the planck mission: scientific expectations

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


Outline

Planck Mission

Looking back down to the time

Planck milestones and challenges

Cosmology @ ISS


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

http://babbage.sissa.it/abs/astro-ph/0604069


Instruments

Planck frequencies & Foregrounds WMAP frequencies & Foregrounds


• 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


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



Acoustic peaks structure of the CMB power spectrum: direct confirmation of the cosmological modelCDM

mor

e cl

ump

y


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


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 )


Toward the Standard Cosmological Model


f=/cdm

M. Tegmark (1998)


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,



Friedmann-Robertson-Walker metric perturbation:

Expansion rate:

Phase-space evolution in the expanding Universe:

Energy-momentum tensor Tμ:


First-order perturbed Einstein equation:

photons

Neutrios

cdm

baryons

Λ

m3=0.05 eV

m2=0.009 eV

m1≈ 0 eV


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



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


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


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


Inflation observables:

Nature of density perturbations:

• Adiabatic • Isocurvature • Mix

Slow-roll inflation conditions:


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


Planck challenge 2


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



without lensing

with with lensinglensing

f = Ω/ΩdmeVmi 1

eVmi 3.0

A. Lewis (2006)


Lesgourgues et al. (2006)


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


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


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

http://babbage.sissa.it/abs/0804.2971



http://arxiv.org/abs/0707.0190v1

http://arxiv.org/abs/0708.2030

http://www.sciencedirect.com/science?_ob=ArticleURL&_udi=B6VNJ-4MSY8RB-3&_user=10&_coverDate=03%2F31%2F2007&_rdoc=1&_fmt=&_orig=search&_sort=d&view=c&_acct=C000050221&_version=1&_urlVersion=0&_userid=10&md5=ab8205d41e7516bb5605b992d5d0f2ce

http://www.sciencedirect.com/science?_ob=ArticleURL&_udi=B6VNJ-4MV1FDT-4&_user=10&_coverDate=03%2F31%2F2007&_rdoc=1&_fmt=&_orig=search&_sort=d&view=c&_acct=C000050221&_version=1&_urlVersion=0&_userid=10&md5=66b67ed5d999851bb7538a9fbaae6e42

the planck mission: scientific expectations

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