The results described here are due to a productive collaboration between the ALFA and 3D teams. We are particularly grateful to S. Anders, N. Thatte, L. E. Tacconi-Garman, F. Eisenhauer, and M. Tezca.
|Objects observed include:|
|1998||HEI 7||0.26" binary - the first result, described below|
|1999||T Tau||intermediate mass young stellar binary object|
|BD +31 643||binary system with dust disk|
|NGC 1161||LINER galaxy|
|G 45.45 +0.06||ultra compact HII region|
|MWC 1080||Herbig Ae/Be star with companion 0.75" away and 3.3mag fainter|
|NGC 1068||archetypal Seyfert 2 galaxy|
Each of the K-band (2.2 micron) images above is 1.2" on a side. The PSF reference (left) shows a diffraction limited core and bits of the first ring. The binary (right) has an extra component above and to the right of the main star - the secondary star, 3 magnitudes (a factor of 10) fainter.
The spectra of the primary star (green) and secondary (red) are shown above. There are some similarities such as the Mg absorption at 2.28 microns But definite differences can also be seen, even though the spectra were extracted from stars only 0.26" apart: the Ca line at 2.26 microns and first CO bandhead at 2.29 microns.
This result is very encouraging, and provides a glimpse of the possibilities that such techniques will open up.
Data reduced & figures drawn by N. Thatte