- Paper title: A Search for Additional Planets in Five of the Exoplanetary Systems Studied by the NASA EPOXI Mission
- Authors: Sarah Ballard, Jessie L. Christiansen, David Charbonneau, Drake Deming, Matthew J. Holman, Michael F. A’Hearn, Dennis D. Wellnitz, Richard K. Barry, Marc J. Kuchner, Timothy A. Livengood, Tilak Hewagama, Jessica M. Sunshine, Don L. Hampton, Carey M. Lisse, Sara Seager, Joseph F. Veverka
- First author’s affiliation: Harvard-Smithsonian Center for Astrophysics
In a previous post, I described NASA’s EPOXI mission to use the Deep Impact spacecraft to detect transiting exoplanets. In this paper, the authors use EPOXI data to search for additional planets in five known exoplanetary systems. The planetary systems investigated are HAT-P-4, TrES-3, TrES-2, WASP-3, and HAT-P-7. The systems are named after the surveys that detected them: the HATNet (Hungarian Automated Telescope Network) Project, the Trans-Atlantic Exoplanet Survey, and the Wide Angle Search for Planets. Although the authors do not find any new candidate planets in these systems, they are able to constrain the presence of other transiting planets in the systems.
As Ellie explained in her discussion of the Kepler mission, a transiting planets is detected due to the dip in the apparent brightness of the host star. Accordingly, Ballard et al. look for the signatures of additional planets in these systems by monitoring the brightness of their target stars for approximately two-week intervals and searching for drops in brightness that are not due to the known planet. They did not find any evidence of additional transits, but there could be other planets in these systems that did not transit during their observations or produced transits that were too small for Ballard et al. to detect. In order to determine their sensitivity to transiting planets with different radii and orbital periods, the authors inject model planetary transits into their acquired light curves and then determine whether their software would be able to detect those planets.
As shown in the figure, the authors would have been sensitive to transiting Saturn-sized planets with orbital periods of 0.5 to 2.5 days for all of the stars and with longer orbital periods (up to 7 days) for the stars with the most complete light curves. In the HAT-P-4, TrES-3, and WASP-3 systems the authors would also have been able to detect sub-Saturn-sized companions, and in the TrES-2 system, they could have detected planets as small as Neptune. They also constrain the radii of planets in orbital resonances with the known planets. For instance, the authors would have been sensitive to 65% of 4 REarth planets in the 3:2 resonance with TrES-2b and to >90% of 5 REarth planets in the 3:2 or 2:1 resonance. These detection limits and the other limits discussed in the paper allow the authors to place significant constraints on the radii and orbital periods of additional planets in these systems.