J/ApJ/916/77 K2 rotation periods for SDSS & Gaia M dwarfs (Popinchalk+, 2021)
Evaluating rotation periods of M dwarfs across the ages.
Popinchalk M., Faherty J.K., Kiman R., Gagne J., Curtis J.L., Angus R.,
Cruz K.L., Rice E.L.
<Astrophys. J., 916, 77 (2021)>
=2021ApJ...916...77P 2021ApJ...916...77P
ADC_Keywords: Stars, M-type; Cross identifications; Radial velocities;
Photometry; Optical; Proper motions; Parallaxes, trigonometric;
Extinction; Spectral types
Keywords: Stellar rotation ; M dwarf stars ; Stellar kinematics ;
Stellar associations ; Stellar magnetic fields ; Light curves
Abstract:
In this work we examine M dwarf rotation rates at a range of ages to
establish benchmarks for M dwarf gyrochronology. This work includes a
sample of 713 spectroscopically classified M0-M8 dwarfs with new
rotation rates measured from K2 light curves. We analyze data and
recover rotation rates for 179 of these objects. We add these to
rotation rates for members of clusters with known ages (5-700Myr), as
well as objects assumed to have field ages (≳1Gyr). We use Gaia DR2
parallax and (G-GRP) photometry to create color-magnitude diagrams
to compare objects across samples. We use color-period plots to
analyze the period distributions across age, as well as incorporate
Hα equivalent width and tangential velocity where possible to
further comment on age dependence. We find that the age of transition
from rapid to slow rotation in clusters, which we define as an elbow
in the period-color plots, depends on spectral type. Later spectral
types transition at older ages: M4 for Praesepe at ∼700Myr, one of the
oldest clusters for which M dwarf rotation rates have been measured.
The transition from active to inactive Hα equivalent width also
occurs at this elbow, as objects transition from rapid rotation to the
slowly rotating sequence. Redder or smaller stars remain active at
older ages. Finally, using Gaia kinematics we find evidence for
rotation stalling for late Ms in the field sample, suggesting the
transition happens much later for mid- to late-type M dwarfs.
Description:
We begin by cross-matching the MLSDSS sample from
Kiman+ (2019, J/AJ/157/231) with K2. This allows us to recover
713 M dwarfs, which we use to define the K2SDSS sample (see Table 1).
It includes objects from 14 K2 campaigns.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 170 713 K2SDSS sample
table3.dat 150 8296 Literature rotation catalog
table4.dat 70 8948 Corrected Gaia DR2 photometry
table5.dat 34 860 Measured rotation rates for light curves of
objects in K2SDSS
table6.dat 22 180 Final rotation rates for objects in K2SDSS sample
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See also:
III/198 : Palomar/MSU nearby star spectroscopic survey (Hawley+ 1997)
IV/34 : K2 Ecliptic Plane Input Catalog (EPIC) (Huber+, 2017)
I/345 : Gaia DR2 (Gaia Collaboration, 2018)
V/154 : Sloan Digital Sky Surveys (SDSS), Release 16 (DR16) (Ahumada+, 2020)
J/A+A/327/1039 : Structure and evolution of low-mass stars (Chabrier+ 1997)
J/A+A/397/147 : Activity-rotation relationship in stars (Pizzolato+ 2003)
J/A+A/430/1005 : VRIHα photometry of NGC 2264 variables (Lamm+, 2005)
J/MNRAS/370/954 : VRIHalpha photometry of M34 (Irwin+, 2006)
J/AJ/133/2258 : Activity and kinematics of ultracool dwarfs (Schmidt+, 2007)
J/MNRAS/384/675 : Monitoring low-mass stars in NGC 2362 (Irwin+ 2008)
J/MNRAS/383/1588 : VIc photometry of NGC 2547 low-mass stars (Irwin+, 2008)
J/ApJ/687/1264 : Age estimation for solar-type dwarfs (Mamajek+, 2008)
J/AJ/135/785 : SDSS-DR5 low-mass star spectroscopic sample (West+, 2008)
J/AJ/137/1 : PMs and astrometry of late-type dwarfs (Faherty+, 2009)
J/ApJ/691/342 : griBVI photometry in M37 (Hartman+, 2009)
J/MNRAS/392/1456 : VIc phot. of M50 (NGC 2323) low-mass stars (Irwin+, 2009)
J/A+A/515/A100 : VI light curves of NGC 1039 solar-type stars (James+, 2010)
J/MNRAS/402/620 : SDSS WD main-sequence binaries (Rebassa-Mansergas+, 2010)
J/ApJ/733/L9 : Stellar rotation for 71 NGC 6811 members (Meibom+, 2011)
J/ApJ/733/115 : Rotation periods and membership in M34 (Meibom+, 2011)
J/AJ/141/97 : SDSS DR7 M dwarfs (West+, 2011)
J/MNRAS/432/1203 : Rotation periods of M-dwarf stars (McQuillan+, 2013)
J/ApJ/795/161 : Activity & rotation in Praesepe & Hyades (Douglas+, 2014)
J/ApJS/211/24 : Rotation periods of Kepler MS stars (McQuillan+, 2014)
J/MNRAS/454/593 : Young moving groups in solar neighbourhood (Bell+, 2015)
J/ApJ/807/45 : Habitable planet search around M dwarfs (Dressing+, 2015)
J/ApJ/810/158 : M,L,T dwarfs fundamental param. and SEDs (Filippazzo+, 2015)
J/ApJ/804/64 : Empirical and model parameters of 183 M dwarfs (Mann+, 2015)
J/AJ/149/158 : The BUD sample. I. L dwarf activity sample (Schmidt+, 2015)
J/ApJ/812/3 : MEarth mid-to-late M dwarfs rot. & kinematics (West+, 2015)
J/ApJS/225/10 : Kinematic analysis of M7-L8 dwarfs (Faherty+, 2016)
J/ApJ/833/281 : Candidate rotating M dwarfs from PS1-MDS (Kado-Fong+, 2016)
J/ApJ/821/93 : Rot. & Galactic kinematics of mid M dwarfs (Newton+, 2016)
J/AJ/152/113 : Pleiades members with K2 LCs. I. Periods (Rebull+, 2016)
J/ApJ/842/83 : Praesepe members rot. periods from K2 LCs (Douglas+, 2017)
J/ApJ/834/85 : Hα emission in nearby M dwarfs (Newton+, 2017)
J/ApJ/862/33 : Expanded membership catalog for NGC752 (Agueros+, 2018)
J/AJ/156/217 : Stellar param. for M dwarfs in MEarth-South (Newton+, 2018)
J/AJ/155/196 : K2 LCs for members of USco & ρ Oph (Rebull+, 2018)
J/AJ/156/275 : Rot. evolution of young, binary M dwarfs (Stauffer+, 2018)
J/ApJ/879/49 : Rot. periods for Gaia members of NGC 6811 (Curtis+, 2019)
J/A+A/621/A126 : CARMENES input catalog of M dwarfs. IV. (Diez Alonso+ 2019)
J/ApJ/879/100 : K2 periods for Hyades & Praesepe members (Douglas+, 2019)
J/AJ/158/75 : Mid-type M dwarfs planets (Hardegree-Ullman+, 2019)
J/ApJ/881/9 : EvryFlare. I. Cool stars's flares (Howard+, 2019)
J/AJ/157/231 : MLSDSS-GaiaDR2 sample of M and L dwarfs (Kiman+, 2019)
J/ApJ/878/21 : Vertical motions of red clump stars (Ting+, 2019)
J/AJ/160/90 : Stellar parameters for 13196 Kepler dwarfs (Angus+, 2020)
J/ApJ/904/140 : R147 members & rot. data for 5 other cl. (Curtis+, 2020)
J/ApJ/903/96 : MUTA; the µTau Association (Gagne+, 2020)
J/ApJ/895/140 : EvryFlare. II. 122 cool flare stars (Howard+, 2020)
J/AJ/161/277 : Sample of 45 HαEW outliers (Kiman+, 2021)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 19 A19 --- SDSS SDSS identifier
21- 29 I9 --- EPIC [60017812/251812050] EPIC identifier
31- 49 I19 --- Gaia Gaia DR2 source identifier
51- 52 A2 --- SpT Spectral type (1)
54- 59 F6.2 0.1nm EW [-4/236] Hα equivalent width; in Å (1)
61- 64 F4.2 0.1nm e_EW [0/9]? Uncertainty in EW
66- 71 F6.1 km/s RVel [-341/206]? Radial velocity (1)
73- 76 F4.1 km/s e_RVel [1/54]? Uncertainty in RVel
78- 91 F14.10 deg RAdeg Gaia DR2 Right Ascension (ICRS) at Epoch=2015.5
93- 106 F14.10 deg DEdeg [-11/26.1] Gaia DR2 Declination (ICRS) at
Epoch=2015.5
108- 115 F8.3 mas/yr pmRA [-330/340] Gaia DR2 proper motion along RA
117- 121 F5.3 mas/yr e_pmRA [0.08/3.5] Uncertainty in pmRA
123- 130 F8.3 mas/yr pmDE [-580/184] Gaia DR2 proper motion along DE
132- 136 F5.3 mas/yr e_pmDE [0.047/2.1] Uncertainty in pmDE
138- 143 F6.3 mag Gmag [14.32/20.68] Mean Gaia DR2 G band magnitude
145- 150 F6.3 mag Bpmag [15.94/22.26] Mean Gaia DR2 Blue passband
magnitude
152- 157 F6.3 mag Rpmag [13.03/18.98] Mean Gaia DR2 Red passband
magnitude
159- 164 F6.3 mas plx [1/54] Gaia DR2 parallax
166- 170 F5.3 mas e_plx [0.04/1.7] Uncertainty in plx
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Note (1): From SDSS spectra calculated by West+ (2011, J/AJ/141/97) and
Schmidt+ (2015, J/AJ/149/158).
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Byte-by-byte Description of file: table3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 19 I19 --- Gaia Gaia DR2 source identifier
21- 40 F20.16 deg RAdeg Right Ascension (ICRS) at Ep=2015.5
42- 64 F23.19 deg DEdeg Declination (ICRS) at Ep=2015.5
66- 74 F9.3 mas/yr pmRA [-2064/1747] Gaia DR2 proper motion along RA
76- 80 F5.3 mas/yr e_pmRA [0.02/1.4] Uncertainty in pmRA
82- 90 F9.3 mas/yr pmDE [-2416/1685] Gaia DR2 proper motion along DE
92- 96 F5.3 mas/yr e_pmDE [0.02/1.1] Uncertainty in pmDE
98- 103 F6.3 mag Gmag [4.5/19.9] Gaia DR2 mean G band magnitude
105- 110 F6.3 mag Bpmag [4.4/21.8]? Gaia DR2 mean blue passband
magnitude
112- 117 F6.3 mag Rpmag [4.6/18.2] Gaia DR2 mean red passband magnitude
119- 125 F7.3 arcsec plx [0.3/336.2] Gaia DR2 parallax
127- 131 F5.3 arcsec e_plx [0.01/0.8] Uncertainty in plx
133- 140 A8 --- Memb Member identifier (1)
142- 150 F9.5 d Per [0/208]? Rotational period
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Note (1): Member as follows:
ngc2547 = NGC 2547; Irwin+ 2008, J/MNRAS/383/1588 (150 occurrences),
ngc2362 = NGC 2362; Irwin+ 2008, J/MNRAS/384/675 (48 occurrences),
m34 = M34; Irwin+ 2006, J/MNRAS/370/954 ; James+ 2010, J/A+A/515/A100
and Meibom+ 2011, J/ApJ/733/115 (90 occurrences),
m37 = M37; Hartman+ 2009, J/ApJ/691/342 (59 occurrences),
m50 = M50; Irwin+ 2009, J/MNRAS/392/1456 (132 occurrences),
hyades = Hyades; Douglas+ 2019, J/ApJ/879/100 (203 occurrences),
plei = Pleiades; Rebull+ 2016, J/AJ/152/113 (661 occurrences),
prae = Praesepe; Douglas+ 2017, J/ApJ/842/83 (589 occurrences),
roph = ρ Ophiuchus; Rebull+ 2018, J/AJ/155/196 (117 occurrences),
usco = Upper Scorpius; Rebull+ 2018, J/AJ/155/196 (921 occurrences).
Field star samples (see Section 2.2.2) as follows:
kepler = Kepler; McQuillan+ 2014, J/ApJS/211/24 (4337 occurrences),
mearth = MEarth North (Newton+ 2016, J/ApJ/821/93) and
South (Newton+ 2018, J/AJ/156/217)(725 occurrences),
carmenes = CARMENES; Diez Alonso+ 2019, J/A+A/621/A126 (113 occurrences),
ps1-mds = the Pan-STARRS1 Medium-Deep Survey; Kado-Fong+ 2016, J/ApJ/833/281
(78 occurrences),
evry = Evryscope; Howard+ 2020, J/ApJ/895/140 (73 occurrences),
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Byte-by-byte Description of file: table4.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 19 I19 --- Gaia Gaia DR2 source identifier
21- 25 F5.3 mag E(B-V) [0/0.6]? The (B-V) color excess
27- 31 F5.3 mag e_E(B-V) [0.006/0.2]? Uncertainty in E (B-V)
33- 37 F5.3 mag AG [0/1.21] Gaia G band extinction coefficient
39- 43 F5.3 mag ABp [0/1.63]? Gaia Blue passband extinction
coefficient
45- 49 F5.3 mag ARp [0/0.98] Gaia Red passband extinction coefficient
51- 56 F6.3 mag Gmag [4.28/20.7] Corrected Gaia DR2 G band magnitude
58- 63 F6.3 mag Bpmag [4.18/22.24]? Corrected Gaia DR2 Blue passband
magnitude
65- 70 F6.3 mag Rpmag [4.5/19] Corrected Gaia DR2 Red passband
magnitude
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 9 I9 --- EPIC [201252056/251812050] EPIC identifier
11- 12 I2 --- K2 [0/18] K2 campaign number
14- 19 F6.3 d Per1 [0.1/68.8] Strongest period
21- 26 F6.3 d Per2 [0.1/68.8] Second strongest period
28 I1 --- Q [0/9] Quality flag (1)
30- 34 A5 --- Notes Additional notes (2)
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Note (1): We considered light curves with a visual score of 0 or 1 to
represent the highest-quality signals in our sample.
Note (2): Note as follows:
irreg = irregular variation;
dd = double dip light curve.
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Byte-by-byte Description of file: table6.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 9 I9 --- EPIC [201384292/251407244] EPIC identifier
11- 16 F6.3 d Per [0.1/32.8] Rotational period (1)
18 I1 --- Q [0/1] Quality flag (2)
20 I1 --- Ap [0/2] Aperture flag (3)
22 I1 --- Bin [0/1] Binary flag (4)
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Note (1): This is intended to be the reported period, except in cases where
Bin is not 0, in which case multiple periods were found to be
likely stellar signals. See Section 3.2.2 and Table 7.
Note (2): From visual inspection of the light curve, and are described
in Section 3.
Note (3): A value of 1 is possible contamination due to other stars in the
light curve, 2 is likely contamination.
Note (4): A zero indicates a non-binary system.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 29-Dec-2022