01h12m36.48s, +17° 04′ 31.8″
The planet GU Piscium b and its star GU Piscium composed of visible and infrared images from the Gemini South telescope and an infrared image from the CFHT. Because infrared light is invisible to the naked eye, astronomers use a colour code in which infrared light is represented by the colour red. GU Piscium b is brighter in infrared than in other filters, which is why it appears red in this image.
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| Discovery[1] | |
|---|---|
| Discovered by | Marie-Eve Naud, Étienne Artigau, Lison Malo, Loïc Albert, René Doyon, David Lafrenière, Jonathan Gagné, Didier Saumon, Caroline V. Morley, France Allard, Derek Homeier, Charles A. Beichman, Christopher R. Gelino, Anne Boucher |
| Orbital characteristics | |
| 2000 AU[2] | |
| 163,000 years[NB 1] | |
| Physical characteristics | |
| Mass | 9–13 MJ[2] |
GU Piscium b (GU Psc b)[2] is a directly imaged planetary-mass companion orbiting the star GU Piscium, with an extremely large orbit of 2,000 AU (3.0×1011 km), and an apparent angular separation of 42 arc seconds.[3][4] The planet is located at right ascension 01h12m 36.48s declination +17° 04′ 31.8″ at a distance of 48 pc (160 ly).[1]
Anorbital revolution around its parent star (which is 1/3 the mass of the Sun) or "year", would take approximately 163,000 years[NB 1] to complete, considering a circular orbit with 2000 AU as the semi-major axis. It is a gas giant[5] located in the constellationofPisces, 155 light-years from the Solar System, and estimated to have a mass nine to thirteen times that of Jupiter,[6] and a surface temperature of 1000 K.[7]
It is a relatively young stellar system, part of the AB Doradus moving group of ca. 30 main stars created from the same molecular cloud less than 100 million years ago, and the only one found among the 90 stars of the group examined.
The discovery was made by an international team of astronomers led by Marie-Eve Naud of the Université de MontréalinQuebec, combining observations from telescopes of the Gemini Observatory, the Mont Mégantic Observatory (OMM), the Canada–France–Hawaii Telescope (CFHT) and the W. M. Keck Observatory.[8] Its large distance away from its parent star permitted the use of combined infrared and visible light images to detect it, a technique astronomers hope to reproduce to discover much closer planets with the Gemini Planet Imager (GPI) in Chile.
Near-infrared spectroscopy of the companion was obtained with the GNIRS spectrograph on the Gemini North Telescope, which shows evidence of low surface gravity confirming the planet's youth. Weak methane absorption was detected in H and K band corresponding to a spectral type of T3.5.
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