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J/ApJ/829/L9       K2 LC of HD 3167 and Robo-AO image       (Vanderburg+, 2016)

Two small planets transiting HD 3167. Vanderburg A., Bieryla A., Duev D.A., Jensen-Clem R., Latham D.W., Mayo A.W., Baranec C., Berlind P., Kulkarni S., Law N.M., Nieberding M.N., Riddle R., Maissa S. <Astrophys. J., 829, L9 (2016)> =2016ApJ...829L...9V
ADC_Keywords: Planets ; Stars, double and multiple ; Photometry, RI Keywords: planetary systems; planets and satellites: detection; stars: individual: HD 3167 Abstract: We report the discovery of two super-Earth-sized planets transiting the bright (V=8.94, K=7.07) nearby late G-dwarf HD 3167, using data collected by the K2 mission. The inner planet, HD 3167 b, has a radius of 1.6R and an ultra-short orbital period of only 0.96d. The outer planet, HD 3167 c, has a radius of 2.9R and orbits its host star every 29.85 days. At a distance of just 45.8±2.2pc, HD3167 is one of the closest and brightest stars hosting multiple transiting planets, making HD 3167 b and c well suited for follow-up observations. The star is chromospherically inactive with low rotational line-broadening, ideal for radial velocity observations to measure the planets' masses. The outer planet is large enough that it likely has a thick gaseous envelope that could be studied via transmission spectroscopy. Planets transiting bright, nearby stars like HD 3167 are valuable objects to study leading up to the launch of the James Webb Space Telescope. Description: Kepler observed HD 3167 between 2016 January 3 and March 23 during Campaign 8 of its K2 mission. We observed HD 3167 with the Tillinghast Reflector Echelle Spectrograph (TRES) on the 1.5m telescope at the Fred L. Whipple Observatory on Mt. Hopkins, AZ. We acquired one spectrum with a spectral resolving power of R=44000 on 2016 July 11. We observed HD 3167 with the Robo-AO adaptive optics system installed at the 2.1m telescope at Kitt Peak National Observatory. We observed HD 3167 with an i'-band filter on 2016 July 11, taking images at a rate of 8.6Hz for a total of 120s. Objects: ---------------------------------------------------------------- RA (ICRS) DE Designation(s) (Period) ---------------------------------------------------------------- 00 34 57.52 +04 22 53.3 HD 3167 = TYC 13-894-1 00 34 57.52 +04 22 53.3 HD 3167 b = HD 3167b (P=0.9596) 00 34 57.52 +04 22 53.3 HD 3167 c = HD 3167c (P=29.845) ---------------------------------------------------------------- File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file fig1.dat 20 3428 K2 light curve of HD 3167 curve.dat 11 81 Robo-AO contrast curve
Description of file: hd3167robo-ao.fits The Robo-AO image of HD 3167 in FITS. The exposure time was 120 seconds and the filter was i'-band. The image is composed of many 116ms exposures which were shifted and coadded in post-processing using HD 3167 as a tip/tilt guide star. See also: J/ApJS/224/2 : K2 EPIC stellar properties for 138600 targets (Huber+, 2016) J/ApJS/224/12 : Kepler planetary candidates. VII. 48-month (Coughlin+, 2016) J/ApJS/222/14 : Planetary candidates from 1st yr K2 mission (Vanderburg+, 2016) J/ApJ/822/86 : False positive proba. for Q1-Q17 DR24 KOIs (Morton+, 2016) J/ApJ/809/77 : Transiting Exoplanet Survey Satellite (TESS) (Sullivan+, 2015) J/other/Nat/486.375 : Stellar parameters of KOI stars (Buchhave+, 2012) Byte-by-byte Description of file: fig1.dat
Bytes Format Units Label Explanations
1- 9 F9.4 d BJD [2560.7/2637.8] Barycentric Julian Date; BJD-2454833 11- 20 F10.8 --- RFlux [0.9986/1.0009] Relative flux
Byte-by-byte Description of file: curve.dat
Bytes Format Units Label Explanations
1- 5 F5.3 arcsec Sep [0.1/1.6] Angular separation from HD 3167 7- 11 F5.3 mag mag [0.4/6.2] Relative brightness of a nearby star at Sep which can be excluded at 5σ confidence; i-band
History: From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 13-Dec-2016
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

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