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We report molecular line and dust continuum observations toward the high-massstar forming region G331.5-0.1, one of the most luminous regions of massivestar-formation in the Milky Way, located at the tangent region of the Normaspiral arm, at a distance of 7.5 kpc. Molecular emission was mapped toward theG331.5-0.1 GMC in the CO (J=1-0) and C18O (J=1-0) lines with NANTEN, while itscentral region was mapped in CS (J=2-1 and J=5-4) with SEST, and in CS (J=7-6)and 13CO (J=3-2) with ASTE. Continuum emission mapped at 1.2 mm with SIMBA andat 0.87 mm with LABOCA reveal the presence of six compact and luminous dustclumps, making this source one of the most densely populated central regions ofa GMC in the Galaxy. The dust clumps are associated with molecular gas and theyhave the following average properties: size of 1.6 pc, mass of 3.2x10^3 Msun,molecular hydrogen density of 3.7x10^4 cm^{-3}, dust temperature of 32 K, andintegrated luminosity of 5.7x10^5 Lsun, consistent with values found towardother massive star forming dust clumps. The CS and 13CO spectra show thepresence of two velocity components: a high-velocity component at ~ -89 kms^{-1}, seen toward four of the clumps, and a low-velocity component at ~ -101km s^{-1} seen toward the other two clumps. Radio continuum emission is presenttoward four of the molecular clumps, with spectral index estimated for two ofthem of 0.8+-0.2 and 1.2+-0.2. A high-velocity molecular outflow is found atthe center of the brightest clump, with a line width of 26 km s^{-1} (FWHM) inCS (J=7-6). Observations of SiO (J=7-6 and J=8-7), and SO (J_K=8_8-7_7 andJ_K=8_7-7_6) lines provide estimates of the gas rotational temperature towardthis outflow >120 K and >75 K, respectively.

Physical characteristics of G331.5-0.1: The luminous central region of a Giant Molecular Cloud