Present and (near) future CMB observations from space Marco - - PowerPoint PPT Presentation
San Servolo, Venezia 27-31 August 2007 A Century of Cosmology: Past, Present and Future Present and (near) future CMB observations from space Marco Bersanelli University of Milano San Servolo, Venezia 27-31 August 2007 A Century
San Servolo, Venezia – 27-31 August 2007 – A Century of Cosmology: Past, Present and Future
Marco Bersanelli University of Milano
Present and (near) future CMB observations from space
San Servolo, Venezia – 27-31 August 2007 A Century of Cosmology: Past, Present and Future
John C. Mather George F. Smoot
“For their discovery of the blackbody form and anisotropy of the cosmic microwave background radiation”
Cosmic Background Explorer
COBE-FIRAS COBE-DMR
High precision New discovery
San Servolo, Venezia – 27-31 August 2007 A Century of Cosmology: Past, Present and Future
Expected CMB power spectrum
San Servolo, Venezia – 27-31 August 2007 A Century of Cosmology: Past, Present and Future
) , ( ) , ( φ ϑ φ ϑ
m m mY
a T
l l l
∑
= Δ
∑
− =
+ = =
l l l l l
l
m m m
a a C
2 2
1 2 1
Multipole l = π/Θ Within Horizon
Primordial fluctuations Acoustic peaks Damping
Θ → 0° Θ = Θ2 ≈ 0.1° Θ = 180° Θ = Θ1 ≈ 1° l → ∞ l ≈ 2000 l = 1 l ≈ 180 Angular scale Θ Beyond Horizon
Anisotropy (μK2 )
DMR
20 < l
San Servolo, Venezia – 27-31 August 2007 A Century of Cosmology: Past, Present and Future
The details of the angular power spectrum depend on the value
Accurate high resolution measurements of CMB anisotropies lead to high precision determination of parameters
R M
Ω + Ω + Ω = Ω
Λ Λ
Ω
M
Ω
B
Ω
Before and after WMAP
San Servolo, Venezia – 27-31 August 2007 A Century of Cosmology: Past, Present and Future
WMAP 3yr T power spectrum and TE correlation
(Hinshaw et al 2006) All measurements before WMAP (Dec 2002)
San Servolo, Venezia – 27-31 August 2007 M.Bersanelli – Present and (near) future CMB observations from space
WMAP
1.4 × 1.6 m primary reflectors Dual back-to-back Greforian optics Secondary reflector Deployed solar array & schield Thermally isolating cylinder Passive thermal radiator Warm S/C and instrument electronics (300K) Focal plane assembly (95K) Feed horns Upper omni antenna Star tracker Reaction wheels
COBE-DMR Heritage
WMAP Instrument Assembly
Pseudo-correlation HEMT coherent radiometers
Università di MIlano
WMAP W-band feed horn Instrument Front-end Assembly
San Servolo, Venezia – 27-31 August 2007 A Century of Cosmology: Past, Present and Future
WMAP 3yr data: Systematics analysis
(Jarosik et al 2006)
The success of WMAP (and COBE) rests on accurate control of systematic effects
If not corrected, would lead to ∼mK effect on maps
Gain data 1st yr model
New model
WMAP 3yrs: six Jupiter-crossing data sets Beam solid angles found 1% larger than assumed in 1st year (1.5% effect on power spectrum).
Foregrounds
minimum of foreground contamination to T and Polarisation fluctuations is at ~ 70 GHz;
frequencies, signal (on average) is dominated by polarized galactic signal
challange
San Servolo, Venezia – 27-31 August 2007 A Century of Cosmology: Past, Present and Future
Design goals
Two complementary cryogenic instruments in focal plane: LFI: Radiometer array (20K) HFI: Bolometer array (0.1K)
Planck Scientific Programme, ESA-SCI(2005)1 (“Blue book”)
San Servolo, Venezia – 27-31 August 2007 A Century of Cosmology: Past, Present and Future
Precision cosmology with Planck: Temparature anisotropy
ESA-SCI(2005)1 (“Blue book”)
San Servolo, Venezia – 27-31 August 2007 A Century of Cosmology: Past, Present and Future
San Servolo, Venezia – 27-31 August 2007 A Century of Cosmology: Past, Present and Future
E-mode polarisation power spectrum Searching for B-mode component
r = 0.1
Planck & CMB polarisation
ESA-SCI(2005)1 (“Blue book”)
Planck SVM, Telescope & Instruments Integration
Planck Science Team: J. Tauber (ESA PS), M. Bersanelli, F. Bouchet, G. Efstathiou, J.M. Lamarre,
Planck Collaboration: ~ 400 scientists!
San Servolo, Venezia – 27-31 August 2007 A Century of Cosmology: Past, Present and Future
Planck CQM
V-grooves SVM 300K 50K 100K 150K PPLM 45K
Primary r ef lect or Ellissoidal 1.5 x 1.9 m Sub-ref lect or Ellissoidal ∼1 m Focal plane unit 20K 4K 0.1K
45K
San Servolo, Venezia – 27-31 August 2007 A Century of Cosmology: Past, Present and Future
Planck Instruments – Calibration Plan
Qualification Model (QM) Qualification Model (QM)
Unit Assembly Instrument Satellite In-flight
Flight Model (FM) Flight Model (FM) Completed Completed Completed Completed Completed Completed Completed Completed On-going On-going I n preparation I n preparation
Supported by Data Processing Centers Supported by Data Processing Centers
LFI HFI
Completed Completed Completed Completed Completed Completed
Back-end unit Back-end unit Waveguides Waveguides Blackbody calibrator Blackbody calibrator Front-end unit Front-end unit
LFI FM cryo testing LFI FM cryo testing
integrating sphere blackbody sources integrating sphere blackbody sources 2K Saturne plate 2K Saturne plate Planck/HFI PFM Planck/HFI PFM polarizer optical system polarizer optical system
HFI FM cryo testing HFI FM cryo testing
Long-duration LFI-RAA data set
45 hours of undisturbed acquisition (MODE 5)
70 GHz LFI# 19 02 Sep 2006
San Servolo, Venezia – 27-31 August 2007 A Century of Cosmology: Past, Present and Future
Long-duration LFI-RAA data set
45 hours of undisturbed acquisition (MODE 5)
70 GHz LFI# 19 02 Sep 2006
San Servolo, Venezia – 27-31 August 2007 A Century of Cosmology: Past, Present and Future
10 mHz
Knee frequency ~ 10mHz
Amplitude spectral density comparison (internal consistency)
Single diode Combined diode Unchopped data
Basic model: Radiometer Equation
Solid line = WN best fit Dashed line = Sqrt(2)* WN
San Servolo, Venezia – 27-31 August 2007 A Century of Cosmology: Past, Present and Future
Temperature and Polarisation time streams compared with relative change in T of the loads during the test.
Data stream: DAE0027, FM 70 GHz RCA21
70 GHz sensitivity to polarisation signals
T= (A+ B) + (C+ D) P= (A+ B) – (C+ D) Tsky – Tref (sensor)
No significant T bleeding into the P signal
San Servolo, Venezia – 27-31 August 2007 A Century of Cosmology: Past, Present and Future
100mK1 PID2N
San Servolo, Venezia – 27-31 August 2007 A Century of Cosmology: Past, Present and Future
HFI Cryogenic testing
100mK stability during the calibration run
143 GHz channel noise properties
Long timescale drifts correlate well with Saturne thermometry
field
SPHERE_MONIT_ISC2_TE MP interpolated and smoothed
fit to bolometer data
using linear regression and subtracted from raw, despiked bolometer timestreams
San Servolo, Venezia – 27-31 August 2007 A Century of Cosmology: Past, Present and Future
HFI Cryogenic testing
100mK stability during the calibration run
Control of Systematic effects
San Servolo, Venezia – 27-31 August 2007 A Century of Cosmology: Past, Present and Future
controlled at μK level
is a key tool to be exploited against systematics
∑
= −
⎟ ⎟ ⎠ ⎞ ⎜ ⎜ ⎝ ⎛ =
N j spin f f f
j N F
1 1
2 cos 1 ) sin( ν ν π τ πν τ πν
– QM mirrors and representative FPU and limited number of frequencies – At room temperature
RFQM measurement campaign
All beams computed with Grasp9 (nominal surfaces and alignment)
–Main beams –Intermediate beams –Full sky beams
San Servolo, Venezia – 27-31 August 2007 A Century of Cosmology: Past, Present and Future
RFQM results at 100GHz
Co-polarisation beam at 100GHz X-polarisation beam at 100GHz
Alcatel-Alenia Space; ESA; HFI + LFI Teams
Main beam
San Servolo, Venezia – 27-31 August 2007 A Century of Cosmology: Past, Present and Future
WMAP LFI 15 months 15 months Cosmic variance limit
Planck-LFI vs WMAP (V-band)
Estec, 11-12 April 2006 – M.Bersanelli PST-27 LFI Instrument Report
LFI
LFI 15 months 8yr Cosmic variance limit 4yr 1yr WMAP
Planck-LFI vs WMAP (V-band)
Estec, 11-12 April 2006 – M.Bersanelli PST-27 LFI Instrument Report
LFI
HFI 15 months Cosmic variance limit 8yr WMAP 4yr 1yr
Planck-HFI vs WMAP (W-band)
Estec, 11-12 April 2006 – M.Bersanelli PST-27 LFI Instrument Report
LFI
Planck CQM tests
Third V-groove: T <50K
Planck SVM
HFI-LFI Integration
PLM SVM mating
Well done
Telescope integration
Finally together