J/A+A/684/A9 Rotation periods for 261 M dwarfs (Shan+, 2024)
The CARMENES input catalog of M dwarfs: VII. New rotation periods for the survey
stars and their correlations with stellar activity.
Shan Y., Revilla D., Skrzypinski S.L., Dreizler S., Bejar V.J.S.,
Caballero J.A., Cardona Guillen C., Cifuentes C., Fuhrmeister B.,
Reiners A., Vanaverbeke S., Ribas I., Quirrenbach A., Amado P.J.,
Aceituno F.J., Casanova V., Cortes-Contreras M., Dubois F., Gorrini P.,
Henning T., Herrero E., Jeffers S.V., Kemmer J., Lalitha S., Lodieu N.,
Logie L., Lopez Gonzalez M.J., Martin-Ruiz S., Montes D., Morales J.C.,
Nagel E., Palle E., Perdelwitz V., Perez-Torres M., Pollacco D., Rau S.,
Rodriguez-Lopez C., Rodriguez E., Schoefer P., Seifert W., Sota A.,
Zapatero Osorio M.R., Zechmeister M.
<Astron. Astrophys. 684, A9 (2024)>
=2024A&A...684A...9S 2024A&A...684A...9S (SIMBAD/NED BibCode)
ADC_Keywords: Stars, M-type ; Stars, nearby ; Photometry ; Optical
Keywords: techniques: photometric - stars: activity - stars: low-mass -
stars: rotation
Abstract:
Knowledge of rotation periods (Prot) is important for understanding
the magnetic activity and angular momentum evolution of late-type
stars, as well as for evaluating radial velocity signals of potential
exoplanets and identifying false positives.We measured photometric and
spectroscopic Prot for a large sample of nearby bright M dwarfs with
spectral types from M0 to M9, as part of our continual effort to fully
characterize the Guaranteed Time Observation programme stars of the
CARMENES survey.
We analyse light curves chiefly from the SuperWASP survey and TESS
data.We supplemented these with our own follow-up photometric
monitoring programme from ground-based facilities, as well as
spectroscopic indicator time series derived directly from the CARMENES
spectra.
From our own analysis, we determined Prot for 129 stars. Combined with
the literature, we tabulated Prot for 261 stars, or 75% of our sample.
We developed a framework to evaluate the plausibility of all periods
available for this sample by comparing them with activity signatures
and checking for consistency between multiple measurements. We find
that 166 of these stars have independent evidence that confirmed their
Prot. There are inconsistencies in 27 periods, which we classify as
debated. A further 68 periods are identified as provisional detections
that could benefit from independent verification. We provide an
empirical relation for the Prot uncertainty as a function of the Prot
value, based on the dispersion of the measurements. We show that
published formal errors seem to be often underestimated for periods
longwards of 10d. We examined rotation-activity relations with
emission in X-rays, H, CaII H&K, and surface magnetic field strengths
for this sample of M dwarfs. We find overall agreement with previous
works, as well as tentative differences in the partially versus fully
convective subsamples. We show Prot as a function of stellar mass,
age, and galactic kinematics. With the notable exception of three
transiting planet systems and TZ Ari, all known planet hosts in this
sample have Prot≳15d.
Inherent challenges in determining accurate and precise stellar Prot
means independent verification is important, especially for inactive M
dwarfs. Evidence of potential mass dependence in activity-rotation
relations would suggest physical changes in the magnetic dynamo that
warrants further investigation using larger samples of M dwarfs on
both sides of the fully convective boundary. Important limitations
need to be overcome before the radial velocity technique can be
routinely used to detect and study planets around young and active
stars.
Description:
We measured photometric and spectroscopic Prot for a large sample of
nearby bright M dwarfs with spectral types from M0 to M9, as part of
our continual effort to fully characterize the Guaranteed Time
Observation programme stars of the CARMENES survey. We determined Prot
for 129 stars. Combined with the literature, we tabulated Prot for 261
stars, or 75% of our sample. We evaluate the plausibility of all
periods available for this sample by comparing them with activity
signatures and checking for consistency between multiple measurements.
We find that 166 of these stars have independent evidence that
confirmed their Prot. There are inconsistencies in 27 periods, which
we classify as debated. A further 68 periods are identified as
provisional detections that could benefit from independent
verification. We provide an empirical relation for the Prot
uncertainty as a function of the Prot value, based on the dispersion
of the measurements. We show that published formal errors seem to be
often underestimated for periods ≳10d. We highlight the
importance of independent verification on Prot measurements,
especially for inactive M dwarfs. We examined rotation-activity
relations with emission in X-rays, Halpha, CaII H & K, and surface
magnetic field strengths. We find overall agreement with previous
works, as well as tentative differences in the partially versus fully
convective subsamples. We show Prot as a function of stellar mass,
age, and galactic kinematics. With the notable exception of three
transiting planet systems and TZ Ari, all known planet hosts in this
sample have Prot ≳15d. This indicates that important limitations need
to be overcome before the radial velocity technique can be routinely
used to detect and study planets around young and active stars.
tablec1.dat presents the basic stellar properties for the CARMENES
survey sample considered in this work. They include fundamental
stellar parameters, computed Rossby number, rotational velocity,
activity indicators, age, and kinematic disk membership. The adopted
best rotation periods as judged by this work are also given here.
tablec2.dat presents all measured rotation periods assessed for the
sample stars. They include both literature values and those derived in
this work.
tablec4.dat tabulates information on all known planet systems in this
sample, including the planetary orbital periods and mpsini's.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablec1.dat 190 348 Properties and best Prots for 348 M dwarfs
tablec2.dat 266 348 All rotation periods considered for 348 M dwarfs
tablec4.dat 184 63 Planet information for 63 planet hosts in sample
refs.dat 76 115 References
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See also:
J/A+A/577/A128 : CARMENES input cat. of M dwarfs. I (Alonso-Floriano+, 2015)
J/A+A/597/A47 : CARMENES input cat. of M dwarfs, II (Cortes-Contreras+ 2017)
J/A+A/614/A76 : CARMENES input cat. of M dwarfs. III (Jeffers+, 2018)
J/A+A/621/A126 : CARMENES input cat. of M dwarfs. IV (Diez Alonso+ 2019)
J/A+A/642/A115 : CARMENES input cat. of M dwarfs. V (Cifuentes+, 2020)
J/A+A/652/A116 : CARMENES time-resolved CaII H&K catalog (Perdelwitz+, 2021)
Byte-by-byte Description of file: tablec1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 11 A11 --- Karmn CARMENES identifier (JHHMMm+DDdA)
13- 18 A6 --- SpType Spectral type (1)
20- 26 F7.2 d Pbest ? Best rotation period (Prot)
28- 33 A6 --- r_Pbest Reference for Pbest (2)
35 A1 --- SPD [SPD] Prot secure flag (G1)
37- 42 F6.2 mag Vmag ? V-magnitude (4)
44- 48 F5.2 mag Kmag Ks-magnitude (4)
50- 53 F4.2 Msun Mstar Stellar mass in solar units
55- 58 F4.2 [d] logtau log(tau_conv/d): convective overturn time
60- 64 F5.2 [-] logRo ? log(Rossby number)
66 A1 --- l_vsini [=<] vsini flag
('=': measured,'<': upper limit) (5)
68- 72 F5.1 km/s vsini ? vsini: projected rotational velocity (5)
74- 77 F4.1 km/s e_vsini ? Error in vsini
79- 84 A6 --- r_vsini vsini reference (5)
86- 90 F5.2 Rsun Rstar ? Stellar radius in solar units
92- 97 F6.2 d Pmax ? Upper limit in Prot from vsini and Rstar
99-105 F7.2 d e_Pmax ? 1-sig upper limit in Pmax
107-112 F6.2 0.1nm pEWHa ? Halpha pseudo-equivalent width
in Angstroems (6)
114-118 F5.2 0.01Lsun Lstar Stellar luminosity (in units of 0.01 Lsun)
120-124 F5.2 [-] logLX ? log10(LX/Lbol):
normalised X-ray luminosity (7)
126-131 F6.3 [-] e_logLX ? Error in logLX (7)
133-137 F5.2 [-] logLHa ? log10(LHa/Lbol):
normalized Halpha luminosity (8)
139-145 F7.3 [-] e_logLHa ? Error in logLHa (8)
147-151 A5 --- r_logHa LHalpha reference (8)
153-157 F5.2 [-] logRhk ? log10(R'hk):
normalized Ca II H&K luminosity
159-164 F6.3 [-] e_logRhk ? Error in logRhk
166-170 F5.2 [G] logB ? log10(B):
average surface magnetic field (9)
172-177 F6.3 [G] e_logB ? Error in logB (9)
179-181 A3 --- SB Spectroscopic binary flag (10)
183-185 I3 Myr Age Age (800 Myr is upper limit) (11)
187-190 A4 --- Kin Kinematic disk membership (12)
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Note (1): Spectral types from Alonso-Floriano et al.
(2015A&A...577A.128A 2015A&A...577A.128A, Cat. J/A+A/577/A128)
Note (2): References in refs.dat file.
Note (4): V and Ks magnitudes from Cifuentes et al.
(2020A&A...642A.115C 2020A&A...642A.115C, Cat. J/A+A/642/A115)
Note (5): Projected rotational velocities (vsini) from Reiners et al.
(2022A&A...662A..41R 2022A&A...662A..41R, Cat. J/A+A/662/A41) or Reiners et al.
(2018A&A...612A..49R 2018A&A...612A..49R, Cat. J/A+A/612/A49), except J04173+088 from
Kesseli et al. (2018AJ....155..225K 2018AJ....155..225K, Cat. J/AJ/155/225).
Note (6): Halpha pseudo-equivalent widths from Schoefer et al.
(2019A&A...623A..44S 2019A&A...623A..44S, Cat. J/A+A/623/A44)
Note (7): X-ray luminosity from Voges et al. (1999A&A...349..389V 1999A&A...349..389V, Cat. IX/10)
Note (8): Normalised Halpha luminosity from Newton et al. (2017ApJ...834...85N 2017ApJ...834...85N,
Cat. J/ApJ/834/85) or Schoefer et al. (2019A&A...623A..44S 2019A&A...623A..44S, Cat. J/A+A/623/A44)
all LHa/Lbol from Schoefer et al. (2019A&A...623A..44S 2019A&A...623A..44S) are converted onto
Newton et al. (2017ApJ...834...85N 2017ApJ...834...85N) scale via:
log(LHa/Lbol)New17scale = -0.943 + 0.768 log(LHa/Lbol)_Sch19
Note (9): Surface magnetic field strengths from Reiners et al.
(2022A&A...662A..41R 2022A&A...662A..41R, Cat. J/A+A/662/A41)
Note (10): Spectroscopic binary status from Baroch et al. (2018A&A...619A..32B 2018A&A...619A..32B,
Cat. J/A+A/619/A32) and Baroch et al. (2021A&A...653A..49B 2021A&A...653A..49B).
Note (11): Ages from Cardona et al. (submitted).
Note (12): Kinematic disk membership assignments from Cortes-Contreras et al.
(in prep).
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Byte-by-byte Description of file: tablec2.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 11 A11 --- Karmn CARMENES identifier (JHHMMm+DDdA)
13- 19 F7.2 d Pbest ? Best rotation period (Prot)
21- 29 A9 --- r_Pbest Reference for Pbest, in refs.dat file
31 A1 --- SPD [SPD] Prot secure flag (G1)
33- 39 F7.2 d P1 ? Rotation period (Prot) 1
41- 46 F6.2 d e_P1 ? Error on Prot 1
48- 56 A9 --- r_P1 Reference 1, in refs.dat file
58- 64 F7.2 d P2 ? Prot 2
66- 71 F6.2 d e_P2 ? Error on Prot 2
73- 81 A9 --- r_P2 Reference 2, in refs.dat file
83- 89 F7.2 d P3 ? Prot 3
91- 96 F6.2 d e_P3 ? Error on Prot 3
98-106 A9 --- r_P3 Reference 3, in refs.dat file
108-114 F7.2 d P4 ? Prot 4
116-121 F6.2 d e_P4 ? Error on Prot 4
123-131 A9 --- r_P4 Reference 4, in refs.dat file
133-139 F7.2 d P5 ? Prot 5
141-145 F5.2 d e_P5 ? Error on Prot 5
147-151 A5 --- r_P5 Reference 5, in refs.dat file
153-158 F6.1 d P6 ? Prot 6
160-164 F5.1 d e_P6 ? Error on Prot 6
166-174 A9 --- r_P6 Reference 6, in refs.dat file
176-181 F6.2 d P7 ? Prot 7
183-187 F5.2 d e_P7 ? Error on Prot 7
189-193 A5 --- r_P7 Reference 7, in refs.dat file
195-201 F7.2 d Pplanet ? Prot from planet discovery/analysis paper
203-208 A6 --- r_Pplanet Reference for planet paper, in refs.dat file
210-216 F7.2 d PLaf21 ? Prot from Lafarga et al.
(2021A&A...652A..28L 2021A&A...652A..28L, Cat. J/A+A/652/A28)
218-223 F6.2 d Pop ? Prot from other photometry facilities
225-234 A10 --- Facility Name of photometry facility and passband
236-241 F6.2 d PTESS ? Prot from TESS light curves
243-248 A6 --- methodTESS TESS light curve version (PDCSAP, SAP, FFI)
250-256 F7.2 d PSWASP ? Prot from SuperWASP light curves
258 A1 --- u_PSWASP [U] SuperWASP uncertainty flag
260-266 F7.2 d PSpect ? Prot from spectroscopic indicator
time series
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Byte-by-byte Description of file: tablec4.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 11 A11 --- Karmn CARMENES identifier (JHHMMm+DDdA)
13- 16 F4.2 Msun Mstar Stellar mass in solar units
18- 24 F7.2 d Prot ? Rotation period
26 A1 --- SPD [SPD] Prot secure flag (G1)
28 A1 --- TransFlag [Y] Transiting system flag
30- 37 F8.3 d Porb1 Orbital period planet 1
39- 45 F7.2 Me mpsini1 ? mp*sini of planet 1 in earth masses
47- 58 A12 --- Ref1 Reference for planet 1
60- 67 F8.2 d Porb2 ? Orbital period planet 2
69- 75 F7.2 Me mpsini2 ? mp*sini of planet 2
77- 87 A11 --- Ref2 Reference for planet 2
89- 94 F6.2 d Porb3 ? Orbital period planet 3
96-101 F6.3 Me mpsini3 ? mp*sini of planet 3
103-108 A6 --- Ref3 Reference for planet 3
110-115 F6.1 d Porb4 ? Orbital period planet 4
117-123 F7.3 Me mpsini4 ? mass mp*sini of planet 4
125-129 A5 --- Ref4 Reference for planet 4
131-135 F5.2 d Porb5 ? Orbital period planet 5
137-141 F5.2 Me mpsini5 ? mp*sini of planet 5
143-147 A5 --- Ref5 Reference for planet 5
149-153 F5.1 d Porb6 ? Orbital period planet 6
155-159 F5.2 Me mpsini6 ? mp*sini of planet 6
161-165 A5 --- Ref6 Reference for planet 6
167-171 F5.1 d Porb7 ? Orbital period planet 7
173-178 F6.3 Me mpsini7 ? mp*sini of planet 7
180-184 A5 --- Ref7 Reference for planet 7
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Byte-by-byte Description of file: refs.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 6 A6 --- Ref Reference code
8- 26 A19 --- BibCode BibCode
28- 50 A23 --- Aut Author's name
52- 76 A25 --- Com Comments
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Global notes:
Note (G1): Prot flags as follows:
S = Secure
P = Provisional
D = Debated
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Acknowledgements:
Yutong Shan, yutong.shan(at)uni-goettingen.de
References:
Alonso-Floriano et al., Paper I 2015A&A...577A.128A 2015A&A...577A.128A, Cat. J/A+A/577/A128
Cortes-Contreras et al., Paper II 2017A&A...597A..47C 2017A&A...597A..47C, Cat. J/A+A/597/A47
Jeffers et al., Paper III 2018A&A...614A..76J 2018A&A...614A..76J, Cat. J/A+A/514/A76
Diez Alonso et al., Paper IV 2019A&A...621A.126D 2019A&A...621A.126D, cat. J/A+A/621/A126
Cifuentes et al., Paper V 2020A&A...642A.115C 2020A&A...642A.115C, Cat. J/A+A/642/A115
Perdelwitz et al., Paper VI 2021A&A...652A.116P 2021A&A...652A.116P, Cat. J/A+A/652/A116
(End) Patricia Vannier [CDS] 11-Mar-2024