Forum for Science, Industry and Business

Sponsored by:     3M 
Search our Site:

 

A First Look at the Doughnut Around a Giant Black Hole

20.06.2003


First detection by infrared interferometry of an extragalactic object


This Photo shows an artist’s impression of an active galaxy that has jets. The central engine is thought to be a supermassive black hole surrounded by an accretion disc and enshrouded in a dusty doughnut-shaped torus. The torus of dust and gas can be seen orbiting a flatter disc of swirling gas. In the centre, the supermassive black hole is surrounded by a flat accretion disc of rapidly orbiting material. The jets are emitted at right angles from the plane of the disc. Courtesy Aurore Simonnet, Sonoma State University.


This Picture shows an image of NGC 1068 taken in the visible wavelength range (courtesy NOAO/AURA/NSF). The image has 820x680 pixels. A blow-up of the central 5x5 pixels is displayed inside the figure on the right. The circle on the central pixel indicates the size of the structure that was observed with MIDI.



Active galactic nuclei (AGN) are one of the most energetic and mysterious phenomena in the universe. In some galaxies indeed, the core generates amounts of energy which surpass those of normal galaxies, such as the Milky Way, by many orders of magnitude.

The central engine of these power stations is thought to be a supermassive black hole. Indirect lines of evidence have suggested that these massive black holes are enshrouded in a thick doughnut-shaped structure of gas and dust, which astronomers call a "torus". However, due to the limited sharpness of images that can be obtained with present telescopes in the 10-m range, such a torus has never been imaged to date.


Using the new and powerful VLT Interferometer [1] - a mode of the ESO Very Large Telescope that combines light from at least two telescopes to obtain information on very fine scales - a team of European astronomers [2] has succeeded for the first time in resolving structures in the dusty torus of the prototype AGN, the famous galaxy NGC 1068. The structures have a size of roughly 0.03 arcsec, corresponding to about 10 light-years at the distance of the galaxy.

This important achievement shows that the VLT Interferometer, using the recently inaugurated MIDI instrument [3], proves an invaluable tool in the study of objects outside our own Galaxy.

Cosmic power station

Active galaxies are among the most spectacular objects in the sky. Their compact nuclei (AGN) are so luminous that they can outshine an entire galaxy. These objects show many interesting observational characteristics over the whole electromagnetic spectrum, ranging from radio to X-ray emission.

Active galaxies take many forms: some have bright nuclei emitting high-energy (i.e. ultraviolet and X-rays) photons, some have high-energy nuclei but appear to be surrounded by a more-or-less "normal" galaxy, while some have long narrow jets or beams of matter streaming out from the centre.

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 (see e.g. ESO PR 04/01). The black hole is fed from a tightly wound accretion disc 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.

Enshrouded in the mystery torus

The central region of an active nucleus is currently believed to be surrounded by a doughnut of dense and opaque gas and dust. It was first thought that the different types of active galaxies were fundamentally different objects. Astronomers now prefer the so-called "unified" model of AGN, meaning that most or all AGN are actually just different versions of the same object. What the object looks like depends on the orientation of the doughnut on our line of sight : can we see through the doughnut hole deep into the bright centre or can we only see the opaque walls ? Some AGN appear indeed very luminous because we see straight down to the emission site, while others would be very dim, since the torus hides the central power station from our view. These doughnuts or tori are, however, very difficult to resolve because of their very small size, typically a few tens of light-years. For the nearest active galaxy, this corresponds to an estimated angular diameter less than 0.05 arcsec, much smaller than what can be observed with present single large telescopes in the 10-m range.

Since, so far, evidence for the tori is only indirect, a large variety of models has been proposed as to how these tori could be, varying from very dense and compact tori, to very extended and fluffy tori. What the astronomers really need, in order to differentiate among the models, is a direct image of a torus. But until now, no telescope could see sharp enough to spot one.

Finding a needle in a haystack

This is where interferometry with large telescopes makes a difference. Interferometry is the technique which combines two or more telescopes to achieve an angular resolution equal to that of a telescope as large as the separation of the individual ones (cf ESO PR 06/01 and 23/01). The recently inaugurated ESO Very Large Telescope Interferometer on top of the Paranal mountain has the ambitious goal of making interferometry a tool available to every astronomer. Just a few months ago, the first of the powerful instruments for the VLTI was installed, the 10 micron beam combiner mid-infrared interferometric instrument (MIDI, cf. ESO PR 25/02). This will be followed in early 2004 by the AMBER instrument [4].

MIDI is sensitive to light of a wavelength near 10 microns, i.e. in the mid-infrared spectral region (the so-called "thermal infrared"). Located at the heart of the VLT Interferometer with its multiple baselines of up to 200 m, MIDI can reach an angular resolution of about 0.01 arcsec. Combined with two powerful 8.2-m VLT Unit Telescopes, MIDI has for the first time in infrared interferometry enough sensitivity to study objects far away from our galaxy, the Milky Way.

With its high sensitivity to thermal radiation, MIDI is ideally suited to study cosmic material near a central object and heated by its radiation. The ultraviolet and optical radiation from the hot material surrounding the black hole indeed heats the dust torus to several hundred degrees. The absorbed energy is then re-radiated in the thermal infrared between 5 and 100 microns.

The MIDI instrument on the VLTI is thus the most appropriate instrument to peer at the enigmatic dust and gas tori believed to be located around giant black holes at the centres of quasars and Active Galactic Nuclei.

And since nobody has ever been able to use interferometry to study faint objects in the thermal infrared, MIDI enters into a whole unexplored territory.

On the nights of June 14 to 16, a team of European astronomers [2] conducted a first series of observations to verify the scientific potential of MIDI on the VLTI. Among them, they studied the active galaxy NGC 1068.

NGC 1068: a prototype AGN

NGC 1068 is among the brightest and most nearby active galaxies. Located in the constellation Cetus at a distance of about 60 million light years, it is also known as Messier 77. It is in fact one of the biggest galaxies in Messier’s catalogue and one of the first recognised spiral galaxies. On optical images, NGC 1068 looks indeed like a rather normal barred spiral galaxy. The core of the galaxy, however, is very luminous not only in the optical, but also in ultraviolet and X-ray light. A black hole with a mass equivalent to approximately 100 million stars like our Sun is required to account for the nuclear activity in NGC 1068.

Fringes in the distant dust: resolving the torus in NGC 1068

The MIDI observations used two of the 8.2 m VLT Unit Telescopes (Antu and Melipal), separated by a baseline of 102 m. Due to projection effects, the actual baseline for the NGC 1068 observations amounted to 79 m. While observing NGC 1068, the astronomers detected interferometric fringes. Fringes are produced when beams of light from two telescopes are brought together exactly in phase. For a point-like source, such fringes have the maximum possible theoretical contrast (i.e. 100%): the source is unresolved. However, sources of increasing angular size produce fringes with decreasing contrast. In the case of NGC 1068, the measured contrast was only about 10% of the maximum one. An exact interpretation of this result will follow in the context of additional measurements along different baselines, which are planned for this coming Autumn [5]. Already this initial result is nevertheless very convincing: the fringes were obtained with consistent values on several measurements over 2 consecutive nights, thanks also to the excellent observing conditions at the Paranal site ("seeing" values were between 0.3 and 0.6 arcsec). It is already possible to state that a structure on a spatial scale of approximately 0.03 arcsec (corresponding to about 10 light-years) has been detected in the dust torus in NGC 1068. The relative size of this structure is shown in ESO PR Photo 18b/03.

A breakthrough in interferometry

This measurement represents the first observation ever by the technique of long-baseline interferometry of an extragalactic object in the thermal infrared. This new success of the VLTI opens the door to a completely new field in astronomy: the study of gas and dust structures surrounding and feeding the biggest monsters in the universe. MIDI and the VLTI will offer for years to come the best combination for astronomers from all over the world to carry out these studies.

Notes

[1] More information about the VLTI and photos of many of the components of the facility are available at the VLTI website, as well as in ESO PR 06/01 ("First Light" in March 2001 and explanation of the interferometric measurements), ESO PR 23/01 (observations with two 8.2-m telescopes in October 2001) and ESO PR 16/02 (observations with four 8.2-m telescopes in September 2002), ESO PR 22/02 (measurements of the diameters of small stars in November 2002) and ESO PR 11/03 (installation of the first MACAO adaptive optics unit in May 2003).

[2]: The observations were planned and carried out by a team led by Andrea Richichi (ESO) and including C. Leinert, R. Koehler, K. Meisenheimer (MPIA), R. Waters (Amsterdam), F. Malbet (Grenoble), M. Schoeller, S. Morel , F. Paresce, A. Glindemann, M.Tarenghi (ESO), H. Roettgering and W. Jaffe (Leiden).

[3]: The MIDI instrument (http://www.mpia-hd.mpg.de/MIDI/) is the result of a collaboration between German, Dutch and French institutes. See ESO PR 25/02.

[4]: The AMBER instrument will equip the VLTI starting from 2004. It will cover the 1-2.5 micron range, combining up to three different telescopes. http://www.obs-nice.fr/amber/

[5]: NGC 1068 is well visible in September/October. The present measurement was obtained under demanding pointing in June, in the very last hour of the night.

Contacts:

ESO Garching
A. Richichi
Phone: +49 89 3200-6803
email: arichich@eso.org

Max-Planck-Institut für Astronomie, Heidelberg
C. Leinert
Phone: +49 6221 528 264
email: leinert@mpia.de


Leiden Observatory, The Netherlands
H. Roettgering
Phone: +31 71-5275851
email: rottgeri@strw.leidenuniv.nl

| EurekAlert!
Further information:
http://www.mpia-hd.mpg.de/MIDI
http://www.obs-nice.fr/amber

More articles from Physics and Astronomy:

nachricht Heating quantum matter: A novel view on topology
22.08.2017 | Université libre de Bruxelles

nachricht Engineering team images tiny quasicrystals as they form
18.08.2017 | Cornell University

All articles from Physics and Astronomy >>>

The most recent press releases about innovation >>>

Die letzten 5 Focus-News des innovations-reports im Überblick:

Im Focus: Fizzy soda water could be key to clean manufacture of flat wonder material: Graphene

Whether you call it effervescent, fizzy, or sparkling, carbonated water is making a comeback as a beverage. Aside from quenching thirst, researchers at the University of Illinois at Urbana-Champaign have discovered a new use for these "bubbly" concoctions that will have major impact on the manufacturer of the world's thinnest, flattest, and one most useful materials -- graphene.

As graphene's popularity grows as an advanced "wonder" material, the speed and quality at which it can be manufactured will be paramount. With that in mind,...

Im Focus: Exotic quantum states made from light: Physicists create optical “wells” for a super-photon

Physicists at the University of Bonn have managed to create optical hollows and more complex patterns into which the light of a Bose-Einstein condensate flows. The creation of such highly low-loss structures for light is a prerequisite for complex light circuits, such as for quantum information processing for a new generation of computers. The researchers are now presenting their results in the journal Nature Photonics.

Light particles (photons) occur as tiny, indivisible portions. Many thousands of these light portions can be merged to form a single super-photon if they are...

Im Focus: Circular RNA linked to brain function

For the first time, scientists have shown that circular RNA is linked to brain function. When a RNA molecule called Cdr1as was deleted from the genome of mice, the animals had problems filtering out unnecessary information – like patients suffering from neuropsychiatric disorders.

While hundreds of circular RNAs (circRNAs) are abundant in mammalian brains, one big question has remained unanswered: What are they actually good for? In the...

Im Focus: RAVAN CubeSat measures Earth's outgoing energy

An experimental small satellite has successfully collected and delivered data on a key measurement for predicting changes in Earth's climate.

The Radiometer Assessment using Vertically Aligned Nanotubes (RAVAN) CubeSat was launched into low-Earth orbit on Nov. 11, 2016, in order to test new...

Im Focus: Scientists shine new light on the “other high temperature superconductor”

A study led by scientists of the Max Planck Institute for the Structure and Dynamics of Matter (MPSD) at the Center for Free-Electron Laser Science in Hamburg presents evidence of the coexistence of superconductivity and “charge-density-waves” in compounds of the poorly-studied family of bismuthates. This observation opens up new perspectives for a deeper understanding of the phenomenon of high-temperature superconductivity, a topic which is at the core of condensed matter research since more than 30 years. The paper by Nicoletti et al has been published in the PNAS.

Since the beginning of the 20th century, superconductivity had been observed in some metals at temperatures only a few degrees above the absolute zero (minus...

All Focus news of the innovation-report >>>

Anzeige

Anzeige

Event News

Call for Papers – ICNFT 2018, 5th International Conference on New Forming Technology

16.08.2017 | Event News

Sustainability is the business model of tomorrow

04.08.2017 | Event News

Clash of Realities 2017: Registration now open. International Conference at TH Köln

26.07.2017 | Event News

 
Latest News

Stretchable biofuel cells extract energy from sweat to power wearable devices

22.08.2017 | Power and Electrical Engineering

New technique to treating mitral valve diseases: First patient data

22.08.2017 | Medical Engineering

IVAM Marketing Prize recognizes convincing technology marketing for the tenth time

22.08.2017 | Awards Funding

VideoLinks
B2B-VideoLinks
More VideoLinks >>>