This contribution focuses on the study of 'cool' sources with surface temperatures in the range of about 500 − 4000 K. In this temperature range spectra are dominated by strong molecular absorption and the tools of modern chemical physics can be applied to compute the molecular opacities needed to simulate the observed spectral energy distributions. (See Bernath (2005) for an introduction to molecular spectroscopy including line intensities and Bernath (2009) The vibration-rotation and pure rotational lines of H2 O and OH appear strongly in cool oxygen-rich objects. The dominant carbon-containing molecule is CO at high temperatures and CH4 for cooler objects, such as T-type brown dwarfs and 'hot Jupiter' extrasolar planets. For nitrogen, N2 is the high temperature molecular form, but NH3 appears in T dwarfs and is predicted to be the distinguishing feature for very cool brown dwarfs ('Y'-type) with surface temperatures below about 700 K.Excellent high resolution ground-based spectra of the Sun are available from the Kitt Peak Fourier transform spectrometer (FTS) and from low earth orbit with the Advanced Composition Explorer (ACE) FTS. The spectra are dominated by the strong first overtone and fundamental vibration-rotation bands of CO. The Meinel bands (OH vibration-rotation bands) near 3 μm are also strong and the OH pure rotational lines are prominent at longer wavelengths. The vibration-rotation bands of CH and NH can be seen at 3 μm and pure rotational lines of NH are also present.A new very high signal-to-noise solar atlas in the 750 − 4400 cm −1 region has recently been prepared by Hase et al. (2009) from ACE satellite observations. Based on ACE, ATMOS and laboratory spectra, the analysis of OH has recently been improved by Bernath & Colin (2009) and similar work is underway for CH and NH.At 5800 K, the Sun's photosphere is too hot for water to exist, but by 3900 K the concentration of OH and H2 O are equal. A large number of unassigned lines were noticed in two Kitt Peak sunspot atlases; it was suspected that these lines were due to hot water but the available laboratory data were inadequate to confirm this. Comparison of a new laboratory emission spectrum of H 2 O at 1800 K with the sunspot absorption spectrum identified most of the unassigned sunspot lines as H2 O lines. Wallace et al. (1995) proved that there is 'water on the Sun'. Through variational calculations of the energy levels using a high quality ab initio potential energy surface, Polyansky et al. (1997) were able to assign most of the strong lines.The water emission in the 500-13 000 cm −1 spectral region was recorded with a high-resolution FTS using an oxy-acetylene torch as a source. Work on this 3000 K spectrum of H2 O has just finished with the publication by Zobov et al. (2008) of the last paper in the series. The latest water linelist of Barber et al. (2006) contains more than 500 million lines and is recommended for simulation of spectral energy distributions of cool stars, brown dwarfs and extrasolar planets.The situation for CH4 ...