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