Constraints on the cosmic star formation history from the far-infrared background

I review the assumptions and observations that motivate the concept of the extragalactic cosmic background radiation, and the issues of energy accounts and star formation history as a function of galaxy morphological type that figure in the interpretation of the measurements of the extragalactic infrared background.

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Star formation history from the cosmic infrared background anisotropies

Astronomy and Astrophysics ◽

10.1051/0004-6361/201732499 ◽

2018 ◽

Vol 614 ◽

pp. A39 ◽

Cited By ~ 12

Author(s):

A. S. Maniyar ◽

M. Béthermin ◽

G. Lagache

Keyword(s):

Dark Matter ◽

Star Formation ◽

Star Formation Rate ◽

Formation Rate ◽

Star Formation History ◽

Dark Matter Halo ◽

Model Parameters ◽

Formation History ◽

Infrared Background ◽

Cosmic Infrared Background

We present a linear clustering model of cosmic infrared background (CIB) anisotropies at large scales that is used to measure the cosmic star formation rate density up to redshift 6, the effective bias of the CIB, and the mass of dark matter halos hosting dusty star-forming galaxies. This is achieved using the Planck CIB auto- and cross-power spectra (between different frequencies) and CIB × CMB (cosmic microwave background) lensing cross-spectra measurements, as well as external constraints (e.g. on the CIB mean brightness). We recovered an obscured star formation history which agrees well with the values derived from infrared deep surveys and we confirm that the obscured star formation dominates the unobscured formation up to at least z = 4. The obscured and unobscured star formation rate densities are compatible at 1σ at z = 5. We also determined the evolution of the effective bias of the galaxies emitting the CIB and found a rapid increase from ~0.8 at z = 0 to ~8 at z = 4. At 2 < z < 4, this effective bias is similar to that of galaxies at the knee of the mass functions and submillimetre galaxies. This effective bias is the weighted average of the true bias with the corresponding emissivity of the galaxies. The halo mass corresponding to this bias is thus not exactly the mass contributing the most to the star formation density. Correcting for this, we obtained a value of log(Mh/M⊙) = 12.77−0.125+0.128 for the mass of the typical dark matter halo contributing to the CIB at z = 2. Finally, using a Fisher matrix analysis we also computed how the uncertainties on the cosmological parameters affect the recovered CIB model parameters, and find that the effect is negligible.

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Cosmic infrared background measurements and star formation history from Planck

Proceedings of the International Astronomical Union ◽

10.1017/s1743921314011065 ◽

2014 ◽

Vol 10 (S306) ◽

pp. 144-146

Author(s):

Paolo Serra ◽

Keyword(s):

Star Formation ◽

Power Spectrum ◽

Signal To Noise Ratio ◽

Spectral Energy Distribution ◽

Power Spectra ◽

Star Formation History ◽

Spectral Energy ◽

Formation History ◽

Infrared Background ◽

Cosmic Infrared Background

AbstractWe present new measurements of Cosmic Infrared Background (CIB) anisotropies using Planck. Combining HFI data with IRAS, the angular auto- and cross-frequency power spectrum is measured from 143 to 3000 GHz. After careful removal of the contaminants (cosmic microwave background anisotropies, Galactic dust and Sunyaev-Zeldovich emission), and a complete study of systematics, the CIB power spectrum is measured with unprecedented signal to noise ratio from angular multipoles ℓ ~ 150 to 2500. The interpretation based on the halo model is able to associate star-forming galaxies with dark matter halos and their subhalos, using a parametrized relation between the dust-processed infrared luminosity and (sub-)halo mass, and it allows to simultaneously fit all auto- and cross- power spectra very well. We find that the star formation history is well constrained up to redshifts around 2, and agrees with recent estimates of the obscured star-formation density using Spitzer and Herschel. However, at higher redshift, the accuracy of the star formation history measurement is strongly degraded by the uncertainty in the spectral energy distribution of CIB galaxies. We also find that the mean halo mass which is most efficient at hosting star formation is log(Meff/M⊙) = 12.6 and that CIB galaxies have warmer temperatures as redshift increases.

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The 0.4 $\mathsf{<}$ z $\mathsf{<}$ 1.3 star formation history of the Universe as viewed in the far-infrared

Astronomy and Astrophysics ◽

10.1051/0004-6361:200811443 ◽

2009 ◽

Vol 496 (1) ◽

pp. 57-75 ◽

Cited By ~ 281

Author(s):

B. Magnelli ◽

D. Elbaz ◽

R. R. Chary ◽

M. Dickinson ◽

D. Le Borgne ◽

...

Keyword(s):

Star Formation ◽

Far Infrared ◽

Star Formation History ◽

Formation History ◽

History Of ◽

The Universe

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Submillimeter Surveys at High Redshift

Highlights of Astronomy ◽

10.1017/s1539299600014106 ◽

2002 ◽

Vol 12 ◽

pp. 469-472

Author(s):

Amy J. Barger

Keyword(s):

Star Formation ◽

Near Infrared ◽

High Redshift ◽

Large Fraction ◽

Far Infrared ◽

Star Formation History ◽

Infrared Galaxies ◽

Small Admixture ◽

Formation History ◽

Ultraluminous Infrared Galaxies

AbstractDeep submillimeter (submm) surveys offer an unobscured view of dust-enshrouded star formation or AGN activity at high red-shifts. SCUBA observations above 2 mJy have resolved 20 – 30% of the far-infrared (FIR) background into discrete sources and have revealed the existence of a distant population of galaxies with properties similar to those of local ultraluminous infrared galaxies. A large fraction of the submm sources have extremely faint optical/near-infrared (NIR) counterparts and hence are inaccessible to optical spectroscopy. Millimetric redshift estimation places the submm population atz= 1 to 3. While the cumulative surface density of the submm sources is low, they are so luminous that if powered mainly by star formation, they dominate the high redshift star formation history. Recent combined SCUBA submm andChandrahard X-ray studies suggest that the majority of the submm sources are star formers with only a small admixture of obscured AGN.

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