# Difference between revisions of "CMB spectrum & Likelihood Code"

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For multipoles equal or greater than <math>\ell=30</math>, instead, the spectrum is derived from the ''Plik'' likelihood {{PlanckPapers|planck2014-a13}} by optimally combining the spectra in the frequency range 100-217 GHz, and correcting them for unresolved foregrounds using the best-fit foreground solution from a Planck TT+lowP <math>\Lambda</math>CDM run. Associated 1-sigma errors include beam uncertainties. Both ''Commander'' and ''Plik'' are described in more details in the sections below. | For multipoles equal or greater than <math>\ell=30</math>, instead, the spectrum is derived from the ''Plik'' likelihood {{PlanckPapers|planck2014-a13}} by optimally combining the spectra in the frequency range 100-217 GHz, and correcting them for unresolved foregrounds using the best-fit foreground solution from a Planck TT+lowP <math>\Lambda</math>CDM run. Associated 1-sigma errors include beam uncertainties. Both ''Commander'' and ''Plik'' are described in more details in the sections below. | ||

− | [[File: | + | [[File: A15 TT.pdf|thumb|center|700px|'''2015 CMB TT spectrum. Logarithmic x-scale up to <math>\ell=30</math>, linear at higher <math>\ell</math>; all points with error bars. The red line is the Planck best-fit primordial power spectrum (cf Planck TT+lowP in Table 3 of {{PlanckPapers|planck2014-a15}}). The blue shaded area shows the uncertainties due to cosmic variance alone.''']] |

====TE and EE==== | ====TE and EE==== |

## Revision as of 09:47, 5 February 2015

## Contents

## 2015 CMB spectra[edit]

### General description[edit]

#### TT[edit]

The Planck best-fit CMB temperature power spectrum, shown in the figure below, covers the wide range of multipoles = 2-2508. Over the multipole range = 2–29, the power spectrum is derived from the *Commander*: component separation algorithm applied to the combination of Planck 2015 temperature data between 30 and 857 GHz, the 9-year WMAP sky maps, and the 408 MHz Haslam et al. (1982) survey, including 93% of the sky Planck-2015-A10^{[1]} . The asymmetric error bars associated to this spectrum are the 68% confidence limits and include the uncertainties due to foreground subtraction.

For multipoles equal or greater than *Plik* likelihood Planck-2015-A11^{[2]} by optimally combining the spectra in the frequency range 100-217 GHz, and correcting them for unresolved foregrounds using the best-fit foreground solution from a Planck TT+lowP CDM run. Associated 1-sigma errors include beam uncertainties. Both *Commander* and *Plik* are described in more details in the sections below.

#### TE and EE[edit]

The Planck best-fit CMB polarization and temperature-polarization cross-correlation power spectra, shown in the figure below, cover the multipole range = 30-1996. The data points relative to the multipole range = 2-29 will be released in a second moment.
Analogously to the TT case, the spectrum is derived from the *Plik* likelihood Planck-2015-A11^{[2]} by optimally combining the spectra in the frequency range 100-217 GHz, and correcting them for unresolved foregrounds using the best-fit foreground solution from a Planck TT,TE,EE+lowP CDM run.

### Production process[edit]

The Planck-2015-A10^{[1]}. The power spectrum at any multipole is given as the maximum probability point for the posterior distribution, marginalized over the other multipoles, and the error bars are 68% confidence level; see Planck-2015-A10^{[1]}.

The Planck-2013-XV^{[4]} and Planck-2015-A11^{[2]}. Frequency spectra are computed as cross-spectra between half-mission maps. Mask and multipole range choices for each frequency spectrum are summarized in Section 3.3 of Planck-2015-A13^{[3]} and in Planck-2015-A11^{[2]}. The final power spectrum is an optimal combination of the 100, 143, 143x217 and 217 GHz spectra, corrected for the best-fit unresolved foregrounds and inter-frequency calibration factors, as derived from the full likelihood analysis (for TT we use the best-fit solutions for the nuisance parameters from the Planck+TT+lowP data combination, while for TE and EE we use the best fit from Planck+TT+lowP, cf Table 3 of Planck-2015-A13^{[3]}). A thorough description of the models of unresolved foregrounds is given in Planck-2015-A11^{[2]}. The spectrum covariance matrix accounts for cosmic variance and noise contributions, together with beam uncertainties. The CMB TT spectrum and associated covariance matrix are available in two formats:

- Unbinned. TT: 2479 bandpowers ( ); TE or EE: 1697 bandpowers ( ).
- Binned, in bins of . TT: 83 bandpowers. TE or EE: 66 bandpowers. We bin the power spectrum with a weight proportional to , so that the binned bandpower centered in is: Equivalently, using the matrix formalism, we can construct the binning matrix B as: where B is a matrix, with the number of bins and the number of unbinned multipoles. Thus: Here, is the vector containing all the binned (unbinned) bandpowers, is the covariance matrix and is the weighted average multipole in each bin. Note that following this definition, can be a non-integer. The binned power spectrum is then calculated as: .

### Inputs[edit]

- Low-l spectrum ( )

- Planck 30 and 44 GHz frequency maps
- Planck 70 to 857 GHz detector and detector set maps
- 9-year WMAP temperature sky maps between 23 and 94 GHz
- 408 MHz survey by Haslam et al. (1982)
- Commander Planck-2015-A10
^{[1]} based LM93 confidence mask

- High-l spectrum ( )

- 100, 143, 143x217 and 217 GHz spectra and their covariance matrix (Sec. 3.3 Planck-2015-A13
^{[3]}) - best-fit foreground templates and inter-frequency calibration factors (Table 3 of Planck-2015-A13
^{[3]}) - Beam transfer function uncertainties Planck-2015-A07
^{[5]}

### File names and Meta data[edit]

The CMB spectrum and its covariance matrix are distributed in a single FITS file named

*COM_PowerSpect_CMB_R2.nn.fits*

which contains 7 *BINTABLE* extensions

- 1. TT low-ell, unbinned (TTLOLUNB)
- with the low ell part of the spectrum, not binned, and for l=2-29. The table columns are

*ELL*(integer): multipole number*D_ELL*(float): as described above*ERRUP*(float): the upward uncertainty*ERRDOWN*(float): the downward uncertainty

- 2. TT high-ell, binned (TTHILBIN)
- with the high-ell part of the spectrum, binned into 83 bins covering in bins of width (with the exception of the last bin that is smaller). The table columns are as follows:

*ELL*(integer): mean multipole number of bin*L_MIN*(integer): lowest multipole of bin*L_MAX*(integer): highest multipole of bin*D_ELL*(float): as described above*ERR*(float): the uncertainty

- 3. TT high-ell unbinned (TTHILUNB)
- with the high-ell part of the spectrum, unbinned, in 2979 bins covering . The table columns are as follows:

*ELL*(integer): multipole*D_ELL*(float): as described above*ERR*(float): the uncertainty

- 4. TE high-ell, binned (TEHILBIN)
- with the high-ell part of the spectrum, binned into 83 bins covering in bins of width (with the exception of the last bin that is smaller). The table columns are as follows:

*ELL*(integer): mean multipole number of bin*L_MIN*(integer): lowest multipole of bin*L_MAX*(integer): highest multipole of bin*D_ELL*(float): as described above*ERR*(float): the uncertainty

- 5. TE high-ell, unbinned (TEHILUNB)
- with the high-ell part of the spectrum, unbinned, in 2979 bins covering . The table columns are as follows:

*ELL*(integer): multipole*D_ELL*(float): as described above*ERR*(float): the uncertainty

- 6. EE high-ell, binned (EELOLBIN)
- with the high-ell part of the spectrum, binned into 83 bins covering in bins of width (with the exception of the last bin that is smaller). The table columns are as follows:

*ELL*(integer): mean multipole number of bin*L_MIN*(integer): lowest multipole of bin*L_MAX*(integer): highest multipole of bin*D_ELL*(float): as described above*ERR*(float): the uncertainty

- 7. EE high-ell, unbinned (EEHILUNB)
- with the high-ell part of the spectrum, unbinned, in 2979 bins covering . The table columns are as follows:

*ELL*(integer): multipole*D_ELL*(float): as described above*ERR*(float): the uncertainty

The spectra give in units of . The covariance matrices of the spectra will be released in a second moment.

## Likelihood[edit]

The likelihood will soon be released with an accompanying paper and an Explanatory Supplement update.

## References[edit]

- ↑
^{1.0}^{1.1}^{1.2}^{1.3}**Planck 2015 results. X. Diffuse component separation: Foreground maps**, Planck Collaboration, 2016, A&A, 594, A10. - ↑
^{2.0}^{2.1}^{2.2}^{2.3}^{2.4}**Planck 2015 results. XI. CMB power spectra, likelihoods, and robustness of cosmological parameters**, Planck Collaboration, 2016, A&A, 594, A11. - ↑
^{3.0}^{3.1}^{3.2}^{3.3}^{3.4}^{3.5}^{3.6}**Planck 2015 results. XIII. Cosmological parameters**, Planck Collaboration, 2016, A&A, 594, A13. - ↑
**Planck 2013 results. XV. CMB power spectra and likelihood**, Planck Collaboration, 2014, A&A, 571, A15 - ↑
**Planck 2015 results. VII. High Frequency Instrument data processing: Time-ordered information and beam processing**, Planck Collaboration, 2016, A&A, 594, A7.

Cosmic Microwave background

Flexible Image Transfer Specification