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evn:evn_scince [2016/04/22 08:31] – michael.lindqvistevn:evn_scince [2016/04/22 08:33] (current) – [Introduction] michael.lindqvist
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 The [[http://www.evlbi.org/|European VLBI Network (EVN)]] is a VLBI network of radio telescopes in Europe and beyond, operated by an international Consortium of institutes. The EVN operates an “open sky” policy and observing proposals are accepted (and peer-reviewed) from astronomers from all over the world. The next deadline is June 1, 2016. In order to inspire you, please have a look at the following 3 science highlights from the EVN.  The [[http://www.evlbi.org/|European VLBI Network (EVN)]] is a VLBI network of radio telescopes in Europe and beyond, operated by an international Consortium of institutes. The EVN operates an “open sky” policy and observing proposals are accepted (and peer-reviewed) from astronomers from all over the world. The next deadline is June 1, 2016. In order to inspire you, please have a look at the following 3 science highlights from the EVN. 
  
-Use of the Network by astronomers not specialised in the VLBI technique is encouraged. The [[http://www.jive.eu/|Joint Institute for VLBI ERIC (JIVE)]] can provide support for schedule making (Bob Campbell, campbell@jive.eu), for correlation and data analysis of EVN projects, as well as advice during proposal preparation, contact Zsolt Paragi (zparagi@jive.eu). 
  
  
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 Figure 1. Relative measured positions of B1929+10 with the best fit proper motion removed. The solid line is the best fit parallax from all available data combined. Solid dots show the most recent measurements at 5 GHz, open stars are the data from Brisken et al. 2002 (ApJ, 571, 906, 2002), and squares are the data from Chatterjee et al. 2004 (ApJ, 604, 339). Figure 1. Relative measured positions of B1929+10 with the best fit proper motion removed. The solid line is the best fit parallax from all available data combined. Solid dots show the most recent measurements at 5 GHz, open stars are the data from Brisken et al. 2002 (ApJ, 571, 906, 2002), and squares are the data from Chatterjee et al. 2004 (ApJ, 604, 339).
  
-===== Star formation =====+===== The magnetic fields around  young stellar objects =====
 Since 2009, Surcis and collaborators have been running a large VLBI project with the EVN to measure the magnetic field at AU scales around 31 massive young stellar objects (YSOs). By observing the polarised emission of 6.7 GHz methanol masers the structure of the magnetic field for 19 sources has been obtained so far, an example is shown in Fig. 2. A first statistical analysis of these sources reveals that the magnetic field around the YSOs is preferentially oriented in the same way as the molecular outflows ejected from the sources (Surcis et al. 2015). For several sources it was possible to obtain a detailed description of the magnetic field. The results are published in Surcis et al. 2013, A&A 556, 73 and Surcis et al. 2015, A&A 578, 102. Since 2009, Surcis and collaborators have been running a large VLBI project with the EVN to measure the magnetic field at AU scales around 31 massive young stellar objects (YSOs). By observing the polarised emission of 6.7 GHz methanol masers the structure of the magnetic field for 19 sources has been obtained so far, an example is shown in Fig. 2. A first statistical analysis of these sources reveals that the magnetic field around the YSOs is preferentially oriented in the same way as the molecular outflows ejected from the sources (Surcis et al. 2015). For several sources it was possible to obtain a detailed description of the magnetic field. The results are published in Surcis et al. 2013, A&A 556, 73 and Surcis et al. 2015, A&A 578, 102.
  
evn/evn_scince.1461313883.txt.gz · Last modified: 2016/04/22 08:31 by michael.lindqvist