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A Planet-like Companion Growing up in the Fast Lane

April 5, 2010

For Immediate Release – April 6th, 2010 - 9:00am Eastern Daylight Time

Gemini Observatory Press Release

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Note: A Hubble Space Telescope version of this release is going out concurrently from the Space Telescope Science Institute and can be found here.

 

The cliché that youth grow up so fast is about to take on a new twist. This is due to the discovery of a very young planet-like object (with a mass somewhere between 5-10 times that of Jupiter), paired with a low-mass brown dwarf. What is unique about this system is that the planet-like body appears to have formed in about a million years–more rapidly than some theories of planet formation predict.

Kamen Todorov of Pennsylvania State University and co-investigators made the discovery using the keen visible-light eyesight of the Hubble Space Telescope combined with high-resolution adaptive optics infrared images from the Gemini Observatory. The images of the pair were obtained as part of a survey of 32 young brown dwarfs in the Taurus star-forming region located some 450 light years away. The team’s paper is in press for an upcoming issue of the Astrophysical Journal Letters, http://iopscience.iop.org/2041-8205/714/1/L84.

Identified as 2M044144, the primary brown dwarf is likely about 20 times the mass of Jupiter and separated from the smaller body by about 3.6 billion kilometers – for comparison, Saturn is about 2.25 billion kilometers from the Sun.

However, it’s the age of the smaller object that is most compelling. According to team-member Kevin Luhman of the Center for Exoplanets and Habitable Worlds at Pennsylvania State University, “This is the youngest planetary-mass companion that has been found so far, and its extreme youth provides constraints on how it could have formed. The formation mechanism of this companion in turn can tell us whether it is truly a planet.”

While different processes or combinations may be relevant for each system, here are three possible scenarios for the formation of planetary-mass companions: 1) Dust in a circumstellar disk slowly agglomerates to form a rocky planet 10 times larger than the Earth, which then accumulates a large gaseous envelope; 2) the disk is unstable causing a clump of gas to quickly collapse and form an object the size of a gas-giant planet; or, 3) rather than forming in a disk, a companion forms from the collapse of the vast cloud of gas and dust in the same manner and at the same time as the primary body.

If the last scenario does occur, then this discovery demonstrates that nature can make planetary-mass bodies through the same mechanism that builds stars. This is the likely solution because the planet-like companion is too young to have formed by the first scenario, which is very slow. The second mechanism occurs rapidly, but any disk around this low-mass brown dwarf probably did not contain enough material to make an object with a mass of 5-10 Jupiter masses.

“The most interesting implication of this result is that it shows that the process that makes binary stars extends all the way down to planetary masses. So it appears that nature is able to make planetary-mass companions through two very different mechanisms,” says Luhman. If 2M044144’s companion formed through cloud collapse and fragmentation, as stellar binary systems do, then the companion is not a planet by the definition that planets build up inside disks.

Brown dwarfs are typically tens of times the mass of Jupiter, and they are too small to sustain nuclear fusion and shine as stars do. Low mass objects like these glow primarily due to internal heating from the collapsing material, and they are warmer when very young, as in the case of the 2M044144 system.

Additional evidence to indicate that the new planetary-mass companion formed like a binary star comes from the presence of a nearby small red star that is gravitationally connected to the pair. When the Gemini observations were made, the adaptive optics system used the distant red star as a reference guide star (see background below). In the process, Gemini discovered yet another brown dwarf very close to the distant red star, making 2M044144 a possible member of a quadruple system. Luhman believes that all four objects may have formed in the same cloud collapse: “The configuration closely resembles quadruple star systems, suggesting that all of its components formed like stars,” Luhman said.

Hubble Space Telescope (top) and Gemini North (bottom) images of the 2M J044144 system showing the smaller companion at 8:00 position. The companion has an estimated mass of between 5-10 times the mass of Jupiter. In the right panel of both the HST and Gemini images the brighter light from the brown dwarf has been removed to show the companion more clearly.

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Photo Credits: (top images): NASA, ESA, and K. Todorov and K. Luhman (Pennsylvania State); (bottom images): Gemini Observatory/AURA and K. Todorov and K. Luhman (Pennsylvania State University)

Credit: Gemini Observatory/AURA artwork by Lynette Cook

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Artist's conception of the binary system 2M J044144 showing the primary ~ 20 Jupiter mass brown dwarf (left) and the 5 - 10 Jupiter mass companion (right). The disk of the primary likely never had enough material to make a companion of this mass. As a result, this small companion probably formed like a binary star. In this illustration, both objects are presented at the same distance to show relative sizes. Not shown are two other nearby objects, a low-mass star and a brown dwarf that are probably both parts of this system.

Gemini North adaptive optics image of both binary systems 2M J044144A/B (bottom) and 2M J044145A/B (top) as imaged using the Gemini Near-Infrared Imager (NIRI) with the Altair adaptive optics system. The Gemini data was used to discover the companion to 2M J044145A which is believed to be associated with this system making it a likely quadruple system.

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Photo Credit: Gemini Observatory/AURA and K. Todorov and K. Luhman (Pennsylvania State University)


The Gemini Observatory is an international collaboration with two identical 8-meter telescopes. The Frederick C. Gillett Gemini Telescope is located at Mauna Kea, Hawai'i (Gemini North) and the other telescope at Cerro Pachón in central Chile (Gemini South), and hence provide full coverage of both hemispheres of the sky. Both telescopes incorporate new technologies that allow large, relatively thin mirrors under active control to collect and focus both optical and infrared radiation from space.

The Gemini Observatory provides the astronomical communities in each partner country with state-of-the-art astronomical facilities that allocate observing time in proportion to each country's contribution. In addition to financial support, each country also contributes significant scientific and technical resources. The national research agencies that form the Gemini partnership include: the US National Science Foundation (NSF), the UK Science and Technology Facilities Council (STFC), the Canadian National Research Council (NRC), the Chilean Comisión Nacional de Investigación Cientifica y Tecnológica (CONICYT), the Australian Research Council (ARC), the Argentinean Consejo Nacional de Investigaciones Científicas y Técnicas (CONICET) and the Brazilian Conselho Nacional de Desenvolvimento Científico e Tecnológico CNPq).