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Dust in debris disks is produced by colliding or evaporating planetesimals,remnants of the planet formation process. Warm dust disks, known by theiremission at < 24 micron, are rare (4% of FGK main sequence stars) andespecially interesting because they trace material in the region likely to hostterrestrial planets, where the dust has a very short dynamical lifetime.Statistical analyses of the source counts of excesses as found with the mid-IRWide Field Infrared Survey Explorer (WISE) suggest that warm-dust candidatesfound for the Kepler transiting-planet host-star candidates can be explained byextragalactic or galactic background emission aligned by chance with the targetstars. These statistical analyses do not exclude the possibility that a givenWISE excess could be due to a transient dust population associated with thetarget. Here we report Herschel/PACS 100 and 160 micron follow-up observationsof a sample of Kepler and non-Kepler transiting-planet candidates' host stars,with candidate WISE warm debris disks, aimed at detecting a possible colddebris disk in any of them. No clear detections were found in any one of theobjects at either wavelength. Our upper limits confirm that most objects in thesample do not have a massive debris disk like that in beta Pic. We also showthat the planet-hosting star WASP-33 does not have a debris disk comparable tothe one around eta Crv. Although the data cannot be used to rule out rare warmdisks around the Kepler planet-hosting candidates, the lack of detections andthe characteristics of neighboring emission found at far-IR wavelengths supportan earlier result suggesting that most of the WISE-selected IR excesses aroundKepler candidate host stars are likely due to either chance alignment withbackground IR-bright galaxies and/or to interstellar emission.

Herschel/PACS photometry of transiting-planet host stars with candidate warm debris disks