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The CMB angular power spectrum via component separation: a study on Planck data
Cosmology and Nongalactic Astrophysics · Submitted 2 Jul 2018
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim The results on cosmological parameters depend on the detail of the foreground residual contamination in the spectrum, and need a tailored modeling of the likelihood foreground model.
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The abstract, sentence by sentence
We investigate the extent to which foreground cleaned CMB maps can be used to estimate the cosmological parameters at small scales. We use the SMICA method, a blind separation technique which works directly at the spectral level. In this work we focus on the small scales of the CMB angular power spectrum, which are chiefly affected by noise and extragalactic foregrounds, such as point sources. We adapt SMICA to use only cross-spectra between data maps, thus avoiding the noise bias. In this study, performed both on simulations and on Planck 2015 data, we fit for extragalactic point sources by modeling them as shot noise of two independent populations. In simulations we correctly recover the point source emission law, and obtain a CMB angular power spectrum that has an average foreground residual of one fifth of the CMB power at $\ell \geq$ 2200. On Planck data, the recovered point source emission law corresponds to external estimates, with some offsets at the highest and lowest frequencies, possibly due to frequency decoherence of point sources. The CMB angular power spectrum residuals are consistent with what we find in simulations. The cosmological parameters obtained from the simulations and the data show offsets up to 1$\sigma$ on average from their expected values. Biases on cosmological parameters in simulations represent the expected level of bias in Planck data. The results on cosmological parameters depend on the detail of the foreground residual contamination in the spectrum, and need a tailored modeling of the likelihood foreground model.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We investigate the extent to which foreground cleaned CMB maps can be used to estimate the cosmological parameters at small scales. | contribution 0.75 | 0.64 | 0.05 | unclear 0.76 |
| s1 | We use the SMICA method, a blind separation technique which works directly at the spectral level. | method 0.99 | 0.60 | 0.03 | asserted 0.99 |
| s2 | In this work we focus on the small scales of the CMB angular power spectrum, which are chiefly affected by noise and extragalactic foregrounds, such as point sources. | background 0.90 | 0.18 | 0.03 | asserted 0.98 |
| s3 | We adapt SMICA to use only cross-spectra between data maps, thus avoiding the noise bias. | method 0.90 | 0.94 | 0.04 | asserted 0.99 |
| s4 | In this study, performed both on simulations and on Planck 2015 data, we fit for extragalactic point sources by modeling them as shot noise of two independent populations. | method 0.90 | 0.96 | 0.06 | asserted 0.98 |
| s5 | In simulations we correctly recover the point source emission law, and obtain a CMB angular power spectrum that has an average foreground residual of one fifth of the CMB power at $\ell \geq$ 2200. | result 1.00 | 0.97 | 0.17 | asserted 1.00 |
| s6 | On Planck data, the recovered point source emission law corresponds to external estimates, with some offsets at the highest and lowest frequencies, possibly due to frequency decoherence of point sources. | result 0.99 | 0.95 | 0.07 | hedged possibility 0.55 |
| s7 | The CMB angular power spectrum residuals are consistent with what we find in simulations. | result 0.99 | 0.94 | 0.10 | hedged possibility 0.66 |
| s8 | The cosmological parameters obtained from the simulations and the data show offsets up to 1$\sigma$ on average from their expected values. | result 1.00 | 0.94 | 0.19 | asserted 1.00 |
| s9 | Biases on cosmological parameters in simulations represent the expected level of bias in Planck data. | interpretation 0.93 | 0.72 | 0.20 | asserted 0.99 |
| s10 | The results on cosmological parameters depend on the detail of the foreground residual contamination in the spectrum, and need a tailored modeling of the likelihood foreground model. | interpretation 0.57 | 0.72 | 0.53 | asserted 0.97 |
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Original abstract
We investigate the extent to which foreground cleaned CMB maps can be used to estimate the cosmological parameters at small scales. We use the SMICA method, a blind separation technique which works directly at the spectral level. In this work we focus on the small scales of the CMB angular power spectrum, which are chiefly affected by noise and extragalactic foregrounds, such as point sources. We adapt SMICA to use only cross-spectra between data maps, thus avoiding the noise bias. In this study, performed both on simulations and on Planck 2015 data, we fit for extragalactic point sources by modeling them as shot noise of two independent populations. In simulations we correctly recover the point source emission law, and obtain a CMB angular power spectrum that has an average foreground residual of one fifth of the CMB power at $\ell \geq$ 2200. On Planck data, the recovered point source emission law corresponds to external estimates, with some offsets at the highest and lowest frequencies, possibly due to frequency decoherence of point sources. The CMB angular power spectrum residuals are consistent with what we find in simulations. The cosmological parameters obtained from the simulations and the data show offsets up to 1$\sigma$ on average from their expected values. Biases on cosmological parameters in simulations represent the expected level of bias in Planck data. The results on cosmological parameters depend on the detail of the foreground residual contamination in the spectrum, and need a tailored modeling of the likelihood foreground model.
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