over 6000 K is necessary.

The general ExoMol approach is molecule-by-molecule. That is, a comprehensive line list is created for a particular molecule which is then made available in the database. For more challenging larger systems such as NH$_3$, PH$_3$ and HNO$_3$, it has been our policy to produce initial, room-temperature line lists, see [@jt466; @jt556; @jt603] respectively. This allows us to improve the model, validate the available experimental data and, in some cases, make spectral assignments. In all instances, the subsequent hot line lists [@jt500; @jt592; @jt614] are both more complete and more accurate and should therefore be used even for studies at low temperatures.

Thus far ExoMol has not considered ultraviolet (UV) absorption; however, there is increasing interest in the consequences of UV radiation on exoplanets [@14FoBiLa; @14LoPaFr; @13BeBaxx] so this may need to be reviewed in future. As discussed in the comments below, molecules are still being added to the database so that coverage by species is steadily increasing.

Tables \[tab:exomoldata\] and \[tab:otherdata\] summarize the molecules for which the ExoMol database currently provides data. The division is between species that have explicitly been studied as part of the ExoMol project (Table \[tab:exomoldata\]) and those for which the 