The shape, expansion rate and distance of supernova 1993J from VLBI measurements

April 1994 • 1994Natur.368..610B

Authors • Bartel, N. • Bietenholz, M. F. • Rupen, M. P. • Conway, J. E. • Beasley, A. J. • Sramek, R. A. • Romney, J. D. • Titus, M. A. • Graham, D. A. • Altunin, V. I. • Jones, D. L. • Rius, A. • Venturi, T. • Umana, G. • Francis, R. L. • McCall, M. L. • Richer, M. G. • Stevenson, C. C. • Weiler, K. W. • van Dyk, S. D. • Panagia, N. • Cannon, W. H. • Popelar, J. • Davis, R. J.

Abstract • SUPERNOVA 1993J is one of the closest supernovae discovered this century, allowing observations with very high linear resolution. Radio emission from the supernova became visible within days of the first optical peak, and has remained strong, making this an ideal source for very-long-baseline interferometry (VLBI) investigations^1-7. Here we report the results of a series of VLBI observations, made from one to three months after the supernova explosion. We find that the supernova is circularly symmetric, which is somewhat surprising in view of suggestions that the progenitor was a member of a binary system^8,9 , and the asymmetry implied by optical observations¹⁰. The supernova shows no sign of deceleration, and the expansion velocities that we estimate from the VLBI measurements are consistent with the maximum optical line velocities¹¹, suggesting that the radio emission indeed arises from the shock front, where the ejecta are hitting the gas that surrounded the progenitor star. We combine the angular expansion rate determined by the VLBI data with the optically derived expansion speed to estimate a distance to M81 of 4.0 +/- 0.6 Mpc, consistent with the value obtained from measurements of Cepheid variables in M81, 3.63 +/-0.34 Mpc (ref. 12).

Links

• SIMBAD http://simbad.u-strasbg.fr/simbo.pl?bibcode=1994Natur.368..610B
• NED https://ned.ipac.caltech.edu/uri/NED::InRefcode/1994Nat...368..610B
• ELECTR https://doi.org/10.1038%2F368610a0