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J. Blomme,
L. M. Sarro,
F. T. O’Donovan,
J. Debosscher,
T. Brown,
M. Lopez,
P. Dubath,
L. Rimoldini,
D. Charbonneau,
E. Dunham, G. Mandushev,
D. R. Ciardi,
J. De Ridder,
C. Aerts
[show abstract]
[hide abstract]
ABSTRACT: We present a novel automated methodology to detect and classify periodic variable stars in a large data base of photometric time series. The methods are based on multivariate Bayesian statistics and use a multistage approach. We applied our method to the ground-based data of the Trans-Atlantic Exoplanet Survey (TrES) Lyr1 field, which is also observed by the Kepler satellite, covering ∼26 000 stars. We found many eclipsing binaries as well as classical non-radial pulsators, such as slowly pulsating B stars, Doradus, β Cephei and δ Scuti stars. Also a few classical radial pulsators were found.
Monthly Notices of the Royal Astronomical Society 09/2011; 418(1):96 - 106. · 4.90 Impact Factor
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J. Blomme,
L. M. Sarro,
F. T. O'Donovan,
J. Debosscher,
T Brown,
M Lopez,
P. Dubath,
L. Rimoldini,
D. Charbonneau,
E. Dunham, G. Mandushev,
D. R. Ciardi,
J. De Ridder,
C. Aerts
[show abstract]
[hide abstract]
ABSTRACT: We present a novel automated methodology to detect and classify periodic
variable stars in a large database of photometric time series. The methods are
based on multivariate Bayesian statistics and use a multi-stage approach. We
applied our method to the ground-based data of the TrES Lyr1 field, which is
also observed by the Kepler satellite, covering ~26000 stars. We found many
eclipsing binaries as well as classical non-radial pulsators, such as slowly
pulsating B stars, Gamma Doradus, Beta Cephei and Delta Scuti stars. Also a few
classical radial pulsators were found.
01/2011;
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F ~T O'Donovan,
D Charbonneau, G Mandushev,
E ~W Dunham,
D ~W Latham,
G Torres,
A Sozzetti,
T ~M Brown,
J ~T Trauger,
J ~A Belmonte,
M Rabus,
J ~M Almenara,
R Alonso,
H ~J Deeg,
G ~A Esquerdo,
E ~E Falco,
L ~A Hillenbrand,
A Roussanova,
R ~P Stefanik,
J ~N Winn
NASA/IPAC/NExScI Star and Exoplanet Database, TrES Lyr1 Catalog; 01/2009
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O. L. Creevey,
G. F. Benedict,
T. M. Brown,
R. Alonso,
P. Cargile, G. Mandushev,
D. Charbonneau,
B. E. McArthur,
W. Cochran,
F. T. O'Donovan,
S. J. Jiménez-Reyes,
J. A. Belmonte,
and D. Kolinski
[show abstract]
[hide abstract]
ABSTRACT: We describe a newly discovered detached M dwarf eclipsing binary system. This system was first observed by the TrES network during a long-term photometry campaign of 54 nights. Analysis of the folded light curve indicates two very similar components orbiting each other with a period of 1.12079 ± 0.00001 days. Spectroscopic observations with the Hobby-Eberly Telescope show the system to consist of two M3e dwarfs in a near-circular orbit. Double-line radial velocity amplitudes, combined with the orbital inclination derived from light-curve fitting, yield Mtotal = 0.983 ± 0.007 M☉, with component masses of M1 = 0.493 ± 0.003 M☉ and M2 = 0.489 ± 0.003 M☉. The light-curve fit yields component radii of R1 = 0.453 ± 0.060 R☉ and R2 = 0.452 ± 0.050 R☉. Although a precise parallax is lacking, broadband VJHK colors and spectral typing suggest component absolute magnitudes of MV(1) = 11.18 ± 0.30 and MV(2) = 11.28 ± 0.30.
The Astrophysical Journal 12/2008; 625(2):L127. · 6.02 Impact Factor
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[show abstract]
[hide abstract]
ABSTRACT: We investigate the origin of a flux increase found during a transit of TrES-1, observed with the HST. This feature in the HST light curve cannot be attributed to noise and is supposedly a dark area on the stellar surface of the host star eclipsed by TrES-1 during its transit. We investigate the likeliness of two possible hypothesis for its origin: A starspot or a second transiting planet. We made use of several transit observations of TrES-1 from space with the HST and from ground with the IAC-80 telescope. On the basis of these observations we did a statistical study of flux variations in each of the observed events, to investigate if similar flux increases are present in other parts of the data set. The HST observation presents a single clear flux rise during a transit whereas the ground observations led to the detection of two such events but with low significance. In the case of having observed a starspot in the HST data, assuming a central impact between the spot and TrES-1, we would obtain a lower limit for the spot radius of 42000 km. For this radius the spot temperature would be 4690 K, 560 K lower then the stellar surface of 5250 K. For a putative second transiting planet we can set a lower limit for its radius at 0.37 R$_J$ and for periods of less than 10.5 days, we can set an upper limit at 0.72 R$_J$. Assuming a conventional interpretation, then this HST observation constitutes the detection of a starspot. Alternatively, this flux rise might also be caused by an additional transiting planet. The true nature of the origin can be revealed if a wavelength dependency of the flux rise can be shown or discarded with a higher certainty. Additionally, the presence of a second planet can also be detected by radial velocity measurements. Comment: 8 pages, 6 figures, accepted for publication in A&A
12/2008;
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D Charbonneau,
L Allen,
T Brown,
R Gilliland,
D Latham, G Mandushev,
T Megeath,
G Torres,
R Alonso Sobrino,
F O'Donovan,
A Sozzetti
Spitzer Proposal. 09/2004;
