J/MNRAS/520/5283 Rotation periods and ages of cool host stars (Gaidos+, 2023)
The TIME Table: rotation and ages of cool exoplanet host stars.
Gaidos E., Claytor Z., Dungee R., Ali A., Feiden G.A.
<Mon. Not. R. Astron. Soc. 520, 5283-5304 (2023)>
=2023MNRAS.520.5283G 2023MNRAS.520.5283G (SIMBAD/NED BibCode)
ADC_Keywords: Stars, variable ; Exoplanets ; Stars, ages ; Stars, M-type ;
Stars, K-type ; Stars, late-type ; Abundances, [Fe/H] ;
Effective temperatures ; Combined data ; References ;
Photometry ; Spectroscopy ; Optical
Keywords: exoplanets - stars: evolution - stars: late-type - stars: low-mass -
planetary systems - stars: rotation
Abstract:
Age is a stellar parameter that is both fundamental and difficult to
determine. Among middle-aged M dwarfs, the most prolific hosts of
close-in and detectable exoplanets, gyrochronology is the most
promising method to assign ages, but requires calibration by
rotation-temperature sequences (gyrochrones) in clusters of known
ages. We curated a catalogue of 249 late K- and M-type
(Teff=3200-4200K) exoplanet host stars with established rotation
periods, and applied empirical, temperature-dependent rotation-age
relations based on relevant published gyrochrones, including one
derived from observations of the 4-Gyr-old open cluster M67. We
estimated ages for 227 of these stars, and upper limits for eight
others, excluding 14 which are too rapidly rotating or are otherwise
outside the valid parameter range of our gyrochronology. We estimated
uncertainties based on observed scatter in rotation periods in young
clusters, error in the gyrochrones, and uncertainties in temperature
and non-solar metallicity. For those stars with measured
metallicities, we provide but do not incorporate a correction for the
effects of deviation from solar-metallicity. The age distribution of
our sample declines to near zero at 10 Gyr, the age of the Galactic
disc, with the handful of outliers explainable by large uncertainties.
Continued addition or extension of cluster rotation sequences to more
thoroughly calibrate the gyrochronology in time and temperature space,
more precise and robust measurement of rotation periods, and more
accurate stellar parameter measurements will enable continued
improvements in the age estimates of these important exoplanet host
stars.
Description:
In this work, we curate a catalogue of rotation periods of late K- and
early M-type dwarfs known to host validated or confi and apply
empirical rotation-age relations based on the M67 gyrochrone of Dungee
et al. (2022ApJ...938..118D 2022ApJ...938..118D, Cat. J/ApJ/938/118) and previously
published gyrochrones (Curtis et al. 2020ApJ...904..140C 2020ApJ...904..140C) to estimate
ages. The rotation periods of many host stars have been established
either using the same space-based photometry (i.e. Kepler, K2, TESS)
used to identify their transiting planets, or by data obtained from
the ground or space as part of the validation/confirmation of
candidate planets. There are also collections of rotation periods of
field stars (including planet hosts) based on data from Kepler (Santos
et al. 2019ApJS..244...21S 2019ApJS..244...21S, 2021ApJS..255...17S 2021ApJS..255...17S, Cat. J/ApJS/255/17,
Cat. J/ApJS/244/21), K2 (Reinhold & Hekker 2020A&A...635A..43R 2020A&A...635A..43R, Cat.
J/A+A/635/A43), TESS (Canto Martins et al. 2020ApJS..250...20C 2020ApJS..250...20C, Cat.
J/ApJS/250/20), and ground-based surveys (Newton et al.
2018AJ....156..217N 2018AJ....156..217N, Cat. J/AJ/156/217; Oelkers et al.
2018AJ....155...39O 2018AJ....155...39O, Cat. J/AJ/155/39; Christy et al.
2023MNRAS.519.5271C 2023MNRAS.519.5271C). We also identify additional candidate rotational
signatures directly in the photometric data sets. We emphasize that
some rotation periods are tentative and that very cool dwarf
gyrochronology is a work in progress and makes assumptions which will
be born out or refuted by future observations.
Mainly, we identified all host stars of validated or confirmed
exoplanets with Teff of 3200-4200K in the NASA Exoplanet Archive as of
2022 August. This included 112 Kepler host stars or KOIs having
rotation periods Prot in Santos et al. (2019ApJS..244...21S 2019ApJS..244...21S). From the
list of the non-Kepler host stars we removed evolved (giant), T Tauri,
and pre-main sequence (PMS) stars, as rotation of these stars
obviously does not follow the gyrochronology of dwarfs, as well as
members of star-forming regions and young-moving groups that have ages
estimated by other techniques, leaving 215 non-Kepler stars (i.e. see
section 2). We revisited the K2 data by matching all stars against the
EPIC catalogue of Huber et al. (2016ApJS..224....2H 2016ApJS..224....2H, Cat.
J/ApJS/224/2) and downloaded all PDCSAP light curves from the MAST
archive. The light curves were further de-trended with the best-fitting
second-order polynomial before a Lomb-Scargle analysis to search for
signals with periods. We retrieved light curves from the ZTF. We
obtained 319 ZTF light curves for 102 stars to analyse periods. Also,
we got ASAS-SN g- and V-band light curves of on which we performed a
similar analysis. Finally, we included Prot values determined from
time-series measurements of spectroscopic indicators of stellar
activity such as CaII, HK and Hα.
Secondly as explained in section 4, we estimated the age of each star
with an established P by comparing it to available empirical cluster
gyrochrones that include the Teff range of interest (i.e see equation
1). Allowing us to estimated ages by simple power-law interpolation
between gyrochrone calibration points (linear interpolation in a
log-log plot of period versus age). If the only available calibration
point was that of M67 (4 Gyr) then we calculate the age of the star
using equation (2). Monte Carlo (MC) realizations of these
calculations were performed to estimate the uncertainty in the age,
incorporating error in rotation period, stellar parameters, the
gyrochronology, and initial conditions as fully detailed in section 5.
Then for the 250 selected cool host stars, we resumed results in
table1.dat, for observational informations, stellar properties as
Teffs, Prots and Ages as well as their literature references.
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 148 250 Cool host stars with established rotation
periods
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See also:
J/MNRAS/519/5271 : New ASAS-SN variable stars using g band lcs (Christy+, 2023)
J/MNRAS/491/5216 : Rotation periods for 107 M dwarfs from APACHE
(Giacobbe+, 2020)
J/MNRAS/474/2094 : Inferring probabilistic stellar rotation periods
(Angus+, 2018)
J/MNRAS/457/2877 : Kepler M dwarf stars revised properties (Gaidos+, 2016)
J/MNRAS/436/1883 : Properties of KOI host stars (Walkowicz+, 2013)
J/MNRAS/411/2099 : Fast-rotating M-dwarf stars in NGC 2547 (Jeffries+, 2011)
J/A+A/658/A194 : Stellar parameters of 18 M dwarfs (Passegger+, 2022)
J/A+A/639/A127 : Age-chemical-clocks-metallicity relations (Casali+, 2020)
J/A+A/638/A20 : M dwarfs X-ray activity and rotation relations
(Magaudda+, 2020)
J/A+A/635/A43 : Stellar rotation periods from K2 Campaigns 0-18
(Reinhold+, 2020)
J/A+A/560/A4 : Rotation periods of active Kepler stars (Reinhold+, 2013)
J/ApJ/923/177 : TESS obs. & rotational periods of T Tauri in Orion
(Serna+, 2021)
J/ApJ/904/140 : Ruprecht 147 members & rot. data for 5 other cl.
(Curtis+, 2020)
J/ApJ/893/67 : Smoothed amplitudes from Kepler, K2 and TESS phot.
(Morris, 2020)
J/ApJ/888/43 : APOGEE-Kepler Cool Dwarf star ages determination
(Claytor+, 2020)
J/ApJ/879/100 : K2 rotation periods for Hyades & Praesepe members
(Douglas+, 2019)
J/ApJ/879/49 : Rotation periods for 171 Gaia members of NGC 6811
(Curtis+, 2019)
J/ApJ/871/174 : Kepler rapid rotators and Ks-band excesses (Simonian+, 2019)
J/ApJ/780/159 : Rotation-mass-age relationship of old field stars
(Epstein+, 2014)
J/ApJ/776/67 : Rotational tracks (van Saders+, 2013)
J/ApJS/255/17 : Surface rotation & activity for Kepler stars. II.
(Santos+, 2021)
J/ApJS/250/20 : Rotation periods in TESS objects of interest (TOIs)
(Canto+, 2020)
J/ApJS/224/2 : K2 EPIC stellar properties for 138600 targets (Huber+, 2016)
J/AJ/164/251 : ZTF measured rotational period of 40553 M- or G-dwarfs
(Lu+, 2022)
II/287 : Northern Sky Variability Survey (NSVS) (Wozniak+, 2004)
II/264 : ASAS Variable Stars in Southern hemisphere
(Pojmanski+, 2002-2005)
IV/34 : K2 Ecliptic Plane Input Catalog (EPIC) (Huber+, 2017)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 16 A16 --- Name Host star name
17- 18 A2 --- f_Name Binary flag as yes 32 times
19- 22 I4 K Teff Effective temperature
24- 28 F5.2 [Sun] [Fe/H] ? Iron to hydrogen abundance ratio
30- 35 F6.2 d Prot Rotation period
37- 41 F5.2 d e_Prot Rotatio period uncertainty
43- 44 A2 --- f_Prot Method for obtaining rotation period (1)
46- 50 F5.2 Gyr Age ? Estimated age
52- 56 F5.2 Gyr e_Age ? Age uncertainty
58- 62 F5.2 Gyr Agecorr ? Metallicity-dependent age correction
64 A1 --- Fail Flag for age assignment failure as yes 16 times
66 A1 --- Upper Flag for age upper limits as 9 times
68 A1 --- PMS Flag for pre-main sequence star as no 250 times
70 A1 --- n_Prot Flag for lack of a reported period error as
yes 20 times (2)
72- 85 A14 --- Inst Instrument key for rotation period (3)
87-148 A62 --- r_Prot Literrature reference for rotation period
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Note (1): Methods are labelles as follows:
P = Photometric, 220 occurences in our sample
S = Spectroscopy, 21 occurences in our sample
PS = Hybrid both P and S methods, 8 occurences in our sample
Note (2): If no error was reported than a value of 1 day was assumed
Note (3): Instrument keys are labelled as follows:
AN = All-Sky Automated Survey for Super-Novae (ASAS-SN),
4 occurences in our sample
AP = APACHE, 2 occurences in our sample
AS = All Sky Automated Survey (ASAS),
14 occurences in our sample
CA = CARMENES, 10 occurences in our sample
ES = ESPRESSO, 3 occurences in our sample
Ev = Evryscope, 1 occurences in our sample
Fa = Fairborn, 6 occurences in our sample
HA = HARPS, 25 occurences in our sample
HI = HIRES, 1 occurences in our sample
K2 = Kepler K2, 55 occurences in our sample
Ke = Kepler, 113 occurences in our sample
LC = Las Cumbres Observatory Global Telescope,
1 occurences in our sample
ME = MEarth, 7 occurences in our sample
NG = Next Generation Transit Survey, 1 occurences in our sample
NS = Northern Sky Variability Survey (NSVS),
3 occurences in our sample
OS = Observatorio de Sierra Nevada, 1 occurences in our sample
SN = Also in Stock et al. 2020A&A...643A.112S 2020A&A...643A.112S,
Cat. J/A+A/643/A112, 1 occurences in our sample
SP = SPIRou, 1 occurences in our sample
ST = STELLA, 1 occurences in our sample
TE = TESSr2014, 6 occurences in our sample
TJ = Telescope Joan Oro (TJO), 4 occurences in our sample
WA = Wide Angle Search for Planets (WASP),
12 occurences in our sample
ZT = ZTF Zwicky Transient Facility, 6 occurences in our sample
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History:
From electronic version of the journal
License: CC-BY-4.0 [see https://spdx.org/licenses/]
(End) Luc Trabelsi [CDS] 09-Apr-2026