On January 25, 2012, RadioAstron has successfully detected the first interferometric signal at 92 cm from individual pulses of the pulsar B0950+08 from the longest distance to the space craft - 300,000 km. Projected interferometer baseline was 220,000 km which provided the highest ever achieved resolution at this wave length of about 1/1000 arcsecond. The ground VLBI stations which participated in this experiment are Arecibo (USA), Westerbork (the Netherlands), and Effelsberg (Germany). The interference fringes were found between the space radio telescope and all three ground telescopes.

Published by the editorial team, 21 March 2012

The observed variations of the correlated signal from the pulsar is due to the propagation effects - pulsar emission scintillation on the inhomogeneous interstellar plasma. Such effect is only seen for emission of very compact objects. Thus, astronomers have got a tool to study characteristics of the interstellar medium and the pulsar itself, to localize the pulsar radiation zone in the magnetosphere of the neutron star - either above the polar cap or near the light cylinder. The conducted experiment has both confirmed RadioAstron capabilities at 92 cm and provided first important scientific data in this band. About ten brightest radio pulsars of our Galaxy are planned to be studied in the RadioAstron early science programme.

Tests of the closed-loop mode of Spektr-R synchronization

A test in a special closed-loop mode of Spektr-R synchronization was successfully performed on January 22, 2012. This mode of operation utilizes the ground based maser clock located at the Pushchino tracking station to synchronize the space radio telescope observations through a special up-down phase link at 7.2 and 8.4 GHz. As a result of these observations at 18 cm, an interference fringe was found by the RadioAstron correlator from the quasar 0212+735 at the projected distance of about 16,000 km.

Successful Spektr-R orbit correction

In order to correct the orbit of Spektr-R, two injections were done on February 22 and March 1, 2012, with a total momentum of about 3 m/sec. The correction was performed successfully. As a result, the perigee of the space craft orbit has increased to about 55,000 km, the ballistic life time of the orbit has increased to ten years.

The RadioAstron early science program and final steps of the fringe search

Regular experiments within the RadioAstron early science program (ESP) have started in February 2012. Hydroxyl and water masers in our Galaxy (W3OH, Orion KL, etc.), the Crab pulsar as well as bright active galactic nuclei were observed since then. These experiments were supported from the ground by more than ten different VLBI stations: the European VLBI Network telescopes including the Russian ones, the Ukrainian Eupatoria, the Japanese Usuda. The international RadioAstron ESP working groups are reducing and analyzing the data together with the Astro Space Center correlator.

The fringe search experiments are finishing. First segments of 1.3 cm observations have failed due to very bad weather conditions on the ground (GBT, Effelsberg). The search for 1.3 cm fringes continues. Additionally, first test experiments with the Australian VLBI network LBA were performed on March 11, 2012, to prepare for science observations with LBA preliminary planned for May 2012.

You can find more information about the RadioAstron project on: http://www.asc.rssi.ru/radioastron/

The Russian version of this news message can be found here: http://www.asc.rssi.ru/radioastron/news/news_ru.pdf


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On June 13-17, the LOFAR Family Meeting took place in Cologne. After two years LOFAR researchers could finally meet in person again. The meeting brings together LOFAR users and researchers to share new scientific results.

Our renewed ‘Melkwegpad’ (Milky Way Path) is finished! The new signs have texts in Dutch on the one side and in English on the other side. The signs concerning planets have a small, 3D printed model of that planet in their centre.
#Melkwegpad @RTVDrenthe

Daily image of the week

The background drawing shows how the subband correlator calculates the array correlation matrix. In the upper left the 4 UniBoard2s we used. The two ACM plots in the picture show that the phase differences of the visibilities vary from 0 to 360 degrees.

Daily image of the week: Testing with the Dwingeloo Test Station (DTS)
One of the key specifications of LOFAR2.0 is measuring using the low- and the highband antenna at the same time. For this measurement we used 9 lowband antenna and 3 HBA tiles.