On the Transit Potential of the Planet Orbiting iota Draconis

TL;DR

This paper reevaluates the transit potential of the massive, eccentric planet orbiting iota Draconis, providing updated transit probability, ephemeris, and discussing observational prospects from ground and space.

Contribution

It offers a revised analysis of the transit likelihood for the iota Draconis planet, incorporating new data and stellar variability analysis, which enhances the understanding of its transit prospects.

Findings

Revised transit probability for the planet is higher than previously estimated.

New radial velocity measurements improve orbital parameter accuracy.

Discussion of observational strategies from ground and space telescopes.

Abstract

Most of the known transiting exoplanets are in short-period orbits, largely due to the bias inherent in detecting planets through the transit technique. However, the eccentricity distribution of the known radial velocity planets results in many of those planets having a non-negligible transit probability. One such case is the massive planet orbiting the giant star iota Draconis, a situation where both the orientation of the planet's eccentric orbit and the size of the host star inflate the transit probability to a much higher value than for a typical hot Jupiter. Here we present a revised fit of the radial velocity data with new measurements and a photometric analysis of the stellar variability. We provide a revised transit probability, an improved transit ephemeris, and discuss the prospects for observing a transit of this planet from both the ground and space.