J/MNRAS/491/5216 Rotation periods for 107 M dwarfs from APACHE (Giacobbe+, 2020)
Photometric rotation periods for 107 M dwarfs from the APACHE survey.
Giacobbe P., Benedetto M., Damasso M., Sozzetti A., Christille J.M.,
Lattanzi M.G., Calcidese P., Carbognani A., Barbato D., Pinamonti M.,
Poggio E., Lanza A.F., Bernagozzi A., Cenadelli D., Lanteri L.,
Bertolini E.
<Mon. Not. R. Astron. Soc., 491, 5216-5237 (2020)>
=2020MNRAS.491.5216G 2020MNRAS.491.5216G (SIMBAD/NED BibCode)
ADC_Keywords: Stars, M-type ; Stars, dwarfs ; Photometry, VRI ;
Rotational velocities ; Radial velocities ; Stars, masses ;
Stars, diameters ; Effective temperatures ;
Parallaxes, trigonometric
Keywords: techniques: photometric - stars: low-mass - stars: rotation -
stars: statistics
Abstract:
We present rotation period measurements for 107 M dwarfs in the mass
range 0.15-0.70M☉ observed within the context of the APACHE
photometric survey. We measure rotation periods in the range 0.5-190d,
with the distribution peaking at ∼30d. We revise the stellar masses
and radii for our sample of rotators by exploiting the Gaia DR2 data.
For ∼20 per cent of the sample, we compare the photometric rotation
periods with those derived from different spectroscopic indicators,
finding good correspondence in most cases. We compare our rotation
periods distribution to the one obtained by the Kepler survey in the
same mass range, and to that derived by the MEarth survey for stars in
the mass range 0.07-0.25M☉. The APACHE and Kepler periods
distributions are in good agreement, confirming the reliability of our
results, while the APACHE distribution is consistent with the MEarth
result only for the older/slow rotators, and in the overlapping mass
range of the two surveys. Combining the APACHE/Kepler distribution
with the MEarth distribution, we highlight that the rotation period
increases with decreasing stellar mass, in agreement with previous
work. Our findings also suggest that the spin-down time scale, from
fast to slow rotators, changes crossing the fully convective limit at
∼0.3M☉ for M dwarfs. The catalogue of 107 rotating M dwarfs
presented here is particularly timely, as the stars are prime targets
for the potential identification of transiting small planets with TESS
and amenable to high-precision mass determination and further
atmospheric characterization measurements.
Description:
APACHE employs an array of five 40-cm telescopes hosted on a single
platform with a roll-off enclosure, located at the Astronomical
Observatory of the Aosta Valley (OAVdA), in the western Italians Alps,
at 1650 meters above the sea level. The telescope array is composed of
five identical Carbon Truss 40-cm f/8.4 Ritchey-Chretien telescopes,
with a GM2000 10-MICRON mount and equipped with a FLI Proline
PL1001E-2 CCD Camera and Johnson-Cousins V & I filters.
We adopted for APACHE an observing strategy consisting of 3
consecutive exposures every 20min. In this way, during a typical night
of observation, each telescope observes ∼12 fields, where the grater
part of them contain only a single target M dwarf. Each target is
observed for the whole time available during the night with airmass
below 2. Exposure times are selected to yield a signal-to-noise ratio
(SNR) for the target star >200 while avoiding detector saturation.
The data considered in this paper are the results of 5yr of
observation between 9th July 2012 and 9th July 2017. This period
corresponds to the nominal duration of the survey. From the APACHE
observations database, we select a sub-sample of 247 M dwarfs with
more than 200 data points taken on at least 10 observation nights and
spanning at least 30d.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 69 248 Observational properties for the APACHE stars
tablea2.dat 114 109 Stellar parameters, kinematics, and rotation
periods for the APACHE rotation candidates
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See also:
I/345 : Gaia DR2 (Gaia Collaboration, 2018)
Byte-by-byte Description of file: tablea1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 12 A12 --- Name Star name (JHHMMS+DDMMA except for GJ3649 and
GJ694.2)
14- 23 F10.6 deg RAdeg Right ascension (J2000)
25- 33 F9.6 deg DEdeg Declination (J2000)
35- 39 F5.2 mag Vmag APACHE V-band magnitude
41- 44 I4 --- Np Number of photometric points per target
46- 48 I3 --- Nn Number of observation nights
50- 53 I4 d DHJD Difference of the Heliocentric Julian date
between the first and the last observation
55- 60 F6.4 mag sigt Single point uncertainty (1)
62- 64 I3 % Phidet Detection efficiency (2)
66- 67 I2 % Phideth Harmonic contamination (3)
69 A1 --- Rot [YN] Indicates if the star is a rotator
(109 Y, 139 N)
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Note (1): The theoretical single point uncertainty σt, is defined by
σt=2.5sqrt(Nstar+Nsky+σscint2)/(ln10xNstar)
where Nstar is the number of photons from the source, Nsky is the
number of photons from the sky background for the photometric aperture
that includes read and dark noise and σscint is the
scintillation noise (Young 1967AJ.....72..747Y 1967AJ.....72..747Y).
Note (2): Relative number of periods that are detected by the Generalized
Lomb-Scargles (GLS) algorithm (Zechmeister & Kurster
2009A&A...496..577Z 2009A&A...496..577Z) with respect to the total number of injected
periods.
Note (3): Relative number of harmonics that are detected by the Generalized
Lomb-Scargles (GLS) algorithm (Zechmeister & Kurster
2009A&A...496..577Z 2009A&A...496..577Z) with respect to the total number of injected
periods.
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Byte-by-byte Description of file: tablea2.dat
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Bytes Format Units Label Explanations
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1- 12 A12 --- Name Star name (JHHMMS+DDMMA except for GJ3649)
14- 18 F5.3 mag B-V ? B-V colour index
20- 27 F8.4 mas plx ? Parallax from Gaia DR2
29- 34 F6.4 mas e_plx ? Error on plx
36- 39 I4 K Teff ? Effective temperature from Gaia DR2
41- 43 I3 K E_Teff ? Upper error on Teff
45- 48 I4 K e_Teff ? Lower error on Teff
50- 54 F5.3 Msun Mstar ? Star mass
56- 60 F5.3 Msun e_Mstar ? Error on Mstar
62- 66 F5.3 Rsun Rad ? Star radius
68- 72 F5.3 Rsun e_Rad ? Error on Rad
74- 79 F6.1 km/s Vr ? Velocity of cylindrical radial component
81- 85 F5.1 km/s Vphi ? Velocity of cylindrical azimuthal component
87- 91 F5.1 km/s Vz ? Velocity of cylindrical vertical component
93-100 F8.4 d Period Rotation period
102-107 F6.4 mag Amp Variability amplitude
109-114 F6.4 --- FAP False Alarm Probability
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History:
From electronic version of the journal
(End) Ana Fiallos [CDS] 22-Feb-2023