SMA, ASTE ALMA SMA, ALMA 10 K 1.1 HCN. ( 40 K) ( 10 7 cm 3 ) 10 5 cm 3, 1.5 km JCMT, CSO P.O.Box

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SMA, ASTE ALMA e-mail: takakuwa@asiaa.sinica.edu.tw 10617 P.O.Box 23 141 1 SMA, ASTE ALMA SMA, ALMA 1. 1.1 CO, CS, HCN 1 7 10 5 cm 3, 10 K, 3,000 5,000 1 1.

1 SMA, ASTE ALMA P.O.Box SMA, ASTE ALMA SMA, ALMA CO, CS, HCN cm 3, 10 K, 3,000 5, km 1) 3) 10 5 cm 3, 10 K ( 40 K) ( 10 7 cm 3 ) SMA ASTE JCMT, CSO

1 SMA ASTE 6m 8 SMA 4) 1 1999 3 SMA 4,100 m 2002 SMA NHK NHK SMA NHK SMA SMA SMA SMA 1.3 mm (230 GHz), 0.8 mm (345 GHz), 0.4 mm (690 GHz) 0.2 0.

2 1 SMA ASTE 6m 8 SMA 4) SMA 4,100 m 2002 SMA NHK NHK SMA NHK SMA SMA SMA SMA 1.3 mm (230 GHz), 0.8 mm (345 GHz), 0.4 mm (690 GHz) m 1 Atacama Submillimeter Telescope Experiment (ASTE) 1 ASTE 0.8 mm 22 4,800 m JCMT, CSO 2 ASTE JCMT, CSO SMA SMA ) ASTE SMA ASTE SMA SMA ASTE

3 1 2. SMA L1551 IRS5 CS (J 7 6) SMA, ASTE SMA 140 pc; 1 pc L1551 IRS5 L1551 IRS5 2,500 1), 6), 7) L1551 IRS ) L1551 IRS5 2 SMA CS (J 7 6; GHz) L1551 IRS5 5) 2 C 18 O(J 1 0; GHz) 2,500 7) K, 10 5 cm 3 ( 40 K) ( 10 7 cm 3 ) L1551 IRS5 2 SMA L1551 IRS5 CS (J 7 6) NMA C 18 O(J 1 0) (Momose et al., 1998) SMA P.A. 60 CS 1.9 K 0.75 K L1551 IRS5 CS (J 7 6) 0.2 km s 1 CS 1.9 K 0.75 K (1 K 0.63 Jy beam 1 ) m APEX

4 CS (J 7 6) C 18 O(J 1 0) 2 C 18 O (J 1 0) 1), 7) SMA SMA CSO L1551 IRS5 CS (J 7 6) 1 9) SMA CSO 11 SMA 400 1,500 ( 40 K) ( 10 7 cm 3 ) 1, ,500 10), 11) 3. SMA JCMT IRAS HCN (J 4 3) 1, pc IRAS SMA JCMT HCN (J 4 3; GHz) IRAS I I ) I ) 3 14) 3 JCMT I16293 HCN (J 4 3) 15 JCMT 3, SMA I16293 HCN (J 4 3) SMA

3 JCMT SMA IRAS 16293 2422 HCN (J 4 3) JCMT SMA JCMT 15 SMA 1.3 1.2 (P.A. 30 ) JCMT 4.

5 K km s 1 22.3 K km s 1 (1 K 0.16 Jy beam 1 ). 4 a b Source A

5 3 JCMT SMA IRAS HCN (J 4 3) JCMT SMA JCMT 15 SMA (P.A. 30 ) JCMT 4.76 K km s K km s 1 SMA 33.5 K km s K km s 1 JCMT SMA 2,600 SMA 33.5 K km s K km s 1 (1 K 0.16 Jy beam 1 ). 4 a b Source A (P.A. 74 ) SMA JCMT HCN 11.2 K 11.2 K Source A 3.6 km s 1 1 JCMT Source A 500 SMA JCMT

Source A L1551 IRS5 I16293 4 Source A a b HCN (J 4 3) 4 Source A 4 Source A 1 4.

6 Source A L1551 IRS5 I Source A a b HCN (J 4 3) 4 Source A 4 Source A 1 4. ASTE SMA, JCMT L1551 IRS5 I ASTE L483 HCN (J 4 3) CS (J 7 6) 2s, 4s, 6s 4s (1s K km s 1 ) 500 1,500 ASTE CS (J 7 6), HCN (J 4 3) 15) 5 ASTE 200 pc L483 HCN (J 4 3), CS (J 7 6) 3,000 L483 L1551 IRS5, I , 7 L483 B335 CS (J 7 6)

7 6 ASTE L483 CS (J 7 6) 5 2s 2s (1s K) ( 5.6 km s 1 ) 6, 7 L483 B335 L483 B335 16), 17) L483, B335 18), 19) L483, B SMA, ASTE

8 7 ASTE B335 CS (J 7 6) 2s, 4s, 6s, 4s (1s K km s 1 ) 2s 2s (1s K) ( 8.1 km s 1 ) 500 2,000 3,000 (L1551 IRS5) (I16293) I16293 L483, B335 ( 40 K) ( 10 7 cm 3 ) 2,000 3,000 10), 11)

9 20) 6. ALMA ASTE 22 SMA SMA JCMT I ASTE Atacama Large Millimeter and submillimeter Array (ALMA) ALMA 12 m m 4 7m m 12 m 7m 12 m Atacama Compact Array (ACA) ACA 12 m ALMA ALMA ALMA ALMA 30 SMA, ASTE, ALMA 5), 14), 15) Paul T. P. Ho 1) Ohashi N., Hayashi M., Ho P. T. P., Momose M., Hiran, N., 1996, ApJ 466, 957 2) Ohashi N., Hayashi M., Ho P. T. P., Momose M., 1997a, ApJ 475, 211 3) Ohashi N., Hayashi M., Ho P. T. P., Momose M., Tamura M., Hirano N., Sargent A. I., 1997b, ApJ 488,

10 4) Ho P. T. P., Moran J. M., Lo K. Y., 2004, ApJ 616, L1 5) Takakuwa S., Ohashi N., Ho P. T. P., Qi C., Wilner D. J., Zhang Q., Bourke T. L., Hirano N., Choi M., Yang J., 2004, ApJ 616, L15 6) Saito M., Kawabe R., Kitamura Y., Sunada K., 1996, ApJ 473, 464 7) Momose M., Ohashi N., Kawabe R., Nakano T., Hayashi M., 1998, ApJ 504, 314 8) Lim J., Takakuwa S., 2006, ApJ 653, 425 9) Moriarty-Schieven G. H., Wannier P. G., Mangum J. G., Tamura M., Olmsted, V. K., 1995, ApJ 455, ) Masunaga H., Miyama S. M., Inutsuka S., 1998, ApJ 495, ) Masunaga H., Inutsuka S., 2000, ApJ 531, ) Mundy L. G., Wootte, A., Wilking B. A., Blake G. A., Sargent A. I., 1992, ApJ, 385, ) Cazaux S., Tielens A., G G. M., Ceccarelli C., Castets A., Wakelam V., Caux E., Parise B., Teyssier D., 2003, ApJ 593, L51 14) Takakuwa S., Ohashi N., Bourke T. L., Hirano N., Ho P. T. P., Jorgensen J. K., Kuan Y.-J., Wilner D. J., Yeh S. C. C., 2007b, ApJ, 662, ) Takakuwa S., Kamazaki T., Saito M., Yamaguchi N., Kohno K., 2007a, PASJ 59, 1 16) Tafalla M., Myers P. C., Mardones D., Bachiller R., 2000, A&A 359, ) Hirano N., Kameya O., Kasuga T., Umemoto T., 1992, ApJ 390, L85 18) Myers P. C., Bachiller R., Caselli P., Fuller G. A., Mardones D., Tafalla M., Wilner D. J., 1995, ApJ 449, L65 19) Saito M., Sunada K., Kawabe R., Kitamura Y., Hirano N., 1999, ApJ 518, ) Nakazato T., Nakamoto T., Umemura M., 2003, ApJ 583, 322 Frontier of Submillimeter Astronomy SMA, ASTE, and ALMA Observations of Protostellar Envelopes in Submillimeter Molecular Lines Shigehisa TAKAKUWA Institute of Astronomy and Astrophysics, Academia Sinica, P.O. Box , Taipei 10617, Taiwan, R.O.C. Abstract: With the advent of new submillimeter instruments such as SMA, ASTE, and ALMA, we are now at the dawn of submillimeter astronomy. Our recent observations in submillimeter molecular lines with the SMA and ASTE have revealed new aspects of protostellar envelopes in the course of star formation. In particular, the distributions of submillimeter molecular lines are more extended ( 2,000 AU) than expected, and the velocity structures traced by submillimeter molecular lines are di#erent from those by millimeter molecular lines

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