Download
Planck component all sky maps.
Additional products of the 2013 release
Galactic Dust maps
Model of thermal dust emission : The model of the thermal dust emission is based on a modify black body fit to the data: I_nu = AxB_nu(T)xnu^beta where B_nu(T) is the Planck function for dust equilibrium temperature T, A is the amplitude of the MBB and beta the dust spectral index.
The dust optical depth at frequency nu is tau_nu = Axnu^beta The dust parameters provided are T, beta and tau_353.
They were obtained by fitting the Planck data at 353, 545 and 857 GHz together with the IRAS (IRIS) 100 micron data.
The MBB fit was performed using a chi-square minimization, assuming errors for each data point that include instrumental noise, calibration uncertainties and uncertainties on the zero level. Because of the known degeneracy between T and beta in the presence of noise, we produced a model of dust emission using data smoothed to 35 arcmin; at such resolution no systematic bias of the parameters is observed. The map of the spectral index beta at 35 arcmin was than used to fit the data for T and tau at 5 arcmin.
For the production of the E(B-V) map, we used Planck and IRAS data from which point sources in diffuse areas were removed to avoid contamination by galaxies. In the hypothesis of constant dust emission cross-section, the optical depth map tau_353 is proportional to dust column density. It can then be used to estimate E(B-V), also proportional to dust column density in the hypothesis of a constant differential absorption cross-section between the B and V bands.
Dust optical depth products :
- Dust optical depth at 353 GHz : Nside=2048, fwhm=5 arcmin, no units
- Dust reddening E(B-V) : Nside=2048, fwhm=5 arcmin, units=magnitude
- Dust temperature : Nside 2048, fwhm=5 arcmin, units=Kelvin
- Dust spectral index : Nside=2048, fwhm=35 arcmin, no units
Dust opacity map nside=2048 |
Multi-plane FITS file with maps of dust optical depth at 353 GHz, dust reddening E(B-V), dust temperature and spectral index. |
CO maps
The released Type 1 CO maps have been produced using the MILCA-b algorithm, Type 2 maps using a specific implementation of the Commander algorithm, and the Type 3 map using the full Commander-Ruler component separation pipeline. We provide Healpix maps with Nside=2048. For one transition, the CO velocity-integrated line signal map is given in K_RJ.km/s units. A conversion factor from this unit to the native unit of HFI maps (K_CMB) is provided in the header of the data files.
Four maps are given per transition and per type :
- The signal map
- The standard deviation map (same unit as the signal),
- A null test noise map (same unit as the signal) with similar statistical properties. It is made out of half the difference of half-ring maps.
- A mask map (0B or 1B) giving the regions (1B) where the CO measurement is not reliable because of some severe identified foreground contamination.
All products of a given type belong to a single file. Type 1 products have the native HFI resolution i.e. approximately 10, 5 and 5 arcminutes for the CO 1-0, 2-1, 3-2 transitions respectively. Type 2 products have a 15 arcminute resolution The Type 3 product has a 5.5 arcminute resolution.
Additional products of the 2018 release
CO maps
First 12CO(J=1-0) and 13CO(J=1-0) fullsky maps constructed from Planck detectors observing the sky in the 100 GHz channel. These maps have been build from the Planck release 2 data (Planck collaboration 2015 results I). Each map is provided in K.km/s at an angular resolution of 9.88' FWHM with its associated error-map and a null-map.
The 12CO map is calibrated accordingly to the Dame et al. (2001) CO survey.
The 13CO map is calibrated accordingly to the BU FCRAO GRS (Jackson et al. 2006).
A full description of these two maps is provided in Hurier 2019 : https://arxiv.org/abs/1903.11883
12CO map |
Map 12CO in nside=2048
Figure shows the signal map smoothed at 30 arcmin FWHM |
|
13CO map |
Map 13CO in nside=2048
Figure shows the signal map smoothed at 30 arcmin FWHM |