Spatial structure in the 10 micron spectrum of HD 44179 (the Red Rectangle)

Grasdalen, G. L.; Sloan, G. C.; LeVan, Paul D.

doi:10.1086/186254

Cited by 2 publications

(1 citation statement)

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“…In contrast, the X‐shaped biconical nebula, which is of principal interest in this work, extends over 1 arcmin (Cohen et al 1975) and contains carbon‐rich material. These unusual characteristics have led to many studies of the morphology, nature and evolution of the star and its associated circumstellar and nebular material (Grasdalen, Sloan & LeVan 1992; Sloan, Grasdalen & LeVan 1993; Bregman et al 1993; Lopez, Mékarnia & Lefèvre 1995; Roddier et al 1995; Jura, Balm & Kahane 1995; Cruzalèbes et al 1996; Hora et al 1996; Jura, Turner & Balm 1997; Lopez et al 1997). The nebula is unique in that strong UIR, ERE and unidentified optical emission bands are all observed in one object.…”

Section: The Red Rectangle Nebula and The Central Star Hd 44179mentioning

confidence: 99%

Observations of the 3.3- m UIR band in the Red Rectangle: relation to unidentified optical emission

Kerr

Hurst

Miles

et al. 1999

Monthly Notices of the Royal Astronomical Society

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A B S T R A C TThe biconical Red Rectangle nebula exhibits very strong unidenti®ed infrared (UIR) emission bands, a subset of the optical diffuse interstellar bands (in emission) and extended red emission (ERE). A key question is the extent to which the carriers of these spectroscopic signatures may be related. In a new study of the 3.3-mm emission, CGS 4 spectra were recorded at UKIRT, which give information on the spatial distribution of the 3.3-mm carrier in the nebula and on the width, peak wavelength and pro®le of the feature as a function of offset from the central star, HD 44179. Both Type 1 (l 0 , 3:289 mm, full width at half-maximum FWHM , 0.042 mm) and Type 2 (l 0 , 3:296 mm, FWHM , 0.020 mm) 3.3-mm features, as de®ned by Tokunaga et al., are found within the nebula. Type 2 is seen predominantly towards the central star, at the bicone interfaces and east and west of the star in the nebula. The broader Type 1 feature appears in the nebula 5 arcsec south of the central star, whereas the 3.3mm band at 5 arcsec north appears to be a blend of Type 1 and Type 2. We ®nd that there is no signi®cant correlation between the intensity of the 3.3-mm feature and that of either the unidenti®ed optical (diffuse) emission bands or ERE. This result suggests that there is at most an indirect link between the carrier(s) of the 3.3-mm band and this subset of diffuse bands. Such a link could arise, for example, if these diffuse band carriers were formed by chemical erosion or photodissociation of polycyclic aromatic hydrocarbon material.q 1999 RAS, MNRAS 303, 446±454 Figure 6. The 3.3-mm spectra along the north-east and south-west interfaces out to approximately 6 arcsec, with the spectra towards HD 44179 for comparison. The spectra in (b) (right column) are normalized to a common peak intensity in order to allow comparison of the band pro®les.

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