We present the results of ISO SWS and LWS grating scans towards the three b
rightest members of the BD+40 degrees 4124 group in the infrared: BD+40 deg
rees 4124 (B2Ve), LkH alpha 224 (A7e) and the embedded source LkH alpha 225
. Emission from the pure rotational lines of H-2. from re-vibrational trans
itions of CO. from PAHs. from H I recombination lines and from the infrared
line structure lines of [Fe II], [Si II], [S I], [O I], [O III] and [C III
was detected. These emission lines arise in the combination of a low-densi
ty (approximate to 10(2) cm(-3)) H II region with a clumpy PDR in the case
of BD+40 degrees 4124. The lower transitions of the infrared H I lines obse
rved in BD+40 degrees 4124 are optically thick: most likely they arise in e
ither a dense wind or a circumstellar disk. This same region is also respon
sible for the optical H1 lines and the radio continuum emission. In the lin
es of sight towards LkH alpha 224 and LkH alpha 225, the observed emission
lines arise in a non-dissociative shock produced by a slow (approximate to
20 km s(-1)) outflow arising from LkHa 225. Toward LkH alpha 225 WE also ob
serve a dissociative shock, presumably located closer to the outflow source
than the non-dissociative shock. Tn the line of sight towards LkH alpha 22
5 we observed absorption features due to solid water ice and amorphous sili
cates, and due to gas-phase H2O, CO and CO2. No solid CO2 was detected towa
rds LkH alpha 225. making this the first line of sight where the bulk of th
e CO2 is in the gas-phase.