J/ApJ/711/619 α-element abundances in galactic PNe (Milingo+, 2010)
Alpha element abundances in a large sample of Galactic planetary nebulae.
Milingo J.B., Kwitter K.B., Henry R.B.C., Souza S.P.
<Astrophys. J., 711, 619-630 (2010)>
=2010ApJ...711..619M 2010ApJ...711..619M
ADC_Keywords: Abundances ; Planetary nebulae ; Spectroscopy ; Milky Way
Keywords: ISM: abundances - nuclear reactions, nucleosynthesis, abundances -
planetary nebulae: general - stars: evolution
Abstract:
In this paper, we present emission line strengths, abundances, and
element ratios (X/O for Ne, S, Cl, and Ar) for a sample of 38 Galactic
disk planetary nebulae (PNe) consisting primarily of Peimbert
classification Type I. Spectrophotometry for these PNe incorporates an
extended optical/near-IR range of 3600-9600Å including the [SIII]
lines at 9069Å and 9532Å, setting this relatively large sample
apart from typical spectral coverage. We have utilized Emission Line
Spectrum Analyzer, a five-level atom abundance routine, to determine
Te, Ne, ionization correction factors, and total element abundances,
thereby continuing our work toward a uniformly processed set of data.
With a compilation of data from >120 Milky Way PNe, we present results
from our most recent analysis of abundance patterns in Galactic disk
PNe. With a wide range of metallicities, galactocentric distances, and
both Type I and non-Type I objects, we have examined the alpha
elements against HII regions and blue compact galaxies (H2BCGs) to
discern signatures of depletion or enhancement in PNe progenitor
stars, particularly the destruction or production of O and Ne.
Description:
We have acquired spectra for 38 Galactic disk PNe with coverage that
extends from 3600Å to 9600Å. Using the same instrumentation and
setup as our previous Type II PNe program (Milingo et al.
2002ApJS..138..279M 2002ApJS..138..279M), observations were obtained over a total of four
runs; Kitt Peak National Observatory (KPNO) in 2003 June & 2004
August, and Cerro Tololo Inter-American Observatory (CTIO) in 2003
November & 2004 August.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
pne.dat 24 38 Extinction measures and Hβ flux for each PN
table2.dat 80 3776 Fluxes and intensities
table3.dat 58 266 Temperatures and densities
table4.dat 47 1692 Ionic abundances
table5.dat 48 456 Total elemental abundances
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See also:
J/A+A/500/1089 : Abundances in planetary nebulae (Gorny+, 2009)
J/A+A/494/591 : Abundances in planetary nebulae (Chiappini+, 2009)
J/PAZh/35/574 : He, C, N and O abundances in planetary nebulae (Milanova+,
2009)
J/AZh/82/437 : Calculated chemical composition of galactic PN (Holovatyy+,
2005)
J/MNRAS/349/793 : Galactic PNe abundances (Perinotto+, 2004)
J/A+A/427/231 : Abundances in planetary nebulae (Gorny+, 2004)
J/A+A/423/199 : Chemical abundances of planetary nebulae (Costa+, 2004)
J/A+A/380/300 : Abundances of PN towards Galactic bulge (Escudero+, 2001)
J/A+A/345/629 : Abundance gradients in planetary nebulae (Maciel+, 1999)
J/A+AS/126/297 : PN abundances (Ratag+ 1997)
J/A+A/280/581 : Chemical abundances of PNe (Pasquali+, 1993)
Byte-by-byte Description of file: pne.dat
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Bytes Format Units Label Explanations
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1- 7 A7 --- Name PN name
9- 12 F4.2 --- c Extinction measure (G1)
14- 17 F4.2 --- Ha/Hb Final converged Hα/Hβ line ratio
19- 24 F6.2 [mW/m2] log(FHb) Log of the observed Hβ flux in units
of erg/s/cm2
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 7 A7 --- Name Planetary nebula identification
9- 25 A17 --- LineID Line identification
27- 34 A8 --- --- [λ]
35- 38 I4 0.1nm lambda Wavelength (Å)
40 A1 --- n_lambda [a] deblended line
42- 47 F6.3 --- f(lam) Reddening function (G1)
49- 56 E8.2 --- F(lam) ? Raw, uncorrected line flux (3)
57- 59 A3 --- f_F(lam) Uncertainty flag on F(lam) (4)
61- 68 E8.2 --- I(lam) ? Dereddened line flux (3)
70- 77 E8.2 --- e_I(lam) ? Uncertainty in I(lam) (3)
78- 80 A3 --- u_I(lam) Uncertainty flag on I(lam) (4)
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Note (3): Scaled to Hβ=100. See pne.dat file for Hβ values.
Note (4): Intensities of strong lines have measurement uncertainties of
≤10%, single colons indicate uncertainties of ≳25%, double
colons indicate uncertainties ≳50%, and triple colons indicate
highly suspect measurements.
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 7 A7 --- Name Planetary nebula identification
10- 22 A13 --- Param Parameter (1)
24- 28 I5 --- Value ? Parameter value (2)
30- 34 I5 --- e_Value ? Uncertainty in Value
36- 58 A23 --- n_Value Note on Value (3)
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Note (1): The parameters are electron temperatures (T, in K) and
densities (N, in cm-3); lines used:
* 5007, 4363 for T[OIII];
* 6584, 5755 for T[NII];
* 3727, 7324 for T[OII];
* 6716, 6731, 4071 for T[SII];
* 9532, 9069, 6312 for T[SIII];
* 6716, 6731 for Ne,[SII];
* 5518, 5538 for Ne,[ClIII].
Note (2): Temperatures and densities given in Kelvin and cm-3.
Note (3): If either 5755 or 6584 is unavailable T[NII] is estimated from
T[OIII] Kwitter & Henry (2001ApJ...562..804K 2001ApJ...562..804K). Given telluric
effects when calculating T[SIII] if the ratio of 9532/9069 is
≥2.48 then 9532 is used as the nebular transition, if the 9532/9069
ratio is less than 2.48 then 9069 is used. Default T[NII] and
Ne,[ClIII] values and the high density limit for Ne,[SII] are
based on criteria discussed in Kwitter & Henry (2001ApJ...562..804K 2001ApJ...562..804K).
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 7 A7 --- Name Planetary nebula identification
9- 20 A12 --- Ion Ion or icf (ionization correction factors)
22- 28 A7 --- Tmeth Method used to determine the temperature (1)
30 A1 --- f_Abd [*] Indicates Abd included in weighted mean
31- 38 E8.2 [-] Abd ? Derived ionic abundance or icf
40- 47 E8.2 [-] e_Abd ? Uncertainty in Abd
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Note (1): ion used for the computation of the temperature;
wm = calculated mean value for the ionic abundance weighted by the
observed flux.
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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1- 7 A7 --- Name Planetary nebula identification
9- 12 A4 --- Ratio Ions concerned
14- 21 E8.2 [-] Abd ? Abundance ratio (1)
23- 30 E8.2 [-] e_Abd ? Uncertainty in Abd (1)
32- 39 E8.2 [-] Solar Asplund et al., 2005ASPC..336...25A 2005ASPC..336...25A, solar
abundance ratio (1)
41- 48 E8.2 [-] Orion Esteban et al., 1998MNRAS.295..401E 1998MNRAS.295..401E, Orion
abundance ratio (1)
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Note (1): All abundances are of the form N(X).
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Global Notes:
Note (G1): Final dereddened intensity ratios are calculated as:
I(λ)/I(Hβ)=F(λ)/F(Hβ)x10cf(λ)
where I(λ)/I(Hβ) is the final intensity ratio of an
emission line to Hβ, F(λ)/F(Hβ) is the observed flux
ratio of the line to Hβ, c is the extinction measure, and
f(λ) is the reddening function. See section 3 for further details.
History:
From electronic version of the journal
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 04-Apr-2012