J/MNRAS/499/3481 Metallicity and rotation in the Kepler field (Amard+, 2020)
Evidence for metallicity-dependent spin evolution in the Kepler field.
Amard L., Roquette J., Matt S.P.
<Mon. Not. R. Astron. Soc., 499, 3481-3493 (2020)>
=2020MNRAS.499.3481A 2020MNRAS.499.3481A (SIMBAD/NED BibCode)
ADC_Keywords: Stars, fundamental ; Stars, distances ; Abundances, [Fe/H] ;
Effective temperatures ; Stars, masses ; Optical
Keywords: stars: abundances - stars: evolution -
stars: fundamental parameters - stars: low-mass - stars: rotation
Abstract:
A curious rotation period distribution in the colour-magnitude-period
diagram (CMPD) of the Kepler field was recently revealed, thanks to
data from Gaia and Kepler spacecraft. It was found that redder and
brighter stars are spinning slower than the rest of the main sequence.
On the theoretical side, it was demonstrated that metallicity should
affect the rotational evolution of stars as well as their evolution in
the Hertzprung-Russel or colour-magnitude diagram. In this work, we
combine this data set with medium- and high-resolution spectroscopic
metallicities and carefully select main-sequence single stars in a
given mass range. We show that the structure seen in the CMPD also
corresponds to a broad correlation between metallicity and rotation,
such that stars with higher metallicity rotate, on average, more
slowly than those with low metallicity. We compare this sample to
theoretical rotational evolution models that include a range of
different metallicities. They predict a correlation between rotation
rate and metallicity that is in the same direction and of about the
same magnitude as that observed. Therefore, metallicity appears to be
a key parameter to explain the observed rotation period distributions.
We also discuss a few different ways in which metallicity can affect
the observed distribution of rotation period, due to observational
biases and age distributions, as well as the effect on stellar wind
torques.
Description:
We used the Gaia-Kepler catalogue as our starting point (Bedell 2018,
available at https://gaia-kepler.fun/), which includes entries for
201312 sources in the Kepler field and was produced by a
cross-matching between Data Release 25 Kepler Catalog and Gaia DR2
source catalogue, using a 1-arcsec radius for matching, and includes
the improved distance prescription from Bailer-Jones et al.
(2018AJ....156...58B 2018AJ....156...58B, Cat. I/347). We then excluded duplicate sources
and selected high-quality Gaia-DR2 data by requiring a parallax error
<0.1mas and (σm/m)<0.01 for every photometric band. Finally, we
merged this Gaia-Kepler sample with the rotation period measurements
from McQuillan et al. (2014ApJS..211...24M 2014ApJS..211...24M, Cat J/ApJS/211/24). This
process results in a sample of 28508 stars with good-quality Gaia DR2
data and measured Kepler rotation periods.
We searched the literature for measurements of [Fe/H] for stars in the
Kepler field that were based on mid- or high-resolution spectroscopy,
ultimately selecting the catalogues from the revised KIC, LAMOST, and
APOGEE.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
catalog.dat 189 28508 Full Gaia-Kepler-metallicity data base
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See also:
I/345 : Gaia DR2 (Gaia Collaboration, 2018)
V/133 : Kepler Input Catalog (Kepler Mission Team, 2009)
I/347 : Distances to 1.33 billion stars in Gaia DR2
(Bailer-Jones+, 2018)
J/ApJS/211/24 : Rotation periods of Kepler MS stars (McQuillan+, 2014)
III/284 : APOGEE-2 data from DR16 (Johnsson+, 2020)
J/AJ/155/181 : LAMOST/SP_Ace DR1 catalog (Boeche+, 2018)
J/A+A/594/A39 : LAMOST-Kepler parameters and activity indicators
(Frasca+, 2016)
J/ApJ/836/5 : Abundances of LAMOST giants from APOGEE DR12 (Ho+, 2017)
V/164 : LAMOST DR5 catalogs (Luo+, 2019)
J/ApJS/229/30 : Revised stellar properties of Q1-17 Kepler targets
(Mathur+, 2017)
J/ApJS/239/32 : APOKASC-2 catalog of Kepler evolved stars
(Pinsonneault+, 2018)
Byte-by-byte Description of file: catalog.dat
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Bytes Format Units Label Explanations
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1- 8 A8 --- --- [Gaia DR2]
10- 28 I19 --- GaiaDR2 Gaia DR2 source identifier
30- 37 I8 --- ID Alternative identifier
39- 45 F7.3 deg RAdeg Right ascension (ICRS) at Ep=2015.5
47- 53 F7.4 deg DEdeg Declination (ICRS) at Ep=2015.5
55- 62 F8.5 mag Gmag Gaia DR2 G-band magnitude
64- 72 F9.6 mag BP-G Gaia DR2 BP-G colour
74- 82 F9.6 mag GMAG Absolute G-band magnitude (1)
84- 93 F10.4 pc rest Estimated distance from Bailer-Jones et al.
(2018AJ....156...58B 2018AJ....156...58B, Cat. I/347)
95- 102 I8 --- KIC KIC identifier
104- 109 F6.3 d Prot Rotational period from McQuillan et al.
(2014ApJS..211...24M 2014ApJS..211...24M, Cat J/ApJS/211/24)
111- 116 F6.3 d e_Prot Error on Prot
118- 126 F9.6 [-] [Fe/H] ? Fe/H abundance ratio
128- 135 F8.6 [-] e_[Fe/H] ? Error on [Fe/H]
137- 143 A7 --- r_[Fe/H] ? Reference for [Fe/H] (2)
145- 152 F8.3 K Teff ? Effective temperature
154- 161 F8.3 K e_Teff ? Error on Teff
163- 169 A7 --- r_Teff ? Reference for Teff (2)
171- 178 F8.6 Msun Mass ? Star mass
180- 187 F8.6 Msun e_Mass ? Error on Mass
189 I1 --- MScut ? Flag indicating that the star is selected to
be part of the final sample of 4055 stars (3)
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Note (1): We converted Gaia apparent magnitudes into absolute magnitudes
(MG=G-5log10(dBJ18/10)) by using the distances from
Bailer-Jones et al. (2018AJ....156...58B 2018AJ....156...58B, Cat. I/347) as a substitute
to a simple inversion of Gaia parallaxes to obtain distances
Note (2): Reference as follows:
APtc = APOGEE Data and Spectral Analysis from SDSS Data Release 16
Jonsson et al. (2020AJ....160..120J 2020AJ....160..120J, Cat. III/284)
B18 = Boeche et al. (2018AJ....155..181B 2018AJ....155..181B, Cat. J/AJ/155/181)
F16 = Frasca et al. (2016A&A...594A..39F 2016A&A...594A..39F, Cat. J/A+A/594/A39)
H17 = Ho et al. (2017ApJ...836....5H 2017ApJ...836....5H, Cat. J/ApJ/836/5)
LaDR5re = LAMOST DR5 (Luo et al. 2019yCat.5164....0L 2019yCat.5164....0L, Cat. V/164)
M17 = Mathur et al. (2017ApJS..229...30M 2017ApJS..229...30M, Cat. J/ApJS/229/30)
P18 = Pinsonneault et al. (2018ApJS..239...32P 2018ApJS..239...32P, Cat. J/ApJS/239/32)
Note (3): In order to focus our study on single, main-sequence stars, we made
cuts to the data, based on distance and photometric binarity. The
final sample consists of 4055 single main-sequence stars.
See Section 2.2 of the articles for details.
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History:
From electronic version of the journal
(End) Ana Fiallos [CDS] 06-Sep-2023