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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
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: ---------------------------------------------------------- RA (2000) DE Designation(s) ---------------------------------------------------------- 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 ---------------------------------------------------------- File Summary:
FileName Lrecl Records Explanations
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
Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
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)
Byte-by-byte Description of file: table4.dat
Bytes Format Units Label Explanations
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)
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).
Byte-by-byte Description of file: table5.dat
Bytes Format Units Label Explanations
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
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.
Byte-by-byte Description of file: table6.dat
Bytes Format Units Label Explanations
1- 2 A2 --- El Element 4- 9 I6 --- HD Star HD number 11- 15 F5.2 --- [Fe/H] Metallicity 17- 20 F4.2 --- <AX> 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_<AX> ?=- Standard deviation in deriving <AX> 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 <AX> with temperature change (3) 51- 55 F5.2 --- dT+ Delta value of <AX> with temperature change (3) 57- 61 F5.2 --- dg- Delta value of <AX> with gravity change (3) 63- 67 F5.2 --- dg+ Delta value of <AX> with gravity change(3) 69- 73 F5.2 --- dv- Delta value of <AX> with turbulence change (3) 75- 79 F5.2 --- dv+ Delta value of <AX> with turbulence change (3)
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 <AX>. 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 <AX> 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.
History: From electronic version of the journal
(End) Patricia Vannier [CDS] 15-Dec-2008
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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