Astron. Astrophys. 346, 892-896 (1999)

4. Conclusions

We observed Z CMa with the integral field spectrograph OASIS coupled to the adaptive optics bonette PUE'O.

The image centroid evolution with wavelength was measured with a super resolution of . Using the binary parameters derived from speckle interferometry observations at similar wavelengths we were able to recover the spectra of each component. The primary emerges as the emission line object and the secondary (optical primary) presents a spectrum typical of the system before the 1987 outburst.

Z CMa jet was imaged at a 0.24" resolution in the [OI]6300. It consists of an elongated structure whose width is unresolved and whose axis passes through the primary, and of an unresolved base with a wide range in velocities. This morphology is similar to Classical TTauri Stars' microjets. The part of the jet sampled by our observations is associated with the material ejected in the 1987 outburst.

We have shown that, for pre-main sequence binaries whose system parameters (separation and flux ratio) are known from broad band high angular resolution observations, integral field spectroscopy can recover their spectra for separations up to 6 times smaller than the actual IFS+AO angular resolution. This technique is very promising for the study of activity in close pre-main sequence binaries.

© European Southern Observatory (ESO) 1999

Online publication: June 17, 1999
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