Difference between revisions of "Astrophysical component maps"
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| + | == Overview == | ||
| + | This section describes the maps of astrophysical components produced from the Planck data. These products are derived from some or all of the nine frequency channel maps described above using different techniques and, in some cases, using other constraints from external data sets. Here we give a brief description of each product and how it is obtained, followed by a description of the FITS file containing the data and associated information. | ||
| + | All the details can be found in {{PlanckPapers|planck2014-a12}} and {PlanckPapers|planck20}}. | ||
| + | |||
== Astrophysical foregrounds from parametric component separation == | == Astrophysical foregrounds from parametric component separation == | ||
We describe diffuse foreground products for the Planck 2015 release. See the Planck Foregrounds Component Separation paper {{PlanckPapers|planck2014-a12}} for a detailed description of these products. Further scientific discussion and interpretation may be found in {{PlanckPapers|planck2014-a31}}. | We describe diffuse foreground products for the Planck 2015 release. See the Planck Foregrounds Component Separation paper {{PlanckPapers|planck2014-a12}} for a detailed description of these products. Further scientific discussion and interpretation may be found in {{PlanckPapers|planck2014-a31}}. | ||
Latest revision as of 08:49, 31 May 2016
Contents
Overview[edit]
This section describes the maps of astrophysical components produced from the Planck data. These products are derived from some or all of the nine frequency channel maps described above using different techniques and, in some cases, using other constraints from external data sets. Here we give a brief description of each product and how it is obtained, followed by a description of the FITS file containing the data and associated information. All the details can be found in Planck-2015-A10[1] and {PlanckPapers|planck20}}.
Astrophysical foregrounds from parametric component separation[edit]
We describe diffuse foreground products for the Planck 2015 release. See the Planck Foregrounds Component Separation paper Planck-2015-A10[1] for a detailed description of these products. Further scientific discussion and interpretation may be found in Planck-2015-A25[2].
Low-resolution temperature products[edit]
- The Planck 2015 astrophysical component separation analysis combines Planck observations with the 9-year WMAP temperature sky maps (Bennett et al. 2013) and the 408 MHz survey by Haslam et al. (1982). This allows a direct decomposition of the low-frequency foregrounds into separate synchrotron, free-free and spinning dust components without strong spatial priors.
Inputs[edit]
The following data products are used for the low-resolution analysis:
- Full-mission 30 GHz frequency map, LFI 30 GHz frequency maps
- Full-mission 44 GHz frequency map, LFI 44 GHz frequency maps
- Full-mission 70 GHz ds1 (18+23), ds2 (19+22), and ds3 (20+21) detector-set maps
- Full-mission 100 GHz ds1 and ds2 detector set maps
- Full-mission 143 GHz ds1 and ds2 detector set maps and detectors 5, 6, and 7 maps
- Full-mission 217 GHz detector 1, 2, 3 and 4 maps
- Full-mission 353 GHz detector set ds2 and detector 1 maps
- Full-mission 545 GHz detector 2 and 4 maps
- Full-mission 857 GHz detector 2 map
- Beam-symmetrized 9-year WMAP K-band map (Lambda)
- Beam-symmetrized 9-year WMAP Ka-band map (Lambda)
- Default 9-year WMAP Q1 and Q2 differencing assembly maps (Lambda)
- Default 9-year WMAP V1 and V2 differencing assembly maps (Lambda)
- Default 9-year WMAP W1, W2, W3, and W4 differencing assembly maps (Lambda)
- Re-processed 408 MHz survey map, Remazeilles et al. (2014) (Lambda)
All maps are smoothed to a common resolution of 1 degree FWHM by deconvolving their original instrumental beam and pixel window, and convolving with the new common Gaussian beam, and repixelizing at Nside=256.
Outputs[edit]
Synchrotron emission[edit]
- File name: COM_CompMap_Synchrotron-commander_0256_R2.00.fits
- Reference frequency: 408 MHz
- Nside = 256
- Angular resolution = 60 arcmin
| Column Name | Data Type | Units | Description |
|---|---|---|---|
| I_ML | Real*4 | uK_RJ | Amplitude posterior maximum |
| I_MEAN | Real*4 | uK_RJ | Amplitude posterior mean |
| I_RMS | Real*4 | uK_RJ | Amplitude posterior rms |
| Column Name | Data Type | Units | Description |
|---|---|---|---|
| nu | Real*4 | Hz | Frequency |
| intensity | Real*4 | W/Hz/m2/sr | GALPROP z10LMPD_SUNfE spectrum |
Free-free emission[edit]
- File name: COM_CompMap_freefree-commander_0256_R2.00.fits
- Reference frequency: NA
- Nside = 256
- Angular resolution = 60 arcmin
| Column Name | Data Type | Units | Description |
|---|---|---|---|
| EM_ML | Real*4 | cm^-6 pc | Emission measure posterior maximum |
| EM_MEAN | Real*4 | cm^-6 pc | Emission measure posterior mean |
| EM_RMS | Real*4 | cm^-6 pc | Emission measure posterior rms |
| TEMP_ML | Real*4 | K | Electron temperature posterior maximum |
| TEMP_MEAN | Real*4 | K | Electron temperature posterior mean |
| TEMP_RMS | Real*4 | K | Electron temperature posterior rms |
Spinning dust emission[edit]
- File name: COM_CompMap_AME-commander_0256_R2.00.fits
- Nside = 256
- Angular resolution = 60 arcmin
Note: The spinning dust component has two independent constituents, each corresponding to one spdust2 component, but with different peak frequencies. The two components are stored in the two first FITS extensions, and the template frequency spectrum is stored in the third extension.
- Reference frequency: 22.8 GHz
| Column Name | Data Type | Units | Description |
|---|---|---|---|
| I_ML | Real*4 | uK_RJ | Primary amplitude posterior maximum |
| I_MEAN | Real*4 | uK_RJ | Primary amplitude posterior mean |
| I_RMS | Real*4 | uK_RJ | Primary amplitude posterior rms |
| FREQ_ML | Real*4 | GHz | Primary peak frequency posterior maximum |
| FREQ_MEAN | Real*4 | GHz | Primary peak frequency posterior mean |
| FREQ_RMS | Real*4 | GHz | Primary peak frequency posterior rms |
- Reference frequency: 41.0 GHz
- Peak frequency: 33.35 GHz
| Column Name | Data Type | Units | Description |
|---|---|---|---|
| I_ML | Real*4 | uK_RJ | Secondary amplitude posterior maximum |
| I_MEAN | Real*4 | uK_RJ | Secondary amplitude posterior mean |
| I_RMS | Real*4 | uK_RJ | Secondary amplitude posterior rms |
| Column Name | Data Type | Units | Description |
|---|---|---|---|
| nu | Real*4 | GHz | Frequency |
| j_nu/nH | Real*4 | Jy sr-1 cm2/H | spdust2 spectrum |
CO line emission[edit]
- File name: COM_CompMap_CO-commander_0256_R2.00.fits
- Nside = 256
- Angular resolution = 60 arcmin
Note: The CO line emission component has three independent objects, corresponding to the J1->0, 2->1 and 3->2 lines, stored in separate extensions.
| Column Name | Data Type | Units | Description |
|---|---|---|---|
| I_ML | Real*4 | K_RJ km/s | CO(1-0) amplitude posterior maximum |
| I_MEAN | Real*4 | K_RJ km/s | CO(1-0) amplitude posterior mean |
| I_RMS | Real*4 | K_RJ km/s | CO(1-0) amplitude posterior rms |
| Column Name | Data Type | Units | Description |
|---|---|---|---|
| I_ML | Real*4 | K_RJ km/s | CO(2-1) amplitude posterior maximum |
| I_MEAN | Real*4 | K_RJ km/s | CO(2-1) amplitude posterior mean |
| I_RMS | Real*4 | K_RJ km/s | CO(2-1) amplitude posterior rms |
| Column Name | Data Type | Units | Description |
|---|---|---|---|
| I_ML | Real*4 | K_RJ km/s | CO(3-2) amplitude posterior maximum |
| I_MEAN | Real*4 | K_RJ km/s | CO(3-2) amplitude posterior mean |
| I_RMS | Real*4 | K_RJ km/s | CO(3-2) amplitude posterior rms |
94/100 GHz line emission[edit]
- File name: COM_CompMap_xline-commander_0256_R2.00.fits
- Nside = 256
- Angular resolution = 60 arcmin
| Column Name | Data Type | Units | Description |
|---|---|---|---|
| I_ML | Real*4 | uK_cmb | Amplitude posterior maximum |
| I_MEAN | Real*4 | uK_cmb | Amplitude posterior mean |
| I_RMS | Real*4 | uK_cmb | Amplitude posterior rms |
Note: The amplitude of this component is normalized according to the 100-ds1 detector set map, ie., it is the amplitude as measured by this detector combination.
Thermal dust emission[edit]
- File name: COM_CompMap_dust-commander_0256_R2.00.fits
- Nside = 256
- Angular resolution = 60 arcmin
- Reference frequency: 545 GHz
| Column Name | Data Type | Units | Description |
|---|---|---|---|
| I_ML | Real*4 | uK_RJ | Amplitude posterior maximum |
| I_MEAN | Real*4 | uK_RJ | Amplitude posterior mean |
| I_RMS | Real*4 | uK_RJ | Amplitude posterior rms |
| TEMP_ML | Real*4 | K | Dust temperature posterior maximum |
| TEMP_MEAN | Real*4 | K | Dust temperature posterior mean |
| TEMP_RMS | Real*4 | K | Dust temperature posterior rms |
| BETA_ML | Real*4 | NA | Emissivity index posterior maximum |
| BETA_MEAN | Real*4 | NA | Emissivity index posterior mean |
| BETA_RMS | Real*4 | NA | Emissivity index posterior rms |
Thermal Sunyaev-Zeldovich emission around the Coma and Virgo clusters[edit]
- File name: COM_CompMap_SZ-commander_0256_R2.00.fits
- Nside = 256
- Angular resolution = 60 arcmin
| Column Name | Data Type | Units | Description |
|---|---|---|---|
| Y_ML | Real*4 | y_SZ | Y parameter posterior maximum |
| Y_MEAN | Real*4 | y_SZ | Y parameter posterior mean |
| Y_RMS | Real*4 | y_SZ | Y parameter posterior rms |
High-resolution temperature products[edit]
High-resolution foreground products at 7.5 arcmin FWHM are derived with the same algorithm as for the low-resolution analyses, but including frequency channels above (and including) 143 GHz.
Inputs[edit]
The following data products are used for the low-resolution analysis:
- Full-mission 143 GHz ds1 and ds2 detector set maps and detectors 5, 6, and 7 maps
- Full-mission 217 GHz detector 1, 2, 3 and 4 maps
- Full-mission 353 GHz detector set ds2 and detector 1 maps
- Full-mission 545 GHz detector 2 and 4 maps
- Full-mission 857 GHz detector 2 map
All maps are smoothed to a common resolution of 7.5 arcmin FWHM by deconvolving their original instrumental beam and pixel window, and convolving with the new common Gaussian beam, and repixelizing at Nside=2048.
Outputs[edit]
CO J2->1 emission[edit]
- File name: COM_CompMap_CO21-commander_2048_R2.00.fits
- Nside = 2048
- Angular resolution = 7.5 arcmin
| Column Name | Data Type | Units | Description |
|---|---|---|---|
| I_ML_FULL | Real*4 | K_RJ km/s | Full-mission amplitude posterior maximum |
| I_ML_HM1 | Real*4 | K_RJ km/s | First half-mission amplitude posterior maximum |
| I_ML_HM2 | Real*4 | K_RJ km/s | Second half-mission amplitude posterior maximum |
| I_ML_HR1 | Real*4 | K_RJ km/s | First half-ring amplitude posterior maximum |
| I_ML_HR2 | Real*4 | K_RJ km/s | Second half-ring amplitude posterior maximum |
| I_ML_YR1 | Real*4 | K_RJ km/s | "First year" amplitude posterior maximum |
| I_ML_YR2 | Real*4 | K_RJ km/s | "Second year" amplitude posterior maximum |
Thermal dust emission[edit]
- File name: COM_CompMap_ThermalDust-commander_2048_R2.00.fits
- Nside = 2048
- Angular resolution = 7.5 arcmin
- Reference frequency: 545 GHz
| Column Name | Data Type | Units | Description |
|---|---|---|---|
| I_ML_FULL | Real*4 | uK_RJ | Full-mission amplitude posterior maximum |
| I_ML_HM1 | Real*4 | uK_RJ | First half-mission amplitude posterior maximum |
| I_ML_HM2 | Real*4 | uK_RJ | Second half-mission amplitude posterior maximum |
| I_ML_HR1 | Real*4 | uK_RJ | First half-ring amplitude posterior maximum |
| I_ML_HR2 | Real*4 | uK_RJ | Second half-ring amplitude posterior maximum |
| I_ML_YR1 | Real*4 | uK_RJ | "First year" amplitude posterior maximum |
| I_ML_YR2 | Real*4 | uK_RJ | "Second year" amplitude posterior maximum |
| BETA_ML_FULL | Real*4 | NA | Full-mission emissivity index posterior maximum |
| BETA_ML_HM1 | Real*4 | NA | First half-mission emissivity index posterior maximum |
| BETA_ML_HM2 | Real*4 | NA | Second half-mission emissivity index posterior maximum |
| BETA_ML_HR1 | Real*4 | NA | First half-ring emissivity index posterior maximum |
| BETA_ML_HR2 | Real*4 | NA | Second half-ring emissivity index posterior maximum |
| BETA_ML_YR1 | Real*4 | NA | "First year" emissivity index posterior maximum |
| BETA_ML_YR2 | Real*4 | NA | "Second year" emissivity index posterior maximum |
Polarization products[edit]
Two polarization foreground products are provided, namely synchrotron and thermal dust emission. The spectral models are assumed identical to the corresponding temperature spectral models.
Inputs[edit]
The following data products are used for the polarization analysis:
- (Only low-resolution analysis) Full-mission 30 GHz frequency map, LFI 30 GHz frequency maps
- (Only low-resolution analysis) Full-mission 44 GHz frequency map, LFI 44 GHz frequency maps
- (Only low-resolution analysis) Full-mission 70 GHz frequency map, LFI 70 GHz frequency maps
- Full-mission 100 GHz frequency map, HFI 100 GHz frequency maps
- Full-mission 143 GHz frequency map, HFI 143 GHz frequency maps
- Full-mission 217 GHz frequency map, HFI 217 GHz frequency maps
- Full-mission 353 GHz frequency map, HFI 353 GHz frequency maps
In the low-resolution analysis, all maps are smoothed to a common resolution of 40 arcmin FWHM by deconvolving their original instrumental beam and pixel window, and convolving with the new common Gaussian beam, and repixelizing at Nside=256. In the high-resolution analysis (including only CMB and thermal dust emission), the corresponding resolution is 10 arcmin FWHM and Nside=1024.
Outputs[edit]
Synchrotron emission[edit]
- File name: COM_CompMap_SynchrotronPol-commander_0256_R2.00.fits
- Nside = 256
- Angular resolution = 40 arcmin
- Reference frequency: 30 GHz
| Column Name | Data Type | Units | Description |
|---|---|---|---|
| Q_ML_FULL | Real*4 | K_RJ km/s | Full-mission Stokes Q posterior maximum |
| U_ML_FULL | Real*4 | K_RJ km/s | Full-mission Stokes U posterior maximum |
| Q_ML_HM1 | Real*4 | K_RJ km/s | First half-mission Stokes Q posterior maximum |
| U_ML_HM1 | Real*4 | K_RJ km/s | First half-mission Stokes U posterior maximum |
| Q_ML_HM2 | Real*4 | K_RJ km/s | Second half-mission Stokes Q posterior maximum |
| U_ML_HM2 | Real*4 | K_RJ km/s | Second half-mission Stokes U posterior maximum |
| Q_ML_HR1 | Real*4 | K_RJ km/s | First half-ring Stokes Q posterior maximum |
| U_ML_HR1 | Real*4 | K_RJ km/s | First half-ring Stokes U posterior maximum |
| Q_ML_HR2 | Real*4 | K_RJ km/s | Second half-ring Stokes Q posterior maximum |
| U_ML_HR2 | Real*4 | K_RJ km/s | Second half-ring Stokes U posterior maximum |
| Q_ML_YR1 | Real*4 | K_RJ km/s | "First year" Stokes Q posterior maximum |
| U_ML_YR1 | Real*4 | K_RJ km/s | "First year" Stokes U posterior maximum |
| Q_ML_YR2 | Real*4 | K_RJ km/s | "Second year" Stokes Q posterior maximum |
| U_ML_YR2 | Real*4 | K_RJ km/s | "Second year" Stokes U posterior maximum |
Thermal dust emission[edit]
- File name: COM_CompMap_DustPol-commander_1024_R2.00.fits
- Nside = 1024
- Angular resolution = 10 arcmin
- Reference frequency: 353 GHz
| Column Name | Data Type | Units | Description |
|---|---|---|---|
| Q_ML_FULL | Real*4 | uK_RJ | Full-mission Stokes Q posterior maximum |
| U_ML_FULL | Real*4 | uK_RJ | Full-mission Stokes U posterior maximum |
| Q_ML_HM1 | Real*4 | uK_RJ | First half-mission Stokes Q posterior maximum |
| U_ML_HM1 | Real*4 | uK_RJ | First half-mission Stokes U posterior maximum |
| Q_ML_HM2 | Real*4 | uK_RJ | Second half-mission Stokes Q posterior maximum |
| U_ML_HM2 | Real*4 | uK_RJ | Second half-mission Stokes U posterior maximum |
| Q_ML_HR1 | Real*4 | uK_RJ | First half-ring Stokes Q posterior maximum |
| U_ML_HR1 | Real*4 | uK_RJ | First half-ring Stokes U posterior maximum |
| Q_ML_HR2 | Real*4 | uK_RJ | Second half-ring Stokes Q posterior maximum |
| U_ML_HR2 | Real*4 | uK_RJ | Second half-ring Stokes U posterior maximum |
| Q_ML_YR1 | Real*4 | uK_RJ | "First year" Stokes Q posterior maximum |
| U_ML_YR1 | Real*4 | uK_RJ | "First year" Stokes U posterior maximum |
| Q_ML_YR2 | Real*4 | uK_RJ | "Second year" Stokes Q posterior maximum |
| U_ML_YR2 | Real*4 | uK_RJ | "Second year" Stokes U posterior maximum |
Modelling of the thermal dust emission with the Draine and Li dust model[edit]
The Planck, IRAS, and WISE infrared observations were fit with the dust model presented by Draine & Li in 2007 (DL07). The input maps, the DL07 model, and the fitting procedure and results are presented in Planck-2014-XXIX[3]. Here, we describe the input maps and the output maps, which are made available on the Planck Legacy Archive.
Inputs[edit]
The following data have been fit:
- WISE 12 micron map
- IRAS 60 micron map
- IRAS 100 micron map
- Full-mission 353 GHz PR2 map
- Full-mission 545 GHz PR2 map
- Full-mission 857 GHz PR2 map
The CIB monopole, the CMB anisotropries and the zodiacal light were subtracted to obtain dust emission maps from the sky emission maps. All maps were smoothed to a common angular resolution of 5'.
Model Parameters[edit]
For each pixel of the inputs maps, we have fitted four parameters of the DL07 model:
- the dust mass surface density, Sigma_Mdust,
- the dust mass fraction in small PAH grains, q_PAH,
- the fraction of the total luminosity from dust heated by intense radiation fields, f_PDR,
- the starlight intensity heating the bulk of the dust, U_min.
The parameter maps and their uncertainties are gathered in one file. This file also includes the chi2 of the fit per degree of freedom.
- File name: COM_CompMap_Dust-DL07-Parameters_2048_R2.00.fits
- Nside = 2048
- Angular resolution = 5 arcmin
| Column Name | Data Type | Units | Description |
|---|---|---|---|
| Sigma_Mdust | Real*4 | Solar masses/kpc^2 | Dust mass surface density |
| Sigma_Mdust_unc | Real*4 | Solar masses/kpc^2 | Uncertainty (1 sigma) on Sigma_Mdust |
| q_PAH | Real*4 | dimensionless | Dust mass fraction in small PAH grains |
| q_PAH_unc | Real*4 | dimensionless | Uncertainty (1 sigma) on q_PAH |
| f_PDR | Real*4 | dimensionless | Fraction of the total luminosity from dust heated by intense radiation fields |
| f_PDR_unc | Real*4 | dimensionless | Uncertainty (1 sigma) on f_PDR |
| U_min | Real*4 | dimensionless | Starlight intensity heating the bulk of the dust |
| U_min_unc | Real*4 | dimensionless | Uncertainty (1 sigma) on U_min |
| Chi2_DOF | Real*4 | dimensionless | Chi2 of the fit per degree of freedom |
Visible extinction maps[edit]
We provide two exinctions maps at the visible V band: the value from the model (Av_DL) and the renormalized one (Av_RQ) that matches extinction estimates for quasars (QSOs) derived from the Sloan digital sky survey (SDSS) data.
- File name: COM_CompMap_Dust-DL07-AvMaps_2048_R2.00.fits
- Nside = 2048
- Angular resolution = 5 arcmin
| Column Name | Data Type | Units | Description |
|---|---|---|---|
| Av_DL | Real*4 | magnitude | Extinction in the V band from the DL model |
| Av_DL_unc | Real*4 | magnitude | Uncertainty (1 sigma) on Av_DL |
| Av_RQ | Real*4 | magnitude | Extinction in the V band renormalized to match estimates from QSO SDSS observations |
| Av_RQ_unc | Real*4 | magnitude | Uncertainty (1 sigma) on Av_RQ |
Model Fluxes[edit]
We provide the model predicted fluxes in the following file.
- File name: COM_CompMap_Dust-DL07-ModelFluxes_2048_R2.00.fits
- Nside = 2048
- Angular resolution = 5 arcmin
| Column Name | Data Type | Units | Description |
|---|---|---|---|
| Planck_857 | Real*4 | MJy/sr | Model flux in the Planck 857 GHz band |
| Planck_545 | Real*4 | MJy/sr | Model flux in the Planck 545 GHz band |
| Planck_353 | Real*4 | MJy/sr | Model flux in the Planck 353 GHz band |
| WISE_12 | Real*4 | MJy/sr | Model flux in the WISE 12 micron band |
| IRAS_60 | Real*4 | MJy/sr | Model flux in the IRAS 60 micron band |
| IRAS_100 | Real*4 | MJy/sr | Model flux in the IRAS 100 micron band |
References[edit]
- ↑ 1.01.1 Planck 2015 results. X. Diffuse component separation: Foreground maps, Planck Collaboration, 2016, A&A, 594, A10.
- ↑ Planck 2015 results. XXV. Diffuse low frequency Galactic foregrounds, Planck Collaboration, 2016, A&A, 594, A25.
- ↑ Planck intermediate results. XXIX. All-sky dust modelling with Planck, IRAS, and WISE observations', Planck Collaboration Int. XXIX, A&A, 586, A132, (2016).
Flexible Image Transfer Specification
Full-Width-at-Half-Maximum
Sunyaev-Zel'dovich
Cosmic Microwave background
