Transcript センチ波電波天文学の将来計画

センチ波電波天文学の将来計画
〜Square Kilometer Array を中心として〜
Hiroyuki Nakanishi (Kagoshima university)
2010/11/17
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Brief history of SKA
1991 First concept appeared (Hydrogen Array)
1993 URSI established the Large Telescope Working Group
1997 six countries signed MoU. “SKA” appeared in 1996.
2000 ISSC was established
2007 SPDO, SSEC were est
CO vs. optical
CO vs Hα
CO vs HI
Nakanishi et al.
(2005)
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HI resolution>10”
others 〜1”
SKA (Square Kilometer Array)
• Freq. range：0.1－10GHz(25GHz)
Low-band: 100-500MHz
Mid-band:500MHz-10GHz
High-band: 10GHz-25GHz
• Antenna：
– Aperture Array
Dense AA, Sparse AA
– Dishes (2000-3000 )
Wideband Single Pixel Feed
Phased Array Feed
• Site
– Australia or South Africa
• Characteristics
–
–
–
–
High sensitivity
Wide-band
Wide field
High resolution
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Sparse Aperture Arrays
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21st Century Astrophysics
20th Century: We discovered our place in the Universe
21st Century: We understand the Universe we inhabit
(J. Lazio SKA-JP WS2010, 4-5 Nov 2010)
Cosmology & Fundamental
Physics
• Gravity
– Can we observe strong gravity
in action?
– What is dark matter and dark
energy? (dark energy and
BAOs with H I galaxies)
• Magnetism
• Strong force
Nuclear equation of state
Galaxies Across Cosmic Time, The
Galactic Neighborhood, Stellar and
Planetary Formation
•Galaxies and the Universe
– How did the Universe emerge from its Dark
Ages?
– How did the structure of the cosmic web
evolve?
– Where are most of the metals throughout
cosmic time?
– How were galaxies assembled?
•Stars, Planets, and Life
– How do planetary systems form and evolve?
– What is the life-cycle of the interstellar
medium and stars? (biomolecules)
– Is there evidence for life on exoplanets?
(SETI)
Key Science
• Cradle of Life
• Probing the Dark
Ages
• Strong-field tests of
General Relativity
• Origin & Evolution
of Cosmic
Magnetism
• Cosmology and
Galaxy Evolution
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1. Cradle of Life
1. Protoplanetary Disks
– protoplanetary disk can be
observed even at cmwavelength
2. Complex molecule
– Large molecules related to
the life radiate longer
emission
3. SETI
– Airport radar and TV radio
etc. can be targets
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Chandler et al. 2005
2. Probing the Dark Ages
I.
Epoch of Reionization
H I brightness temperature
(w.r.t. CMB)
– HI brightness temperature
versus redshift constrain
model
II. First Molecule
– At higher redshifts, CO
transitions shift out of ALMA
frequency coverage, into SKA
frequency coverage.
Pritchard & Loeb 2008
1”
5.5 kpc
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J114816.64+525150.2
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z = 6.42
VLA
P
d
B
I
PdBI
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3. Cosmic Magnetic Field
All Sky RM Survey
– Rotation Measure (RM) can be measured
towards million QSOs
– Probing evolution of cosmic magnetic field from
z=o to 5
– Role of magnetic force in the universe
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4. Test of General Relativity
I.
Test of GR under
strong gravity
– measurement of pulses from
binary pulsar or pulsar-BH
I.
Detection of
Gravitaional wave
– Pulsar as a precise
clock
– Pulsar timing can
detect GW
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5. Cosmology and Galaxy Evolution
Meyer et al. 2004
• Baryon Acoustic
Oscillations
WMAP
(z ~ 1100)
–DA(z) = angular size distance
as a function of redshift
–standard ruler
–Measures expansion rate of
Universe
Next-generation goal:
Survey large
volume
Slice into redshift
bins
Detect BAOs in
each z bin
• Galaxy evolution
star
Hopkins & Beacom
gas
SDSS (z ~ 0.35)
SDSS surveyed ~ 1 Gpc3
SKA goal ~ 100 Gpc3
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Johnston et al. 2008
International Structure
•SSEC member
Australia・Canada・China・ Europe・
India・South Africa・USA
•Observer:
Russia, Japan, Korea, New Zealand
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電波専門委員会(2010/9/13)
NAOJ NRO川辺所長
が天文台側の代表に
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Timeline
2010-11: PrepSKA
2012-15: Pre-construction phase
2016-18:SKA phase 1 (SKA1) construction
2016: Advanced Instrumentation Programme
(AIP) decision
2019: Full SKA1 science operations begin
2019-2022: SKA phase 2 (SKA2) construction
2023: Full SKA science operations begin
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Reference Design for SKA1
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Overview of the System/Engineering
Dense Aperture Arrays
Dishes
3-Core
Central
Region
Sparse Aperture
Arrays
Peter Dewdney @SKA2010
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Pathfinders/Precursors
Pathfinder
Precursor
LOFAR (NL)
ATA(USA)
e-MERLIN(UK)
e-EVN(EU)
EVLA(USA)
LWA(USA)
SKAMP(Aus)
Arecibo(USA)
ASKAP(Aus)
MeerKAT(ZA)
MWA(Aus, USA)
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Design Studies
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Canadian SKA
program
TDP(USA)
SKADS(EU)
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Eng. Development/low-SKA Sparse AA
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Eng. Development/low-SKA DenseAA
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Eng. Development/mid-SKA Dishes
KAT-7
ATA
7 x12m
composite
dishes
Prototype 15
m
42x6m
hydroform
ed dishes
composite dish
ASKAP
CART
36x12m
panel
dishes
2010/11/17
10 m composite prototype
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Eng. Development/mid-SKA PAF
ASKAP
chequer
board
array
Chequer-board phased
Chequer-board
phased
array (ASKAP,
Australia)
array (ASKAP, Australia)
ASKAP, Australia
APERTIF
(Astron, NL)
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DRAO
Canada
Vivaldi arrays
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Eng. Development/mid-SKA WBSPF
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Japan SKA consortium
• Establishment：May 2008
ＳＷＧ
• Member：86 individuals from 26inst.
• Organizers：
H. Nakanishi（Kagoshima uni. ; chair)
Y. Hagiwara (NAOJ)
O. Kameya (NAOJ)
• Aim：






10xBandwidth
Magnetic field
＋spectral fitting
⇒3x Increase in
AGN
Dyncamic range
⇒ Higher sensitivity
High-z galaxy
・Distant faint object can be detected
・Increase of reference source for
Pulsar
astrometry
Astrometry
Astro-chemistry
8-50GHz linesurvey
towards TMC-1
(Kaifu et al. 2004)
To promote Japanese researchers to be
involved into the international SKA project
• Activities：
EWG
AGN CTD93 SED (Nagai
et al. 2006)
Cotton (SKA2009＠
Capetown)
3C287
Polarization angle
over
wideband → More
accurate rotation
Key Word
UltraWideband
Sharing informations via ML
 Wideband feed
Monthly telecon
 Wideband receiver
Science Working group(SWG),
 Wideband backend
Handmade tapered slot antenna
Engineering Working Group(EWG)
InP HBT fast 3bit A/D sampler
（upper） mesurement in the rqdio
quiet room（lower）(Kozuma 2010)
Discussion on collaboration with
↑spectra obtained
Industry Forum
with fast A/D
converter
Hosting Workshop
NTT Photonics Laboratory
Applying for research budget
← Spectra obtained with
Industry forum
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 ガンマ線研究会
Collaboration
heterodyne receiver（Kawaguchi
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NAOJ, 2008)
Benefits of Wideband Receiver
•Wideband spectrum
Polarization observation
Cont. observation
3C287
Polarization angle [°]
Line observation
Ultra wideband Line survey for
TMC-1 in 8-50GHz(Kaifu et al. 2004)
λ2[cm2]
Wideband SED (2.2-15.3GHz)
of AGN CTD93 (Nagai et al.
2006)
Polarization
angle
over
wideband → More accurate
rotation measure (slope)
•Higher sensitivity： ΔT∝B-1/2
・Distant faint object can be detected
・Increase of reference source for astrometry
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Taylor et al. 2009
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Astronomy Achieved by Wideband
1. Astro-chemistry (wideband line survey)
–
S. Yamamoto (U. Tokyo)
2. Active Galactic Nuclei (wideband SED)
–
N. Kawakatsu (U. Tsukuba)
3. Magnetic field of the universe (wideband polarization angle)
–
K. Takahashi (U. Nagoya)
4. High-z galaxies (high sensitivity)
–
H. Hirashita (ASIAA)
5. Astrometry (high sensitivity obs. of phase-reference sources)
–
H. Imai (Kagoshima U.)
6. Pulsars (high sensitivity and wideband pulsar timing)
–
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O. Kameya (NAOJ)
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Homodyne receiver with Fast A/D converter
Fast InP HBC 3bit sampler （Kawaguchi@SKA-JP WS 2008)
Heterodyne
Homodyne
Amplifier
Amplifier
Rec
Rec
Mixer, LO
Experiment
(3 mm × 3mm）
Spectra obtained with heterodyne
receiver (fLO=(16.85+3)GHｚ、fIF=2.22.6GHz, fsample=8.192GHz)
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NTT Photonics Laboratory
Spectrum obtained with homodyne
reciver (fRF=20.480-24.576GHz, fsample
=8.192GHz, BW=4.096GHz)
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Other possible contributions
Elementary study for Wideband Tapered Slot
Antenna（Kozuma@EAVNWS2010)
Return Loss [dB]
• Development of
wideband feed
• Low Noise Amplifier
• A/D converter
• Correlator
• Software
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SKA-Japan Workshop 2010
• Date: 4-5 Nov, 2010
• Place: NAOJ, Mitaka Tokyo, Japan
• Topics: Revealing the Universe with Wide-band
cm-Wavelength Observation
• Aim:
 To understand the status of international SKA project
 To form more international networks
 Key science and engineering for Japanese community
• Invited speakers：
John Bunton (CSIRO)：ASKAP
Minho Choi (KASI)：status SKA-Korea
Jasper Horrell(South African SKA Project Office)：MeerKAT
Joseph Lazio (JPL-SPDO)：Science with the SKA
Steve Rawlings (Oxford U) Overview of SKA
Peter Dewdney (SPDO) Engineering
Phil Diamond )CSIRO)
H. Imai (Kagoshima U.): Astrometry
K. Omukai (U. Kyoto): Star-formation
O. Kameya (NAOJ): Pulsar
N. Kawakatsu (U. Tsukuba): Active Galactic Nuclei
N. Kawaguchi (NAOJ)：Japanese Engineering
R. Kawabe (NAOJ)：Synergy with the ALMA
T. Kumazawa (Toyo Technica): from Industry forum
K. Takahashi (U. Nagoya): Cosmic Magnetic field
T. Takeuchi (U. Nagoya): Galaxy evolution and distant universe
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S. Yamamoto (U. Tokyo)：Interstellar chemistry
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A part of outcomes from SKA-JP WS2010
• “Wideband” must be a good keyword to encourage
people in both science and engineering sides
• Precursor project welcome new collaborators from
international community including Japan.
• There are interests from international community,
Japanese industries, as well as domestic science
community
• Though science is discussed intensively, detailed
requirement is not obvious yet
• 98 participants ; 12 from abroad, 12 from industry
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For further information
Please visit the webpage
http://skajp.org/ws2010
A part of this presentation is from
SKA-JP WS2010.
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