In this report, a wide range of spectroscopic studies was undertaken on the astrophysical significant deuterated methanol $(\mathit{C}\mathit{D}{3}_{\mathit{O}}\mathit{D})$ species. In the submillimeter wave$(SMMW)$ wave a large number of very accurate spectral line positions in the useful range of $130-750\mathit{G}\mathit{H}\mathit{z}$ have been reported. The actual spectral recording of the spectrum in the range $325-344\mathit{G}\mathit{H}\mathit{z}$ with a high signal to noise ratio $(\mathit{S}/\mathit{N})$ have been presented. These will serve the radio astronomers a laboratory back-up to detect this species in interstellar space which will help to determine the deuterium/Hydrogen (D/H) ratio to understand the evolution of chemistry and the formation process of large molecules in space. At the low temperature of interstellar space, the quantum tunneling effect can be better understood by the deuterium fragmentation process. The study is extended in the far-infrared $(\mathit{F}\mathit{I}\mathit{R})$ region by high-resolution Fourier transform measurements. The spectral lines originating in the first excited state and those terminating in the first excited states have been assigned. About $2500$ lines have been identified and atlas of the assigned lines along with previously not repotted, lines have been reported. The Hamiltonian model used has been clearly explained in terms of rotation and torsional-rotational molecular motion. All the $\mathit{S}\mathit{M}\mathit{M}\mathit{W}$ $(\mathit{a}\mathit{c}\mathit{c}\mathit{u}\mathit{r}\mathit{a}\mathit{c}\mathit{y}\pm 100\mathit{k}\mathit{H}\mathit{z})$ lines along with the FIR lines (accuracy $\pm 0.0004{\mathit{cm}}^{-1}$) have been fitted with the model and the parameters determined. The molecular parameters reproduce the measured transition wavenumbers approximately within the experimental uncertainty. It should be noted the exact term values for the connected ground state levels are included in an Appendix-1, for economy this is submitted as a depository. In the infrared $(IR)$ region a number of vibrational bands have been recorded but the presence of water vapour hindered the analysis work. However, with the knowledge of the molecular parameters and low-resolution knowledge about 10 different $C{O}_2$ lasers pumped FIR laser system have been assigned and a number of FIR lines have been predicted.

在本报告中，对天体物理上重要的氘代甲醇进行了广泛的光谱研究 $（\mathit{C}\mathit{d}{3}_{\mathit{Ø}}\mathit{d}）$物种。在亚毫米波中$（\mathrm{小号}\mathrm{中号}\mathrm{中号}\mathrm{w\; ^}）$ 在有用范围内波动大量非常精确的光谱线位置 $130--750\mathit{G}\mathit{H}\mathit{ž}$已经报道。范围内光谱的实际光谱记录$325--344\mathit{G}\mathit{H}\mathit{ž}$ 信噪比高 $（\mathit{小号}/\mathit{ñ}）$已经提出。这些将为射电天文学家提供实验室支持，以检测星际空间中的该物种，这将有助于确定氘/氢（D / H）比率，以了解化学的演变以及太空中大分子的形成过程。在星际空间的低温下，氘碎裂过程可以更好地理解量子隧穿效应。该研究在远红外领域进行了扩展$（\mathit{F}\mathit{一世}\mathit{[R}）$通过高分辨率傅立叶变换测量区域。已经分配了起源于第一激发态和终止于第一激发态的谱线。关于$2500$已确定行，并且已报告已分配行的地图集以及以前未报告的行。旋转和扭转-旋转分子运动方面已经清楚地解释了所使用的哈密顿模型。所有的$\mathit{小号}\mathit{中号}\mathit{中号}\mathit{w\; ^}$ $（\mathit{一种}\mathit{C}\mathit{C}\mathit{ü}\mathit{[R}\mathit{一种}\mathit{C}\mathit{ÿ}\pm 100\mathit{ķ}\mathit{H}\mathit{ž}）$ 线和FIR线（精度 $\pm 0.0004{\mathit{厘米}}^{--\mathrm{1个}}$）已拟合模型并确定了参数。分子参数大致在实验不确定性范围内再现了测得的跃迁波数。应该注意的是，附录1中包含了所连接的基态水平的确切术语值，为节省起见，它是作为保管人提交的。在红外$（\mathrm{一世}\mathrm{[R}）$在该区域记录了许多振动带，但是水蒸气的存在阻碍了分析工作。但是，有了分子参数知识和低分辨率知识，大约有10种不同$C{Ø}_{\mathrm{2个}}$ 已分配了抽运FIR激光系统的激光器，并已预测了许多FIR线。