Context. Deep spectral-line surveys in the mm and sub-mm range can detect thousands of
lines per band uncovering the rich chemistry of molecular clouds, star forming regions and
circumstellar envelopes, among others objects. The ability to study the faintest features of
spectroscopic observation is, nevertheless, limited by a number of factors. The most
important are the source complexity (line density), limited spectral resolution and insufficient
sideband (image) rejection (SRR). Dual sideband (2SB) millimeter receivers separate upper …

Context. Deep spectral-line surveys in the mm and sub-mm range can detect thousands of
lines per band uncovering the rich chemistry of molecular clouds, star forming regions and
circumstellar envelopes, among others objects. The ability to study the faintest features of
spectroscopic observation is, nevertheless, limited by a number of factors. The most
important are the source complexity (line density), limited spectral resolution and insufficient
sideband (image) rejection (SRR). Dual sideband (2SB) millimeter receivers separate upper …