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IRAS 18511+0146 is a young embedded (proto)cluster located at 3.5 kpcsurrounding what appears to be an intermediate mass protostar. In this paper,we investigate the nature of cluster members (two of which are believed to bethe most massive and luminous) using imaging and spectroscopy in the near andmid-infrared. The brightest point-like object associated with IRAS 18511+0146is referred to as S7 in the present work (designated UGPS J185337.88+015030.5in the UKIRT Galactic Plane survey). Seven of the nine objects show risingspectral energy distributions (SED) in the near-infrared, with four objectsshowing Br-gamma emission. Three members: S7, S10 (also UGPSJ185338.37+015015.3) and S11 (also UGPS J185338.72+015013.5) are bright inmid-infrared with diffuse emission being detected in the vicinity of S11 in PAHbands. Silicate absorption is detected towards these three objects, with anabsorption maximum between 9.6 and 9.7 um, large optical depths (1.8-3.2), andprofile widths of 1.6-2.1 um. The silicate profiles of S7 and S10 are similar,in contrast to S11 (which has the largest width and optical depth). The colddust emission investigated using Herschel HiGal peaks at S7, with temperatureat 26 K and column density N(H2) ~ 7 x 10^(22) cm^(-2). The bolometricluminosity of IRAS 18511 region is L ~ 1.8 x 10^4 L_sun. S7 is the maincontributor to the bolometric luminosity, with L (S7) > 10^4 L_sun. S7 is ahigh mass protostellar object with ionised stellar winds, evident from thecorrelation between radio and bolometric luminosity as well as the asymmetricBr-gamma profile. The differences in silicate profiles of S7 and S11 could bedue to different radiation environment as we believe the former to be moremassive and in an earlier phase than the latter.

Dust and Gas environment of the young embedded cluster IRAS 18511+0146