J/A+A/688/A23 Stellar chromospheric activity of LAMOST sources (Zhang+, 2024)
Stellar chromospheric activity database of solar-like stars based on the LAMOST
Low-Resolution Spectroscopic Survey:
II. The bolometric and photospheric calibration.
Zhang W., Zhang J., He H., Luo A., Zhang H.
<Astron. Astrophys. 688, A23 (2024)>
=2024A&A...688A..23Z 2024A&A...688A..23Z (SIMBAD/NED BibCode)
ADC_Keywords: Stars, G-type ; Spectroscopy ; Stars, activity ; Optical
Keywords: stars: activity - stars: chromospheres
Abstract:
The dependence of stellar magnetic activity on stellar parameters is
inspired by the chromospheric activity studies based on the
large-scale spectroscopic surveys.
The main objective of this project is to provide the chromospheric
activity parameter database for the LAMOST Low-Resolution
Spectroscopic Survey (LRS) spectra of solar-like stars and explore the
overall property of stellar chromospheric activity.
The CaII H and K lines were employed to construct indicators for
assessing and studying the chromospheric activity of solar-like stars.
We investigated the widely used bolometric- and
photospheric-calibrated chromospheric activity index R'HK, derived
from the method in the classic literature (R'HK,classic) and the
method based on the PHOENIX model (R'HK,PHOENIX). Since the detailed
stellar atmospheric parameters, effective temperature (Teff),
surface gravity (logg), and metallicity ([Fe/H]) are available for
LAMOST, we estimated the chromospheric activity index R'HK,PHOENIX,
along with the corresponding bolometric calibrated index
RHK,PHOENIX, taking these parameters into account.
We provided the database of the derived chromospheric activity
parameters for 1,122,495 LAMOST LRS spectra of solar-like stars.
Our calculations show that logR'HK,PHOENIX is approximately linearly
correlated with logR'HK,classic. The results based on our extensive
archive support the view that the dynamo mechanism of solar-like stars
is generally consistent with the Sun; and the value of the solar
chromospheric activity index is located at the midpoint of the
solar-like star sample. We further investigated the proportions of
solar-like stars with different chromospheric activity levels (very
active, active, inactive, and very inactive). The investigation
indicates that the occurrence rate of high levels of chromospheric
activity is lower among the stars with effective temperatures between
5600 and 5900K.
Description:
We identify 1122495 high-quality LRS spectra of solar-like stars from
LAMOST DR8 and provide a database of stellar chromospheric activity
parameters based on this spectral sample. The database contains the
stellar chromospheric activity parameters Stri, SMWO, RHK; and
R'HK, as well as their uncertainties. RHK and R'HK are derived
from the method in the classic literature (denoted with classic) and
the method based on the PHOENIX model (denoted as PHOENIX).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table3.dat 357 1122495 Catalogue data
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See also:
https://doi.org/10.5281/zenodo.8378849 : Paper data
Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 9 I9 --- ObsId Unique observation identifier of
LAMOST LRS spectrum
11- 20 A10 "date" ObsDate Spectral observation date
22- 66 A45 --- fitsname FITS file name of LAMOST LRS spectrum
68- 73 F6.2 --- snrg Signal-to-noise ratio in the g band
(S/Ng) of LAMOST LRS spectrum
75- 80 F6.2 --- snrr Signal-to-noise ratio in the r band
(S/Nr) of LAMOST LRS spectrum
82- 88 F7.2 K Teff Effective temperature (Teff) derived from
the LASP
90- 97 F8.2 K e_Teff ?=-9999 Uncertainty of Teff derived from
the LASP
99-103 F5.3 [cm/s2] logg Surface gravity (logg) derived from the LASP
105-113 F9.3 [cm/s2] e_logg ?=-9999 Uncertainty of logg derived from
the LASP
115-120 F6.3 --- [Fe/H] Metallicity ([Fe/H]) derived from the LASP
122-130 F9.3 --- e_[Fe/H] ?=-9999 Uncertainty of [Fe/H] derived from
the LASP
132-138 F7.2 km/s RV Radial velocity (Vr) derived from the LASP
140-147 F8.2 km/s e_RV ?=-9999 Uncertainty of RV derived from
the LASP
149-162 F14.10 deg RAdeg Right ascension (RA) of fiber pointing
(J2000)
164-176 F13.10 deg DEdeg Declination (DEC) of fiber pointing (J2000)
178-196 I19 --- GaiaDR3 Source identifier in Gaia DR3 catalog
198-211 F14.8 ag Gmag G magnitude in Gaia DR3 catalog
213-220 F8.6 --- Stri Stri index of LAMOST LRS
222-233 F12.6 --- e_Stri ?=-9999 Uncertainty of Stri
235-246 F12.6 --- SMWO SMWO activity index
248-259 F12.6 --- e_SMWO ?=-9999 Uncertainty of SMWO
261-269 F9.6 --- logRHKcl logRHK activity index derived from the
method in the classic literature
271-282 F12.6 --- e_logRHKcl ?=-9999 Uncertainty of logRHKcl
284-292 F9.6 --- logRHKPh logRHK activity index derived from the
method based on the PHOENIX model
294-305 F12.6 --- e_logRHKPh ?=-9999 Uncertainty of logRHKPh
307-318 F12.6 --- logRpHKcl logR'HK activity index derived from the
method in the classic literature
320-331 F12.6 --- e_logRpHKcl ?=-9999 Uncertainty of logRpHKcl
333-344 F12.6 --- logRpHKPh logR'HK activity index derived from the
method based on the PHOENIX model
346-357 F12.6 --- e_logRpHKPh ?=-9999 Uncertainty of logRpHKPh
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Acknowledgements:
Weitao Zhang, b21101012(at)stu.ahu.edu.cn
References:
Zhang et al., Paper I 2022ApJS..263...12Z 2022ApJS..263...12Z
(End) Patricia Vannier [CDS] 07-Jun-2024