J/A+A/660/A7 Optical atomic and NIR atomic/molecular lines (Fanelli+, 2022)
Stellar population astrophysics (SPA) with the TNG.
The chemical content of the red supergiant population in the Perseus complex.
Fanelli C., Origlia L., Oliva E., Dalessandro E., Mucciarelli A., Sanna N.
<Astron. Astrophys. 660, A7 (2022)>
=2022A&A...660A...7F 2022A&A...660A...7F (SIMBAD/NED BibCode)
ADC_Keywords: Atomic physics ; Optical ; Infrared
Keywords: techniques: spectroscopic - stars: abundances - stars: late-type -
stars: supergiants
Abstract:
The Perseus complex in the outer disk of the Galaxy hosts a number of
clusters and associations of young stars. Gaia is providing a detailed
characterisation of their kinematic structure and evolutionary
properties. Within the SPA Large Programme at the TNG, we secured
HARPS-N and GIANO-B high-resolution optical and near-infrared (NIR)
spectra of the young red supergiants (RSG) stars in the Perseus
complex, in order to obtain accurate radial velocities, stellar
parameters and detailed chemical abundances. We used spectral
synthesis to best-fit hundreds of atomic and molecular lines in the
spectra of the observed 27 RSGs. We obtained accurate estimates of the
stellar temperature, gravity, micro and macro turbulence velocities
and chemical abundances for 25 different elements. We also measured
the 12C/13C abundance ratio.
Our combined optical and NIR chemical study provides homogeneous
half-solar iron with a small dispersion, about solar-scaled abundance
ratios for the iron-peak, alpha and other light elements and a small
enhancement of Na, K and neutron-capture elements, consistent with the
thin disk chemistry traced by older stellar populations at a similar
Galactocentric distance of about 10kpc. We inferred enhancement of N,
depletion of C and of the 12C/13C isotopic abundance ratio,
consistent with mixing processes in the stellar interiors during the
RSG evolution.
Description:
Table 1 and 2 list the optical and in the NIR atomic lines,
respectively, used for the chemical analysis.
Table 3 is a compilation of the NIR CO, OH, CN and HF molecular lines
used to derive CNO and F abundances. All wavelengths are in Å and
in the air.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 38 189 *Optical atomic lines
tablea2.dat 38 210 *NIR atomic lines
tablea3.dat 38 143 *NIR molecular lines
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Note on table*.dat: Lines are ordered by wavelengths.
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Byte-by-byte Description of file: tablea1.dat tablea2.dat tablea3.dat
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Bytes Format Units Label Explanations
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2- 10 F9.3 0.1nm lambdaAir Air wavelength
14- 19 F6.2 --- Line Line identification
25- 28 F4.2 eV EP Potential energy
33- 38 F6.3 --- log(gf) Oscillator strength
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Acknowledgements:
Cristiano Fanelli, cristiano.fanelli3(at)unibo.it
(End) C. Fanelli [INAF - OAS Bologna, UNIBO], P. Vannier [CDS] 30-Dec-2021