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This study explores the effects of different assumptions and systematics onthe determination of the local, spatially resolved star formation law. Usingfour star formation rate (SFR) tracers (H\alpha with azimuthally averagedextinction correction, mid-infrared 24 micron, combined H\alpha andmid-infrared 24 micron, and combined far-ultraviolet and mid-infrared 24micron), several fitting procedures, and different sampling strategies we probethe relation between SFR and molecular gas at various spatial resolutions andsurface densities within the central 6.5 kpc in the disk of NGC4254. We findthat in the high surface brightness regions of NGC4254 the form of themolecular gas star formation law is robustly determined and approximatelylinear and independent of the assumed fraction of diffuse emission and the SFRtracer employed. When the low surface brightness regions are included, theslope of the star formation law depends primarily on the assumed fraction ofdiffuse emission. In such case, results range from linear when the fraction ofdiffuse emission in the SFR tracer is ~30% or less (or when diffuse emission isremoved in both the star formation and the molecular gas tracer), tosuper-linear when the diffuse fraction is ~50% and above. We find that thetightness of the correlation between gas and star formation varies with thechoice of star formation tracer. The 24 micron SFR tracer by itself shows thetightest correlation with the molecular gas surface density, whereas theH\alpha corrected for extinction using an azimuthally-averaged correction showsthe highest dispersion. We find that for R<0.5R_25 the local star formationefficiency is constant and similar to that observed in other large spirals,with a molecular gas depletion time ~2 Gyr.

CARMA Survey Toward Infrared-bright Nearby Galaxies (STING): Molecular Gas Star Formation Law in NGC4254