J/ApJS/239/19 Absorption lines in 21 Lyn A-type star (Sameshima+, 2018)
WINERED high-resolution near-infrared line catalog: A-type star.
Sameshima H., Ikeda Y., Matsunaga N., Fukue K., Kobayashi N., Kondo S.,
Hamano S., Kawakita H., Yasui C., Izumi N., Mizumoto M., Otsubo S.,
Takenaka K., Watase A., Asano A., Yoshikawa T.
<Astrophys. J. Suppl. Ser., 239, 19 (2018)>
=2018ApJS..239...19S 2018ApJS..239...19S
ADC_Keywords: Stars, A-type; Equivalent widths; Line Profiles; Spectra, infrared
Keywords: atlases ; line: identification ; stars: fundamental parameters ;
stars: individual (21 Lyn)
Abstract:
We present a catalog of absorption lines in the z', Y, and J bands
that we identified in 21 Lyn, a slowly rotating A0.5V star. We
detected 155 absorption features in the high-resolution (0.90-1.35um,
R=28000) spectrum obtained with the WINERED spectrograph after the
telluric absorption was carefully removed using a spectrum of a B-type
star as a telluric standard. With a visual comparison with synthetic
spectra, we compiled a catalog of 219 atomic lines for the 155
features, some of which are composed of multiple fine structure lines.
The high-quality WINERED spectrum enabled us to detect a large number
of weak lines down to ∼1% in depth, which are identified for an A-type
star for the first time. The catalog includes the lines of H, C, N, O,
Mg, Al, Si, S, Ca, Fe, and Sr. These new lines are expected to be
useful for spectral classification and chemical abundance analyses,
while the line catalog is useful for observers who plan to use A-type
stars as telluric standards because it is necessary to distinguish
between stellar lines and telluric absorption lines in high-resolution
spectra. ASCII versions of the spectra are available in the online
version of the journal.
Description:
The observation of 21 Lyn was carried out on 2014 January 23 using the
WINERED echelle spectrograph (coverage of 0.90-1.35um and R=28000)
mounted on the 1.3m Araki Telescope at the Koyama Astronomical
Observatory in Kyoto, Japan.
Objects:
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RA (ICRS) DE Designation(s)
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07 26 42.85 +49 12 41.5 * 21 Lyn = TYC 3401-1648-1
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table3.dat 46 155 Measurement of the absorption features in 21 Lyn
table4.dat 106 219 Line catalog
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See also:
J/ApJS/99/135 : Rotation and Spectral Peculiarities (Abt+ 1995)
J/ApJS/124/527 : Oscillator strengths for lines in J & H bands (Melendez+,
1999)
J/A+AS/137/521 : 8500-8750Å high resolution spectroscopy (Munari+, 1999)
J/ApJ/535/325 : Spectra of normal stars in the J-band (Wallace+ 2000)
J/A+A/585/A143 : NIR spectroscopy of the Sun and HD20010 (Andreasen+, 2016)
Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- Seq [1/155] Identifier
5- 11 F7.1 0.1nm lamAir [9094.8/13177] Wavelength in air; Angstroms
13- 16 F4.1 % Depth [0.4/26.7]? Percent depth of absorption feature
18- 22 F5.1 10-13m EW [2.7/278]? Equivalent width; milliAngstroms
24- 27 F4.1 km/s FWHM [9.2/56]? Feature Full-Width at Half-Maximum
29- 30 A2 --- Rank Rank (G1)
32- 46 A15 --- El Element identifier
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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- 10 F10.4 0.1nm lamAir [9094.8/13177] Wavelength in air; Angstroms
12- 21 F10.4 0.1nm lamVac [9097.3/13180.5] Wavelength in vacuum; Angstroms
23- 37 A15 --- El Element identifier
39- 44 F6.3 [-] log(gf)V [-3/1.3] VALD log oscillator strength
46- 50 F5.2 [-] log(gf)M [-3.2/1.1]? Melendez & Barbuy (1999,
J/ApJS/124/527) log oscillator strength
52- 58 F7.4 eV EPlow [1.8/13] Lower level excitation potential
60- 66 F7.4 eV EPup [2.9/14.1] Upper level excitation potential
68- 81 A14 --- Termlow Lower level term
83- 96 A14 --- Termup Upper level term
98- 99 A2 --- Rank Rank (G1)
101-103 A3 --- --- [ID=]
104-106 I3 --- Seq [1/155] Identifier from Table 3
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Global notes:
Note (G1): The scatter in the measured FWHM increases with decreasing depth,
which is simply due to the random noise of the photon counts. The
scatter is clearly small for the lines stronger than 5% in depth.
Considering these trends, we classified the detected features into
three strength classes: 1 for lines stronger than 5% in depth, 2 for
lines with a depth of 2%-5%, and 3 for lines weaker than 2%. The lines
in our line catalog are mainly ranked according to these strength
classes. "B" for blended lines; "F" for fine structure lines.
See section 3 for further explanations.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 29-Jan-2019