GSC 03549-02811

GSC 03549-02811 and TrES-2b as seen from the Kepler spacecraft. Celestial north is to the left.
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Draco
A
Right ascension 19h 07m 14.0376s[1]
Declination +49° 18′ 59.091″[1]
Apparent magnitude (V) 11.41
B
Right ascension ~19h 07m 14s[2]
Declination ~+49° 18′ 59″[2]
Characteristics
A
Spectral type G0V[3]
Apparent magnitude (B) ~12.030[4]
Apparent magnitude (V) 11.411±0.005[4]
Apparent magnitude (I) 11.07[2]
Apparent magnitude (Z) 11.04[2]
Apparent magnitude (J) 10.232±0.020[5]
Apparent magnitude (H) 9.920±0.026[5]
Apparent magnitude (K) 9.846±0.022[5]
Variable type Planetary transit[3]
B
Spectral type K[2]
Apparent magnitude (I) 14.73[2]
Apparent magnitude (Z) 14.47[2]
Astrometry
Proper motion (μ) RA: 5.434(15) mas/yr[1]
Dec.: 1.572(16) mas/yr[1]
Parallax (π)4.6308 ± 0.0116 mas[1]
Distance704 ± 2 ly
(215.9 ± 0.5 pc)
Details
A
Mass1.05[2] M☉
Radius1.000+0.036
−0.033[6] R☉
Temperature5850±50[6] K
Metallicity−0.15±0.1[6]
Age5.1+2.7
−2.3×109[6] years
B
Mass0.67[2] M☉
Other designations
TrES-2 Parent Star, V581 Dra, WDS J19072+4919AB, Kepler-1, KOI-1, KIC 11446443, TYC 3549-2811-1, 2MASS J19071403+4918590[4]
Database references
SIMBADdata

GSC 03549-02811 (sometimes referred to as Kepler-1, or either TrES-2A or TrES-2 parent star in reference to its exoplanet TrES-2b)[7] is a yellow main-sequence star similar to the Sun. This star is located approximately 704 light-years away in the constellation of Draco. The apparent magnitude of this star is 11.41, which means it is not visible to the naked eye but can be seen with a medium-sized amateur telescope on a clear dark night. The age of this star is about 5 billion years.[4]

Planetary system

In 2006 the exoplanet TrES-2b was discovered by the TrES program using the transit method. It is also within the field of view of the previously operational Kepler Mission planet-hunter spacecraft.[3] This system continues to be studied by other projects and the parameters are continuously improved.[6] The planet orbits the primary star.[2]

The GSC 03549-02811 planetary system[8][2]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b 1.199(52) MJ 0.03555(75) 2.4706133738(187) 0 (assumed) 83.908(9)° 1.189(25) RJ

Though TrES-2b is currently the darkest known exoplanet, reflecting less than 1 percent of local sunlight, it shows a faint red glow. This is because its surface is 1,100 °C, it is so hot that it glows red. It is assumed to be tidally locked to its parent star.[9]

Binary star

In 2008 a study was undertaken of fourteen stars with exoplanets that were originally discovered using the transit method through relatively small telescopes. These systems were re-examined with the 2.2M reflector telescope at the Calar Alto Observatory in Spain. This star system, along with two others, was determined to be a previously unknown binary star system. The previously unknown secondary star is a dim magnitude 15 K-type star separated by about 232 AU from the primary, appearing offset from the primary by about one arc second in the images. This discovery resulted in a significant recalculation of parameters for both the planet and the primary star.[2]

The Kepler mission

An image from Kepler with TrES-2b and another point of interest outlined. Celestial north is towards the lower left corner.

In March 2009 NASA launched the Kepler spacecraft. This spacecraft was a dedicated mission to discover extrasolar planets by the transit method from solar orbit. In April 2009 the project released the first light images from the spacecraft and TrES-2b was one of two objects highlighted in these images. Although TrES-2b is not the only known exoplanet in the field of view of this spacecraft it is the only one identified in the first-light images. This object is important for calibration and check-out.[10]

See also

References

  1. 1 2 3 4 5 Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv:2012.01533. Bibcode:2021A&A...649A...1G. doi:10.1051/0004-6361/202039657. S2CID 227254300. (Erratum: doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
  2. 1 2 3 4 5 6 7 8 9 10 11 12 Daemgen, S.; et al. (2009). "Binarity of transit host stars. Implications for planetary parameters". Astronomy and Astrophysics. 498 (2): 567–574. arXiv:0902.2179. Bibcode:2009A&A...498..567D. doi:10.1051/0004-6361/200810988. S2CID 9893376.
  3. 1 2 3 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.
  4. 1 2 3 4 "Kepler-1". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2009-04-22.
  5. 1 2 3 Skrutskie, Michael F.; et al. (1 February 2006). "The Two Micron All Sky Survey (2MASS)". The Astronomical Journal. 131 (2): 1163–1183. Bibcode:2006AJ....131.1163S. doi:10.1086/498708. Vizier catalog entry
  6. 1 2 3 4 5 Alessandro Sozzetti; Torres, Guillermo; Charbonneau, David; Latham, David W.; Holman, Matthew J.; Winn, Joshua N.; Laird, John B.; o’Donovan, Francis T. (August 1, 2007). "Improving Stellar and Planetary Parameters of Transiting Planet Systems: The Case of TrES-2". The Astrophysical Journal. 664 (2): 1190–1198. arXiv:0704.2938. Bibcode:2007ApJ...664.1190S. doi:10.1086/519214. S2CID 17078552.
  7. ↑ D. Mislis; S. Schroter; J.H.M.M. Schmitt; O. Cordes; K. Reif (December 2009). "Multi-band transit observations of the TrES-2b exoplanet". arXiv:0912.4428v1 [astro-ph.EP].
  8. ↑ Raetz, St.; et al. (2014). "Transit timing of TrES-2: A combined analysis of ground- and space-based photometry". Monthly Notices of the Royal Astronomical Society. 444 (2): 1351–1368. arXiv:1408.7022. Bibcode:2014MNRAS.444.1351R. doi:10.1093/mnras/stu1505.
  9. ↑ "Coal-Black Alien Planet is Darkest Ever Seen". 11 August 2011.
  10. ↑ "Kepler Eyes Cluster and Known Planet". NASA. 2009-04-16. Retrieved 2009-05-09.
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