whole population of IR galaxies and to the cosmic infrared background is likely not more than 15% (e.g., Jauzac et al 2011), so their possible contamination in our sample can not be the main explanation for the incompleteness of the IRAC peaker method.…”

Section: Application To the 24 µM Selected Galaxy Populations In Cosmosmentioning

confidence: 90%

Dust-obscured star formation and the contribution of galaxies escaping UV/optical color selections atz ~ 2

Riguccini¹,

Floc’h²,

Ilbert³

et al. 2011

A&A

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Context. A substantial amount of the stellar mass growth across cosmic time occurred within dust-enshrouded environments. So far, identification of complete samples of distant star-forming galaxies from the short wavelength range has been strongly biased by the effect of dust extinction. Nevertheless, the exact amount of star-forming activity that took place in high-redshift dusty galaxies but that has currently been missed by optical surveys has barely been explored. Aims. Our goal is to determine the number of luminous star-forming galaxies at 1.5 < ∼ z < ∼ 3 that are potentially missed by the traditional color selection techniques because of dust extinction. We also aim at quantifying the contribution of these sources to the IR luminosity and cosmic star formation density at high redshift. Methods. We based our work on a sample of 24 μm sources brighter than 80 μJy and taken from the Spitzer survey of the COSMOS field. Almost all of these sources have accurate photometric redshifts. We applied to this mid-IR selected sample the BzK and BM/BX criteria, as well as the selections of the IRAC peakers and the Optically-Faint IR-bright (OFIR) galaxies. We analyzed the fraction of sources identified with these techniques. We also computed 8 μm rest-frame luminosity from the 24 μm fluxes of our sources, and considering the relationships between L 8 μm and L Paα and between L 8 μm and L IR , we derived ρ IR and then ρ SFR for our MIPS sources. Results. The BzK criterion offers an almost complete (∼90%) identification of the 24 μm sources at 1.4 < z < 2.5. In contrast, the BM/BX criterion misses 50% of the MIPS sources. We attribute this bias to the effect of extinction, which reddens the typical colors of galaxies. The contribution of these two selections to the IR luminosity density produced by all the sources brighter than 80 μJy are on the same order. Moreover the criterion based on the presence of a stellar bump in their spectra (IRAC peakers) misses up to 40% of the IR luminosity density, while only 25% of the IR luminosity density at z ∼ 2 is produced by OFIR galaxies characterized by extreme mid-IR to optical flux ratios. Conclusions. Color selections of distant star-forming galaxies must be used with care given the substantial bias they can suffer. In particular, the effect of dust extinction strongly affects the completeness of identifications at the bright end of the bolometric luminosity function, which implies large and uncertain extrapolations to account for the contribution of dusty galaxies missed by these selections. In the context of forthcoming facilities that will operate at long wavelengths (e.g., JWST, ALMA, SAFARI, EVLA, SKA), this emphasizes the importance of minimizing the extinction biases when probing the activity of star formation in the early Universe.

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The cosmic far-infrared background buildup since redshift 2 at 70 and 160 microns in the COSMOS and GOODS fields

Cited by 34 publications

References 73 publications

Planckearly results. XVIII. The power spectrum of cosmic infrared background anisotropies

Planckearly results. XVIII. The power spectrum of cosmic infrared background anisotropies

HerMES: COSMIC INFRARED BACKGROUND ANISOTROPIES AND THE CLUSTERING OF DUSTY STAR-FORMING GALAXIES

Dust-obscured star formation and the contribution of galaxies escaping UV/optical color selections atz ~ 2

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