Astrophysical observations of cyanoacetylene have been enabled by numerous laboratory spectroscopy studies-thoroughly documented in HITRAN ) and the Cologne Database for Molecular Spectroscopy )-most of which have been conducted at room temperature , with non-equilibrium conditions sometimes achieved by means of electrical discharge for assignment of vibrational excited states . With the spectroscopic capabilities now available through the James Webb Space Telescope (JWST), and in the near future SPHEREx, attention has turned toward detection of biosignatures (including cyanoacetylene) in exoplanetary atmospheres across regions of the mid-and near-infrared, increasing the demand for extended spectroscopic line lists. Rimmer et al. constructed an extensive cyanoacetylene line list to demonstrate the potential use of JWST for detection of this species in the atmosphere around the exoplanet 1132b . While it was not considered in their model, the first overtone of the C -H stretching vibration (2ν 1 ) lies near 1.5 µm, making it a potential target for transmission spectroscopy in the near-infrared. The goal of the present work is to provide laboratory spectroscopy data for cyanoacetylene in the near-infrared region-where data is sparse-that could be used in future JWST observations. Cyanoacetylene spectroscopy is complicated by the low-lying bending mode (ν 7 ) and several combination bands that all lie below 450 cm -1 . Their thermal population at room temperature adds complexity to the spectra as we move into the nearinfrared-a problem that is mitigated in the laboratory by measuring spectra at low temperature. Beyond the goal of simplifying the spectroscopy, we aim to produce thermalized, low-temperature cyanoacetylene for future measurements of collisional cross sections and kinetics and therefore have implemented buffer-gas (sympathetic/collisional) cooling into our spectroscopy instrument.