Large-scale Maps of the Cosmic Infrared Background from Planck

Lenz, Daniel; Doré, O.; Lagache, G.

doi:10.3847/1538-4357/ab3c2b

Cited by 54 publications

(70 citation statements)

References 58 publications

(61 reference statements)

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“…Each redshift shell is populated with CIB galaxies and galaxy clusters with probabilities proportional to the density contrast distribution, with a population-dependent bias. The CIB maps constructed in this way have power spectra that agree with measurements from Planck data at high frequencies using several different methods for dealing with Galactic dust and CMB contamination (Planck Collaboration XXX 2014;Mak et al 2017;Lenz et al 2019).…”

Section: Tests Of Cmb Lensing Foreground Correlationsmentioning

confidence: 63%

Planck2018 results

Aghanim¹,

Akrami²,

Ashdown³

et al. 2020

A&A

523

170

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We present measurements of the cosmic microwave background (CMB) lensing potential using the final Planck 2018 temperature and polarization data. Using polarization maps filtered to account for the noise anisotropy, we increase the significance of the detection of lensing in the polarization maps from 5σ to 9σ. Combined with temperature, lensing is detected at 40σ. We present an extensive set of tests of the robustness of the lensing-potential power spectrum, and construct a minimum-variance estimator likelihood over lensing multipoles 8 ≤ L ≤ 400 (extending the range to lower L compared to 2015), which we use to constrain cosmological parameters. We find good consistency between lensing constraints and the results from the Planck CMB power spectra within the ΛCDM model. Combined with baryon density and other weak priors, the lensing analysis alone constrains σ8Ωm0.25 = 0.589 ± 0.020 (1σ errors). Also combining with baryon acoustic oscillation data, we find tight individual parameter constraints, σ8 = 0.811 ± 0.019, H0 = 67.9−1.3+1.2 km s−1 Mpc−1, and Ωm = 0.303−0.018+0.016. Combining with Planck CMB power spectrum data, we measure σ8 to better than 1% precision, finding σ8 = 0.811 ± 0.006. CMB lensing reconstruction data are complementary to galaxy lensing data at lower redshift, having a different degeneracy direction in σ8 − Ωm space; we find consistency with the lensing results from the Dark Energy Survey, and give combined lensing-only parameter constraints that are tighter than joint results using galaxy clustering. Using the Planck cosmic infrared background (CIB) maps as an additional tracer of high-redshift matter, we make a combined Planck-only estimate of the lensing potential over 60% of the sky with considerably more small-scale signal. We additionally demonstrate delensing of the Planck power spectra using the joint and individual lensing potential estimates, detecting a maximum removal of 40% of the lensing-induced power in all spectra. The improvement in the sharpening of the acoustic peaks by including both CIB and the quadratic lensing reconstruction is detected at high significance.

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Section: Tests Of Cmb Lensing Foreground Correlationsmentioning

confidence: 63%

Planck2018 results

Aghanim¹,

Akrami²,

Ashdown³

et al. 2020

A&A

523

170

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show abstract

“…In Fig. C.1 we show the measurements of the CIB power spectra from Planck/HFI (Planck Collaboration XXX 2014), Herschel/SPIRE (Viero et al 2013), and Lenz et al (2019) at 857 GHz. We also show the best-fit values of the one-halo, shot noise, and the total power spectrum when the model was fit to the Planck or Herschel data alone.…”

Section: Resultsmentioning

confidence: 99%

Simple halo model formalism for the cosmic infrared background and its correlation with the thermal Sunyaev-Zel’dovich effect

Maniyar

Béthermin

Lagache

2021

A&A

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Modelling the anisotropies in the cosmic infrared background (CIB) on all the scales is a challenging task because the nature of the galaxy evolution is complex and too many parameters are therefore often required to fit the observational data. We present a new halo model for the anisotropies of the CIB using only four parameters. Our model connects the mass accretion on the dark matter haloes to the star formation rate. Despite its relative simplicity, it is able to fit both the Planck and Herschel CIB power spectra and is consistent with the external constraints for the obscured star formation history derived from infrared deep surveys used as priors for the fit. Using this model, we find that the halo mass with the maximum efficiency for converting the accreted baryons into stars is log 10 M max = 12.94 +0.02 −0.02 M , consistent with other studies. Accounting for the mass loss through stellar evolution, we find for an intermediate-age galaxy that the star formation efficiency defined as M (z)/M b (z) is equal to 0.19 and 0.21 at redshift 0.1 and 2, respectively, which agrees well with the values obtained by previous studies. A CIB model is used for the first time to simultaneously fit Planck and Herschel CIB power spectra. The high angular resolution of Herschel allows us to reach very small scales, making it possible to constrain the shot noise and the one-halo term separately, which is difficult to do using the Planck data alone. However, we find that large angular scale Planck and Herschel data are not fully compatible with the small-scale Herschel data (for > 3000). The CIB is expected to be correlated with the thermal Sunyaev-Zel'dovich (tSZ) signal of galaxy clusters. Using this halo model for the CIB and a halo model for the tSZ with a single parameter, we also provide a consistent framework for calculating the CIB × tSZ cross correlation, which requires no additional parameter. To a certain extent, the CIB at high frequencies traces galaxies at low redshifts that reside in the clusters contributing to the tSZ, giving rise to the one-halo term of this correlation, while the two-halo term comes from the overlap in the redshift distribution of the tSZ clusters and CIB galaxies. The CIB × tSZ correlation is thus found to be higher when inferred with a combination of two widely spaced frequency channels (e.g. 143 × 857 GHz). We also find that even at ∼ 2000, the two-halo term of this correlation is still comparable to the one-halo term and has to be accounted for in the total cross-correlation. The CIB, tSZ, and CIB × tSZ act as foregrounds when the kinematic SZ (kSZ) power spectrum is measured from the cosmic microwave background power spectrum and need to be removed. Because of its simplistic nature and the low number of parameters, the halo model formalism presented here for these foregrounds is quite useful for such an analysis to measure the kSZ power spectrum accurately.

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“…In principle we might have a precise location of ASGWB in the observed space frame. Indeed, the ASGWB signal is resembling other astrophysical backgrounds, such as e.g., the cosmic infrared background (CIB), that have been studied in the past (see e.g., [28][29][30]).…”

Section: Introductionmentioning

confidence: 92%

“…In this case we are able to write explicitly Eqs. (23) and (30), and obtain the final equation for the affine parameter Eq. (29) δχ…”

Section: First Order Metric Termsmentioning

confidence: 99%

Projection effects on the observed angular spectrum of the astrophysical stochastic gravitational wave background

et al. 2020

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The detection and characterization of the stochastic gravitational wave background (SGWB) is one of the main goals of gravitational wave (GW) experiments. The observed SGWB will be the combination of GWs from cosmological (as predicted by many models describing the physics of the early universe) and astrophysical origins, which will arise from the superposition of GWs from unresolved sources whose signal is too faint to be detected. Therefore, it is important to have a proper modeling of the astrophysical SGWB (ASGWB) in order to disentangle the two signals; moreover, this will provide additional information on astrophysical properties of compact objects. Applying the cosmic rulers formalism, we compute the observed ASGWB angular power spectrum, hence using gauge-invariant quantities, accounting for all effects intervening between the source and the observer. These are the so-called projection effects, which include Kaiser, Doppler, and gravitational potentials effect. Our results show that these projection effects are the most important at the largest scales, and they contribute to up to tens of percent of the angular power spectrum amplitude, with the Kaiser term being the largest at all scales. While the exact impact of these results will depend on instrumental and astrophysical details, a precise theoretical modeling of the ASGWB will necessarily need to include all these projection effects.

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Large-scale Maps of the Cosmic Infrared Background from Planck

Cited by 54 publications

References 58 publications

Planck2018 results

Planck2018 results

Simple halo model formalism for the cosmic infrared background and its correlation with the thermal Sunyaev-Zel’dovich effect

Projection effects on the observed angular spectrum of the astrophysical stochastic gravitational wave background

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