24 June 1998
Until now, disks have only been found around less massive stars. Planets are formed in such disks. The new discovery may thus have important implications for our understanding of the formation of planetary systems around stars.
TIMMI (Thermal Infrared Multi Mode Instrument) is a general-purpose camera spectrometer operating at a wavelength of 10 micrometer. To reach sufficient sensitivity, the camera must be cooled to approx. -260 C, i.e. a few degrees above the absolute minimum, by use of liquid Helium. Astronomical objects whose temperatures are between -120 C and 300 C radiate most of their energy at this wavelength. In addition, dust and haze that are absolutely impenetrable for light visible to the human eye, are often found to be nearly transparent at this wavelength. This is why fire-fighters now use similar equipment to look through smoke.
Earlier observations with radio telescopes of the object G339.88-1.26, deeply embedded in an interstellar nebula, had been interpreted in terms of the possible existence of a circumstellar disk around a high-mass star. It was concluded that the star responsible for heating the surrounding gas must be very hot and also that it must be intrinsically very bright. The star, most likely of spectral type O9, would have a luminosity 10,000 times higher than that of the Sun and a mass of about 20 times that of the Sun. From the measured velocity, the likely distance of this object is about 10,000 light-years.
The object is associated with several "spots" of very strong radio emission from methanol molecules (methanol masers). Interestingly, they form a chain in the sky and the measured velocities of the individual spots are indicative for orbital motion in a rotating disk around the central star.
As far as known, this is the first direct image of a disk around a very massive star. At a wavelength of 10 micrometer, however, the central star that is responsible for heating the dust disc, cannot be seen in spite of its rather high luminosity. This is because it radiates mostly in the ultra-violet part of the spectrum. Moreover, the dust disk in which the hot star is embedded, absorbs the stellar ultraviolet light extremely efficiently, thereby re-emitting this energy in the infrared. And any stellar light that escapes the dust shroud is in any case completely blocked by intervening interstellar material in the nebula.
In view of the extremely high luminosity of such massive stars, any surrounding disks are subject to a fierce attack by the enormous flux of light to which they are exposed. Hence the existence of such disks around massive and luminous stars has been questioned by astronomers interested in the physical process of star formation.
The discovery of the disk around G339.88-1.26 now settles the question whether such disks can indeed be formed and are stable over periods long enough that they can be observed.
Supplementary measurements to investigate the molecules and dust around G339.88-1.26 have been performed with the SEST submillimeter telescope at La Silla in March 1998. Near-infrared images have also been taken at the NTT and at the 2.2-m telescope.
The team responsible for this project also includes Thomas Henning and Markus Feldt (Astrophysikalisches Institut & Universitats-Sternwarte, Jena, Germany), Andreas Eckart (Max-Planck-Institut fur extraterrestrische Physik, Garching, Germany) and Lars-Ake Nyman (ESO).
Further information on this subject.
This Press Release is accompanied by ESO PR Photo 22a/98 and ESO PR Photo 22b/98. They may be reproduced, if credit is given to the European Southern Observatory.
ESO PR Photo 22a/98
ESO PR Photo 22b/98
The TIMMI 10 micrometer image of the inclined dust disk around a hot O9 star at the G339.88-1.26 radio source. The diameter of the disk is of the order of 5 arcsec, i.e. at the most probable distance to the object (10,000 lightyears) it is 20,000 times larger than the diameter of the Earth's orbit around the Sun.