Planetary Nebulae, PN PNe PN

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Sarolta Jónás
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1 2 2 masaaki@oao.nao.ac.jp Subaru Telescope, National Astronomical Observatory of Japan, 650 North A ohoku Place, Hilo, Hawaii 96720, U.S.A. tajitsu@subaru.naoj.org iso@kiso.ioa.s.u-tokyo.ac.jp Planetary Nebulae, PN PNe PN 2 3 PN PN 2 PN 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

2 1 HR PN (Pottasch, 1984, p. 214) 0.6 0.

2 2 1 HR PN (Pottasch, 1984, p. 214) NGC, IC 1,000 PNe 3) 4) 5) PN 2 NGC 7009 (Acker, et al., 1992) 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

2 1 PN 70 10 3 Manchado (2003) PN 65 (23.

3 2 1 PN 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 PN 2 3 PN 4 PN 2 A PN B 4 A PN PN B

4 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 HIDES 3 3. HIDES PN HIDES 1.88-m Position Angle, P.A. P.A. PN 5 3 P.A PI

5 2 P.A. 5 PN HIDES cm P.A. PN HIDES 6,000 6,800 AÕ 16, 4,300 5,100 AÕ 5 5 PN Tylenda 13) HIDES IC 2149 HST HST 4 5 [O III]l5007, [O I]l6300, Ha, [NII]l AÕ

6 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 IC 2149 HST IC ) P.A

7 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

8 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 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

9 2 Halo PN, H 4-1 IC 2149 PN 5. IC PN PN PN PN AGB PN PN Kinematical Age, PN Illinois James. B. Kaler Critical Reading

10 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, ) Bryce M., et al., 1994, MNRAS 266, ) Tylenda R., et al., 2003, A&A 405, ) Balick B., 1987, AJ 94, ) Otsuka M., et al., 2002, 16) Vázquez R., et al., 2002, ApJ 576, ) Bloecker T., 1995, A&A 299, ) Otsuka M., 2004, 19) Calvet N., Peimbert M., 1983, RMxAA 5, ) 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 Akito TAJITSU Subaru Telescope, National Astronomical Observatory of Japan, 650 North A ohoku Place, Hilo, Hawaii Mizuki ISOGAI Kiso Observatory, Institute of Astronomy, The University of Tokyo, Tarusawa, Mitake-mura, Kiso-gun, Nagano 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

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