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We present results from a Chandra observation of the NGC346 cluster. Thiscluster contains numerous massive stars and is responsible for the ionizationof N66, the most luminous HII region and the largest star formation region inthe SMC. In this first paper, we will focus on the characteristics of the mainobjects of the field. The NGC346 cluster itself shows only relatively faintX-ray emission (with L_X^{unabs} ~ 1.5 times 10^{34} erg s^{-1}), tightlycorrelated with the core of the cluster. In the field also lies HD5980, a LBVstar in a binary (or possibly a triple system) that is detected for the firsttime at X-ray energies. The star is X-ray bright, with an unabsorbed luminosityof L_X^{unabs} ~ 1.7 times 10^{34} erg s^{-1}, but needs to be monitoredfurther to investigate its X-ray variability over a complete 19d orbital cycle.The high X-ray luminosity may be associated either with colliding winds in thebinary system or with the 1994 eruption. HD5980 is surrounded by a region ofdiffuse X-ray emission, which is a supernova remnant. While it may be only achance alignment with HD5980, such a spatial coincidence may indicate that theremnant is indeed related to this peculiar massive star.Comment: 12 pages, 9 figures (3 in jpg and 6 in ps), to be published in Ap

An X‐Ray Investigation of the NGC 346 Field in the Small Magellanic Cloud I. The Luminous Blue Variable HD 5980 and the NGC 346 Cluster