3. 1936 T. Page letter in Nature
NGC 7027 & NGC 7662: Ar, Ne >> Earth
1939 Bowen & Wyse, Lick Obs. Bulletin
NGC 6572, NGC 7027, NGC 7662: ~solar composition
2006-2011 >300 refereed papers in ADS on PN
abundances: familiar elements,
heavier elements, s-process,
molecules, dust
4. bpc.edu
Péquignot & Baluteau (1994); Baluteau et al. (1995); Zhang, Dinerstein, Sterling et al.
(2001, 2008); Liu et al. (2005, 2007); Sharpee et al. (2007)
5. bpc.edu
* *
reflect progenitor’s ISM
*There is some evidence that nuclear processes can affect
these (Pequignot et al. 2000, Dinerstein et al. 2003; Herwig
2005, Wang & Liu 2008, Milingo et al. 2010 – more later)
6. bpc.edu
s-process
affected by star’s
nucleosynthesis http://en.wikipedia.org/wiki/en:Creative_Commons
7.
8. WIYN,NOAO,NSF
• get 1-D information @ medium
resolution; typically ≲150 lines
down to ~1% x Hb
for brighter objects can get deep
spectra w/high S/N; at right, in
NGC 7009 Fang & Liu (2011; poster
here) have identified 1170 features
down to ~0.01% x Hb
but, LSS fails to fully utilize the
potential of 2D detectors…
9. Milky Way: Kingsburgh & Barlow
Liu & colleagues
Maciel, Costa & colleagues
Milanova & Koltygin
Perinotto & colleagues
Juan Carlos Casado (TWAN) Stasińska & colleagues
Henry, Kwitter & colleagues
Magellanic Clouds:
Boroson & Liebert
Leisy & Dennefeld
Maciel, Costa & colleagues
Dopita & colleagues
Stanghellini, Shaw et al.
Fred Espenak
Vasiliadis & colleagues.
10. exploits 2D detectors with serious multiplexing
Tsamis & collaborators; Sandin & collaborators
Te
NGC 5882
Hb
Tsamis et al. 2008
IC 3568
He II
Sandin et al. 2008
[O III] 4686
4959 NGC 7662, center
c
FLAMES/Giraffe Argus, VLT PMAS, Calar Alto
11. Spitzer/JPL M1-42 (Pottasch et al. 2007)
• Spitzer IRS provided high-
quality spectra covering
important ions of e.g., Ne,
O, S, Ar (& Fe, Si, Mg)
• Need for ICFs is reduced
• Fine-structure lines have
small T-dependence
Pottasch, Bernard-Salas & collaborators
Stanghellini, Shaw & collaborators
Guzman-Ramirez & collaborators
12. HST/STIS
TS-01
• prominent ions of He, C, N, O
[C IV] He II
Stasińska et al. 2010
• avoids usually large ICF(N) [N V]
STIS
• at right, TS01, the most O-poor PN [N IV]
known (O/H~1/70 x solar)
• IUE quality superseded by HST COS
& STIS; as yet, small database
HST/STIS Cy19 : Dufour et al. – 10 MW PNe
Guerrero et al. – NGC 6543
13.
14. • correct reduced slit fluxes for reddening
• calculate Te, Ne, X+i/H+ N-level atom codes
• calculate ICF’s per some recipe or model*
to derive X/H:
total X abundance
ICF(X) =
sum of observable X ions
*unless you have all relevant ionization stages
15. • correct reduced slit fluxes for reddening
- Whitford 1958
- Miller & Mathews 1972
- Savage & Mathis 1979
- Seaton 1979 fl
- Howarth 1983
- Fitzpatrick 1999
- Clayton, Cardelli & Mathis 1989
An example:
For c=1, the corrected ratio of
[O II] I3727/I7323 obtained using
CCM vs. SM differs by ~15%, leading to ~1000K difference in the
derived T[O II]…
16. • calculate: Te , Ne , X+i/H+
Il(X+i)/I(Hb) Te , Ne ,
Abundance Software
N(X+i)/N(H+)
Il (X i ) N(X i )
f (Te ,N e ) C
I(Hb) N(H )
17. on the ground… poster by
Wesson;
talk by
Luridiana
N/H
…in NGC 6543, the
systematic uncertainty
introduced by the choice
of atomic data is
comparable to or larger
than the statistical T[S II]
uncertainties for some
temperatures, densities
and abundances.
R. Wesson (private communication)
…not a stationary target
18. talk by
Gonçalves
•calculate ionization correction factors (ICFs)
per a recipe or model* to derive X/H
*unless you have observed all relevant ionization stages
ICFs best determined using photoionization
models; otherwise, exploit IP coincidences
• Kingsburgh & Barlow (1994): developed a good set
still used by many
• Henry & Ferland are currently running sets of
CLOUDY models to evaluate ICFs under a wide
range of stellar T*, Ne, and Z.
… so at each step we have an opportunity for
divergence, independent of measured fluxes!
19. posters by
Peimberts;
Fierro et al.;
McNabb et al.;
ADF=(X/H)ORL/(X/H)CEL R.-Garcia & Peña
recent summary by Peña (2011); Bob Rubin’s talk yesterday
(Liu & colleagues) (Peimbert, Torres-Peimbert & colleagues)
• Yuan et al. (2011): NGC 6153 - 3D bi- • Georgiev et al. (2008): NGC 6543
abundance model with 800K NLTE star and wind model agrees
inclusions best reproduces observed with ORL values for He, C, O (but
spectrum not N)
• Zhang (2008): NGC 7009 - high • García-Rojas et al. (2009): observed
resolution line profiles suggest ORLs, several PNe with WC central stars;
CELs may originate in kinematically t2 ~0.04; no evidence of cool, C-rich
different regions inclusions, even when the central
stars are H-deficient
• Williams et al. (2008): UV absorption
abundances in 3 PNe agree better
with CEL than ORL abundances
This is becoming testable, and will eventually be sorted out…
20. : 1D photoionization code (Stasińska 2005)
: 1D photoionization code (Ferland et al. 1998)
: 1D photoionization/shock code (Kewley 2001)
: 1D photoionization code (Rubin et al. 1994)
: Pseudo-3D photoionization code (Morriset 2005)
: fully 3D Monte Carlo photoionization code
(Ercolano et al. 2003)
: 1-D RHD code (Perinotto et al. 1998) – poster by Jacob
21.
22. different He+
recomb coeff
all abundances are
medians; error bars
show characteristic
uncertainties
X
X
23. DISK BULGE & HALO
• good agreement
within uncertainties
• O, Ne, Ar ≈ solar
N,C > solar
S < solar
26. log(N/H) vs. log(He/H)
log(N/O) vs. He/H
Maciel et al. 2010
+: SMC •: LMC •: MW
models: Karakas & Lattanzio 2007, 1-6
M
similar behavior in all 3
galaxies implies similar
origin of N, He
HKB04 all recalculated, Karakas (2009): 1-6 M
good T & N determinations
Marigo (2001): 0.8-5 M
27.
28. • LMC PNe show
negative trend,
HBB
• Type I MWPNe
may also
• SMC PNe do not
no HBB
29. Ne vs. O Maciel et al. 2010
+ SMC LMC MW
Maciel et al.: no correlation between
Ne/O and O over >2 dex in O/H
• Wang & Liu (2008): Ne, O production only at 12+log(O/H) < 8 (<ZSMC)
• Milingo et al. (2010): some evidence for Ne production, based on on
comparison with H II regions; no difference between Type I and Type II PNe
• Peimbert et al. (1992); Peña et al. (this meeting): argue that the ICF for Ne
(Ne/O=Ne++/O++) is inadequate at low ionization typically found in H II regions
lower limits, offering an explanation for Milingo et al.’s finding
30. posters by
Henry et al.
Jacob et al.
Ar follows H II region Sulfur stinks!
trend, but with larger Karakas: 1-6 M
scatter than Ne…
31. MW disk PNe – Maciel & Costa (2011) LMC/SMC – Stanghellini et al. (2009)
Aasymm,symm - Aall filled: SMC
open: LMC
• Average He and N are higher for asymmetric PNe than for
symmetric PNe
• The opposite is true for C.
• Higher O, Ne, S, Ar in asymmetric PNe younger progenitors
• SMC PNe tend to be C-rich, implying no HBB
32. talk by
Karakas;
poster by
Sterling et al.
• Sharpee et al. (2007) detected lines of Br, Kr,
Se
Xe, Rb, Ba, and Pb; Te & I (?); Kr, Xe
enhanced
• Sterling & Dinerstein (2008), detected Kr &/or
Se in 81 of 120 PNe:
- Non-Type I: [Se/(O)]ave= +0.36
[Kr/(O)]ave = +1.02
Kr significantly enhanced Kr
- Type I PNe show little s-process enrichment
- Positive correlation between s-process
enrichments and C/O, as expected in TDU
- No significant difference with central star type
• Future progress relies heavily on knowing
transition rates and collision strengths
33. poster by
Delgado
Inglada et al.
• Delgado Inglada et al. (2009): 33 low-ionization PNe
• median 12+log(Fe/H) = 5.85 (4.27 – 6.49)
• depletion range [Fe/H]: -1.01 to -3.2 (=7.50; Asplund et al. 2009)
- Fe > 90% depleted
- Mdust/Mgas ≥ 1.3 x 10-3
- depletion scales with C/O ratio (poster)
See also: Rodriguez & Rubin (2005); Stasińska & Szczerba (1999)
34.
35. • He, C, N, O, Ne, S, Ar, Fe, s-process abundances have been
determined in 10’s -100’s of PNe in the MW and MC’s.
• IR & UV observations have provided some improved results.
• Significant disparities result from different analysis choices.
• O, Ne, and Ar are positively correlated with each other, as
expected. S is problematic. In general, scatterPNe > scatterH2BCG.
• C, N generally exceed solar, consistent with current LIMS model
predictions including TDU; low-C PNe in the Milky Way & LMC
show evidence of HBB.
• Models cover the parameter space of observed abundances
• s-process elements can be significantly enhanced above solar in
non-Type I PNe.
• Fe is significantly depleted in PNe
36. (aside from big ground & space telescopes & good spectrographs)
• atomic data for more atoms, wider regimes
- “normal data” for heavy atoms (Sterling poster)
- low-T parameters for light atoms (Fang poster)
• improved ICFs (metallicity; ionization; geometry)
• more 2D abundance studies/3D modeling
• abundance discrepancy resolution
• coordination/testing among 5-LA programs
• understanding the effect of binarity on observed
abundances in CE scenario
• development of a “strong-line method” when direct
Te measurement not possible
37. Collaborators:
Dick Henry
Bruce Balick
Reggie Dufour
Gary Ferland
Jacquelynne Milingo
Dick Shaw
Students: Funding Sources:
Jesse Levitt ’08 NSF
Matt Johnson ’07 NASA
Peter O’Malley ’07 U. Oklahoma
Julie Skinner ’07 Williams College
Anne Jaskot ’08
Emma Lehman ’10
Tim Miller (‘G OU)
