Abstract: Using the IRAM (Institut de Radioastronomie Millimétrique) 30 m for a molecular line imaging survey at 1.3–4.0 mm, in conjuntion with archival dust contiunuum images spanning 70−870 μm, and \rmNH_3(J, K) = (1, 1) and (2, 2) images from GBT (Green Bank Telescope), a pair of neighboring clumps within the tail of filamentary molecular cloud G 011.0970–0.1093 is studied. While both clumps coincide spatially with the dust continuum emission peak at 870 μm, they exhibit contrasting brightnesses at 70 μm. Comparative analysis of these two clumps reveals: (1) The gas and dust temperatures are tightly coupled within this extremely young high-mass star-forming region. (2) Gas-dust temperatures of the 70 μm bright clump decrease from the center ( \sim17 K) to the envelope edge, suggesting the initiation of protostellar activities within the clump; conversely, the central region of the 70 μm dark cloud clump is colder ( \sim11 K) and denser ( \sim5\times10^22\, \rmcm^-2 ) compared to its periphery, with a strong anti-correlation between the \rmH_2 column density and dust temperature pixel by pixel, indicating dominant external heating shaping the temperature profile of this clump. (3) A strong positive correlation exists between the gaseous \rmC^18\rmO depletion (f_\rmD(\rmC^18\rmO)) and the deuterium fraction of \rmHCO^+ at pc scales, with f_\rmD(\rmC^18\rmO) reaching up to 7 in the cold and dense \rmDCO^+ dominated region. (4) With gas-dust temperatures ranging from 10 K to 20 K and \rmH_2 column densities ranging from 10^22\,\rmcm^-2 to 10^23\,\rmcm^-2, \rmHCO^+, \rmN_2\rmH^+, and \rmHNC exhibit significant deuteration enhancements towards the colder and denser clump, while \rmHCN shows greater deuteration enhancement in slightly warmer and 70 μm brighter clumps, and \rmNH_3 deuteration shows no significant change. These deuteration differentiation among species are likely related to their gas-dust forming pathways.