Changes compared to the 171019 version: 1. Resolution changed to 0 arcmin (5 arcmin in 171019 version) 2. Bandpass integration in units of brightness temparature (K_RJ) -------------------------------- DUST AND SYNCHROTRON SIMULATIONS -------------------------------- NSIDE = 2048 FWHM = NO BEAM (IQU synchrotron, QU dust) LMAX = 2000 for dust I UNITS = uK_CMB The resolution of the intensity part of the dust is spatially dependent (see Fig. 2 of [2]). Set of frequencies: __________________________________ central freq | fractional bandpass ---------------------------------- 10 | 0.33 15 | 0.25 20 | 0.30 30 | 0.30 40 | 0.30 85 | 0.24 90 | 0.24 95 | 0.24 145 | 0.22 150 | 0.22 155 | 0.22 215 | 0.22 220 | 0.22 245 | 0.22 270 | 0.22 The central frequency can be found in the header in the keyword NUCEN -------------------------------- -------------------------------- DUST SIMULATIONS -------------------------------- 1. One realisation of a dust template at 353GHz is realised following the prescription of [1] with one major difference: the simulation contained in this folder have no TE correlation. In brief: - Intensity is a zero-level and color corrected version of the CIB-supressed dust intensity map of [2]. - A realisation of the turbulence of the galactic magnetic field is drawn and added to a regular (large scale) magnetic field. - Dust polarisation angles are computed from the realisation of the magnetic field. - The template reproduces the Planck dust spectra for ell > 40 at 353 GHz - The template features E-B power asymmetry but no TE correlation due to the poor resolution of the total instensity map. 2. The template is then bandpassed and extrapolated through frequencies in units of K_RJ (the top-hat bandpasses are flat in those units) using a pixel-dependent modified blackbody emission law. We use the same spectra law than that used in FFP10, which is very similar to FFP8 sims (end of section 3.2.1 of [3], in brief: temperature map and polarization beta map from [2] and polarization beta map following prescription of [4]). 3. Each bandpassed map is then converted in uK_CMB. -------------------------------- -------------------------------- SYNCHROTRON SIMULATIONS -------------------------------- 1. One realisation of a synchrotron template at 23GHz is realised following a similar process as that used for the dust. The realisation of the magnetic field used to produce the template is different to that of the dust. It is the same mean field but a different realisation of the turbulence (without correlation to the realisation of the turbulent field used to produce the dust template). The template features E-B power asymmetry but no TE correlation. 2. The template is bandpassed and extrapolated through frequencies in units of K_RJ (the top-hat bandpasses are flat in those units) using a pixel-dependent power law emission. 3. Each bandpassed map is then converted in uK_CMB. -------------------------------- -------------------------------- SKY SIMULATIONS -------------------------------- For each frequency, the sum of the dust and the synchrotron simulation. -------------------------------- -------------------------------- CONTACT -------------------------------- For questions and/or comments: flavien.vansyngel@ias.u-psud.fr -------------------------------- -------------------------------- References -------------------------------- [1] Vansyngel et al. - https://arxiv.org/abs/1611.02577 [2] Planck intermediate results XLVIII - https://arxiv.org/abs/1605.09387 [3] Planck intermediate results XII - https://arxiv.org/abs/1509.06348 [4] Planck intermediate results XVII - https://arxiv.org/abs/1312.5446