J/PASJ/59/1127 Abundances in 5 post-AGB candidates (Takeda+, 2007)
Abundances of volatile elements in post-AGB candidates.
Takeda Y., Taguchi H., Yoshioka K., Hashimoto O., Aikawa T., Kawanomoto S.
<Publ. Astron. Soc. Jap., 59, 1127-1140 (2007)>
=2007PASJ...59.1127T 2007PASJ...59.1127T
ADC_Keywords: Stars, supergiant ; Abundances
Keywords: stars: abundances - stars: AGB and post-AGB - stars: atmospheres -
stars: evolution - stars: individual (HD 112374, HD 148743, HD 161796,
HD 163506, HD 187203)
Abstract:
A detailed non-LTE study on the abundances of C, N, O, S, and Zn was
carried out for five F-G supergiants of suspected post-AGB candidates
with IR excesses (HD 112374, HD 148743, HD 161796, HD 163506, and HD
187203), since these volatile elements can provide the key to
inferring the original metallicity as well as an evolution-induced
change due to mixing, given that they are free from depletion caused
by dust-gas separation.
Description:
The observations were carried out on 2005 April 15-21, by using the
HIgh-Dispersion Echelle Spectrograph (HIDES) at the coude focus of the
188cm reflector of Okayama Astrophysical Observatory (OAO).
Objects:
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RA (2000) DE Designation(s)
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12 56 30.1 -26 27 37 HD 112374 = V* LN Hya
16 30 30.0 -07 30 52 HD 148743 = BD-07 4305
17 44 55.5 +50 02 39 HD 161796 = V* V814 Her
17 55 25.2 +26 03 00 HD 163506 = * 89 Her
19 48 30.5 +10 41 39 HD 187203 = BD+10 4058
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 53 665 Line data and equivalent widths of Fe lines along
with the resulting abundances corresponding to
the final atmospheric parameters
table4.dat 60 45 Adopted atomic data of spectral lines
table5.dat 37 150 Line-by-line equivalent widths, abundances,
and non-LTE corrections
table6.dat 79 25 Averaged abundances and sensitivities to
atmospheric parameters
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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- 2 A2 --- --- [HD]
4- 9 I6 --- HD Star HD number
11- 14 I4 --- No Number
16- 20 F5.2 --- Ion Ion code
22- 29 F8.3 0.1nm lambda Line wavelength
31- 35 F5.3 eV EP Excitation potential
37- 42 F6.3 --- loggf Oscillator strength
44- 48 F5.1 0.1pm EW ?=- Equivalent width
50- 53 F4.2 ---- Abund ?=- Abundance (AH=12)
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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- 4 A4 --- Region Region (1)
6- 8 A3 -- Ion Ion designation (1)
10- 14 A5 --- RMT Multiplet number (1)
16- 19 I4 0.1nm Line ? Line (1)
21- 28 F8.3 0.1nm lambda Wavelength (1)
30- 34 F5.2 eV EP ? Excitation potential (1)
36- 40 F5.2 --- loggf Oscillator strength (1)
42- 45 F4.2 [-] Gammar ? Radiation damping constant (log(gammared))
46 A1 --- n_Gammar [*] Note (2)
48- 52 F5.2 [-] Gammas ? Stark damping width per electron density
at 104K, log(gammae/Ne)
53 A1 --- n_Gammas [*] Note (2)
55- 59 F5.2 [-] Gammaw ? van der Waals damping width per hydrogen
density at 104K, log(gammaw/NH)
60 A1 --- n_Gammaw [*] Note (2)
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Note (1): All data except for the loggf values of CI 7111-9 lines
(empirically adjusted solar loggf values) were taken from Kurucz
and Bell's (1995, Kurucz CD-ROM, No. 23) compilation.
Note (2): * : Computed as default values in the Kurucz's WIDTH program
(cf. Leushin & Topil'skaya 1987, Ap, 25, 415).
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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- 2 A2 --- --- [HD]
4- 9 I6 --- HD Star HD number
11- 14 A4 --- Region Region
16- 19 I4 0.1nm Line Line
21- 25 F5.1 0.1pm EW ?=- Equivalent width
27- 30 F4.2 --- Abund ?=- Abundance
31 A1 --- n_Abund [)] Note (1)
33- 37 F5.2 --- DN ?=- Non-LTE correction
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Note (1): Parenthesis for abundances (those from CI 5052 and CI 5380 for HD
112374 and that from ZnI 4680 for HD 148743) were not used in deriving
the final averaged abundances (table6.dat) because of appreciably
large discrepancies as well as less reliabilities.
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Byte-by-byte Description of file: table6.dat
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Bytes Format Units Label Explanations
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1- 2 A2 --- El Element
4- 9 I6 --- HD Star HD number
11- 15 F5.2 --- [Fe/H] Metallicity
17- 20 F4.2 --- Final (averaged) logarithmic abundance for
element X with the usual normalization
of AH=12 (1)
22- 26 F5.2 [Sun] [X/H] Relative abundance in comparison to the Sun (2)
28- 31 F4.2 --- e_ ?=- Standard deviation in deriving
33- 37 F5.2 --- [X/Fe] Relative abundance to Fe
39- 43 F5.2 --- [X/Zn] Relative abundance to Zn
45- 49 F5.2 --- dT- Delta value of with temperature change (3)
51- 55 F5.2 --- dT+ Delta value of with temperature change (3)
57- 61 F5.2 --- dg- Delta value of with gravity change (3)
63- 67 F5.2 --- dg+ Delta value of with gravity change(3)
69- 73 F5.2 --- dv- Delta value of with turbulence change (3)
75- 79 F5.2 --- dv+ Delta value of with turbulence change (3)
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Note (1): In deriving this, we first calculated the "region means"
corresponding to each region (i.e., mean over the individual lines
belonging to the region), which were further combined and averaged
to obtain .
Note (2): Where the adopted solar abundances are
8.56 (C), 8.05 (N), 8.93 (O), 7.21 (S), 4.60 (Zn), and 7.50 (Fe).
Note (3): Six δ values are the resulting variations of in
response to changing one of the three atmospheric parameters:
-250K (dT-) and +250K (dT+) in Teff,
-0.3 (dg-) and +0.3 (dg+) in log(g), and
-1.5km/s (dv-) and +1.5km/s (dv+) in vt.
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 15-Dec-2008