2008/3/13 1 Application of Michelson type bolometric interferometer to CMB B mode polarization...
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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
2008/3/13 1 Application of Michelson type bolometric
interferometer to CMB B mode polarization observations Makoto
Hattori Astronomical Institute Tohoku University KEK
Slide 2
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
Slide 3
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
Slide 4
4 E B separation by interferometer 2008/3/13 KEK Stokes
parameters In Fourier space:locally separable y
Slide 5
: prove inflational universe and nature of DE by B mode
obs..
Slide 6
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
Slide 7
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
Slide 8
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
Slide 9
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
Slide 10
10 CMB power spectrum 2008/3/13 KEK
Slide 11
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
Slide 12
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
Slide 13
13 Application of Fiseau typeEPIC 2008/3/13 KEK Timbie et al
(2006) - = Adding type interferometer Fringe Baseline fluctuation
Data
Slide 14
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
Slide 15
15 Problem in application of Michelson type to CMB B mode
experiment D b D
Slide 16
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
Slide 19
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.
Slide 20
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.
Slide 21
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