Planetary nebulae beyond the Milky Way - May , Magellanic Cloud planetary nebulae as probes of stellar evolution and populations Letizia Stanghellini

Planetary nebulae beyond the Milky Way - May 19-21, Magellanic Cloud PNe The known distances, low field reddening, relative proximity, and metallicity range make them  Absolute probes of post-AGB evolution  Benchmarks for extragalactic PN populations

Planetary nebulae beyond the Milky Way - May 19-21, Probes of post-AGB evolution Nebular analysis Morphology chemistry Links to central stars (CSs) Transition time Winds

Planetary nebulae beyond the Milky Way - May 19-21, Benchmarks for extragalactic PN populations PNe and UCHII regions Luminosity distribution and metallicity PNe types in the PNLF

Planetary nebulae beyond the Milky Way - May 19-21, PN morphology ·Depends on the formation and dynamic evolution of the PN, on the evolution of the central star and of the stellar progenitor, and on the environment. ·From Galactic PNe: ·Round, Elliptical, Bipolar [includes bipolar core and multipolar], and Point-symmetric ·Bipolar PNe are located in the Galactic plane, have high N, He, indication of massive CSs: remnant of 3-8 M stars?

6 Round PNe (R) are a minority (22 % of all Galactic PNe with studied morphology) 49% elliptical (E) 17% bipolar (or multi-polar) (B) 9% have an equatorial enhancement, or ring (lobe-less bipolar, or bipolar cores) (BC) 3% point-symmetric Symmetric | Asymmetric

7 HST and spatial resolution LMC SMP 10 HST STIS  arcsec   arcsec 

8 _4861 H  _4959 [O III]_5007 [O III] _6300 [O I] 6584 [N II]6563 H  6548 [N II] 6732 [S II]6716 [S II] Slitless Spectra of LMC SMP 16 G430M (4818 — 5104) and G750M (6295 — 6867)

9 Round Elliptical Bipolar Point-symmetric Galaxy LMC SMC Symmetric | Asymmetric

10 Morphological distribution LMCSMC Round R29 %35 % Elliptical E17 %29 % R+E (symm.)46 %64 % Bipolar B34 %6 % Bipolar core BC17 %24 % B+BC (asymm.)51 %30 % Point-symmetric3 %6 %

11 What is the physical origin of the equatorial disks? stellar rotation? Maybe associated with a strong magnetic field? Garcia-Segura 97 (single magnetic WD are more massive than non- magnetic WDs! Wickramasinge & Ferrario 2000) Binary evolution of the progenitor (CE)? Morris 81; Soker 98

Planetary nebulae beyond the Milky Way - May 19-21, Chemistry ·PNe enrich the ISM ·He, C, N, O abundances are linked to the evolution of the progenitors ·C-rich for massive progenitors (M ZAMS < 3 Msun) ·He- and N-rich (and C-poor) if M ZAMS > 3 Msun ·Ar, S, Ne are invariant during the evolution of stars in this mass range  they are signature of the protostellar ambient, thus test previous evolutionary history

13 Primordial elements, LMC O Round * Elliptical  Bipolar core Bipolar  LMC HII regions (average)

14 Primordial elements, LMC O Round * Elliptical  Bipolar core Bipolar  LMC HII regions (average)

15 LMC PN morphology and the products of stellar evolution O Round * Elliptical  Bipolar core Bipolar  LMC HII regions (average)

16 SMP16 SMP 95 SMP 34 Si IV N IV C IV] He II Decreasing excitation class --->

17 SMP16 SMP 95 SMP 34 C III ] C II] [Ne IV]

18 Optical AND UV morphology C III]1908 C II] 2327 [Ne IV] 2426 nebular continuum LMC SMP 95 Broad band [O III] 5007 [N II] H  [N II]

Planetary nebulae beyond the Milky Way - May 19-21, UV spectra fitting

Planetary nebulae beyond the Milky Way - May 19-21, P-Cygni profiles

21 Wind momentum vs. luminosity See poster by A. Arrieta

22 Transition time ·Transition time (t tr ) is measured from the envelope ejection quenching (EEQ) and the PN illumination; it is regulated by wind and/or nuclear evolution ·M e R (residual envelope mass at EEQ) determines t tr  dyn =D PN /v exp represent the dynamic PN age. If D PN is measured on main shell,  dyn tracks time from EEQ  dyn =t tr + t ev (t ev = time after PN illumination, corresponding to evolutionary time if tracks have zero point at illumination)

Planetary nebulae beyond the Milky Way - May 19-21, Dealing with unsynchronized clocks ·t tr is an essential parameter in post-AGB population synthesis (e.g., PNLF high luminosity cutoff, and UV contribution from post-AGB stars in galaxies) ·Mass-loss at TP-AGB and beyond not completely understood, and M e R now known ·Only way to constraint t tr is observationally · > Magellanic PNe offer the first direct estimates of transition time ·Assumptions: no acceleration of shells; He- tracks scaled to H-burning tracks

24  dyn and t ev LMC SMC Round: symm. PNe (R,E) Square: asymm. PNe (B,BC,P) H-burning central stars

25 Distribution of t tr in MC PNe

26 M e R =1e-3 M e R =2e-3 M e R =5e-3M e R =1e-2 Data LMC PNe SMC Pne Models t wind t nucl t tr

27 Total mass loss (IMFMR) Data: optically thin LMC and SMC PNe Hydro models: solid line =PN shells broken line=outer halos --> To constrain IMFMR we need to measure mass in PN halos (and in CSs)

Planetary nebulae beyond the Milky Way - May 19-21, Importance of spatially- resolved PN populations ·We sampled ~50 (+30) LMC and ~30 SMC PNe, chosen among the brightest known (based on on H  and [O III] 5007 fluxes ) ·All LMC PN candidates are indeed PNe ·~10% of the SMC PN candidates are H II regions

Planetary nebulae beyond the Milky Way - May 19-21, MA 1796MA 1797MG 2 Log F  C Size [arcsec] Size [pc]

30 Observed distributions of I(5007)/I(Hb) LMC SMC

31 Cloudy models Galaxy LMC SMC

32 Cloudy models, varying density SMC LMC Galaxy

33 SMC Galaxy LMC PN cooling in different galaxies Our HST data: LMC =9.4 (3.1) =5 (5) SMC =5.7 (2.5) UV: Cycle 13

34 PNe in the PNLF Open circles: R Asterisks: E Triangles: BC Squares: B Filled circles: P O round; * elliptical;  bipolar core; bipolar LMC SMC Faint > bright

35 CSs in PNLF LMC SMC Faint > bright SMC HLCO LMC HLCO

Planetary nebulae beyond the Milky Way - May 19-21, Summary, and the future HST fundamental for shapes/ radii, but also for identification (misclassified H II regions in SMC but not in LMC  metallicity effect?) Same morphology types in Galaxy, LMC, SMC, but more asymmetric PNe in LMC than SMC  different stellar generations? Asymmetric LMC PNe have high Ne, S, Ar--> signature of younger progenitors Similar UV and optical morphology

Planetary nebulae beyond the Milky Way - May 19-21, Summary, cont. Carbon higher for symmetric PNe, STIS UV spectra of LMC PNe to be analyzed; SMC PNe in Cycle 13 P-Cygni profiles as signature of CS winds, distance indicator for galactic PNe Transition time constrained from observation enlarge sample, hydro+stellar modeling IMFM relation constraints [O III]/H  flux ratio of a PN population variant with host galaxy

Planetary nebulae beyond the Milky Way - May 19-21, Symmetric PNe populate the high luminosity parts of the PNLF High mass CSs populate the faint end of the LF, sample to be extended Summary, cont. ·