The microwave spectrum of SO+

Amano, Tatsuya; Warner, H. E.

doi:10.1016/0022-2852(91)90023-4

Cited by 19 publications

(10 citation statements)

References 15 publications

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“…For the convenience to compare with the fitting results from Ref. [18], the effective spin-rotation coupling constant c eff was chosen to be fitted by assuming A D to be equal to zero. Ten parameters, namely A 1 , B 0 , B 1 , D 0 , D 1 , p 0 , p 1 , c eff0 , c eff1 and v 0 , were floated in our fit.…”

Section: Results and Analysismentioning

confidence: 99%

“…[18] was carried out using Pickett's program SPFIT [24]. A standard effective Hamiltonian for 2 P states derived by Brown et al [25] was adopted.…”

Section: Results and Analysismentioning

confidence: 99%

“…The A 2 P i À X 2 P r system of SO + have also been observed in rotationally cold supersonic expansion and the most complete molecular constants for the X 2 P r and A 2 P i states have been obtained [16,17]. In 1991, Amano et al reported the microwave spectrum of SO + and determined more precise molecular constants for the ground state [18]. No infrared spectrum has been reported.…”

Section: Introductionmentioning

confidence: 93%

“…Rovibrational transitions for both X = 1/2 and 3/2 subbands have been recorded. Our observed transitions were analyzed together with the microwave data reported by Amano et al [18].…”

Section: Introductionmentioning

confidence: 94%

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Mid-infrared diode laser spectroscopy of SO+

Zheng

Duan

2008

Journal of Molecular Spectroscopy

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Section: Results and Analysismentioning

confidence: 99%

“…[18] was carried out using Pickett's program SPFIT [24]. A standard effective Hamiltonian for 2 P states derived by Brown et al [25] was adopted.…”

Section: Results and Analysismentioning

confidence: 99%

Section: Introductionmentioning

confidence: 93%

“…Rovibrational transitions for both X = 1/2 and 3/2 subbands have been recorded. Our observed transitions were analyzed together with the microwave data reported by Amano et al [18].…”

Section: Introductionmentioning

confidence: 94%

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Mid-infrared diode laser spectroscopy of SO+

Zheng

Duan

2008

Journal of Molecular Spectroscopy

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“…The energy levels of a 2 Π-molecule exhibit the additional splittings due to the electron spin and orbital angular momentum interactions (Ω-and Λ-doublets). The rotational levels are defined with three quantum numbers, Ω, J, l, which represent the absolute value of the projection of the total electronic angular momentum on the molecular axis, the total angular momentum from rotation and electronic motion, and the parity, respectively (Amano et al 1991).…”

Section: Somentioning

confidence: 99%

Molecular ions in the O-rich evolved star OH231.8+4.2: HCO⁺, H¹³CO⁺and first detection of SO⁺, N₂H⁺, and H₃O⁺

Contreras

Velilla-Prieto

Agúndez

et al. 2015

A&A

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ABSTRACT+ transitions observed are consistent with this ion arising from denser, inner (and presumably warmer) layers of the fossil remnant of the slow AGB CSE at the core of the nebula. From rotational diagram analysis, we deduce excitation temperatures of T ex ∼ 10−20 K for all ions except for H 3 O + , which is most consistent with T ex ≈ 100 K. Although uncertain, the higher excitation temperature suspected for H 3 O + is similar to that recently found for H 2 O and a few other molecules, which selectively trace a previously unidentified, warm nebular component. The column densities of the molecular ions reported here are in the range N tot ≈ [1−8] × 10 13 cm −2 , leading to beam-averaged fractional abundances relative to H 2 of X(HCO + ) ≈ 10 −8 , X(H 13 CO + ) ≈ 2 × 10 −9 , X(SO + ) ≈ 4 × 10 −9 , X(N 2 H + ) ≈ 2 × 10 −9 , and X(H 3 O + ) ≈ 7 × 10 −9 cm −2 . We have performed chemical kinetics models to investigate the formation of these ions in OH 231.8 as the result of standard gas phase reactions initiated by cosmic-ray and UV-photon ionization. The model predicts that HCO + , SO + , and H 3 O + can form with abundances comparable to the observed average values in the external layers of the slow central core (at ∼[3−8] × 10 16 cm); H 3 O + would also form quite abundantly in regions closer to the center (X(H 3 O + ) ∼ 10 −9 at ∼10 16 cm). For N 2 H + , the model abundance is lower than the observed value by more than two orders of magnitude. The model fails to reproduce the abundance enrichment of HCO + , SO + , and N 2 H + in the lobes, which is directly inferred from the broad emission profiles of these ions. Also, in disagreement with the narrow H 3 O + spectra, the model predicts that this ion should form in relatively large, detectable amounts (≈10 −9 ) in the external layers of the slow central core and in the high-velocity lobes. Some of the model-data discrepancies are reduced, but not suppressed, by lowering the water content and enhancing the elemental nitrogen abundance in the envelope. The remarkable chemistry of OH 231.8 probably reflects the molecular regeneration process within its envelope after the passage of fast shocks that accelerated and dissociated molecules in the AGB wind ∼800 yr ago.

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Millimeter and Submillimeter Wave Spectroscopy and Astrophysical Applications

Ziurys

2011

Handbook of High‐resolution Spectroscopy

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Millimeter and submillimeter spectroscopy has played a crucial role in the discovery and study of interstellar molecules by radio astronomy, as well as in the characterization of the rotational energy levels for numerous chemical compounds. A broad range of spectrometer designs have been developed for this basic direct absorption technique. Certain systems employ “free space” cells and Gaussian beam optics, while others incorporate mirrors in multipass configurations. Fast scanning methods have additionally been implemented. Synthetic techniques are also important in the astrophysical application of millimeter/submillimeter spectroscopy, as many potential interstellar species are free radicals and molecular ions. Many instruments employ glow discharges, ovens, and other exotic gas‐phase methods for the creation of transient molecules. Radical spectra usually exhibit a range of fine structure and hyperfine interactions which can complicate their analysis. Another challenge for millimeter/submillimeter spectroscopy is the study of simple organic molecules with functional groups that undergo hindered rotation. Millimeter and submillimeter spectroscopic measurements continue to provide the necessary rotational “rest frequencies” for molecule identification in space. Recent work has led to the interstellar discoveries of long‐chain carbon anions C 4 H − and C 6 H − , more complex organic molecules including CH 3 CONH 2 , and unusual refractory species such as CCP and AlO.

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The microwave spectrum of SO+

Cited by 19 publications

References 15 publications

Mid-infrared diode laser spectroscopy of SO+

Mid-infrared diode laser spectroscopy of SO+

Molecular ions in the O-rich evolved star OH231.8+4.2: HCO⁺, H¹³CO⁺and first detection of SO⁺, N₂H⁺, and H₃O⁺

Millimeter and Submillimeter Wave Spectroscopy and Astrophysical Applications

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The microwave spectrum of SO+

Cited by 19 publications

References 15 publications

Mid-infrared diode laser spectroscopy of SO+

Mid-infrared diode laser spectroscopy of SO+

Molecular ions in the O-rich evolved star OH231.8+4.2: HCO+, H13CO+and first detection of SO+, N2H+, and H3O+

Millimeter and Submillimeter Wave Spectroscopy and Astrophysical Applications

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Molecular ions in the O-rich evolved star OH231.8+4.2: HCO⁺, H¹³CO⁺and first detection of SO⁺, N₂H⁺, and H₃O⁺