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J/A+A/306/924              Optical spectrum of HR 4049      (Bakker+, 1996)

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)
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=5.2x104. These observations are supplemented with four high-resolution spectra of the NaI D1 & D2 and CaII K lines at R≃105 (CAT/CES). The optical spectrum shows 217 spectral lines: the Balmer series (Hα - H35), the Paschen series (P9 - P23), NI, OI and numerous CI lines. We show that the lines of Hα, Hβ, Hγ 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±4x10-7M/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: -------------------------------------------------- RA (2000) DE Name(s) -------------------------------------------------- 10 18 07.6 -28 59 31 HR 4049 = HD 89353 = AG Ant -------------------------------------------------- File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table11 137 217 The line identification of HR 4049 fig9.ps 76 6976 The optical spectrum of HR 4049 (Postscript)
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) -------------------------------------------------------------------- λc run (code) run (code) run (code) run (code) -------------------------------------------------------------------- 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 --------------------------------------------------------------------- Byte-by-byte Description of file: table11
Bytes Format Units Label Explanations
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)
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

(End) Simona Mei [CDS] 26-Jul-1995
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