TY - JOUR
T1 - SN 2007gr
T2 - 10th European VLBI Network Symposium and EVN Users Meeting: VLBI and the New Generation of Radio Arrays, EVN Symposium 2010
AU - Paragi, Zsolt
AU - Van Der Horst, Alexander
AU - Tanaka, Masaomi
AU - Taylor, Gregory
AU - Kouveliotou, Chryssa
AU - Granot, Jonathan
AU - Ramirez-Ruiz, Enrico
AU - Pidopryhora, Yurii
AU - Bourke, Stephen
AU - Campbell, Robert
AU - Garrett, Michael
AU - Van Langevelde, Huib
N1 - Publisher Copyright:
© Copyright owned by the author(s) under the terms of the Creative Commons Attribution-NonCommercial-ShareAlike Licence.
PY - 2010
Y1 - 2010
N2 - A nearby type Ic supernova, SN 2007gr was observed with the EVN in two epochs 60 days apart (second observation also included the Green Bank Telescope). In both cases one of the EVN stations was the Westerbork Synthesis Radio Telescope (WSRT), which recorded the observational data not only in the VLBI mode, but also in its normal interferometric mode. Thus it provided an important reference observation. In the first epoch the fluxes measured by the VLBI network and the WSRT alone match well. However in the second epoch the peak brightness observed in the VLBI experiment is much lower than the total flux recorded by the WSRT. There could be multiple reasons for this discrepancy: a resolution effect, coherence losses in VLBI, or extended emission contaminating the WSRT measurement. With new WSRT observations we costrain the level of background emission and find that there is still a difference between the corrected total flux density and the VLBI peak brightness. If one assumes that this is dominated by resolution, this would correspond to an average apparent expansion speed of ∼ 0.4c.
AB - A nearby type Ic supernova, SN 2007gr was observed with the EVN in two epochs 60 days apart (second observation also included the Green Bank Telescope). In both cases one of the EVN stations was the Westerbork Synthesis Radio Telescope (WSRT), which recorded the observational data not only in the VLBI mode, but also in its normal interferometric mode. Thus it provided an important reference observation. In the first epoch the fluxes measured by the VLBI network and the WSRT alone match well. However in the second epoch the peak brightness observed in the VLBI experiment is much lower than the total flux recorded by the WSRT. There could be multiple reasons for this discrepancy: a resolution effect, coherence losses in VLBI, or extended emission contaminating the WSRT measurement. With new WSRT observations we costrain the level of background emission and find that there is still a difference between the corrected total flux density and the VLBI peak brightness. If one assumes that this is dominated by resolution, this would correspond to an average apparent expansion speed of ∼ 0.4c.
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M3 - Conference article
AN - SCOPUS:85053735568
SN - 1824-8039
VL - 125
JO - Proceedings of Science
JF - Proceedings of Science
Y2 - 20 September 2010 through 24 September 2010
ER -