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J/A+A/306/924 Optical spectrum of HR 4049 (Bakker+, 1996)
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The optical spectrum of HR 4049 (includes a line identification
from 3650 to 10850 Angstroems)
Bakker E.J., Van Der Wolf F.L.A., Lamers H.J.G.L.M., Gulliver A.F.,
Ferlet R., Vidal-Madjar A.
<Astron. Astrophys. 306, 924 (1996)>
=1996A&A...306..924B (SIMBAD/NED BibCode)
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ADC_Keywords: Line Profiles ; Spectra, infrared
Keywords: line identification - line profiles - binaries: close -
stars: chemical peculiar - stars: HR 4049 - stars: AGB and post-AGB
Description:
High-resolution optical spectra (UES/WHT) of the extreme metal-poor
post-AGB star HR 4049 were obtained at four different orbital phases.
The spectra cover the wavelength region from 3650A to 10850A at a
resolution of R=5.2x10^4^. These observations are supplemented with
four high-resolution spectra of the NaI D1 & D2 and CaII K lines at
R=~10^5^ (CAT/CES). The optical spectrum shows 217 spectral lines:
the Balmer series (H{alpha} - H35), the Paschen series (P9 - P23), NI,
OI and numerous CI lines. We show that the lines of H{alpha}, H{beta},
H{gamma} and NaI D show significant changes in profile between
different observation dates. Nine components were identified in the
profile of the NaI D lines of which three are circumstellar and six
interstellar. The stronger CI lines are asymmetric and we derive a
post-AGB mass-loss of {dot}(M)=6+/-4x10^-7^M_{sun}_/yr from the
asymmetry. The [OI]6300A line has been detected in emission at the
system velocity and we argue that the emission is from an almost
edge-on disk with a radius of about 20R_*_.
HR 4049 is at J2000 position: 00 42 45.8 - 20 21 36
Objects:
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RA (2000) DE Name(s)
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10 18 07.6 -28 59 31 HR 4049 = HD 89353 = AG Ant
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table11 137 217 The line identification of HR 4049
fig9.ps 76 6976 The optical spectrum of HR 4049 (Postscript)
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See also:
J/A+A/336/263 : Radial velocities of HR 4049 (Bakker+1998), Paper II.
Table 2: Log of the WHT/UES observations of HR 4049 (only the number of the
spectra)
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{lambda}_c_ run (code) run (code) run (code) run (code)
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7128.9 A 41655(1.1) 72597(2.1) 74256(3.1) 75240(4.1)
90 s 90 s 90 s 120 s
5260.9 A 41656(1.2) 72594(2.2) 74262(3.2) 75238(4.2)
90 s 120 s 90 s 120 s
4020.0 A 41660(1.3) 72592(2.3) 74269(3.3) 75230(4.3)
300 s 60 s 1500 s 120 s
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Byte-by-byte Description of file: table11
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Bytes Format Units Label Explanations
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3- 11 F9.3 0.1nm LamLab []? Laboratory wavelength of the
identified absorption line
12 A1 --- n_run [*] When '*' the run code is not 3.1,
3.2 or 3.3 (6)
15- 29 A15 --- Multiplet Element and multiplet number of the
given absorption line
36- 40 F5.2 eV Chi []? Lower level excitation energy
of the transition
45- 50 F6.3 --- log(gf) []? Oscillator strength of the transition
56- 64 F9.3 0.1nm LamObs Observed wavelength of the absorption
feature (1)
68- 71 F4.1 % Depth []? Observed depth of the central
absorption relative to the continuum (2)
77- 80 I4 0.1pm EW []? Observed equivalent width (3)
86- 88 I3 km/s FWHM []? Full-Width-Half-Maximum of the
absorption feature (4)
94- 96 I3 km/s HRV []? Radial heliocentric velocity for the
identified absorption feature (5)
101-103 F3.1 --- run Run code (6)
109 I1 --- q_LamLab Quality factor for the identification of
the absorption feature (7)
114-137 A24 --- Remarks Remarks on the line identification (8)
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Note (1): The estimated accuracy is about 3km/s, based on S/N ratio and
internal accuracy of the calibration method
Note (2): A line to zero intensity gives a depression of 100%. A mean error
of 2% is adopted
Note (3): The estimated error on the equivalent width is 10%
Note (4): The accuracy is dependent on the S/N ratio and is estimated as 3km/s
Note (5): The accuracy is 3 km/s
Note (6): The number of the spectra is given in Table 2. They refer to the
number which was assigned to this spectrum during the observations
Note (7): 1: lines are severely polluted or very weak and can not be used
for further studies
2: line is lightly blended
3: line is positively uniquely identified
Note (8): a: asymmetric line profile
b: line profile is blended
f: forbidden line
IS: interstellar
CS: circumstellar
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(End) Simona Mei [CDS] 26-Jul-1995