Trans-Atlantic Exoplanet Survey

In this article, we will explore the topic of Trans-Atlantic Exoplanet Survey in depth, addressing its most relevant and current aspects. From its origins to its impact on today's society, through the different approaches and perspectives that have developed over time. This topic is of utmost importance today, since it has generated extensive debate and reflection in various areas, from politics to culture, and has marked a turning point in the way we address different problems. Throughout the development of this article, we will analyze the different aspects of Trans-Atlantic Exoplanet Survey, delving into its implications and generating a space for critical reflection around this phenomenon.

"TrES" redirects here. For other uses, see tres (disambiguation).

The Trans-Atlantic Exoplanet Survey, or TrES, used three 4-inch (10 cm) telescopes located at Lowell Observatory, Palomar Observatory, and Teide Observatory to locate exoplanets. It was made using the network of small, relatively inexpensive telescopes designed to look specifically for planets orbiting bright stars using the transit method. The array used 4-inch Schmidt telescopes having CCD cameras and automated search routines. The survey was created by David Charbonneau of the Center for Astrophysics, Timothy Brown of the National Center for Atmospheric Research, and Edward Dunham of Lowell Observatory.[1]

The TrES survey is no longer operational.

Discoveries

The TrES project discovered a total of five planets in its years of operation. All were discovered using the transit method. Note that the discovery papers do not use the "b" suffix typically used in extrasolar planet designations. While forms with and without the b are used in the literature, the table here uses the designations assigned by the discoverers.

Star Constellation Right
ascension 		Declination App.
mag. 		Distance
(ly) 		Spectral
type 		Planet Mass
(MJ) 		Radius
(RJ) 		P
(days) 		a
(AU) 		e i
(°) 		Discovery
year
GSC 02652-01324[1] Lyra 19h 04m 09s +36° 37′ 57″ 11.79 512 K0V TrES-1 0.61 1.081 3.030065 0.0393 0.135 88.2 2004
GSC 03549-02811(*)[2] Draco 19h 07m 14s +49° 18′ 59″ 11.41 750 ± 30 G0V TrES-2 1.199 1.272 2.47063 0.03556 0 83.62 2006
GSC 03089-00929[3] Hercules 17h 52m 07s +37° 32′ 46″ 12.4 1300 G TrES-3 1.92 1.295 1.30619 0.0226 ? 82.15 2007
GSC 02620-00648(*)[4] Hercules 17h 53m 13s +37° 12′ 42″ 11.592 1400 F8 TrES-4 0.919 1.799 3.553945 0.05091 0 82.86 2007
GSC 03949-00967[5] Cygnus 20h 20m 53s +59° 26′ 56″ 13.718 1170 G TrES-5 1.778 1.209 1.4822446 0.02446 ? 84.529 2011
Note: (*) indicates that the planet orbits one of the stars in a binary star system.

See also

TrES light curves of the Kepler field are available at the NASA Exoplanet Archive

Similar exoplanet discovery projects

Exoplanet hunting spacecraft

References

  1. ^ a b Alonso, Roi; et al. (2004). "TrES-1: The Transiting Planet of a Bright K0V Star". The Astrophysical Journal Letters. 613 (2): L153 – L156. arXiv:astro-ph/0408421. Bibcode:2004ApJ...613L.153A. doi:10.1086/425256.
  2. ^ O'Donovan, Francis T.; et al. (2006). "TrES-2: The First Transiting Planet in the Kepler Field". The Astrophysical Journal Letters. 651 (1): L61 – L64. arXiv:astro-ph/0609335. Bibcode:2006ApJ...651L..61O. doi:10.1086/509123.
  3. ^ O'Donovan, Francis T.; et al. (2007). "TrES-3: A Nearby, Massive, Transiting Hot Jupiter in a 31 Hour Orbit". The Astrophysical Journal Letters. 663 (1): L37 – L40. arXiv:0705.2004. Bibcode:2007ApJ...663L..37O. doi:10.1086/519793.
  4. ^ Mandushev, Georgi; et al. (2007). "TrES-4: A Transiting Hot Jupiter of Very Low Density". The Astrophysical Journal Letters. 667 (2): L195 – L198. arXiv:0708.0834. Bibcode:2007ApJ...667L.195M. doi:10.1086/522115.
  5. ^ Mandushev, Georgi; et al. (2011). "TrES-5: A Massive Jupiter-sized Planet Transiting A Cool G-dwarf". The Astrophysical Journal. 741 (2). 114. arXiv:1108.3572. Bibcode:2011ApJ...741..114M. doi:10.1088/0004-637X/741/2/114.