Abstract
Hot Jupiters seem to get rarer with decreasing stellar mass. The goal of the Pan-Planets transit survey was the detection of such planets and a statistical characterization of their frequency. Here, we announce the discovery and validation of two planets found in that survey, Wendelstein-1b and Wendelstein-2b, which are two short-period hot Jupiters that orbit late K host stars. We validated them both by the traditional method of radial velocity measurements with the HIgh Resolution Echelle Spectrometer and the Habitable-zone Planet Finder instruments and then by their Transit Color Signature (TraCS). We observed the targets in the wavelength range of 4000−24 000 Å and performed a simultaneous multiband transit fit and additionally determined their thermal emission via secondary eclipse observations. Wendelstein-1b is a hot Jupiter with a radius of 1.0314−0.0061+0.0061 RJ and mass of 0.592−0.129+0.0165 MJ, orbiting a K7V dwarf star at a period of 2.66 d, and has an estimated surface temperature of about 1727−90+78 K. Wendelstein-2b is a hot Jupiter with a radius of 1.1592−0.0210+0.0204 RJ and a mass of 0.731−0.311+0.0541 MJ, orbiting a K6V dwarf star at a period of 1.75 d, and has an estimated surface temperature of about 1852−140+120 K. With this, we demonstrate that multiband photometry is an effective way of validating transiting exoplanets, in particular for fainter targets since radial velocity follow-up becomes more and more costly for those targets.
Highlights
The field of exoplanets is undergoing rapid changes with the impact of space-based telescopes and their sheer number of candidate discoveries
We observed the targets in the wavelength range of 4000−24 000 Å and performed a simultaneous multiband transit fit and determined their thermal emission via secondary s1poetc.afa1lrrai5tpiba9csot2ueua+−loat00pb..r100es22f8r01eoi540ror2vRdfa+−aJ11toii24anfo00ntn2eKds.r6..at6WWamrdgei,atneshatdsnsetdohslsfiihnts0ea,c.isew7na3-re1na1bdd+−ei00esia..sm53tli41am11voehnMalostoetJtrcd,Jaiouttsyerpubirftitohfteailarnlctowgewmitate-uhuKmlpta6ipbbVreaaerndacddtiowuumprsaehreofosofstfm1otaa.m0obr3roeae1tutr4atayn+−1p00di7..se002m00ra667in11oo+−dRr79ee80JfoKfcfaeo.n1csWd.tt7ilv5ymeendfaowd,sresaalntyoshdtfoeo0hisfn.ea5v-st29aaabl2rin−+gdi00seea..t11stas26itn.95ihmgMoattJtrJe,audnopsrsibituteiirtnrifnagwcgeietaxhtoKeapm7lrapVanededritauwsts,uaoirrneff Key words. planets and satellites: detection – planets and satellites: gaseous planets – stars: low-mass – techniques: image processing – techniques: photometric – occultations
Based on observations obtained with the Hobby-Eberly Telescope, which is a joint project of the University of Texas at Austin, the Pennsylvania State University, Stanford University, Ludwig-MaximiliansUniversität München, and Georg-August-Universität Göttingen
Summary
The field of exoplanets is undergoing rapid changes with the impact of space-based telescopes and their sheer number of candidate discoveries. 1 and 2 show the light curves yielded by the Pan-Planets survey (black dots) and the initial WWFI follow-up (red diamonds) for the candidates PP140-14 711/Wendelstein-1b and PP12721 645/Wendelstein-2b, respectively, including the best-fit model (blue line) Based on this survey and its improved photometry over Pan-Planets, we already disregarded a number of candidates as false positive detections of eclipsing binaries. We can create so-called night sky flats by masking out stars in every image and stacking those pattern series into one frame, filling the gaps This allows for the identification and removal of perturbation sources like hot and cold pixels, stray light and fixed pattern noises by on-sky calibration without the need for any additional overhead. If the data are dominated by photon noise, the algorithm cannot identify the systematic effects as accurately and applies less corrections
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