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Hot Topic Deep Space Cosmic Evolution Brown Dwarf Detectives
 
Brown Dwarf Detectives
based on UCLA report
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Cosmic Evolution
Posted:   09/06/03

Summary: Studying the chemical fingerprints, or spectra, from fifty brown dwarf stars has revealed not only features of why such failed stars (about the size of Jupiter) are hard to find, but also some guesses as to why they may outnumber the visible stars in our solar neighborhood.

Brown Dwarf Detectives

Elusive brown dwarfs, the missing link between gas giant planets like Jupiter and small, low-mass stars, have now been "fingerprinted" by UCLA astronomy professor Ian S. McLean and colleagues, using the Keck II Telescope at the W.M. Keck Observatory in Hawaii.

gliese_299b
Click here for larger image. Brown dwarfs, such as Gliese 229B, lack sufficient mass (at least 75-80 Jupiters) to ignite core hydrogen fusion.
Credit: American Scientist/Linda Huff


McLean and his research team will publish the most systematic and comprehensive near-infrared spectral analysis of more than 50 brown dwarfs in the Oct. 10 issue of the Astrophysical Journal, the premier journal in astronomy, published by the American Astronomical Society.

"The infrared spectra of brown dwarfs reveal their atomic and molecular fingerprints," said McLean. "Each class of brown dwarfs has a unique fingerprint. We have taken the spectra of more than 50 of them, which reveal their physical and chemical properties."

Brown dwarfs are failed stars about the size of Jupiter, with a much larger mass but not quite large enough to become stars. Like the sun and Jupiter, they are composed mainly of hydrogen gas, perhaps with swirling cloud belts. Unlike the sun, they have no internal energy source and emit almost no visible light. Brown dwarfs are formed along with stars by the contraction of gases and dust in the interstellar medium, McLean said. The first brown dwarf was not discovered until 1995, yet McLean suspects the galaxy is teeming with them.

jupiter
Gas giant planets like Jupiter were formed from gaseous material surrounding the young star.
Credit: NASA


"Brown dwarfs are so elusive, so hard to find," McLean said. "They can be detected best in the infrared, and even within the infrared, they are very difficult to detect. We detect the heat glow from these faint objects in the infrared. Typically, they have to be relatively close by, within 100 light years, for us to even detect the heat signature."

McLean and his colleagues do so using a sophisticated instrument that McLean designed and built at UCLA with other astronomers from UCLA and the University of California, Berkeley. The instrument, attached to the W.M. Keck Observatory's 10-meter Keck II Telescope atop Mauna Kea in Hawaii -- the world's largest optical and infrared telescope -- is called NIRSPEC. It is six feet high, weighs one ton and contains the most powerful infrared spectrometer in the world.

"This is the first time a large quantity of high quality spectral data are presented systematically in the infrared, where brown dwarfs emit most of their light," said Davy Kirkpatrick, staff scientist at the California Institute of Technology's NASA-funded Infrared Processing and Analysis Center. "Approximately 2 percent of brown dwarfs near the sun are oddballs, and we are starting to be able to identify them and understand what makes them different. In addition, many brown dwarfs have been reported in different ways, and we now present them in a consistent manner that will become a standard reference for the future."

McLean built the world's first infrared camera for wide use by astronomers in 1986, and he has built six increasingly sophisticated infrared cameras and spectrometers since then. (A spectrometer splits light into its component colors.)

"The quality of infrared spectra has improved drastically over the last decade," he said.

oort_cloud
The Oort-cloud.
Credit: University of Hawaii


The detectors in McLean's spectrometers, such as NIRSPEC, have more than 250 times as many picture elements as in the 1980s.

"The spectrum reveals what's present and what's missing," McLean said. "What's missing in the light tells us something in the atmosphere of the brown dwarf has absorbed the light.

"When we first studied the brown dwarf spectra, they were peculiar like no star we had ever seen before. The reason we saw missing light in the spectra of the coolest brown dwarfs is the presence of methane in the atmosphere, which we also see in the outer gas giants of the solar system: Jupiter, Saturn, Uranus, Neptune.

"We also see evidence of water in the form of superheated steam, which we don't see in any normal star like the sun. The sun is much too hot to have water molecules. Methane and water sculpt the infrared spectrum in a very distinctive way. The spectra of brown dwarfs show a gradual change from that of a star to that of Jupiter.

"Brown dwarfs are the missing link between gas giant planets like Jupiter and small stars like red dwarfs," he said.

If large numbers of brown dwarfs exist, they "could make a small, but significant contribution to dark matter," the so-called "missing mass" in the universe, McLean said.

LP_94420
The brown dwarf LP 944-20 (Digital Sky Survey).
Credit: European Southern Observatory


"Brown dwarfs won't account for all of the so-called dark matter," he said. "There is mass in the form of ordinary matter that is unaccounted for because we don't yet have the technology to find it. There are brown dwarfs, and maybe small black holes, and faint white dwarfs regular stars that lost their outer gaseous envelopes leaving the burned-out core of old stars. White dwarfs, brown dwarfs, black holes and gas account for some of the dark matter. The rest is presumably a new form of matter."

McLean and his colleagues Kirkpatrick; Adam Burgasser, a UCLA postdoctoral scholar in McLean's group and recipient of a NASA-funded Hubble fellowship; UCLA graduate student Mark McGovern and postdoctoral scholar Lisa Prato, who both work in McLean's group; and former UCLA postdoctoral scholar Sungsoo Kim will publish an atlas and analysis of the brown dwarf infrared spectra in the Oct. 10 Astrophysical Journal. Kirkpatrick and Burgasser were responsible for most of the initial brown dwarf identifications using an infrared all-sky survey called 2MASS. McLean praised the members of his research team as "instrumental to the success" of the research.

"After four years of data gathering from NIRSPEC, we have obtained and studied spectra from more than 50 brown dwarfs, and analyzed the variations," McLean said. "Astronomers in the future will be able to obtain the infrared spectrum of a newly discovered brown dwarf and compare the spectrum with those we have published and instantly identify what kind of brown dwarf they have found. Probing more distant regions of the galaxy to study the youngest, recently-formed brown dwarfs is the next step."

His research, including NIRSPEC, was funded by the California Association for Research in Astronomy, the entity that operates the W.M. Keck Observatory.

To do his research, McLean designs and builds spectrometers and analyzes astrophysics data.

"The astronomy motivates me, but I have to be a bit of an engineer and experimental physicist as well," he said, "because technology is the key to new discoveries."

What's Next

Since the discovery of brown dwarfs less than a decade ago, astronomers have come to think that they might be more numerous than the visible stars in the sky. In broad terms, 80 percent of the nearby stars are (red) dwarfs, 10 percent are solar-type stars, and 10 percent are more massive. There are probably around the same number of brown dwarfs as stars within the immediate solar neighborhood.

The true abundance of brown dwarfs, sub-brown dwarfs and extrasolar planets is not known, and large areas of the sky still need to be explored. Most of the brown dwarfs have been located by the Two Micron All Sky Survey (2MASS), although the Sloan Digital Sky Survey (SDSS) and the planet-finding Doppler technique also have been used to find brown dwarfs. Reid is completing a census of low-mass stars and brown dwarfs in the immediate solar neighborhood.


Related Web Pages

2MASS
IAU Working Group on Extrasolar Planets
Star Bright: Part I
Star Bright: Part II


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