WHAT IS STILL IN THE FBS PLATES

5350 interesting objects have been selected from the FBS plates, including 300 AGN. There are 3 catalogs at CDS with objects discovered using the FBS. Its observational material is still useful. A number of new surveys may be undertaken using the FBS spectra. And especially it will be efficient to use the digitized FBS for any studies. The use of the digitized spectra will increase the efficiency and homogeneity of object selection. A few research projects are planned based on the DFBS low-dispersion spectra, such as:

·         new bright QSOs (<18^m). One can expect some 200 new bright QSOs with m<16^m from FBS, and some 1000 fainter objects, and it will be the most complete sample for study of their local density;

·         new Markarian (UVX) galaxies. The eye selection has missed objects near the limits of the plates. It will be particularly useful to study their population at higher redshifts; 

·         new blue stellar objects. The 2nd part of the FBS will be continued for the whole area and a total number of some 4500 objects is expected (new WDs, sds, CVs, PNN, etc.);

·         new blue compact dwarf galaxies. 22 Markarian galaxies and 135 SBS galaxies are candidate BCDGs. BCDGs are important for understanding the early stages of galaxy evolution, and they are crucial targets for SST because they represent the primordial stages of galaxy formation.

·         optical counterparts of IR, radio, X-ray and other sources (optical identifications). The use of the DFBS will allow continue the program of IRAS identifications to other regions of the FBS with a comparison with 2MASS data and their future study with SST, as well as identify radio and X-ray sources;

·         late-type stars (M, S, carbon stars). For automatic selection it will be easier to separate real spectra from artifacts having the modeled templates beforehand;

·         planetary nebulae; to locate all PN in the Galaxy, particularly at high galactic latitudes;

·         all emission line stars (cataclysmic variables, etc). 1D spectral cuts and computer analysis will greatly improve discovery of such objects;

·         non-UVX white dwarfs. There are a lot of WDs without UVX. Many such objects have been located during the Second part of the FBS. They will complement the sample of high-latitude WDs for further studies on stellar evolution and evolution of the Galactic halo;

·         studies of star clusters and clusters of galaxies. It is useful to study clusters using homogeneous observational material, especially having low-dispersion spectra of all the objects.

DFBS provides an earlier time epoch for comparison with other all-sky surveys (such as SDSS), which are now underway, opening a new window in the time domain. For example, changes in brightness and optical spectra on the time scale of decades can be studied.