Variations in the 3 micron spectrum across the Orion Bar:  polycyclic aromatic hydrocarbons and related molecules.
Long-slit spectra across the Orion Bar reveal significant differences in the spatial behavior of the components of the 3 microns polycyclic aromatic hydrocarbon (PAH) spectrum. The strong PAH band at 3.29 microns generally decreases exponentially with distance from the ionization front into the molecular cloud (scale height approximately 12"), although excesses appear approximately 10" and 20" behind the ionization front, close to layers of H2 and CO emission, respectively. The 3.40 microns PAH feature separates into two components with very different spatial distributions. The main component (at 3.395 microns), along with the 3.51 microns band and the PAH plateau (3.3-3.6 microns), shows excess emission approximately 10" and approximately 20" behind the ionization front, stronger than the excesses in the 3.29 microns band. The extra component of the 3.40 microns band, which peaks at approximately 3.405 microns, has a spatial distribution very similar to the H2 emission. Aromatic C-H stretches in PAHs most likely produce the 3.29 microns feature. Aliphatic C-H stretches in either attached methyl side-groups or superhydrogenated PAHs, or perhaps both, could produce the complicated spectral and spatial structure at 3.40 microns.
Sloan
G C
GC
NASA Ames Research Center, Moffett Field, CA 94035-1000, USA.  sloan@ssa1.arc.nasa.gov
Bregman
J D
JD
Geballe
T R
TR
Allamandola
L J
LJ
Woodward
C E
CE
D001256:Astronomy / Q000295:instrumentation / Q000379:methods*; D005118:Extraterrestrial Environment; D006859:Hydrogen; D011084:Polycyclic Aromatic Hydrocarbons; D013055:Spectrophotometry, Infrared / Q000379:methods
D011084:Polycyclic Aromatic Hydrocarbons; D006859:Hydrogen