あかり遠赤外線全天サーベイによる...
Transcript of あかり遠赤外線全天サーベイによる...
あかり遠赤外線全天サーベイによる銀河ダスト構造の解明
土井靖生 (東京大学)FIS diffuse map making team
FIS Map Making Team
Yasuo DoiShinya Komugi
Norio IkedaTakafumi OotsuboMasahiro Tanaka
Mitsunobu KawadaShuji Matsuura
Yoshimi KitamuraTakao Nakagawa
Makoto HattoriLys Figueredo
Mireya Etxaluze AzkonagaGlenn White
AKARI satellite
Continuous All-Sky Survey Mapping● Sun synchronous polar orbit – just like IRAS● 900 km orbital altitude / 98 min orbital period
Band center [um] 65 90 140 16074x56 93x64 107x85 94x78
12 2 4 7PSF size [arcsec]Detection limit [1σ, MJy/sr]
AKARIAKARI 90um+140um Cygnus
Far-infrared all sky mappingFar-infrared all sky mapping
Note that the numbers are preliminary.
Survey coverage
all sky map in ecliptic coordinates
blue: 1black: 0 light blue: 2 green: 3~ red: 10~
Survey coverage
● >99% of the sky has been covered, >97-98% of them are multiply scanned
● Scan coverage is not spatially uniform● stripy non-observed regions around the ecliptic plane● Data quality depends upon Nscan (under investigation)
● Better coverage is expected with careful investigation/recovery of the data around Moon
Higher spatial resolution than IRAS, comparable to Spitzer
FIS 90μm FIS 140μm MIPS 160μmHPBW 38”
Herschel 160μmHPBW 12”
AKARI covers the whole sky with ~1’ resolution
AKARI/SW wide AKARI/LW wide
Characteristics of the AKARI FIR survey Extended wavelength coverage beyond 100 mμ
BGs' color temperature, SED investigation
Unprecedented spatial dynamic range of >104
From arcminute-scale to the whole sky
AKARI
N60
WideS
WideL
N160
All sky images Shorter wavebands ISRF intensity∝ Longer wavebands ISRF intensity × dust column∝
Cygnus X (20°×15°, 65, 90, 140μm)
AKARIIRISDIRBE
CygnusX SED
Model by DustEM (Compiegne 2011)
Multiple component along LoS?
Galliano et al. 2011
Polaris Flare (15°×15°)
WideS(90μm) WideL(140μm)0~60 MJy/sr0~20 MJy/sr
Spatial power spectraStructure down to ~2'(WideL) & ~1'(WideS) can be successfully traced
Miville-Deschenes (2010)
∝k^-2.65±0.1
SPIRE250μm in central Polaris Flare
Spatial power spectraStructure down to ~2'(WideL) & ~1'(WideS) can be successfully traced
Miville-Deschenes (2010)
∝k^-2.65±0.1
SPIRE250μm in central Polaris Flare
銀河系内星間物質の成分分離
● Planck による飛躍的進展
● ダストピークの観測が重要● DIRBE(42' beam) → AKARI(1'-2' beam)!!
● Herschel/Hi-GAL● 70, 170, 250, 350, 500μm● 銀緯±1°以内
● 100μm前後のデータが欠損→AKARI 90μmの重要性
● 高空間分解能を活かし、よりローカルな星間環境の分離へ● 誰かやりませんか??
Cosmic Web??
WideS(90μm) WideL(140μm)0~60 MJy/sr0~20 MJy/sr
Polaris Flare (15°×15°)
Interstellar filaments
Andre et al. 2010
Hill et al. 2011
Interstellar filaments● As a site of star-formation● Typical width: ~0.1 pc
⇔ 3.4 arcmin @ 100pc, 1.1 arcmin @ 300pc● AKARI provides a complete map of the local
interstellar filaments
Arzoumanian et al. 2011
Hill et al. 2011
Interstellar filaments● Typical width: ~0.1 pc
⇔ 3.4 arcmin @ 100pc, 1.1 arcmin @ 300pc● AKARI provides a complete map of the local
interstellar filaments
Interstellar filaments● Typical width: ~0.1 pc
⇔ 3.4 arcmin @ 100pc, 1.1 arcmin @ 300pc● AKARI provides a complete map of the local
interstellar filaments!! → 誰かやりませんか??
近日公開予定
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