2 2 e-mail: masaaki@oao.nao.ac.jp 719 0232 3037 5 Subaru Telescope, National Astronomical Observatory of Japan, 650 North A ohoku Place, Hilo, Hawaii 96720, U.S.A. e-mail: tajitsu@subaru.naoj.org 397 0101 10762 30 e-mail: iso@kiso.ioa.s.u-tokyo.ac.jp Planetary Nebulae, PN PNe PN 2 3 PN PN 2 PN 1. 1 8 HR AGB Asymptotic Giant Branch, Planetary Nebulae PN PNe 1 HR 1) PNe PNe 1782 Saturn Nebula NGC 7009 Acker 2) 2 1 PN NGC 7009 220 1 97 6 351
2 1 HR PN (Pottasch, 1984, p. 214) 0.6 0.8 NGC, IC 1,000 PNe 3) 4) 5) PN 2 NGC 7009 (Acker, et al., 1992). 3 3. 2. PN 2.1 PN PN Kwok 6) Interacting Stellar Wind (ISW) PN AGB km/s Post-AGB km/s km/s PN PN HST Hubble Space Telescope, PNe 352 2004 6
2 1 PN 70 10 3 Manchado (2003) PN 65 (23.2 ) 149 (53.2 ) 36 (12.8 ) 8(2.9 ) 7(2.5 ) 15 (5.4 ) PN 3 7) PN IC 418 NGC 3242 M2 9 PN NGC 6543 IC 2149 2.2 PN 2 3 PN 4 PN 2 A PN B 4 A PN PN B 2 97 6 353
2 Manchado 8) 280 PNe 7 1 PN PN 2.3 PNe km/s, PN Otsuka 9) Tajitsu Otsuka 10) Halo PN H4-1 Bachiller 11) Bryce 12) Ring Nebula, NGC 6720 (M 57) PN 2001 2 1 HIDES 3 3. HIDES PN HIDES 1.88-m Position Angle, P.A. P.A. PN 5 3 P.A. 3 2000 PI 2001 354 2004 6
2 P.A. 5 PN HIDES 4 10 15 cm 3 4 4 P.A. PN HIDES 6,000 6,800 AÕ 16, 4,300 5,100 AÕ 5 5 PN Tylenda 13) HIDES 4 90 5 6 IC 2149 HST HST 4 5 [O III]l5007, [O I]l6300, Ha, [NII]l6583 11 20AÕ 97 6 355
2 7 IC 2149 PV Map. P.A. 68 P.A. 331 PV Map [O III], Ha, [N II]). P.A. 331 [N II] 3 30 P.A. 331 [N II] (c) 15 (km/s) (arcsec) A C P.A. 331 [O III] (a) sub flow 1 sub flow 2 4. HIDES HIDES 2003 1 6 IC 2149 HST IC 2149 14) P.A. 68 5 356 2004 6
2 8 IC 2149 PV Map. P.A. 68 P.A. 331 PV Map [N II]/Ha, [OIII]/Ha). Ha P.A. 331 [O III]/Ha Map (d)) sub flow 97 6 357
2 2002 2 P.A. 331 [O III]l5007 [O III] Position-Velocity Map PV Map 15) [O III] 5 7 P.A. 68 P.A. 331 PV Map [O III] Ha [N II] l6583 [N II] P.A. P.A. 331 [O III] 7, 30 km/s sub flow 1 sub flow 2 Ha sub flows [O III]/Ha 8, [N II] P.A. PV Map 7, (P.A. 68 ), (P.A. 331 ) P.A. 68 Ring sub flows IC 2149 IC 2149 P.A. 68 (P.A. 331 ) PN IC 2149 Web 2003 11 Multiple Mirror Telescope Observatory 6.5-m IC 2149 P.A. 331 sub flows IC 2149 Halo PN Vazquez 16) Bloecker 17) 0.5 PN 18) ) PN ZAMS Zero Age Main Sequence, PN 19) ) Phillips 20) IC 2149 ZAMS PN 358 2004 6
2 Halo PN, H 4-1 IC 2149 PN 5. IC 2149 2 PN PN PN PN AGB PN PN Kinematical Age, PN Illinois James. B. Kaler Critical Reading 97 6 359
2 1) Pottasch S. R., 1984, Planetary Nebulae, Astrophysics and Space Science Library 2) Acker A., et al., 1992, Strasbourg-ESO catalogue of Galactic Planetary Nebulae, ESO publication 3) Ford H. C., Jacoby G. H., 1978, ApJS 38, 351 4) Jacoby G. H., 1983, IAUS 103, 427 5) Feldmeier J. J., et al., 1998, ApJ 503, 109 6) Kwok S., et al., 1978, ApJL 219, L125 7) Manchado A., et al., 2000, A.S.P. Conf. Ser. Vol. 199, 17 8) Manchado A., et al., 1996, The IAC Morphological Catalog of Northern Galactic Planetary Nebulae 9) Otsuka M., et al., 2003, PASP 115, 67 10) Tajitsu A., Otsuka M., 2004, in preparation 11) Bachiller R., et al., 1989, A&A 218, 252 12) Bryce M., et al., 1994, MNRAS 266, 721 13) Tylenda R., et al., 2003, A&A 405, 627 14) Balick B., 1987, AJ 94, 671 15) Otsuka M., et al., 2002, 16) Vázquez R., et al., 2002, ApJ 576, 860 17) Bloecker T., 1995, A&A 299, 755 18) Otsuka M., 2004, 19) Calvet N., Peimbert M., 1983, RMxAA 5, 319 20) Phillips J. P., 2001, MNRAS 326, 1041 High Dispersion Two-Dimensional Spectroscopy of Planetary Nebulae Masaaki OTSUKA Okayama Astrophysical Observatory, National Astronomical Observatory, Kamogata, Okayama 719 0232 Akito TAJITSU Subaru Telescope, National Astronomical Observatory of Japan, 650 North A ohoku Place, Hilo, Hawaii 96720 Mizuki ISOGAI Kiso Observatory, Institute of Astronomy, The University of Tokyo, Tarusawa, Mitake-mura, Kiso-gun, Nagano 397 0101 Abstract: Planetary Nebulae (PNe) are known as objects which are situated in the final evolutionary stage of the relatively less massive stars, and show various shapes. Classification of PN structure has been strongly dependent on direct two-dimensional images projected onto the sky. Such images are often insu$cient to fully understand the real three-dimensional structure of PNe. Since most of studies on PNe are involved in the morphology, it is important to recognize precisely their structure. It is essential to examine the velocity fields as the information along the line of sight in addition to the projected spatial information by images. Here, we show our recent results on a peculiar PN obtained by the high-dispersion twodimensional spectroscopy, which allowed a precise determination of its morphology as bipolar. 360 2004 6