Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008
The Planck Mission:Scientific expectations
Lucia A. Popa
ISS Institute for Space Sciences, Bucharest
Scientific Expectations
Lucia Popa
ISS Institute for Space Sciences, Bucharest
Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008
Outline
Planck Mission
Looking back down to the time
Planck milestones and challenges
Cosmology @ ISS
Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008
Third generation space CMB Mission
• Primary scientific goal: measure the CMB temperaturand polarization anisotropies to fundamental limits down to 5’
• Current launch date: December 2008 together with Hershel on an Ariane 5 rocket
Schedule
• Primary anisotropiescosmological parameters, dark energy,inflation
• Secondary anisotropies:Gravitational lensing, reionization,galaxy clusters,massive neutrinos
• Non-CMB science-Extragalactic-Galactic
Broad Science
The Scientific Program of PlanckESA-SCI (2005) 1 (Blue Book)
arXiv:astro-ph/0604069
Planck home page: http://www.rsd.esa.int/index.phd?project=Planck
Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008
Instruments
Planck frequencies & Foregrounds WMAP frequencies & Foregrounds
Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008
• CMB photons emerge from the photosphere at recombination
•Temperature inhomogeneities at recombination become anisotropy to the observer at present
• Spot sizes ranging from fraction of a degree to 180 degrees
• Spots of a given angular scale gives the power spectrum
• linear theory510
cmbT
T
KTcmb 004.02728.2
COBE: http://aether.lbl.gov/www/projects/cobe
Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008
Anisotropy Formation
Initial temperature inhomogeneities oscillate as sound waves in the plasma before recombination
- T ~ 3000 K photons ionize hydrogen- Coulomb interactions + Thomson scattering: baryon-photon plasma – perfect fluid - Fluid falls into CDM potential wells : acoustic oscillations - Oscillations frozen at recombination -Compression=hot spots Rarefaction=cold spots-Hot and cold spots appear as temperature anisotropies
Spectrum of sound shows harmonics at integer ratios of the fundamental based on the distance sound travels by recombination
• First peak = mode that just compresses• Second peak = mode that compresses then rarefies• Harmonic peaks: 1:2:3 in wavenumber
Angular scales measure the angular diameter distance to recombination involving the curvature,dark energy, matter and radiation content of the Universe
)(
)(
recA
recs
zd
zr
Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008
Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008
Acoustic peaks structure of the CMB power spectrum: direct confirmation of the cosmological modelCDM
mor
e cl
ump
y
Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008
First acoustic peak: curvature of the Universe
mk 1
k< 0 open= 0 flat> 0 closed
CMBCMB + HSTCMB +HST + SN1ASN1A
027.0357.0 m
030.0742.0
100.0085.0099.1
tot
direct prediction of inflation
Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008
Second acoustic peak : baryonic content of the Universe
• baryons drag the fluid into potential wells• enhance the compressional peaks (odd) over the rarefaction peaks (even)
e.g. suppression of the second peak
0030.0041.0 b
agreement with BBN prediction
Third acoustic peak : Cold Dark Matter content of the Universe 027.0214.0 cdm
W. Hu ( 2007 )
Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008
Toward the Standard Cosmological Model
Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008
f=/cdm
M. Tegmark (1998)
Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008
Milestones: Past & Present
• Large-scale anisotropy: COBE DMR 1992
• Degree-scale anisotropy many: 1993-1999
• First acoustic peak: Toco, Boom, Maxima, WMAP 1999 -2008
• Secondary acoustic peak(s): DASI, Boom 2001
• Damping tail CBI: 2002
W. Hu (2001)
Measurement + Data reduction +Physical assumptions
Cosmic Variance:
Anisotropy power spectrum:
Homogeneity and Isotropy: ),(Y a
TΔT
ml,l
l
lmml,
,
Random Gaussian field:
12l
Cδδaa ensl
mmllmlml, ''''
enslC
ensl
1/21/22
ensllCVl C
12l2
C C ΔC
Criticalities: fsky , angular resolution, sensitivity (μK/pixel)
0a ml,
Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008
Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008
Friedmann-Robertson-Walker metric perturbation:
Expansion rate:
Phase-space evolution in the expanding Universe:
Energy-momentum tensor Tμ:
Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008
First-order perturbed Einstein equation:
photons
Neutrios
cdm
baryons
Λ
m3=0.05 eV
m2=0.009 eV
m1≈ 0 eV
Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008
CDM standard cosmological model
CDM issues:
• Dark Matter: cold, warm, hot
• Nature of Dark Energy: -cosmological constant or quintessence filed -equation of state: constant or time varying -GR is not correct?
• Primordial density perturbations generation mechanism: Inflation or Topological Defects (strings, global monopoles, textures, etc…)
• Reionization of the IGM
Planck Milestone 1: to measure the CMB temperature anisotropy power spectrum limited only by
the cosmic variance out into the damping tail.
Planck has : 10 × the sensitivity of WMAP 3 × the angular resolution
Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008
Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008
Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008
Planck Milestone 2: to measure the CMB polarization power spectrum (E-mode) up to l=1000
Limiting factors: - knowledge of polarized foregrounds at Planck frequencies - instrumental noise
Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008
Planck Milestone 3: challenge the Cosmological Standard Model
- break the cosmological parameters degeneracy
- Increase the precision of all cosmological parameters: high discovery potential
Baryon density
Cold Dark Matter density
Optical depth to reionization of IGM
Primordial perturbations spectral index
Running
Primordial amplitude
Hubble constant
WMAP
Planck
Planck challenge 1: detection of B-mode polarization of the CMB as signature of primordial gravitational waves
Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008
Polarization is generated by Thomson scattering of the anisotropic radiation
Anisotropies can be generated by: scalar perturbation: E-mode polarization E’ (n’) = E (n) gravitational waves: B-mode polarization B’ (n’) = B (n)
- Amplitude ~ energy scale of inflation inf2
2
EA
AR
s
t 1.0R GeVE 16inf 102
Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008
Inflation observables:
Nature of density perturbations:
• Adiabatic • Isocurvature • Mix
Slow-roll inflation conditions:
Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008
Present
r=0.1
Planck
Vacuum Energy Density: cosmological constant or quintessence ?
Common parameterization: 1wpρ
Cosmological constant: w=-1
Dynamical Dark Energy generated by a scalar field (cosmon): w(t) <
-1
Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008
Planck challenge 2
Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008
Quintessence slows down the growth of structure
Gravitational potential can be statistically reconstructed from the CMB maps
z~1100 z=0
CMB weak lensing
Planck BPOL
Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008
Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008
without lensing
with with lensinglensing
f = Ω/ΩdmeVmi 1
eVmi 3.0
A. Lewis (2006)
Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008
Lesgourgues et al. (2006)
Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008
ijI 2 X 2 tensor
11I 12I
21I 22I
T=(I11+I22)/4
Q=(I11-I22)/2
U=I12/2
•After Planck, we will have precise knowledge of the Universe at z 1000
• We will have tightly constrained the physics densities of matter and baryons, theamplitude of the fluctuations in the linear phase over three decades in lengthscale, and the shape of the primordial power spectrum
• Our knowledge of physical conditions and large-scale structure at z 1000 will bebetter than our knowledge of such quantities at z = 0
• If dark energy is a “recent” phenomenon, then we can translate this knowledgereliably to intermediate redshifts, currently at the observational frontier
• Many of the Planck achievements will be assumed as priors by future mission concepts, etc. (e.g., all JDEM concepts, Cosmic Inflation Probe, CMBPol, EUCLID)
Conclusions
Cosmology @ ISShttp://venus.nipne.ro/new1/cosmo
Main Research Topics :
•Standard and non-Standard Cosmological Models •Constraints on Cosmological Parameters •Formation and Evolution of the Cosmological Structures •Reionization History •Magnetic Field Topology in Galactic Winds •Neutrino Cosmology •Statistics and Topology of the Cosmic Radiation field
Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008
Main Projects: Planck, SPACE
SPACE: Spectroscopic All-sky Cosmic Explorer): near-infrared 3-D spectra of 109 galaxies
ESA Cosmic Vision (2015-2025)
• 1.5m non-cryogenic telescope• large-format infrared detectors with nearly perfect quantum efficiency• digital micro-mirrors (DMD) : reconfigurable focal plane for multi-object spectroscopy
Dark Energy European Mission
Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008
WMP 5-year constraints on the lepton asymmetry and radiation energy density: Implications for PLANCK, Jour. Of Cosmology and Astropart. Physics, 06, 028 (2008) arXiv:0804.2971
CMB polarization constraints on radiative feedback, Monthly Notices of the Royal Astronomical Society, Volume 385, Issue 1, pp. 404-410, 2008 arXiv:07.1913
Detectable Signature of Cosmic Radiative Feedback, Monthly Notices of the Royal Astronomical Society, Volume 384, Issue 4, pp. 1525-1532, 2008 arXiv:0712.0538
Constraints on time variation of fine structure constant from WMAP-3yr data, New Astronomy, Volume 12, Issue 8, p. 635-640 arXiv:0707.0190v1
Constraints on non-thermal Dark Matter from Planck lensing extraction, Jour. of Cosmology Astropart. Phys., 10, 017 (2007) arXiv:0708.2030
PLANCK-LFI scientific goals: Implications for the reionization history, New Astronomy Rev. 51 (3-4): 298-304 (2007)
The Planck LFI RCA flight model test campaign, New Astronomy Rev. 51 (3-4): 305-309 (2007)
The low frequency instrument on-board the Planck satellite: Characteristics and performance, New Astronomy Rev. 51 (3-4): 287-297 (2007)
Probing neutrino properties with Planck Mission, Cosmic Microwave Radiation, Aspen Center for Physics 27-Jan. – 2 Feb. 2008
Observational constraints on the lepton asymmetry and radiation endergy density, Proceedings of the Carpathian Summer School of Physics, Sinaia Aug 20-31, 2007 (edt. L. Trache, S. Stoica), American Institute of Physics Conference Proceedings
Sterile Neutrino as Dark Matter candidate from CMB alone, Proceedings of Eleventh Marcel Grossmann Meeting on General Relativity, (edt. H. Kleinert, R.T. Jantzen, R. Ruffini) World Scientific, Singapore, 2007 arXiv:astro-ph/0701331
Probing cosmic dark ages with CMB polarization measurements, Proceedings of Eleventh Marcel Grossmann Meeting on General Relativity, (edt. H. Kleinert, R.T. Jantzen and R. Ruffini) World Scientific, Singapore, 2007
Past year publications