J/MNRAS/421/679 IRAS 22023+5249 spectroscopy (Sarkar+, 2012)
High-resolution spectroscopy of the high-velocity hot post-AGB star
LS III +52°24 (IRAS 22023+5249).
Sarkar G., Garcia-Hernandez D.A., Parthasarathy M., Manchado A.,
Garcia-Lario P., Takeda Y.
<Mon. Not. R. Astron. Soc., 421, 679-699 (2012)>
=2012MNRAS.421..679S 2012MNRAS.421..679S
ADC_Keywords: Stars, giant ; Infrared sources ; Spectroscopy
Keywords: stars: abundances - stars: AGB and post-AGB - stars: atmospheres -
stars: early-type - stars: evolution -
stars: individual: IRAS 22023+5249
Abstract:
The first high-resolution (R∼50000) optical spectrum of the B-type
star, LS III +52 24, identified as the optical counterpart of the hot
post-asymptotic giant branch (post-AGB) candidate IRAS 22023+5249
(I22023) is presented. We report the detailed identifications of the
observed absorption and emission features in the full wavelength range
(4290-9015Å) as well as the atmospheric parameters and
photospheric abundances (under the local thermodynamic equilibrium
approximation) for the first time. The nebular parameters (Te, Ne) are
also derived.
Description:
IRAS 22023+5249 was observed on 14 July 2001 using the Utrecht Echelle
Spectrograph on the 4.2m William Herschel Telescope at the Roque de
los Muchachos Observatory in La Palma (Spain).
Objects:
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RA (2000) DE Designation(s)
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22 04 12.30 +53 04 01.4 LS III +52 24 = IRAS 22023+5249
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 78 79 Absorption lines in IRAS 22023+5249
table3.dat 78 71 Emission lines in IRAS 22023+5249
table4.dat 66 20 P-Cygni lines in IRAS 22023+5249
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Byte-by-byte Description of file: table2.dat table3.dat
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Bytes Format Units Label Explanations
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1- 8 F8.3 0.1nm lam.O [4300/8900]?=- Observed wavelength λO
9 A1 --- n_lam.O Note on individual lines (1)
10 A1 --- --- [+]
11- 18 F8.3 0.1nm lam.L [4300/8900]?=- Laboratory wavelength λL
19 A1 --- n_lam.L [bcdefghi] Note on individual lines (1)
21- 33 A13 --- Id Line identification (UN for unknown)
35- 40 F6.4 0.1nm EW ?=- Line equivalent width
42- 47 F6.3 [-] loggf ?=- Oscillator strength
49- 53 F5.2 eV chil ?=- Lower value of energy potential interval
54 A1 --- --- [-]
55- 59 F5.2 eV chiu ? Upper value of energy potential interval
61- 65 F5.3 0.1nm |Dlam| ?=- Rest wavelength |Δλ| (2)
67- 73 F7.2 km/s RV ? Radial velocity
74- 78 A5 --- n_RV Note on RV: Blend or Weak
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Note (1): Notes as follows:
b = OII(5) 4414.899Å is blended with FeII(32)Å emission
c = OII(5) 4416.975Å is blended with the absorption component of the
FeIII(114) 449.596 P-Cygni profile
d = OII(28) 4906.88Å is blended with [FeII](20F) 4905.35Å emission
e = Diffuse Interstellar Band (DIB) 6283.84Å is blended with
telluric absorption lines in this region
f = FeII(32) 4413.601Å is blended with OII(5) 4414.899Å absorption
feature
g = [FeII](20F) 4905.35Å is blended with OII(28) 4906.88Å absorption
feature
h = [NII](1F) 6583.6Å is blended with the emission component of the
CII(2) 6582.88Å P-Cygni profile
i = These emission lines are weak and are blended with the atmospheric
absorption lines in this region
Note (2): Note that the rest wavelengths from Hobbs et al.
(2008ApJ...680.1256H 2008ApJ...680.1256H) are given for the DIBs (Diffuse Interstellar Bands).
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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 A1 --- --- [+]
2- 9 F8.3 0.1nm lam.L [4300/8900] Laboratory wavelength {almbda}L
10 A1 --- n_lam.L [abcd] Note on individual lines (1)
12- 19 A8 --- Id Line identification (UN for unknown)
21- 26 F6.4 0.1nm EWa ?=- Equivalent width (absorption)
28- 34 F7.4 0.1nm EWe ?=- Equivalent width (emission)
36- 41 F6.3 [-] loggf ?=- Oscillator strength
43- 47 F5.2 eV chil ?=- Lower value of energy potential interval
48 A1 --- --- [-]
49- 53 F5.2 eV chiu ? Upper value of energy potential interval
55- 61 F7.2 km/s WV ? Wind velocity estimated from the blue
absorption edges of the P-Cygni profiles
62- 66 A5 --- n_WV Note on WV: Blend or Weak
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Note (1): Notes as follows:
a = The absorption component of FeIII(114) 4419.596Å is blended with
OII(5) 4416.975 absorption feature.
b = The emission components of the Hβ and Hα profiles have broad
wings. Gaussian fits to the absorption and emission components of these
profiles could not be obtained. Using iraf, the equivalent widths of
these components were estimated by subtracting the linear continuum
between the points of interest and summing the pixels with partial
pixels at the ends.
c = These lines are blended
d = CII(2) 6582.88Å P-Cygni profile is blended with [NII](1F) 6583.6Å
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 19-Oct-2012