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- -cloud interaction cloud interaction cloud interaction SNR SNR 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 Arikaw a, Tatematsu et al. W28 W28 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 submm Examples of Examples of submm submm J=3 submm 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 0 0 stepctra 0 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 3 Mo – shocked: T>=60K, n>=10 4 cm -3 , M=2X10 3 Mo � 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 -going and near future going and near future going and near future On On 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: Atacama ASTE: ASTE: Atacama Atacama Submillimeter Atacama 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- -J Prototype for J Prototype for J Prototype for ALMA ALMA J Prototype for � USA Japan � competition: competition: Japan Japan USA USA competition: competition: Japan USA

ALMA: ALMA: Atacama ALMA: ALMA: Atacama Atacama Large Large Large Atacama Large Milimmeter/submillimeter Milimmeter /submillimeter Aray /submillimeter Aray Aray Milimmeter Milimmeter /submillimeter 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” ” band low est center highest bandw idth Trx (DSB) (GHz) (GHz) (GHz) (highest- over 80% low est)/center (1) 30 35 40 0.286 7.5 K (2) 67 79 90 0.291 14 K 3 84 100 116 0.320 17 K 4 125 144 163 0.264 23.5 K (5) 163 187 211 0.257 30 K 6 211 243 275 0.263 37.5 K 7 275 323 370 0.294 66.5 K 8 385 442 500 0.260 90.5 K 9 602 660 720 0.179 168 K 10 787 869 950 0.188 219 K Prospects for SNR Prospects for SNR- -cloud cloud cloud Prospects for SNR Prospects for SNR 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