Synthetic spectra for the Arizona Airglow Experiment

Johnston, J. E.; Hatfield, D. B.; Broadfoot, A. L.

doi:10.1117/12.187559

Cited by 3 publications

(2 citation statements)

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“…They are the (3-2) and (4-3) bands of the Au = H-1 sequence, in the wavelength ranges XX7043-7086 and XX7141-7185, and probably also the (5-4) band in the range XX7240-7280. The identifications of the (3-2) and (4-3) bands are confirmed by their close agreement with a synthetic spectrum of 0 2 in this region kindly calculated for us by Dr. D. B. Hatfield, using an assumed rotational temperature T=300 K (Johnstone et al 1994). These two bands are marked on Fig.…”

Section: 2 Bandssupporting

confidence: 76%

Night-Sky High-Resolution Spectral Atlas of OH and O2 Emission Lines for Echelle Spectrograph Wavelength Calibration

Osterbrock¹,

Fulbright²,

Martel³

et al. 1996

PASP

322

262

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The potential of night-sky emission lines recorded on every long-exposure astronomical spectrum, for wavelength calibration, is emphasized. A high-resolution atlas, based on spectra obtained with the Keck 10-m telescope on Mauna Kea and the high-resolution echelle spectrograph (HIRES) is presented. This atlas shows OH, 0 2 , and a few other night-sky lines, and will make it possible to identify them easily on high-resolution spectra. Accurate wavelengths and references to their sources are given. Date UT Orders AA Exp. a (1950) S (1950) Zen. Dist. (°) Azimuth (°) left right

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Section: 2 Bandssupporting

confidence: 76%

Night-Sky High-Resolution Spectral Atlas of OH and O2 Emission Lines for Echelle Spectrograph Wavelength Calibration

Osterbrock¹,

Fulbright²,

Martel³

et al. 1996

PASP

322

262

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“…The techniques for generating synthetic spectra are well known. The approach used in our laboratory has been described in the literature [Johnston, et al, 1994]. The atmospheric temperature estimated by the MSIS model, 1200 K, was used for both the vibrational and rotational energy distributions in the N2 ground state.…”

Section: The Case a Synthetic Spectrummentioning

confidence: 99%

The N₂ + O⁺ charge‐exchange reaction and the dayglow N₂⁺ emission

Broadfoot¹,

Stone²

1999

J. Geophys. Res.

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Abstract. Dayglow spectra were recorded by the Arizona Airglow Experiment from the payload bay of the shuttle, STS-74. These spectra are used to reexamine the role of the prominent N2 + first negative emission from the dayglow thermosphere. Many reports of the N2 + emissions identify problems in validating the intensity of the emission. Also, an extended vibrational and rotational structure of the bands remains unexplained in the historical analysis. These anomalies appear to be due to the charge-exchange reaction, N2+O+(2D,2p)-• N2++O, which is the dominant source of N2 + ions in the sunlit atmosphere at high altitudes. In the present work the N2 + emission was considered to originate from two separate ion sources. First are those emissions originating from ions produced by photoionizaton and electron bombardment; these emissions can be modeled. Second are the emissions originating from ions produced by the charge-exchange reaction; these emissions cannot be modeled. Synthetic emission profiles due to the first ion source were modeled and subtracted from the observed spectrum, leaving emission profiles resulting from the charge-exchange ion source. These residual vibrational and rotational profiles were analyzed to retrieve resonance scattering rates for these ions. These scattering rates can be used to estimate the N2 + first negative emission rate expected from the thermosphere with a model of the

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