Planck Pre-Launch Status Papers - APC - Université Paris Diderot ...
Planck Pre-Launch Status Papers - APC - Université Paris Diderot ... Planck Pre-Launch Status Papers - APC - Université Paris Diderot ...
J. A. Tauber et al.: Planck pre-launch status: The Planck missionFig. 16. AsketchofthecentresinvolvedinthePlanck ground segmentand the main data exchanges between them.the satellite during the past 24 h. The downlinked data aretransferred from New Norcia to the MOC over a period oftypically 8 h; at MOC they are put onto a data server fromwhere they are retrieved by the two Data Processing Centres.– The Planck Science Office (PSO), located at ESA’s EuropeanSpace Astronomy Centre in Madrid (Spain) is responsiblefor coordinating scientific operations of the Planck instruments,and for planning the sky surveying strategy. It providesto MOC a detailed pointing plan with a periodicity ofabout 1 month. PSO will also develop and operate the archivewhich will store and distribute the final scientific products tothe community.– The LFI instrument operations and data processing centre,located at the Osservatorio Astronomico di Trieste (Italy), isresponsible for the optimal operation of the LFI instrument,and for the processing of the data acquired by LFI into thefinal scientific products of the mission.– The HFI instrument operations and data processing centres,located respectively at the Institut d’Astrophysique Spatialein Orsay (France) and at the Institut d’Astrophysique de Paris(France), are similarly responsible for the optimal operationof the HFI instrument, and (with several other institutes inFrance and the UK) for the processing of the data acquiredby HFI into the final scientific products of the mission.The principal objective of Planck is to enable CMB-based scientificanalysis, as described in the Planck Bluebook. Thesuccessof the mission depends on the combination of measurementsfrom both instruments to produce a sensitive and wellunderstoodset of maps of the Stokes I, Q and U components ofthe CMB anisotropies . The combination of LFI and HFI dataposes significant challenges arising from the different technologiesinvolved, but also provides advantages in terms of crosscheckingand cross-calibration. To use these advantages fully requiresthe co-analysis of LFI and HFI data at all levels startingat that of individual detector timelines, and not only at the levelof frequency channel maps. The two data processing centres(DPCs) have set up a system of periodic data exchanges which isgeared to make full use of these advantages and to ensure that asingle coherent set of products is generated by the mission. Thephilosophy underlying this system is that:– The calibration of each instrument and cleaning of spuriousartifacts requires deep expert knowledge and is carriedout within each DPC; nonetheless, LFI and HFI data (timelines,detector maps, frequency channel maps) are exchangedat frequent intervals to allow cross-calibration and crosscheckingfor systematic effects as much as possible.– Frequency maps will be produced by each DPC for theirrespective instruments and will form a common input tocomponent separation pipelines which are geared to isolatethe CMB signals from all systematic effects and non-CMBsignals (so-called “foregrounds”). Finding the best algorithmfor this purpose will be an iterative process involving bothDPCs.– Scientific analysis is the main driver in the search for thebest products and cannot be separated from data calibrationor processing issues; it is therefore intertwined and willalso be repeatedly iterated. To enable this feedback to takeplace, the DPCs will issue at regular intervals (typically6months)products-principallymaps–ofincreasingsophisticationand quality for the scientific users within the PlanckCollaboration (see Annex 1).The iterative data processing outlined above will gradually yieldamaturesetofscientificproductswhichwillbedeliveredbytheDPCs to ESA 2 years after the end of the baseline surveying periodof 15 months 11 .Thedataproducts,whichwillbedistributedto the community via an online archive developed by ESA about3.5 years after launch (i.e. in November 2012), will consist of:– Calibrated and cleaned time-ordered data for each detector.– Maps of the whole sky at each Planck frequency. This is themain product of the mission.– All-sky Stokes I, Q, and U maps of the CMB anisotropies– All-sky Stokes I, Q, and U maps of a set of non-CMBcomponents, the exact definition of which is still open, butwhich will contain at least Galactic synchrotron, free-free,and dust emission; and most likely also the diffuse (unresolved)Sunyaev-Zeldovich and extragalactic background.– An all-sky catalogue of compact and point sources extractedfrom the Planck sky maps. These sources will include bothGalactic and extra-galactic sources. Of particular interestamong the extra-galactic sources will be those detected viathe signature of the Sunyaev-Zeldovich effect.– Asufficient set of information and data which allows theproducts to be useable by a typical astronomer, e.g. calibrationdata, uncertainty descriptors, likelihood functions, ancillarydata used in the product generation, descriptive documentation,etc.In addition to the above products, an Early Release CompactSource Catalogue (ERCSC) will be released to the community∼19 months after launch, which is targeted to identification andquick follow-up of scientifically interesting objects, in particularby the limited-lifetime Herschel Observatory 12 .TheERCSCwill be based on the data gathered during the first sky surveyonly, and the detection algorithm will emphasize reliability ofthe included sources rather than completeness. The algorithmwill not attempt to use any channel cross-correlation information,except in the case of two particular classes of sources whichare of particular interest for Herschel follow-up and which willbe identified on specific color criteria, namely Galactic coldcores and extragalactic Sunyaev-Zeldovich sources. The typical11 If the Planck mission is extended by a year, the first delivery of productsbased on the initial period will be followed by a second delivery,one year later, of products based on the full data set.12 See http://www.esa.int/HerschelPage 17 of 22
A&A 520, A1 (2010)flux limit of the ERCSC at high Galactic latitudes will be ∼10σof the noise or confusion level (see Table 4).6. The core scientific programmeThe organisation of the Planck Collaboration (see Appendix A)is geared not only to generate the final scientific productsdescribed in Sect. 5, but also to enable scientific analysis duringthe proprietary period. The science potential of Planck hasbeen described previously in detail in the Planck Bluebook. ThePlanck Collaboration is focussing its efforts into a number ofareas each covering a set of well defined projects (as enumeratedbelow). Each of the projects has been assigned to a specificteam of people within the overall Collaboration. In mostcases a substantial amount of preparatory work has been doneby these teams so that scientific papers can be completed by thetime that the products of Planck are publicly released. Together,these projects form the core of the Planck Scientific Programme:1. CMB-based cosmology(a) Analysis of the isotropy and statistics of the CMBanisotropies, in particular by– blind application of a range of statistical tools to theCMB maps;– investigation of the large-scale “anomalies” suspectedin the WMAP data;– investigation of large-scale “anomalies” in Planckpolarization maps.(b) Estimation of the temperature and polarisation angularpower spectra and likelihood functions(c) Estimation of cosmological parameters, based on– Planck data alone– Planck data and constraints from other astrophysicaldata. Special attention will be paid to constraintswhich can be put on inflationary models.(d) Search for and constraints on B-mode polarisationanisotropies.(e) Determination of the gravitational lensing signatures inthe CMB caused by intervening large-scale structure.2. Non-Gaussianity of the CMB(a) Bispectrum analysis and constraints on the f NL parameterfor “squeezed” triangular wave vector shapes and ofmore general forms of non-Gaussianity.(b) Testing any measured non-Gaussianity against the predictionsof specific inflationary models (e.g. multi-fieldinflation, curvaton perturbations, DBI inflation etc.).(c) Measuring or setting upper limits on the existence andstrength of primordial magnetic fields.(d) Probing the geometry and topology of the Universe, bytesting against the predictions of specific models such asBianchi universes.(e) Testing for the presence of cosmic strings or other classesof defects.3. Secondary anisotropies(a) Production and analysis of a catalogue of Sunyaev-Zeldovich (SZ) sources detected by Planck.(b) Analysis of the combination of Planck SZ-selectedgalaxy clusters with a wide range of other observations(X-ray, optical, near-IR, sub-mm), either from existingsurveys or by dedicated follow-up, to study their physicsand evolution.(c) Reconstruction of the ionisation history of the Universe.(d) Estimation of the Integrated Sachs-Wolfe effect and itsconstraints on cosmological parameters e.g. the dark energyequation of state.(e) Extraction and analysis of diffuse and kinetic Sunyaev-Zeldovich components.4. Extragalactic sources(a) Analysis of the statistical properties and evolution ofradio and sub-mm sources, and their classification intodominant populations(b) Survey of extreme radio sources, i.e. those with unusual,sharply peaked, or inverted spectra.(c) Construction and analysis of a catalogue of quasars andBL Lac objects, combining Planck data with data from awide variety of other wavelengths. Specific effort is beingmade to detect flaring sources and follow them upquickly with ground facilities.(d) Construction and analysis of a catalogue of nearby galaxies,and the detailed study of a small number of resolvedgalaxies (LMC, SMC, M 31, M 33).(e) All-sky survey and analysis of bright high-redshift dustygalaxies, and possibly proto-clusters.(f) Extraction of the cosmic far-infrared background believedto consist of unresolved galaxies, and analysis ofthe angular power spectra of this component.5. Galactic science(a) Construction of a model of the large scale ordered magneticfield in the Galaxy, based on the polarised Planckmaps.(b) Study of the diffuse warm ionized gas in the Galaxy,based on the Planck map of free-free emission.(c) Reconstruction of the Galacto-centric distribution ofemission of the different phases of the interstellarmedium in the Galaxy (H 2 ,HI,H + ), by correlation ofthe Planck maps to tracers of each phase.(d) Study of the diffuse synchrotron emission from theGalaxy, in particular its spectrum and its spatial structure.(e) Study of the physical characteristics of the circumstellarenvironment of various types of stellar objects in the finalphases of their evolution.(f) Construction and analysis of a catalogue of compact andultra-compact HII regions and massive young stellar objects.(g) Construction and analysis of a catalogue of cold prestellarcores in the Galaxy.(h) Study of the spectral energy distributions of SupernovaRemnants across the Planck bands.(i) Study of the spatial and spectral distribution of thermaldust polarisation to elucidate the nature of dust in thevarious phases of the interstellar medium.(j) Establishment of the spatial and spectral properties ofthe anomalous emission so far attributed to spinning dustparticles.(k) Combination of Planck maps with lower frequencylarge-scale ground-based surveys to study the relationshipsbetween the various phases of the Galactic interstellarmedium (atomic, molecular, ionized, relativistic,magnetic, etc.).(l) Study of the properties of dust in regions at high Galacticlatitudes and in intermediate and high velocity clouds,using the Planck data in combination withothertracerssuch as HI, IRAS/IRIS etc.(m) Study of the Planck maps to determine the structure anddistribution of mass in molecular clouds.Page 18 of 22
- Page 1 and 2: A&A 520, E1 (2010)DOI: 10.1051/0004
- Page 3 and 4: ABSTRACTThe European Space Agency
- Page 5 and 6: A&A 520, A1 (2010)Fig. 2. An artist
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- Page 11 and 12: A&A 520, A1 (2010)Table 4. Summary
- Page 13 and 14: A&A 520, A1 (2010)three frequency c
- Page 15 and 16: A&A 520, A1 (2010)Fig. 12. The left
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- Page 21 and 22: A&A 520, A1 (2010)- University of C
- Page 23 and 24: A&A 520, A1 (2010)57 Instituto de A
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- Page 29 and 30: A&A 520, A2 (2010)Table 2. Predicte
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- Page 35 and 36: A&A 520, A2 (2010)Fig. 11. Comparis
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- Page 41 and 42: A&A 520, A2 (2010)Table 7. Optical
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A&A 520, A1 (2010)flux limit of the ERCSC at high Galactic latitudes will be ∼10σof the noise or confusion level (see Table 4).6. The core scientific programmeThe organisation of the <strong>Planck</strong> Collaboration (see Appendix A)is geared not only to generate the final scientific productsdescribed in Sect. 5, but also to enable scientific analysis duringthe proprietary period. The science potential of <strong>Planck</strong> hasbeen described previously in detail in the <strong>Planck</strong> Bluebook. The<strong>Planck</strong> Collaboration is focussing its efforts into a number ofareas each covering a set of well defined projects (as enumeratedbelow). Each of the projects has been assigned to a specificteam of people within the overall Collaboration. In mostcases a substantial amount of preparatory work has been doneby these teams so that scientific papers can be completed by thetime that the products of <strong>Planck</strong> are publicly released. Together,these projects form the core of the <strong>Planck</strong> Scientific Programme:1. CMB-based cosmology(a) Analysis of the isotropy and statistics of the CMBanisotropies, in particular by– blind application of a range of statistical tools to theCMB maps;– investigation of the large-scale “anomalies” suspectedin the WMAP data;– investigation of large-scale “anomalies” in <strong>Planck</strong>polarization maps.(b) Estimation of the temperature and polarisation angularpower spectra and likelihood functions(c) Estimation of cosmological parameters, based on– <strong>Planck</strong> data alone– <strong>Planck</strong> data and constraints from other astrophysicaldata. Special attention will be paid to constraintswhich can be put on inflationary models.(d) Search for and constraints on B-mode polarisationanisotropies.(e) Determination of the gravitational lensing signatures inthe CMB caused by intervening large-scale structure.2. Non-Gaussianity of the CMB(a) Bispectrum analysis and constraints on the f NL parameterfor “squeezed” triangular wave vector shapes and ofmore general forms of non-Gaussianity.(b) Testing any measured non-Gaussianity against the predictionsof specific inflationary models (e.g. multi-fieldinflation, curvaton perturbations, DBI inflation etc.).(c) Measuring or setting upper limits on the existence andstrength of primordial magnetic fields.(d) Probing the geometry and topology of the Universe, bytesting against the predictions of specific models such asBianchi universes.(e) Testing for the presence of cosmic strings or other classesof defects.3. Secondary anisotropies(a) Production and analysis of a catalogue of Sunyaev-Zeldovich (SZ) sources detected by <strong>Planck</strong>.(b) Analysis of the combination of <strong>Planck</strong> SZ-selectedgalaxy clusters with a wide range of other observations(X-ray, optical, near-IR, sub-mm), either from existingsurveys or by dedicated follow-up, to study their physicsand evolution.(c) Reconstruction of the ionisation history of the Universe.(d) Estimation of the Integrated Sachs-Wolfe effect and itsconstraints on cosmological parameters e.g. the dark energyequation of state.(e) Extraction and analysis of diffuse and kinetic Sunyaev-Zeldovich components.4. Extragalactic sources(a) Analysis of the statistical properties and evolution ofradio and sub-mm sources, and their classification intodominant populations(b) Survey of extreme radio sources, i.e. those with unusual,sharply peaked, or inverted spectra.(c) Construction and analysis of a catalogue of quasars andBL Lac objects, combining <strong>Planck</strong> data with data from awide variety of other wavelengths. Specific effort is beingmade to detect flaring sources and follow them upquickly with ground facilities.(d) Construction and analysis of a catalogue of nearby galaxies,and the detailed study of a small number of resolvedgalaxies (LMC, SMC, M 31, M 33).(e) All-sky survey and analysis of bright high-redshift dustygalaxies, and possibly proto-clusters.(f) Extraction of the cosmic far-infrared background believedto consist of unresolved galaxies, and analysis ofthe angular power spectra of this component.5. Galactic science(a) Construction of a model of the large scale ordered magneticfield in the Galaxy, based on the polarised <strong>Planck</strong>maps.(b) Study of the diffuse warm ionized gas in the Galaxy,based on the <strong>Planck</strong> map of free-free emission.(c) Reconstruction of the Galacto-centric distribution ofemission of the different phases of the interstellarmedium in the Galaxy (H 2 ,HI,H + ), by correlation ofthe <strong>Planck</strong> maps to tracers of each phase.(d) Study of the diffuse synchrotron emission from theGalaxy, in particular its spectrum and its spatial structure.(e) Study of the physical characteristics of the circumstellarenvironment of various types of stellar objects in the finalphases of their evolution.(f) Construction and analysis of a catalogue of compact andultra-compact HII regions and massive young stellar objects.(g) Construction and analysis of a catalogue of cold prestellarcores in the Galaxy.(h) Study of the spectral energy distributions of SupernovaRemnants across the <strong>Planck</strong> bands.(i) Study of the spatial and spectral distribution of thermaldust polarisation to elucidate the nature of dust in thevarious phases of the interstellar medium.(j) Establishment of the spatial and spectral properties ofthe anomalous emission so far attributed to spinning dustparticles.(k) Combination of <strong>Planck</strong> maps with lower frequencylarge-scale ground-based surveys to study the relationshipsbetween the various phases of the Galactic interstellarmedium (atomic, molecular, ionized, relativistic,magnetic, etc.).(l) Study of the properties of dust in regions at high Galacticlatitudes and in intermediate and high velocity clouds,using the <strong>Planck</strong> data in combination withothertracerssuch as HI, IRAS/IRIS etc.(m) Study of the <strong>Planck</strong> maps to determine the structure anddistribution of mass in molecular clouds.Page 18 of 22
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