J/ApJ/976/175 HD 76151 and Sun near-infrared spectroscopy (Senturk+, 2024)
Near-infrared spectroscopy of the Sun and solar analog star HD 76151:
compiling an extensive line list in the Y, J, H, and K bands.
Senturk S.A., Sahin T., Guney F., Bilir S., Marismak M.
<Astrophys. J. 976, 175 (2024)>
=2024ApJ...976..175S 2024ApJ...976..175S (SIMBAD/NED BibCode)
ADC_Keywords: Sun ; Stars, ages ; Stars, masses ; Stars, dwarfs ;
Spectra, infrared ; Abundances ; Spectroscopy
Keywords: Spectral line lists - The Sun - Solar abundances -
Infrared spectroscopy - Spectral line identification - Atomic data -
Stellar abundances - Stellar kinematics
Abstract:
Determining the physical nature of a star requires precise knowledge
of its stellar atmospheric parameters, including effective
temperature, surface gravity, and metallicity. This study presents a
new atomic line list covering a broad spectral range (1-2.5um; YJHK
bands) for iron (Fe) and α-elements (Ca, Mg, Ti, Si) to improve
stellar parameter determination using near-infrared (NIR)
spectroscopy. We highlight the limitations of existing line lists,
stemming primarily from inconsistencies in oscillator strengths for
ionized iron lines within the Apache Point Observatory Galactic
Evolution Experiment DR17. The line list was validated using the
high-resolution and high-quality disk-center NIR spectra of the Sun
and its solar analog HD 76151. As a result of the spectroscopic
analyses, the effective temperature of HD 76151 was calculated as
5790±170K, surface gravity as 4.35±0.18cgs, metal abundance as
0.24±0.09dex, and microturbulence velocity of 0.30+0.5-0.3km/s
by combining the optical and NIR line lists. A comparison of the model
atmospheric parameters calculated for HD 76151 with the PARSEC
isochrones resulted in a stellar mass of , radius
1.125+0.035-0.011R☉ , and an age of 5.5+2.5_-2.1^Gyr. For
the first time, kinematic and dynamical orbital analyses of HD 76151
using a combination of Gaia astrometric and spectroscopic data showed
that the star was born in a metal-rich region within the solar circle
and is a member of the thin disk population. Thus, the slightly
metal-rich nature of the star, as reflected in its spectroscopic
analysis, was confirmed by dynamical orbital analysis.
Description:
table1.dat provides the atmospheric parameters of the adopted stellar
model for the Sun and Sun-like HD76151, along with the error values
for the relevant parameters (effective temperature, surface gravity,
metallicity, and microturbulation velocity). The table also contains
information about the spectral data used, such as the instrument and
wavelength range.
table2.dat provides chemical abundance measurements for multiple
elements derived from high-resolution optical, near-infrared, and
optical+NIR spectroscopy. The abundances are expressed as [X/Fe]
ratios relative to Sun, along with the corresponding uncertainties,
number of lines used, calculated solar abundances and solar reference
(Asplund 2009) abundances.
table3.dat contains the line list with atomic parameters (adopted
loggf value), derived solar abundances with calculated EW value,
damping constant, and RMT number.
Objects:
------------------------------------------------
RA (2000) DE Designation(s)
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08 54 17.94 -05 26 04.0 HD 76151 = HR 3538
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File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table2.dat 73 6 Stellar atmospheric parameters
table3.dat 62 38 Chemical abundances for Sun and HD 76151
tablea.dat 51 273 NIR line list
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See also:
J/ApJS/94/221 : New multiplet table for FeI (Nave+, 1994)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- Star Target star identifier
9- 22 A14 --- Spectrum Instrument used for spectral observation
23- 34 A12 --- WaveRange Wavelength range of the spectrum
(in Angstoems)
36- 39 I4 K Teff Effective temperature
41- 43 I3 K e_Teff Uncertainty in Teff
45- 48 F4.2 [cm/s2] logg Surface gravity
50- 53 F4.2 [cm/s2] e_logg Uncertainty in logg
55- 58 F4.2 [-] [Fe/H] Metallicity
60- 63 F4.2 [-] e_[Fe/H] Uncertainty in [Fe/H]
65- 68 F4.2 km/s ksi Microturblence velocity
70- 73 F4.2 km/s e_ksi Uncertainty in ksi
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 16 A16 --- Species Elemental ionization state and spectral data
used (e.g. Fe II (VIS), Fe II (VIS+NIR))
17 A1 --- n_Species [ab] Note on Species (1)
19- 23 F5.2 [-] [X/Fe]* ?=- Elemental abundance of HD76151
relative to Sun
25- 28 F4.2 [-] e_[X/Fe]* ?=- Uncertainty in [X/Fe]*
30- 32 I3 --- o_[X/Fe]* ?=- Number of the lines measured in HD76151
34- 37 F4.2 [-] logepsSun Calculated solar reference abundances
39- 42 F4.2 [-] e_logepsSun Uncertainty in the solar reference abundance
44- 46 I3 --- o_logepsSun Number of the lines measured in the Sun
48- 51 F4.2 [-] Asp09 Reported solar abundances in the Asplund
(2009RA+A...47..681A 2009RA+A...47..681A)
53- 56 F4.2 [-] sigma Uncertainty abundances for Asplund
(2009RA+A...47..681A 2009RA+A...47..681A)
58- 62 F5.2 [-] delta Solar abundances in the this study - Asp09
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Note (1): Notes as follows:
a = The abundance was determined using the spectrum synthesis method
b = The abundance was determined using a combined optical and NIR line list
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Byte-by-byte Description of file: tablea.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 F8.2 0.1nm Wave Wavelength of the transition in air
10- 13 F4.1 --- Species Ionization state of the elements
15- 19 F5.2 eV LEP Lower excitation potantial of the transition
21- 25 F5.2 --- loggf Oscilator strength (transition probability)
27- 31 F5.1 0.1pm EW Equivalent width
33- 36 F4.2 [-] logepsSun Calculated solar abundances for this
transition
38- 42 F5.2 [rad.cm3/s] logGAMMA ? Damping constant for this transition
43 A1 --- n_logGAMMA [U] U for Unsold damping
45- 48 I4 --- RMT ?=- Rowland Multiplet Number for this
transition
49- 51 A3 --- n_RMT [U/I ] U/I for Unidentified line by
Nave et al. (1994ApJS...94..221N 1994ApJS...94..221N,
Cat. J/ApJS/94/221).
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Acknowledgements:
Sena Aleyna Senturk, senturksenaaleyna(at)gmail.com
(End) Sena Aleyna Senturk [Akdeniz Univ.], Patricia Vannier [CDS] 08-Sep-2025