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We have identified a low surface brightness stellar stream from visualinspection of SDSS imaging for the edge-on, spiral galaxy NGC5387. A blueoverdensity was also identified in SDSS coincident with the stream intersectionwith the NGC5387 disk. The overdensity was also detected in the GALEX DeepImaging Survey and found to contribute 38% of the total FUV integrated fluxfrom NGC5387, which suggests that the region is actively forming stars. Deeperimaging was acquired with the Vatican Advanced Technology Telescope (VATT) inthe B, V, and R filters that confirmed the presence of both the stellar streamand the blue overdensity. Analysis of the VATT photometry indicates the stellarstream is red in color, B-V = 0.7, and has a stellar mass of 6x10^8M$_{\odot}$, which implies a merger ratio of 1:50. Assessment of the streammorphology suggests that the merger event has a circular radius, R~16 kpc, thestream formed in ~400 Myr, and the progenitor had a total mass of ~2x10M$_{\odot}$. Spectroscopy from LBT+MODS1 was used to determine that the blueoverdensity is at the same redshift as NGC5387, consists of young stellarpopulations (~10 Myr), is metal-poor (12 + log(O/H) = 8.03), and forming starsat an enhanced rate (~1-3 M$_{\odot}$/year) given its total stellar mass(2x10^7 M$_{\odot}$). Several interpretations are posited to explain theseobservational data, of which the most likely are (i) that the blue overdensityis a region of enhanced star formation in the outer disk of NGC5387 induced bythe minor accretion event, and (ii) that the blue overdensity is the progenitorof the stellar stream undergoing a period of enhanced star formation as aresult of its interaction with NGC5387. Confirmation and theoreticalexploration of these scenarios are presented in a companion paper.

Cannibalization and Rebirth in the NGC5387 System. I. The Stellar Stream & Star Forming Region