Stellar Population Synthesis Including Planetary Nebulae
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Stellar Population SynthesisIncluding Planetary Nebulae
Paola Marigo Astronomy Department, Padova University, Italy
Lèo Girardi Trieste Observatory, INAF, Italy
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Why population synthesis of PNe?
Understand basic properties of PNe and their nucleie.g. M-R relation, line ratios, optical thickness/thinness,transition time, nuclear regime (H-burn. or He-burn.)
Analyse PNLFs in different galaxiese.g. depedence of the bright cut-off on SFR, IMF, Z(t)
Constrain progenitors’ AGB evolutione.g. superwind phase, Mi-Mf relation, nucleosynthesisand dredge-up
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Basic requirements: extended grids of PN models
Kahn (1983,1989)
Kahn & West (1985)
Volk & Kwok (1985)
Stasińska (1989)
Ciardullo et al. (1989)
Jacoby (1989)
Kahn & Breitschwerdt (1990)
Dopita et al. (1992)
Mendez et al. (1993)
Stanghellini (1995)
Mendez & Soffner (1997)
Stasińska et al. (1998)
Stanghellini & Renzini (2000)
Marigo et al. (2001; 2004)
Simplified approach still necessary. Various degrees of approximation: AGB evolution, nebular dynamics; photoionisation
Recent improvements of hydrodynamical calculations: large sets now becoming available
Perinotto et al. 2004
Schoenberner et al. 2005
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central star mass (Mi, Z) [p] AGB wind density and chemical comp. of the ejecta (r, t)
POST-AGB EVOLUTION logL-logTeff tracks (H-burn./He burn.) [p] fast wind
DYNAMICAL EVOLUTION OF THE NEBULA
IONISATION AND NEBULAR EMISSION LINES
photoionisation code [p] or other semi-empirical recipe [p]
(Mneb, Vexp) parametrisation .interacting-winds model [p]
Synthetic PN evolution:basic ingredients
AGB EVOLUTION
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Mi=1.7 M; MCS= 0.6 M; Z=0.019
Output of a synthetic PN model
Time evolution of:
• Ionised mass
• nebular radius
• expansion velocity
• optical configurations
• emission line luminosities
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Synthetic Samples of PNe
MONTE CARLO TECHNIQUE
SCHEME A) (Jacoby, Mendez, Stasinska, Stanghellini)
Randomly generate a synthetic PN sample obeying a given central-star mass N(Mc) distribution
Mi an age is randomly assigned in the [0, tPN] interval
Stellar and nebular parameters (L, Teff, Vexp, Mion, Rion, F) from grid-interpolations
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Synthetic Samples of PNe
N(Mi,Z) (Mi) (t – H) tPN
H(Mi,Z) Main Sequence lifetime
tPN PN lifetime «H
(Mi) Initial mass function
(t – H) Star formation rate
Z(t) Age-metallicity relation
SCHEME B) (Marigo et al. 2004)
Randomly generate a synthetic PN sample obeying a given initial mass N(Mi,Z) distribution
Mi an age is randomly assigned in the [0, tPN] interval
Stellar and nebular parameters (L, Teff, Vexp, Mion, Rion, F) from grid-interpolations
N(Mi)
Mi
MONTE CARLO TECHNIQUE
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Different synthetic schemes
Author Jacoby 89 Stasinska91 Mendez97 Stanghellini00 Marigo04 ————————————————————————————————————————————————
CS masses gaussian gaussian exponential+cut-off pop-synthesis pop-synthesis
PAGB tracks S83+WF86 S83 S83+B95 VW94 VW94
Dynamics (Mneb,Vneb) (Mneb,Vneb) interacting winds
Line fluxes phot. model phot. model analytic recipe phot. model
SFR constant +cut-off constant various choices
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Properties of PNe and their Central Stars
Mion-Rion relation
Nel-Rion relation
Line ratios
Optical thickness/thinness
Transition time
Nuclear burning regime
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How to explain the observed invariance of the bright cut-off ?
I. Jacoby (1996): narrow CSPN mass distribution (0.58 ± 0.02 M) over the age range (3-10 Gyr) , i.e. initial mass range (1-2 M)
II. Ciardullo & Jacoby (1999) : circumstellar extinction always estinguishes the overluminous and massive-progenitor PNe below the cut-off. III. Marigo et al. (2004): still open problem, difficult to recover for Ellipticals
IV. Ciardullo (2005): Possible contribution of PNe in binary systems
SO FAR NOT ROBUST THEORETICAL EXPLANATION
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WHICH PNe FORM THE CUT-OFF?
1. OIII 5007 LUMINOSITIES AS A FUNCTION OF AGE
Jacoby 1989
Stasińska et al. 1998
Marigo et al. 2004
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WHICH PNe FORM THE CUT-OFF?
2. CENTRAL MASS DISTRIBUTION AS A FUNCTION OF LIMITING MAGNITUDE
Marigo et al. 2004
MCSPN 0.70-0.75 M; Mi 2-3 M; age 0.5-1.0 Gyr
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DEPENDENCE ON THE AGE OF THE LAST EPISODE OF STAR FORMATION
Mmax=0.63Mmax=0.70Mmax=1.19
0.680.6950.77
Jacoby 1989
Mendez & Soffner 1997
Stanghellini 1995
Marigo et al. 2004
0.610.650.680.741.15
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A FEW CONCLUDING REMARKS
Population-age dependence of the PNLF: difficulty to explain the observed invariance of the bright cut-off in galaxies from late to early types
Still to be included: full hydrodynamics, non-sphericity, binary progenitors, etc.
Population synthesis including PNe is a powerful — still not fully exploited — tool to get insight into several aspects of PNe and their central stars e.g. ionised mass-radius rel.; electron density-radius rel.; [OIII]5007/HeII4686 anticorrel., Te distribution; [OIII]5007/H distribution; optical thickness/thinness; H-/He-burners, transition time; Mi-Mf relation; distribution of chemical abundances
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TRANSITION TIME
MOSTLY UNKNOWN PARAMETER: dependence on Menv, pulse phase, MLR, Mcs, etc.
Stanghellini & Renzini 2000
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DEPENDENCE OF THE PNLF ON TRANSITION TIME
(continued)
Stanghellini 1995 Marigo et al. 2004
Differences in the bright cut-off due to different ttr show up for larger Mmax, or equivalently for younger ages
Solid line: constat ttr; dashed line: mass -dependent ttr
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DEPENDENCE OF THE PNLF ON H-/He-BURNING TRACKS
Jacoby 1989 Marigo et al. 2004
H-burn.
He-burn.
Differences in the bright cut-off due to different tracks show up for older ages
The bright cut-off is reproduced by more massive H-burningCS (0.65 M) compared to He-burning CS (0.61 M)
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C-star LF Mi-Mf relation WD mass distr.
Renzini & Voli 1981
Marigo 1999
Van der Hoek & Groenewegen 1997
Synthetic AGB evolution: observational constraints
Marigo 2001
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Mostly used sets:
Schoenberner (1983) +Bloecker (1995)CS masses: 0.53 – 0.94 M
Metallicities: Z=0.021
Vassiliadis & Wood (1994) CS masses: 0.59 – 0.94 M
Metallicities: Z= 0.016, 0.008, 0.004, 0.001
Recent sets (synthetic):
Frankovsky (2003)CS masses : 0.56 – 0.94 M
Metallicities: Z= 0.016, 0.004
H-burning central stars
He-burning central stars
loops less luminous longer evolutionary timescales
Post-AGB evolutionary tracks
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PN DYNAMICS
(Kahn 1983; Volk & Kwok 1985; Breitschwerdt & Kahn 1990)
Interacting-winds model
Simple scheme Combination of constant parameters (Mneb, Vexp, R/R)
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NEBULAR FLUXES:photoionisation codes
INPUT • Nebular geometry• Rin, Rout• density N(H) • Elemental abundances (H,He,C,N,O,etc.)• L and Teff of the CSPN
Example: CLOUDY (Ferland 2001)Mi=2.0 M; MCSPN=0.685 M; Z=0.008; H-burn.; Mion=0.091 M; tPN=3000 yr
OUTPUT• Te (volume average)• ionisation fractions• line fluxes
Jacoby, Ciardullo et al.Stasinska et al.Marigo et al.
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OPTICAL PROPERTIES OF THE NEBULA
ABSORBING FACTOR (MKCJ93)
ABSORBED IONISING PHOTONS EMITTED IONISING PHOTONS
Mendez et al. : randomly assigned as a function of Teff, following results of model atmospheres applied to Galactic CSPN.
In particular, on heating tracks with T>40000 K a
random uniform distribution 0.05 max
Jacoby et al.
Stasinska et al. derives from the coupling between nebular dynamics and photoionisation Marigo et al.
Simulated PN sample:
M5007 < 1; Ntot = 500SFR=const.; Z=0.019; ttr=500 yrH-burn. and He-burn. tracks optically thick ; optically thin
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Ionised mass-radius relation
Observed data from Zhang (1995), Boffi & Stanghellini (1994)
Simulated PN sample:
M5007 < 1; Ntot = 500SFR=const.; Z=0.019; ttr=500 yrH-burn. and He-burn. tracks optically thick ; optically thin
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Electron density-radius relation
Observed data from Phillips (1998)
Simulated PN sample:
M5007 < 1; Ntot = 500SFR=const.; Z=0.019; ttr=500 yrH-burn. and He-burn. tracks optically thick ; optically thin
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Line ratios
Stasinska 1989
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NEBULAR FLUXES: a semi-empirical recipe
Mendez et al. : Once specified (L,Teff) of the CSPN
Recombination theory for optically thick case H fluxes
Random -factor correction true H fluxes
Empirical distribution I(5007)I(H) HOIII 5007 fluxes
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I([OIII]5007)/I(H) DISTRIBUTION of GALACTIC PNe
Observed (McKenna et al. 1996)
Predicted (He-burning tracks)
Predicted (He-burning tracks)