Integral Identifies Supernova Rate For Milky Way

STELLAR CHEMISTRY

Radioactive decay of unstable isotopes leads to emission of gamma rays with a characteristic energy (in colour) being determined by properties of the atomic nucleus. ESA�s Integral satellite observatory has been measuring such gamma rays since October 2002. Radioactive isotopes are by-products of nuclear fusion reactions, which produce new atomic nuclei in stellar interiors and in supernovae. In the gamma-ray light of Al 26 isotopes, which decay after about a million years to magnesium, one sees the radioactive glow of regions of the galaxy with recent production of new nuclei. Visible light, on the other hand, often cannot reach us from stars in those regions, due to occulting interstellar gas clouds. The background image shows our Milky Way galaxy, as it would appear in visible wavelengths, if projected into a galactic co-ordinate system where the plane of the galaxy is a horizontal straight line; superimposed is the Al 26 sky image from COMPTEL, which shows bright emission from regions with massive young stars. The insets at lower right show the effect of the rotating galaxy on the gamma rays reaching Integral. Credits: MPE

Garching, Germany (SPX) Jan 10, 2006
Using ESA's Integral observatory, an international team of researchers has been able to confirm the production of radioactive aluminium (Al 26) in massive stars and supernovae throughout our galaxy and determine the rate of supernovae - one of its key parameters.

The team, led by Roland Diehl of the Max Planck Institute for Extraterrestrial Physics in Garching, Germany, determined that gamma rays from the decay of Al 26 originate from the central regions of our galaxy, implying that production of new atomic nuclei is an ongoing process and occurs in star-forming regions galaxy-wide.

Our environment is composed of chemical elements formed long ago by nuclear fusion reactions in stellar interiors and supernovae. This process of 'nucleosynthesis' leads to the emission of gamma rays, which easily reach us from all regions of our galaxy. ESA's Integral observatory has been measuring such gamma rays since October 2002.

Roland Diehl and his colleagues were able to measure the Al 26 gamma-ray emissions along the plane of the inner galaxy.

However, because the disc of the galaxy rotates about its central axis, with the inner regions orbiting faster, gamma rays from decaying Al 26 observed from these regions should be moderated by the Doppler effect in a characteristic way. It is this characteristic pattern that has been found by Integral.

From this measurement, the team found that Al 26 decay gamma rays do indeed reach us from the inner regions of the galaxy, rather than from foreground regions along the same line of sight possibly caused by local and peculiar Al 26 production. These regions would not have the observed high relative velocity.

From these new observations, it is possible to estimate the total amount of radioactive Al 26 in our galaxy as is equivalent to three solar masses. This is a lot, given that Al 26 is an extremely rare isotope; the fraction estimated for the early Solar System is 5/100 000 of Al 26, in proportion to its stable aluminium isotope (Al 27).

Because astrophysicists had inferred that the likely sources are mainly massive stars, which end their lives as supernovae, they could estimate the rate of such supernova events. They obtained a rate of one supernova every 50 years - consistent with what had been indirectly found from observations of other galaxies and their comparison to the Milky Way.

Integral's study of gamma rays will continue to operate for several more years. Astrophysicists hope to increase the precision of such measurements. Project leader Roland Diehl said, "These gamma-ray observations provide insights about our home galaxy, which are difficult to obtain at other wavelengths due to interstellar absorption."

These Integral based studies appear in the 439th issue of the scientific journal Nature, in an article titled: 'Radioactive 26Al and massive stars in the Galaxy', by R. Diehl, lead author, H. Halloin, K. Kretschmer, G.G. Lichti, V. Sch�nfelder, A.W. Strong, A. von Kienlin and W. Wang, (Max Planck Institute for Extraterrestrial Physics, Garching, Germany), P. Jean, J. Kn�dlseder, J.P.Roques, G.Weidenspointner (Centre d'Etude Spatiale des Rayonnements and Universit� Paul Sabatier, Toulouse, France), S. Schanne (DSM/DAPNIA/Service d'Astrophysique, CEA Saclay, Gif-Sur-Yvette, France), D.H.Hartmann (Clemson University, USA), C. Winkler (ESA, Noordwijk, the Netherlands), and C. Wunderer (Space Sciences Lab., Berkeley, USA)

MILKY WAY

Galaxy's Neighboring Spiral Arm Is Closer Than Thought

Boston MA (SPX) Dec 28, 2005
The Perseus spiral arm - the nearest spiral arm in the Milky Way outside the Sun's orbit - lies only half as far from Earth as some previous studies had suggested. An international team of astronomers measured a highly accurate distance to the Perseus arm for the first time using a globe-spanning system of radio dishes known as the Very Long Baseline Array (VLBA), which offers the sharpest vision of any telescope in existence. Additional VLBA measurements will help astronomers to determine the true structure of the Milky Way.