他波長観測時代におけるALMAの役割
齋藤 正雄
East Asian ALMA Project Scientist(National AstronomicalObservatoryy of Japan)p )2011/8/11

ALMA and High Energy Physics

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今日の話• ミリ波サブミリ波天文学
ブ• ALMAの紹介• 期待される高エネルギー天体の観測

ALMAポスターもご覧ください。

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ALMA and High Energy Physics3ミリ波サブミリ波• 連続波観測– ガス・ダストの質量・温度分布(10-100K)– 制動放射、シンクロトロン放射( 小）• 原子・分子の輝線・吸収線観測– ガス運動分布(0.1 km/s)– 分子・原子の物理状態(温度/密度/輻射場など– メーザー観測• 偏波観測– ダストの磁場による整列方向

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ALMA and High Energy Physics4ミリ波サブミリ波注意• 高密度
4 6 cm-3
3104-6• 高温30 – 50 K
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ALMA(Atacama Large Millimeter/Submillimeter Array)• ALMAはミリ波サブミリ波電波干渉計– 日、北米、欧、台湾、チリの国際協力– チリ北部標高5000mの乾燥大地に設置– アンテナ台数：12 m 54 台、7m 12 台
– 波長10 mmから0.35 mmをカバー– 分解能：0.01
0.01秒角秒角。HST の 10 倍
– 感度：従来の電波望遠鏡の 30 – 100
100倍程度倍程度– 品質が保証された画像データをユーザーに提供– データ占有権は1年、その後パブリックアーカイブへ– Target of Opportunityも事前にプロポーザルを提出
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ALMA
• チリ山頂施設でのアルマアンテナ群（CG）
施群

日本が担当するアタカマ・コンパク
日本が担当するアタカマコンパク
ト・アレイ（ACA）システム
12m アンテナ：4台77m
アンテナ 12台
アンテナ：12台© ALMA/ESO/NAOJ/NRAO
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2011.8現在5000mサイトでアンテナ16台稼働
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Major Specification
ScienceSi
RRequirementit
1. To detect CO/CII from milky way like galaxy at Z = 32 To
2.
T imagei
protostars/protoplanetaryt t / t lt
disks
di k att 150 pc
3. to provide precise images at 0.”1.
Parameter
Number of Antennas
Antenna Diameter
Antenna Surface Precision
All-Sky Pointing Accuracy
Antenna Pointing Accuracy
Antenna primary beamFinest Angular Resolution
2011/8/1112m Spec
5412 m< 25 m rms< 2”.0 rms< 0".6 rms
17" x  (mm)17
".015 x  (mm)ALMA and High Energy Physics

7m Spec
127m< 20 m rms< 2”.0 rms< 0".6 rms
" x  (mm)5" x  (mm)9Imaging Quality
DM Tau with NMA ((5 antennas))
Saito et al. 1995

M87 with VLA ((27 antennas))
NRAO / AUI / NSF

ALMA will be better!

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ALMA and High Energy Physics

10初期科学運用
建設完了前に高い能力を生かし運用開始• 2011.3. Cycle 0 Call for Proposal• 2011.9.
2011 9 Cycle0
C l 0 観測開始
• 2012. 2. Cycle1 Call for Proposal• 2012. 3末. Cycle 1 Proposal deadline• Cycle0 (best effort)– 919件の応募、現在審査中– 観測時間は8カ月、500-700 hr– limited Target of Opportunity観測
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Cycle 0 仕様••••

16 x 12m antenna array18-125m, 36-400m baselines, 2 configurations
Single field imaging and Mosaics up to 50 fields
Frontend– Band 3 (2SB: 84GHz - 116GHz)– Band 6 ((2SB: 211GHz - 275GHz))– Band 7 (2SB: 275GHz - 373GHz)– Band 9 (DSB: 602GHz – 720GHz)• Ampp Calibration ggood to 5% ((band 3)) and less accurate
at high frequenciesf• The goals are: better than 10% in bands 6 and 7, andbetter than 20% in band 9.

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ALMA and High Energy Physics

12大気透過率2011/8/11

ALMA and High Energy Physics

13分解能と感度1

1

2

1: 5 sigma
1
icontinuumti
sensitivity
iti it ffor 1 hhr
2: 3 sigma line sensitivity for 4 hr (1 km/s)
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Cycle0の感度：SMAと比較• Spatial Resolution
Max baseline of SMA～600m
ALMA ES (cycle0) ～400m

Similar to SMA extended Configuration• 感度 （2GHz Bandwidth 1 3.2mJy @ 345GHz)
SMA integ time(WV 2.50mm) τ=4.0hr
ALMA integ
i t time(WVti (WV 11.26mm)
26) τ=7.8sec
78※ (SMA http://sma1.sma.hawaii.edu/beamcalc.html , ALMA OT)

SMA

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例1：SZ効果• 高エネルギー電子によるCMBのゆがみ
高ギが• X線観測と合わせ密度や温度• 強度は~1 mK、 Z依存性なし

218 GHz

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SZE gallary

Story+11 South Pole Telescope
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例2：AGN探査• 分子輝線観測でAGNの有無を診断
線• ALMAの感度で遠方銀河の診断可• 分子トーラス探査

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ALMA and High Energy Physics

Kohnoo o 05

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系外銀河の高温ガス• 振動励起した分子の回転遷移
転• 高温ガス（数100 K）の分布、運動Costagliola+10 NGC4414
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例3：SNR• SNRと分子雲の相互作用• ショックの物理• 粒子加速も？
• SNRは星形成のトリガー
成ガ

F k i 03
Fukui+03
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例4 原始惑星系円盤• X-ray ionization and heating alter diskychemistry.
• Disk dissipation
UV onlyUV+Xray

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ALMA and High Energy Physics

21Exploration of the unknown• Lessons from History– Majority
j y of discoveries were not from theory.
y– What a Radio telescope built for is almost
never what it is known fore.g. VLA case
• A quarter of its time during its initial decade ofoperation on the key science drivers listed in thegp
proposal.
pfunding

既存の常識にとらわれないプロポーザルをあるいはALMAアーカイブデータの活用を
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ALMA and High Energy Physics

22まとめ• ALMA E
Earlyl SScienceiCCyclel 0 Operation
Otiwith unprecedented sensitivity will start.
• Submit proposal to ALMA with originalideas or data.
• EA-ARC will support users to carry out
ALMA science via observation and archive
astronomy.
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ALMA Cycle 0 Capability

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www almaobservatory org
www.almaobservatory.org
The Atacama Large Millimeter/submillimeter Array (ALMA), an international astronomy facility, is a partnership among Europe, North
America and East Asia in cooperation with the Republic of Chile. ALMA is funded in Europe by the European Organization for
Astronomical Research in the Southern Hemisphere (ESO), in North America by the U.S. National Science Foundation (NSF) incooperation with the National Research Council of Canada (NRC) and the National Science Council of Taiwan (NSC) and in Japan by theNational Institutes of Natural Sciences (NINS) in cooperation with the Academia Sinica (AS) in Taiwan. ALMA construction andoperations are led on behalf of Europe by ESO, on behalf of North America by the National Radio Astronomy Observatory (NRAO), which
is managed by Associated Universities, Inc. (AUI) and on behalf of East Asia by the National Astronomical Observatory of Japan (NAOJ).
The Joint ALMA Observatory (JAO) provides the unified leadership and management of the construction, commissioning and operation ofALMAALMA..

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