High flying astronomy with German instrument
Infrared Spectrometer on board the Sofia observatory successfully completes maiden flight
As the Jumbo touched down on the runway of the Dryden Aircraft Operations Facility in Palmdale/California at 6.40 am local time it heralded in a new era for observational astronomy: it was April 6, 2011, and the jet which had been converted into the Sofia infrared observatory had just completed its first research flight with Great, the spectrometer developed by a team which included the Max Planck Institute for Radio Astronomy. The observation programme included the M 17 molecular cloud, a region of our galaxy with increased star formation, and also galaxy IC 342 only a few million light years away.
“These very first spectra recorded by Great are the reward for investing years of hard work in cutting-edge technology developments for the spectrometer. They demonstrate the outstanding scientific potential of airborne far-infrared spectroscopy,” says a delighted project leader Rolf Güsten, one of the scientists at the Max Planck Institute for Radio Astronomy in Bonn/Germany, after the maiden flight. The large collecting area of the 2.7-m diameter telescope coupled with great progress in terahertz technologies in recent years allow Great to collect data 100 times faster than in earlier experiments. “This opens up the way for unique scientific observations.”
Great is an acronym for German Receiver for Astronomy at Terahertz Frequencies and was developed under Güsten’s leadership by researchers at the Bonn Max Planck Institute and the University of Cologne, in collaboration with the Max Planck Institute for Solar System Research and the DLR Institute of Planetary Research. The instrument uses the high flight altitude of the Sofia stratospheric observatory, currently the only flying observatory in the whole world, because at altitudes of ten to 13 kilometres above ground level the earth’s atmosphere becomes transmissive to the far-infrared radiation from space as well, radiation which is absorbed by the water vapour in the layers below. This gives the observatory access to spectral lines which are important for astronomical observations.
On its flight on April 6, Great observed not only the radiation from ionised carbon at a frequency of 1.9 terahertz (corresponding to a wavelength of 0.158 millimetres) but also spectral lines of warm carbon monoxide at high excitation in the M 17 and IC 342 sources. These lines bear witness to atomic processes which lead to a cooling of the interstellar matter. The balance between heating and cooling processes, on the other hand, regulates the temperature of the interstellar medium, thereby controlling the initial conditions for the formation of new stars.
Jürgen Stutzki from the University of Cologne, the team’s second project manager, says: “The ionized carbon line is excited by the intense ultraviolet radiation from new-born stars. It provides us with a unique insight into the physical processes and chemical conditions in the stellar nurseries. Sofia enables us to understand how infant stars form and how they change the clouds which gave birth to them.”
“The receiver’s first scientific flight marks the beginning of German-American scientific collaboration in the Sofia project. We are looking forward to the future measurement operations with confidence," says Alois Himmes, Sofia Project Manager at the German Aerospace Center (DLR). After these initial characterization flights, the observatory will become available for the use of interested astronomers. “In summer 2011, German astronomers will conduct scientific observations with Sofia for the first time,” explains Alfred Krabbe, the Head of the German Sofia Institute (DSI) at the University of Stuttgart.
(HOR / NJ)
the German Receiver for Astronomy at Terahertz Frequencies, is a receiver for spectroscopic observations in the far-infrared region of the electromagnetic spectrum between frequencies of 1.25 and 5 terahertz (60-240 microns wavelength), which are not accessible from the ground because they are absorbed by water vapour in the atmosphere. Great was developed by the Max Planck Institute for Radio Astronomy (MPIfR) and the University of Cologne, in collaboration with the Max Planck Institute for Solar System Research and the DLR Institute of Planetary Research. Rolf Güsten (MPIfR) is the project manager for Great. The development of the instrument was financed by the participating institutes, the Max Planck Society, the German Research Foundation and the German Aerospace Center (DLR).
The Stratospheric Observatory for Infrared Astronomy is a joint project between the German Aerospace Center (DLR) and the National Aeronautics and Space Administration (NASA). It is funded on behalf of the DLR by the Federal Ministry of Economics and Technology on the basis of legislation by the German Parliament, and also by the State of Baden-Württemberg, and the University of Stuttgart. The operation of the scientific programme is coordinated in Germany by the German Sofia Institute (DSI) at the University of Stuttgart; in the US the coordination is undertaken by the Universities Space Research Association (USRA).
An interstellar molecular cloud containing around 10,000 solar masses of gas that is illuminated by a cluster of young stars with a total luminosity of more than one million solar luminosities. The ultraviolet radiation from the cluster ionises and heats the molecular gas, possibly compressing it into a state which gives rise to more stars. The Sofia observations make it possible to measure the effect of this compression and compare it to the heating effect of the gas that leads to an expansion. This enables us to investigate the star-forming process.
The nearest gas-rich spiral galaxy with active star formation in its nucleus. Within its central 30 arc seconds two spiral arms with molecular gas end in a clumpy central ring of dense gas, which in turn surrounds a young star cluster. Its massive young stars heat the ambient gas and dust and create a rich chemistry and intense emission from this region, which specialists call a photon dominated region (PDR). The intense emission from these PDRs allows the in-depth study of the chemical and physical conditions for the formation of massive stars - not only in our Milky Way, but also in neighbouring galaxies.