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Application of Michelson type bolometric interferometer to CMB B mode polarization observations

Application of Michelson type bolometric interferometer to CMB B mode polarization observations. Makoto Hattori Astronomical Institute Tohoku University. Contents. Merit of interferometer for E ・ B mode separation and for minimizing contamination of instrumental polarization

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Application of Michelson type bolometric interferometer to CMB B mode polarization observations

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

  2. Contents • 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 KEK

  3. Single dish imaging obs. VS interferometer:E・B separation Single dish:ex. PLANCK Fourier Spectrum of I, Q,U, V are observed variables Interferometer: ex. DASI KEK

  4. E・B separation by interferometer Stokes parameters In Fourier space:locally separable y Ｘ KEK

  5. 宇宙創世記: prove inflational universe and nature of DE by B mode obs..

  6. Instrumental Polarization in Single dish (Huetal. (2003)) Pauli matrix expansion of P matrix Instrumental Jones matrix Monopole leakage due to cross polar mixing is significant KEK

  7. Do not have to worry about Monopole leakage in interferometer Don’t do Try to measure directly by Prof.A.Suzuki KEK

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

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

  10. CMBpower spectrum KEK

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

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

  13. Application of Fiseau type：EPIC Timbie et al (2006) Adding type interferometer Data - Baseline fluctuation = Fringe KEK

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

  15. Problem inapplication of Michelson type to CMB B mode experiment D b D<b Required baseline length b=10cm@90GHz for l=100 • Low power of light collection • Hard to mount massive detector array • Lowest observable l is limited by D. KEK

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

  17. Observed variables of MuFTPol KEK

  18. E・B mode separation by MuFTPol m 以下 N×Mpixel detector array n KEK

  19. E・B mode separation by MuFTPol Base line vector // ｘdirection Sum up 10×10 pixels data The B mode are measured by direct observed varibales of DET1,2,3,4. KEK

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

  21. Observational site 1st session: Summit of Mt.Fuji Sekimoto et al. (1996) 80-100Gz with Δν=10GHz 1.4m telescope 0<b<40cm variable 2nd session Balloon 60－300GHｚwith Δν=10GHz KEK

  22. Sensitivity of 1st session MuFT KEK

  23. Summary • We propose Michelson type bolometric interferometer which is able relax D< b constraint • Application of this instrument to CMB B mode experiment is orthogonal to other projects, eg. B mode is the direct observable, minimizing instrumental polarization. • Summit of Mt.Fuji is atractive site for CMB experiment • By applying it to balloon born or space born mission, super broad band observation is possible which mazimize component separation of FG and CMB KEK

  24. To improve physical prior information of dust components All sky diffuse map making @60, 100, 160μ with Akari/FIS all sky survey data (Doi (Univ.Tokyo), EtxaluuzeAzkonaga, M., Figueredo, E., White, G. (Open University),Chinone, Hattori (Tohoku University)、Nakagawa (JAXA)Akari team) 0.75’@160μ IRAS:12,25,60, 100μm, 2’@100μm KEK

  25. CMB実験グループの立ち上げおめでとうございます。若い研究者にQUIET・Polarbearのデータにさわる機会を作って頂きありがとうございます。日本がCMB観測の歴史に一つでも足跡を残すことに、微力ながら手助けができれば幸いです。CMB実験グループの立ち上げおめでとうございます。若い研究者にQUIET・Polarbearのデータにさわる機会を作って頂きありがとうございます。日本がCMB観測の歴史に一つでも足跡を残すことに、微力ながら手助けができれば幸いです。 KEK

  26. Sensitivity of 1st session MuFT KEK

  27. mm-wave sky –Foreground=CMB 23GHz Synchrotron Dust emission 33GHz 60GHz - 93GHz 41GHz Free-free = Synchrotron and dust are significantly polarized KEK

  28. Cross Polarization mixing in MuFTPol Cross polarization transmitance of wire grid % 0.2%@100GHz KEK

  29. MuFT仕様 当面 • Ｇｒｏｕｎｄ　ｂａｓｅ observation • Φ1.4m ナスミス焦点望遠鏡 • ベースライン間隔:0<b<40cm可変 • 帯域80－100ＧＨｚ・周波数分解能１０ＧHz • 10×10 ＴＥＳボロメータアレイ×8セット • （NEP～数×E-17 W/√Hz,τ～1msec) • 機械式冷却 • 目的：ｌ～200-400の重力レンズ起源Bモード • パワースペクトル測定 将来 大気球帯域40－300GHｚ 理研仙台

  30. Option U+Vのみ測定 デメリット：Δδの補正時の情報が減る メリット：cross polarization mixing が防げる。 光学系が簡略化 理研仙台

  31. MuFTpathfinder@NROJ 月の観測データ （ルオ 2007) 世界で初めて積算型 ボロメトリック天体干渉計 の実現に成功 理研仙台

  32. Nasmis focus at Az-El telescope 理研仙台

  33. E and B mode polarization Stokes parameters Polarization vector Bmap must satisfy Emap must satisfy KEK

  34. E・B mode separation In Real space:whole sky P map is neccessary B mode y In Fourier space:locally separable E mode Ｘ KEK

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