Planck Legacy Archive - Rencontres de Moriond
Transcription
Planck Legacy Archive - Rencontres de Moriond
Planck nominal mission data Planck Legacy Archive Main references for this talk are • Planck 2013 results. Explanatory supplement • Planck 2013 results. I. Overview of products and results • Planck 2013 results. XI. All-sky model of thermal dust emission • Planck 2013 results. XII. Component separation • Planck 2013 results. XIII. Galactic CO emission • Planck 2013 results. XIV. Zodiacal emission • Planck 2013 results. XV. CMB power spectra and likelihood • Planck 2013 results. XVI. Cosmological parameters • Planck 2013 results. XVII. Gravitational lensing by large-scale structure • Planck 2013 results. XXVIII. The Planck Catalogue of Compact Sources • Planck 2013 results. XXIX. The Planck catalogue of Sunyaev-Zeldovich sources Cécile Renault (LPSC Grenoble) on behalf of the Planck collaboration The instruments The RIMO gathers performance and instrumental characteristics of both instruments • Focal plane database • Beam: solid angle, FWHM • Effective beam window functions B(l) • Band averaged spectral response • Noise / detector (white noise level, slope, knee freq.) Credits : ESA- AOES medialab The explanatory supplement contains information which is more “convenience” oriented than description provided in the papers. Cécile Renault (LPSC, Planck collaboration) Area of the sky masked due to Solar system objects (143 GHz SWB) Color depends on the survey. Around Mars. Rencontres de Moriond, cosmology session March 2014 Frequency maps • frequency (LFI from 30 to 70 GHz, HFI from 100 to 857 GHz) • which data are projected: nominal mission, survey 1 or 2, half-rings (odd or even cicles) • with zodiacal light correction applied or not • Nside (30 & 44 GHz @ 1024, 70 GHZ @ 1024 & 2048, 100 to 857 GHz @ 2048) 30 GHz 100 GHz 353 GHz 44 GHz 70 GHz 143 GHz 217 GHz 545 GHz 857 GHz Cécile Renault (LPSC, Planck collaboration) Set of maps are provided to allow use for astrophysics, cosmology (component separation, noise estimation from half-rings ...) Rencontres de Moriond, cosmology session March 2014 PCCS: almost 25,000 sources almost 8,000 extragalactic sources Type of galaxy Frequency Emission process Nb of sources radio-galaxies & blazars 30-217 GHz emission by synchrotron effect of e- in the host galaxy or in the jets. few hundreds Close galaxies, or luminous or ultra-luminous infrared galaxies 353-857 GHz thermal emission of the dust few thousands 30 GHz 143 GHz 857 GHz more than 17,000 galactic sources bright enough to be visible above the diffuse background mainly cores of cold molecular clouds detailed study by Herschel Catalogue provides position, flux, shape, validation flags, info on neighbours Cécile Renault (LPSC, Planck collaboration) Rencontres de Moriond, cosmology session March 2014 SZ catalogue 1227 clusters of galaxies detected by SZ effect search on 83.6 % of the sky 683 known clusters, 178 confirmed by XMM, 366 other clusters • Results from the 3 algorithms used to detect sources by SZ effect, union of them + valid catalogue • SZ effect unsensitive to distance of the cluster (except dilution in the beam) --> redshift distribution less concentrated on low z than X-ray clusters. Catalogue provides position, SNR, (external name, z), algo + validation information Cécile Renault (LPSC, Planck collaboration) Rencontres de Moriond, cosmology session March 2014 Galactic diffuse emission The COMMANDER comp. separation method provides the maps of the diffuse galactic emissions. • The low-frequency signal is due to synchrotron, free-free and Haze emissions. Its contribution affects almost only LFI maps. • The high-frequency diffuse component is due to the thermal emission of galactic dust. A set of map is provided, with different physical content to allow a full characterization of the dust. radiance (W/m2/sr) optical depth @ 353 [7 10-10 - 0.025] Cécile Renault (LPSC, Planck collaboration) dust spectral index beta [1-2.5] temperature (K) ~[10-60 K] Rencontres de Moriond, cosmology session March 2014 CO lines Dedicated component separations to extract CO velocity-integrated emission maps of the J=1-0 (115 GHz), J=2-1 (230 GHz), J=3-2 (345 GHz) lines from 100, 217, 353 GHz maps • Type 1: low SNR but high reliability: different transmission in each single bolometer at a given frequency channel allows computation of the CO lines contribution • Type 2: higher SNR but possible residual contamination from other diffuse foregrounds. J=1-0 or 2-1 only, using frequency maps and assumption on spectral behavior of other foregrounds. DAME survey Planck type2 • Type 3: sensitive finder chart for low-intensity diffuse CO emission. Uses prior information on CO line ratios and a multi-frequency component separation method Taurus region Cécile Renault (LPSC, Planck collaboration) J=1-0 line Rencontres de Moriond, cosmology session March 2014 CMB maps • CMB map (nside 256 or 2048, inpainted) • nominal (SMICA) + 3 additionnal component separation results (NILC, SEVEM, COMMANDER-ruler) • Inputs are the frequency maps (30-857 or 30-353 GHz) • Methods are linear combination in pixel or in harmonic space with weighting on the sky or with templates (from Planck data) optimized to extract the CMB component Cécile Renault (LPSC, Planck collaboration) Rencontres de Moriond, cosmology session March 2014 Lensing Map of CMB lensing potential derived by minimum-variance using 143 & 217 GHz maps on ~ 70% of the sky. , n o i t ! a g m n r i o n f r n o i m e r y o a m d s r e n Fo d e W e m o c Cécile Renault (LPSC, Planck collaboration) Rencontres de Moriond, cosmology session March 2014 Tools: masks and effective beams A set of masks, mainly useful for cosmology studies, is provided: • Galaxy, LFI or HFI point source masks • CMB, likelihood or power spectrum masks CMB union mask Likelihood mask • Effective beams per frequency are also provided: true sky X the effective beam = observed sky 217 GHz Compact sources, effective beams, PSFs Cécile Renault (LPSC, Planck collaboration) • The effective beam results from the optical+electronic response of the detectors after deconvolution and filtering of the timelines (4 time constants from ~ 10 ms to 2 s, Fourier filtering above ~80 Hz for CMB channels, 3-point filtering for galactic channels) + scanning strategy + mix of detectors. Rencontres de Moriond, cosmology session March 2014 Temperature power spectra LFI map power spectra • no component separation, apodized mask of 60 % of the sky • power spectra per LFI frequency • binning scheme provided in the ExplSuppl HFI map power spectra • no component separation, apodized mask of 42.8% of the sky • Set of HFI auto & cross-power spectra between SWB and SWB or detset @ 100, 143, 217 GHz (unbinned estimated power spectrum for allℓup to 3508) Cécile Renault (LPSC, Planck collaboration) Rencontres de Moriond, cosmology session March 2014 Likelihood & CMB TT power spectrum • one low-ℓ T only likelihood (commander ℓin [2-49] from 30– 353 GHz over 91% of the sky) • one low-ℓ T and WMAP9 polarization likelihood (lowlike ℓin [2-32]) • one high-ℓT only likelihood (CAMspecℓin [50-2500] with ~ 58% of the sky @ 100 GHz, and 37% @ 143 & 217 GHz) • lensing likelihoodℓin [40-400] • delivered with the code to read them 6 cosmological and 11 nuisance parameters (PS, CIB, tSZ, kSZ) from the CAMspec likelihood CMB power spectrum (with covar matrix) provided in FITS (+ ASCII format for spectrum only) • Each multipole from 2 to 49, derived from the component-separation algorithm, Commander, applied to frequency maps • Per bin of increasing size from multipoles 32 to 2479. Derived from the CAMspec likelihood by optimally combining the spectra in the frequency range 100-217 GHz, and correcting them for unresolved foregrounds Cécile Renault (LPSC, Planck collaboration) Rencontres de Moriond, cosmology session March 2014 Cosmological parameters Planck+lensing Planck+WP WMAP-9 Variety of models, using Planck and combinations of Planck with other data Parameter chains • full grid or direct access to chains for baseline models and several dataset Files use the standard March 2013 CosmoMC outputs • MCMC chain • marginalized constraint on individual parameters • best-fit theoretical power spectra (without foregrounds) for each model Ωbh2 Ωch2 ns τ Cécile Renault (LPSC, Planck collaboration) ln(1010As) ΩΛ Rencontres de Moriond, cosmology session March 2014 Where are the data ? !"#$%&'()*#%+',-%./0) .11234455567%/8276)7#6/$14/$9):62.2;2-8<)%1=2"#$%&>2#666 ESA webpage (PLA Planck in google) & LAMBDA webpage (updated after peculiar requests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script More convenient for multiple requests. Contains effective beams. 56$,&7(8"9$&3(0%&'+:"(=,1"%.2"%$>+6+13(*3#1"/ Easy access to most products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lanck_2013_results_explanatory_supplement (pdf or on-line) contains details on all Planck products PL$61&$,78,2),4*,$2%.>6"/#$&:)4H$-0,$32*0)I,$)4-,2L3*,N$L)2:-$*14:&(-$1&2$/21&'(,$:011-)4H$83H,M$PL$61&$*3441-$:1(I,$34$)::&,$61&2:,(L$12$03I,$$Q&,:-)14:$2,(3-,<$-1$%(34*5$821<&*-:N$8(,3:,$:&'=)-$3$2,Q&,:-$I)3$1&2$0,(8<,:5$3-$0--8C[[SSSM:*)18:M,:3M)4-[0,(8<,:5\8)3M G1'"%(%"#.C%&"#H(=50I(56$,&7(-./"(5$9"J $ $$$R1862)H0-$]$?@>A$!&218,34$"83*,$#H,4*6M$#(($2)H0-:$2,:,2I,<M 2014 release will include polarization ,.=3)($-0,$S,'=3:-,2$$$$ /0):$83H,$S3:$L)2:-$*2,3-,<$14$KL(M"&"/>"%N(KLOL(34<$S3:$(3:-$&8<3-,<$14$KP(?$,C$%3N(KLOQM • content of the FITS file, informations in the Header • information on how these data have been obtained • information on codes which have to be used to use the product Cécile Renault (LPSC, Planck collaboration) • I, Q , U maps per frequency, time period, detector, detector set ... • TT, TE, EE, EB, BB power spectra 2014 release will include timelines Rencontres de Moriond, cosmology session March 2014 The Universe seen by Planck From our galactic environment up to the last scattering surface, Planck provides maps of the sky. Enjoy ! * * simulations of the reionization Cécile Renault (LPSC, Planck collaboration) Rencontres de Moriond, cosmology session March 2014