J/MNRAS/442/2081 Praesepe members light curves (Kovacs+, 2014)
Stellar rotational periods in the planet hosting open cluster Praesepe.
Kovacs G., Hartman J.D., Bakos G.A., Quinn S.N., Penev K., Latham D.W.,
Bhatti W., Csubry Z., de Val-Borro M.
<Mon. Not. R. Astron. Soc. 442, 2081 (2014)>
=2014MNRAS.442.2081K 2014MNRAS.442.2081K
ADC_Keywords: Clusters, open ; Photometry, SDSS
Keywords: planetary systems - stars: rotation - starspots -
stars: variables: delta Scuti -
open clusters and associations: individual: Praesepe
Abstract:
By using the dense coverage of the extrasolar planet survey project
HATNet (Hungarian-made Automated Telescope Network), we Fourier
analyse 381 high-probability members of the nearby open cluster
Praesepe (Beehive/M44/NGC 2632). In addition to the detection of 10
variables (of delta Scuti and other types), we identify 180 rotational
variables (including the two known planet hosts). This sample
increases the number of known rotational variables in this cluster for
spectral classes earlier than M by more than a factor of 3. These
stars closely follow a colour/magnitude - period relation from early F
to late K stars. We approximate this relation by polynomials for an
easier reference to the rotational characteristics in different
colours. The total (peak-to-peak) amplitudes of the large majority
(94%) of these variables span the range of 0.005-0.04mag. The periods
cover a range from 2.5 to 15d. These data strongly confirm that
Praesepe and the Hyades have the same gyrochronological ages.
Regarding the two planet hosts, Pr0211 (the one with the shorter
orbital period) has a rotational period that is ∼2d shorter than the
one expected from the main rotational pattern in this cluster. This,
together with other examples discussed in the paper, may hint that
star-planet interaction via tidal dissipation can be significant in
some cases in the rotational evolution of stars hosting hot Jupiters.
Description:
Light curves used in the time series analysis of Praesepe are
presented. There are 381 light curves on instrumental Sloan r'
magnitude scale with the zero points determined by the 2MASS
magnitudes according to Eq. (1) of the paper. We present two types of
magnitudes: a) external parameter decorrelated (EPD) and b), the ones
obtained after the application of a trend filtering algorithm (TFA) on
the EPD time series. These two methods are briefly described in the
paper and in detail in the references therein. Here we just note that
both methods are intended to filter out systematics due to
environmental effects (instrumental, weather, etc.). For TFA filtering
we used 600 templates and did not apply signal reconstruction.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 104 180 HATNet rotational variables in the Praesepe
tablea1.dat 90 10 Non-rotational variables in Praesepe detected
in the HATNet data base
tableb1.dat 60 24 SBs in Praesepe
list.dat 33 381 HATNet IDs and the corresponding 2MASS IDs of
the 381 stars analyzed in the paper
lc/* . 381 Individual light curves
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See also:
J/AJ/128/1761 : HATNET variability survey (Hartman+, 2004)
J/AJ/141/166 : HATNet variability survey of K and M dwarfs (Hartman+, 2011)
J/MNRAS/408/475 : HATNet Pleiades Rotation Period Catalogue (Hartman+, 2010)
J/AJ/135/907 : Variables in Praesepe identified with KELT (Pepper+, 2008)
J/MNRAS/426/3419 : UKIDSS GCS Praesepe members (Boudreault+, 2012)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 4 A4 --- --- [HAT-]
5- 15 A11 --- HATNet Internal name used in the HATNet database
17 A1 --- Type [a-d] HAT variable type (1)
19- 33 A15 --- 2MASS Internal name used in the 2MASS database
35- 42 F8.6 d-1 nu [0.05/0.4] Frequency
44- 45 A2 --- n_nu Note on nu (2)
47- 52 F6.4 d-1 1/T [0.001/0.021] Inverse of the total time span
(as a proxy of the error of the frequency)
54- 59 F6.3 mag Bmag Johnson B magnitude
61- 66 F6.3 mag Vmag Johnson V magnitude
68- 73 F6.3 mag rmag Sloan r magnitude
75- 80 F6.3 mag Kmag 2MASS Ks magnitude
82- 86 F5.3 mag J-H 2MASS J-H colour index
88- 92 F5.3 mag J-K 2MASS J-K colour index
94- 99 F6.4 mag Amp [0.003/0.11] Amplitude (3)
101-104 F4.1 --- SNR Signal-to-noise ratio of the peak frequency (4)
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Note (1): based on the classification of their frequency spectra
(see Sect. 3.3):
a = these variables apparently have monoperiodic sinusoidal light variation
(i.e. no residual power left near the main peak after pre-whitening).
b = variables with a single but unstable sinusoidal component.
c = we can observe two peaks separated by a few times of the overall line
width
d = stars that have residual power either at the corresponding first
harmonic or at a sub-harmonic frequency.
Note (2): Frequencies flagged by xn indicate that the frequency value shown
is the most dominant frequency of the DFT (Discrete Fourier Transformation)
spectrum divided by n (ν=νmax/n)
Note (3): Amplitudes are peak-to-peak values from the fourth-order Fourier fit
to the data without TFA filtering (Trend Filtering Algorithm) and using the
frequencies as given in this table.
Note (4): computed from the data without TFA filtering and refers to
the [0, 0.5]d-1 band.
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Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 4 A4 --- --- [HAT-]
5- 15 A11 --- HATNet Internal name used in the HATNet database
17- 32 A16 --- 2MASS Internal name used in the 2MASS database
34- 43 A10 --- OName Other name
45- 54 F10.7 d-1 nu Frequency
56- 60 F5.3 mag Kmag 2MASS Ks magnitude
62- 66 F5.3 mag J-K 2MASS J-K colour index
68- 73 F6.4 mag Amp Amplitude (1)
75- 78 F4.1 --- SNR Signal-to-noise ratio (2)
80- 90 A11 --- Type Variable type
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Note (1): Amplitudes are peak-to-peak values from the fourth-order Fourier fit
to the instrumental Sloan 'r' LCs, without TFA filtering.
For the special case of HAT-269-0000465, the amplitude is a rough visual
estimate of the total range of variation. For other details of this object,
see the text.
Note (2): For variables with peak frequency 1<nu<10d-1, the signal-to-noise
ratio (SNR) is computed in the [1,10]d-1 band.
For those with nu>10d-1, the [10,50]d-1 band is used.
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Byte-by-byte Description of file: tableb1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 4 A4 --- --- [HAT-]
5- 15 A11 --- HATNet Internal name used in the HATNet database
17- 20 I4 --- KW KW number, Cl* NGC 2632 KW NNNN in Simbad
22- 26 F5.3 mag Kmag 2MASS Ks magnitude
28- 32 F5.3 mag J-K 2MASS J-K colour index
34- 40 F7.5 d-1 fphot Photometric frequency (1)
42- 48 F7.5 d-1 forb Orbial frequency (1)
50- 55 F6.4 --- fphot/forb Photometric to orbital frequency ratio
57- 60 F4.1 --- SNR Signal to noise ratio (2)
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Note (1): Photometric and orbital frequencies are taken from this paper and
from Mermilliod et al. (2009, Cat. J/A+A/498/949).
Note (2): The signal-to-noise ratio (SNR) refers to the peak frequency in
the [0,10]d-1 band, and is computed from the Fourier spectra of the
TFA-filtered data. See the text for more about fphot and on the status
of HAT-269-0000465.
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Byte-by-byte Description of file: list.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 4 A4 --- --- [HAT-]
5- 15 A11 --- HATNet Internal name used in the HATNet database
18- 33 A16 --- 2MASS Internal name used in the 2MASS database
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Byte-by-byte Description of file: lc/*
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Bytes Format Units Label Explanations
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2- 15 F14.6 d BJD Barycentric Julian Date
18- 25 F8.5 mag r(EPD) External Parameter Decorrelation magnitude
on approximate Sloan r scale
28- 35 F8.5 mag r(TFA) Trend Filter Algorithm magnitude
on approximate Sloan r scale
38- 40 I3 --- Field HATNet field number associated with data point
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Acknowledgements:
Geza Kovacs, kovacs(at)konkoly.hu
History:
* 10-Jul-2014: First on-line version
* 11-Jan-2016: tables A1 and B1 added (from electronic version)
(End) Patricia Vannier [CDS] 09-Jul-2014