TY - JOUR
T1 - Variations in the 3 micron spectrum across the orion bar
T2 - Polycyclic aromatic hydrocarbons and related molecules
AU - Sloan, G. C.
AU - Bregman, J. D.
AU - Geballe, T. R.
AU - Allamandola, L. J.
AU - Woodward, Charles E.
PY - 1997
Y1 - 1997
N2 - Long-slit spectra across the Orion Bar reveal significant differences in the spatial behavior of the components of the 3 μm polycyclic aromatic hydrocarbon (PAH) spectrum. The strong PAH band at 3.29 μm generally decreases exponentially with distance from the ionization front into the molecular cloud (scale height ∼12″), although excesses appear ∼10″ and ∼20″ behind the ionization front, close to layers of H2 and CO emission, respectively. The 3.40 μm PAH feature separates into two components with very different spatial distributions. The main component (at 3.395 μm), along with the 3.51 μm band and the PAH plateau (3.3-3.6 μm), shows excess emission ∼10″ and ∼20″ behind the ionization front, stronger than the excesses in the 3.29 μm band. The extra component of the 3.40 μm band, which peaks at ∼ 3.405 μm, has a spatial distribution very similar to the H2 emission. Aromatic C - H stretches in PAHs most likely produce the 3.29 μm 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 μm.
AB - Long-slit spectra across the Orion Bar reveal significant differences in the spatial behavior of the components of the 3 μm polycyclic aromatic hydrocarbon (PAH) spectrum. The strong PAH band at 3.29 μm generally decreases exponentially with distance from the ionization front into the molecular cloud (scale height ∼12″), although excesses appear ∼10″ and ∼20″ behind the ionization front, close to layers of H2 and CO emission, respectively. The 3.40 μm PAH feature separates into two components with very different spatial distributions. The main component (at 3.395 μm), along with the 3.51 μm band and the PAH plateau (3.3-3.6 μm), shows excess emission ∼10″ and ∼20″ behind the ionization front, stronger than the excesses in the 3.29 μm band. The extra component of the 3.40 μm band, which peaks at ∼ 3.405 μm, has a spatial distribution very similar to the H2 emission. Aromatic C - H stretches in PAHs most likely produce the 3.29 μm 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 μm.
KW - Dust, extinction
KW - ISM: individual (Orion Bar)
KW - ISM: molecules
KW - Infrared: ISM: lines and bands
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U2 - 10.1086/303484
DO - 10.1086/303484
M3 - Article
C2 - 11539404
AN - SCOPUS:0031561491
SN - 0004-637X
VL - 474
SP - 735
EP - 740
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 2 PART I
ER -