Cosmologia con la radiazione cosmica di fondo - INFN · PDF fileNazzareno Mandolesi –...

Nazzareno Mandolesi – Copenahgen 9th June 2011

Cosmologia con la radiazione cosmica di fondo

Paolo Natoli Dipartimento di Fisica e Scienze della Terra Università di Ferrara

Nazzareno Mandolesi – Copenahgen 9th June 2011

Nazzareno Mandolesi – Copenahgen 9th June 2011

Fluctuation and GW generator

Fluctuation amplifier But GW dissipator…

The main objective of CMB experiments is to measure the spatial temperature and polarization anisotropies of the cosmic microwave background (CMB) radiation The CMB is a blackbody radiation with T=2.7 K extremely uniform across the whole sky; it is the relic radiation emitted at the time the nuclei and electrons recombined to form neutral hydrogen, when the Universe was ~ 400,000 years old. Its tiny (~ 10-5) temperature and polarization anisotropies encode a wealth of cosmological information.

Full sky temperature map from Planck (2013)

Power spectrum of temperature fluctuations from Planck (2013)

The fluctuations are observed to be Gaussian distributed: all the statistical information in the map is encoded in the two point correlation function or in its harmonic transform, the angular power spectrum: �(n̂) =

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Full sky map of CMB anisotropy (Planck 2015)

Science with the Cosmic Microwave Background !"#"$%&'&'()*+,%+-+(&*.-)/.$.%"#"$,)#+)0&(0).**1$.*23)

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Cosmic Microwave Background Radiation Overview

The oldest light or the first light of the Universe

2009 Planck

Discovered the remnant afterglow from the Big Bang. !! 2.7 K

Blackbody radiation, Discovered the patterns (anisotropy) in the afterglow. !! angular scale ~ 7° at a level !T/T of 10-5

(Wilkinson Microwave Anisotropy Probe): ! angular scale ~ 15’

! angular scale ~ 5’, !T/T ~ 2x10-6, 30~867 Hz

Planck

Planck history in short-! 1993 – COBRAS & SAMBA proposals -! 1996 – Selection of COBRAS/SAMBA,

then named Planck -! 1999 – LFI and HFI consortia are

formed -! […] Lots of Instrument development &

tests -! 2009 – Planck is launched -! Jan. 2012 – HFI End of life -! Mar. 2013 – First cosmological data

release -! Oct. 2013 – LFI End of life -! Feb 2015 – Second cosmological data

release -! 2017 – Third cosmological data

release

What is yet to be done?

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500 1000 1500 2000 2500 3000 3500Multipole ` (linear scale)

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Planck (2015)ACTpol (2014)SPTpol (2013/2014)BICEP2/Keck/Planck (2015)PolarBear (2014)fsky = 73%

Plot by D. Molinari et al.

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Galaxy (100 GHz)

500 1000 1500 2000 2500 3000 3500Multipole ` (linear scale)

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Galaxy (70 GHz)

Galaxy 10% (70 GHz)

Galaxy 5% (70 GHz)Galaxy 1% (70 GHz)

Galaxy (353 GHz)

Galaxy (150 GHz)

Galaxy (44 GHz)

Planck (2015)ACTpol (2014)SPTpol (2013/2014)BICEP2/Keck/Planck (2015)PolarBear (2014)fsky = 73%

Plot by D. Molinari et al.

SWIPE STRIP

STAR SENSORS

PIVOT

RACK

BATTERIES

BALLAST FRAME

LSPE gondola : frame + pivot + STRIP + SWIPE to balloon

Actuators: Azimuth pivot with torque motors

Linear elevation actuators

Processor: PC104 with ADC in / PWM out

H-bridges for motors

Attitude sensors: Star sensors (Nati et al. RSI 2003)

Laser Gyroscopes Elevation Encoders

TM TC

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5

17

Launched - June 14th, 2006

Svalbard

Impact – July 1st, 2006

17 DAY FLIGHT

Contatti (@ unife.it)

francesco.forastieri PhD massimiliano.lattanzi PostDoc nazzareno.mandolesi Prof paolo.natoli Prof linda.polastri PhD diego.molinari PostDoc

Principali collaborazioni INAF/IASF (Bologna) ASI (Roma) SNS (Pisa), UniPisa, UniSapienza, SISSA (Trieste) Caltech/JPL, IAP/CNRS (Paris), Cambridge (UK), Univ. Valencia, OKC (Stoccolma), Vancouver (CA),…