SNR SNR- -cloud interaction cloud interaction cloud interaction - - PDF document

ALMA and the Prospects ALMA and the Prospects ALMA and the Prospects ALMA and the Prospects for Studies of SNR for Studies of SNR for Studies of SNR for Studies of SNR-

• Cloud

Cloud Cloud Cloud Interaction Interaction Interaction Interaction

Ken Tatematsu NAOJ, Japan

SNR SNR SNR SNR-

• cloud interaction

cloud interaction cloud interaction cloud interaction

One of the possible mechanisms

for γ-rays

– Pollock 1985 – Sturner & Dermer 1995

SNR W28 SNR W28 SNR W28 SNR W28

(Arikaw a, Tatematsu et al. 1999) (Arikaw a, Tatematsu et al. 1999) (Arikaw a, Tatematsu et al. 1999) (Arikaw a, Tatematsu et al. 1999)

W28 W28 W28 W28 Arikaw a, Tatematsu et al.

Arikaw a, Tatematsu et al. Arikaw a, Tatematsu et al. Arikaw a, Tatematsu et al.

Submillimeter molecular lines as

efficient tracer of shocks in molecular clouds

– Denser gas: 10 5-7 cm -3(submm) vs. 10 2-4 cm -3(mm) – Warmer gas: >30 K(submm) vs. 10-20 K (mm) – More sensitive: larger optical depth due to the statistical w eight 2J+1

Examples of Examples of Examples of Examples of submm submm submm submm J=3 J=3 J=3 J=3-

• 2

2 2 2 and mm J=1 and mm J=1 and mm J=1 and mm J=1-

0 stepctra stepctra stepctra stepctra

Results (1) from W28 Results (1) from W28 Results (1) from W28 Results (1) from W28

Detailed structure of SNR-cloud

interaction: 0.6-1 pc displacement betw een unshocked and shocked gas

Association w ith 1720-MHz OH

maser

Possible coincidence w ith

EGRET γ-ray

Results (2) from W28 Results (2) from W28 Results (2) from W28 Results (2) from W28

Enhancement of synchrotron near

molecular clouds

Physical properties

– unshocked: T<=20K, n<=10 3 cm -3, M=4X10 3Mo – shocked: T>=60K, n>=10 4 cm -3, M=2X10 3Mo

Energy deposited in shock: 3X10 48

ergs or 0.3% of the SNR energy

Rowell, Naito, et al. (2000) Rowell, Naito, et al. (2000)

Constraint on γ-ray production

mechanism by CANGALOO

Submillimeter Astronomy Submillimeter Astronomy Submillimeter Astronomy Submillimeter Astronomy

Kuiper Airborne Observatory: 1980- JCMT, CSO: 1988-

+HHT,AST/RO,

Mt.Fuji: 1998- No large submm in the southern

hemisphere

No interferometric submm

On On On On-

• going and near future

going and near future going and near future going and near future

10 m ASTE now in Chile 5000m 12m Japanese ALMA prototype

now being shipped to NRAO Socorro for competition

ALMA interferometer 2007

interim operation and 2011 completion

ASTE: ASTE: ASTE: ASTE: Atacama

Atacama Atacama Atacama Submillimeter Submillimeter Submillimeter Submillimeter Telescope Experiment, NAOJ Telescope Experiment, NAOJ Telescope Experiment, NAOJ Telescope Experiment, NAOJ

Transportation to 5000m: 2002

March

ASTE operating at ASTE operating at ASTE operating at ASTE operating at 100,200,350,500,800 GHz 100,200,350,500,800 GHz 100,200,350,500,800 GHz 100,200,350,500,800 GHz

ASTE operating at ASTE operating at ASTE operating at ASTE operating at 100,200,350,500,800 GHz 100,200,350,500,800 GHz 100,200,350,500,800 GHz 100,200,350,500,800 GHz ALMA ALMA ALMA ALMA-

• J Prototype for

J Prototype for J Prototype for J Prototype for competition: competition: competition: competition: Japan Japan Japan Japan USA USA USA USA

ALMA: ALMA: ALMA: ALMA: Atacama

Atacama Atacama Atacama Large Large Large Large Milimmeter Milimmeter Milimmeter Milimmeter/submillimeter /submillimeter /submillimeter /submillimeter Aray Aray Aray Aray

ALMA ALMA ALMA ALMA

North America (USA, Canada),

Europe (ESO), and Japan

USA and Europe: signed on 2003

Feb 25: Director=M. Tarenghi

Japan: R& D budget for 2002-

2003, 2004- construction budget planned

ALMA ALMA ALMA ALMA

2007 interim operation, 2011

completion

~80 antenna (32 12-m by USA,

32 12-m by Europe, and ACA consisting of 4 12-m and 12 7-m by Japan) across 14 km area

dow n to 0.01 arcsec resolution

ALMA ALMA ALMA ALMA

10 receiver bands mm, submm!

– 100, 230 GHz by USA – 330, 660 GHz by Europe – 140, 450, 850 GHz by Japan – 35, 80, 190 GHz in later years

Correlator

– “Baseline” w ith by USA – flexible “Second generation” by Japan/Europe

Details of 10 frequency Details of 10 frequency Details of 10 frequency Details of 10 frequency bands covering bands covering bands covering bands covering “ “w indow s w indow s w indow s w indow s” ”

219 K 0.188 950 869 787 10 168 K 0.179 720 660 602 9 90.5 K 0.260 500 442 385 8 66.5 K 0.294 370 323 275 7 37.5 K 0.263 275 243 211 6 30 K 0.257 211 187 163 (5) 23.5 K 0.264 163 144 125 4 17 K 0.320 116 100 84 3 14 K 0.291 90 79 67 (2) 7.5 K 0.286 40 35 30 (1) Trx (DSB)

• ver 80%

bandw idth (highest- low est)/center highest (GHz) center (GHz) low est (GHz) band

Prospects for SNR Prospects for SNR Prospects for SNR Prospects for SNR-

• cloud

cloud cloud cloud studies studies studies studies

Details of SNR shock layer

propagating into molecular clouds: comparison w ith theory

Study of CR ionization through

chemistry (HCO+, atomic C)

Study of SNR role in ISM

evolution in nearby galaxies

Summary Summary Summary Summary

SNR-cloud example in W28 (see

PASJ 51, L7)

ASTE operating in Chile

– 10-15 arcsec resolution at submm

ALMA-J prototype ALMA 0.01 arcsec universe in

submm