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We present a study of the molecular gas and interstellar dust distribution inthe environs of the HII region NGC 3503 associated with the open cluster Pis 17with the aim of investigating the spatial distribution of the molecular gaslinked to the nebula and achieving a better understanding of the interaction ofthe nebula and Pis 17 with their molecular environment.  We based our study in ^{12}CO(1-0) observations of a region of ~0.6 deg. insize obtained with the 4-m NANTEN telescope, unpublished radio continuum dataat 4800 and 8640 MHz obtained with the ATCA telescope, radio continuum data at843 MHz obtained from SUMSS, and available IRAS, MSX, IRAC-GLIMPSE, and MIPSGALimages.  We found a molecular cloud (Component 1) having a mean velocity of -24.7 kms^{-1}, compatible with the velocity of the ionized gas, which is associatedwith the nebula and its surroundings. Adopting a distance of 2.9 +/- 0.4 kpcthe total molecular mass and density yield (7.6 +/- 2.1) x 10^3 Msun and 400+/- 240 cm^{-3}, respectively.  The radio continuum data confirm the existence of an electron densitygradient in NGC 3503. The IR emission shows the presence of a PDR bordering thehigher density regions of the nebula. The spatial distribution of the COemission shows that the nebula coincides with a molecular clump, with thestrongest CO emission peak located close to the higher electron density region.The more negative velocities of the molecular gas (about -27 km s^{-1}), iscoincident with NGC 3503. Candidate YSOs were detected towards the HII region,suggesting that embedded star formation may be occurring in the neighbourhoodof the nebula. The presence of a clear electron density gradient, along withthe spatial distribution of the molecular gas and PAHs in the region indicatesthat NGC 3503 is a blister-type HII region that probably has undergone achampagne phase.

NGC 3503 and its molecular environment