J/A+A/547/A108 Comparative modelling of cool giants spectra (Lebzelter+, 2012)
Comparative modelling of the spectra of cool giants.
Lebzelter T., Heiter U., Abia C., Eriksson K., Ireland M., Neilson H.,
Nowotny W., Maldonado J., Merle T., Peterson R., Plez B., Short C.I.,
Wahlgren G.M., Worley C., Aringer B., Bladh S., de Laverny P., Goswami A.,
Mora A., Norris R.P., Recio-Blanco A., Scholz M., Thevenin F., Tsuji T.,
Kordopatis G., Montesinos B., Wing R.F.
<Astron. Astrophys. 547, A108 (2012)>
=2012A&A...547A.108L 2012A&A...547A.108L
ADC_Keywords: Models, atmosphere ; Stars, giant ; Spectroscopy
Keywords: stars: atmospheres - stars: late-type - methods: analytical -
stars: fundamental parameter
Abstract:
Our ability to extract information from the spectra of stars depends
on reliable models of stellar atmospheres and appropriate techniques
for spectral synthesis. The corresponding paper aims to compare a wide
variety of model codes and strategies for the analysis of stellar
spectra that are available today. The online tables list spectral
lines used during the analysis together with the basic line
parameters.
Description:
Spectra representing four cool giant stars were made available to
various groups and individuals working in the area of spectral
synthesis, asking them to derive stellar parameters from the data
provided. The results were discussed at a workshop in Vienna in 2010.
Most of the major codes currently used in the astronomical community
for analyses of stellar spectra were included in this experiment.
The files contain the spectra in the same form as they were made
available to the experiment participants.
The spectra for Star 1 and Star 2 are on the heliocentric wavelength
scale (i.e. corrected for Earth motion, but not for stellar radial
velocity). The spectra are normalized to the continuum by an automatic
pipeline, which first divides the spectrum by a flat field response
function and then removes the overall slope of the whole spectrum.
These optical spectra also contain a number of telluric lines.
The spectra for Star 3 and Star 4 are on the laboratory wavelength
scale and the flux is normalized to the continuum. They do not contain
telluric lines.
Additional information which was provided to the experiment
participants:
----------------------------------------------------------------
FileName Spectral resolution Signal-to-noise ratio
----------------------------------------------------------------
star1.dat 80000 463 at 871 nm
star2.dat 80000 517 at 871 nm
star3.dat 70000 125
star4.dat 70000 125
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Objects:
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RA (2000) DE Designation(s) (File)
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04 35 55.24 +16 30 33.5 Aldebaran = HR 1457 (K5III) (star1.dat)
03 02 16.77 +04 05 23.1 Menkar = HR 911 (M1.5IIIa) (star2.dat)
-----------------------------------------------------------------------
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table6.dat 33 26 Iron line selection for the M6 stellar parameter
determination
table7.dat 42 32 Lines used in the A1 analysis to determine
abundances for Star 1 (HR 1457)
table8.dat 37 5 Fe lines used in the A1 analysis to determine
abundances for Star 3 (artificial star)
table9.dat 46 65 Lines used by the A2 participants
table10.dat 48 60 Lines analysed by the A5 team
table11.dat 52 14 Measured CO 3-0 lines in Star 4 (artificial star)
from the T analysis
star1.dat 20 114979 Observed optical spectrum for Albedaran (HR 1457)
star2.dat 20 114973 Observed optical spectrum for Menkar (HR 911)
star3.dat 18 2101 Simulated observed H-band spectrum for Star 3
(T=4257K, logg=1.47, M=1.165M☉, [Fe/H]=-0.4)
star4.dat 18 2101 Simulated observed H-band spectrum for Star 4
(T=3280K, logg=0.06, M=1.509M☉, [Fe/H]=+0.1)
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Byte-by-byte Description of file: table6.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 5 A5 --- El Element (Fe I or Fe II)
7- 13 F7.3 nm lambda Wavelength
15- 20 F6.3 eV Elow Lower level excitation potential
24- 29 F6.3 --- log(gf) gf value
31- 33 A3 --- Source Line data source (1)
--------------------------------------------------------------------------------
Note (1): References as follows:
K07 = Kurucz, 2007, http://kurucz.harvard.edu/atoms/2000/gf2000.lines
BWL = O'Brian et al. (1991, Journal of the Optical Society of
America B Optical Physics, 8, 1185)
RU = Raassen & Uylings (1998, Cat. J/A+A/340/300)
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Byte-by-byte Description of file: table7.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 2 I2 --- Z Atomic number
5- 11 F7.3 nm lambda Wavelength
13- 18 F6.3 --- log(gf) gf value
21- 24 A4 --- Source Line data source (1)
27- 35 F9.3 cm-1 Elow Lower level excitation potential
39- 42 F4.2 --- abund Abundance (log(NH)=12.00)
--------------------------------------------------------------------------------
Note (1): References as listed in
http://kurucz.harvard.edu/LINELISTS/LINES/gfall.ref
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table8.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 F8.3 nm lambda Wavelength
10- 15 F6.3 --- log(gf) gf value
17- 19 A3 --- Source Line data source (1)
22- 30 F9.3 cm-1 Elow Lower level excitation potential
34- 37 F4.2 --- abund Abundance (log(NH)=12.00)
--------------------------------------------------------------------------------
Note (1): References as listed in
http://kurucz.harvard.edu/LINELISTS/LINES/gfall.ref
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table9.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 5 F5.2 --- Ion Species code following Kurucz's notation
7 A1 --- n_Ion [*] Line included in the final fit
10- 16 F7.3 nm lambda Wavelength
19- 24 F6.3 --- log(gf) gf value
27- 29 A3 --- Source line data source (1)
33- 38 F6.2 0.1pm EW1 ? Equivalent width Star 1 (HR 1457); in mÅ
41- 46 F6.2 0.1pm EW2 ? Equivalent width Star 2 (HR 911); in mÅ
--------------------------------------------------------------------------------
Note (1): References as listed in
http://kurucz.harvard.edu/LINELISTS/LINES/gfall.ref
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table10.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 5 A5 --- El Element (Fe I or Fe II)
7- 14 F8.4 nm lambda Wavelength
20- 24 F5.3 eV Elow Lower level excitation potential
28- 33 F6.3 --- log(gf) gf value
38- 42 F5.1 0.1pm EW Equivalent width in mÅ
46- 48 A3 --- Source Line data source (1)
--------------------------------------------------------------------------------
Note (1): References as listed in
http://kurucz.harvard.edu/LINELISTS/LINES/gfall.ref
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table11.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 F8.3 nm lambda Wavelength
11- 16 F6.3 --- log(gf) gf value
19- 26 F8.3 cm-1 Elow Lower level excitation potential
30- 35 F6.3 --- logW/nu Equivalent width over wavenumber
38- 52 A15 --- Ident Line identification
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Byte-by-byte Description of file: star1.dat star2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 F8.3 0.1nm lambda [4900/9800] Air wavelength (see description)
10- 20 E11.4 --- Flux Flux normalized to continuum (see description)
--------------------------------------------------------------------------------
Byte-by-byte Description of file: star3.dat star4.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 9 F9.3 0.1nm lambda [15456/15677] Air wavelength (see description)
11- 18 F8.6 --- Flux Flux normalized to continuum (see description)
--------------------------------------------------------------------------------
Acknowledgements:
Thomas Lebzelter, thomas.lebzelter(at)univie.ac.at
(End) Patricia Vannier [CDS] 12-Sep-2012