J/A+A/621/A126 CARMENES input catalogue of M dwarfs. IV. (Diez Alonso+ 2019)
CARMENES input catalogue of M dwarfs.
IV. New rotation periods from photometric time series.
Diez Alonso E., Caballero J.A., Montes D., de Cos Juez F.J., Dreizler S.,
Dubois F., Jeffers S.V., Lalitha S., Naves R., Reiners A., Ribas I.,
Vanaverbeke S., Amado P.J., Bejar V.J.S., Cortes-Contreras M., Herrero E.,
Hidalgo D., Kuerster M., Logie L., Quirrenbach A., Rau S., Seifert W.,
Schoefer P., Tal-Or L.
<Astron. Astrophys. 621, A126 (2019)>
=2019A&A...621A.126D 2019A&A...621A.126D (SIMBAD/NED BibCode)
ADC_Keywords: Stars, standard; Stars, dwarfs; Stars, M-type; Stars, late-type;
Stars, double and multiple
Keywords: stars: activity - stars: late type - stars: rotation -
techniques: photometry
Abstract:
The main goal of this work is to measure rotation periods of the
M-type dwarf stars being observed by the CARMENES exoplanet survey to
help distinguish radial-velocity signals produced by magnetic activity
from those produced by exoplanets. Rotation periods are also
fundamental for a detailed study of the relation between activity and
rotation in late-type stars.
We look for significant periodic signals in 622 photometric time
series of 337 bright, nearby M dwarfs obtained by long-time baseline,
automated surveys (MEarth, ASAS, SuperWASP, NSVS, Catalina, ASAS-SN,
K2, and HATNet) and, for 20 stars, obtained by us with four 0.2-0.8m
telescopes at high geographical latitudes.
We present 142 rotation periods (73 new) from 0.12d to 133d and ten
long-term activity cycles (six new) from 3.0a to 11.5a. We compare our
determinations with those in the existing literature, investigate the
distribution of Prot in the CARMENES input catalogue, the amplitude of
photometric variability, and their relation to vsini and
pEW(Hα), and identify three very active stars with new rotation
periods between 0.34d and 23.6d.
Description:
During guaranteed time observations (GTOs), the double-channel
CARMENES spectrograph has so far observed a sample of 336 bright,
nearby M dwarfs with the goal of detecting low-mass planets in their
habitable zone with the radial-velocity method (Quirrenbach et al.,
2015, in 18th Cambridge Workshop on Cool Stars, Stellar Systems, and
the Sun, Proceedings of the conference held at Lowell Observatory,
8-14 June 2014. Edited by G. van Belle and H.C. Harris., pp. 897-906;
Reiners et al., 2018, Cat. J/A+A/612/A49). Of these, 324 were
presented by Reiners et al. (2018, Cat. J/A+A/612/A49), three did not
have enough CARMENES observations at the time of preparing the
spectral templates for the study, and nine are new spectroscopic
binaries (Baroch et al., 2018, A&A, in prep, arXiv:1808.06895). Here,
we investigate the photometric variability of these 336 M dwarfs and
of G 34-23 AB (J01221+221AB), which Cortes-Contreras et al. (2017,
Cat. J/A+A/597/A47) found to be a close physical binary just before
GTO start. This results in a final sample size of 337 stars.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
photom.dat 128 625 M dwarfs searched for photometric periods
for 337 stars
rotper.dat 98 142 Rotation periods obtained for stars in our
sample
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See also:
J/A+A/577/A128 : CARMENES input catalogue of M dwarfs. I
(Alonso-Floriano+, 2015)
J/A+A/597/A47 : CARMENES input catalogue of M dwarfs. II
(Cortes-Contreras+ 2017)
J/A+A/612/A49 : 324 CARMENES M dwarfs velocities (Reiners+, 2018)
J/A+A/619/A32 : CARMENES SB2 orbital parameters (Baroch+, 2019)
Byte-by-byte Description of file: photom.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- Karmn CARMENES designation (JHHMM+DDdA)
13- 33 A21 --- Name Other Name of the star
35- 46 A12 --- OName Other Name of the star
48- 49 I2 h RAh Right ascension (J2000.0)
51- 52 I2 min RAm Right ascension (J2000.0)
54- 58 F5.2 s RAs Right ascension (J2000.0)
60 A1 --- DE- Declination sign (J2000.0)
61- 62 I2 deg DEd Declination (J2000.0)
64- 65 I2 arcmin DEm Declination (J2000.0)
67- 70 F4.1 arcsec DEs Declination (J2000.0)
72- 88 A17 --- Survey Survey
90- 94 I5 --- Nobs ?=- Number of data points before cleaning
95 A1 --- --- [/]
96-100 I5 ---- Nused ?=- Number of data points after cleaning
102-107 F6.4 yr Dt ?=- Time between first and last visit
109-114 F6.3 mag ?=- Mean magnitude
116-122 F7.4 mag s_mag []?=- Standard deviation of the individual
magnitudes
124-128 F5.3 mag e_ ?=- Mean error of magnitude
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Byte-by-byte Description of file: rotper.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- Karmn CARMENES designation (JHHMM+DDdA)
12 A1 --- n_Karmn [bcde] Individual note (1)
14- 22 F9.5 d Prot Rotation period determined in this work
24- 31 F8.5 d e_Prot rms uncertainty on Prot
34- 38 F5.3 mag Amp Amplitude of Prot from this work
40 A1 --- l_FAP Limit flag on FAP
41- 48 F8.5 % FAP False alarm probability (this work)
50- 63 A14 ---- Survey Survey used to compute Prot in this work
66- 73 F8.4 d ProtLit ?=- Previous published rotation period
75- 80 F6.4 d e_ProtLit ? rms uncertainty on ProtLit
81- 86 F6.4 mag AmpLit ?=- Amplitude of previous published Prot
88 A1 --- l_FAPLit Limit flag on FAPLit
89- 92 F4.1 % FAPLit ?=- False alarm probability of previous
published Prot
94- 98 A5 --- r_ProtLit References of previous published Prot (2)
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Note (1): Individual notes as follows:
b = J00051+457 = GJ 2: the periodogram of the ASAS light curve displays
several secondary peaks around 15.37d, including at 21.2d as found
by Suarez-mascareno et al., 2015MNRAS.452.2745S 2015MNRAS.452.2745S.
c = J04472+206 = RX J0447.2+2038: we also measured Prot=0.342±0.002d,
in the Montcabrer dataset
d = J06318+414 = LP 205-044: the periodogram of the SuperWASP light curve
displays a second peak at 0.482d of approximately the same power
as at 0.299d.
e = J10508+068 = EE Leo: we increased the frequency search to less than
half of the inverse of the time baseline of about 80d, so the
tabulated period is uncertain.
Note (2): References as follows:
GR98 = Greimel & Robb , 1998IBVS.4652....1G 1998IBVS.4652....1G
Fek00 = Fekel & Henry, 2000AJ....120.3265F 2000AJ....120.3265F
Tes04 = Testa et al., 2004ApJ...617..508T 2004ApJ...617..508T
Riv05 = Rivera et al., 2005ApJ...634..625R 2005ApJ...634..625R, Cat. J/ApJ/634/625
KS07 = Kiraga and Stepien, 2007AcA....57..149K 2007AcA....57..149K
Nor07 = Norton et al., 2007A&A...467..785N 2007A&A...467..785N, Cat. J/A+A/467/785
Hal08 = Hallinan et al., 2008ApJ...684..644H 2008ApJ...684..644H
Har11 = Hartman et al., 2011AJ....141..166H 2011AJ....141..166H, Cat. J/AJ/141/166
Irw11 = Irwin et al., 2011ApJ...727...56I 2011ApJ...727...56I
Kir12 = Kiraga, 2012AcA....62...67K 2012AcA....62...67K, Cat. J/AcA/62/67
KS13 = Kiraga & Stepien, 2013AcA....63...53K 2013AcA....63...53K, Cat. J/AcA/63/53
SM15 = Suarez-mascareno et al., 2015MNRAS.452.2745S 2015MNRAS.452.2745S
Wes15 = West et al., 2015ApJ...812....3W 2015ApJ...812....3W, Cat. J/ApJ/812/3
Dav16 = David et al., 2016Natur.534..658D 2016Natur.534..658D
New16 = Newton et al., 2016ApJ...821...93N 2016ApJ...821...93N, Cat. J/ApJ/821/93
SM16 = Suarez Mascareno et al., 2016A&A...595A..12S 2016A&A...595A..12S
SM17 = Mascareno et al., 2018A&A...612A..89M 2018A&A...612A..89M
Clo17 = Cloutier et al., 2017A&A...608A..35C 2017A&A...608A..35C, Cat. J/A+A/608/A35
Vid17 = Vida et al., 2017ApJ...841..124V 2017ApJ...841..124V
Lot18 = Lothringer et al., 2018AJ....155...66L 2018AJ....155...66L
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Acknowledgements:
Enrique Diez Alonso, enridiez(at)ucm.es
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
(End) Patricia Vannier [CDS] 05-Sep-2018