Spectral Distortions of CMB C Burigana A De

Spectral Distortions of CMB C. Burigana, A. De Rosa, L. Valenziano, G. Morgante, F. Villa, R. Salvaterra, P. Procopio and N. Mandolesi Frascati workshop, May 7, 2007 - Burigana, De Rosa, Valenziano, Morgante, Villa, Salvaterra, Procopio, Mandolesi

Cosmic Microwave Background Radiation Anisotropies Angular power spectrum Polarization P 2 = Q 2+ U 2 Example: Scattering Thomson of radiation with quadrupole anisotropy generates linear polarization Spectrum Photon distribution function Frascati workshop, May 7, 2007 - Burigana, De Rosa, Valenziano, Morgante, Villa, Salvaterra, Procopio, Mandolesi

CMBR SPECTRUM T 0 = 2. 725 ± 0. 002 °K (Mather et al. 1999) Redshift Dimensioneless frequency Has the CMBR a black body spectrum? Frascati workshop, May 7, 2007 - Burigana, De Rosa, Valenziano, Morgante, Villa, Salvaterra, Procopio, Mandolesi

CMB Spectrum measures WP 1430 – C. Burigana, N. Mandolesi, L. Valenziano Recent measures of CMB spectrum (collected by Burigana and Salvaterra, 1999) >1 cm: typical error > 0. 1 K FIRAS measures: typical error ± 0. 0001 K Frascati workshop, May 7, 2007 - Burigana, De Rosa, Valenziano, Morgante, Villa, Salvaterra, Procopio, Mandolesi

Impact of various sources of errors: note the atmosphere relevance Frascati workshop, May 7, 2007 - Burigana, De Rosa, Valenziano, Morgante, Villa, Salvaterra, Procopio, Mandolesi

Spectral distortions In the primordial universe some processes can lead the matter-radiation fluid out of thermal equilibrium (energy dissipation because of density fluctuations, Physical processes out of the equilibrium, radiative decay of particles, energy release related to the first stages of structures formation, free-free distortions) The photon distribution function isn’t a Planckian one The Kompaneets equation in cosmological contest provides the best tool to compute the evolution of the photon distribution function, but a numerical code is needed! KYPRIX An extremely precise fortran based code, able to simulate the effects of the primordial physical processes that can affect thermodynamic equilibrium of the CMBR Frascati workshop, May 7, 2007 - Burigana, De Rosa, Valenziano, Morgante, Villa, Salvaterra, Procopio, Mandolesi

Cosmological applications Primordial distortions today BIG BANG zterm z. BE Bose-Einstein like spectrum with µ function of X z zric z Superposition of black bodies where Free-free distortions Late distortions Related (mainly) to the reionization history of the universe Cosmological application of a numerical code for the solution of the Kompaneets equation, P. Procopio and C. Burigana, INAF-IASF Bologna, Internal Report, 421 Frascati workshop, May 7, 2007 - Burigana, De Rosa, Valenziano, Morgante, Villa, Salvaterra, Procopio, Mandolesi

Theoretical CMB Spectral Distortions Free-free Late Comptonization like Middle age Early Bose-Einstein like Distorted spectra in the presence of a late energy injection with Δ / i = 5 x 10 -6 plus an early/intermediate energy injection with Δ / i = 5 x 10 -6 occurring at yh=5, 1, 0. 01 (from the bottom to the top; in the figure the cases at yh=5 and 1 are indistiguishable at short wavelengths; solid lines) and plus a free-free distortion with y. B=10 -6 (dashes). Frascati workshop, May 7, 2007 - Burigana, De Rosa, Valenziano, Morgante, Villa, Salvaterra, Procopio, Mandolesi

Te/TR = 104 z. R = 20 d / = 10 -5 Cosmological application One of the representative cases Distortions due to reionization of the universe at low redshifts m= 1 = 0 m = 0. 29 Frascati workshop, May 7, 2007 - Burigana, De Rosa, Valenziano, Morgante, Villa, Salvaterra, Procopio, Mandolesi = 0. 73

In the Planckian Hypothesis: limits achievable with a new low frequency experiment – DIMES Example: 6 freq. channels between 2 & 90 GHz Limits achievable with a low frequency experiment with the same FIRAS sensitivity Current limits Hypothesis to be checked Burigana and Salvaterra, 2003 Cosmic time Frascati workshop, May 7, 2007 - Burigana, De Rosa, Valenziano, Morgante, Villa, Salvaterra, Procopio, Mandolesi

CMB spectrum: Key parameters Configuration A and B • Frequency operating range: 0. 4 – 50 GHz (75 - 0. 6 cm) • Spectral resolution: 10% • Angular resolution: 7°/8° • Sensitivity: < 1 m. K sec-1/2 • Field of View: > 104 deg 2 • Final sensitivity (E. O. L) better than 0. 1 m. K per resolution element • Low sidelobes optics • Ground shield –avoid ground signal pickup –thermal stability Channel Frequency (GHz) Wavelength (cm) 1 100 0. 300000 2 63. 0957 0. 475468 3 39. 8107 0. 753566 4 25. 1189 1. 19432 5 15. 8489 1. 89287 6 10. 0000 3. 00000 7 6. 30957 4. 75468 8 3. 98107 7. 53566 9 2. 51189 11. 9432 10 1. 58489 18. 9287 11 1. 00000 30. 0000 12 0. 630957 47. 5468 13 0. 398107 75. 3566 Frascati workshop, May 7, 2007 - Burigana, De Rosa, Valenziano, Morgante, Villa, Salvaterra, Procopio, Mandolesi

Calibrator requirements • Return Loss < -60 d. B in the whole frequency range • Intercalibration between frequency bands better than 30 K • Thermal stability better than 1 m. K with well sampled temperature monitoring (temperature accuracy better than 10 K) The ARCADE calibrator Frascati workshop, May 7, 2007 - Burigana, De Rosa, Valenziano, Morgante, Villa, Salvaterra, Procopio, Mandolesi

Radiometers • Differential radiometers (using low noise amplifiers) • Absolute calibration One of the ARCADE radiometers (Kogut, 2002) Frascati workshop, May 7, 2007 - Burigana, De Rosa, Valenziano, Morgante, Villa, Salvaterra, Procopio, Mandolesi

Sketch of the large payload Mass: ~1000 Kg, height ~ 6 m, deployed in a shaded crater Frascati workshop, May 7, 2007 - Burigana, De Rosa, Valenziano, Morgante, Villa, Salvaterra, Procopio, Mandolesi

Scientific performance as function of (low) frequency coverage C = 2, 5, 8 freq. channels, 0. 48, 1. 9, 7. 54 cm D = 3, 6, 9 freq. channels, 0. 75, 3. 0, 11. 9 cm E = 3, 5, 7 freq. Channels, 0. 75, 1. 9, 4. 75 cm R = recent data @ l ≥ 1 cm F = COBE/FIRAS Note that even with observations @ l ≤ 5 cm the improvement is very good! Frascati workshop, May 7, 2007 - Burigana, De Rosa, Valenziano, Morgante, Villa, Salvaterra, Procopio, Mandolesi

New Concept Design Requirements • • Mass < 300 Kg Simplify cooling system Location at the pole Continuous operation (day and night) Simplify pointing system Autonomous, unmanned operation Simplify deployment Frascati workshop, May 7, 2007 - Burigana, De Rosa, Valenziano, Morgante, Villa, Salvaterra, Procopio, Mandolesi

Reduce Dimension and Mass • Reduce the number of channels Ø Use a smaller payload Ø Use a smaller cooler • Select highest frequency bands Ø Reduce horn and calibrator dimension • Enlarge FOV (14° FWHM) Ø Reduce horn dimensions • Passive cooling for the optics Ø Use a smaller cooler • Introduce steerable optical system Ø Reduce horn dimension Ø Avoid an alt-az mounting Frascati workshop, May 7, 2007 - Burigana, De Rosa, Valenziano, Morgante, Villa, Salvaterra, Procopio, Mandolesi

New Location • Select a location at the Pole Ø Reduce the size of passive cooling radiators Ø Reduce the observed portion of the sky (acceptable from the scientific point of view) Ø Avoid rover and deployment system (reduce mass) • Shaded crated location not strictly required Ø Simplified deployment on the final site Ø Operation on the landing module possible Ø Power generation from solar panels on the payload • Operation from the near side of the Moon Ø Higher frequency less affected by man-made interference Frascati workshop, May 7, 2007 - Burigana, De Rosa, Valenziano, Morgante, Villa, Salvaterra, Procopio, Mandolesi

New Payload Concept (conf. E) • 3 channels – 6 GHz – 15 GHz – 63 GHz • FOV: 14 deg • Passive cooling for the optics • Steerable optical element at horn aperture 6 GHz Channel 15 GHz Channel Steerable Mirror Feed Horn 63 GHz Channel Absolute Reference@4 K Internal Reference @4 K Thermal Link @4 K Radiometer @4 K Frascati workshop, May 7, 2007 - Burigana, De Rosa, Valenziano, Morgante, Villa, Salvaterra, Procopio, Mandolesi Cold Head

New Payload Concept 15 GHz Channel 63 GHz Channel Cold Head Electonics box Compressor Frascati workshop, May 7, 2007 - Burigana, De Rosa, Valenziano, Morgante, Villa, Salvaterra, Procopio, Mandolesi • Pointing system obtained using steerable mirrors and Moon rotation

Location External passive cooling Shield • Location at the Pole Instrument – Passive cooling possible. Smaller radiators • Easy deployment, unmanned operation Internal passive cooling shield Solar panel Middle Shield Cooler’s Radiators – Shields deployed in-situ – Operation from the lander possible – Solar panels on the payload Frascati workshop, May 7, 2007 - Burigana, De Rosa, Valenziano, Morgante, Villa, Salvaterra, Procopio, Mandolesi

• • Estimated mass: < 200 Kg In situ overall dimension: diameter: 8 m, height: 3 m • Passive shield deployed Estimated power requirements: 3 k. W Continuous operation possible Frascati workshop, May 7, 2007 - Burigana, De Rosa, Valenziano, Morgante, Villa, Salvaterra, Procopio, Mandolesi

CONCLUSIONS • The Moon is a unique opportunity for accurate cm & dm CMB spectrum measures free from atmosphere contamination • dm observations requires ≈ 103 Kg experiments • cm observations need ≈ 102 Kg experiments and represents, @ 0. 1 m. K sensivity, a great improvement with respect to the current observation status in particular for free-free distortions & BE-like (early) distortions • A compact design for early cm experiments has been proposed • Definitive cm & dm missions will map the cosmic thermal history with high precision up redshifts of ~ 107 Frascati workshop, May 7, 2007 - Burigana, De Rosa, Valenziano, Morgante, Villa, Salvaterra, Procopio, Mandolesi

Thanks for the attention! Frascati workshop, May 7, 2007 - Burigana, De Rosa, Valenziano, Morgante, Villa, Salvaterra, Procopio, Mandolesi

Frascati workshop, May 7, 2007 - Burigana, De Rosa, Valenziano, Morgante, Villa, Salvaterra, Procopio, Mandolesi

KYPRIX How does it work? Input parameters a)cosmological par. b)integration par. MAIN PROGRAM Initialization of the solution vector U D 03 PCF Discretization of the Kompaneets FUNCTION Subroutine for boundary cond. in point A Increasing time y Subroutine for boundary cond. in point B Subroutine PDEDEF Discretization in the x axis Computation of the rates of the physical processes Frascati workshop, May 7, 2007 - Burigana, De Rosa, Valenziano, Morgante, Villa, Salvaterra, Procopio, Mandolesi For specific phys. quant. Cosmic exp Output files ( , t) Integral quan.

KYPRIX’ update(s) ‘ 90 2004 -2005 2006 -2007 activity first KYPRIX release by Carlo Burigana update related to the NAG libraries* sensitivity e efficiency increased** introduction of the cosmological constant** CPU platform transfer (still in progress) update related to the relative abundances of H and He introduction of the ionization fraction of e- * Updating a numerical code for the solution of the Kompaneets equation in cosmological context, P. Procopio and C. Burigana, INAF-IASF Bologna, Internal Report, 419; **Accuracy and performance of a numerical code for the solution of hte Kompaneets equation in cosmological context, P. Procopio and C. Burigana, INAF-IASF Bologna, Internal Report, 420; Frascati workshop, May 7, 2007 - Burigana, De Rosa, Valenziano, Morgante, Villa, Salvaterra, Procopio, Mandolesi

Reionization Nowday, the most precise measurements related to the parameters of the standard model (of the universe) are those realized by the NASA satellite WMAP • optical depth of the universe =0. 09 +- 0. 03 (3 -years WMAP data) Effects of a reionization are visible in all the properties of the CMBR: --- Temperature anisotropies suppression at high multipoles* --- gain of power in T-E cross-correlation PS and in the E and B modes mainly at low and middle multipoles --- raising of free-free and compotonization like distortions in the spectrum Given that, we need a performing tool able to simulate the stages of evolution of the reionization as better as possible not only for effects related to the anisotropies, but also for what concern the CMBR spectrum *Planck-LFI scientific goals: implications for the reionization history L. Popa, C. Burigana, N. Mandolesi, …, P. Procopio, et. al. , Publ. By New Astronomy Frascati workshop, May 7, 2007 - Burigana, De Rosa, Valenziano, Morgante, Villa, Salvaterra, Procopio, Mandolesi