No planet for HD 166435

By D. Queloz, G. Henry, J. Sivan, S. Baliunas, J. Beuzit, R. Donahue, M. Mayor, D. Naef, C. Perrier, S. Udry. 2001

660 citations recorded by the source corpus.

The G0 V star HD 166435 has been observed by the ber-fed spectrograph ELODIE as one of the targets in the large extra-solar planet survey that we are conducting at the Observatory of Haute-Provence. We detected coherent, low-amplitude, radial-velocity variations with a period of 3.7987 days, suggesting a possible close-in planetary companion. Subsequently, we initiated a series of high-precision photometric observations to search for possible planetary transits and an additional series of Ca II H and K observations to measure the level of surface magnetic activity and to look for possible rotational modulation. Surprisingly, we found the star to be photometrically variable and magnetically active. A detailed study of the phase stability of the radial-velocity signal revealed that the radial-velocity variability remains coherent only for durations of about 30 days. Analysis of the time variation of the spectroscopic line proles using line bisectors revealed a correlation between radial velocity and line-bisector orientation. All of these observations, along with a one-quarter cycle phase shift between the photometric and the radial-velocity variations, are well explained by the presence of dark photospheric spots on HD 166435. We conclude that the radial-velocity variations are not due to gravitational interaction with an orbiting planet but, instead, originate from line-prole changes stemming from star spots on the surface of the star. The quasi-coherence of the radial-velocity signal over more than two years, which allowed a fair t with a binary model, makes the stability of this star unusual among other active stars. It suggests a stable magnetic eld orientation where spots are always generated at about the same location on the surface of the star.

Subfields: Astronomy and Astrophysics, Instrumentation, Statistical and Nonlinear Physics

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Citations in the corpus

WASP-121 b: a hot Jupiter close to tidal disruption transiting an active F star (2015, methodology): “The cross-correlation function (CCF) bisector span (Queloz et al. 2001) and FWHM values are plotted in Fig.”
DISCOVERY OF A TRANSITING PLANET AND EIGHT ECLIPSING BINARIES IN HATNet FIELD G205 (2009, background): “In that case, the “bisector span” of the average spectral line should vary periodically with amplitude and phase similar to the measured velocities themselves (Queloz et al. 2001; Mandushev et al. 2005).”
Five New Multicomponent Planetary Systems (2005, background): “Queloz et al. (2001) and Paulson et al. (2004) have presented several examples of periodic radial velocity variations in solar-type stars caused by photospheric spots and plages.”
HST hot-Jupiter transmission spectral survey: detection of potassium in WASP-31b along with a cloud deck and Rayleigh scattering (2014, background): “Since the 8.6- day stellar rotation period and the 3.4-day planetary orbital period are well separated, the radial velocity variations are clearly due to planetary reflex motion with very little jitter caused by surface activity (e.g., Queloz et al. 2001; Paulson et al. 2004).”
CHROMOSPHERIC ACTIVITY AND JITTER MEASUREMENTS FOR 2630 STARS ON THE CALIFORNIA PLANET SEARCH (2010, background): “Queloz et al. (2001) reported the remarkable case of HD 166435, a young G0V star with quasi-period radial velocities that were correlated to line bisector variations and Ca II emission.”
Extrasolar planets and brown dwarfs around A-F type stars. II. A planet found with ELODIE around the F6V star HD 33564 (2005, background): “First, the bisector shape of the lines is estimated on the cross-correlation function (inverse bisector slope) in the same way as in Queloz et al. (2001a).”
The CARMENES search for exoplanets around M dwarfs (2018, background): “These periodic variations induce signals in the RV data that could be wrongly interpreted as of planetary origin (e.g. Queloz et al. 2001; Robertson et al. 2014; Sarkis et al. Article number, page 1 of 15 ar X iv :1 81 0.”
The planet search programme at the ESO CES and HARPS - IV. The search for Jupiter analogues around solar-like stars (2012, methodology): “To test this, one can analyse theR′HK-index and the shape of the cross-correlation function (CCF) function in particular its full width at half maximum (FWHM) and bisector span (BIS, Queloz et al. 2001) which are measures for the averaged stellar line width and asymmetry, respectively.”
THE CALIFORNIA PLANET SURVEY. I. FOUR NEW GIANT EXOPLANETS (2010, methodology): “Therefore, pho- tometric observations can help to establish whether observed radial velocity variations in a star are due to reflex motion caused by a planetary companion or due to the effects of stellar activity (e.g., Queloz et al. 2001; Paulson et al. 2004).”
Search for exoplanets with the radial-velocity technique : quantitative diagnostics of stellar activity (2007, methodology): “This case is similar to the one of HD 166 435 (Queloz et al. 2001).”
HAT-P-7b: An Extremely Hot Massive Planet Transiting a Bright Star in the Kepler Field (2008, background): “In that case the “bisector span” of the average spectral line should vary periodically with amplitude and phase similar to the measured velocities themselves (Queloz et al. 2001; Mandushev et al. 2005).”
SOAP 2.0: A TOOL TO ESTIMATE THE PHOTOMETRIC AND RADIAL VELOCITY VARIATIONS INDUCED BY STELLAR SPOTS AND PLAGES (2014, background): “These correlations are often a powerful diagnostic to decide if the observed RV signal is of activity or planetary origin (e.g. Boisse et al. 2009; Bonfils et al. 2007; Queloz et al. 2001).”
WASP-19b: THE SHORTEST PERIOD TRANSITING EXOPLANET YET DISCOVERED (2010, background): “Table 1 presents the RV measurements of WASP-19 at each Barycentric Julian date, the 1σ Poisson errors on the velocities, and the line bisector span measurements (Gray 1988; Queloz et al. 2001).”
TW Hydrae: evidence of stellar spots instead of a Hot Jupiter (2008, methodology): “To test this, we computed the BIS values for our CORALIE measurements (for the definition see Queloz et al. 2001).”
Magnetospheric accretion-ejection processes in the classical T Tauri star AA Tauri (2006, methodology): “Following the method outlined by Queloz et al. (2001), we computed the bissector of the photospheric cross-correlation function (CCF) at each phase (cf. Fig.”
The HARPS search for southern extra-solar planets. X. A m sin i = 11 M_â planet around the nearby spotted M dwarf GJ 674 (2007, background): “Observationally, these inhomogeneities translate into flux variations, as well as into changes of both the shape and the centroid of spectral lines (Saar & Donahue 1997; Queloz et al. 2001).”
HD 147506b: A Supermassive Planet in an Eccentric Orbit Transiting a Bright Star (2007, result): “…profiles arising from contamination of the spectrum by the presence of a binary with a period of 5.63 days, we would expect the bisector spans (which measure line asymmetry) to vary with this period and with an amplitude similar to the velocities (see, e.g., Queloz et al. 2001; Torres et al. 2005).”
TrES-2: The First Transiting Planet in the Kepler Field (2006, result): “Within the measurement error (∼0.5 km s 1), the RVs are constant with a mean velocity of and a scatter of 10.56 km s 0.55 .”
RETIRED A STARS AND THEIR COMPANIONS. III. COMPARING THE MASS–PERIOD DISTRIBUTIONS OF PLANETS AROUND A-TYPE STARS AND SUN-LIKE STARS (2009, background): “Queloz et al. (2001) and Paulson et al. (2004) have found periodic radial velocity variations in solartype stars that are caused by starspots.”