Abstract
Context.Co-orbital bodies are the byproduct of planet formation and evolution, as we know from the solar system. Although planet-size co-orbitals do not exists in our planetary system, dynamical studies show that they can remain stable for long periods of time in the gravitational well of massive planets. Should they exist, their detection is feasible with the current instrumentation.Aims.In this paper, we present new ground-based observations searching for these bodies co-orbiting with nine close-in (P< 5 days) planets, using various observing techniques. The combination of all of these techniques allows us to restrict the parameter space of any possible trojan in the system.Methods.We used multi-technique observations, comprised of radial velocity, precision photometry, and transit timing variations, both newly acquired in the context of the TROY project and publicly available, to constrain the presence of planet-size trojans in the Lagrangian points of nine known exoplanets.Results.We find no clear evidence of trojans in these nine systems through any of the techniques used down to the precision of the observations. However, this allows us to constrain the presence of any potential trojan in the system, especially in the trojan mass or radius vs. libration amplitude plane. In particular, we can set upper mass limits in the super-Earth mass regime for six of the studied systems.
Highlights
The development of state-of-the-art instrumentation and spacebased facilities in recent decades has boosted the discoveryBased on observations collected at the Centro Astronómico Hispano Alemán (CAHA) at Calar Alto, operated jointly by the Max-Planck Institut für Astronomie and the Instituto de Astrofísica de Andalucía (CSIC).Partly based on data obtained with the STELLA robotic telescopes in Tenerife, an AIP facility jointly operated by AIP and IAC.Based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under European Southern Observatory (ESO) programs 297.C-5051, 098.C-0440(A), and 298.C-5009 of extrasolar planets up to several thousands of detections1
We present an extensive amount of dedicated radial velocity and light curve data of nine of these systems to look for the planet-mass co-orbital candidates found in our previous work
Results per system Based on the analysis of the multi-technique data presented in Sect. 3, we can constrain the presence of co-orbital bodies in the surroundings of the Lagrangian points in these nine systems
Summary
Based on observations collected at the Centro Astronómico Hispano Alemán (CAHA) at Calar Alto, operated jointly by the Max-Planck Institut für Astronomie and the Instituto de Astrofísica de Andalucía (CSIC). Target sample Nine systems were selected for further follow up from our radial velocity analysis in Lillo-Box et al (2018a) because these systems presented hints of some mass imbalance between the two Lagrangian points. The WiFSIP field of view is 22 × 22 arcmin and the plate scale corresponds to 0.322 arcsec/pix In this case, given the robotic nature of the telescope and in order to increase the execution probability of the program, we asked observations of three times three hours around the Lagrangian point midtransit time, starting at random phases between two hours and half an hour before the start of the expected transit.
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