Universe of Spectroscopy

12Spectrum of the First Low-Temperature Brown Dwarf

A brown dwarf is a substellar object with a mass ≤ 8% that of Sun, which is approximately 80 times the mass of Jupiter. Similar to a star, it is formed from gas and dust. A brown dwarf is an object formed when both increase in the central temperature and gravitational contraction stop before the central temperature reaches the temperature of hydrogen combustion (Note 1), and the objects continue to cool from that point onward. The radius of a brown dwarf does not significantly depend on mass. All objects with a mass 80 times that of Jupiter have a radius nearly the same as that of Jupiter.

It has previously been determined that a brown dwarf is distinguished from a low-temperature star by its surface temperature of 1800 K or less. However, its spectra have not been predictable. Since the 1960s, a lots of candidates for brown dwarfs have been discovered and forgotten.

We used a coronagraph with a wavelength of 0.8 microns to investigate near-Earth objects through objects that were four magnitudes dimmer than main-sequence stars. In 1995, a dim companion star was located 7 arcseconds (40 astronomical units) from red dwarf star Gliese 229, which was located 18 light years from the Sun. In a follow-up observation, one of the observers, K. Matthews, saw the two-dimensional near-infrared spectrum and exclaimed "this is Jupiter!" because the spectrum of this object consisted of absorption bands of water vapor and methane and its reflection spectrum was more similar to methane-based Jupiter than to a star.

In the past, Professor Takashi Tsuji of the University of Tokyo predicted that methane appears in objects with surface temperatures of 1000 K or less. Gliese 229B was confirmed as the first object with a surface temperature of 1000 K or less to be found outside of our solar system. Gliese 229B was also the first object of the new spectral category of T dwarfs (the letter "T" refers to Tsuji).

Column “T-type dwarfs and others”

In the search for brown dwarfs, wide-range surveying of individual objects is generally employed rather than searching for companion stars. A wide-area deep survey by the United Kingdom Infrared Telescope (UKIRT), following the 2 Micron All-Sky Survey (2MASS) and Sloan Digital Sky Survey (SDSS), has succeeded in detecting T dwarfs of even lower temperatures. Classifying T-dwarves of its surface temperature down to 600K is possible with near-infrared observations. For classification of objects of even lower temperatures, a 5-micron band mid-infrared observation is necessary.

The brown dwarf with the lowest temperature currently known has a ratio of near-infrared flux to mid-infrared flux of 3:7 based on observations by the Spitzer Space Telescope.

Image 1: Gliese 229B imaged at a wavelength of 0.8 microns. On the left is the image of its discovery, obtained by the Palomar 1.5 m telescope. On the right is an image obtained one year later by the Hubble Space Telescope.
Image 2: Optical and infrared images of Gliese 229. Top left: 0.6 microns, top right: 0.8 microns, bottom left: 0.9 microns. These values are from a visibility coronagraph on an adaptive optics device attached to the 1.5 m Palomar telescope. The primary star A is hidden by a mask on the focal plane. In addition, diffracted light is controlled by a mask on the eyepiece. At the bottom right is a 2 micron image obtained from a multiobject infrared camera and spectrograph attached to a 5 m telescope. The primary star A is hidden by a cold mask on the focal plane (Nature vol. 378, 30 November 1995).
Image 3: Two-dimensional spectrum of the H band. The vertical axis covers 5.4 arcseconds of width, and the horizontal axis spans frequencies of 1.5 to 1.8 microns. The dark band toward the top is the spectrum of the primary star A diffracted by the spider of the telescope and evenly covers the H band. On the other hand, the dark band toward the bottom, the spectrum of companion star B, has strong peaks at 1.6 microns or less and a small flux toward the longer frequencies. This characteristic is unseen in stars (Science vol. 270, 1 December 1995).
Image 4: The spectra of Gliese 229B and Jupiter. The spectrum of Jupiter is placed vertically for easier comparison. The vertical lines toward the top indicate the positions of methane bands (Science vol. 270, 1 December 1995).

Note

Gravitational contraction stops because at the center of the object, electrons degenerate after they are freed from hydrogen atoms owing to pressure ionization, and gravity is then balanced by the degeneracy pressure of the electrons. Because of this, temperature also ceases to rise and the nuclear fusion reaction of hydrogen or hydrogen combustion necessary for an object to shine as a star does not occur.

Data

Date
July 19, 2013
Object
Brown-dwarf Glise 229B
Instrument
Near-Infrared Camera and Spectrograph, Palomar Observatory
Wavelength
Near-Infrared

Warning: Undefined variable $browser in /data/www/htdocs_prc/extra/uos/en/footer.php on line 1

Warning: Undefined variable $browser in /data/www/htdocs_prc/extra/uos/en/footer.php on line 78