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

Correlation of PN morphology and nebular parameters

Arturo Manchado

Instituto de Astrofísica de Canarias

Colaborators

Eva VillaverSTSCI

Letizia StanghelliniSTSCI

Martín GuerreroInstituto 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 7009Guerrero, Gruendl, Chu 2002, A&A 387, L1

Elliptical

Interacting wind model with an ecuatorial density enhancement Frank, Balick, Icke, Mellema 1993, ApJ 404, L25Mellema 1995, "Asymmetrical PN", ed. Harpaz, p. 229

Jets & ansaeFrank, A., Balick, B., Livio, M. 1996 ApJ, 471, L53

Bipolar

Binaries, commom envelope phase, substellar interaction (Soker, 1997, ApJSS, 112, 487)

Magnetic fields  García-Segura et al. 1999 ApJ, 517, 767

Pointsymmetric

García-Segura, G. & López, J.A. 2000 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, L4920 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, 70

•108 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, 671

•41 Multiple shells Chu, Y. -H., Jacoby, G. H., & Arendt, R. 1987, ApJS 64, 529

•250 PNe; stellar (S), elliptical (E), bipolar (B), pointsymmetric (P), and irregular (I) Schwarz, H. E., Corradi, R. L. M., & Melnik J. 1992 A&AS 96, 23

•243 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 http://www.iac.es/nebula/nebula.html

•101 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, 417 35% show asymmetry

50 PNs with low-ionization structures (LISs), Goncalves, Corradi, Mampaso 2001, AJ 547, 302

56 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. 1984 Planetary Nebulae, ed. Reidel

•Evolutionary scheme: early, middle, late; round, elliptical, butterfly Balick , B. 1987, AJ 94, 671

•50 % of PNe are Multiple Shell Planetary NebulaeChu, 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 neonGiant dimensions

•Górny, S.K., Stasinska, G., & Tylenda, R. 1997, A&A 318, 256 (125 PNe)Bipolar: higher mass, smaller z, higher N/OPointsymmetric 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 %Round 29 %Bipolar 51 %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 statisticsSample 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, 671

•22 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 Systemhttp://adsabs.harvard.edu/

Chemical abundances

•Emission lines: Kaler, J.B., Shaw, R.A., Browning, L. 1997, PASP 109, 289Guerrero, M.A. 1995, PhD Thesis

•Plasma diagnostic + ionic chemical abundances nebular analysis package in IRAF/STSDAS (Shaw et al.1998)

•Helium abundancescollisional 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

<D>= 10 and 27.5 arcsec

a/b < 1 +0.06

Projected ellipsoid (c:1:1)

Observed ellipse

x= (c2(sin(i)2)+(cos(i))2)x a/bi inclination angle

On the projection effects

On the projection effects

1.2< c <1.5

P 7.3 %

N(elliptical)=149

11 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

<R>=638

<E>=276

<E+P>=259

<B>=56

<B+P>=135

<R>=0.102

< E>=0.121

<B>=0.136

<R>=0.27

<E>=0.31

<B>=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 temperatureHigher T for bipolar than for round + elliptical

N/OR=0.27, E=0.31, B=1.3 type I PNe for bipolartype II PNe for round and elliptical

Galactic latitude |b|round 12elliptical 7bipolar 3

He/H R=0.102, E=0.121, B=0.136type I PNe for bipolartype 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 310 M 1.0 M

elliptical 308 M 1.0 M

bipolar + pointsymmetric 248 M 1.2 M

bipolar 110 M 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 0.6584 microns

H2 S(1)(1-0) 2.1218 microns

IRAS 16594-4656