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tokens: in the two transitions. There is no known maser association with this core but the two are both associated with H 2 O (clusters 1 and 2, respectively), and CH 3 OH masers (Slysh etal. 1999 ). Based on our detections of two bipolar outflows in Sh2-76E, we can confirm the presence of at least two YSOs. This does not rule out the possibility of the presence of a much earlier stage YSO that is not yet driving maser emissions. However, we have explore the infrared point source catalogue to verify the nature of the possible driving sources of the outflows. We have selected infrared source with 1arcsec from the cluster positions and used them to construct the spectral energy distribution (SED) of the driving sources using Robitaille etal. ( 2006 ) SED fit tool while adopting our parallax distance. We found Two Micron All Sky Survey (2MASS) and Wide-field Infrared Space Exploration ( WISE ) points sources associated with Sh2-76EMM1 but only 2MASS point source for Sh2-76EMM2. Fig. 6 shows the SED of Sh2-76EMM1 (left-hand panel) and Sh2-76EMM2 (right-hand panel). The SED of Sh2-76EMM1 corresponds to that of a class I YSO. In the case of Sh2-76EMM2, only three data points from 2MASS was used and the error in the fitting is large. We cannot conclude on the class of the YSO/driving source Sh2-76EMM2. However, the 2MASS K -band and H -band magnitude were very similar, thus we speculate that the YSO could be a class II object. Figure 6. P(top) SED of Sh2-76EMM1 and (bottom) SED of Sh2-76EMM2. 4.2 A Plausible Probe for Binary/Multiplicity Along Same Line of Sight Line-of-sight effect on the observed properties of an object can be influenced strongly by the interception effect of another object. This could be in the form of strong absorption of the molecular line emission from the background source. With a reasonable angular resolution, the nature of molecular line emission could reveal the presence of more than one source within a region. The two driving sources of Sh2-76Eare located along the same line of sight with V LSR difference of 5kms 1 . Zinchenko etal. ( 1994 ) reported an unusual HCN emission spectrum with a missing main component, which they argued may have been caused by a foreground, 5kms 1 blue-shifted cloud. Zinchenko etal. ( 1997 ) also reported two core components based on their NH 3 (1,1) spectra, which showed additional component after a single Gaussian fitted component was subtracted. In the case of the HCN emission, it is imperative that only a very dense core could have completely absorbed the main component of the line emission. Self-absorption could have affected only the emissions around the systemic velocity of the central source, leaving a fraction of the emission to be detected. The NH 3 line observational results of Zinchenko etal. ( 1997 ) support the existence of a second component. We propose the Sh2-76EMM2 is responsible for the absorption of the HCN main component. MM2 is only 0.5arcsec from MM1 and will provided the