THE EARLY ULTRAVIOLET, OPTICAL, AND RADIO EVOLUTION OF THE SOFT-X-RAYTRANSIENT GRO J0422+32

We have monitored the evolution of the transient X-ray source GRO J042 2 + 32 from approximately 2 weeks postdiscovery into its early decline phase at ultraviolet, optical, and radio wavelengths. Optical and ult raviolet spectra exhibit numerous, but relatively weak, high-excitatio n emission lines such as those arising from He II, N III, N V, and C I V superposed on an intrinsically blue continuum. High-resolution optic al spectroscopy reveals line profiles which are double peaked, and in the case of the higher order Balmer lines, superposed on a broad absor ption profile. The early outburst optical-ultraviolet continuum energy distribution is well represented by a two power-law fit with a break at congruent-to 4000 angstrom. Radio observations with the VLA reveal a flat-spectrum source, slowly increasing in intensity at the earliest epochs observed, followed by an approximate power-law decay light cur ve with an index of - 1. Light curves for each wavelength domain are p resented and discussed. Notable are the multiple secondary outbursts s een in the optical more than 1 year postdiscovery, and spectral change s associated with secondary rises seen in the radio and UV. We find th at the ultraviolet and optical characteristics of GRO J0422 + 32 as we ll as its radio evolution, are similar to other recent well-observed s oft X-ray transients (also called X-ray novae) such as Cen X-4, A0620- 00 (V616 Mon), and Nova Muscae 1991 (GS 1124-683), suggesting that GRO J0422 + 32 is also a member of that subclass of low-mass X-ray binari es. We present definitive astrometric determination of the source posi tion, and place an upper limit of R congruent-to 20 from our analysis of the POSS. Additionally, we derive distinct values for color excess from analysis of the optical [E(B - V) = 0.23] and ultraviolet [E(B - V) = 0.4] data, suggesting an intrinsic magnitude of 19-19.5 for the p rogenitor if it is mid-K dwarf. This leads to a likely range of 2.4-3. 0 kpc for the source distance, which is consistent with our separate e stimate of 2.4 +/- 0.4 kpc based on measurement of the NaD interstella r line profile. Adopting 2.4 kpc and E(B - V ) = 0.23, the outburst ab solute magnitude was M congruent-to 0.0, which is a typical value for this class of objects.