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| TrES-1 | |
|---|---|
| Name | TrES-1 |
| Discoverers | Alonso, Charbonneau, Brown, Mandushev |
| Discovery site | Lowell Observatory, Palomar Observatory, Palomar Transient Factory |
| Discovery method | Transit photometry |
| Discovery year | 2004 |
| Semimajor axis | 0.0393 AU |
| Eccentricity | 0.0 (assumed) |
| Period | 3.03 d |
| Mass | 0.76 M_J |
| Radius | 1.08 R_J |
| Density | ~0.7 g/cm^3 |
| Temperature | ~1150 K |
TrES-1 is a transiting extrasolar planet discovered in 2004 by the Trans-Atlantic Exoplanet Survey teams using small-aperture telescopes and follow-up observations. The planet orbits a K-type dwarf in the constellation Lyra and was one of the earliest hot Jupiters found by ground-based transit surveys, marking a milestone comparable to discoveries by teams operating instruments like the Kepler space telescope, Hubble Space Telescope, and Spitzer Space Telescope. Its detection stimulated coordinated follow-up across observatories including the W. M. Keck Observatory, the Harvard-Smithsonian Center for Astrophysics, and the Massachusetts Institute of Technology-led groups.
The discovery announcement credited a collaboration of observers and institutions including the Lowell Observatory team, the California Institute of Technology observers, the Harvard-Smithsonian Center for Astrophysics, and the Smithsonian Astrophysical Observatory, with lead authors from the Instituto de Astrofísica de Canarias and the Instituto de Astrofísica de Andalucía. The detection used transit photometry similar to methods employed by projects such as SuperWASP, HATNet, and the OGLE project, and required radial-velocity confirmation with spectrographs at the Keck Observatory and the Palomar Observatory to exclude false positives like eclipsing binaries flagged in surveys by the European Southern Observatory and the Anglo-Australian Telescope programs. The discovery spurred comparisons in the literature to landmark detections like 51 Pegasi b and HD 209458 b by teams at Geneva Observatory and the Haute-Provence Observatory.
The host is a K-type main-sequence dwarf cataloged by surveys like the Two Micron All Sky Survey and the Tycho-2 Catalogue, characterized by effective temperature estimates refined using spectra from instruments operated by the National Optical Astronomy Observatory and the European Southern Observatory. Stellar parameters were cross-checked against models from the Geneva stellar evolution group and Yale-Yonsei isochrones, and photometry from the Sloan Digital Sky Survey and the Hipparcos mission provided parallax-based distance constraints. Follow-up spectroscopy by researchers affiliated with the Space Telescope Science Institute and the Carnegie Institution for Science helped establish metallicity and activity levels, with comparisons drawn to well-studied stars such as HD 189733 and HD 209458 in catalogs maintained by the SIMBAD database and the NASA Exoplanet Archive.
The planet has physical parameters determined through combined transit and radial-velocity analyses carried out by teams collaborating with institutions like the Harvard-Smithsonian Center for Astrophysics, the Massachusetts Institute of Technology, and the Max Planck Institute for Astronomy. Mass and radius estimates place it in the hot Jupiter class alongside objects cataloged by projects such as WASP, HAT, and CoRoT, comparable in bulk properties to planets like OGLE-TR-56 b and HD 209458 b. Interior structure modeling invoked equations of state developed by researchers at the Jet Propulsion Laboratory and the Institute for Advanced Study, and considerations of irradiation-driven inflation referenced work from Princeton University and the University of Cambridge. Comparative studies have used frameworks from the Royal Astronomical Society and the American Astronomical Society to place the planet within statistical samples compiled by the Exoplanet.eu database and the NASA Exoplanet Science Institute.
The target became a focus for multiwavelength campaigns using observatories including the Spitzer Space Telescope, the Hubble Space Telescope, the Chandra X-ray Observatory, and ground-based facilities like the W. M. Keck Observatory, the Very Large Telescope, and the Calar Alto Observatory. Photometric monitoring campaigns involved collaborations among institutions such as the California Institute of Technology, the Jet Propulsion Laboratory, and the University of Arizona, while spectroscopic transit and occultation observations engaged teams from the Max Planck Institute for Extraterrestrial Physics and the European Southern Observatory. Time-series analyses employed methods from the Carnegie Institution and the Institute for Astronomy, University of Hawaii, and were compared to transit timing studies produced by groups at Yale University and the University of Exeter.
Early attempts to probe the atmosphere used secondary-eclipse photometry with the Spitzer Space Telescope and transmission spectroscopy with the Hubble Space Telescope, interpreted using radiative-transfer codes developed by researchers at the University of Chicago and the University of California, Santa Cruz. Reported constraints addressed molecular species and thermal inversions discussed in work from institutions such as the University of Amsterdam, the University of Oxford, and the University of Bern, with comparisons to atmospheric detections on HD 209458 b and HD 189733 b from teams at the University of Geneva and the Institut d'Astrophysique de Paris. Analyses considered opacity sources modeled by groups at the Max Planck Institute for Solar System Research and the University of Southampton, and chemical kinetics frameworks from the Jet Propulsion Laboratory and the University of Cambridge informed interpretations of possible water vapor, carbon monoxide, and methane signatures.
Orbital parameters were refined using radial-velocity datasets from the W. M. Keck Observatory and photometric baselines coordinated by the Trans-Atlantic Exoplanet Survey and follow-up networks including the Las Cumbres Observatory Global Telescope Network and the Universidad de Chile teams. Dynamical stability analyses referenced N-body simulation techniques developed at Princeton University and the University of California, Santa Cruz, with contextual discussion drawing on migration theories advanced by researchers at the University of Toronto, the University of Arizona, and the Swiss Federal Institute of Technology Zurich. Tidal interaction studies invoked formulations from institutions such as the University of Cambridge and the University of California, Berkeley, while long-term stability comparisons were made with compact systems cataloged by the European Southern Observatory and by the Kepler mission teams.
The discovery catalyzed development of small-aperture transit surveys like TrES itself, SuperWASP, HATNet, and KELT, and informed strategy for space missions such as the Kepler mission, the Transiting Exoplanet Survey Satellite, and the CHEOPS mission. The planet’s role in early comparative atmospheric and structural studies connected research groups at institutions including the Harvard-Smithsonian Center for Astrophysics, the Massachusetts Institute of Technology, and the Max Planck Society, influencing theoretical work from Princeton University, the University of Cambridge, and the University of Chicago. It features in pedagogical materials and review articles produced by the American Astronomical Society and the Royal Astronomical Society, and remains part of legacy datasets curated by the NASA Exoplanet Archive, the European Space Agency, and the Centre de Données astronomiques de Strasbourg.