SPECTROSCOPY OF STARS IN THE GALAXY NGC-2403

We present the results of multiobject spectroscopy of 44 stars in NGC 2403, which is aimed at searching for SS 433 and LBV candidates. The p arameters of the H alpha line and the relative intensities of the [N I I] lambda 6583 and [S II] lambda 6716 lines are given. We identified 1 9 LBV candidates, nine of which are most reliable-three nonvariable st ars and six from among the known variables; we also identified seven c andidates for supergiants. Five of these stars (ZH 702, 917, S 44, 182 , and v35) can be considered as SS 433 candidates. Many objects have a mbiguous identifications, because either the spectrum of an H II regio n or the spectrum of a supernova remnant contributes to their spectra. We identified nine candidates for supernova remnants, 13 H II regions , two probable star clusters, and four (Galactic) field stars. The bri ghtest visual star in NGC 2403 is the LBV candidate S 185 with the lum inosity M-V = -10(m). The red star SR 195 is as bright as the star eta Car, if it is not a chance projection of a Galactic dwarf onto a stru ctured H Il region in NGC 2403. We corroborate the conclusion that the re are more young massive stars in NGC 2403 than in M 81. We conclude that NGC 2403 is similar in the luminosity of the brightest blue stars to M 33.