J/A+A/506/519 Supervised classification of CoRoT variables (Debosscher+, 2009)
Automated supervised classification of variable stars in the CoRoT programme.
Debosscher J., Sarro L.M., Lopez M., Deleuil M., Aerts C., Auvergne M.,
Baglin A., Baudin F., Chadid M., Charpinet S., Cuypers J., De Ridder J.,
Garrido R., Hubert A.M., Janot-Pacheco E., Jorda L., Kaiser A.,
Kallinger T., Kollath Z., Maceroni C., Mathias P., Michel E., Moutou C.,
Neiner C., Ollivier M., Samadi R., Solano E., Surace C., Vandenbussche B.,
Weiss W.W.
<Astron. Astrophys. 506, 519 (2009)>
=2009A&A...506..519D 2009A&A...506..519D
ADC_Keywords: Stars, variable
Keywords: stars: variables: general - stars: binaries: general -
techniques: photometric - methods: statistical -
methods: data analysis
Abstract:
In this work, we describe the pipeline for the fast supervised
classification of light curves observed by the CoRoT exoplanet CCDs.
We present the classification results obtained for the first four
measured fields, which represent a one-year in-orbit operation. The
basis of the adopted supervised classification methodology has been
described in detail in a previous paper, as is its application to the
OGLE database. Here, we present the modifications of the algorithms
and of the training set, to optimize the performance when applied to
the CoRoT data. Classification results are presented for the observed
fields IRa01, SRc01, LRc01, and LRa01 of the CoRoT mission. Statistics
on the number of variables and the number of objects per class are
given and typical light curves of high-probability candidates are
shown. We also report on new stellar variability types discovered in
the CoRoT data. The full classification results are publicly
available.
Description:
Light curve parameters and classification results are presented for
all the objects measured in the first four CoRoT observing runs:
IRa01, SRc01, LRc01, and LRa01. The information presented here should
allow scientists to make candidate lists of their objects of study and
to obtain some basic light curve information. We recall that we did
not perform detailed light curve modelling, only a basic one,
sufficient for producing variability class memberships for each
target. We refer to the paper for a detailed description of the light
curve parameters, and the classification results. It is strongly
advised to read the paper prior to using the results presented here.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
ira01-n3.dat 473 9869 N3-results for IRa01
lra01-n3.dat 473 11408 N3-results for LRc01
lrc01-n3.dat 473 11408 N3-results for SRc01
src01-n3.dat 473 6971 N3-results for LRa01
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See also:
B/corot : CoRoT observation log (CoRoT, 2009)
J/AJ/134/1560 : BEST periodic variable stars in IR01 field (Kabath+, 2007)
J/AJ/134/766 : BEST variable stars in LRc1 field (Karoff+, 2007)
J/AJ/136/654 : BEST periodic variable stars in LRa1 field (Kabath+, 2008)
J/AJ/137/3911 : BEST periodic variable stars in LRc2 field (Kabath+, 2009)
J/A+A/506/569 : BEST II CoRoT LRa02 field periodic variables (Kabath+, 2009)
J/A+A/475/1159 : Supervised classification of variable stars (Debosscher+ 2007)
Byte-by-byte Description of file: *n3.dat
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Bytes Format Units Label Explanations
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1- 9 I9 --- CoRoT CoRoT Identifier
22- 29 F8.6 --- pV1 Class V1 probability 1 (1)
31- 38 F8.6 --- pV2 Class V2 probability 2 (1)
40- 47 F8.6 --- pV3 Class V3 probability 3 (1)
49- 53 A5 --- V1 Class code 1 (2)
56- 60 A5 --- V2 Class code 2 (2)
63- 67 A5 --- V3 Class code 3 (2)
70- 77 F8.6 --- Pf1 [0,1] Significance parameter of f1 (3)
79- 86 F8.6 --- Pf2 [0,1] Significance parameter of f2 (3)
88- 95 F8.6 --- Pf3 [0,1] Significance parameter of f3 (3)
97-109 F13.8 1/d f1 First (dominant) detected frequency
111-123 F13.8 1/d f2 Second detected frequency
125-137 F13.8 1/d f3 Third detected frequency
139-151 F13.8 mag amp11 Amplitude of f1
153-165 F13.8 mag amp12 Amplitude of 2*f1
167-179 F13.8 mag amp13 Amplitude of 3*f1
181-193 F13.8 mag amp14 Amplitude of 4*f1
195-207 F13.8 mag amp21 Amplitude of f2
209-221 F13.8 mag amp22 Amplitude of 2*f2
223-235 F13.8 mag amp23 Amplitude of 3*f2
237-249 F13.8 mag amp24 Amplitude of 4*f2
251-263 F13.8 mag amp31 Amplitude of f3
265-277 F13.8 mag amp32 Amplitude of 2*f3
279-291 F13.8 mag amp33 Amplitude of 3*f3
293-305 F13.8 mag amp34 Amplitude of 4*f3
307-319 F13.8 rad phd12 Phase of 2*f1, if phase of f1=0 (5)
321-333 F13.8 rad phd13 Phase of 3*f1, if phase of f1=0 (5)
335-347 F13.8 rad phd14 Phase of 4*f1, if phase of f1=0 (5)
349-361 F13.8 rad phd21 Phase of f2, if phase of f1=0 (5)
363-375 F13.8 rad phd22 Phase of 2*f2, if phase of f1=0 (5)
377-389 F13.8 rad phd23 Phase of 3*f2, if phase of f1=0 (5)
391-403 F13.8 rad phd24 Phase of 4*f2, if phase of f1=0 (5)
405-417 F13.8 rad phd31 Phase of f3, if phase of f1=0 (5)
419-431 F13.8 rad phd32 Phase of 2*f3, if phase of f1=0 (5)
433-445 F13.8 rad phd33 Phase of 3*f3, if phase of f1=0 (5)
447-459 F13.8 rad phd34 Phase of 4*f3, if phase of f1=0 (5)
461-473 F13.8 --- varred [0,1] Total variance reduction (4)
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Note (1): relative probabilities for the three most likely class
memberships, obtained with the MSBN (multistage Bayesian networks)
classifier.
Note (2): corresponding to the three most likely variability class
memberships, in decreasing order of probability.
The classes are as follows:
BCEP = β-Cephei stars
BE = Variable Be-stars
CLCEP = Classical Cepheids (δ-Cep)
CP = Chemically peculiar stars
DMCEP = Double-mode Cepheids
DSCUT = δ-Scuti stars
ECL = Eclipsing binaries (all types)
ELL = Ellipsoidal variables
FUORI = FU-Ori stars
GDOR = γ-Doradus stars
HAEBE = Herbig Ae/Be stars
LAPV = Low-amplitude periodic variables
LBOO = λ-Bootis variables
LBV = Luminous Blue variables
MIRA = Mira variables
PTCEP = Population II Cepheids
PVSG = Periodically variable supergiants
RRAB = RR-Lyrae stars, subtype ab
RRC = RR-Lyrae stars, subtype c
RRD = Double-mode RR-Lyrae stars
RVTAU = RV-Tauri stars
SDBV = Pulsating subdwarf B-stars
SPB = Slowly pulsating B-stars
SPDS = Short-period δ-Scuti variables
SR = Semi-regular variables
SXPHE = SX-Phe stars
TTAU = T-Tauri stars
WR = Wolf-Rayet stars
XB = X-ray binaries
Note (3): significance parameters (P-values) resulting from a statistical
F-test. For each of the 3 detected frequencies, the reduction in
variance obtained by subtracting a least-squares fit with 4 harmonics
is checked. If this reduction is not significant (can be explained by
noise), the significance parameters will be close to 1, if the
reduction is significant, the values will be close to 0. We refer to
the paper again for a detailed description of these parameters.
Note (4): total variance reduction of the trend-subtracted light curve,
after subtraction of the least-squares fits with the 3 frequencies and
their 4 harmonics (this parameter has values close to 1 if the fit is
good, close to 0 if the fit is poor).
Note (5): Phase in the range (-π, π).
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Acknowledgements:
Jonas Debosscher, jonas.debosscher(at)ster.kuleuven.ac.be
(End) Patricia Vannier [CDS] 26-Oct-2009