J/MNRAS/428/678 Transiting exoplanet TrES-3b CCD UBVR photometry (Turner+, 2013)
Near-UV and optical observations of the transiting exoplanet TrES-3b.
Turner J.D., Smart B.M., Hardegree-Ullman K.K., Carleton T.M.,
Walker-Lafollette A.M., Crawford B.E., Smith C.-T.W., McGraw A.M.,
Small L.C., Rocchetto M., Cunningham K.I., Towner A.P.M., Zellem R.,
Robertson A.N., Guvenen B.C., Schwarz K.R., Hardegree-Ullman E.E.,
Collura D., Henz T.N., Lejoly C., Richardson L.L., Weinand M.A.,
Taylor J.M., Daugherty M.J., Wilson A.A., Austin C.L.
<Mon. Not. R. Astron. Soc., 428, 678-690 (2013)>
=2013MNRAS.428..678T 2013MNRAS.428..678T (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Planets ; Photometry, CCD
Keywords: planets and satellites: individual: TrES-3b -
techniques: photometric - planets and satellites: magnetic fields -
planetary systems
Abstract:
We observed nine primary transits of the hot Jpiter TrES-3b in several
optical and near-UV photometric bands from 2009 June to 2012 April in
an attempt to detect its magnetic field. Vidotto, Jardine and Helling
suggest that the magnetic field of TrES-3b can be constrained if its
near-UV light curve shows an early ingress compared to its optical
light curve, while its egress remains unaffected. Predicted magnetic
field strengths of Jupiter-like planets should range between 8G and
30G. Using these magnetic field values and an assumed B* of 100G, the
Vidotto et al. method predicts a timing difference of 5-11min. We did
not detect an early ingress in our three nights of near-UV
observations, despite an average cadence of 68 s and an average
photometric precision of 3.7mmag. However, we determined an upper
limit of TrES-3b's magnetic field strength to range between 0.013 and
1.3G (for a 1-100G magnetic field strength range for the host star,
TrES-3) using a timing difference of 138s derived from the
Nyquist-Shannon sampling theorem. To verify our results of an
abnormally small magnetic field strength for TrES-3b and to further
constrain the techniques of Vidotto et al., we propose future
observations of TrES-3b with other platforms capable of achieving a
shorter near-UV cadence. We also present a refinement of the physical
parameters of TrES-3b, an updated ephemeris and its first published
near-UV light curve. We find that the near-UV planetary radius of
Rp=1.386+0.248-0.144RJup is consistent with the planet's
optical radius.
Description:
Light curves for TrES-3b in the UBVR and J-CR filters.
Objects:
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RA (2000) DE Designation(s)
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17 52 07.02 +37 32 46.2 TrES-3b = NAME TrES-3b
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
lc.dat 26 2097 Light curves of TrES-3b
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See also:
J/AJ/136/267 : Six occultations of the exoplanet TrES-3 (Winn+, 2008)
J/ApJ/691/1145 : Spectrophotometry of TrES-3 and TrES-4 (Sozzetti+, 2009)
J/MNRAS/408/1494 : Planetary transits of TrES-2 and TrES-3 (Colon+, 2010)
J/AJ/145/68 : Five new transit light curves of TrES-3 (Jiang+, 2013)
Byte-by-byte Description of file: lc.dat
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Bytes Format Units Label Explanations
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1- 5 A5 --- Filt [UBVR J-CR] Filter (1)
6- 17 F12.7 d HJD Heliocentric Julian Date (HJD-2450000)
19- 26 F8.6 --- Flux Relative flux
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Note (1): Filters used:
B = Harris B, R = Harris R, V = Harris V, U = Bessell U and
J-CR = Johnson-Cousins R.
Telescopes used:
1.55-m Kuiper Telescope, ULO 0.36-m EAST telescope and
ULO 0.36-m WEST telescope
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Acknowledgements:
Jake D. Turner, jt6an(at)virginia.edu
(End) Patricia Vannier [CDS] 20-Apr-2016