Planck 2014 The Microwave Sky in Temperature and Polarisation Ferrara, 1 5 December The Planck mission
|
|
- Shauna Gibson
- 5 years ago
- Views:
Transcription
1
2 Planck 2014 The Microwave Sky in Temperature and Polarisation Ferrara, 1 5 December 2014 The Planck mission Marco Bersanelli Dipartimento di Fisica, Università degli Studi di Milano Planck-LFI Deputy PI and Instrument Scientist On behalf of the Planck Collaboration
3 The Planck Collaboration START SURVEY EXTENSION 2 EXTENSION 1 NOMINAL MISSION months 15.5 months months 2014 COBRAS & SAMBA PROPOSALS COBRAS/SAMBA SELECTION REDBOOK LFI & HFI CONSORTIA INSTRUMENT & DPC DEVELOPMENT INSTRUMENT LEVEL TESTS BLUEBOOK CSL TEST LAUNCH EARLY RESULTS HFI EOL LFI EOL 2013 RELEASE 2015 RELEASE 2014 RELEASE
4 Early times START SURVEY EXTENSION 2 EXTENSION 1 NOMINAL MISSION months 15.5 months months 2014 COBRAS & SAMBA PROPOSALS COBRAS/SAMBA SELECTION REDBOOK LFI & HFI CONSORTIA INSTRUMENT & DPC DEVELOPMENT INSTRUMENT LEVEL TESTS BLUEBOOK CSL TEST LAUNCH EARLY RESULTS HFI EOL Wide spectral range ( GHz) Two different technologies Control of systematics LFI EOL 2013 RELEASE 2015 RELEASE 2014 RELEASE dt/t ~ 2 x 10-6 θ ~ 15 No requirements on polarisation
5 Instrument & DPC development Ground & in-flight calibration Kourou, French Guyana, 14 May 2009, h 10: LFI cooled to 20K Ref loads to 4K 1998 HFI Polarisation Sensitive Bolometers EXTENSION 2 EXTENSION 1 NOMINAL MISSION 2006 START SURVEY months 15.5 months months 2014 COBRAS & SAMBA PROPOSALS COBRAS/SAMBA SELECTION REDBOOK LFI & HFI CONSORTIA INSTRUMENT & DPC DEVELOPMENT INSTRUMENT LEVEL TESTS BLUEBOOK CSL TEST LAUNCH EARLY RESULTS HFI EOL LFI EOL 2013 RELEASE 2015 RELEASE 2014 RELEASE Qualification Model Flight Model Data Processing Centers Flight Data analysis
6 PLANCK Looking back to the dawn of time Planck Telescope 1.5x1.9m off-axis Gregorian T = 50 K LFI Radiometers GHz, T = 20 K HFI Bolometers GHz, T = 0.1 K
7 In-flight cryo-chain performance & mission lifetime Thermal stability 0.1K 50µK 1.4K 4K 100µK 500µK 20K 4K 0.1K 40K 50K 100K 150K 20K 300K 370K Excellent Planck cryo-chain performance more-than-doubled mission lifetime
8 2014 release: Planck full mission 2013 Nominal SS1 SS2 SS3 yr1 Phase φ = release takes full advantage of multiple full-sky redundancies (main motivation for extension) 2014 HFI LFI Extension 1 (LFI+HFI) SS1 SS2 SS3 SS4 yr1 yr2 Phase φ = 340 Extension 2 (LFI Only) SS1 SS2 SS3 SS4 yr1 yr2 Phase φ = 340 SS5 φ = 250 SS5 yr3 Due to Planck scanning strategy, odd and even surveys couple differently with sky signal SS6 SS7 SS8 yr4 Phase φ = 250 Galactic straylight (simulation) Odd survey Even survey
9 Planck scanning strategy Phase shift between S4 and S5 At beginning of Survey 5 the precession phase ϕ was shifted by ϕ = 90 degrees with a dedicated maneuvre Field of view (Spin rate: 1rpm) Precession circle, ω = 2π/6months Sun 85 θ = 7.5 ϕ Sun-Planck direction 1 /day Boresight (85 from spin axis)
10 Planck scanning strategy Phase shift between S4 and S5 At beginning of Survey 5 the precession phase ϕ was shifted by ϕ = 90 degrees with a dedicated maneuvre Field of view (Spin rate: 1rpm) Precession circle, ω = 2π/6months Sun θ = 7.5 ϕ = 90 Sun-Planck direction 1 /day Boresight (85 from spin axis)
11 Planck sensitivity Noise measured in-flight, full mission (CMB channels) 30GHz 44GHz 70GHz 100GHz 143GHz 217GHz 353GHz Angular resolution [arcmin] Noise sensitivity [µk CMB s 1/2 ] NOISE/PIXEL From detector sensitivity [µk CMB ] Measured from maps [µk CMB ] Extended mission [months] End-of-missioni [µk CMB ] Measured End-of-Mission [ T/T, µk/k] : Blue book GOAL [ T/T, µk/k] : Red book GOAL [ T/T, µk/k] ~ 2 At end of mission Planck fulfills completely the very ambitious sensitivity goals proposed in the design phase several years ago
12 Dipole calibration: Planck vs WMAP 2014: Orbital dipole calibration for both LFI and HFI Amplitude (µk) Latitude (deg) Longitude (deg) LFI ± HFI ± ± ±0.03 Planck (LFI+HFI) ± ± ±0.03 WMAP 3355± ± ±0.14 Accuracy ~0.05%, limited by foregrounds Residual dipoles from component separation: ~1µK Very good agreement with WMAP (1σ, 0.3% amplitude, 3 direction)
13 Calibration consistency LFI vs HFI, Planck vs WMAP LFI vs HFI Planck vs WMAP Temperature ratio HFI100 / LFI70 HFI143 / LFI70 Temperature ratio LFI70 / WMAP-V HFI100 / WMAP-W LFI70 / WMAP-V (2013) HFI100 / WMAP-W (2013) Internal consistency confirmed by tests from component separation analysis Changes in LFI and HFI since 2013 from better control of (independent) systematics and beams Excellent consistency between independent experiments
14 Planck 2014 frequency maps: Temperature 30GHz 44GHz 70GHz 100 GHz 143 GHz 217 GHz 353 GHz 545 GHz 857 GHz
15 Planck Temperature power spectrum
16 Planck Temperature power spectrum
17 Planck 2014 frequency maps: Polarisation 30GHz 44GHz Q U
18 Planck 2014 frequency maps: Polarisation 70GHz 353GHz Q U
19 Planck polarisation power spectra BlueBook predictions TE Planck 2014 TT best fit model EE TT best fit model 2014 Low-ell polarisation: based on 70GHz, cleaned with 30GHz and 353GHz
20 Component separation Temperature CMB maps: 4 versions coming from different methods SMICA, SEVEM, COMMANDER, NICL Excellent agreement Polarisation CMB map (ell>30) Foregrounds: dust, synchrotron 30GHz Foregrounds: dust, synchrotron, free-free, spinning dust, diffuse SZ, CO 353GHz
21 Estimating B-contamination from foregrounds Planck multifrequency polarisation maps provide unique support to new generation of ground-based experiments seeking to measure B-modes North South Power Collaborative effort is on-going between Bicep2/Keck/Planck teams Bicep2 field Uncertainty Planck Collaboration, 2014 A&A Submitted arxiv:
22 Summary of main products of 2014 Planck release - Frequency maps: intensity and polarization: 30,44,70,353 GHz; intensity only: GHz and GHz; - CMB map: intensity and polarization (ell> 30), four versions from comp separation methods; - Likelihood: CMB+lensing Temp+Pol; - Low-ell likelihood based on LFI 70 GHz (replaces WMAP); - Foregrounds: dust (temp and pol), synchrotron (temp and pol), free-free, spinning dust, diffuse SZ emission (temp), CO emission; - Map of integrated lensing potential; - New catalogue of compact sources; - New catalogue of SZ sources (from 1227 to 1653 sources; cosmological sample more than doubled) - And more Aim at delivering data & papers before end of 2014
23 The scientific results that we present today are a product of the Planck Collaboration, which includes individuals from more than 100 scientific institutes in Europe, the USA and Canada Planck is a project of the European Space Agency, with instruments provided by two scientific Consortia funded by ESA member states (in particular the lead countries: France and Italy) with contributions from NASA (USA), and telescope reflectors provided in a collaboration between ESA and a scientific Consortium led and funded by Denmark.
The microwave sky as seen by Planck
The microwave sky as seen by Planck Ingunn Kathrine Wehus Jet Propulsion Laboratory California Institute of Technology on behalf of the Planck Collaboration Bayesian component separation We adopt a parametric
More informationTHE PLANCK MISSION The most accurate measurement of the oldest electromagnetic radiation in the Universe
THE PLANCK MISSION The most accurate measurement of the oldest electromagnetic radiation in the Universe Rodrigo Leonardi Planck Science Office ESTEC/ESA OVERVIEW Planck observational objective & science.
More informationThe international scenario Balloons, LiteBIRD, PIXIE, Millimetron
The international scenario Balloons, LiteBIRD, PIXIE, Millimetron Francesco Piacentini Sapienza Università di Roma, Dipartimento di Fisica on behalf of the Italian CMB community Overview International
More informationLFI frequency maps: data analysis, results and future challenges
LFI frequency maps: data analysis, results and future challenges Davide Maino Università degli Studi di Milano, Dip. di Fisica New Light in Cosmology from the CMB 22 July - 2 August 2013, Trieste Davide
More informationThe CMB in Italy. Marco Bersanelli Università degli Studi di Milano on behalf of the Italian CMB community
The CMB in Italy Marco Bersanelli Università degli Studi di Milano on behalf of the Italian CMB community The CMB and the era of precision Cosmology Special status of CMB for precision science: - Simple
More informationBipoSH Representation: Modulation & Systematics
Isotropy of Planck map in C l L=0 BipoSH Representation: Modulation & Systematics Planck 2013 results. XXIII. Isotropy and statistics of the CMB L=10 Spherical harmonic l Planck unveils the Cosmic Microwave
More informationPlanck. Report on the status of the mission Carlo Baccigalupi, SISSA
Planck Report on the status of the mission Carlo Baccigalupi, SISSA Outline CMB The Planck satellite Data processing center Expectations from Planck Planck data CMB CMB angular power spectrum Angle 200/l
More informationCMB studies with Planck
CMB studies with Planck Antony Lewis Institute of Astronomy & Kavli Institute for Cosmology, Cambridge http://cosmologist.info/ Thanks to Anthony Challinor & Anthony Lasenby for a few slides (almost) uniform
More informationPLANCK lately and beyond
François R. Bouchet, Institut d Astrophysique de Paris PLANCK lately and beyond CORE/M5 TT, EE, BB 2016 status Only keeping points w. sufficiently small error bars, Fig. E Calabrese τ = 0.055±0.009 1 114
More informationWhat I heard about Planck Eiichiro Komatsu (MPA) December 9, 2014 December 22, 2014
What I heard about Planck 2014 Eiichiro Komatsu (MPA) [v1@ipmu] December 9, 2014 [v2@utap] December 22, 2014 Disclaimer I am not involved in Planck I did not attend the conference in Ferrara, Italy, for
More informationLarge Scale Polarization Explorer
Science goal and performance (Univ. Roma La Sapienza) for the LSPE collaboration Page 1 LSPE is a balloon payload aimed at: Measure large scale CMB polarization and temperature anisotropies Explore large
More information4.3 Planck. Scientific goals. Planck payload
4.3 Planck In late 1992, the NASA COBE team announced the detection of intrinsic temperature fluctuations in the Cosmic Background Radiation Field (CBRF), observed on the sky at angular scales larger than
More informationThe CMB sky observed at 43 and 95 GHz with QUIET
The CMB sky observed at 43 and 95 GHz with QUIET Hans Kristian Eriksen for the QUIET collaboration University of Oslo Munich, November 28th, 2012 QUIET (Q/U Imaging ExperimenT) QUIET is a ground-based
More informationPoS(MULTIF2017)017. Highlights of Planck results
European Space Agency Scentific Support Office Keplerlaan 1 2201AZ Noordwijk The Netherlands E-mail: jtauber@cosmos.esa.int The aim of my presentation was to summarize the main cosmological results obtained
More informationThe first light in the universe
The first light in the universe Aniello Mennella Università degli Studi di Milano Dipartimento di Fisica Photons in the early universe Early universe is a hot and dense expanding plasma 14 May 1964, 11:15
More informationPILOT. A far-infrared balloon-borne polarization experiment. Jonathan Aumont IRAP Toulouse, France
PILOT A far-infrared balloon-borne polarization experiment Jonathan Aumont IRAP Toulouse, France J.-Ph. Bernard (PI), A. Mangilli, A. Hughes, G. Foënard, I. Ristorcelli, G. De Gasperis, H. Roussel, on
More informationPlanck constraints on neutrinos. Massimiliano Lattanzi Università di Ferrara on behalf of the Planck Collaboration
Planck constraints on neutrinos Massimiliano Lattanzi Università di Ferrara on behalf of the Planck Collaboration The Cosmic Neutrino Background (CnB) The presence of a background of relic neutrinos is
More informationShort course: 101 level introductory course to provide a foundation for everyone coming to the workshop to understand the field.
Designing future CMB experiments: how this will work Short course: 101 level introductory course to provide a foundation for everyone coming to the workshop to understand the field. Study visions and goals
More informationMeasurements of the CMB by the PLANCK satellite
Measurements of the CMB by the PLANCK satellite M.C. Falvella Italian Space Agency (ASI) on behalf of Planck collaboration In 1992 two space-based CMB experiments (COBRAS and SAMBA) were proposed to ESA.
More informationFirst Results from the Planck satellite A satellite to measure the Universe
First Results from the Planck satellite A satellite to measure the Universe F.-X. Désert IPAG: Institut de Planétologie et d Astrophysique de Grenoble and LPSC + Institut Néel-MCBT The Mission Makers ESA
More informationarxiv: v1 [astro-ph.co] 3 Feb 2016
Astronomische Nachrichten, 1 October 2018 Excess B-modes extracted from the Planck polarization maps H. U. Nørgaard - Nielsen National Space Institute (DTU Space), Technical University of Denmark, Elektrovej,
More informationScientific results from QUIJOTE. constraints on CMB radio foregrounds
Scientific results from QUIJOTE constraints on CMB radio foregrounds Flavien Vansyngel, Instituto de Astrofísica de Canarias, on the behalf of the QUIJOTE collaboration @ 53rd rencontres de Moriond The
More informationChallenges present and future in the observation of the Cosmic Microwave Background
Challenges present and future in the observation of the Cosmic Microwave Background Aniello (Daniele) Mennella Università degli Studi di Milano Dipartimento di Fisica Today Today We're looking at the universe
More informationData analysis of massive data sets a Planck example
Data analysis of massive data sets a Planck example Radek Stompor (APC) LOFAR workshop, Meudon, 29/03/06 Outline 1. Planck mission; 2. Planck data set; 3. Planck data analysis plan and challenges; 4. Planck
More informationDust Polarization. J.Ph. Bernard Institut de Recherche en Astrophysique et Planetologie (IRAP) Toulouse
Dust Polarization J.Ph. Bernard Institut de Recherche en Astrophysique et Planetologie (IRAP) Toulouse 1 Layout - Dust polarization (Extinction) - Dust polarization (Emission) - Dust polarization observational
More informationPrimordial B-modes: Foreground modelling and constraints
Primordial B-modes: Foreground modelling and constraints Carlo Contaldi Imperial College London Model Polarisation Amplitude 40 60-180 160 140 120 100 20 80 0 60 40 20 0-20 -40-60 -80-100 -120-140 -160-20
More informationExploring the primordial Universe with QUBIC
Exploring the primordial Universe with the Q U Bolometric Interferometer for Cosmology J.-Ch. Hamilton, APC, Paris, France (CNRS, IN2P3, Université Paris-Diderot) Expected difficulties in the B-Modes Quest
More informationBINGO simulations and updates on the performance of. the instrument
BINGO simulations and updates on the performance of BINGO telescope the instrument M.-A. Bigot-Sazy BINGO collaboration Paris 21cm Intensity Mapping Workshop June 2014 21cm signal Observed sky Credit:
More informationOVERVIEW OF NEW CMB RESULTS
OVERVIEW OF NEW CMB RESULTS C. R. Lawrence, JPL for the Planck Collaboration UCLA Dark Matter 2016 2016 February 17 Overview of new CMB results Lawrence 1 UCLA, 2016 February 17 Introduction Planck First
More informationPlanck and Virtual Observatories: Far Infra-red / Sub-mm Specificities
JF Sygnet (Planck HFI DPCM) Planck and Virtual Observatories: Far Infra-red / Sub-mm Specificities Planck Mission, Planck Data and its Specificities (4) Data Treatment and its Specificities (4) Planck
More informationFirst scientific results from QUIJOTE. constraints on radio foregrounds
First scientific results from QUIJOTE constraints on radio foregrounds Flavien Vansyngel, Instituto de Astrofísica de Canarias @ CMB Foregrounds, UCSD, 2017/11/29 The QUIJOTE experiment Tenerife experiment
More informationQUIET-I and QUIET-II:
QUIET-I and QUIET-II: HEMT-based coherent CMB polarimetry Great Lakes Cosmology Workshop X June 14, 2010 Immanuel Buder (for the QUIET Collaboration) Department of Physics, U. of Chicago Outline Science
More informationMeasurements of Degree-Scale B-mode Polarization with the BICEP/Keck Experiments at South Pole
Measurements of Degree-Scale B-mode Polarization with the BICEP/Keck Experiments at South Pole Benjamin Racine for the BICEP/Keck Collaboration March 18th, 2018 53 èmes Rencontres de Moriond La Thuile
More informationPrimordial gravitational waves detected? Atsushi Taruya
21 May 2014 Lunch seminar @YITP Primordial gravitational waves detected? Atsushi Taruya Contents Searching for primordial gravitational waves from cosmic microwave background polarizations Gravitational-wave
More informationConsistency tests for Planck and WMAP in the low multipole domain
PREPARED FOR SUBMISSION TO JCAP arxiv:1305.4033v1 [astro-ph.co] 17 May 2013 Consistency tests for Planck and WMAP in the low multipole domain A. Frejsel, M. Hansen and H. Liu Niels Bohr Institute and Discovery
More informationPreparation to the CMB Planck analysis: contamination due to the polarized galactic emission. L. Fauvet, J.F. Macías-Pérez
Preparation to the CMB Planck analysis: contamination due to the polarized galactic emission 1, J.F. Macías-Pérez Polarized foregrounds 3D model of the galaxy: optimization Expected constraints with Planck
More informationNews from BICEP/Keck Array CMB telescopes
News from BICEP/Keck Array CMB telescopes Zeeshan Ahmed KIPAC, SLAC National Accelerator Laboratory Pi Day, 2016 Southern Methodist University Outline 1. Cosmology CMB, Inflation, B-modes 2. The Compact
More informationSPIDER: A Balloon-Borne Polarimeter for Measuring Large Angular Scale CMB B-modes
SPIDER: A Balloon-Borne Polarimeter for Measuring Large Angular Scale CMB B-modes, Dick Bond, Olivier Doré CITA, University of Toronto, Canada E-mail: cmactavi@cita.utoronto.ca Rick Bihary, Tom Montroy,
More informationPlanck 2015 parameter constraints
Planck 2015 parameter constraints Antony Lewis On behalf of the Planck Collaboration http://cosmologist.info/ CMB temperature End of inflation Last scattering surface gravity+ pressure+ diffusion Observed
More informationHerschel and Planck: ESA s New Astronomy Missions an introduction. Martin Kessler Schloss Braunshardt 19/03/2009
Herschel and Planck: ESA s New Astronomy Missions an introduction Martin Kessler Schloss Braunshardt 19/03/2009 Missions in Operations Rosetta Hubble Integral Newton Mars Express SOHO Ulysses Cluster Venus
More informationThe Planck mission. 0.1 From wishes and hopes to bits on the ground
The Planck mission François R. Bouchet Institut d Astrophysique de Paris (IAP), CNRS & UPMC, 98 bis Bd Arago, F75014, Paris On behalf of the Planck collaboration for the results. All further mistakes are
More informationarxiv:astro-ph/ v1 9 Dec 2001
XXX-XXXXX YYY-YYYYYY November 2, 2018 arxiv:astro-ph/0112205v1 9 Dec 2001 Archeops: CMB Anisotropies Measurement from Large to Small Angular Scale Alexandre Amblard, on behalf of the Archeops Collaboration
More informationCosmology Large Angular Scale Surveyor. Wednesday, September 25, 13
Cosmology Large Angular Scale Surveyor T. Marriage for the CLASS Collaboration U. Michigan Cosmology After Planck Sep 24, 2013 CLASS Collaborators NASA GSFC D. Chuss K. Denis A. Kogut N. Miller H. Moseley
More informationCMB anomalies (in WMAP9 and Planck)
CMB anomalies (in WMAP9 and Planck) Dragan Huterer Physics Department University of Michigan Copi, Huterer, Schwarz & Starkman arxiv:1310.3831 (low power) arxiv:1311.4862 (alignments) review in Adv. Astro.,
More informationPLANCK SZ CLUSTERS. M. Douspis 1, 2
SF2A 2011 G. Alecian, K. Belkacem, R. Samadi and D. Valls-Gabaud (eds) PLANCK SZ CLUSTERS M. Douspis 1, 2 Abstract. We present here the first results on galaxy clusters detected by the Planck satellite
More informationToward an Understanding of Foregrounds in the BICEP2 Region
Toward an Understanding of Foregrounds in the BICEP2 Region Raphael Flauger JCAP08(2014)039 (arxiv:1405.7351) w/ Colin Hill and David Spergel Status and Future of Inflationary Theory, KICP, August 22,
More informationPlanck. Ken Ganga. APC/CNRS/ University of Paris-Diderot
Planck Ken Ganga APC/CNRS/ University of Paris-Diderot A Brief History of the Cosmos The CMB was emitted when the Universe was about 3 10-5 of its current age. 2 Planck/HFI Timeline The HFI builds on the
More informationDoppler boosting the CMB
Doppler boosting the CMB Based on Planck 2013 Results. XXVII. Doppler boosting of the CMB Douglas Scott on behalf of the Planck Collaboration Doppler boosting the CMB Based on Planck 2013 Results. XXVII.
More informationConstraints on inflationary models of the Universe based on CMB data
Astrophysics Group Cavendish Laboratory Constraints on inflationary models of the Universe based on CMB data Andrés Curto Martín Enrique Martínez González 8 th RES User Conference, Santander, 23/Sept/2014
More informationFirst Cosmology Results from Planck. Alessandro Melchiorri University of Rome La Sapienza On behalf of the Planck collaboration
First Cosmology Results from Planck Alessandro Melchiorri University of Rome La Sapienza On behalf of the Planck collaboration Planck Collaboration 300+ names Planck Core-Team (a fraction of it) Planck
More informationThe cosmic background radiation II: The WMAP results. Alexander Schmah
The cosmic background radiation II: The WMAP results Alexander Schmah 27.01.05 General Aspects - WMAP measures temperatue fluctuations of the CMB around 2.726 K - Reason for the temperature fluctuations
More informationThe ultimate measurement of the CMB temperature anisotropy field UNVEILING THE CMB SKY
The ultimate measurement of the CMB temperature anisotropy field UNVEILING THE CMB SKY PARAMETRIC MODEL 16 spectra in total C(θ) = CMB theoretical spectra plus physically motivated templates for the
More informationC-BASS: The C-Band All-Sky Survey. Luke Jew
C-BASS: The C-Band All-Sky Survey Luke Jew The C-Band All-Sky Survey All-sky map 5GHz (bandwidth 1GHz) Resolution ~0.73 degrees Stokes I, Q & U High S/N (0.1mK beam -1 ) 1. Overview of project 2. Current
More informationFuture experiments from the Moon dedicated to the study of the Cosmic Microwave Background
Future experiments from the Moon dedicated to the study of the Cosmic Microwave Background C. Burigana, A. De Rosa, L. Valenziano, R. Salvaterra, P. Procopio, G. Morgante, F. Villa, and N. Mandolesi Cosmic
More informationForthcoming CMB experiments and expectations for dark energy. Carlo Baccigalupi
Forthcoming CMB experiments and expectations for dark energy Carlo Baccigalupi Outline Classic dark energy effects on CMB Modern CMB relevance for dark energy: the promise of lensing Lensing (B modes)
More informationCMB Lensing Reconstruction on PLANCK simulated data
CMB Lensing Reconstruction on PLANCK simulated data L. Perotto, J. Bobin, S. Plaszczynski, J.-L. Starck, A. Lavabre Laurence Perotto - LAL Orsay ADA V, may 7-9 Outlines CMB lensing as a cosmological tools
More informationPower spectrum exercise
Power spectrum exercise In this exercise, we will consider different power spectra and how they relate to observations. The intention is to give you some intuition so that when you look at a microwave
More informationPrecise measurement of CMB polarisation from Dome-C: the BRAIN and CLOVER experiments
Precise measurement of CMB polarisation from Dome-C: the BRAIN and CLOVER experiments M. Piat, C. Rosset To cite this version: M. Piat, C. Rosset. Precise measurement of CMB polarisation from Dome-C: the
More informationThe Planck Telescope
The Planck Telescope F.Villa 1, M.Bersanelli 2, C.Burigana 1, R.C.Butler 1, N.Mandolesi 1, A.Mennella 3, G.Morgante 1, M.Sandri 1, L.Terenzi 1, L.Valenziano 1 1 Istituto TESRE/CNR Bologna Italy 2 Università
More informationTitle Sunyaev Zel dovich Signal & Cross Correlations
Title Sunyaev Zel dovich Signal & Cross Correlations Relatore Pasquale Mazzotta Universita di Roma Tor Vergata on behalf of the Italian CMB community Overview Cosmic web and Clusters of Galaxies Observing
More informationThe PLANCK Cluster Catalog:
The PLANCK Cluster Catalog: SZ/X-ray Expected Properties Antoine Chamballu James G. Bartlett Jean-Baptiste Melin in the framework of the Planck consortium The Planck mission Background Successfully launched
More informationPILOT balloon experiment
PILOT balloon experiment J.-Ph. Bernard CESR Toulouse Context: Planck & B-pol Polarized foregrounds The PILOT experiment PILOT:Science Objectives Polarized Instrument for Long-Wavelength Observations of
More informationThe Planck Mission and Ground-based Radio Surveys
The Planck Mission and Ground-based Radio Surveys Russ Taylor University of Calgary Kingston Meeting UBC, November 2003 Current state of that art in ground-based radio surveys How Planck factors into the
More informationDetection of B-mode Polarization at Degree Scales using BICEP2. The BICEP2 Collaboration
Detection of B-mode Polarization at Degree Scales using BICEP2 The BICEP2 Collaboration 2 The BICEP2 Postdocs Colin Bischoff Immanuel Buder Jeff Filippini Stefan Fliescher Martin Lueker Roger O Brient
More informationPICO - Probe of Inflation and Cosmic Origins
PICO - Probe of Inflation and Cosmic Origins Shaul Hanany University of Minnesota Executive Committee Bock, Borrill, Crill, Devlin, Flauger, Hanany, Jones, Knox, Kogut, Lawrence, McMahon, Pryke, Trangsrud
More informationPlanck Mission and Technology
Planck Mission and Technology Petri Jukkala, Nicholas Hughes, Mikko Laaninen, Ville-Hermanni Kilpiä YLINEN Electronics Ltd Jussi Tuovinen, Jussi Varis, Anna Karvonen MilliLab, VTT Information Technology
More informationCMB polarization and cosmology
Fundamental physics and cosmology CMB polarization and cosmology Institut d'astrophysique Spatiale Orsay Standard cosmology : reverse the expansion... 10 16 GeV GUT 10-42 s 10 15 GeV 10-32 s 300 GeV 0.1
More informationX name "The talk" Infrared
X name "The talk" Infrared 1 Cosmic Infrared Background measurement and Implications for star formation Guilaine Lagache Institut d Astrophysique Spatiale On behalf of the Planck collaboration Cosmic Infrared
More informationPhysics of CMB Polarization and Its Measurement
Physics of CMB Polarization and Its Measurement HEP seminar at Kyoto University April 13 th, 2007 Akito KUSAKA University of Tokyo Outline Physics of CMB and its Polarization What does WMAP shed light
More informationD une masse de données à une poignée de paramètres cosmologiques: quelques aperçus sur le traitement des données du satellite Planck.
Journée thématique : Traitement de masses de données. 11 Déc. 2013 Séminaire Méthodes Mathématiques du Traitement d Images. Laboratoire Jacques-Louis Lions. UPMC. D une masse de données à une poignée de
More informationThe Einstein Polarization Interferometer for Cosmology (EPIC)
The Einstein Polarization Interferometer for Cosmology (EPIC) Peter Timbie UW-Madison for the EPIC collaboration Brown, Cardiff, Illinois, Ireland-Maynooth, LLNL, Manchester, Richmond, UCSD, Wisconsin,
More informationThe X-ray view of Planck SZ clusters
The X-ray view of Planck SZ clusters M. ARNAUD CEA- Service d Astrophysique On behalf of the Planck collaboradon With inputs from non- Planck sciendsts The Planck catalogue of SZ sources ESZ Planck Early
More informationPolarised foregrounds (synchrotron, dust and AME) and their effect on the detection of primordial CMB B-modes
Polarised foregrounds (synchrotron, dust and AME) and their effect on the detection of primordial CMB B-modes Ricardo T. Génova Santos Instituto de Astrofísica de Canarias Cosmology School in the Canary
More informationAME characterisation in the Taurus Molecular Clouds with the QUIJOTE experiment
AME characterisation in the Taurus Molecular Clouds with the QUIJOTE experiment Frédérick Poidevin Marie-Curie Individual Fellow at IAC-Tenerife, Spain With the QUIJOTE team. ESA/ESTEC, 23 June, 20156
More informationPlanck was conceived to confirm the robustness of the ΛCDM concordance model when the relevant quantities are measured with much higher accuracy
12-14 April 2006, Rome, Italy Francesco Melchiorri Memorial Conference Planck was conceived to confirm the robustness of the ΛCDM concordance model when the relevant quantities are measured with much higher
More informationMichel Piat for the BRAIN collaboration
Precise measurement of CMB polarisation from Dome-C: the BRAIN experiment Michel Piat for the BRAIN collaboration Laboratoire Astroparticule et Cosmologie Université Paris 7 Denis Diderot 1 Outline 1.
More informationConstraints on Neutrino Physics from Cosmology
Constraints on Neutrino Physics from Cosmology The Future of Neutrino Mass Measurements 4th February 2013, Milano Bicocca Alessandro Melchiorri Universita di Roma, La Sapienza Xmas 2012: a very good one
More informationChallenges of foreground subtraction for (primordial) CMB B-modes
Challenges of foreground subtraction for (primordial) CMB B-modes Clive Dickinson Jodrell Bank Centre for Astrophysics University of Manchester Bennett et al. (2013) CMB2013, OIST, Okinawa, Japan, 10-14
More informationGalactic radio loops. Philipp Mertsch with Subir Sarkar. The Radio Synchrotron Background Workshop, University of Richmond 21 July 2017
Galactic radio loops Philipp Mertsch with Subir Sarkar The Radio Synchrotron Background Workshop, University of Richmond 21 July 2017 Foregrounds in B-modes Adam et al., arxiv:1502.01588 1409.5738 (Planck
More informationCosmic Microwave Background
Cosmic Microwave Background Following recombination, photons that were coupled to the matter have had very little subsequent interaction with matter. Now observed as the cosmic microwave background. Arguably
More informationThe Planck high-l temperature and polarization CMB power spectra and likelihood
The Panck high- temperature and poarization CMB power spectra and ikeihood Franz Esner on behaf of the Panck coaboration 1/12/14 Overview Updates since 213 Part 1: Power spectra Anaysis masks The Panck
More informationCMB component separation intution and GreenPol
CMB component separation intution and GreenPol Hans Kristian Eriksen University of Oslo Nordita, Stockholm July 2017 in collaboration with Unni Fuskeland, Ari Kaplan, Ingunn Wehus, Hao Liu, Phil Lubin,
More informationastro-ph/ Sep 1996
THE CMB DIPOLE: THE MOST RECENT MEASUREMENT AND SOME HISTORY Charles H. Lineweaver astro-ph/9609034 5 Sep 1996 Universite Louis Pasteur Observatoire Astronomique de Strasbourg 11 rue de l'universite, 67000
More informationFOUR-YEAR COBE 1 DMR COSMIC MICROWAVE BACKGROUND OBSERVATIONS: MAPS AND BASIC RESULTS
THE ASTROPHYSICAL JOURNAL, 464 : L1 L4, 1996 June 10 1996. The American Astronomical Society. All rights reserved. Printed in U.S.A. FOUR-YEAR COBE 1 DMR COSMIC MICROWAVE BACKGROUND OBSERVATIONS: MAPS
More informationFondo Cosmico di Microonde: implicazioni delle moderne osservazioni, prospettive future
Fondo Cosmico di Microonde: implicazioni delle moderne osservazioni, prospettive future Carlo Baccigalupi SISSA, Trieste Societa Italiana di Fisica Italiana September 23, 2013 Outline CMB anisotropies
More informationHerschel Mission Overview and Key Programmes
Herschel Mission Overview and Key Programmes SPIE Astronomical Instrumentation 2008 Space Telescopes and Instrumentation I: Optical, Infrared, and Millimeter Wave Marseille, 23-28 June 2008 Göran L. Pilbratt
More informationarxiv: v1 [astro-ph.co] 8 Oct 2010
Astronomy & Astrophysics manuscript no. 14288 c ESO 2017 July 13, 2017 Foreground removal from WMAP 5 yr temperature maps using an MLP neural network 1 National Space Institute (DTU Space), Technical University
More informationIn-Flight Retrieval of Reflector Anomalies for the Planck Space Telescope
Presented at The 4 th European Conference on Antennas and Propagation (EuCAP 2010), Barcelona, Spain, 12-16 April 2010. In-Flight Retrieval of Reflector Anomalies for the Planck Space Telescope Frank Jensen*,
More informationMicrocosmo e Macrocosmo
Microcosmo e Macrocosmo Paolo de Bernardis Dipartimento di Fisica Sapienza Università di Roma Lezioni della Cattedra Fermi 23 Gennaio 2014 Dipartimento di Fisica Sapienza Università di Roma Friedman s
More informationHigh latitude Galactic dust emission in the BOOMERanG maps
High latitude Galactic dust emission in the BOOMERanG maps S. Masi 1, P.A.R. Ade 2,J.J Bock 3,4, A. Boscaleri 5, B.P. Crill 3, P. de Bernardis 1, M. Giacometti 1, E. Hivon 3, V.V. Hristov 3, A.E. Lange
More informationReally, really, what universe do we live in?
Really, really, what universe do we live in? Fluctuations in cosmic microwave background Origin Amplitude Spectrum Cosmic variance CMB observations and cosmological parameters COBE, balloons WMAP Parameters
More informationPIXIE: The Primordial Inflation Explorer. Al Kogut GSFC
PIXIE: The Primordial Inflation Explorer Al Kogut GSFC History of the Universe Standard model leaves many open questions NASA Strategic Guidance: 2010 Astrophysics Decadal Survey Top Mid-Scale Priorities
More informationCosmic Microwave Background
Cosmic Microwave Background Carlo Baccigalupi,, SISSA CMB lectures at TRR33, see the complete program at darkuniverse.uni-hd.de/view/main/winterschoollecture5 These lectures are available in pdf format
More informationTesting parity violation with the CMB
Testing parity violation with the CMB Paolo Natoli Università di Ferrara (thanks to Alessandro Gruppuso)! ISSS L Aquila 24 April 2014 Introduction The aim is to use observed properties of CMB pattern to
More informationNeutrinos in the era of precision Cosmology
Neutrinos in the era of precision Cosmology Marta Spinelli Rencontres du Vietnam Quy Nhon - 21 July 2017 The vanilla model: -CDM (Late times) cosmological probes Supernovae Ia standard candles fundamental
More informationExoplanetary transits as seen by Gaia
Highlights of Spanish Astrophysics VII, Proceedings of the X Scientific Meeting of the Spanish Astronomical Society held on July 9-13, 2012, in Valencia, Spain. J. C. Guirado, L.M. Lara, V. Quilis, and
More informationarxiv:astro-ph/ v1 12 Jan 1996
COBE Preprint 96-01, Submitted To ApJ Letters 4-Year COBE 1 DMR Cosmic Microwave Background Observations: Maps and Basic Results arxiv:astro-ph/9601067v1 12 Jan 1996 C. L. Bennett 2,3, A. Banday 4, K.
More informationPolarized Foregrounds and the CMB Al Kogut/GSFC
Polarized Foregrounds and the CMB Al Kogut/GSFC The Problem In A Nutshell Galactic foregrounds are 2 orders of magnitude brighter than primordial B-mode polarization from 30 to 200 GHz Polarized vs Unpolarized
More informationThe Quest for Gravity Wave B-modes
The Quest for Gravity Wave B-modes Clem Pryke (University of Minnesota) Moriond Conference, La Thuile 13 March, 2012 Outline Review of CMB polarization and history of detection Why go after B-modes? How
More informationCosmology with CMB & LSS:
Cosmology with CMB & LSS: the Early universe VSP08 lecture 4 (May 12-16, 2008) Tarun Souradeep I.U.C.A.A, Pune, India Ω +Ω +Ω +Ω + Ω +... = 1 0 0 0 0... 1 m DE K r r The Cosmic Triangle (Ostriker & Steinhardt)
More information