eso0414 — Communiqué de presse scientifique
Closer to the Monster
Trailblazing VLT Interferometer Studies of the Central Region in Active Galaxy NGC 1068.
5 mai 2004
Fulfilling an old dream of astronomers, observations with the Very Large Telescope Interferometer (VLTI) at the ESO Paranal Observatory (Chile) have now made it possible to obtain a clear picture of the immediate surroundings of the black hole at the centre of an active galaxy. The new results concern the spiral galaxy NGC 1068, located at a distance of about 50 million light-years. They show a configuration of comparatively warm dust (about 50°C) measuring 11 light-years across and 7 light-years thick, with an inner, hotter zone (500°C), about 2 light-years wide. These imaging and spectral observations confirm the current theory that black holes at the centres of active galaxies are enshrouded in a thick doughnut-shaped structure of gas and dust called a "torus." For this trailblazing study, the first of its kind of an extragalactic object by means of long-baseline infrared interferometry, an international team of astronomers  used the new MIDI instrument in the VLTI Laboratory. It was designed and constructed in a collaboration between German, Dutch and French research institutes . Combining the light from two 8.2-m VLT Unit Telescopes during two observing runs in June and November 2003, respectively, a maximum resolution of 0.013 arcsec was achieved, corresponding to about 3 light-years at the distance of NGC 1068. Infrared spectra of the central region of this galaxy were obtained that indicate that the heated dust is probably of alumino-silicate composition. The new results are published in a research paper appearing in the May 6, 2004, issue of the international research journal Nature.
NGC 1068 - a typical active galaxy
Active galaxies are among the most spectacular objects in the sky. Their compact nuclei (AGN = Active Galaxy Nuclei) are so luminous that they can outshine the entire galaxy; "quasars" constitute extreme cases of this phenomenon. These cosmic objects show many interesting observational characteristics over the whole electromagnetic spectrum, ranging from radio to X-ray emission.
There is now much evidence that the ultimate power station of these activities originate in supermassive black holes with masses up to thousands of millions times the mass of our Sun. The one in the Milky Way galaxy has only about 3 million solar masses. The black hole is believed to be fed from a tightly wound accretion disc of gas and dust encircling it. Material that falls towards such black holes will be compressed and heated up to tremendous temperatures. This hot gas radiates an enormous amount of light, causing the active galaxy nucleus to shine so brightly.
NGC 1068 (also known as Messier 77) is among the brightest and most nearby active galaxies. Located in the constellation Cetus (The Whale) at a distance of about 50 million light-years, it looks like a rather normal, barred spiral galaxy. The core of this galaxy, however, is very luminous, not only in optical, but also in ultraviolet and X-ray light. A black hole with a mass equivalent to about 100 million times the mass of our Sun is required to account for the nuclear activity in NGC 1068.
The VLTI observations
On the nights of June 14 to 16, 2003, a team of European astronomers  conducted a first series of observations to verify the scientific potential of the newly installed MIDI instrument on the VLTI. They also studied the active galaxy NGC 1068. Already at this first attempt, it was possible to see details near the centre of this object.
MIDI is sensitive to light of a wavelength near 10 µm, i.e. in the mid-infrared spectral region ("thermal infrared"). With distances between the contributing telescopes ("baselines") of up to 200 m, MIDI can reach a maximum angular resolution (image sharpness) of about 0.01 arcsec. Equally important, by combining the light beams from two 8.2-m VLT Unit Telescopes, MIDI now allows, for the first time, to perform infrared interferometry of comparatively faint objects outside our own galaxy, the Milky Way.
With its high sensitivity to thermal radiation, MIDI is ideally suited to study material in the highly obscured regions near a central black hole and heated by its ultraviolet and optical radiation. The energy absorbed by the dust grains is then re-radiated at longer wavelengths in the thermal infrared spectral region between 5 and 100 µm.
The central region in NGC 1068
Additional interferometric observations were secured in November 2003 at a baseline of 42 m. Following a careful analysis of all data, the achieved spatial resolution (image sharpness) and the detailed spectra have allowed the astronomers to study the structure of the central region of NGC 1068.
They detect the presence of an innermost, comparatively "hot" cloud of dust, heated to about 500°C and with a diameter equal to or smaller than the achieved image sharpness, i.e. about 3 light-years. It is surrounded by a cooler, dusty region, with a temperature of about 50°C, measuring 11 light-years across and about 7 light-years thick. This is most likely the predicted central, disc-shaped cloud that rotates around the black hole.
The comparative thickness of the observed structure (the thickness is ~ 65% of the diameter) is of particular relevance in that it can only remain stable if subjected to a continuous injection of motion ("kinetic") energy. However, none of the current models of central regions in active galaxies provide a convincing explanation of this.
The MIDI spectra, covering the wavelength interval from 8 - 13.5 µm, also provide information about the possible composition of the dust grains. The most likely constituent is calcium aluminum-silicate (Ca2Al2SiO7), a high-temperature species that is also found in the outer atmospheres of some super-giant stars. Still, these pilot observations cannot conclusively rule out other types of non-olivine dust.
These are the first-ever long-baseline imaging and spectral inteferometric observations of an extragalactic object in the thermal infrared. They open the door to a completely new field in astronomy: the study of gas and dust structures surrounding and feeding the heaviest black holes in the universe.
Says Dutch astronomer Walter Jaffe from the Leiden Observatory and first author of the research paper about the MIDI observations: "Already these first results show that we are far from understanding what really goes on near those monster objects. MIDI and the VLTI will offer for years to come the best combination for astronomers from all over the world to carry out these exciting studies."
 The observations were planned and carried out by a team that includes Walter Jaffe, Huub Röttgering, B. Heijliger, G.K. Miley, and P.T. de Zeeuw (Leiden University, the Netherlands), O. Chesneau, U. Grasser, R. Köhler, Ch. Leinert, K. Meisenheimer, and F. Przygodda (MPIA, Germany), L.B.F.M. Waters (Amsterdam, the Netherlands), D. Fraix-Burnet, and F. Malbet (Grenoble, France), A. Galzenborg-Kluttig (Dwingeloo, the Netherlands), G.-L. Granato (Padova, Italy), A. Glindemann, S. Morel, F. Paresce, Andrea Richichi, and M. Schoeller (ESO), J.-W. Pel (Groningen, the Netherlands), G. Perrin, H. Sol, and J. Woillez (OBSPM, Paris, France), and G. weigelt (MPIR, Bonn, Germany).
 The MIDI instrument (http://www.mpia-hd.mpg.de/MIDI/) is the result of a collaboration between German, Dutch and French institutes.
 More information about the VLTI and photos of many of the components of the facility are available at the VLTI website.
The results described in this press release are described in a research paper "The central dusty torus in the active nucleus of NGC 1068" by W. Jaffe, K. Meisenheimer, H. Röttgering, Ch. Leinert, A. Richichi et al., appearing in the May 6, 2004, issue of the journal Nature
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A propos du communiqué de presse
|Communiqué de presse N°:||eso0414|
|Legacy ID:||PR 10/04|
|Nom:||M 77, Messier 77, NGC 1068, Very Large Telescope Interferometer|
|Type:||Local Universe : Star : Evolutionary Stage : Neutron Star : Magnetar|
|Facility:||Very Large Telescope, Very Large Telescope Interferometer|