The angular resolution of conventional astronomical spectroscopy is limited to about 1 aresec by
the turbulent atmosphere. Much higher resolution can be obtained by
(a) objective prism speckle spectroscopy1, which yields diffraction-limited objective prism spectra, and by
(b) wideband projection speckle spectroscopy1, which yields spectrally dispersed 1-dimensional projections
of the object, i. e., object/spectrum reconstructions O(x,X) or O(x,y,X).