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2008/3/13 1 Application of Michelson type bolometric interferometer to CMB B mode polarization observations Makoto Hattori Astronomical Institute Tohoku University KEK

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2 ContentsContents Merit of interferometer for E B mode separation and for minimizing contamination of instrumental polarization Demerit of interferometer with heterodyne receiver for CMB B mode experiments. Bolometric interferometer as ideal instrument for B mode experiments. Propose an B mode experiment with Michelson type bolometric interferometer. Summary & bit about Akari/FIS all sky survey 2008/3/13 KEK

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3 Single dish imaging obs. VS interferometer: EB separation 2008/3/13 KEK Single dish:ex. PLANCK Interferometer: ex. DASI Fourier Spectrum of I, Q,U, V are observed variables

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4 E B separation by interferometer 2008/3/13 KEK Stokes parameters In Fourier space:locally separable y

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: prove inflational universe and nature of DE by B mode obs..

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6 Instrumental Polarization in Single dish (Hu etal. (2003)) Pauli matrix expansion of P matrix Instrumental Jones matrix 2008/3/13 KEK Monopole leakage due to cross polar mixing is significant

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Dont do Try to measure directly by Prof.A.Suzuki 7 Do not have to worry about Monopole leakage in interferometer 2008/3/13 KEK

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8 CMB vs foreground 2008/3/13 KEK Thermal emission from dust Atmospheric emission Quantum limit of heterodyne receiver Synchrotron Free-free T mode frequency intensity Cosmic window @70GHz Atmospheric window @90GHz

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9 Interferometer with heterodyne receivers is not suitable to B mode observations 2008/3/13 KEK Quantum limit of heterodyne receiver since it performs coherent detection realistically Nosie level is Quantum limit limited around cosmic window Construction of large element interferometer is practically hard. One receiver is mounted on focal plane of one telescope. DASI

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10 CMB power spectrum 2008/3/13 KEK

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11 Explosive improvement of sensitivity of single dish obs. due to emergence of large format TES bolometer array 2008/3/13 SPT 330 elements Not quantum limit limited since incoherent detection

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12 Interferometer with bolometer is the ideal coupling: bolometric interferometer 2008/3/13 It shares the both merit of interferometer and bolometer Fiseau type Michelson type

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13 Application of Fiseau typeEPIC 2008/3/13 KEK Timbie et al (2006) - = Adding type interferometer Fringe Baseline fluctuation Data

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14 Merit of Michelson type VS Fiseau type Multiplying type bolometric interferometer is able to realize. Broad band spectroscopy is possible: advantagious component separation of foreground and CMB is possible. Mathematical basis of the instruments are fully explored. 2008/3/13 KEK Path finder@NAOJ The moon interferogram Intrenal light path difference Luo, Ohta, Hattori, Chinone, et al. (2008in preparation) 70GHz 170GHz

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15 Problem in application of Michelson type to CMB B mode experiment D b D

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16 New Michelson type bolometric interferometer satisfies D>b: MuFTPol 2008/3/13 KEK Ex Ey D b Telescope DET1,2,3,4=Ex Ey =UV DET5,6,7,8 =(Ex+Ey)(Ex-Ey) =QV Ohta, Hattori, Matsuo (2006,2007), Ohta et al. (2008 in prep.) Hattori, Ohta, Koga (2008 in preparation) HarryBotte x y

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17 Observed variables of MuFTPol 2008/3/13 KEK

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18 EB mode separation by MuFTPol n m 2008/3/13 KEK NM pixel detector array

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19 EB mode separation by MuFTPol Base line vector // direction Sum up 1010 pixels data 2008/3/13 KEK The B mode are measured by direct observed varibales of DET1,2,3,4.

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20 Detector:8 set of 10 10TES array 2008/3/13 KEK Operation temperature:300mK NEP a few Time constant msec Spider web and TES are going to be fabricated by MEMS at Esasi Labo. in Tohoku University SQUID time domain mutiplexing: cooperation of Prof.K.Irwin, NIST (USA) Any cooperations are very helpful and collaborations are very welcome.

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21 Observational site 1 st session: Summit of Mt.Fuji 2 nd session Balloon 60 300GH with =10GHz 2008/3/13 KEK Sekimoto et al. (1996) 80-100Gz with =10GHz 1.4m telescope 0