TrES-1b was discovered by the
Trans-Atlantic Exoplanet Survey by detecting the
transit of the planet across its parent star using a telescope. The discovery was confirmed by the
Keck Observatory using the
radial velocity method, which allowed its mass to be determined. In the
infrared panel, the colors reflect what our eyes might see if we could retune them to the invisible, infrared portion of the light spectrum. The hot star is less bright in infrared light than in visible and appears fainter. The warm planet peaks in infrared light, so is shown brighter. Their hues represent relative differences in temperature. Because the star is hotter than the planet, and because hotter objects give off more blue light than red, the star is depicted in blue, and the planet, red. The overall look of the planet is inspired by theoretical models of hot, gas giant planets. These "hot Jupiters" are similar to Jupiter in composition and mass, but are expected to look quite different at such high temperatures.
Radial velocity The
transit light-curve signature in the course of the TrES multi-site transiting planet survey, and confirmed the planetary nature of the companion via multicolor photometry and precise
radial velocity measurements. With this, the planet has an orbital period similar to that of
HD 209458 b, but about twice as long as those of the
Optical Gravitational Lensing Experiment (OGLE) transiting planets. Its mass is similar to that of HD 209458 b, but its radius is significantly smaller and fits the theoretical models without the need for an additional source of heat deep in the atmosphere, as has been invoked by some investigators for HD 209458 b. ==Rotation==