https://wiki.cosmos.esa.int/planckpla2015/api.php?action=feedcontributions&user=Dhanson&feedformat=atomPlanck PLA 2015 Wiki - User contributions [en-gb]2022-12-10T09:09:47ZUser contributionsMediaWiki 1.31.6https://wiki.cosmos.esa.int/planckpla2015/index.php?title=Simulation_data&diff=10100Simulation data2014-12-14T20:53:21Z<p>Dhanson: /* Lensing Simulations */</p>
<hr />
<div>The simulation data can be downloaded from the PLA Java interface (Windows -> Supplementary Data).<br />
<br />
== Introduction ==<br />
The 2013 Planck data release is supported by a set of simulated maps of the model sky, by astrophysical component, and of that sky as seen by Planck. The simulation process consists of <br />
# modeling each astrophysical component of the sky emission for each Planck detector, using pre-Planck data and the relevant characteristics of the Planck instruments (namely the detector plus filter transmissions curves). <br />
# simulating each detector's observation of each sky component following the Planck scanning strategy and using the best estimates of the detector's beam and noise properties (now obtained in flight), then combining these timelines into a single one per detector, and projecting these simulated timelines onto ''observed'' maps (the ''fiducial'' sky), as is done with the on-orbit data;<br />
# generating Monte Carlo realizations of the CMB and of the noise, again following the Planck scanning strategy and using our best estimates of the detector beams and noise properties respectively. <br />
The first step is performed by the ''Planck Sky Model'' (PSM), and the last two by the ''Planck Simulation Tools'' (PST), both of which are described in the sections below. <br />
<br />
The production of a full focal plane (FFP) simulation, and including the many MC realizations of the CMB and the noise, requires both HFI and LFI data and includes large, computationally challenging, MC realizations. They are too large to be generated on either of the DPC's own cluster. Instead the PST consists of three distinct tools, each designed to run on the largest available supercomputers, that are used to generate the fiducial sky realization, the CMB MC, and the noise MC respectively. The simulations delivered here are part of the 6th generation FFP simulations, known as FFP6. They were primarily generated on the Hopper and Edison systems at [http://www.nersc.gov NERSC], with some of the LFI noise MCs generated on the Louhi system at [http://www.csc.fi/english CSC].<br />
<br />
While FFP6 includes our best measurements of the detector band-passes, main beams and noise power spectral densities, and is guaranteed to be internally self-consistent, there are a number of differences with the real data that should be borne in mind, although all tests performed to date indicate that these are statistically insignificant:<br />
* the beams do not include far side-lobes;<br />
* the detector noise characteristics are assumed stable: a single noise spectrum per detector is used for the entire mission;<br />
* it assumes perfect calibration, transfer function deconvolution and deglitching;<br />
* it uses the HFI pointing solution for the LFI frequencies, rather than the DPC's two focal plane model.<br />
* it uses a different map-maker to HFI, and as a consequence implements very slightly different data cuts - primarily at ring boundaries - resulting in marginally different hit-maps.<br />
<br />
== The Planck Sky Model ==<br />
=== Overall description ===<br />
<br />
The Planck Sky Model, PSM, consists of a set of data and of code used to simulate sky emission at millimeter-wave frequencies; it is described in detail in Delabrouille et al., (2013){{BibCite|delabrouille2012}}, henceforth the PSM paper..<br />
<br />
The Planck Sky Model is available here:<br />
http://www.apc.univ-paris7.fr/~delabrou/PSM/psm.html<br />
<br />
The main simulations used to test and validate the Planck data analysis pipelines (and, in particular, component separation) makes use of simulations generated with version 1.7.7 of the PSM software. The total sky emission is built from the CMB plus ten foreground components, namely thermal dust, spinning dust, synchrotron, CO lines, free-free, thermal Sunyaev-Zel'dovich (SZ) effect (with first order relativistic corrections), kinetic SZ effect, radio and infrared sources, Cosmic Infrared Background (CIB).<br />
<br />
The CMB is modeled using [http://camb.info CAMB]. It is based on adiabatic initial perturbations, with the following cosmological parameters:<br />
* T_CMB = 2.725<br />
* H = 0.684<br />
* OMEGA_M = 0.292<br />
* OMEGA_B = 0.04724<br />
* OMEGA_NU = 0<br />
* OMEGA_K = 0<br />
* SIGMA_8 = 0.789<br />
* N_S = 0.9732<br />
* N_S_RUNNING = 0<br />
* N_T = 0<br />
* R = 0.0844<br />
* TAU_REION = 0.085<br />
* HE_FRACTION = 0.245<br />
* N_MASSLESS_NU = 3.04<br />
* N_MASSIVE_NU = 0<br />
* W_DARK_ENERGY = -1<br />
* K_PIVOT = 0.002<br />
* SCALAR_AMPLITUDE = 2.441e-9<br />
and all other parameters are set to the default standard of the Jan 2012 version of CAMB. In addition, this simulated CMB contains non-Gaussian corrections of the local type, with an f<sub>NL</sub> parameter of 20.4075.<br />
<br />
The Galactic ISM emission comprises five components: thermal dust, spinning dust, synchrotron, CO lines, and free-free emission. We refer the reader to the PSM publication for details. For the simulations generated here, however, the thermal dust model has been modified in the following way: instead of being based on the 100 micron map of Schlegel, Finkbeiner and Davis (2008){{BibCite|schlegel1998}}, henceforth SFB, the dust template uses an internal release of the 857 GHz Planck observed map itself, in which point sources have been subtracted, and which has been locally filtered to remove CIB fluctuations in the regions of lowest column density. A caveat is that while this reduces the level of CIB fluctuations in the dust map in some of the regions, in regions of moderate dust column density the CIB contamination is actually somewhat larger than in the SFD map (by reason of different emission laws for dust and CIB, and of the higher resolution of the Planck map).<br />
<br />
The other emissions of the galactic ISM are simulated using the prescription described in the PSM paper. Synchrotron, free-free and spinning dust emission are based on WMAP observations, as analyzed by Miville-Deschenes et al. (2008){{BibCite|Miville2008}}. Small scale fluctuations have been added to increase the variance on small scales and compensate the lower resolution of WMAP as compared to Planck (in particular for the HFI channels). The main limitation of these maps is the presence at high galactic latitude of fluctuations that may be attributed to WMAP noise. The presence of noise and of added Gaussian fluctuations on small scales may result in a few occasional pixels being negative (e.g. in the spinning dust maps). Low frequency foreground maps are also contaminated by some residuals of bright radio sources that have not been properly subtracted from the templates of diffuse emission.<br />
<br />
The CO maps are simulated using the CO J=1-0 observations of Dame et al. (2001){{BibCite|dame2001}}. The main limitations are limited sky coverage, lower resolution than that of Planck high frequency channels, line ratios (J=2-1)/(J=1-0) and (J=3-2)/(J=2-1) constant over the sky. The CO in the simulation is limited to the three lowest <sup>12</sup>CO lines. No CO maps has been simulated at the LFI frequnecy (30, 44 and 70 GHz).<br />
<br />
Galaxy clusters are generated on the basis of cluster number counts, following the Tinker et al. (2008){{BibCite|Tinker2008}} mass function, for the cosmological parameters listed above. Clusters are assumed perfectly spherical, isothermal, and are modeled using the universal pressure profile of Arnaud et al. (2010){{BibCite|arnaud2010}}. Relativistic corrections following Itoh et al. (1998){{BibCite|Nozawa1998}} are included to first order. The simulated kinetic SZ effect assumes no bulk flow, and a redshift-dependent average cluster velocity compatible with the linear growth of structures.<br />
<br />
Point sources comprise radio sources (based on extrapolations across frequencies of radio observations between 800 MHz and 5 GHz) and infrared sources (based on extrapolations in frequencies of IRAS sources). One caveat is that due to the unevenness of the radio source surveys, the equatorial southern part of the sky has less faint radio sources than the northern part. Although all the missing sources are well below the Planck detection level, this induces a small variation of the total emission background over the sky. Check the individual faint point source emission maps if this is a potential problem for your applications. See also the PSM paper for details about the PSM point source simulations. The PSM separates bright and faint point source; the former are initially in a catalog, and the latter in a map, though a map of the former can also be produced. In the processing below, the bright sources are simulated via the catalog, but for convenience they are delivered as a map.<br />
<br />
Finally, the far infrared background due to high redshift galaxies has been simulated using a procedure is based on the distribution of galaxies in shells of density contrast at various redshifts (Castex et al., PhD thesis; paper in preparation). This simulation has been modified by gradually substituting an uncorrelated extra term of CIB emission at low frequencies, artificially added in particular to decorrelate the CIB at frequencies below 217 GHz from the CIB above that frequency, to mimic the apparent decorrelation observed in the Planck Early Paper on CIB power spectrum ({{PlanckPapers|planck2011-6-6}}). <br />
<br />
While the PSM simulations described here provide a reasonably representative multi-component model of sky emission, users are warned that it has been put together mostly on the basis of data sets and knowledge pre-existing the Planck observations themselves. While it is sophisticated enough to include variations of emission laws of major components of the ISM emission, different emission laws for most sources, and a reasonably coherent global picture, it is not (and is not supposed to be) identical to the real sky emission. The users are warned to use these simulations with caution.<br />
<br />
=== PSM Products ===<br />
<br />
To build maps corresponding to the Planck channels, the models described above are convolved with the [[Spectral_response | spectral response]] of the channel in question. The products given here are for the full frequency channels, and as such they are not used in the Planck specific simulations, which use only individual detector channels. The frequency channel spectral responses used (given in [[the RIMO|the RIMO]]), are averages of the responses of the detectors of each frequency channel weighted as they are in the mapmaking step. They are provided for the purpose of testing user's own software of simulations and component separation.<br />
<br />
PSM maps of the CMB and of the ten foregrounds are given in the following map products:<br />
<br />
HFI<br />
* ''{{PLASingleFile | fileType=file | name=HFI_SimMap_cmb_2048_R1.10.fits | link=HFI_SimMap_cmb_2048_R1.10.fits}}''<br />
* ''{{PLASingleFile | fileType=file | name=HFI_SimMap_co_2048_R1.10.fits | link=HFI_SimMap_co_2048_R1.10.fits}}''<br />
* ''{{PLASingleFile | fileType=file | name=HFI_SimMap_firb_2048_R1.10.fits | link=HFI_SimMap_firb_2048_R1.10.fits}}''<br />
* ''{{PLASingleFile | fileType=file | name=HFI_SimMap_strongps_2048_R1.10.fits | link=HFI_SimMap_strongps_2048_R1.10.fits}}''<br />
* ''{{PLASingleFile | fileType=file | name=HFI_SimMap_faintps_2048_R1.10.fits | link=HFI_SimMap_faintps_2048_R1.10.fits}}''<br />
* ''{{PLASingleFile | fileType=file | name=HFI_SimMap_freefree_2048_R1.10.fits | link=HFI_SimMap_freefree_2048_R1.10.fits}}''<br />
* ''{{PLASingleFile | fileType=file | name=HFI_SimMap_synchrotron_2048_R1.10.fits | link=HFI_SimMap_synchrotron_2048_R1.10.fits}}''<br />
* ''{{PLASingleFile | fileType=file | name=HFI_SimMap_thermaldust_2048_R1.10.fits | link=HFI_SimMap_thermaldust_2048_R1.10.fits}}''<br />
* ''{{PLASingleFile | fileType=file | name=HFI_SimMap_spindust_2048_R1.10.fits | link=HFI_SimMap_spindust_2048_R1.10.fits}}''<br />
* ''{{PLASingleFile | fileType=file | name=HFI_SimMap_kineticsz_2048_R1.10.fits | link=HFI_SimMap_kineticsz_2048_R1.10.fits}}''<br />
* ''{{PLASingleFile | fileType=file | name=HFI_SimMap_thermalsz_2048_R1.10.fits | link=HFI_SimMap_thermalsz_2048_R1.10.fits}}'' <br />
<br />
LFI<br />
* ''{{PLASingleFile | fileType=file | name=LFI_SimMap_cmb_1024_R1.10.fits | link=LFI_SimMap_cmb_1024_R1.10.fits}}''<br />
* ''{{PLASingleFile | fileType=file | name=LFI_SimMap_firb_1024_R1.10.fits | link=LFI_SimMap_firb_1024_R1.10.fits}}''<br />
* ''{{PLASingleFile | fileType=file | name=LFI_SimMap_strongps_1024_R1.10.fits | link=LFI_SimMap_strongps_1024_R1.10.fits}}''<br />
* ''{{PLASingleFile | fileType=file | name=LFI_SimMap_faintps_1024_R1.10.fits | link=LFI_SimMap_faintps_1024_R1.10.fits}}''<br />
* ''{{PLASingleFile | fileType=file | name=LFI_SimMap_freefree_1024_R1.10.fits | link=LFI_SimMap_freefree_1024_R1.10.fits}}''<br />
* ''{{PLASingleFile | fileType=file | name=LFI_SimMap_synchrotron_1024_R1.10.fits | link=LFI_SimMap_synchrotron_1024_R1.10.fits}}''<br />
* ''{{PLASingleFile | fileType=file | name=LFI_SimMap_thermaldust_1024_R1.10.fits | link=LFI_SimMap_thermaldust_1024_R1.10.fits}}''<br />
* ''{{PLASingleFile | fileType=file | name=LFI_SimMap_spindust_1024_R1.10.fits | link=LFI_SimMap_spindust_1024_R1.10.fits}}''<br />
* ''{{PLASingleFile | fileType=file | name=LFI_SimMap_kineticsz_1024_R1.10.fits | link=LFI_SimMap_kineticsz_1024_R1.10.fits}}''<br />
* ''{{PLASingleFile | fileType=file | name=LFI_SimMap_thermalsz_1024_R1.10.fits | link=LFI_SimMap_thermalsz_1024_R1.10.fits}}'' <br />
<br />
<br />
Each file contains a single ''BINTABLE'' extension with either a single map (for the CMB file) or one map for each HFI/LFI frequency (for the foreground components). In the latter case the columns are named ''F030'', ''F044'' ,''F070'',''F100'', ''F143'', … , ''F857''. Units are microK<sub>CMB</sub> for the CMB, K<sub>CMB</sub> at 30, 44 and 70 GHz and MJy/sr for the others. The structure is given below for multi-column files. <br />
<br />
Note: Original PSM foreground components has been generated at NSIDE 2048 and using a gaussian beam of 4 arcmin, LFI maps where then smoothed to LFI resolution (32.0, 27.0 and 13.0 arcmin for the 30, 44 and 70 GHz) and donwgraded at NSIDE 1024. LFI CMB maps has been smoothed at 13.0 arcmin (70 GHz resolution) and downgraded at NSIDE 1024. <br />
<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px<br />
|+ '''HFI FITS file structure'''<br />
|- bgcolor="ffdead" <br />
!colspan="4" | 1. EXTNAME = 'SIM-MAP' : Data columns<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|F100 || Real*4 || MJy/sr || 100GHz signal map<br />
|-<br />
|F143 || Real*4 || MJy/sr || 143GHz signal map<br />
|-<br />
|F217 || Real*4 || MJy/sr || 217GHz signal map<br />
|-<br />
|F353 || Real*4 || MJy/sr || 353GHz signal map<br />
|-<br />
|F545 || Real*4 || MJy/sr || 545GHz signal map<br />
|-<br />
|F857 || Real*4 || MJy/sr || 857GHz signal map<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || string || HEALPIX ||<br />
|-<br />
|COMP || string || component || Astrophysical omponent<br />
|-<br />
|COORDSYS || string || GALACTIC || Coordinate system <br />
|-<br />
|ORDERING || string || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 2048 || Healpix Nside for LFI and HFI, respectively<br />
|-<br />
|FIRSTPIX || Int*4 || 0 || First pixel number<br />
|-<br />
|LASTPIX || Int*4 || 50331647 || Last pixel number, for LFI and HFI, respectively<br />
|-<br />
|BAD_DATA || Real*4 || -1.63750E+30 || Healpix bad pixel value <br />
|-<br />
|BEAMTYPE || string || GAUSSIAN || Type of beam <br />
|-<br />
|BEAMSIZE || Real*4 || size || Beam size in arcmin<br />
|-<br />
|PSM-VERS || string || || PSM Versions used <br />
|}<br />
<br />
<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px<br />
|+ '''LFI FITS file structure'''<br />
|- bgcolor="ffdead" <br />
!colspan="4" | 1. EXTNAME = 'SIM-MAP' : Data columns<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|F030 || Real*4 || KCMB || 30GHz signal map<br />
|-<br />
|F044 || Real*4 || KCMB || 44GHz signal map<br />
|-<br />
|F070 || Real*4 || KCMB || 70GHz signal map<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || string || HEALPIX ||<br />
|-<br />
|COMP || string || component || Astrophysical omponent<br />
|-<br />
|COORDSYS || string || GALACTIC || Coordinate system <br />
|-<br />
|ORDERING || string || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int || 1024 || Healpix Nside for LFI and HFI, respectively<br />
|-<br />
|FIRSTPIX || Int*4 || 0 || First pixel number<br />
|-<br />
|LASTPIX || Int*4 || 12582911 || Last pixel number, for LFI and HFI, respectively<br />
|-<br />
|BAD_DATA || Real*4 || -1.63750E+30 || Healpix bad pixel value <br />
|-<br />
|BEAMTYPE || string || GAUSSIAN || Type of beam <br />
|-<br />
|BEAMS_30 || Real*4 || 32.0 || Beam size at 30 GHz in arcmin<br />
|-<br />
|BEAMS_44 || Real*4 || 27.0 || Beam size at 44 GHz in arcmin<br />
|-<br />
|BEAMS_70 || Real*4 || 13.0 || Beam size at 70 GHz in arcmin<br />
|-<br />
|PSM-VERS || string || || PSM Versions used <br />
|}<br />
<br />
== The Fiducial Sky Simulations==<br />
For each detector, fiducial time-ordered data are generated separately for each of the ten PSM components using the LevelS software{{BibCite|reinecke2006}} as follows:<br />
* the detector's beam and PSM map are converted to spherical harmonics using ''beam2alm'' and ''anafast'' respectively;<br />
* the beam-convolved map value is calculated over a 3-dimensional grid of sky locations and beam orientations using ''conviqt'';<br />
* the map-based timelines are calculated sample-by-sample by interpolating over this grid using ''multimod'';<br />
* the catalogue-based timelines are produced sample-by-sample by beam-convolving any point source laying within a given angular distance of the pointing at each sample time using ''multimod''.<br />
<br />
For each frequency, fiducial sky maps are generated for <br />
* the total signal (i.e. sky + instrument noise), for both the nominal mission and the halfrings thereof (see [[Frequency_Maps#Types_of_maps| details]])<br />
* the foreground sky alone (excluding CMB but including noise), <br />
* the point source sky, and <br />
* the noise alone<br />
All maps are built using the ''MADAM'' destriping map-maker{{BibCite|keihanen2010}} interfaced with the ''TOAST'' data abstraction layer . In order to construct the total timelines required by each map, for each detector ''TOAST'' reads the various component timelines separately and sums then, and, where necessary, simulates and adds a noise realization time-stream on the fly. HFI frequencies are mapped at ''HEALPix'' resolution Nside=2048 using ring-length destriping baselines, while LFI frequencies are mapped at Nside=1024 using 1s baselines.<br />
<br />
=== Products delivered ===<br />
A single simulation is delivered, which is divided into two types of products: <br />
<br />
1. six files of the full sky signal at each HFI and LFI frequency, and their corresponding halfring maps: <br />
<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px<br />
|-<br />
| ''{{PLASingleFile | fileType=file | name=HFI_SimMap_100_2048_R1.10_nominal.fits | link=HFI_SimMap_100_2048_R1.10_nominal.fits }}'' || ''{{PLASingleFile | fileType=file | name=HFI_SimMap_100_2048_R1.10_nominal_ringhalf_1.fits | link=HFI_SimMap_100_2048_R1.10_nominal_ringhalf_1.fits }}'' || ''{{PLASingleFile | fileType=file | name=HFI_SimMap_100_2048_R1.10_nominal_ringhalf_2.fits | link=HFI_SimMap_100_2048_R1.10_nominal_ringhalf_2.fits }}''<br />
|-<br />
| ''{{PLASingleFile | fileType=file | name=HFI_SimMap_143_2048_R1.10_nominal.fits | link=HFI_SimMap_143_2048_R1.10_nominal.fits }}'' || ''{{PLASingleFile | fileType=file | name=HFI_SimMap_143_2048_R1.10_nominal_ringhalf_1.fits | link=HFI_SimMap_143_2048_R1.10_nominal_ringhalf_1.fits }}'' || ''{{PLASingleFile | fileType=file | name=HFI_SimMap_143_2048_R1.10_nominal_ringhalf_2.fits | link=HFI_SimMap_143_2048_R1.10_nominal_ringhalf_2.fits }}''<br />
|-<br />
| ''{{PLASingleFile | fileType=file | name=HFI_SimMap_217_2048_R1.10_nominal.fits | link=HFI_SimMap_217_2048_R1.10_nominal.fits }}'' || ''{{PLASingleFile | fileType=file | name=HFI_SimMap_217_2048_R1.10_nominal_ringhalf_1.fits | link=HFI_SimMap_217_2048_R1.10_nominal_ringhalf_1.fits }}'' || ''{{PLASingleFile | fileType=file | name=HFI_SimMap_217_2048_R1.10_nominal_ringhalf_2.fits | link=HFI_SimMap_217_2048_R1.10_nominal_ringhalf_2.fits }}''<br />
|-<br />
| ''{{PLASingleFile | fileType=file | name=HFI_SimMap_353_2048_R1.10_nominal.fits | link=HFI_SimMap_353_2048_R1.10_nominal.fits }}'' || ''{{PLASingleFile | fileType=file | name=HFI_SimMap_353_2048_R1.10_nominal_ringhalf_1.fits | link=HFI_SimMap_353_2048_R1.10_nominal_ringhalf_1.fits }}'' || ''{{PLASingleFile | fileType=file | name=HFI_SimMap_353_2048_R1.10_nominal_ringhalf_2.fits | link=HFI_SimMap_353_2048_R1.10_nominal_ringhalf_2.fits }}''<br />
|-<br />
| ''{{PLASingleFile | fileType=file | name=HFI_SimMap_545_2048_R1.10_nominal.fits | link=HFI_SimMap_545_2048_R1.10_nominal.fits }}'' || ''{{PLASingleFile | fileType=file | name=HFI_SimMap_545_2048_R1.10_nominal_ringhalf_1.fits | link=HFI_SimMap_545_2048_R1.10_nominal_ringhalf_1.fits }}'' || ''{{PLASingleFile | fileType=file | name=HFI_SimMap_545_2048_R1.10_nominal_ringhalf_2.fits | link=HFI_SimMap_545_2048_R1.10_nominal_ringhalf_2.fits }}''<br />
|-<br />
| ''{{PLASingleFile | fileType=file | name=HFI_SimMap_857_2048_R1.10_nominal.fits | link=HFI_SimMap_857_2048_R1.10_nominal.fits }}'' || ''{{PLASingleFile | fileType=file | name=HFI_SimMap_857_2048_R1.10_nominal_ringhalf_1.fits | link=HFI_SimMap_857_2048_R1.10_nominal_ringhalf_1.fits }}'' || ''{{PLASingleFile | fileType=file | name=HFI_SimMap_857_2048_R1.10_nominal_ringhalf_2.fits | link=HFI_SimMap_857_2048_R1.10_nominal_ringhalf_2.fits }}''<br />
|}<br />
<br />
<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px<br />
|-<br />
| ''{{PLASingleFile | fileType=file | name=LFI_SimMap_030_1024_R1.10_nominal.fits | link=LFI_SimMap_030_1024_R1.10_nominal.fits }}'' || ''{{PLASingleFile | fileType=file | name=LFI_SimMap_030_1024_R1.10_nominal_ringhalf_1.fits | link=LFI_SimMap_030_1024_R1.10_nominal_ringhalf_1.fits }}'' || ''{{PLASingleFile | fileType=file | name=LFI_SimMap_030_1024_R1.10_nominal_ringhalf_2.fits | link=LFI_SimMap_030_1024_R1.10_nominal_ringhalf_2.fits }}''<br />
|-<br />
| ''{{PLASingleFile | fileType=file | name=LFI_SimMap_044_1024_R1.10_nominal.fits | link=LFI_SimMap_044_1024_R1.10_nominal.fits }}'' || ''{{PLASingleFile | fileType=file | name=LFI_SimMap_044_1024_R1.10_nominal_ringhalf_1.fits | link=LFI_SimMap_044_1024_R1.10_nominal_ringhalf_1.fits }}'' || ''{{PLASingleFile | fileType=file | name=LFI_SimMap_044_1024_R1.10_nominal_ringhalf_2.fits | link=LFI_SimMap_044_1024_R1.10_nominal_ringhalf_2.fits }}''<br />
|-<br />
| ''{{PLASingleFile | fileType=file | name=LFI_SimMap_070_1024_R1.10_nominal.fits | link=LFI_SimMap_070_1024_R1.10_nominal.fits }}'' || ''{{PLASingleFile | fileType=file | name=LFI_SimMap_070_1024_R1.10_nominal_ringhalf_1.fits | link=LFI_SimMap_070_1024_R1.10_nominal_ringhalf_1.fits }}'' || ''{{PLASingleFile | fileType=file | name=LFI_SimMap_070_1024_R1.10_nominal_ringhalf_2.fits | link=LFI_SimMap_070_1024_R1.10_nominal_ringhalf_2.fits }}''<br />
|}<br />
<br />
<br />
: These files have the same structure as the equivalent ''SkyMap'' products described in the [[Frequency_Maps | Frequency Maps ]] chapter, namely one ''BINTABLE'' extension with three columns containing 1) Signal, 2) hit-count, and 3) variance. Units are K<sub>CMB</sub> for all channels.<br />
<br />
2. Three files containing 1) the sum of all astrophysical foregrounds, 2) the point sources alone, and 3) the noise alone: which are subproducts of the above, and are in the form of the PSM maps described in the previous section. <br />
* ''{{PLASingleFile | fileType=file | name=HFI_SimMap_foreground_2048_R1.10_nominal.fits | link=HFI_SimMap_foreground_2048_R1.10_nominal.fits }}''<br />
* ''{{PLASingleFile | fileType=file | name=HFI_SimMap_noise_2048_R1.10_nominal.fits | link=HFI_SimMap_noise_2048_R1.10_nominal.fits }}''<br />
* ''{{PLASingleFile | fileType=file | name=HFI_SimMap_ps_2048_R1.10_nominal.fits | link=HFI_SimMap_ps_2048_R1.10_nominal.fits }}'' <br />
<br />
* ''{{PLASingleFile | fileType=file | name=LFI_SimMap_foreground_1024_R1.10_nominal.fits | link=LFI_SimMap_foreground_1024_R1.10_nominal.fits }}''<br />
* ''{{PLASingleFile | fileType=file | name=LFI_SimMap_noise_1024_R1.10_nominal.fits | link=LFI_SimMap_noise_1024_R1.10_nominal.fits }}''<br />
* ''{{PLASingleFile | fileType=file | name=LFI_SimMap_ps_1024_R1.10_nominal.fits | link=LFI_SimMap_ps_1024_R1.10_nominal.fits }}'' <br />
<br />
These files have the same structure as the PSM output maps described above, namely a single ''BINTABLE'' extension with 6 columns named ''F100'' -- ''F857'' each containing the given map for that HFI band and with 3 columns named ''F030'', ''F044'', ''F070'' each containing the given map for that LFI band. Units are alway K<sub>CMB</sub>.<br />
<br />
Note that the CMB alone is not delivered as a separate product, but it can be recovered by simple subtraction of the component maps for the total signal map.<br />
<br />
== Monte Carlo realizations of CMB and of noise==<br />
The CMB MC set is generated using ''FEBeCoP''{{BibCite|mitra2010}}, which generates an effective beam for each pixel in a map at each frequency by accumulating the weights of all pixels within a fixed distance of that pixel, summed over all observations by all detectors at that frequency. It then applies this effective beam pixel-by-pixel to each of 1000 input CMB sky realizations.<br />
<br />
The noise MC set is generated just as the fiducial noise maps, using ''MADAM/TOAST''. In order to avoid spurious correlations within and between the 1000 realizations, each stationary interval for each detector for each realization is generated from a distinct sub-sequence of a single statistically robust, extremely long period, pseudo-random number sequence.<br />
<br />
=== Products delivered ===<br />
100 realizations of the CMB (lensed) and of the noise are made available. They are named<br />
* ''HFI_SimMap_cmb-{nnnn}_2048_R1.nn_nominal.fits''<br />
* ''HFI_SimMap_noise-{nnnn}_2048_R1.nn_nominal.fits''<br />
* ''LFI_SimMap_cmb-{nnnn}_2048_R1.nn_nominal.fits''<br />
* ''LFI_SimMap_noise-{nnnn}_2048_R1.nn_nominal.fits''<br />
<br />
where ''nnnn'' ranges from 0000 to 0099.<br />
<br />
The FITS file structure is the same as for the other similar products above, with a single ''BINTABLE'' extension with six columns, one for each HFI frequency, named ''F100'', ''F143'', … , ''F857'' and with three columns, one for each LFI frequency, named ''F030'', ''F044'', ''F070''. Units are always microK<sub>CMB</sub> ''(NB: due to an error in the HFI file construction, the unit keywords in the headers indicate K<sub>CMB</sub>, the "micro" is missing there)''.<br />
<br />
== Lensing Simulations ==<br />
<br />
The lensing simulations package contains 100 realisations of the Planck 2014 "MV" lensing potential estimate, as well as the input lensing realizations. They can be used to determine error bars as well eas effective normalizations for cross-correlation with other tracers of lensing. These simulations are of the lensing convergence map contained in the [[Specially processed maps#Lensing map | Lensing map]] release file. The production and characterisation of this lensing potential map are described in detail in {{PlanckPapers|planck2014-xxx}}, which also describes the procedure used to generate the realizations given here.<br />
<br />
<br />
<br />
The simulations are delivered as a gzipped tarball of approximately 8 GB in size. For delivery purposes, the package has been split into 2GB chunks using the unix command<br />
: <tt> split -d -b 2048m </tt><br />
After downloading the individual chunks, the full tarball can be reconstructed with the command<br />
: <tt>cat COM_SimMap_Lensing_R0.00.tar.* | tar xvf - </tt><br />
<br />
<br />
The contents of the tarball are described below:<br />
<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left"<br />
|+ ''' Contents of {{PLASingleFile|fileType=map|name=COM_SimMap_Lensing_2048_R0.00.tgz|link=COM_SimMap_Lensing_2048_R0.00.tgz}} '''<br />
|- bgcolor="ffdead" <br />
! Filename || Format || Description<br />
|-<br />
| obs_klms/sim_????_klm.fits || HEALPIX FITS format alm, with <math> L_{\rm max} = 2048 </math> || Contains the simulated convergence estimate <math> \hat{\kappa}_{LM} = \frac{1}{2} L(L+1)\hat{\phi}_{LM} </math> for each simulation.<br />
|-<br />
| sky_klms/sim_????_klm.fits || HEALPIX FITS format alm, with <math> L_{\rm max} = 2048 </math> || Contains the input lensing convergence for each simulation.<br />
|-<br />
| inputs/mask.fits.gz || HEALPIX FITS format map, with <math> N_{\rm side} = 2048 </math> || Contains the lens reconstruction analysis mask.<br />
|-<br />
| inputs/cls/cl??.dat || ASCII text file, with columns = (<math>L</math>, <math>C_L </math>) || Contains the fiducial theory CMB power spectra for TT, EE, BB, <math> \kappa \kappa </math> and <math> T \kappa </math>, with temperature and polarization in units of <math> \mu K </math>.<br />
|- <br />
|}<br />
<br />
== References ==<br />
<br />
<References /><br />
<br />
<br />
<br />
[[Category:Mission products|012]]</div>Dhansonhttps://wiki.cosmos.esa.int/planckpla2015/index.php?title=Specially_processed_maps&diff=10099Specially processed maps2014-12-14T20:52:41Z<p>Dhanson: /* Lensing map */</p>
<hr />
<div>{{DISPLAYTITLE:Additional maps}}<br />
==Overview==<br />
<br />
This section describes products that require special processing. Only one such product is available at this time; this section will be expanded with time as more products are added.<br />
<br />
== Lensing map ==<br />
<br />
We distribute the minimum-variance (MV) lensing potential estimate presented in {{PlanckPapers|planck2014-xxx}} as part of the 2014 data release. This map represents an estimate of the CMB lensing potential on approximately 70% of the sky, and also forms the basis for the Planck 2014 lensing likelihood. It is produced using filtered temperature and polarization data from the SMICA DX11 CMB map; its construction is discussed in detail in {{PlanckPapers|planck2014-xxx}}.<br />
<br />
<br />
The estimate is contained in a single gzipped tarball named ''{{PLASingleFile|fileType=map|name=COM_CompMap_Lensing_2048_R0.00.tgz|link=COM_CompMap_Lensing_2048_R0.00.tgz}}''. Its contents are described below.<br />
<br />
<br />
<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left"<br />
|+ ''' Contents of {{PLASingleFile|fileType=map|name=COM_CompMap_Lensing_2048_R0.00.tgz|link=COM_CompMap_Lensing_2048_R0.00.tgz}} '''<br />
|- bgcolor="ffdead" <br />
! Filename || Format || Description<br />
|-<br />
| dat_klm.fits || HEALPIX FITS format alm, with <math> L_{\rm max} = 2048 </math> || Contains the estimated lensing convergence <math> \hat{\kappa}_{LM} = \frac{1}{2} L(L+1)\hat{\phi}_{LM} </math>.<br />
|-<br />
| mask.fits.gz || HEALPIX FITS format map, with <math> N_{\rm side} = 2048 </math> || Contains the lens reconstruction analysis mask.<br />
|-<br />
| nlkk.dat || ASCII text file, with columns = (<math>L</math>, <math>N_L </math>, <math>C_L+N_L</math>) || The approximate noise <math>N_L</math> (and signal+noise, <math>C_L+N_L</math>) power spectrum of <math> \hat{\kappa}_{LM} </math>, for the fiducial cosmology used in {{PlanckPapers|planck2014-xxx}}.<br />
|}<br />
<br />
== IRAM Maps of the Crab nebula ==<br />
<br />
Maps of the Crab nebula at 89.189 GHz (HCO+(1-0) transition) in both temperature and polarization, prodouced from observations performed at the IRAM 30m telescope from January 9th to January 12th 2009, are delivered as a tarball of 416 KB in the file<br />
<br />
: [[File:Crab_IRAM_2010.zip]]<br />
<br />
See README in the tarball for full details. These data were used in{{BibCite|aumont2010}}<br />
<br />
==References==<br />
<References /><br />
<br />
<br />
<br />
<br />
<br />
[[Category:Mission products|010]]</div>Dhansonhttps://wiki.cosmos.esa.int/planckpla2015/index.php?title=Specially_processed_maps&diff=6459Specially processed maps2013-03-15T02:17:06Z<p>Dhanson: </p>
<hr />
<div>==Overview==<br />
<br />
== Lensing map ==<br />
<br />
=== Description ===<br />
<br />
Here we present the minimum-variance (MV) lens reconstruction which forms the basis for the main results of <cite>#planck2013-p12</cite>. This map is produced using a combination of the 143 and 217 GHz Planck maps on approximately 70% of the sky, and is the same map on which the Planck lensing likelihood is based.<br />
<br />
We distribute:<br />
<br />
; PHIBAR : A (transfer-function convolved) map of the lensing potential, in NSIDE 2048 HEALPix RING format. It is obtained by convolving the lensing potential estimate $\hat{\phi}$ with the lensing response function $R_L^{\phi\phi}$. This map has been band-limited between multipoles $10 \le L \le 2048$.<br />
; MASK : This is a NSIDE = 2048 HEALPix map, containing the analysis mask used in the lens reconstruction. ''Note'': the lensing map PHIBAR may take small but non-zero values inside the masked regions because it has been bandlimited.<br />
; RLPP : This column contains the response function $R_L^{\phi\phi}$.<br />
; NLPP : This column contains a sky-averaged estimate of the noise power spectrum of PHIBAR, $N_L^{\phi\phi}$. The noise is highly coloured. There is a dependence of the noise power spectrum on the local noise level of the map, discussed in Appendix A of <cite>#planck2013-p12</cite>. Note that the noise power spectrum estimate here is not sufficiently accurate for a power spectrum analysis.<br />
<br />
=== Production process ===<br />
<br />
The construction PHIBAR, RLPP and NLPP are described in detail in Sec. 2.1 of <cite>#planck2013-p12</cite>. The response function $R_L^{\phi\phi}$ here is analogous to the the beam transfer function in a CMB temperature or polarization map. We have chosen to distribute this transfer-function convolved map rather than the normalized lens reconstruction as it is a significantly more localized function of the CMB temperature map from which it is derived, and therefore more useful for cross-correlation studies.<br />
<br />
===Inputs===<br />
<br />
This product is built from the 143 and 217 GHz Planck [[Frequency Maps|frequency maps]], with 857GHz projected out as a dust template.<br />
The analysis mask is constructed from a combination of thresholding in the 857GHz map (to remove the regions which are most contaminated by Galactic dust) and the [[Component maps | Type2 CO map]] (to reduce contamination from CO lines at 217GHz). This is joined with a compact object mask synthesized from several Planck source [[Catalogues | catalogues]], including the [[ Catalogues#ERCSC | ERCSC]], [[ Catalogues#SZ | SZ ]] and [[ Catalogues#The Catalogue of Compact Sources | PCCS ]]. The reconstruction was performed using the fiducial beam window functions B(l) from the [[ The RIMO | HFI RIMO ]]. Details of the procedure used to produce a lensing estimate from these inputs are given in <cite>#planck2013-p12</cite>.<br />
<br />
===References===<br />
<br />
<biblio force=false><br />
#[[References]] <br />
</biblio><br />
<br />
===File names and format===<br />
<br />
A single file named <br />
*''COM_CompMap_Lensing_2048_R1.10.fits'' <br />
with two BINTABLE extensions containing the items described below. <br />
<br />
<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left"<br />
|+ '''FITS file structure'''<br />
|- bgcolor="ffdead" <br />
!colspan="4" | 1. EXTNAME = ''LENS-MAP''<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|PHIBAR || Real*4 || none || Map of the lensing potential estimate, convolved with RLPP<br />
|-<br />
|MASK || Int || none || Region over which the lensing potential is reconstructed<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || string || HEALPIX || colspan="2"| <br />
|-<br />
|COORDSYS || string || GALACTIC || Coordinate system <br />
|-<br />
|ORDERING || string || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int*4 || 2048 ||colspan="2"| Healpix Nside<br />
|-<br />
|FIRSTPIX || Int*4 || 0 || <br />
|-<br />
|LASTPIX || Int*4 || 50331647 ||<br />
|- bgcolor="ffdead" <br />
!colspan="4"| 2. EXTNAME = ''TransFun''<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|RLPP || Real*4 || none || Response function<br />
|-<br />
|NLPP || Real*4 || none || Sky-averaged noise power spectrum estimate<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|L_MIN || Int*4 || 0 || First multipole<br />
|-<br />
|L_MAX || Int*4 || 2048 || Last multipole<br />
|}<br />
<br />
<br />
<br />
<br />
<br />
<br />
<br />
<br />
<br />
[[Category:Mission science products|010]]</div>Dhansonhttps://wiki.cosmos.esa.int/planckpla2015/index.php?title=Specially_processed_maps&diff=6458Specially processed maps2013-03-15T02:16:15Z<p>Dhanson: </p>
<hr />
<div>==Overview==<br />
<br />
== Lensing map ==<br />
<br />
=== Description ===<br />
<br />
Here we present the minimum-variance (MV) lens reconstruction which forms the basis for the main results of <cite>#planck2013-p12</cite>. This map is produced using a combination of the 143 and 217 GHz Planck maps on approximately 70% of the sky, and is the same map on which the Planck lensing likelihood is based.<br />
<br />
We distribute:<br />
<br />
; PHIBAR : A (transfer-function convolved) map of the lensing potential, in NSIDE 2048 HEALPix RING format. It is obtained by convolving the lensing potential estimate $\hat{\phi}$ with the lensing response function $R_L^{\phi\phi}$. This map has been band-limited between multipoles $10 \le L \le 2048$.<br />
; MASK : This is a NSIDE = 2048 HEALPix map, containing the analysis mask used in the lens reconstruction. ''Note'': the lensing map PHIBAR may take small but non-zero values inside the masked regions because it has been bandlimited.<br />
; RLPP : This column contains the response function $R_L^{\phi\phi}$.<br />
; NLPP : This column contains a sky-averaged estimate of the noise power spectrum of PHIBAR, $N_L^{\phi\phi}$. The noise is highly coloured. There is a weak dependence of the noise power spectrum with the local noise level of the map, discussed in Appendix A of <cite>#planck2013-p12</cite>. Note that the noise power spectrum estimate here is not sufficiently accurate for a power spectrum analysis.<br />
<br />
=== Production process ===<br />
<br />
The construction PHIBAR, RLPP and NLPP are described in detail in Sec. 2.1 of <cite>#planck2013-p12</cite>. The response function $R_L^{\phi\phi}$ here is analogous to the the beam transfer function in a CMB temperature or polarization map. We have chosen to distribute this transfer-function convolved map rather than the normalized lens reconstruction as it is a significantly more localized function of the CMB temperature map from which it is derived, and therefore more useful for cross-correlation studies.<br />
<br />
===Inputs===<br />
<br />
This product is built from the 143 and 217 GHz Planck [[Frequency Maps|frequency maps]], with 857GHz projected out as a dust template.<br />
The analysis mask is constructed from a combination of thresholding in the 857GHz map (to remove the regions which are most contaminated by Galactic dust) and the [[Component maps | Type2 CO map]] (to reduce contamination from CO lines at 217GHz). This is joined with a compact object mask synthesized from several Planck source [[Catalogues | catalogues]], including the [[ Catalogues#ERCSC | ERCSC]], [[ Catalogues#SZ | SZ ]] and [[ Catalogues#The Catalogue of Compact Sources | PCCS ]]. The reconstruction was performed using the fiducial beam window functions B(l) from the [[ The RIMO | HFI RIMO ]]. Details of the procedure used to produce a lensing estimate from these inputs are given in <cite>#planck2013-p12</cite>.<br />
<br />
===References===<br />
<br />
<biblio force=false><br />
#[[References]] <br />
</biblio><br />
<br />
===File names and format===<br />
<br />
A single file named <br />
*''COM_CompMap_Lensing_2048_R1.10.fits'' <br />
with two BINTABLE extensions containing the items described below. <br />
<br />
<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left"<br />
|+ '''FITS file structure'''<br />
|- bgcolor="ffdead" <br />
!colspan="4" | 1. EXTNAME = ''LENS-MAP''<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|PHIBAR || Real*4 || none || Map of the lensing potential estimate, convolved with RLPP<br />
|-<br />
|MASK || Int || none || Region over which the lensing potential is reconstructed<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || string || HEALPIX || colspan="2"| <br />
|-<br />
|COORDSYS || string || GALACTIC || Coordinate system <br />
|-<br />
|ORDERING || string || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int*4 || 2048 ||colspan="2"| Healpix Nside<br />
|-<br />
|FIRSTPIX || Int*4 || 0 || <br />
|-<br />
|LASTPIX || Int*4 || 50331647 ||<br />
|- bgcolor="ffdead" <br />
!colspan="4"| 2. EXTNAME = ''TransFun''<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|RLPP || Real*4 || none || Response function<br />
|-<br />
|NLPP || Real*4 || none || Sky-averaged noise power spectrum estimate<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|L_MIN || Int*4 || 0 || First multipole<br />
|-<br />
|L_MAX || Int*4 || 2048 || Last multipole<br />
|}<br />
<br />
<br />
<br />
<br />
<br />
<br />
<br />
<br />
<br />
[[Category:Mission science products|010]]</div>Dhansonhttps://wiki.cosmos.esa.int/planckpla2015/index.php?title=Specially_processed_maps&diff=6457Specially processed maps2013-03-15T02:14:50Z<p>Dhanson: </p>
<hr />
<div>==Overview==<br />
<br />
== Lensing map ==<br />
<br />
=== Description ===<br />
<br />
Here we present the minimum-variance (MV) lens reconstruction which forms the basis for the main results of <cite>#planck2013-p12</cite>. This map is produced using a combination of the 143 and 217 GHz Planck maps on approximately 70% of the sky, and is the same map on which the Planck lensing likelihood is based.<br />
<br />
We distribute:<br />
<br />
; PHIBAR : A (transfer-function convolved) map of the lensing potential, in NSIDE 2048 HEALPix RING format. It is obtained by convolving the lensing potential estimate $\hat{\phi}$ with the lensing response function $R_L^{\phi\phi}$. This map has been band-limited between multipoles $10 \le L \le 2048$.<br />
; MASK : This is a NSIDE = 2048 HEALPix map, containing the analysis mask used in the lens reconstruction. Note: the lensing map PHIBAR may take small but non-zero values inside the masked regions because it has been bandlimited.<br />
; RLPP : This column contains the response function $R_L^{\phi\phi}$.<br />
; NLPP : This column contains a sky-averaged estimate of the noise power spectrum of PHIBAR, $N_L^{\phi\phi}$. The noise is highly coloured. There is a weak dependence of the noise power spectrum with the local noise level of the map, discussed in Appendix A of <cite>#planck2013-p12</cite>. Note that the noise power spectrum estimate here is not sufficiently accurate for a power spectrum analysis.<br />
<br />
=== Production process ===<br />
<br />
The construction PHIBAR, RLPP and NLPP are described in detail in Sec. 2.1 of <cite>#planck2013-p12</cite>. The response function $R_L^{\phi\phi}$ here is analogous to the the beam transfer function in a CMB temperature or polarization map. We have chosen to distribute this transfer-function convolved map rather than the normalized lens reconstruction as it is a significantly more localized function of the CMB temperature map from which it is derived, and therefore more useful for cross-correlation studies.<br />
<br />
===Inputs===<br />
<br />
This product is built from the 143 and 217 GHz Planck [[Frequency Maps|frequency maps]], with 857GHz projected out as a dust template.<br />
The analysis mask is constructed from a combination of thresholding in the 857GHz map (to remove the regions which are most contaminated by Galactic dust) and the [[Component maps | Type2 CO map]] (to reduce contamination from CO lines at 217GHz). This is joined with a compact object mask synthesized from several Planck source [[Catalogues | catalogues]], including the [[ Catalogues#ERCSC | ERCSC]], [[ Catalogues#SZ | SZ ]] and [[ Catalogues#The Catalogue of Compact Sources | PCCS ]]. The reconstruction was performed using the fiducial beam window functions B(l) from the [[ The RIMO | HFI RIMO ]]. Details of the procedure used to produce a lensing estimate from these inputs are given in <cite>#planck2013-p12</cite>.<br />
<br />
===References===<br />
<br />
<biblio force=false><br />
#[[References]] <br />
</biblio><br />
<br />
===File names and format===<br />
<br />
A single file named <br />
*''COM_CompMap_Lensing_2048_R1.10.fits'' <br />
with two BINTABLE extensions containing the items described below. <br />
<br />
<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left"<br />
|+ '''FITS file structure'''<br />
|- bgcolor="ffdead" <br />
!colspan="4" | 1. EXTNAME = ''LENS-MAP''<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|PHIBAR || Real*4 || none || Map of the lensing potential estimate, convolved with RLPP<br />
|-<br />
|MASK || Int || none || Region over which the lensing potential is reconstructed<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || string || HEALPIX || colspan="2"| <br />
|-<br />
|COORDSYS || string || GALACTIC || Coordinate system <br />
|-<br />
|ORDERING || string || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int*4 || 2048 ||colspan="2"| Healpix Nside<br />
|-<br />
|FIRSTPIX || Int*4 || 0 || <br />
|-<br />
|LASTPIX || Int*4 || 50331647 ||<br />
|- bgcolor="ffdead" <br />
!colspan="4"| 2. EXTNAME = ''TransFun''<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|RLPP || Real*4 || none || Response function<br />
|-<br />
|NLPP || Real*4 || none || Sky-averaged noise power spectrum estimate<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|L_MIN || Int*4 || 0 || First multipole<br />
|-<br />
|L_MAX || Int*4 || 2048 || Last multipole<br />
|}<br />
<br />
<br />
<br />
<br />
<br />
<br />
<br />
<br />
<br />
[[Category:Mission science products|010]]</div>Dhansonhttps://wiki.cosmos.esa.int/planckpla2015/index.php?title=Specially_processed_maps&diff=6456Specially processed maps2013-03-15T02:14:06Z<p>Dhanson: </p>
<hr />
<div>==Overview==<br />
<br />
== Lensing map ==<br />
<br />
=== Description ===<br />
<br />
Here we present the minimum-variance (MV) lens reconstruction which forms the basis for the main results of <cite>#planck2013-p12</cite>. This map is produced using a combination of the 143 and 217 GHz Planck maps on approximately 70% of the sky, and is the same map on which the Planck lensing likelihood is based.<br />
<br />
We distribute:<br />
<br />
; PHIBAR : A (transfer-function convolved) map of the lensing potential, in NSIDE 2048 HEALPix RING format. It is obtained by convolving the lensing potential estimate $\hat{\phi}$ with the lensing response function $R_L^{\phi\phi}$. This map has been band-limited between multipoles $10 \le L \le 2048$.<br />
; MASK : This is a NSIDE = 2048 HEALPix map, containing the analysis mask used in the lens reconstruction. Note: the lensing map PHIBAR may take small but non-zero values inside the masked regions because it has been bandlimited.<br />
; RLPP : This column contains the response function $R_L^{\phi\phi}$.<br />
; NLPP : This column contains a sky-averaged estimate of the noise power spectrum of PHIBAR, $N_L^{\phi\phi}$. The noise is highly coloured. There is a weak dependence of the noise power spectrum with the local noise level of the map, discussed in Appendix A of <cite>#planck2013-p12</cite>. Note that the noise power spectrum estimate here is not sufficiently accurate for a power spectrum analysis.<br />
<br />
=== Production process ===<br />
<br />
The construction PHIBAR, RLPP and NLPP are described in detail in Sec. 2.1 of <cite>#planck2013-p12</cite>. The response function $R_L^{\phi\phi}$ here is analogous to the the beam transfer function in a CMB temperature or polarization map. We have chosen to distribute this transfer-function convolved map rather than the normalized lens reconstruction as it is a significantly more localized function of the CMB temperature map from which it is derived, and therefore more useful for cross-correlation studies.<br />
<br />
===Inputs===<br />
<br />
This product is built from the 143 and 217 GHz Planck [[Frequency Maps|frequency maps]], with 857GHz projected out as a dust template.<br />
The analysis mask is constructed from a combination of thresholding in the 857GHz map (to remove the regions which are most contaminated by Galactic dust) and the [[Component maps | Type2 CO map]] (to reduce contamination from CO lines at 217GHz). This is combined with a compact object mask synthesized from several Planck source [[Catalogues | catalogues]], including the [[ Catalogues#ERCSC | ERCSC]], [[ Catalogues#SZ | SZ ]] and [[ Catalogues#The Catalogue of Compact Sources | PCCS ]]. The reconstruction was performed using the fiducial beam window functions B(l) from the [[ The RIMO | HFI RIMO ]]. Details of the procedure used to produce a lensing estimate from these inputs are given in <cite>#planck2013-p12</cite>.<br />
<br />
===References===<br />
<br />
<biblio force=false><br />
#[[References]] <br />
</biblio><br />
<br />
===File names and format===<br />
<br />
A single file named <br />
*''COM_CompMap_Lensing_2048_R1.10.fits'' <br />
with two BINTABLE extensions containing the items described below. <br />
<br />
<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left"<br />
|+ '''FITS file structure'''<br />
|- bgcolor="ffdead" <br />
!colspan="4" | 1. EXTNAME = ''LENS-MAP''<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|PHIBAR || Real*4 || none || Map of the lensing potential estimate, convolved with RLPP<br />
|-<br />
|MASK || Int || none || Region over which the lensing potential is reconstructed<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || string || HEALPIX || colspan="2"| <br />
|-<br />
|COORDSYS || string || GALACTIC || Coordinate system <br />
|-<br />
|ORDERING || string || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int*4 || 2048 ||colspan="2"| Healpix Nside<br />
|-<br />
|FIRSTPIX || Int*4 || 0 || <br />
|-<br />
|LASTPIX || Int*4 || 50331647 ||<br />
|- bgcolor="ffdead" <br />
!colspan="4"| 2. EXTNAME = ''TransFun''<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|RLPP || Real*4 || none || Response function<br />
|-<br />
|NLPP || Real*4 || none || Sky-averaged noise power spectrum estimate<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|L_MIN || Int*4 || 0 || First multipole<br />
|-<br />
|L_MAX || Int*4 || 2048 || Last multipole<br />
|}<br />
<br />
<br />
<br />
<br />
<br />
<br />
<br />
<br />
<br />
[[Category:Mission science products|010]]</div>Dhansonhttps://wiki.cosmos.esa.int/planckpla2015/index.php?title=Specially_processed_maps&diff=6455Specially processed maps2013-03-15T02:11:09Z<p>Dhanson: </p>
<hr />
<div>==Overview==<br />
<br />
== Lensing map ==<br />
<br />
=== Description ===<br />
<br />
Here we present the minimum-variance (MV) lens reconstruction which forms the basis for the main results of <cite>#planck2013-p12</cite>. This map is produced using a combination of the 143 and 217 GHz Planck maps on approximately 70% of the sky, and is the same map on which the Planck lensing likelihood is based.<br />
<br />
We distribute:<br />
<br />
; PHIBAR : A (transfer-function convolved) map of the lensing potential, in NSIDE 2048 HEALPix RING format. It is obtained by convolving the lensing potential estimate $\hat{\phi}$ with the lensing response function $R_L^{\phi\phi}$. This map has been band-limited between multipoles $10 \le L \le 2048$.<br />
; MASK : This is a NSIDE = 2048 HEALPix map, containing the analysis mask used in the lens reconstruction. Note: the lensing map PHIBAR may take small but non-zero values inside the masked regions because it has been bandlimited.<br />
; RLPP : This column contains the response function $R_L^{\phi\phi}$.<br />
; NLPP : This column contains a sky-averaged estimate of the noise power spectrum of PHIBAR, $N_L^{\phi\phi}$. The noise is highly coloured. There is a weak dependence of the noise power spectrum with the local noise level of the map, discussed in Appendix A of <cite>#planck2013-p12</cite>. Note that the noise power spectrum estimate here is not sufficiently accurate for a power spectrum analysis.<br />
<br />
=== Production process ===<br />
<br />
The construction PHIBAR, RLPP and NLPP are described in detail in Sec. 2.1 of <cite>#planck2013-p12</cite>. The response function $R_L^{\phi\phi}$ here is analogous to the the beam transfer function in a CMB temperature or polarization map. We have chosen to distribute this transfer-function convolved map rather than the normalized lens reconstruction as it is a significantly more localized function of the CMB temperature map from which it is derived, and therefore more useful for cross-correlation studies.<br />
<br />
===Inputs===<br />
<br />
This product is built from the 143 and 217 GHz Planck [[Frequency Maps|frequency maps]], with 857GHz projected out as a dust template.<br />
The analysis mask is constructed from a combination of thresholding in the 857GHz map (to reduce Galactic dust contamination) and the [[Component maps | Type2 CO map]] (to reduce contamination from CO lines at 217GHz). This is combined with a compact object mask synthesized from several Planck source [[Catalogues | catalogues]], including the [[ Catalogues#ERCSC | ERCSC]], [[ Catalogues#SZ | SZ ]] and [[ Catalogues#The Catalogue of Compact Sources | PCCS ]]. The reconstruction was performed using the fiducial beam window functions B(l) from the [[ The RIMO | HFI RIMO ]]. Details of the procedure used to produce a lensing estimate from these inputs are given in <cite>#planck2013-p12</cite>.<br />
<br />
===References===<br />
<br />
<biblio force=false><br />
#[[References]] <br />
</biblio><br />
<br />
===File names and format===<br />
<br />
A single file named <br />
*''COM_CompMap_Lensing_2048_R1.10.fits'' <br />
with two BINTABLE extensions containing the items described below. <br />
<br />
<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left"<br />
|+ '''FITS file structure'''<br />
|- bgcolor="ffdead" <br />
!colspan="4" | 1. EXTNAME = ''LENS-MAP''<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|PHIBAR || Real*4 || none || Map of the lensing potential estimate, convolved with RLPP<br />
|-<br />
|MASK || Int || none || Region over which the lensing potential is reconstructed<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || string || HEALPIX || colspan="2"| <br />
|-<br />
|COORDSYS || string || GALACTIC || Coordinate system <br />
|-<br />
|ORDERING || string || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int*4 || 2048 ||colspan="2"| Healpix Nside<br />
|-<br />
|FIRSTPIX || Int*4 || 0 || <br />
|-<br />
|LASTPIX || Int*4 || 50331647 ||<br />
|- bgcolor="ffdead" <br />
!colspan="4"| 2. EXTNAME = ''TransFun''<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|RLPP || Real*4 || none || Response function<br />
|-<br />
|NLPP || Real*4 || none || Sky-averaged noise power spectrum estimate<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|L_MIN || Int*4 || 0 || First multipole<br />
|-<br />
|L_MAX || Int*4 || 2048 || Last multipole<br />
|}<br />
<br />
<br />
<br />
<br />
<br />
<br />
<br />
<br />
<br />
[[Category:Mission science products|010]]</div>Dhansonhttps://wiki.cosmos.esa.int/planckpla2015/index.php?title=Specially_processed_maps&diff=6454Specially processed maps2013-03-15T02:10:35Z<p>Dhanson: </p>
<hr />
<div>==Overview==<br />
<br />
== Lensing map ==<br />
<br />
=== Description ===<br />
<br />
Here we present the minimum-variance (MV) lens reconstruction which forms the basis for the main results of <cite>#planck2013-p12</cite>. This map is produced using a combination of the 143 and 217 GHz Planck maps on approximately 70% of the sky, and is the same map on which the Planck lensing likelihood is based.<br />
<br />
We distribute:<br />
<br />
; PHIBAR : A (transfer-function convolved) map of the lensing potential, in NSIDE 2048 HEALPix RING format. It is obtained by convolving the lensing potential estimate $\hat{\phi}$ with the lensing response function $R_L^{\phi\phi}$. This map has been band-limited between multipoles $10 \le L \le 2048$.<br />
; MASK : This is a NSIDE = 2048 HEALPix map, containing the analysis mask used in the lens reconstruction. Note: the lensing map PHIBAR may take small but non-zero values inside the masked regions because it has been bandlimited.<br />
; RLPP : This column contains the response function $R_L^{\phi\phi}$.<br />
; NLPP : This column contains a sky-averaged estimate of the noise power spectrum of PHIBAR, $N_L^{\phi\phi}$. The noise is highly coloured. There is a weak dependence of the noise power spectrum with the local noise level of the map, discussed in Appendix A of <cite>#planck2013-p12</cite>. Note that the noise power spectrum estimate here is not sufficiently accurate for a power spectrum analysis.<br />
<br />
=== Production process ===<br />
<br />
The construction PHIBAR, RLPP and NLPP are described in detail in Sec. 2.1 of <cite>#planck2013-p12</cite>. The response function $R_L^{\phi\phi}$ here is analogous to the the beam transfer function in a CMB temperature or polarization map. We have chosen to distribute this transfer-function convolved map rather than the normalized lens reconstruction as it is a significantly more localized function of the CMB temperature map from which it is derived, and therefore more useful for cross-correlation studies.<br />
<br />
===Inputs===<br />
<br />
This product is built from the 143 and 217 GHz Planck [[Frequency Maps|frequency maps]], with 857GHz projected out as a dust template.<br />
The analysis mask is constructed from a combination of thresholding in the 857GHz map (to reduce Galactic dust contamination) and the [[Component maps | Type2 CO map]] (to reduce contamination from CO lines at 217GHz). This is combined with a compact object mask synthesized from several Planck source [[Catalogues | catalogues]], including the [[ Catalogues#ERCSC | ERCSC]], [[ Catalogues#SZ | SZ ]] and [[ Catalogues#The Catalogue of Compact Sources | PCCS ]]. The reconstruction was performed using the fiducial beam window functions B(l) from the [[ The RIMO | HFI RIMO ]]. Details of the procedure used to produce a lensing estimate from these inputs is given in <cite>#planck2013-p12</cite>.<br />
<br />
===References===<br />
<br />
<biblio force=false><br />
#[[References]] <br />
</biblio><br />
<br />
===File names and format===<br />
<br />
A single file named <br />
*''COM_CompMap_Lensing_2048_R1.10.fits'' <br />
with two BINTABLE extensions containing the items described below. <br />
<br />
<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left"<br />
|+ '''FITS file structure'''<br />
|- bgcolor="ffdead" <br />
!colspan="4" | 1. EXTNAME = ''LENS-MAP''<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|PHIBAR || Real*4 || none || Map of the lensing potential estimate, convolved with RLPP<br />
|-<br />
|MASK || Int || none || Region over which the lensing potential is reconstructed<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || string || HEALPIX || colspan="2"| <br />
|-<br />
|COORDSYS || string || GALACTIC || Coordinate system <br />
|-<br />
|ORDERING || string || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int*4 || 2048 ||colspan="2"| Healpix Nside<br />
|-<br />
|FIRSTPIX || Int*4 || 0 || <br />
|-<br />
|LASTPIX || Int*4 || 50331647 ||<br />
|- bgcolor="ffdead" <br />
!colspan="4"| 2. EXTNAME = ''TransFun''<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|RLPP || Real*4 || none || Response function<br />
|-<br />
|NLPP || Real*4 || none || Sky-averaged noise power spectrum estimate<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|L_MIN || Int*4 || 0 || First multipole<br />
|-<br />
|L_MAX || Int*4 || 2048 || Last multipole<br />
|}<br />
<br />
<br />
<br />
<br />
<br />
<br />
<br />
<br />
<br />
[[Category:Mission science products|010]]</div>Dhansonhttps://wiki.cosmos.esa.int/planckpla2015/index.php?title=Specially_processed_maps&diff=6453Specially processed maps2013-03-15T02:02:28Z<p>Dhanson: </p>
<hr />
<div>==Overview==<br />
<br />
== Lensing map ==<br />
<br />
=== Description ===<br />
<br />
Here we present the minimum-variance (MV) lens reconstruction which forms the basis for the main results of <cite>#planck2013-p12</cite>. This map is produced using a combination of the 143 and 217 GHz Planck maps on approximately 70% of the sky, and is the same map on which the Planck lensing likelihood is based.<br />
<br />
We distribute:<br />
<br />
; PHIBAR : A (transfer-function convolved) map of the lensing potential, in NSIDE 2048 HEALPix RING format. It is obtained by convolving the lensing potential estimate $\hat{\phi}$ with the lensing response function $R_L^{\phi\phi}$. This map has been band-limited between multipoles $10 \le L \le 2048$.<br />
; MASK : This is a NSIDE = 2048 HEALPix map, containing the analysis mask used in the lens reconstruction. Note: the lensing map PHIBAR may take small but non-zero values inside the masked regions because it has been bandlimited.<br />
; RLPP : This column contains the response function $R_L^{\phi\phi}$.<br />
; NLPP : This column contains a sky-averaged estimate of the noise power spectrum of PHIBAR, $N_L^{\phi\phi}$. The noise is highly coloured. There is a weak dependence of the noise power spectrum with the local noise level of the map, discussed in Appendix A of <cite>#planck2013-p12</cite>. Note that the noise power spectrum estimate here is not sufficiently accurate for a power spectrum analysis.<br />
<br />
=== Production process ===<br />
<br />
The construction PHIBAR, RLPP and NLPP are described in detail in Sec. 2.1 of <cite>#planck2013-p12</cite>. The response function $R_L^{\phi\phi}$ here is analogous to the the beam transfer function in a CMB temperature or polarization map. We have chosen to distribute this transfer-function convolved map rather than the normalized lens reconstruction as it is a significantly more localized function of the CMB temperature map from which it is derived, and therefore more useful for cross-correlation studies.<br />
<br />
===Inputs===<br />
<br />
This product is built from the 143 and 217 GHz Planck [[Frequency Maps|frequency maps]], with 857GHz projected out as a dust template.<br />
The analysis mask is constructed using a Galaxy mask produced by thresholding the 857GHz map to a sky fraction of fsky=0.7, which is then combined with a source mask built using several Planck source [[Catalogues | catalogues]], including the [[ Catalogues#ERCSC | ERCSC]], [[ Catalogues#SZ | SZ ]] and [[ Catalogues#The Catalogue of Compact Sources | PCCS ]]. The reconstruction was performed using the fiducial beam window functions B(l) from the [[ The RIMO | HFI RIMO ]]. Details of the procedure used to produce a lensing estimate from these inputs is given in <cite>#planck2013-p12</cite>.<br />
<br />
===References===<br />
<br />
<biblio force=false><br />
#[[References]] <br />
</biblio><br />
<br />
===File names and format===<br />
<br />
A single file named <br />
*''COM_CompMap_Lensing_2048_R1.10.fits'' <br />
with two BINTABLE extensions containing the items described below. <br />
<br />
<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left"<br />
|+ '''FITS file structure'''<br />
|- bgcolor="ffdead" <br />
!colspan="4" | 1. EXTNAME = ''LENS-MAP''<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|PHIBAR || Real*4 || none || Map of the lensing potential estimate, convolved with RLPP<br />
|-<br />
|MASK || Int || none || Region over which the lensing potential is reconstructed<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || string || HEALPIX || colspan="2"| <br />
|-<br />
|COORDSYS || string || GALACTIC || Coordinate system <br />
|-<br />
|ORDERING || string || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int*4 || 2048 ||colspan="2"| Healpix Nside<br />
|-<br />
|FIRSTPIX || Int*4 || 0 || <br />
|-<br />
|LASTPIX || Int*4 || 50331647 ||<br />
|- bgcolor="ffdead" <br />
!colspan="4"| 2. EXTNAME = ''TransFun''<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|RLPP || Real*4 || none || Response function<br />
|-<br />
|NLPP || Real*4 || none || Sky-averaged noise power spectrum estimate<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|L_MIN || Int*4 || 0 || First multipole<br />
|-<br />
|L_MAX || Int*4 || 2048 || Last multipole<br />
|}<br />
<br />
<br />
<br />
<br />
<br />
<br />
<br />
<br />
<br />
[[Category:Mission science products|010]]</div>Dhansonhttps://wiki.cosmos.esa.int/planckpla2015/index.php?title=Specially_processed_maps&diff=6452Specially processed maps2013-03-15T01:52:15Z<p>Dhanson: </p>
<hr />
<div>==Overview==<br />
<br />
== Lensing map ==<br />
<br />
=== Description ===<br />
<br />
Here we present the minimum-variance (MV) lens reconstruction which forms the basis for the main results of <cite>#planck2013-p12</cite>. This map is produced using a combination of the 143 and 217 GHz Planck maps on approximately 70% of the sky, and is the same map on which the Planck lensing likelihood is based.<br />
<br />
We distribute:<br />
<br />
; PHIBAR : A (transfer-function convolved) map of the lensing potential, in NSIDE 2048 HEALPix RING format. It is obtained by convolving the lensing potential estimate $\hat{\phi}$ with the lensing response function $R_L^{\phi\phi}$. This map has been band-limited between multipoles $10 \le L \le 2048$.<br />
; MASK : This is a NSIDE = 2048 HEALPix map, containing the analysis mask used in the lens reconstruction. Note: the lensing map PHIBAR may take small but non-zero values inside the masked regions because it has been bandlimited.<br />
; RLPP : This column contains the response function $R_L^{\phi\phi}$.<br />
; NLPP : This column contains a sky-averaged estimate of the noise power spectrum of PHIBAR, $N_L^{\phi\phi}$. The noise is highly coloured. There is a weak dependence of the noise power spectrum with the local noise level of the map, discussed in Appendix A of <cite>#planck2013-p12</cite>. Note that the noise power spectrum estimate here is not sufficiently accurate for a power spectrum analysis.<br />
<br />
=== Production process ===<br />
<br />
The construction PHIBAR, RLPP and NLPP are described in detail in Sec. 2.1 of <cite>#planck2013-p12</cite>. The response function $R_L^{\phi\phi}$ here is analogous to the the beam transfer function in a CMB temperature or polarization map. We have chosen to distribute this transfer-function convolved map rather than the normalized lens reconstruction as it is a significantly more localized function of the CMB temperature map from which it is derived, and therefore more useful for cross-correlation studies.<br />
<br />
===Inputs===<br />
<br />
This product is built from the 143 and 217 GHz Planck [[Frequency Maps|frequency maps]], with 857GHz projected out as a dust template.<br />
The analysis mask is constructed using a synthesis of several planck source [[Catalogues | catalogues]], including the [[ Catalogues#ERCSC | ERCSC]], [[ Catalogues#SZ | SZ ]] and [[ Catalogues#The Catalogue of Compact Sources | PCCS ]] catalogues. <br />
<br />
===References===<br />
<br />
<biblio force=false><br />
#[[References]] <br />
</biblio><br />
<br />
===File names and format===<br />
<br />
A single file named <br />
*''COM_CompMap_Lensing_2048_R1.10.fits'' <br />
with two BINTABLE extensions containing the items described below. <br />
<br />
<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left"<br />
|+ '''FITS file structure'''<br />
|- bgcolor="ffdead" <br />
!colspan="4" | 1. EXTNAME = ''LENS-MAP''<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|PHIBAR || Real*4 || none || Map of the lensing potential estimate, convolved with RLPP<br />
|-<br />
|MASK || Int || none || Region over which the lensing potential is reconstructed<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || string || HEALPIX || colspan="2"| <br />
|-<br />
|COORDSYS || string || GALACTIC || Coordinate system <br />
|-<br />
|ORDERING || string || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int*4 || 2048 ||colspan="2"| Healpix Nside<br />
|-<br />
|FIRSTPIX || Int*4 || 0 || <br />
|-<br />
|LASTPIX || Int*4 || 50331647 ||<br />
|- bgcolor="ffdead" <br />
!colspan="4"| 2. EXTNAME = ''TransFun''<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|RLPP || Real*4 || none || Response function<br />
|-<br />
|NLPP || Real*4 || none || Sky-averaged noise power spectrum estimate<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|L_MIN || Int*4 || 0 || First multipole<br />
|-<br />
|L_MAX || Int*4 || 2048 || Last multipole<br />
|}<br />
<br />
<br />
<br />
<br />
<br />
<br />
<br />
<br />
<br />
[[Category:Mission science products|010]]</div>Dhansonhttps://wiki.cosmos.esa.int/planckpla2015/index.php?title=Specially_processed_maps&diff=6451Specially processed maps2013-03-15T01:27:59Z<p>Dhanson: </p>
<hr />
<div>==Overview==<br />
<br />
== Lensing map ==<br />
<br />
=== Description ===<br />
<br />
Here we present the minimum-variance (MV) lens reconstruction which forms the basis for the main results of <cite>#planck2013-p12</cite>. This map is produced using a combination of the 143 and 217 GHz Planck maps on approximately 70% of the sky, and is the same map on which the Planck lensing likelihood is based.<br />
<br />
We distribute:<br />
<br />
; PHIBAR : A (transfer-function convolved) map of the lensing potential, in NSIDE 2048 HEALPix RING format. It is obtained by convolving the lensing potential estimate $\hat{\phi}$ with the lensing response function $R_L^{\phi\phi}$. This map has been band-limited between multipoles $10 \le L \le 2048$.<br />
; MASK : This is a NSIDE = 2048 HEALPix map, containing the analysis mask used in the lens reconstruction. Note: the lensing map PHIBAR may take small but non-zero values inside the masked regions because it has been bandlimited.<br />
; RLPP : This column contains the response function $R_L^{\phi\phi}$.<br />
; NLPP : This column contains a sky-averaged estimate of the noise power spectrum of PHIBAR, $N_L^{\phi\phi}$. The noise is highly coloured. There is a weak dependence of the noise power spectrum with the local noise level of the map, discussed in Appendix A of <cite>#planck2013-p12</cite>. Note that the noise power spectrum estimate here is not sufficiently accurate for a power spectrum analysis.<br />
<br />
=== Production process ===<br />
<br />
The construction PHIBAR, RLPP and NLPP are described in detail in Sec. 2.1 of <cite>#planck2013-p12</cite>. The response function $R_L^{\phi\phi}$ here is analogous to the the beam transfer function in a CMB temperature or polarization map. We have chosen to distribute this transfer-function convolved map rather than the normalized lens reconstruction as it is a significantly more localized function of the CMB temperature map from which it is derived, and therefore more useful for cross-correlation studies.<br />
<br />
===Inputs===<br />
<br />
This product is built from the 143 and 217 GHz Planck sky maps.<br />
<br />
===References===<br />
<br />
<biblio force=false><br />
#[[References]] <br />
</biblio><br />
<br />
===File names and format===<br />
<br />
A single file named <br />
*''COM_CompMap_Lensing_2048_R1.10.fits'' <br />
with two BINTABLE extensions containing the items described below. <br />
<br />
<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left"<br />
|+ '''FITS file structure'''<br />
|- bgcolor="ffdead" <br />
!colspan="4" | 1. EXTNAME = ''LENS-MAP''<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|PHIBAR || Real*4 || none || Map of the lensing potential estimate, convolved with RLPP<br />
|-<br />
|MASK || Int || none || Region over which the lensing potential is reconstructed<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|PIXTYPE || string || HEALPIX || colspan="2"| <br />
|-<br />
|COORDSYS || string || GALACTIC || Coordinate system <br />
|-<br />
|ORDERING || string || NESTED || Healpix ordering<br />
|-<br />
|NSIDE || Int*4 || 2048 ||colspan="2"| Healpix Nside<br />
|-<br />
|FIRSTPIX || Int*4 || 0 || <br />
|-<br />
|LASTPIX || Int*4 || 50331647 ||<br />
|- bgcolor="ffdead" <br />
!colspan="4"| 2. EXTNAME = ''TransFun''<br />
|- bgcolor="ffdead" <br />
! Column Name || Data Type || Units || Description<br />
|-<br />
|RLPP || Real*4 || none || Response function<br />
|-<br />
|NLPP || Real*4 || none || Sky-averaged noise power spectrum estimate<br />
|- bgcolor="ffdead" <br />
! Keyword || Data Type || Value || Description<br />
|-<br />
|L_MIN || Int*4 || 0 || First multipole<br />
|-<br />
|L_MAX || Int*4 || 2048 || Last multipole<br />
|}<br />
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[[Category:Mission science products|010]]</div>Dhansonhttps://wiki.cosmos.esa.int/planckpla2015/index.php?title=Specially_processed_maps&diff=5626Specially processed maps2013-03-11T22:12:44Z<p>Dhanson: </p>
<hr />
<div>==Overview==<br />
<br />
== Lensing map ==<br />
<br />
=== Description ===<br />
<br />
Here we present the minimum-variance (MV) lens reconstruction which forms the basis for the main results of <span style="color:red">P12_Lensing</span>. This map is produced using a combination of the 143 and 217 GHz Planck maps on approximately 70% of the sky, and is the same map on which the Planck lensing likelihood is based.<br />
<br />
We distribute:<br />
<br />
; PHIBAR : A (transfer-function convolved) map of the lensing potential, in NSIDE 2048 HEALPix RING format. It is obtained by convolving the lensing potential estimate $\hat{\phi}$ with the lensing response function $R_L^{\phi\phi}$. This map has been band-limited between multipoles $10 \le L \le 2048$.<br />
; MASK : This is a NSIDE = 2048 HEALPix map, containing the analysis mask used in the lens reconstruction. Note: the lensing map PHIBAR may take small but non-zero values inside the masked regions because it has been bandlimited.<br />
; RLPP : This column contains the response function $R_L^{\phi\phi}$.<br />
; NLPP : This column contains a sky-averaged estimate of the noise power spectrum of PHIBAR, $N_L^{\phi\phi}$. The noise is highly coloured. There is a weak dependence of the noise power spectrum with the local noise level of the map, discussed in Appendix A of <span style="color:red">P12_Lensing</span>. Note that the noise power spectrum estimate here is not sufficiently accurate for a power spectrum analysis.<br />
<br />
=== Production process ===<br />
<br />
The construction PHIBAR, RLPP and NLPP are described in detail in Sec. 2.1 of <span style="color:red">P12_Lensing</span>. The response function $R_L^{\phi\phi}$ here is analogous to the the beam transfer function in a CMB temperature or polarization map. We have chosen to distribute this transfer-function convolved map rather than the normalized lens reconstruction as it is a significantly more localized function of the CMB temperature map from which it is derived, and therefore more useful for cross-correlation studies.<br />
<br />
===Inputs===<br />
<br />
This product is built from the 143 and 217 GHz Planck sky maps.<br />
<br />
===File names and format===<br />
<br />
A single file named ''COM_CompMap_Lensing_2048_R1.10.fits'' with two BINTABLE extensions containing the items described above. <br />
<br />
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left"<br />
! Column Name || Data Type || Units || Description<br />
|-<br />
!colspan="4" style="background:#ffdead;"| 1. EXTNAME = 'LENS-MAP' : Data columns<br />
|-<br />
|PHIBAR || Real*4 || none || Map of the lensing potential estimate, convolved with RLPP<br />
|-<br />
|MASK || Int || none || Region over which the lensing potential is reconstructed<br />
|-<br />
!colspan="4"| Keywords<br />
|-<br />
|PIXTYPE || HEALPIX || colspan="2"| <br />
|-<br />
|COORDSYS || GALACTIC ||colspan="2"| Coordinate system <br />
|-<br />
|ORDERING || NESTED ||colspan="2"| Healpix ordering<br />
|-<br />
|NSIDE || 2048 ||colspan="2"| Healpix Nside<br />
|-<br />
|FIRSTPIX || 0 ||colspan="2"|<br />
|-<br />
|LASTPIX || 50331647 ||colspan="2"|<br />
|-<br />
!colspan="4" style="background:#ffdead;"| 2. EXTNAME = 'TransFun' : Data columns<br />
|-<br />
|RLPP || Real*4 || none || Response function (see above)<br />
|-<br />
|NLPP || Real*4 || none || Sky-averaged noise power spectrum estimate (see above)<br />
|-<br />
!colspan="4"| Keywords<br />
|-<br />
|L_MIN || 0 ||colspan="2"|<br />
|-<br />
|L_MAX || 2048 ||colspan="2"|<br />
|}<br />
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[[Category:Mission science products|010]]</div>Dhanson