Correlation of PN morphology and nebular parameters Arturo Manchado Instituto de Astrofísica de Canarias

Colaborators Eva Villaver STSCI Letizia Stanghellini STSCI Martín Guerrero Instituto de Astrofísica de Andalucía

PNe morphology vs. stellar evolution An AGB star can lose up to 80% of its mass Round Interacting wind model: The PN is formed by the interaction of a low density fast wind with a high density slow wind (e.g Kwok, Purton & Fitzgerald 1978, ApJ 219, 17) First observational evidence hot bubble in NGC 7009 Guerrero, Gruendl, Chu 2002, A&A 387, L1 Elliptical Interacting wind model with an ecuatorial density enhancement Frank, Balick, Icke, Mellema 1993, ApJ 404, L25 Mellema 1995, "Asymmetrical PN", ed. Harpaz, p. 229

Jets & ansae Frank, A., Balick, B., Livio, M ApJ, 471, L53 Bipolar Binaries, commom envelope phase, substellar interaction (Soker, 1997, ApJSS, 112, 487) Magnetic fields García-Segura et al ApJ, 517, 767 Pointsymmetric García-Segura, G. & López, J.A ApJ, 544, 336 Muliple Shell PNe Villaver, Manchado, García-Segura, 2002 ApJ, 581, 1204 Steffen, M.; Schönberner, D. 2000A&A, 357, 180

Interaction with the Insterstellar Medium Villaver, García-Segura, Manchado,2003 ApJ, 585, L49 20 km/s causes asymmetry due to interaction with the IM Morphology of PPNe Ueta, Meixner, Bobrowsky 2000 AJ, 528, 861 sole - round, elliptical duplex - bipolar Review on Shapes and Saphing of Planetary Nebulae Balick, Frank 2002, Annu. Rev. Astron. Astrophys. 40, 439

On the Morphology Extended halos Curtis, H.D. 1918, Pub. Lick Obs. 13, 57 "binebulous" and circular nebula Greig, W. E., 1972, A&A 18, of non-stellar PNe bipolar, round, disk-like, and annular Zuckerman, B., & Aller, L. H. 1986, ApJ 301, 772 Round, elliptical and butterfly Balick, B. 1987, AJ 94, Multiple shells Chu, Y. -H., Jacoby, G. H., & Arendt, R. 1987, ApJS 64, PNe; stellar (S), elliptical (E), bipolar (B), pointsymmetric (P), and irregular (I) Schwarz, H. E., Corradi, R. L. M., & Melnik J A&AS 96, PNe; round(R), bipolar(B), elliptical(E),quadrupolar(Q), pointsymmetric (P) Manchado, A., Guerrero, M.A., Stanghellini, L., & Serra-Ricart, M. 1996, The IAC Morphological Catalog of Northern Galactic PN, ed. IAC PNe Górny, S.K., Schwarz, H.E., Corradi, R.L.M., Winckel, H. van, 1999, A&AS 136, 145

On the Morphology 50 MSPN, Corradi, Schoenberner, Steffen, Perinotto 2003, Mon. Not. R. Astron. Soc. 340, % show asymmetry 50 PNs with low-ionization structures (LISs), Goncalves, Corradi, Mampaso 2001, AJ 547, PNs Large Magellanic Cloud Stanghellini, Blades, Osmern Barlow, Liu, 1999 AJ, 510,687 Shaw, Stanghellini, Mutchler, Balick, Blades, 2001, 548, 727

On the structural classification Projection effects Pottasch, S.R Planetary Nebulae, ed. Reidel Evolutionary scheme: early, middle, late; round, elliptical, butterfly Balick, B. 1987, AJ 94, % of PNe are Multiple Shell Planetary Nebulae Chu, Y. -H., Jacoby, G. H., & Arendt, R. 1987, ApJS 64, 529 Central star mass distribution different for bipolar and elliptical. Elliptical are younger and more luminous than MPSN Stanghellini, L., Corradi, R. L. M, & Schwarz, H. E, 1993 A&A 279, 521

Classification scheme Balick, B. 1987, AJ 94, 671

Corradi, R. L. M, & Schwarz, H. E. 1995, A&A 293, 871 (250 PNe) Elliptical z = 320 M < 1.1 M  Bipolar z = 130 M > 1.5 M  Overabundance helium, nitrogen and neon Giant dimensions Górny, S.K., Stasinska, G., & Tylenda, R. 1997, A&A 318, 256 (125 PNe) Bipolar: higher mass, smaller z, higher N/O Pointsymmetric a separate class Elliptical z = 680 Mean Central Star mass 0.61 M  Bipolar z = 360 Mean Central Star mass 0.68 M  Pointsymmetric z = 800 Mean Central Star mass 0.59 M  Shaw,R.A, Stanghellini,L.,Mutchler,M.,Balick,B.,Blades,J.C. 2000, ApJ, 548, 727 (29 PNe) Elliptical 17 % Round29 % Bipolar51 % Pointsymmetric 3 %

Stanghellini, Manchado, Villaver, Guerrero 2002, AJ 576, 285 Different mass ranges for Round, Elliptical and Bipolar PNs Soker 2002, A&A 386, 885 Spherical PN low metalicity 70% are further away from the galactic center than the sun is from the galactic center.

Górny, S.K., Stasinska, G., & Tylenda, R. 1997, A&A 318, 256

On the statistics Sample selection Complete sample (255 PNe) All PNe larger than 4 arcseconds in Acker´s catalog (1992). All northern PNe (  >  11) H , [N II], [O III] images 213 PNe from: Manchado, A., Guerrero, M.A., Stanghellini, L., & Serra- Ricart, M. 1996, The IAC Morphological Catalog of Northern Galactic PN ed. IAC 20 PNe from Balick, B. 1987, AJ 94, PNe from Schwarz, H. E., Corradi, R. L. M., & Melnik J. 1992, A&AS 96, 23

Database Statistical distances: Cahn, J.H., Kaler, J.B., Stanghellini, L. 1992, A&AS 94, 399 NASA Astrophysics Data System

Chemical abundances Emission lines: Kaler, J.B., Shaw, R.A., Browning, L. 1997, PASP 109, 289 Guerrero, M.A. 1995, PhD Thesis Plasma diagnostic + ionic chemical abundances nebular analysis package in IRAF/STSDAS (Shaw et al.1998) Helium abundances collisional effects Clegg (1987)

Abell 39

Abell 50

NGC 2438

Abell 72

NGC 1501

IC 1295

NGC 6853

He 2-429

NGC 650

K 4-55

He 2-437

M 3-28

On the projection effects Round classification = 10 and 27.5 arcsec a/b < Projected ellipsoid (c:1:1) Observed ellipse x=  (c 2  (sin(i) 2 )+(cos(i)) 2 ) x  a/b i inclination angle

On the projection effects

1.2< c <1.5 P  7.3 % N(elliptical)= elliptical seen as round N(round)=63 17 % of round could be elliptical 40 % of MSPN are asymmetrical

d < 6.5 Kpc

Morphological classes whole sample E=58 %,R=25 %, B=17 % Taking into account projection effect E=63 %, R=20 %, B=17 % d < 6.5 Kpc E=62 %, R=26 %, B=12 % Taking into account projection effect E=66 %, R=22 %, B=12 %

d < 6 Kpc

Round, Bipolar, Elliptical

=638 =276 =259 =56 =135

=0.102 =0.121 =0.136

=0.27 =0.31 =1.3

Conclusions Sample complete up to 6.5 Kpc - 66 % elliptical - 22 % round - 12 % bipolar -46 % of round are MSPN -35 % of elliptical are MSPN -40 % of MSPN are asymmetrical Central star temperature Higher T for bipolar than for round + elliptical

N/O R=0.27, E=0.31, B=1.3 type I PNe for bipolar type II PNe for round and elliptical Galactic latitude |b| round 12 elliptical 7 bipolar 3 He/H R=0.102, E=0.121, B=0.136 type I PNe for bipolar type II PNe for round and elliptical

Galactic height  z  round 753 elliptical 308 M 1.0 M  bipolar 179 M 1.5 M  elliptical + pointsymmetric 310M 1.0 M  elliptical 308M 1.0 M  bipolar + pointsymmetric 248 M 1.2 M  bipolar 110M 1.9 M  Different progenitor masses for round, elliptical, bipolar and bipolar + pointsymetric Higher mass for the central stars of bipolar Two different mass distribution on the formation of bipolar PNe (García-Segura et al. 2000, RevMexAA) Single high mass stars will form bipolar PNe due to rotation Binary systems will form bipolar + poitsymmetric PNe

Future work Complete the data set: Abundances, expansion velocities, central star parameters Extend the study to the other galaxies (LMC) Extend the study to molecular gas (near-IR+ALMA) and dust (medium-IR)

NGC 2346 HST+WFPC2+N II microns H2 S(1)(1-0) microns

IRAS