Simulations of sky emission and of its observations with two configurations of the COrE satellite are available below. These simulations are made available only for preparing the COrE proposal in answer to the ESA 2010 call for a Medium-sized Mission Opportunity. If you have any questions about using them or the content, please contact me (delabrouille@apc.univ-paris7.fr).
The simulations uses the standard v1.7 PSM sky model, for which the sky emission is represented as the sum of 4 main components:
The Planck Sky Model is developed by the Component Separation Working Group (WG2) of the Planck Collaboration (coordinators Jacques Delabrouille and Gianfranco De Zotti).
The data available below comprises three compressed tarballs, one for the sky components (components.tar.gz), one for the sky emission in the channels of COrE configuration 1 (skyinbands-config1.tar.gz), with 8 frequency channels ranging from 60 to 820 GHz, and one for the sky emission in the channels of COrE configuration 2 (skyinbands-config2.tar.gz), with 15 frequency channels ranging from 45 to 795 GHz. The sky emission is generated with a resolution of 25 arcminutes (gaussian beam) and at nside=512. 'Observations' with the instruments are provided at the same resolution.
The CMB simulated here is a standard gaussian LCDM CMB drawn at random using a power spectrum output of CAMB.
Everything concerning the PSM component is in 'components/cmb'. CAMB configuration files, output files, and the CMB map and alm are available there.
Galactic emission consists in 4 components: Synchrotron, free-free, spinning dust, and thermal dust. It is based on a model by Marc-Antoine Miville-Deschênes.
The SZ effect is based on Nbody+hydrodynamical simulations. Hydrodynamical simulations are based on maps created by Klaus Dolag from a constrained simulation of the Local Universe. Only gas particles with z < 0.025 are used. Reference is astro-ph/0505258. Nbody simulations are based on Maps created by Bjoern Schaefer using the Hubble Volume simulation and individual cluster simulations from Volker Springel. Only clusters with z > 0.025 are used. Reference is astro-ph/0407089.
Point source simulations produce 6 different catalogues of point sources, and a set of maps which model the far infrared background. The catalogues are infrared sources (based on IRAS), radio sources (based on NVSS, GB6, and SUMSS), ultracompact H-II regions, and WMAP sources.
The first two (IR and radio sources) are split, for convenience, into faint and strong sources. Faint radiosources are those which have a flux less than 100 mJy at 20GHz, the other ones are strong. Faint IR sources are those with a 1THz (300 micron) flux of less than 500 mJy.
Radio and IR sources are polarised, with a small polarisation fraction on average (few percent max.). Finally, the FIRB emission is simulated in the form of a set of maps, which are interpolated for the observations.
Warning: Numbers for configuration A have changed as of november 15th, after discussion with Martin Bucher and Michel Piat. Please make sure you use the correct version! Numbers for configuration B correspond to the 'baseline configuration' frozen on november 16th by the instrument team, and are the ones to be used for the COrE proposal.
The first configuration (observations available in 'skyinbands-config1.tar.gz') has 8 channels:
| nu (GHz) | 60 | 100 | 140 | 180 | 220 | 340 | 540 | 820 |
| delta-nu (GHz) | 20 | 20 | 20 | 20 | 20 | 20 | 20 | 20 |
| number of detectors | 275 | 380 | 560 | 900 | 1600 | 100 | 100 | 100 |
| FWHM (arcmin) | 17.5 | 10.5 | 7.5 | 5.8 | 4.8 | 3.1 | 1.9 | 1.3 |
| I sensitivity (uK in a 1 arcmin2 pixel) | 2.31 | 2.30 | 2.30 | 2.30 | 2.31 | 30.71 | 440.0 | 28332 |
| Q and U sensitivity (uK in a 1 arcmin2 pixel) | 3.98 | 3.98 | 3.97 | 3.97 | 3.99 | 53.07 | 760.2 | 48963 |
The second configuration (observations available in 'skyinbands-config2.tar.gz') has 15 channels, with the objective of additional robustness against complications in the total polarised emission of the ISM:
| nu (GHz) | 45 | 75 | 105 | 135 | 165 | 195 | 225 | 255 | 285 | 315 | 375 | 435 | 555 | 675 | 795 |
| delta-nu (GHz) | 15 | 15 | 15 | 15 | 15 | 15 | 15 | 15 | 15 | 15 | 15 | 15 | 15 | 15 | 15 |
| number of detectors | 64 | 300 | 400 | 550 | 750 | 1150 | 1800 | 575 | 375 | 100 | 64 | 64 | 64 | 64 | 64 |
| FWHM (arcmin) | 23.3 | 14.0 | 10.0 | 7.8 | 6.4 | 5.4 | 4.7 | 4.1 | 3.7 | 3.3 | 2.8 | 2.4 | 1.9 | 1.6 | 1.3 |
| I sensitivity (uK in a 1 arcmin2 pixel) | 5.20 | 2.70 | 2.65 | 2.61 | 2.64 | 2.60 | 2.62 | 6.01 | 9.98 | 26.64 | 67.79 | 147.6 | 787.3 | 4574 | 27923 |
| Q and U sensitivity (uK in a 1 arcmin2 pixel) | 8.99 | 4.67 | 4.58 | 4.51 | 4.57 | 4.50 | 4.52 | 10.39 | 17.25 | 46.03 | 117.15 | 255.1 | 1360.5 | 7904 | 48257 |
Simulated noise maps will be made available soon.
These PRELIMINARY simulations are still being validated. Please check them carefully before using them. The units of the 'observed' sky (skyinbands) are mK_CMB.
| Download | Description | Size | Format |
| components.tar.gz | PSM Components | 542 MB | gzipped tarball |
| skyinbands-config1.tar.gz | PSM Components observed with COrE (configuration 1 with 8 channels) | 2.40 GB | gzipped tarball |
| skyinbands-config2.tar.gz | PSM Components observed with COrE (configuration 2 with 15 channels) | 4.45 GB | gzipped tarball |
The CMB used in the simulations above is unlensed. An alternate input for CMB, which uses lensed spectra as input, can be downloaded below. The original CMB component map (for both cases) is in uK_CMB, and is converted to mK_CMB for 'observed' maps. Hence, divide the 'lensed' CMB component by 1000 for replacing the original observed CMB by the 'lensed' CMB in the simulations above.
| Download | Description | Size | Format |
| lensed-cmb-component.tar.gz | PSM lensed CMB component | 49 MB | gzipped tarball |
The CMB power spectra (both unlensed and lensed) are displayed in the plots below.
Here is a mask which can be used for the analysis of the simulations. The mask cuts completely the part of the sky at galactic latitudes lower than 10 degrees, and makes a smooth transition from 0 to 1 between galactic latitudes of 10 and 20. This mask, obviously, has not been optimised, but seems to do most of the job!
| Download | Description | Size | Format |
| mask_COrE.fits.gz | Mask for component separation | 37 kB | gzipped HEALPix fits map |