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

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