Computer Science
Scientific paper
Dec 1988
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988msngr..54...22c&link_type=abstract
The Messenger, vol. 54, p. 22-28
Computer Science
Infrared Interferometry:Supernovae, Infrared Radiation:Supernovae, Speckle Interferometry:Supernovae, Supernova 1987A In Lmc, Supernovae:Infrared Interferometry, Supernovae:Infrared Radiation, Supernovae:Speckle Interferometry
Scientific paper
The fireball in the LMC called SN 1987A offered an exceptional opportunity to study spatial structure of a supernova phenomenon. Obviously, special high angular resolution techniques at large telescopes had to be employed. The results of speckle interferometry in the visible spectral range, carried out at CTIO and AAT were reviewed by Meikle (1988). Here, we would like to present the results of speckle interferometry in the near infrared (xx 2-5 flm), carried out at the ESO 3.6-m telescope during May-August 1987. In contrast with the work in the visible range, mainly concerned with the ejecta (= 10 marcsec), the near IR speckle interferometry deals with the structure of the close environment of the supernova (= 100 marcsec). In particular, it addresses the interesting question whether this environment contained dust and thus provides a useful test of current models of the progenitor evolution. Indeed, some models suggest that the exploded blue supergiant (BSg) Sk69° 202 has once been a red supergiant (RSg). Part of the dust, condensed around the progenitor during its RSg phase, could survive destruction by the fast and hot wind of the BSg (Chevalier, 1987; Renzini, 1987). The burst of supernova radiation at shock breakout with Lb - 1043_1044 erg · S-1 should heat this dust up to 1,000-2,000°K. The corresponding thermal emission should then appear as an infrared echo (Bode and Evans, 1979). The size of the dusty region was expected to be of the order of 10^17-10^16 cm. At Earth, the corresponding angular size of 0.1 -1.0 arcsec is weil within the possibilities of speckle equipment. Shortly after the announcement of the supernova, we began to study the feasibility of observations. Computer modelling showed that the IR echo, if it existed, could be resolved already during the first months following the arrival of the explosion light. Independently, Prof. L. Woltjer, ESO Director General at that time, reserved 5 nights in May 1987 at the ESO 3.6-m telescope for IR speckle observations. After an exchange of telexes, we were in a plane to Santiago.
Chalabaev A. A.
Mariotti Jean-Marie
Perrier Ch.
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