ALMA Early Science ” Cycle1” Capability, Policy & Science Case

Presentation on theme: "ALMA Early Science ” Cycle1” Capability, Policy & Science Case"— Presentation transcript:

1 ALMA Early Science ” Cycle1” Capability, Policy & Science Case
Kazuya Saigo, Eiji Akiyama, Yasutaka Kurono, Yuichi Matsuda (NAOJ Chile Observatory) This Talk ALMA Overview ALMA Early Science Cycle 1 Capability I 　Basic (Frequency/Sensitivity/Resolution) ALMA Early Science Cycle 1 Capability II 　Observational Modes/Limit ACA ALMA Science M100 (CSV result 12m array + ACA) Town Meeting Cycle1 Capability, Policy, & Scince Case 2012/6

2 Town Meeting Cycle1 Capability, Policy, & Scince Case
What is ALMA Project. ＡＬＭＡ Project Overview BBC (C) 2012 Atacama Large Millimeter/submillimeter Array at 5000 m high site in northern Chile ALMA is in construction phase now. Early Science Phase (Construction phase) 2011 Cycle 0 operation Cycle 1 operation … we are here! 2013 Cycle 2 operation Inauguration (The end of a construction phase) Full Operation Phase (All observation modes become available.) Main Array: 12m x 50 Antennas 　 - Atacama Compact Array: 12m x 4 + 7m x 12 Even in cycle1 phase , ALMA achieves with the highest sensitivity and the highest spatial resolution in observation at submillimeter wavelength. The ALMA Project is a joint project among East Asia, Europe, and North America in cooperation with Chile. Town Meeting Cycle1 Capability, Policy, & Scince Case 2012/6

3 ALMA Early Science Cycle 1 Timeline
31 May, 2012 (15:00UT) Call for Proposal Opening of the Archive for proposal submission 12 July 2012 (15:00 UT) Proposal submission deadline November Announcement of the outcome of the Proposal Review Process 1 January 　　 Start of ALMA Cycle 1 Science Observations （May 2013　Expected deadline for proposal submission for Cycle 2 ) 31 October 　　 End of ALMA Cycle 1 Total observation time in Cycle1 800 hours for 12m main array Up to 800 hours for ACA system 　(see later) About 200 highest priority projects are expected to be prepared for scheduling. ←　we are here! Town Meeting Cycle1 Capability, Policy, & Scince Case 2012/6

4 Cycle 1 Basic Capability – Spectral Setting -
1. Band (Frontend Detector) example line - Band 3 (2SB: 84GHz - 116GHz) : CO(1-0), HCO+(1-0), CS(2-1), N2H+(1-0),,, - Band 6 (2SB: 211GHz - 275GHz) : CO(2-1), HCO+(3-2), CS(5-4), N2D+(3-2),,,, - Band 7 (2SB: 275GHz - 373GHz) : CO(3-2), HCO+(4-3), CS(6-5/7-6), N2H+(3-2), N2D+(4-3), - Band 9 (DSB: 602GHz - 720GHz): CO(6-5), HCO+(7-6/8-7), CS(13-12/14-13), H2D+(8-7/9-8), H2S, 2. Frequency Resolution & Setting (Correlator) - We can select spectral setting from 15 spectral modes for each line. Effective Channel Number: 3840 (x 2 pol.) for each spectral line Frequency resolution: kHz～976.5kHz (⇔ Bandwidth=58.6MHz～2GHz) Correlator Modes, dual-polarization (Proposers Guide A5) 27km/s 0.85km/s 0.42km/s 0.21km/s 0.11km/s 0.053km/s 0.027km/s Velocity Resolution at 345GHz Bandwidth (MHz) Channel spacing Spectral Resolution (MHz)　　　 ↓ dv at 100GHz Number of channels Correlator mode 2000 15.6 (93.7km/s) 128 TDM 1875 0.488 (2.93km/s) 3840 FDM 938 0.244 (1.46km/s) 469 0.122 (0.732km/s) 234 0.061 (0.366km/s) 117 0.0305 (0.183km/s) 58.6 0.0153 (0.091km/s) Town Meeting Cycle1 Capability, Policy, & Scince Case 2012/6

5 Cycle 1 Basic Capability – Spectral Setting -
1. Band (Frontend Detector) example line - Band 3 (2SB: 84GHz - 116GHz) : CO(1-0), HCO+(1-0), CS(2-1), N2H+(1-0),,, - Band 6 (2SB: 211GHz - 275GHz) : CO(2-1), HCO+(3-2), CS(5-4), N2D+(3-2),,,, - Band 7 (2SB: 275GHz - 373GHz) : CO(3-2), HCO+(4-3), CS(6-5/7-6), N2H+(3-2), N2D+(4-3), - Band 9 (DSB: 602GHz - 720GHz): CO(6-5), HCO+(7-6/8-7), CS(13-12/14-13), H2D+(8-7/9-8), H2S, 2. Frequency Resolution & Setting (Correlator) - We can select spectral setting from 15 spectral modes for each line. Effective Channel Number: 3840 (x 2 pol.) for each spectral line Frequency resolution: kHz～976.5kHz (⇔ Bandwidth=58.6MHz～2GHz) - ALMA can observe 4 spectral lines with different frequency resolution simultaneously. Frequency Band which can be observed simultaneously Band 7 Band 7 example1 Upper Sideband Lower Sideband CO (3-2) n = 345.8GHz BW=938MHz (dv=0.42km/s) H13CO+(4-3) n = 347.0GHz BW=469MHz (dv=0.21km/s) HCO+(4-3) n = 356.7GHz BW=469MHz (dv=0.21km/s) Continuum n= 358GHz BW = 2000MHz Town Meeting Cycle1 Capability, Policy, & Scince Case 2012/6

6 Cycle 1 Basic Capability – Spectral Setting -
1. Band (Frontend Detector) example line - Band 3 (2SB: 84GHz - 116GHz) : CO(1-0), HCO+(1-0), CS(2-1), N2H+(1-0),,, - Band 6 (2SB: 211GHz - 275GHz) : CO(2-1), HCO+(3-2), CS(5-4), N2D+(3-2),,,, - Band 7 (2SB: 275GHz - 373GHz) : CO(3-2), HCO+(4-3), CS(6-5/7-6), N2H+(3-2), N2D+(4-3), - Band 9 (DSB: 602GHz - 720GHz): CO(6-5), HCO+(7-6/8-7), CS(13-12/14-13), H2D+(8-7/9-8), H2S, 2. Frequency Resolution & Setting (Correlator) - We can select spectral setting from 15 spectral modes for each line. Effective Channel Number: 3840 (x 2 pol.) for each spectral line Frequency resolution: kHz～976.5kHz (⇔ Bandwidth=58.6MHz～2GHz) - ALMA can observe 4 spectral lines with different frequency resolution simultaneously. Band 7 example2 Continuum emission only (single continuum mode) Bandwidth=8GHz (2GHz x4) Band 7 Band 7 Lower Sideband Upper Sideband Town Meeting Cycle1 Capability, Policy, & Scince Case 2012/6

7 Cycle 1 Basic Capability – Sensitivity & Resolution -
1. Band (Frontend Detector) example line - Band 3 (2SB: 84GHz - 116GHz) : CO(1-0), HCO+(1-0), CS(2-1), N2H+(1-0),,, - Band 6 (2SB: 211GHz - 275GHz) : CO(2-1), HCO+(3-2), CS(5-4), N2D+(3-2),,,, - Band 7 (2SB: 275GHz - 373GHz) : CO(3-2), HCO+(4-3), CS(6-5/7-6), N2H+(3-2), N2D+(4-3), - Band 9 (DSB: 602GHz - 720GHz): CO(6-5), HCO+(7-6/8-7), CS(13-12/14-13), H2D+(8-7/9-8), H2S, 2. Frequency Resolution & Setting (Correlator) - We can select spectral setting from 15 spectral modes for each line. Effective Channel Number: 3840 (x 2 pol.) for each spectral line Frequency resolution: kHz～976.5kHz (⇔ Bandwidth=58.6MHz～2GHz) - ALMA can observe 4 spectral lines with different frequency resolution simultaneously. 3. Sensitivity (Number of Antennas) Main Array: x 12m antennas Additional subarray: 7 x 7m anntenas + 2 x 12m single dish (ACA system) New!　 Sensitivity in Cycle1 = x 2 of Cycle0 Image quality improves! 4. Spatial Resolution (Configurations) configurations Maximum baseline = 166m ～ 1 km The maximum spatial resolution becomes times higher than that in cycle 0. 　 Town Meeting Cycle1 Capability, Policy, & Scince Case 2012/6

8 Town Meeting Cycle1 Capability, Policy, & Scince Case
干渉計観測 参考 天球上の位置ベクトル r 天球 相関機 最大18km 干渉計は普通の観測と違い、天体からのフラックス強度分布のフーリエ分解成分を観測し、それを逆フーリエで画像に戻します※。　　 ※天体からの電磁波を相関機で干渉させると、ビジビリティー（visibility,干渉縞の明暗強度)が得られます。簡単のために１次元uで考えると、 となります(実際は２次元)。逆フーリエ変換し天体輝度分布 I(r) を得ます。 Point 1: アンテナ間距離（基線）が長いアンテナペアで観測すると空間周波数が高い　（小さな空間スケールのフーリエ成分）情報が得られます(最大基線長⇔空間分解能)。 Point 2: 最短基線長間の相関からはもっとも低い空間周波数情報が得られます。より低い空間周波数情報は得られないため、より広がった空間構造成分は干渉計観測画像から落とされます(最短基線長⇔Resolve Out)。flux強度絶対値の不定性となります。 Point 3: 単一鏡電波観測と異なり、干渉計観測では１つの座標の観測でも画像が得られます。画像サイズはアンテナ口径で決まり各アンテナの視野(=Beam Size)と同じです。 Spatial Resolution:　　　　　　　　　　　　　　　　　　　　　　　n: 観測周波数、Lmax:最大基線長 Resolve Outスケール：　　　　　　　　　　　　　　　　　　　　n:観測周波数、Lmin:(実効)最短基線長 視野サイズ（画像サイズ）：　　　　　　　　　　　　　　　　　n:観測周波数、Dantenna:アンテナ口径 Town Meeting Cycle1 Capability, Policy, & Scince Case 2012/6

9 Cycle 1 Basic Capability Sensitivity Examples1 (Continuum emission)
BW=8GHz, t = 60 min s sensitivity Point Source Most Compact Conf. Most Extended Conf. Band 3 (100GHz) : mJ mK (3.7”) mK (0.57”) Band 6 (230GHz) : mJ mK (1.6”) mK (0.25”) Band 7 (345GHz) : mJ mK (1.1”) mK (0.16”) Band 9 (675GHz) : mJ mK (0.55”) mK (0.08”) Town Meeting Cycle1 Capability, Policy, & Scince Case 2012/6

10 Cycle 1 Basic Capability Sensitivity Examples2 (Line emission)
・ALMA Science Verification Data (TW Hya) integrated intensity, intensity weighted velocity field, TW Hya is neayby protoplanetary disk (d=50pc). This is HCO+(4-3) maps from TW Hya, with white continuum contours at 3 and 100 sigma. ・Sensitivity and Spatial Resolution in Cycle1 In Cycl1, ALMA enable us to obtain the emission line image map of nearby protoplanetary disks with the spatial resolution of a 0.1" order. ALMA HCO+(4-3) moment maps from TW Hya, with white continuum contours at 3 and 100 sigma. From left to right: integrated intensity, intensity weighted velocity field, intensity weighted velocity dispersion are shown. Most Compact, dn=0.244MHz, t = 60 min Beam Size 1s Band 3 (100GHz) : 3.7”, mK Band 6 (230GHz) : 2.6”, mK Band 7 (345GHz) : 1.1”, mK Band 9 (675GHz) : 0.55”, mK Most Extended, dn=0.244MHz, t = 60 min Beam Size 1s Band 3 (100GHz) : 0.57”, K Band 6 (230GHz) : 0.25”, K Band 7 (345GHz) : 0.16”, K Band 9 (675GHz) : 0.08”, K Town Meeting Cycle1 Capability, Policy, & Scince Case 2012/6

11 Cycle 1 Basic Capability UV plane/Beam Pattern
Most Compact Configuration Case (Lmax=160m, t = 10min) Antenna Configuration UV y (m) Side lobes: below 10%! x (m) Most Extend Configuration (Lmax=1000m, t = 10min) Antenna Configuration UV y (m) Side lobes: below 10%! x (m) Town Meeting Cycle1 Capability, Policy, & Scince Case 2012/6

12 Town Meeting Cycle1 Capability, Policy, & Scince Case
参考 ALMA Cycle1 beam patterns with various configurations (integration time =10min, f = 345GHz) Configuration C32-1 Configuration C32-1 Configuration C32-3 Configuration C32-4 Configuration C32-5 Configuration C32-6 12-m Array Configuration Min Baseline (meters) Max Baseline1 ACA Allowed? C32-1 15 166 Yes C32-2 304 C32-3 21 443 C32-4 558 C32-5 26 820 No C32-6 43 1091 Even in only 10 minutes observation, - Beam: almost round shape! - Side lobes: below 10%-20%! Town Meeting Cycle1 Capability, Policy, & Scince Case 2012/6

13 ALMA Early Science Cycle1 Capability
- Observing Mode/Operation - Observation Mode No sub-array Mosaic (up to 150 field) No Polarization No solar Observation Operation - Target of Opportunity (ToO) and Director Discretionary Time (DDT) Like standard proposals, these proposals must be submitted by the Cycle 1 proposal deadline. - Only a few ToO proposals are likely to be among the highest ranked Cycle 1 proposals. The reaction time for its execution from triggered may be as long as 3 weeks. Shorter reaction times (few days) may be possible but are not guaranteed. ACA (Atacama Compact Array) ACA(7m array + Single Dish) operation start! M100 Rectangle field 300”x280” Mosaic (149 fields) at n=115GHz Town Meeting Cycle1 Capability, Policy, & Scince Case 2012/6

14 ALMA Early Science Cycle1 Capability
Cycle 1 Obs. Modes ALMA Early Science Cycle1 Capability - Additional Limitations - Up to five Science Goals per proposal. * Science Goal: an Observational Setting (Spectral Setting/Sensitivity) Limitation of Target Number 　 Up to 15 individual sources (within 15 degrees on the sky) in a single Science Goal We can set multi-points observation to each target. But total number of positions (fields) in each proposal should be less than 151. The maximum observing time per proposal is 100 hours (Standard Program) Cycle 1 observations will be scheduled mainly during nighttime. All Cycle 1 Early Science observing will be conducted on a best effort basis. Cycle 1 projects that have not been completed by the end of the cycle will not be carried over to Cycle 2. Target Position Pointing Fields X 14 Town Meeting Cycle1 Capability, Policy, & Scince Case 2012/6

15 Town Meeting Cycle1 Capability, Policy, & Scince Case
Accuracy ALMA observatory provides calibrator (PI can define it). Accuracy of Absolute Amplitude Calibration Band 3: good to 5% Band 6/Band 7: good to 10% Band 9 : good to 20% (Goal) Positional Accuracy about 1/10th of synthetic beam size (It depends on noise level when a S/N ratio is low. ) Town Meeting Cycle1 Capability, Policy, & Scince Case 2012/6

16 ACA (Atacama Compact Array)
　ACA is the tool for imaging of spread structure correctly. By combining the data of 12-m array and ACA array, we can recover Resolve Out which is a weak point of an interferometer with keeping high spatial resolution. ACA System in Cycle1 9 x 7m antennas array 　 One configuration (baseline = 8.5m ～ 43m Baseline) 2～3台 x12m Single Dish (TP: Total Power Array) ACA Cycle 1 Capability In Cycle 1, we can use ACA in compact 12-m Array configurations (tminimum baselines less than 25 m = Lmax < 558m) . TP array can not observe continuum emission. (7m-array can observe continuum) Observation time of ACA 3 x (12-m Array observation time) 　 12-m Array Configuration Min Baseline (meters) Max Baseline1 ACA Allowed? C32-1 15 166 Yes C32-2 304 C32-3 21 443 C32-4 558 C32-5 26 820 No C32-6 43 1091 Town Meeting Cycle1 Capability, Policy, & Scince Case 2012/6

17 Town Meeting Cycle1 Capability, Policy, & Scince Case
参考 干渉計観測 天球上の位置ベクトル r 天球 相関機 最大18km 干渉計観測とは、天体からのフラックス強度分布のフーリエ分解成分を観測する装置。それを逆フーリエ変換で画像に戻します※。　　 ※天体からの電磁波を相関機で干渉させると、ビジビリティー（visibility,干渉縞の明暗強度)が得られます。簡単のために１次元uで考えると、 となります(実際は２次元)。逆フーリエ変換し天体輝度分布 I(r) を得ます。 Point 1: アンテナ間距離（基線）が長いアンテナペアで観測すると空間周波数が高い　（小さな空間スケールのフーリエ成分）情報が得られます(最大基線長⇔空間分解能)。 Point 2: 最短基線長間の相関からはもっとも低い空間周波数情報が得られます。それより低い空間周波数情報は得られないため、広がった空間構造成分は干渉計観測画像から欠落します(最短基線長⇔Resolve Out)。 Point 3: 単一鏡電波観測と異なり、干渉計観測では１つの座標の観測でも画像が得られます。画像サイズはアンテナ口径で決まり各アンテナの視野(=Beam Size)と同じです。 Spatial Resolution:　　　　　　　　　　　　　　　　　　　　　　　n: 観測周波数、Lmax:最大基線長 Resolve Outスケール：　　　　　　　　　　　　　　　　　　　　n:観測周波数、Lmin:(実効)最短基線長 視野サイズ（画像サイズ）：　　　　　　　　　　　　　　　　　n:観測周波数、Dantenna:アンテナ口径 Town Meeting Cycle1 Capability, Policy, & Scince Case 2012/6

18 Town Meeting Cycle1 Capability, Policy, & Scince Case
Recovered flux of a uniform disk, with a total flux of 1 Jy, observed at 100 GHz with three different 12-m Array configurations, as a function of the disk size. Town Meeting Cycle1 Capability, Policy, & Scince Case 2012/6

19 ACA (Atacama Compact Array)
　ACA is the tool for imaging of spread structure correctly. By combining the data of 12-m array and ACA array, we can recover Resolve Out which is a weak point of an interferometer with keeping high spatial resolution. ACA System in Cycle1 9 x 7m antennas array 　 Single configuration (baseline = 8.5m ～ 43m Baseline) 2 antennas x12m Single Dish (TP: Total Power Array) ACA Cycle 1 Capability In Cycle 1, we can use ACA in compact 12-m Array configurations (tminimum baselines less than 25 m = Lmax < 558m) . TP array can not observe continuum emission. (7m-array can observe continuum) Observation time of ACA 3 x (12-m Array observation time) 　 12-m Array Configuration Min Baseline (meters) Max Baseline1 ACA Allowed? C32-1 15 166 Yes C32-2 304 C32-3 21 443 C32-4 558 C32-5 26 820 No C32-6 43 1091 Town Meeting Cycle1 Capability, Policy, & Scince Case 2012/6

20 Demonstration of Data Combine (M100)
ACA例 Demonstration of Data Combine (M100) 12m main array only Very Large Telescope (VLT) FORS ALMA band 3, CO(1-0) moment 1 ALMA Science Verification Data: M100 Town Meeting Cycle1 Capability, Policy, & Scince Case 2012/6

21 Demonstration of Data Combine (M100) CO(1-0) Moment Map
ACA例 Demonstration of Data Combine (M100) CO(1-0) Moment Map 12m array (Main array) + 12m Total Power (single dish) On the fly mapping 7m array Town Meeting Cycle1 Capability, Policy, & Scince Case 2012/6

22 Demonstration of Data Combine (M100)
ACA例 Demonstration of Data Combine (M100) 12m array ALMA band 3, CO(1-0) moment 1 Recovering by ACA 12m array only 12m array + ACA Velocity [km/s] mJy/Beam CO(1-0) line profile Very Large Telescope (VLT) FORS Town Meeting Cycle1 Capability, Policy, & Scince Case 2012/6

23 ACA (Atacama Compact Array)
　ACA is the tool for imaging of spread structure correctly. By combining the data of 12-m array and ACA array, we can recover Resolve Out which is a weak point of an interferometer with keeping high spatial resolution. ACA System in Cycle1 9 x 7m antennas array 　 Single configuration (baseline = 8.5m ～ 43m Baseline) 2 antennas x12m Single Dish (TP: Total Power Array) ACA Cycle 1 Capability In Cycle 1, we can use ACA in compact 12-m Array configurations (tminimum baselines less than 25 m = Lmax < 558m) . Observation time of ACA 3 x observation time of 12m main array → Total observation time = obs time of 12m main array obs time of ACA TP array can not observe continuum. (7m-array can observe continuum) 　　 12-m Array Configuration Min Baseline (meters) Max Baseline1 ACA Allowed? C32-1 15 166 Yes C32-2 304 C32-3 21 443 C32-4 558 C32-5 26 820 No C32-6 43 1091 Town Meeting Cycle1 Capability, Policy, & Scince Case 2012/6

24 Town Meeting Cycle1 Capability, Policy, & Scince Case
参考 Angular resolution and Maximum Angular Scale for the six Cycle 1 12-m Array configurations (Proposers Guide Table A.2) この配列では、5”を超える空間スケール構造はResolve Outする （観測できない）。⇔ Max Ang Scale そのような観測にはACAを使うことが必要となる。 たとえば、 - 周波数 345GHzの観測 空間分解能0.4” を要求する。 つまり、12mアンテナ配列 C32-3が観測で使われる配列である。 Town Meeting Cycle1 Capability, Policy, & Scince Case 2012/6

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参考 Angular resolution and Maximum Angular Scale for the six Cycle 1 12-m Array configurations (Proposers Guide Table A.2) Angular resolution and maximum angular scales for continuum4 observations using the allowed 12-m Array & ACA combinations 5”以上に広がった構造を観測したいならばACAを用いるが、 さらに、13”までは7m array + 12m arrayで事足りる。 それ以上は、TP(12m single dish)を足さないとだめ。 たとえば、周波数 345GHzの観測をする。空間分解能は0.4”を要求する。 Town Meeting Cycle1 Capability, Policy, & Scince Case 2012/6

26 Town Meeting Cycle1 Capability, Policy, & Scince Case
Shadowing ALMA is located at latitude = 23.029°, longitude = 67.755°. Targets as far north as declination +40°, corresponding to a maximum source elevation at Chajnantor of ~25°, can in principle be observed from the ALMA site, but shadowing by adjacent antennas becomes an increasing problem at low elevations. The imaging capability, as well as the time on source, will necessarily be limited for such northern sources. Shadowing depends on the antenna configuration. Given the short baselines in the ACA configuration, sources with declinations less than −60° or greater than +20° will be subject to significant shadowing. For the 12-meter array, shadowing becomes significant (> 5 %) in the most compact configuration for sources with declination lower than −75° or higher than +25°. Shadowing fraction vs. Declination for the two most compact configurations of the 12-m Array and for the 7-m Array with a track duration of 2 hours (±1h HA). Town Meeting Cycle1 Capability, Policy, & Scince Case 2012/6

27 Town Meeting Cycle1 Capability, Policy, & Scince Case
Weather Condition Cycle 1 observations will be scheduled mainly during nighttime. The numbers indicate the percentage of time when the pwv is below 1 mm as a function of Local Sidereal Time (LST) and week number beginning with January 1, 2013. local midnight shuotdown ALMA engineering time ALMA Band Band 3 Band 6 Band 7 Band 9 Fraction of time 100% 70% 40% 10% Estimated maximum fraction of Early Science observing time suitable for observations in each band in Cycle 1 Town Meeting Cycle1 Capability, Policy, & Scince Case 2012/6

28 Summary of Cycle1 Capablity
Call for Proposal is scheduled the end of May. Proposal submission deadline is scheduled 12th of July. Total observation time of 12m main array is 800hours. Compared with Cycle0, The sensitivity: x The maximum spatial resolution: x 2.5 (1.2" - ACA is available. Summary of Most Extended Configuration Lmax= 1km ( )<=Most Compact Lmax=160m Band Frequency (GHz) Angular Resolution Maximum Scale Flux *1 (mJy) Tb *2 (K) Field of View 3 100 0.57” (3.7”) 8.6” (25”) 0.06 2.4 (0.056) 62” 6 230 0.25” (1.6”) 3.7” (11”) 0.09 1.9 (0.047) 27” 7 345 0.16” (1.1”) 2.5” (7.1”) 0.15 2.9 (0.062) 18” 9 670 0.08” (0.55”) 1.3” (3.6”) 1.10 16 (0.35) 9” 1: 5 sigma continuum sensitivity (Bandwidth=8GHz) for 1hr 2: 3 sigma line sensitivity for 1 hr (1 km/s) Town Meeting Cycle1 Capability, Policy, & Scince Case 2012/6

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ALMAによるサイエンス例 Town Meeting Cycle1 Capability, Policy, & Scince Case 2012/6

31 The narrow dust ring around Fomalhaut (Boley +12, Cycle0 paper)
Optical images trace micron-sized grains, which are strongly affected by stellar radiation. Radio continuum trace millimeter-sized grains, which trace parent bodies. => ALMA high spatial resolution observation. © ALMA (ESO/NAOJ/NRAO). Visible image: the NASA/ESA (HST) ALMA obs. Suggest that debris confined by shepherd planets is the most consistent with the ring’s morphology. Town Meeting Cycle1 Capability, Policy, & Scince Case 2012/6

32 [CII]158um emission at z=5 (Wagg+12, science verification)
[CII] line detection in a pair of gas-rich galaxies L[CII] = 10.0 x 109 L⊙ L[CII] = 6.5 x 109 L⊙ [CII]-to-FIR ratio ~ 0.1 – 1% The total observing time 25 min (on-source) 20h SMA simeq 3 sigma (Iono + 06) Follow up observation of K.Ohta +96, Iono +06 20h SMA obs. => only 3 sigma (Iono + 06) Town Meeting Cycle1 Capability, Policy, & Scince Case 2012/6

33 [NII]205um emission at z=5 (Nagao+12, cycle 0 paper)
The first measurement of the [NII]/[CII] flux ratio in high-z galaxies (SMGs are chemically evolved) Total observing time 3.6hrs Town Meeting Cycle1 Capability, Policy, & Scince Case 2012/6

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Materials Town Meeting Cycle1 Capability, Policy, & Scince Case 2012/6

36 Town Meeting Cycle1 Capability, Policy, & Scince Case
Cycle1 Continuum emission（Bandwidth = 8GHz）　Sensitivity Cycle 1 (３２ 12m array) t = 60 min　 Dec 　　　 = -30deg Most Compact (L=160m) Most Extended(L=1km) Town Meeting Cycle1 Capability, Policy, & Scince Case 2012/6

37 Town Meeting Cycle1 Capability, Policy, & Scince Case
Review Process プロポーザルは、5つのCategoriesに分けられる。 各CategoryにあるReview Panelに振り分けられ、科学的審査される。 ※各Categoryには 2つ程度のReview Panel(６名程度)が作られる。 High priority proposalになる可能性が高いものは技術審査を受け、観測実現不可なProposalを除く。 全プロポーザルで採点の高い順からHigh priority proposalを採択する。 　ただし、以下の割合となるようにされる。 22.5% for East Asia (EA); 33.75% for Europe (EU); 33.75% for North America (NA); 10% for Chile. Review Panelによる審査は11月に行われる予定である。 Town Meeting Cycle1 Capability, Policy, & Scince Case 2012/6

38 Town Meeting Cycle1 Capability, Policy, & Scince Case
観測デモンストレーション ALMAが提供するCASA(解析ツール)には観測シミュレーターが付随している。視直径0.8secのタイタンを例にCycle1での空間分解能をデモンストレーションすると、 最大160m基線長 最大1000m基線長 Titan表面のHST画像より モデル作成 (Smith et al. 1996) (注意) 今回は画像変換のデモンストレーション Town Meeting Cycle1 Capability, Policy, & Scince Case 2012/6

39 Titan (Full Operation Phase)
ビームサイズ 0.02” モデルTitan ALMAで観測すると, フーリエ成分 (u-v 平面） 差分 　 Titan表面のイメージ HST画像より作成 (Smith et al. 1996) ALMAなら詳細な構造や リム部分も空間分解 d=8AUで100kmを分解能 50台の12mアンテナ、最大基線長 11.5km、積分時間2時間、230GHzの場合 The Common Astronomy Software Applications (CASA) 　干渉計simulatorを使用　 　 Town Meeting Cycle1 Capability, Policy, & Scince Case 2012/6