J/A+A/672/A183 Gaia DR3 data of 15062 gravity-mode pulsators (Aerts+, 2023)
Astrophysical properties of 15062 Gaia DR3 gravity-mode pulsators.
Aerts C., Molenberghs G., De Ridder J.
<Astron. Astrophys. 672, A183 (2023)>
=2023A&A...672A.183A 2023A&A...672A.183A (SIMBAD/NED BibCode)
ADC_Keywords: Stars, dwarfs ; Stars, variable ; Stars, B-type ; Stars, F-type ;
Effective temperatures ; Rotational velocities
Keywords: asteroseismology - methods: statistical - astronomical databases -
stars: oscillations - stars: rotation - stars: interiors
Abstract:
Gravito-inertial asteroseismology saw its birth thanks to
high-precision CoRoT and Kepler space photometric light curves. So
far, it gave rise to the internal rotation frequency of a few hundred
intermediate-mass stars, yet only several tens of these have been
weighed, sized, and age-dated with high precision from asteroseismic
modelling.
We aim to increase the sample of optimal targets for future
gravito-inertial asteroseismology by assessing the properties of 15062
newly found Gaia DR3 gravity-mode pulsators.We also wish to
investigate if there is any connection between their fundamental
parameters and dominant mode on the one hand, and their spectral line
broadening measured by Gaia on the other hand.
After re-classifying about 22% of the F-type gravity-mode pulsators as
B-type according to their effective temperature, we construct
histograms of the fundamental parameters and mode properties of the
15062 new Gaia DR3 pulsators. We compare these histograms with those
of 63 Kepler bona fide class members.We fit errors-in-variables
regression models to couple the effective temperature, luminosity,
gravity, and oscillation properties to the two Gaia DR3 parameters
capturing spectral line broadening for a fraction of the pulsators.
We find that the selected 15062 gravity-mode pulsators have properties
fully in line with those of their well-known Kepler analogues,
revealing that Gaia has a role to play in asteroseismology. The
dominant g-mode frequency is a significant predictor of the spectral
line broadening for the class members having this quantity measured.
We show that the Gaia vbroad parameter captures the joint effect of
time-independent intrinsic and rotational line broadening and
time-dependent tangential pulsational broadening.
While the Gaia mission was not designed to detect non-radial
oscillation modes, its multitude of data and homogeneous data
treatment allow us to identify a vast amount of new gravity-mode
pulsators having fundamental parameters and dominant mode properties
in agreement with those of such Kepler bona fide pulsators. This large
new sample of Gaia DR3 pulsators can be followed up with dedicated
high-precision photometric or high-resolution spectroscopic
instruments to embark upon asteroseismic modelling.
Description:
Observables for 15062 stars deduced from Gaia DR3 data are presented.
For each star the Gaia DR3 identification number is given, as well as
the spectral line broadening, the projected surface rotation velocity,
the effective temperature, the surface gravity, the luminosity, the
dominant frequency of variability in the Gaia G band, the amplitude of
this dominant frequency, the radius, and the projected surface
rotation frequency. The radius is computed from the luminosity and
effective temperature. Missing values of the observables are indicated
in the same format as measured values for coding convenience.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
gdor.dat 194 11636 Gamma Dor candidate pulsators
spb.dat 194 3426 SPB candidate pulsators
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See also:
I/355 : Gaia DR3 Part 1. Main source (Gaia Collaboration, 2022)
Byte-by-byte Description of file: gdor.dat spb.dat
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Bytes Format Units Label Explanations
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1- 19 I19 --- GaiaDR3 Gaia DR3 source_id (gaia.source_id)
21- 29 F9.3 km/s Vbroad ?=-999 Gaia DR3 spectral line broadening
parameter (gaia.vbroad) (1)
30- 38 F9.3 km/s e_Vbroad ?=-999 Gaia DR3 spectral line broadening
parameter error (gaia.vbroad_error) (1)
39- 47 F9.3 km/s vsini-HS ?=-999 Gaia DR3 projected rotational velocity
from ESP-HS (astro.vsini_esphs) (1)
48- 56 F9.3 km/s e_vsini-HS ?=-999 Gaia DR3 projected rotational velocity
from ESP-HS error
(astro.vsiniesphsuncertainty) (1)
57- 65 F9.4 K Teff Gaia DR3 effective temperature from GSP-Phot
(astro.teff_gspphot) (1)
66- 73 F8.4 K b_Teff Lower confidence level of Gaia DR3 effective
temperature from GSP-Phot
(astro.teffgspphotlower) (1)
74- 81 F8.4 K B_Teff Upper confidence level of Gaia DR3 effective
temperature from GSP-Phot
(astro.teffgspphotupper) (1)
82- 89 F8.4 [cm/s2] logg Gaia DR3 surface gravity from GSP-Phot
(astro.logg_gspphot) (1)
90- 97 F8.4 [cm/s2] b_logg Lower confidence level of Gaia DR3 surface
gravity from GSP-Phot
(astro.logggspphotlower) (1)
98-105 F8.4 [cm/s2] B_logg Upper confidence level of Gaia DR3 surface
gravity from GSP-Phot
(astro.logggspphotupper) (1)
106-113 F8.4 [Lsun] logL log10 of luminosity (2)
114-121 F8.4 [Lsun] e_logL 1-sigma error of log_10 (luminosity) (2)
122-132 F11.7 d-1 FrepD Dominant frequency in Gaia DR3
G light curve (2)
133-143 F11.7 mag AmpD Amplitude of dominant frequency (2)
144-154 F11.7 mag e_AmpD 1-sigma error of amplitude (2)
155-165 F11.7 Rsun Radius Radius computed in this work
166-176 F11.7 Rsun e_Radius [] 1-sigma error of radius
computed in this work
177-185 F9.3 d-1 Freqpsr ?=-999 Projected surface rotation frequency
computed in this work
186-194 F9.3 d-1 e_Freqpsr []?=-999 1-sigma error of projected surface
rotation frequency computed in this work
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Note (1): see Gaia DR3 online documentation:
https://www.cosmos.esa.int/web/gaia-users/archive/gdr3-documentation
Note (2): computed by Gaia Collaboration, De Ridder, J., et al.,
2023, A&A, in press (arXiv:2206.06075)
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Acknowledgements:
Conny Aerts, conny.aerts(at)kuleuven.be
(End) Conny Aerts [KU Leuven, Belgium], Patricia Vannier [CDS] 16-Feb-2023