Universe Today

Image credit: ESO
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 [2] used the new MIDI instrument in the VLTI Laboratory. It was designed and constructed in a collaboration between German, Dutch and French research institutes [3].

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, cf. e.g., ESO PR 04/01. The one in the Milky Way galaxy has only about 3 million solar masses, cf. ESO PR 17/02. 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 [2] 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, cf. ESO PR 17/03.

MIDI is sensitive to light of a wavelength near 10 ?m, 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 ?m.
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 ?m, 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.

Original Source: ESO News Release

Image credit: NASA
Astronomers who want to study the early universe face a fundamental problem. How do you observe what existed during the “dark ages,” before the first stars formed to light it up? Theorists Abraham Loeb and Matias Zaldarriaga (Harvard-Smithsonian Center for Astrophysics) have found a solution. They calculated that astronomers can detect the first atoms in the early universe by looking for the shadows they cast.

To see the shadows, an observer must study the cosmic microwave background (CMB) – radiation left over from the era of recombination. When the universe was about 370,000 years old, it cooled enough for electrons and protons to unite, recombining into neutral hydrogen atoms and allowing the relic CMB radiation from the Big Bang to travel almost unimpeded across the cosmos for the past 13 billion years.

Over time, some of the CMB photons encountered clumps of hydrogen gas and were absorbed. By looking for regions with fewer photons – regions that are shadowed by hydrogen – astronomers can determine the distribution of matter in the very early universe.

“There is an enormous amount of information imprinted on the microwave sky that could teach us about the initial conditions of the universe with exquisite precision,” said Loeb.

Inflation and Dark Matter
To absorb CMB photons, the hydrogen temperature (specifically its excitation temperature) must be lower than the temperature of the CMB radiation – conditions that existed only when the universe was between 20 and 100 million years old (age of Universe: 13.7 billion years). Coincidentally, this is also well before the formation of any stars or galaxies, opening a unique window into the so-called “dark ages.”

Studying CMB shadows also allows astronomers to observe much smaller structures than was possible previously using instruments like the Wilkinson Microwave Anisotropy Probe (WMAP) satellite. The shadow technique can detect hydrogen clumps as small as 30,000 light-years across in the present-day universe, or the equivalent of only 300 light-years across in the primordial universe. (The scale has grown larger as the universe expanded.) Such resolution is a factor of 1000 times better than the resolution of WMAP.

“This method offers a window into the physics of the very early universe, namely the epoch of inflation during which fluctuations in the distribution of matter are believed to have been produced. Moreover, we could determine whether neutrinos or some unknown type of particle contribute substantially to the amount of ‘dark matter’ in the universe. These questions – what happened during the epoch of inflation and what is dark matter – are key problems in modern cosmology whose answers will yield fundamental insights into the nature of the universe,” said Loeb.

An Observational Challenge
Hydrogen atoms absorb CMB photons at a specific wavelength of 21 centimeters (8 inches). The expansion of the universe stretches the wavelength in a phenomenon called redshifting (because a longer wavelength is redder). Therefore, to observe 21-cm absorption from the early universe, astronomers must look at longer wavelengths of 6 to 21 meters (20 to 70 feet), in the radio portion of the electromagnetic spectrum.

Observing CMB shadows at radio wavelengths will be difficult due to interference by foreground sky sources. To gather accurate data, astronomers will have to use the next generation of radio telescopes, such as the Low Frequency Array (LOFAR) and the Square Kilometer Array (SKA). Although the observations will be a challenge, the potential payoff is great.

“There’s a gold mine of information out there waiting to be extracted. While its full detection may be experimentally challenging, it’s rewarding to know that it exists and that we can attempt to measure it in the near future,” said Loeb.

This research will be published in an upcoming issue of Physical Review Letters, and currently is available online at http://arxiv.org/abs/astro-ph/0312134.

Headquartered in Cambridge, Mass., the Harvard-Smithsonian Center for Astrophysics is a joint collaboration between the Smithsonian Astrophysical Observatory and the Harvard College Observatory. CfA scientists, organized into six research divisions, study the origin, evolution and ultimate fate of the universe.

Original Source: Harvard CfA News Release

Image credit: Fermilab
With the first data from their underground observatory in Northern Minnesota, scientists of the Cryogenic Dark Matter Search have peered with greater sensitivity than ever before into the suspected realm of the WIMPS. The sighting of Weakly Interacting Massive Particles could solve the double mystery of dark matter on the cosmic scale and of supersymmetry on the subatomic scale.

The CDMS II result, described in a paper submitted to Physical Review Letters, shows with 90 percent certainty that the interaction rate of a WIMP with mass 60 GeV must be less than 4 x 10-43 cm2 or about one interaction every 25 days per kilogram of germanium, the material in the experiment’s detector. This result tells researchers more than they have ever known before about WIMPS, if they exist. The measurements from the CDMS II detectors are at least four times more sensitive than the best previous measurement offered by the EDELWEISS experiment, an underground European experiment near Grenoble, France.

“Think of this improved sensitivity like a new telescope with twice the diameter and thus four times the light collection of any that came before it,” said CDMS II cospokesperson Blas Cabrera of Stanford University. “We are now able to look for a signal that is just one-fourth as bright as any we have seen before. Over the next few years, we expect to improve our sensitivity by a factor of 20 or more.”

The results are being presented at the April Meeting of the American Physical Society on May 3 and 4 in Denver by Harry Nelson and graduate student Joel Sanders, both of the University of California-Santa Barbara, and by Gensheng Wang and Sharmila Kamat of Case Western Reserve University.

“We know that neither our Standard Model of particle physics nor our model of the cosmos is complete,” said CDMS II spokesperson Bernard Sadoulet of the University of California at Berkeley. “This particular missing piece seems to fit both puzzles. We are seeing the same shape from two different directions.”

WIMPs, which carry no charge, are a study in contradictions. While physicists expect them to have about 100 times the mass of protons, their ghostly nature allows them to slip through ordinary matter leaving barely a trace. The term “weakly interacting” refers not to the amount of energy deposited when they interact with normal matter, but rather to the fact that they interact extremely infrequently. In fact, as many as a hundred billion WIMPs may have streamed through your body as you read these first few sentences.

With 48 scientists from 13 institutions, plus another 28 engineering, technical and administrative staffers, CDMS II operates with funding from the Office of Science of the U.S. Department of Energy, from the Astronomy and Physics Divisions of the National Science Foundation and from member institutions. The DOE’s Fermi National Accelerator Laboratory provides the project management for CDMS II.

“The nature of dark matter is fundamental to our understanding of the formation and evolution of the universe,” said Dr. Raymond L. Orbach, Director of DOE’s Office of Science. “This experiment could not have succeeded without the active collaboration of the DOE’s Office of Science and the National Science Foundation.”

Michael Turner, Assistant Director for Math and Physical Sciences at NSF, described identifying the constituent of the dark matter as one of the great challenges in both astrophysics and particle physics.

“Dark matter holds together all structures in the universe-including our own Milky Way-and we still do not know what the dark matter is made of,” Turner said. “The working hypothesis is that it is a new form of matter-which, if correct will shed light on the inner workings of the elementary forces and particles. In pursuing the solution to this important puzzle, CDMS is now at the head of the pack, with another factor of 20 in sensitivity still to come.”

Dark matter in the universe is detected through its gravitational effects on all cosmic scales, from the growth of structure in the early universe to the stability of galaxies today. Cosmological data from many sources confirm that this unseen dark matter totals more than seven times the amount of ordinary visible matter forming the stars, planets and other objects in the universe.

“Something out there formed the galaxies and holds them together today, and it neither emits nor absorbs light,” said Cabrera. “The mass of the stars in a galaxy is only 10 percent of the mass of the entire galaxy, so the stars are like Christmas tree lights decorating the living room of a large dark house.”

Physicists also believe WIMPs could be the as-yet unobserved subatomic particles called neutralinos. These would be evidence for the theory of supersymmetry, introducing intriguing new physics beyond today’s Standard Model of fundamental particles and forces.

Supersymmetry predicts that every known particle has a supersymmetric partner with complementary properties, although none of these partners has yet been observed. However, many models of supersymmetry predict that the lightest supersymmetric particle, called the neutralino, has a mass about 100 times that of the proton.

“Theorists came up with all of these so-called ‘supersymmetric partners’ of the known particles to explain problems on the tiniest distance scales,” said Dan Akerib of Case Western Reserve University. “In one of those fascinating connections of the very large and the very small, the lightest of these superpartners could be the missing piece of the puzzle for explaining what we observe on the very largest distance scales.”

The CDMS II team practices “underground astronomy,” with particle detectors located nearly a half-mile below the earth’s surface in a former iron mine in Soudan, Minnesota. The 2,341 feet of the earth’s crust shields out cosmic rays and the background particles they produce. The detectors are made of germanium and silicon, semiconductor crystals with similar properties. The detectors are chilled to within one-tenth of a degree of absolute zero, so cold that molecular motion becomes negligible. The detectors simultaneously measure the charge and vibration produced by particle interactions within the crystals. WIMPS will signal their presence by releasing less charge than other particles for the same amount of vibration.

“Our detectors act like a telescope equipped with filters that allow astronomers to distinguish one color of light from another,” said CDMS II project manager Dan Bauer of Fermilab. “Only, in our case, we are trying to filter out conventional particles in favor of dark matter WIMPS.”

Physicist Earl Peterson of the University Minnesota oversees the Soudan Underground Laboratory, also home to Fermilab’s long-baseline neutrino experiment, the Main Injector Neutrino Oscillation Search.

“I’m excited about the significant new result from CDMS II, and I congratulate the collaboration,” Peterson said. “I’m pleased that the facilities of the Soudan Laboratory contributed to the success of CDMS II. And I’m especially pleased that the work of Fermilab and the University of Minnesota in expanding the Soudan Laboratory has resulted in superb new physics.”

As CDSMII searches for WIMPs over the next few years, either the dark matter of our universe will be discovered, or a large range of supersymmetric models will be excluded from possibility. Either way, the CDMS II experiment will play a major role in advancing our understanding of particle physics and of the cosmos.

The CDMS II collaborating institutions include Brown University, Case Western Reserve University, Fermi National Accelerator Laboratory, Lawrence Berkeley National Laboratory, the National Institutes of Standards and Technology, Princeton University, Santa Clara University, Stanford University, the University of California-Berkeley, the University of California-Santa Barbara, the University of Colorado at Denver, the University of Florida, and the University of Minnesota.

Fermilab is a DOE Office of Science national laboratory operated under contract by Universities Research Association, Inc.

Original Source: Fermilab News Release