Access to Astronomical Catalogues

← Click to display the menu
J/A+A/530/A5     WASP-4b Ks-band detection of thermal emission  (Caceres+, 2011)

A ground-based Ks-band detection of the thermal emission from the transiting exoplanet WASP-4b. Caceres C., Ivanov V.D., Minniti D., Burrows A., Selman F., Melo C., Naef D., Mason E., Pietrzynski G. <Astron. Astrophys. 530, A5 (2011)> =2011A&A...530A...5C
ADC_Keywords: Stars, double and multiple ; Planets ; Occultations ; Magnitudes Keywords: planetary systems - eclipses - stars: individual: WASP-4b - techniques: photometric Abstract: Secondary eclipses are a powerful tool to measure directly the thermal emission from extrasolar planets, and to constrain their type and physical parameters. We started a project to obtain reliable broad-band measurements of the thermal emission of transiting exoplanets. Ground-based high-cadence near-infrared relative photometry was used to obtain a sub-millimagnitude precision light curve of a secondary eclipse of WASP-4b -- a 1.12MJ hot Jupiter on a 1.34-day orbit around G7V star. The data show a clear ∼10σ detection of the planet's thermal emission at 2.2µ. The calculated thermal emission corresponds to a fractional eclipse depth of 0.185+0.014-0.013%, with a related brightness temperature in Ks of TB=1995±40K, centered at Tc=2455102.61162+0.00071-0.00077HJD. We could set a limit on the eccentricity of e*cosω=0.0027±0.0018, compatible with a near-circular orbit. The calculated brightness temperature, and the specific models suggest a highly inefficient redistribution of heat from the day-side to the night-side of the planet, and a consequent emission mainly from the day-side. The high-cadence ground-based technique is capable of detecting the faint signal of the secondary eclipse of extrasolar planets, which makes it a valuable complement to space-based mid-IR observations. Description: The relative photometric series of the Ks-band occultation of the planet WASP-4b. Extra digits are given to avoid round-up errors. Objects: ---------------------------------------------------------------- RA (2000) DE Designation(s) ---------------------------------------------------------------- 23 34 15.1 -42 03 41 WASP-4 = 1SWASP J233415.06-420341.1 ---------------------------------------------------------------- File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 31 24071 Secondary eclipse light curve
See also: J/MNRAS/408/1680 : WASP-2 transiting planetary system (Southworth+, 2010) J/MNRAS/399/287 : WASP-4 transiting planetary system (Southworth+, 2009) J/AJ/137/3826 : WASP-4b, two transits of the giant planet (Winn+, 2009) J/MNRAS/396/1023 : WASP-5 transiting planetary system (Southworth+, 2009) J/A+A/501/785 : WASP-6b, discovery and characterization of (Gillon+, 2009) J/A+A/527/A8 : WASP-7 transiting planetary system (Southworth+, 2011) J/A+A/517/L1 : WASP-8b radial velocities (Queloz+, 2010) J/ApJ/692/L100 : WASP-10 relative photometry (Johnson+, 2009) J/A+A/528/A65 : WASP-12b transits (Maciejewski+, 2011) J/A+A/502/391 : WASP-13b photometry and radial velocities (Skillen+, 2009) J/ApJ/707/167 : WASP-18 transiting planetary system (Southworth+, 2009) J/A+A/513/L3 : WASP-19b H-band thermal emission (Anderson+, 2010) J/A+A/519/A98 : WASP-21b transit (Bouchy+, 2010) J/A+A/520/A56 : WASP-26b RV and photometric data (Smalley+, 2010) J/A+A/526/L10 : WASP-33 photometric follow-up (Herrero+, 2011) J/A+A/526/A130 : WASP-34b photometry and radial velocities (Smalley+, 2011) J/A+A/525/A54 : WASP-38b transits (Barros+, 2011) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 15 F15.7 d HJD Heliocentric Julian Date 17- 23 F7.5 --- Flux Normalized flux 25- 31 F7.5 --- e_Flux Flux error estimation
Acknowledgements: Claudio Caceres, cccacere(at)astro.puc.cl
(End) C. Caceres [P. Univ. Catolica de Chile], P. Vannier [CDS] 08-Apr-2011
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

catalogue service

© UDS/CNRS

Contact