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BOOMERanG Launch (Dec. 28, 1998)

BOOMERanG Launch (Dec. 28, 1998). EPS HEPP Prizes – Grenoble July 25, 2011 P. de Bernardis – Sapienza – Roma. QMAP/TOCO. DASI/CBI. MAXIMA. ARCHEOPS. WMAP. first peak. 2000. BOOMERanG-98 & MAXIMA : The first views of causal horizons at recombination. 2001. 3 peaks.

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BOOMERanG Launch (Dec. 28, 1998)

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  1. BOOMERanG Launch (Dec. 28, 1998) EPS HEPP Prizes – Grenoble July 25, 2011 P. de Bernardis – Sapienza – Roma

  2. QMAP/TOCO DASI/CBI MAXIMA ARCHEOPS WMAP

  3. first peak 2000 BOOMERanG-98 & MAXIMA : The first views of causal horizons at recombination 2001 3 peaks

  4. Evidence from these experiments : • “Acoustic”, adiabatic oscillations in the primeval photons-baryons plasma • Geometry of the universe and its mass-energy density • its composition in terms of baryons, dark matter and dark energy • An early inflation process is neededAll these have a huge impact on our understanding of fundamental physics.

  5. 2006 2011 9 peaks (!) There is, however, much more. A lot is still to be gained from precision measurements of the CMB .

  6. Planck carries a complex CMB experiment all the way to L2 improving the sensitivity wrt WMAP by at least a factor 10, the angular resolution by a factor 2-3 and extending the frequency coverage towards high frequencies by a factor about 10

  7. LFI HFI 857 143 217 353 545 70 100 30 44 P P P P P P P These characteristics boost the reliability of the cosmological fluctuations detected.

  8. Thermal performance : Planck collaboration: astro-ph/1101:2023

  9. Mission : Planck collaboration: astro-ph/1101:2022

  10. ESA-SCI(2005)1

  11. EE TE ESA-SCI(2005)1

  12. ERCSC : Planck collaboration: astro-ph/1101:2041 Faintest source vs. frequency band # sources

  13. ERCSC (>15000) …… Early Cold Cores Sample (915) All sky Early Sunyaev-Zeldovich cluster sample (189) Galaxies ……

  14. All-sky Sunyaev-Zeldovich clusters • Thanks to its all-sky coverage, Planck has a unique capability to detect the rarest and most massive clusters in the exponential tail of the mass function. • As a matter of fact, two of the newly-discovered clusters in the ESZ and confirmed by XMM-Newton have estimated total masses larger than 1015Msol.

  15. Forthcoming :(with Planck and after Planck)

  16. B-modes & non-gaussianity • High precision polarization measurements might detect the rotational component of the polarization pattern of the CMB, which is related to the tensor fluctuations generated during the inflation process. • This is a generic prediction of all inflation scenarios. • At the moment the upper limit on the ratio of tensor to scalar fluctuations is of the order of r = 0.3. • Planck can well reach r = 0.01, but future, optimized measurements can reach r = 0.001. • If these measurements will be successful we will be able to constrain the energy scale of the inflation process down to 6.5x1015 GeV, probing physics at energies so high that are not testable in current and future accelerators. • Similar constraints are expected from detections of non-gaussianity of the CMB. astro-ph / 11022181 http://www.core-mission.org

  17. Neutrino masses • Massive neutrinos (a fraction of eV) are relativistic during the early matter domination era, and not relativistic today. • They escape from overdensities and suppress structure growth. Also, the lensing from modified matter fluctuations is modified. • For both reasons, the anisotropy and polarization power spectra of the CMB are sensitive to neutrino mass. • Planck: detection if > 0.2 eV • Future optimized instruments: 50 meV , sufficient to distinguish normal and inverted mass hierarchies. • CMB measurements probe an early linear pase, and complement very well optical measurements in the non-linear phase (BAO & lensing) Blue: no mass Red:Nn=3, Smn=0.65 eV

  18. From Fogli et al. 2008, Astro-ph/0805.2517 With Planck : < 0.2 eV

  19. Constraints on Neutrino Masses from CMB +Priors Limits at 95% c.l.: Red: 1000 riv+ Prior 1% H0+ Priori 2% Wm Blue: 5000 riv+ Prior 1% H0+ Priori 2% Wm Red Dashed: 1000 riv+ Prior 0.5% H0+ Priori 1% Wm Blue Dashed: 5000 riv+ Prior 0.5% H0+ Priori 1% Wm With external priors on the Hubble parameter And the matter density also the Normal Hierarchy can be probed: safe detection of a neutrino mass. • constraints on neutrino masses (from Pagano & Melchiorri)

  20. 1ES0657-556 7.5 ’

  21. OLIMPO balloon payload (Masi et al. 2008), with solar panels, ground shield and sun shield removed. Note the tiltable 2.6m primary mirror and the lightweigth secondary. Pointing is obtained rotating the payload around an azimuth pivot and changing the elevation of the inner frame, including the telescope, the FTS and the detector’s cryostat The total mass of the payload is 1.5 tons.

  22. Azimuth pivot The Payload Cryostat with cold optics and detector arrays FTS Readout electronics LN 60L Elevation motor LHe 60 L arrays window Reimaging optics dichroics

  23. Simulated OLIMPO measurement of a cluster l.o.s. with tth=0.005, Te=10 keV, tnonth=0.0001, vpec=500 km/s, Idust=6kJy/sr@150GHz The data with the error bars are simulated observations from a single pixel of the OLIMPO-FTS, for an integration time of 3 hours. The two lines through the data points represent the input theory (thin) and the best fit for the plotted data realization (thick). The other thin lines represent thermal plus non-thermal SZE, and dust emission. The high-frequency excess is due to a modest amount of dust thermal + non-thermal SZ dust this shift is due to the peculiar velocity of the cluster

  24. Kinetic Inductance Detectors (KIDs) arrays Caltech, Grenoble, SRON, Cardiff … and also made in Italy, FBK + Sapienza + Perugia, M. Calvo et al. Experimental Astronomy (2010) 28: 185–194

  25. Applications of mm-wave imagers and polarimeters • Vision through fog • Non-invasive mm-wave scanners • In-vivo detection of breast / skin cancer • Quality control – internal structure of wood, plastics etc. • …

  26. CMB research is not over…. Stay tuned !

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