# Difference between revisions of "Frequency map angular power spectrum"

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==CMB angular power spectra== | ==CMB angular power spectra== | ||

− | Auto and cross angular power spectra | + | Auto and cross angular power spectra for the 13 detset maps available at 100, 143 and 217GHz are provided in the Planck Legacy Archive with the following file structure: |

<span style="color:red">to be written by A. Moneti</span> | <span style="color:red">to be written by A. Moneti</span> | ||

− | They were obtained by Spice (run 1731634056805856210) with the Galactic and point sources | + | They were obtained by Spice (run 1731634056805856210) with the so-called Galactic mask2 apodized to 2degrees, and point sources mask apodized at 30arcmin |

− | + | combining the sources detected by HFI at any frequency between 100 and 353GHz with the SZ and ERCSC sources. | |

− | + | ||

− | + | The spectra, computed up to ell=3508, are corrected from the effect of the cut sky, and from the nominal beam window function and average pixel function. (Spice reference) | |

− | |||

The covariance matrix only describes the statistical correlation induced by the sample variance and cut sky, | The covariance matrix only describes the statistical correlation induced by the sample variance and cut sky, | ||

− | using the formalism described in Efstathiou ?? | + | using the formalism described in Efstathiou ??, also sketched in the appendix of P08 paper (likelihood), assuming the instrumental noise |

+ | to be white and uniform. | ||

[[Category:Mission science products]] | [[Category:Mission science products]] |

## Revision as of 16:01, 8 February 2013

## CMB angular power spectra[edit]

Auto and cross angular power spectra for the 13 detset maps available at 100, 143 and 217GHz are provided in the Planck Legacy Archive with the following file structure: to be written by A. Moneti

They were obtained by Spice (run 1731634056805856210) with the so-called Galactic mask2 apodized to 2degrees, and point sources mask apodized at 30arcmin combining the sources detected by HFI at any frequency between 100 and 353GHz with the SZ and ERCSC sources.

The spectra, computed up to ell=3508, are corrected from the effect of the cut sky, and from the nominal beam window function and average pixel function. (Spice reference)

The covariance matrix only describes the statistical correlation induced by the sample variance and cut sky, using the formalism described in Efstathiou ??, also sketched in the appendix of P08 paper (likelihood), assuming the instrumental noise to be white and uniform.

Cosmic Microwave background

(Planck) High Frequency Instrument

Sunyaev-Zel'dovich

Early Release Compact Source Catalog