Detection of Thermal Emission from an Extrasolar Planet

  title={Detection of Thermal Emission from an Extrasolar Planet},
  author={David Charbonneau and Lori E. Allen and S. Thomas Megeath and Guillermo Torres and Roi Alonso and Timothy M. Brown and Ronald L. Gilliland and David W. Latham and Georgi I. Mandushev and Francis T. O'Donovan and Alessandro Sozzetti},
  journal={The Astrophysical Journal},
  pages={523 - 529}
We present Spitzer Space Telescope infrared photometric time series of the transiting extrasolar planet system TrES-1. The data span a predicted time of secondary eclipse, corresponding to the passage of the planet behind the star. In both bands of our observations, we detect a flux decrement with a timing, amplitude, and duration as predicted by published parameters of the system. This signal represents the first direct detection of (i.e., the observation of photons emitted by) a planet… 

A Ground‐based Search for Thermal Emission from the Exoplanet TrES‐1

Eclipsing planetary systems give us an important window on extrasolar planet atmospheres. By measuring the depth of the secondary eclipse, when the planet moves behind the star, we can estimate the

Infrared radiation from an extrasolar planet

A class of extrasolar giant planets—the so-called ‘hot Jupiters’ (ref. 1)—orbit within 0.05 au of their primary stars (1 au is the Sun–Earth distance). These planets should be hot and so emit

A spectrum of an extrasolar planet

Observations of the infrared spectrum of the transiting extrasolar planet HD 209458b reveal a hot thermal continuum for the planetary spectrum, with an approximately constant ratio to the stellar flux over this wavelength range.

Strong Infrared Emission from the Extrasolar Planet HD 189733b

We report detection of strong infrared thermal emission from the nearby (d = 19 pc) transiting extrasolar planet HD 189733b by measuring the flux decrement during its prominent secondary eclipse. A 6

Resolving the Surfaces of Extrasolar Planets with Secondary Eclipse Light Curves

We present a method that employs the secondary eclipse light curves of transiting extrasolar planets to probe the spatial variation of their thermal emission. This technique permits an observer to

Rapid heating of the atmosphere of an extrasolar planet

8-μm photometric observations of the planet HD 80606b during a 30-hour interval bracketing the periastron passage of its extremely eccentric 111.4-day orbit indicate the global heating rate is ∼4.5 h, in comparison with 3–5 days in Earth’s stratosphere, and a secondary eclipse for the planet is detected.

The hottest planet

Direct detection of thermal emission from the smallest known transiting planet, HD 149026b, that indicates a brightness temperature of 2,300 ± 200 K at 8 µm is reported, which may give rise to novel atmospheric properties yet to be investigated.

3.8-μm photometry during the secondary eclipse of the extrasolar planet HD 209458b

We report infrared photometry of the extrasolar planet HD 209458b during the time of secondary eclipse (planet passing behind the star). Observations were acquired during two secondary eclipses at

Hot nights on extrasolar planets: mid‐infrared phase variations of hot Jupiters

We present results from Spitzer Space Telescope observations of the mid-infrared phase variations of three short-period extrasolar planetary systems: HD 209458, HD 179949 and 51 Peg. We gathered


We present here the results of our observations of TrES-2 using the Infrared Array Camera on Spitzer. We monitored this transiting system during two secondary eclipses, when the planetary emission is



Infrared radiation from an extrasolar planet

A class of extrasolar giant planets—the so-called ‘hot Jupiters’ (ref. 1)—orbit within 0.05 au of their primary stars (1 au is the Sun–Earth distance). These planets should be hot and so emit

Detection of Planetary Transits Across a Sun-like Star

High-precision, high-cadence photometric measurements of the star HD 209458 are reported, which is known from radial velocity measurements to have a planetary-mass companion in a close orbit and the detailed shape of the transit curve due to both the limb darkening of thestar and the finite size of the planet is clearly evident.

An extrasolar planet that transits the disk of its parent star

Planets orbiting other stars could in principle be found through the periodic dimming of starlight as a planet moves across—or ‘transits’—the line of sight between the observer and the star.

Detection of an Extrasolar Planet Atmosphere

We report high-precision spectrophotometric observations of four planetary transits of HD 209458, in the region of the sodium resonance doublet at 589.3 nm. We find that the photometric dimming

Infrared Observations during the Secondary Eclipse of HD 209458b. II. Strong Limits on the Infrared Spectrum Near 2.2 μm

We report observations of the transiting extrasolar planet, HD 209458b, designed to detect the secondary eclipse. We employ the method of "occultation spectroscopy," which searches in combined light

TrES-1: The Transiting Planet of a Bright K0 V Star

We report the detection of a transiting Jupiter-sized planet orbiting a relatively bright (V = 11.79) K0 V star. We detected the transit light-curve signature in the course of the TrES multisite

Hubble Space Telescope Time-Series Photometry of the Transiting Planet of HD 209458

We have observed four transits of the planet of HD 209458 using the STIS spectrograph on the Hubble Space Telescope (HST). Summing the recorded counts over wavelength between 582 and 638 nm yields a

A Comparison of Observationally Determined Radii with Theoretical Radius Predictions for Short-Period Transiting Extrasolar Planets

Two extrasolar planets, HD 209458b and TrES-1, are currently known to transit bright parent stars for which physical properties can be accurately determined. The two transiting planets have very

Photometric Light Curves and Polarization of Close-in Extrasolar Giant Planets

The close-in extrasolar giant planets (CEGPs), ≲0.05 AU from their parent stars, may have a large component of optically reflected light. We present theoretical optical photometric light curves and

The Evolution of Irradiated Planets: Application to Transits

Extending the theory that we derived recently for HD 209458b to different cases of strongly irradiated gaseous exoplanets, we have calculated the consistent evolution of a new transiting planet,