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The infrared emission bands. III - Southern IRAS sources

The Astrophysical journal, 1989-06, Vol.341 (1), p.246-269

1989

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2-12.5 micron imaging of IRAS 21282+5050 : the structure of a young planetary nebula

The Astrophysical journal, 1993-07, Vol.411 (1), p.266-273

1993

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Spectral line profiles of nickel and argon in supernova 1987A - Expansion velocity and electron scattering effects

The Astrophysical journal, 1989-03, Vol.338 (1), p.L9-L12

1989

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Hydrocarbon emission features in the infrared spectra of warm supergiants

The Astrophysical journal, 1990-12, Vol.365 (1), p.L23-L26

1990

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Spectral imaging of the Orion Bar at 3.3, 8.4, and 11.3 microns: Comparison with a fluorescent polycyclic aromatic hydrocarbon model

The Astrophysical journal, 1994-03, Vol.423 (1), p.326

1994

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3.3 and 11.3 micron images of HD 44179 - Evidence for an optically thick polycyclic aromatic hydrocarbon disk

The Astrophysical journal, 1993-07, Vol.411 (2), p.794-796

1993

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Observations of NGC 7027 from 5.2 to 7.5 microns - The detection of Ni II and additional dust features

The Astrophysical journal, 1983-11, Vol.274 (2), p.666-670

1983

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The discovery of a new infrared emission feature at 1905 wavenumbers (5.25 microns) in the spectrum of BD +30 degrees 3639 and its relation to the polycyclic aromatic hydrocarbon model

The Astrophysical journal, 1989-10, Vol.345 (1), p.L59-L62

1989

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Spectral imaging of the 3.3 and 11.3 micron emission bands in NGC 1333 - Discovery of spatially separate band emissions

The Astrophysical journal, 1993-06, Vol.410 (2), p.668-672

1993

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Extended infrared emission around IRAS 21282 + 5050

The Astrophysical journal, 1992-09, Vol.396 (1, Se), p.120-123

1992

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3 micron spectrophotometry of Comet Halley - Evidence for water ice

The Astrophysical journal, 1988-11, Vol.334 (2), p.1044-1048

1988

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Infrared observations of SN 1987A from 5.3 to 12.6 microns - Evidence for an early dust echo

The Astrophysical journal, 1988-02, Vol.325 (1), p.L1-L4

1988

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The infrared emission bands. I - Correlation studies and the dependence on C/O ratio

The Astrophysical journal, 1986-03, Vol.302 (2), p.737-749

1986

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The discovery of a new infrared emission feature at 1905 wavenumbers (5.25 microns) in the spectrum of BD + 30 deg 3639 and its relation to the polycyclic aromatic hydrocarbon model

The Astrophysical journal, 1989-10, Vol.345, p.L59

1989

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The abundance of argon at the galactic center

The Astrophysical journal, 1981-09, Vol.248, p.524

1981

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Spectral and spatial resolution of the 12.8 micron NE II emission from the galactic center

The Astrophysical journal, 1976-04, Vol.205, p.L5

1976

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The discovery of a new infrared emission feature at 1905 wavenumbers (5.25 microns) in the spectrum of BD +30°3639 and its relation to the polycyclic aromatic hydrocarbon model

The Astrophysical journal, 1989, Vol.345 (1), p.L59-L62

1989

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Infrared Line Emission from Planetary Nebulae

The Astrophysical journal, 1971-01, Vol.164, p.L29

1971

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Hydrocarbon emission features in the IR spectra of warm supergiants

The Astrophysical journal, 1990-12, Vol.365, p.L23

1990

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Observations of Silicon Monoxide in Cool Stars at 4.05 Microns

The Astrophysical journal, 1973-09, Vol.184, p.L85

1973

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Identification of the 890 per CM carbonate signature in NGC 7027

The Astrophysical journal, 1975-02, Vol.195, p.L125

1975

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Observation of the nu-squared band of PH3 in the atmosphere of Saturn

The Astrophysical journal, 1975-11, Vol.202, p.L55

1975

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Spectral observations of Eta Carinae at 4 microns

The Astrophysical journal, 1977-10, Vol.217, p.103

1977

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Detection of 10.5-MICRON Line Emission from the Planetary Nebula NGC 7027

The Astrophysical journal, 1970-01, Vol.161, p.L185

1970

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NE II 12.8 micron emission from the galactic center. II

The Astrophysical journal, 1977-12, Vol.218, p.L103

1977

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The infrared emission bands. III - Southern IRAS sources

2-12.5 micron imaging of IRAS 21282+5050 : the structure of a young planetary nebula

Spectral line profiles of nickel and argon in supernova 1987A - Expansion velocity and electron scattering effects

Hydrocarbon emission features in the infrared spectra of warm supergiants

Spectral imaging of the Orion Bar at 3.3, 8.4, and 11.3 microns: Comparison with a fluorescent polycyclic aromatic hydrocarbon model

3.3 and 11.3 micron images of HD 44179 - Evidence for an optically thick polycyclic aromatic hydrocarbon disk

Observations of NGC 7027 from 5.2 to 7.5 microns - The detection of Ni II and additional dust features

The discovery of a new infrared emission feature at 1905 wavenumbers (5.25 microns) in the spectrum of BD +30 degrees 3639 and its relation to the polycyclic aromatic hydrocarbon model

Spectral imaging of the 3.3 and 11.3 micron emission bands in NGC 1333 - Discovery of spatially separate band emissions

Extended infrared emission around IRAS 21282 + 5050

3 micron spectrophotometry of Comet Halley - Evidence for water ice

Infrared observations of SN 1987A from 5.3 to 12.6 microns - Evidence for an early dust echo

The infrared emission bands. I - Correlation studies and the dependence on C/O ratio

The discovery of a new infrared emission feature at 1905 wavenumbers (5.25 microns) in the spectrum of BD + 30 deg 3639 and its relation to the polycyclic aromatic hydrocarbon model

The abundance of argon at the galactic center

Spectral and spatial resolution of the 12.8 micron NE II emission from the galactic center

The discovery of a new infrared emission feature at 1905 wavenumbers (5.25 microns) in the spectrum of BD +30°3639 and its relation to the polycyclic aromatic hydrocarbon model

Infrared Line Emission from Planetary Nebulae

Hydrocarbon emission features in the IR spectra of warm supergiants

Observations of Silicon Monoxide in Cool Stars at 4.05 Microns

Identification of the 890 per CM carbonate signature in NGC 7027

Observation of the nu-squared band of PH3 in the atmosphere of Saturn

Spectral observations of Eta Carinae at 4 microns

Detection of 10.5-MICRON Line Emission from the Planetary Nebula NGC 7027

NE II 12.8 micron emission from the galactic center. II

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