J/A+A/688/A13 K2 asteroseismic KEYSTONE Sample. I. (Lund+, 2024)
The K2 asteroseismic KEYSTONE sample of dwarf and subgiant solar-like
oscillators. I. Data and asteroseismic parameters.
Lund M.N., Basu S., Bieryla A., Casagrande L., Huber D., Hekker S.,
Viani L., Davies G.R., Campante T.R., Chaplin W.J., Serenelli A.,
Ong J.M.J., Ball W.H., Stokholm A., Bellinger E.P., Bazot, M., Stello D.,
Latham D.W., White T.R., Sayeed M., Aguirre Borsen-Koch V., Chontos A.
<Astron. Astrophys. 688, A13 (2024)>
=2024A&A...688A..13L 2024A&A...688A..13L (SIMBAD/NED BibCode)
ADC_Keywords: Stars, G-type; Stars, F-type ; Asteroseismology ;
Effective temperatures
Keywords: asteroseismology - methods: data analysis - catalogs -
stars: fundamental parameters - stars: oscillations -
planetary systems
Abstract:
The KEYSTONE project aims to enhance our understanding of
solar-like oscillators by delivering a catalogue of global
asteroseismic parameters (Δν and νmax) for 173 stars,
comprising mainly dwarfs and subgiants, observed by the K2 mission in
its short-cadence mode during campaigns 6-19.
We derive atmospheric parameters and luminosities using spectroscopic
data from TRES, astrometric data from Gaia, and the infrared flux
method (IRFM) for a comprehensive stellar characterisation.
Asteroseismic parameters are robustly extracted using three
independent methods, complemented by an iterative refinement of the
spectroscopic analyses using seismic log(g) values to enhance
parameter accuracy.
Our analysis identifies new detections of solar-like oscillations in
159 stars, providing an important complement to already published
results from previous campaigns. The catalogue provides homogeneously
derived atmospheric parameters and luminosities for the majority of
the sample. Comparison between spectroscopic Teff and those obtained
from the IRFM demonstrates excellent agreement. The iterative approach
to spectroscopic analysis significantly enhances the accuracy of the
stellar properties derived.
Description:
There are three datasets in total providing information on
atmospheric, astrometric, and asteroseismic properties. In all tables
each star is identified by its K2 EPIC ID. Additional identifiers
(HIP, GAIA) are provided in the table containing astrometric
information. The table with atmospheric parameters provide
measurements of Teff, [Fe/H], log(g), vsin(i), and radial velocity
from a spectroscopic analysis. Additionally, Teff and theta (angular
diameter) is provided from the infrared flux method (IRFM). The table
with astrometric parameters provide information on reddening,
distances, and luminosities. The asteroseismic properties table
provide measurements of the global asteroseismic parameters
Δν and νmax from three different analysis pipelines.
Where relevant, uncertainties defined either as a symmetric error (e_)
or as upper (E_) and lower (e_) uncertainties. The atmospheric and
astrometric tables include relevant notes on the individual stars
providing information on, e.g., binarity, know exoplanets, and sources
to the literature.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table3.dat 154 173 Astrometric properties
table2.dat 111 173 Atmospheric properties
table4.dat 104 221 Seismologic properties
refs.dat 83 22 References
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See also:
B/wds : The Washington Visual Double Star Catalog (Mason+ 2001-2020)
I/311 : Hipparcos, the New Reduction (van Leeuwen, 2007)
I/347 : Distances to 1.33 billion stars in Gaia DR2
(Bailer-Jones+, 2018)
I/350 : Gaia EDR3 (Gaia Collaboration, 2020)
I/352 : Distances to 1.47 billion stars in Gaia EDR3
(Bailer-Jones+, 2021)
III/284 : APOGEE-2 data from DR16 (Johnsson+, 2020)
IV/34 : K2 Ecliptic Plane Input Catalog (EPIC) (Huber+, 2017)
J/A+A/530/A138 : Geneva-Copenhagen survey re-analysis (Casagrande+, 2011)
J/A+A/616/A7 : Gaia DR2 radial velocity standard stars catalog
(Soubiran+, 2018)
J/AJ/153/21 : Abundances in the local region. II. F, G, and K dwarfs
(Luck+, 2017)
https://stilism.obspm.fr/ : Stilim reddening catalogue
Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 9 I9 -- EPIC EPIC identification number
11- 16 F6.3 mag Kpmag Kepler magnitude
18- 23 I6 -- HIP ? Hipparcos identification number
25- 43 I19 -- GaiaDR3 Gaia DR3 identification number
45- 51 F7.3 pc Dist Photogeometric distance (1)
53- 58 F6.3 pc E_Dist Upper statistical distance uncertainty
60- 65 F6.3 pc e_Dist Lower statistical distance uncertainty
67- 72 F6.3 -- RUWE ? Renormalised Unit Weight Error (2)
74- 76 I3 mmag E(B-V) ? Reddening from Stilism project (3)
78- 79 I2 mmag E_E(B-V) ? Upper statistical reddening uncertainty
81- 82 I2 mmag e_E(B-V) ? Lower statistical reddening uncertainty
84- 89 F6.3 solLum LSPC ? Luminosity based on Gaia and SPC
91- 95 F5.3 solLum e_LSPC ? Uncertainty on luminosity
based on Gaia and SPC
97-102 F6.3 solLum LIRFM ? Luminosity based on Gaia and IRFM
104-108 F5.3 solLum e_LIRFM ? Uncertainty on luminosity
based on Gaia and IRFM
110-154 A45 -- Notes Notes on individual stars (4)
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Note (1): Bailer-Jones et al. (2021AJ....161..147B 2021AJ....161..147B), unless otherwise stated
in the notes.
Note (2): RUWE from Lindegren et al. (2018A&A...616A...2L 2018A&A...616A...2L)
Note (3): from Capitanio et al., (2017A&A...606A..65C 2017A&A...606A..65C), unless otherwise
stated in the notes.
Note (4): Notes:
a = the star is a member of M67
b = M67 reddening from Taylor (2007AJ....133..370T 2007AJ....133..370T)
c = Distance from Gaia DR2 (Bailer-Jones et al., 2018AJ....156...58B 2018AJ....156...58B)
d = Distance from inverted Hipparcos parallax (van Leeuwen,
2007A&A...474..653V 2007A&A...474..653V)
Notes on individual stars including membership of the Washington
Double Star (WDS) catalog; if the star is a known radial velocity
exoplanet host (RVEH); if the star is a know exoplanet host from K2 data;
if a seismic analysis has been conducted earlier (S); if the star is
a know member of a binary system. The number(s) in parenthesis refer
to the literature source following:
1 = Vanderburg et al. (2016ApJ...827L..10V 2016ApJ...827L..10V)
2 = Lund et al. (2019AJ....158..248L 2019AJ....158..248L)
3 = Bryant et al. (2021MNRAS.504L..45B 2021MNRAS.504L..45B)
4 = Stello et al. (2016ApJ...832..133S 2016ApJ...832..133S)
5 = Giguere et al. (2015ApJ...799...89G 2015ApJ...799...89G)
6 = Ment et al. (2018AJ....156..213M 2018AJ....156..213M, Cat. J/AJ/156/213)
7 = Grunblatt (2019AJ....158..227G 2019AJ....158..227G, Cat. J/AJ/158/227)
8 = Washington Double Star Catalog (Mason et al., 2001AJ....122.3466M 2001AJ....122.3466M,
Cat. B/wds)
9 = Ong et al. (2021ApJ...922...18O 2021ApJ...922...18O)
10 = Pope et al. (2016MNRAS.461.3399P 2016MNRAS.461.3399P)
11 = Kruse et al. (2019ApJS..244...11K 2019ApJS..244...11K, Cat. J/ApJS.244/11)
12 = Robinson et al. (2007ApJ...670.1391R 2007ApJ...670.1391R)
13 = North et al. (2017MNRAS.472.1866N 2017MNRAS.472.1866N)
14 = Pourbaix et al. (2004A&A...424..727P 2004A&A...424..727P, Cat. V/122)
15 = Griffin (2013Obs...133....1G 2013Obs...133....1G)
16 = Johnson et al. (2011ApJS..197...26J 2011ApJS..197...26J)
17 = Luhn et al. (2019AJ....157..149L 2019AJ....157..149L, Cat. J/AJ/157/149)
18 = Tamuz et al (2008A&A...480L..33T 2008A&A...480L..33T, Cat. J/A+A/480/L33)
19 = Moutou et al. (2011A&A...527A..63M 2011A&A...527A..63M, Cat. J/A+A/527/A63)
20 = Ginski et al. (2016MNRAS.457.2173G 2016MNRAS.457.2173G)
21 = Van Eylen et al. (2018MNRAS.478.4866V 2018MNRAS.478.4866V)
22 = Jones et al. (2021A&A...646A.131J 2021A&A...646A.131J, Cat. J/A+A/546/A131)
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 9 I9 -- EPIC EPIC identification number
11- 22 A12 -- Campaign K2 observing Campaign(s) (1)
24- 29 F6.3 mag Kpmag Kepler magnitude
31- 33 I3 uarcsec theta ? IRFM angular diameter
35 I1 uarcsec e_theta ? Uncertainty on IRFM angular diameter
37- 40 I4 K teffIRFM ? IRFM effective temperature
42- 44 I3 K e_teffIRFM ? Uncertainty on IRFM effective temperature
46- 49 I4 K teffSPC ? SPC effective temperature
51- 53 I3 K e_teffSPC ? Uncertainty on SPC effective temperature
55- 59 F5.3 [cm/s2] logg ? Log SPC surface gravity
61- 65 F5.3 [cm/s2] e_logg ? Uncertainty on log SPC surface gravity
67- 72 F6.3 [Sun] [Fe/H] ? SPC metallicity
74- 78 F5.3 [Sun] e_[Fe/H] Uncertainty on SPC metallicity
80- 85 F6.3 km/s vsini ? SPC projected rotation velocity
87- 91 F5.3 km/s e_vsini ? Uncertainty on SPC projected rotation
velocity
93-100 F8.3 km/s RVLOS ? SPC radial velocity
102-107 F6.3 km/s e_RVLOS ? Uncertainty on SPC radial velocity
109-111 A3 -- Notes Notes on cluster membership and
non-standard spectroscopic and
astrometric inputs (2)
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Note (1): No seismic detections were made from individual campaigns followed
by an asterisk (*). An "A" indicates that seismic values are based
on the combined data from all campaigns.
Note (2): Notes as follows:
a = Star is member of M67
b = Spectroscopic parameters from APOGEE DR16 (Jonsson et al.,
2020AJ....160..120J 2020AJ....160..120J, Cat. III/284)
c = Spectroscopic parameters from Luck (2017AJ....153...21L 2017AJ....153...21L, Cat. J/AJ/153/21),
uncertainty on [Fe/H] assigned based on spread from the
Geneva-Copenhagen Survey (Casagrande et al., 2011A&A...530A.138C 2011A&A...530A.138C,
Cat. J/A+A/530/A138)
d = Using average metallicity from the Geneva-Copenhagen Survey
(Casagrande et al., 2011A&A...530A.138C 2011A&A...530A.138C, Cat. J/A+A/530/A138)
e = RV from Gaia DR2 (Soubiran et al., 2018A&A...616A...7S 2018A&A...616A...7S, cat. J/A+A/616/A7)
f = Poor 2MASS-EDR3 cross-match
g = High photbprpexcessfactor on Gaia photometry
h = Poor 2MASS photometry
* = SPC has poor Quality Factor
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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- 9 I9 -- EPIC PIC identification number
11- 12 A2 -- Campaign K2 observing Campaign (1)
14- 21 F8.3 uHz numaxCV ? numax from CV method (2)
23- 28 F6.3 uHz e_numaxCV ? Uncertainty on numax from CV method (2)
30- 36 F7.3 uHz dnuCV ? dnu from CV method (2)
38- 42 F5.3 uHz e_dnuCV ? Uncertainty on dnu from CV method (2)
44- 51 F8.3 uHz numaxSYD ? numax from SYD method (3)
53- 60 F8.3 uHz e_numaxSYD ? Uncertainty on numax from SYD method (3)
62- 68 F7.3 uHz dnuSYD ? dnu from SYD method (3)
70- 74 F5.3 uHz e_dnuSYD ? Uncertainty on dnu from SYD method (3)
76- 83 F8.3 uHz numaxTACO ? numax from TACO/OCT method (4)
85- 90 F6.3 uHz e_numaxTACO ? Uncertainty on numax from TACO/OCT
method (4)
92- 98 F7.3 uHz dnuTACO ? dnu from TACO/OCT method (4)
100-104 F5.3 uHz e_dnuTACO ? Uncertainty on dnu from TACO/OCT method (4)
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Note (1): An "A" indicates the combination of data from all available campaigns.
Note (2): Coefficient of Variation method by Bell et al. (2019MNRAS.482..616B 2019MNRAS.482..616B,
Cat. J/MNRAS/482/616) and Viani et al. (2019ApJ...879...33V 2019ApJ...879...33V)
Note (3): Coefficient of Variation method by Sydney Pipeline by Huber et al.
(2009; 2009CoAst.160...74H 2009CoAst.160...74H)
Note (4): Coefficient of Variation method by
TACO/OCT = Tools for the Automated Characterisation of Oscillations
(TACO) by Hekker et al. in prep) and the OCT/Octave code by
Hekker (2010MNRAS.402.2049H 2010MNRAS.402.2049H)
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Byte-by-byte Description of file: refs.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- Ref Reference number
4- 22 A19 --- BibCode BibCode
24- 40 A17 --- Aut Author's name
42- 83 A42 --- Com Comments
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Acknowledgements:
Mikkel Lund, mikkelnl(at)phys.au.dk
(End) Mikkel N. Lund [Aarhus Univ., DK], Patricia Vannier [CDS] 24-May-2024