Difference between revisions of "Sky temperature maps"
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The cleaned and un-calibrated (in Watt) TOIs of each detector are first used to built Healpix rings. These are calibrated against the solar dipole, for the 100–353 GHz channels, and against FIRAS data for the 545–857 ones. | The cleaned and un-calibrated (in Watt) TOIs of each detector are first used to built Healpix rings. These are calibrated against the solar dipole, for the 100–353 GHz channels, and against FIRAS data for the 545–857 ones. | ||
==== Dipole calibration ==== | ==== Dipole calibration ==== | ||
| − | Gains are initially determined for each pointing period. These estimate are systematically biased by Galactic foregrounds. We average these gains over a time interval in the first survey where the Solar dipole amplitude is large enough to reduce these bias. For 100 to 217 GHz, evidence of apparent gain variations of order 1 to 2% over a few tens to thousands of pointing periods led us to adopt a more | + | Gains are initially determined for each pointing period. These estimate are systematically biased by Galactic foregrounds. We average these gains over a time interval in the first survey where the Solar dipole amplitude is large enough to reduce these bias. For 100 to 217 GHz, evidence of apparent gain variations of order 1 to 2% over a few tens to thousands of pointing periods led us to adopt a more sophisticated approach, where we determined relative gains |
for each pointing period, smoothed with a 50 pointing period width. | for each pointing period, smoothed with a 50 pointing period width. | ||
==== FIRAS calibration ==== | ==== FIRAS calibration ==== | ||
Revision as of 16:24, 9 October 2012
Introduction[edit]
Frequency maps produced by combining appropriately the data of several detectors over some period of the mission. They may be intensity only or polarized, meaning that they will consist of a set of three maps of I, Q, and U. These will be accompanied by a hit-count map and by a set of variance maps. The maps are packaged into a single BINTABLE extension; the structure of the FITS file is given in the FITS file structure section below. The FITS filenames are of the form {H|L}FI_fff_nnnn_yyyymmdd_{type}_{mission}.fits, where fff are three digits to indicated the Planck frequency band, and nnnn is the Healpix Nside of the map (2048 for HFI frequency, 1024 for LFI frequency), the optional type indicates the subset of input data used, and mission indicates the coverage period, i.e., full, nominal, or survey_n. A full list of products, by their names, is given in the List of products below.
HFI processing[edit]
The cleaned and un-calibrated (in Watt) TOIs of each detector are first used to built Healpix rings. These are calibrated against the solar dipole, for the 100–353 GHz channels, and against FIRAS data for the 545–857 ones.
Dipole calibration[edit]
Gains are initially determined for each pointing period. These estimate are systematically biased by Galactic foregrounds. We average these gains over a time interval in the first survey where the Solar dipole amplitude is large enough to reduce these bias. For 100 to 217 GHz, evidence of apparent gain variations of order 1 to 2% over a few tens to thousands of pointing periods led us to adopt a more sophisticated approach, where we determined relative gains for each pointing period, smoothed with a 50 pointing period width.
FIRAS calibration[edit]
At the higher frequencies, 545 and 857 GHz, calibration is map-based ; a constant gain is determined by fitting HFI data onto FIRAS ones, together with a zero-point (as FIRAS is absolutely calibrated). These zero point are apoplied for all frequencies to set them at the same scale.
Map-making[edit]
We use the destriping approach, where noise is modelled as the coaddition of a white noise component and one constant, aka offset, per pointing period which represent the low frequency 1/f noise. After subtraction these offsets, calibrated data are projected onto Healpix maps, with the data of each bolometer weighed by a factor of 1/NET of that bolometer.
Together with signal maps, hit count and variance maps are also produced. The hit maps indicate the (integer) number of valid TOI-level samples that contribute to the signal of each pixel. All valid samples are counted in the same way, i.e., there is no weighting factor applied. The variance maps project the white noise estimation, provided by the NET, in the sky domain. They give the covariance between the Stokes parameters I,Q andU inside each pixels, whenever polarization is reconstructed.
LFI processing[edit]
TBW
Types of maps[edit]
Full channel maps[edit]
Full channel maps are built using all the valid detectors of a frequency channel and cover the full mission (or the nominal mission for the 1st release). For HFI, the 143-8 and 545-3 bolometers are rejected entirely as they are seriously affected by RTS noise.
Single survey maps[edit]
Single survey maps are built using all valid detectors of a frequency channel, but cover separately the different sky surveys. The single sky surveys are defined in terms of the direction of the satellite's spin axis: the first survey covers from the beginning of the science observations (the First Light Survey) to the time when the spin axis has rotated by 180 degrees (to the nearest pointing period), the following ones covers from 180 to 360, and so on. In the case of the nominal mission, the process stops at the third survey, which is incomplete. In the case of the full mission the 4th survey was interrupted shortly before completing the 180 degree rotation (see LINK), in order to begin observing with a different scanning law. The HFI mission ended slightly before the natural end of the 5th survey, the LFI mission continued to the XXX survey. The coverage of each of these periods in terms of ring number, pointingID, and OD, is given in the table below. Note that the OD numbers are only to indicate during which OD the period boundary occurs.
| Name | Ini_OD | Ini_Ring | Ini_ptgID | End_OD | End_ring | End_ptgID |
|---|---|---|---|---|---|---|
| Nominal | 91 | 240 | 00004200 | 807 | 14724 | 04243900 |
| HFI-Full | 91 | 240 | 00004200 | 563 | 27008 | 06344800 |
| LFI-Full | 91 | 240 | 00004200 | TBD | TBD | TBD |
| SCAN1 | 91 | 240 | 00004200 | 270 | 5720 | 01059820 |
| SCAN2 | 270 | 5721 | 01059830 | 456 | 11194 | 02114520 |
| SCAN3-nom | 456 | 11195 | 02114530 | nnn | nnn | nnnn |
| SCAN3-full | 456 | 11195 | 02114530 | 636 | 16691 | 03193660 |
| SCAN4 | 636 | 16692 | 03193670 | 807 | 21720 | 04243990 |
| SCAN5 | 807 | 21721 | 95000020 | 974 | 27008 | 06344800 |
Detector-set maps[edit]
Detector-set (detset) maps are built for the full (or nominal) mission using a minimal set of detectors. This concept is applicable to polarization maps, which are built using 4 PSBs at the proper orientations. The HFI polarized channels are designed to provide 2 detsets (or quads) each, namely:
| 100–ds1: 100-1a,100-1b,100-4a,100-4b | 100–ds2: 100-2a,100-2b,100-3a,100-3b |
| 143–ds1: 143-1a,143-1b,143-3a,143-3b | 143–ds2: 143-2a,143-2b,143-4a,143-4b |
| 217–ds1: 217-5a,217-5b,217-7a,217-7b | 217–ds2: 217-6a,217-6b,217-8a,217-8b |
| 353–ds1: 353-5a,353-5b,353-3a,353-3b | 353–ds2: 353-6a,353-6b,353-4a,353-4b |
The LFI Detector-set maps are built using the horn in the same scanning row, namely:
| 18_23: 18M,18S,23M,23S |
| 19_22: 19M,19S,22M,22S |
| 20_21: 20M,20S,21M,21S |
| 24: 24M,24S |
| 25_26: 25M,25S,26M,26S |
Half-ring maps[edit]
Half-ring maps are built using only the first or the second half of the stable pointing period data. There are thus two half-ring maps per frequency channel named ringhalf_1 and ringhalf_2 respectively. These maps are built for characterization purposes in order to perform null tests.
List of products[edit]
First release[edit]
For the first release, all maps will be Intensity-only
- Full channel maps
LFI_030_2048_yyyymmdd_nominal.fits LFI_044_2048_yyyymmdd_nominal.fits LFI_070_2048_yyyymmdd_nominal.fits HFI_100_2048_yyyymmdd_nominal.fits HFI_143_2048_yyyymmdd_nominal.fits HFI_217_2048_yyyymmdd_nominal.fits HFI_353_2048_yyyymmdd_nominal.fits HFI_545_2048_yyyymmdd_nominal.fits HFI_857_2048_yyyymmdd_nominal.fits
- Single survey maps
LFI_030_2048_yyyymmdd_survey_1.fits LFI_030_2048_yyyymmdd_survey_2.fits LFI_030_2048_yyyymmdd_survey_3.fits LFI_044_2048_yyyymmdd_survey_1.fits LFI_044_2048_yyyymmdd_survey_2.fits LFI_044_2048_yyyymmdd_survey_3.fits LFI_070_2048_yyyymmdd_survey_1.fits LFI_070_2048_yyyymmdd_survey_2.fits LFI_070_2048_yyyymmdd_survey_3.fits HFI_100_2048_yyyymmdd_survey_1.fits HFI_100_2048_yyyymmdd_survey_2.fits HFI_100_2048_yyyymmdd_survey_3.fits HFI_143_2048_yyyymmdd_survey_1.fits HFI_143_2048_yyyymmdd_survey_2.fits HFI_143_2048_yyyymmdd_survey_3.fits HFI_217_2048_yyyymmdd_survey_1.fits HFI_217_2048_yyyymmdd_survey_2.fits HFI_217_2048_yyyymmdd_survey_3.fits HFI_353_2048_yyyymmdd_survey_1.fits HFI_353_2048_yyyymmdd_survey_2.fits HFI_353_2048_yyyymmdd_survey_3.fits HFI_545_2048_yyyymmdd_survey_1.fits HFI_545_2048_yyyymmdd_survey_2.fits HFI_545_2048_yyyymmdd_survey_3.fits HFI_857_2048_yyyymmdd_survey_1.fits HFI_857_2048_yyyymmdd_survey_2.fits HFI_857_2048_yyyymmdd_survey_3.fits
- Half-ring maps
LFI_030_2048_yyyymmdd_ringhalf_1_nominal.fits LFI_030_2048_yyyymmdd_ringhalf_2_nominal.fits LFI_044_2048_yyyymmdd_ringhalf_1_nominal.fits LFI_044_2048_yyyymmdd_ringhalf_2_nominal.fits LFI_070_2048_yyyymmdd_ringhalf_1_nominal.fits LFI_070_2048_yyyymmdd_ringhalf_2_nominal.fits HFI_100_2048_yyyymmdd_ringhalf_1_nominal.fits HFI_100_2048_yyyymmdd_ringhalf_2_nominal.fits HFI_143_2048_yyyymmdd_ringhalf_1_nominal.fits HFI_143_2048_yyyymmdd_ringhalf_2_nominal.fits HFI_217_2048_yyyymmdd_ringhalf_1_nominal.fits HFI_217_2048_yyyymmdd_ringhalf_2_nominal.fits HFI_353_2048_yyyymmdd_ringhalf_1_nominal.fits HFI_353_2048_yyyymmdd_ringhalf_2_nominal.fits HFI_545_2048_yyyymmdd_ringhalf_1_nominal.fits HFI_545_2048_yyyymmdd_ringhalf_2_nominal.fits HFI_857_2048_yyyymmdd_ringhalf_1_nominal.fits HFI_857_2048_yyyymmdd_ringhalf_2_nominal.fits
Second release[edit]
All the above + TBD, including polarization for the polarized frequency channels.
FITS file structure[edit]
The FITS file will have one of the following structures:
The exact order of the columns is indicative only, and the details will be given in the keywords. Keywords will also indicate the coordinate system (GALACTIC), the Healpix ordering scheme (NESTED), the units (K_cmb), and of course the detector. Details of the FITS file general structure can be found in the EFDD (ref), and the specifics of certain parameters in ICD-031 (ref)
Header keywords[edit]
A typical header for the data extension of an intensity only map is:
XTENSION= 'BINTABLE' / binary table extension BITPIX = 8 / 8-bit bytes NAXIS = 2 / 2-dimensional binary table NAXIS1 = 12 / width of table in bytes NAXIS2 = 50331648 / number of rows in table PCOUNT = 0 / size of special data area GCOUNT = 1 / one data group (required keyword) TFIELDS = 3 / number of fields in each row TTYPE1 = 'I_Stokes' / label for field 1 TFORM1 = '1E8 ' / data format of field: 4-byte REAL TUNIT1 = 'K_CMB ' / physical unit of field TTYPE2 = 'Hits ' / label for field 2 TFORM2 = '1J ' / data format of field: 4-byte INTEGER TUNIT2 = 'none ' / physical unit of field TTYPE3 = 'II_cov ' / label for field 3 TFORM3 = '1E8 ' / data format of field: 4-byte REAL TUNIT3 = '(K_CMB)^2' / physical unit of field EXTNAME = 'CH-MAP ' / name of this binary table extension FREQ = '857 ' PIXTYPE = 'HEALPIX ' COORDSYS= 'GALACTIC' ORDERING= 'NESTED ' FILENAME= 'HFI_857-2_2048_20120210_nominal.fits' NSIDE = 2048 CHANNEL = '857-2 ' FIRSTPIX= 0 LASTPIX = 50331647 EXTVER = '1 ' PROCVER = 'v50 ' BAD_DATA= '-1.63750E+30' COMMENT = 'Rel DR4 ' END
and for a polarized frequency map:
XTENSION= 'BINTABLE' / binary table extension BITPIX = 8 / 8-bit bytes NAXIS = 2 / 2-dimensional binary table NAXIS1 = 40 / width of table in bytes NAXIS2 = 50331648 / number of rows in table PCOUNT = 0 / size of special data area GCOUNT = 1 / one data group (required keyword) TFIELDS = 10 / number of fields in each row TTYPE1 = 'I_Stokes' / label for field 1 TFORM1 = '1E8 ' / data format of field: 4-byte REAL TUNIT1 = 'K_CMB ' / physical unit of field TTYPE2 = 'Q_Stokes' / label for field 2 TFORM2 = '1E8 ' / data format of field: 4-byte REAL TUNIT2 = 'K_CMB ' / physical unit of field TTYPE3 = 'U_Stokes' / label for field 3 TFORM3 = '1E8 ' / data format of field: 4-byte REAL TUNIT3 = 'K_CMB ' / physical unit of field TTYPE4 = 'Hits ' / label for field 4 TFORM4 = '1J ' / data format of field: 4-byte INTEGER TUNIT4 = 'none ' / physical unit of field TTYPE5 = 'II_cov ' / label for field 5 TFORM5 = '1E8 ' / data format of field: 4-byte REAL TUNIT5 = '(K_CMB)^2' / physical unit of field TTYPE6 = 'IQ_cov ' / label for field 6 TFORM6 = '1E8 ' / data format of field: 4-byte REAL TUNIT6 = '(K_CMB)^2' / physical unit of field TTYPE7 = 'IU_cov ' / label for field 7 TFORM7 = '1E8 ' / data format of field: 4-byte REAL TUNIT7 = '(K_CMB)^2' / physical unit of field TTYPE8 = 'QQ_cov ' / label for field 8 TFORM8 = '1E8 ' / data format of field: 4-byte REAL TUNIT8 = '(K_CMB)^2' / physical unit of field TTYPE9 = 'QU_cov ' / label for field 9 TFORM9 = '1E8 ' / data format of field: 4-byte REAL TUNIT9 = '(K_CMB)^2' / physical unit of field TTYPE10 = 'UU_cov ' / label for field 10 TFORM10 = '1E8 ' / data format of field: 4-byte REAL TUNIT10 = '(K_CMB)^2' / physical unit of field EXTNAME = 'FR-MAP ' / name of this binary table extension FREQ = '217 ' PIXTYPE = 'HEALPIX ' COORDSYS= 'GALACTIC' ORDERING= 'NESTED ' FILENAME= 'HFI_217_2048_20120210_nominal.fits' NSIDE = 2048 FIRSTPIX= 0 LASTPIX = 50331647 EXTVER = '1 ' PROCVER = 'v50 ' BAD_DATA= '-1.63750E+30' COMMENT = 'Rel DR4 ' END
Flexible Image Transfer Specification
(Planck) High Frequency Instrument
(Planck) Low Frequency Instrument
Noise Equivalent Temperature
random telegraphic signal
Operation Day definition is geometric visibility driven as it runs from the start of a DTCP (satellite Acquisition Of Signal) to the start of the next DTCP. Given the different ground stations and spacecraft will takes which station for how long, the OD duration varies but it is basically once a day.
To be defined / determined
Interface Control Document
Cosmic Microwave background
