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Transcript of Space Infrared Astronomy in Japan 2009 UN BSS & IHY Workshop, September 22, 2009 MATSUMOTO, Toshio...
![Page 1: Space Infrared Astronomy in Japan 2009 UN BSS & IHY Workshop, September 22, 2009 MATSUMOTO, Toshio Seoul National University, ISAS/JAXA.](https://reader035.fdocuments.us/reader035/viewer/2022062516/56649e385503460f94b29166/html5/thumbnails/1.jpg)
Space Infrared Astronomy in Japan
2009 UN BSS & IHY Workshop, September 22, 2009
MATSUMOTO, Toshio
Seoul National University, ISAS/JAXA
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Infrared observation is inevitable to understand the evolution of the Universe
IRAS 12, 60, & 100 µm (NASA/IPAC)
Most of energy is emitted in infrared Wavelength (1mm – 1mm)
Far infrared view of ORIONThermal emission of interstellar dust is Indication of star forming activity
Optical image
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Why space infrared observation?
●Wide wavelength coverage
Atmosphere is opaque in infrared region
Some windows at near and mid IR
FIR observation can be done only from space
●Very low background
High sensitivity
Absolute observation of diffuse extended sources
But telescope must be cooled down!
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Thermal emission and transparency of the atmosphere
1.0
0.0
10-3
10-6
10-9
Surf
ace
brig
htne
ss (W
.m-2
.mm
-1.s
r-1)
T
rans
pare
ncy
1 10 100 1000
Wavelength (mm)
220k Blackbody
4 km
14 km
40 km
250 kmZodiacal light
IPD emission
ISD emission
CMB
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Cooled telescope is necessary to utilize low background condition
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Space infrared observation is difficult!
• How to keep liquid Helium at zero gravity?Separation of gas from liquid
Porous plug
• How can we realize long life of coolant?Cryostat must survive after the shock and vibration during launch
GFRP tension support
cf UFURU:1970IRAS:1983 COBE, ISO, Spitzer
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Many rocket and balloon flights(1970’ – 1980’)
● Short time scale and low cost, but limited capabilityshort observing time (rocket)narrow wavelength coverage, high background (Balloon)
● BenefitsDevelopment of key technology for futureGood training for students
Must be scientifically significant !
19 sounding rocket experiments, 13 balloon flights, 2 satellite launch
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Balloon born liquid Nitrogen cooled telescope
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Rocket experiment to measure infrared background with liq.He cooled telescope
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IRTS (Infrared Telescope in
Space)
One of mission instruments of small space platform, SFU
launched on March 15, 1995
15cm cold telescope Optimized for diffuse Extended sources Mission life ~ 1 month
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Focal Plane Instrument
NIRS (Near Infrared Spectrometer)wavelength coverage 1.4-4.0 mm spectral resolution 0.13 mmbeam size 8 arcmin. x 8arcmin.
MIRS (Mid infrared spectrometer)wavelength coverage 4.5-11.7mm spectral resolution ~0.3 mmbeam size 8 arcmin. x 8arcmin.
FILM (Far-Infrared Line mapper)wavelength coverage 158(CII) and 63 (OI) mm spectral resolution l/Dl~ 400beam size 8 arcmin. x 13 arcmin.
FIRP (Far-Infrared Photometer)wavelength coverage 150-700 mm spectral resolution l/Dl~ 3beam size 8 arcmin. x 13 arcmin.detector temperature 0.3K
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IRTS detected excess emission that could be pop.III origin
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Based on the success of IRTS, we proposed dedicated infrared astronomical satellite to ISAS, ASTRO-F (AKARI), on 1995
ASTRO-F●70 cm aperture, liq.He cooled telescope●Survey mission,
higher sensitivity and better spatial resolution longer wavelength band (200mm)
than IRAS
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Advanced space cryogenics
• Effective use of radiative cooling • 2-stage Stirling Cooler
Life time of liquid Helium 550 days with 170 liter Liq. He
cf . IRAS and COBE 10 months with 600 liter Liq. He
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Satellite system
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AKARI, Focal Plane Instrumnets
IRC(Infrared Camera) 512x412 InSb array camera, 1.5”/pixel imaging observation at 2.4, 3.2, and 4.1 mm low resolution spectroscopy256x256 SiAs array, 2.4”/pixel imaging observation at 7~24 mm low resolution spectroscopy
FIS(Far Infrared Surveyor) all sky survey with 4 bands
from 50 – 200 mm Fourier spectroscopy
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• ASTRO-F was launched on February 22, 2006, and named as “AKARI”
• Orbit : sun synchronous orbit, 705 km altitude
• Liq. He ran out on August 2007
• Near infrared observation is still being continued (phase 3) owing to cooler
http://www.ir.isas.jaxa.jp/ASTRO-F/Observation/
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Far infrared image of reflection nebulae IC4954
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Star forming region observed with AKARI
Visible light
AKARI 9 & 18 mmCredit: Davide De Martin (http://www.skyfactory.org/), ESA/ESO/NASA FITS Liberator & Digitized Sky Survey
Reflection nebulae IC1396
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Large Megellanic Cloud
Visible light
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Far infrared image of LMC observed with AKARI
AKARI65, 90, & 140 µm
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AKARI detected fluctuation of sky brightness which could be pop.III origin
2.4mm 3.2 mm 4.1 mm
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90% of the whole sky was surveyed
~880,000 sources are detected
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AKARI-FIS BSC b-2
PRELIMINARY
WIDE-S (90 µm)
284,633 sources
•First point source catalogue will be opened to public in next spring
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Next mission after AKARI?
Space observation is very sensitive, but angular resolution is not so good compared with optical and radio due to the diffraction limit.
l/D ~ 30 arcsec, at 100 mm for AKARI
It is too heavy to install large aperture telescope for the traditional space infrared mission (IRAS, ISO, AKARI).
New idea is required!
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No cryogen, warm launchCooled down in space with mechanical coolerEffective radiation cooling at L2 orbit
-> SPICASpace Infrared Telescope for Cosmology and Astrophysics
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Outline of SPICATo reveal the history of Universethrough Infrared Observations
Telescope: 3.5m, 4.5 K HSO: 3.5m, 80K JWST: ~6m, <50K
Core λ: 5-200 μmMIR imaging, spectroscopyFIR imaging, spectroscopy (SAFARI)NIR, MIR coronagraph (option)NIR camera (FPC, option)
Orbit: Sun-Earth L2 Halo Warm Launch, Cooling in Orbit No Cryogen
SPICA is now pre-project phase Final approval will be on 2010 fall
Launch: ~ 2017
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SPICA will be opened to world wide community
• We welcome participation of other countriesfocal plane instrumentsDevelopment of softwareSatellite operationObservation and science
• Open time to general community (~20%) is planned
Contact person: [email protected]
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AKARI Point Source Catalogue(s)
MIR FIR b-2
Wavelength (µm)
9, 1865, 90, 140,
160
Number of sources
~880,000 284,633
Detection limit
50 & 130 mJy0.5~ 7 ~ 13
Jy
Photometric uncertainty
7–15 % 30 ~ 50 %
Spatial resolution
~10 arcsec ~1 arcmin
Position uncertainty
1–3 arcsec 4–5 arcsec
•First point source catalogue will be opened to public in next spring