Vibration-rotation transition probabilities in CH+ and CD+

Folomeg, B.; Rosmus, P.; Werner, Hans‐Joachim

doi:10.1016/0009-2614(87)80518-3

Cited by 22 publications

(11 citation statements)

References 10 publications

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“…This is in contrast to the CH emission, indicating that CH + and CH may largely exist in different regions of the medium. Since CH + has a large dipole moment predicted by ab initio theory to be near 1.7 D (Ornellas & Machado 1986;Follmeg et al 1987;Sun & Freed 1988), the Einstein coefficient for the J ¼ 6 ! 5 rotational transition is A % 2 s À1 .…”

Section: Molecular Linesmentioning

confidence: 98%

Atomic and Molecular Emission Lines from the Red Rectangle

Hobbs

Thorburn

Oka

et al. 2004

ApJ

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HD 44179 is the binary, post-asymptotic giant branch, central star of the Red Rectangle Nebula. Echelle spectra of the star have been obtained over a wavelength range from about 3800 to 10000 8 at a resolving power R ¼ 38; 000. A maximum S/ N of 850 was achieved near 6800 8. Fifty-seven identified atomic or ionic emission lines of 12 elements are detected in the star's spectrum, along with 76 emission lines of CH, CH + , or CN. Three other CN lines are also present in absorption. Fewer than 30 of these 136 lines apparently have been previously reported, and the newly detected species include N ii, Mg i, S ii, K i, Fe i, Fe ii, Rb i, Ba ii, CH, and CN. On the basis of their shapes and widths, the line profiles of the various species can be classified into three groups: narrow, broad, or double-peaked. The emission apparently originates in an unusual, compact H ii region and in associated neutral gas, both concentrated primarily within the small, dusty torus that optically obscures the central star. The detection of the Ba ii emission from the gas may support the hypothesis of Waelkens et al. that HD 44179 is destined to become a barium star.

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Section: Molecular Linesmentioning

confidence: 98%

Atomic and Molecular Emission Lines from the Red Rectangle

Hobbs

Thorburn

Oka

et al. 2004

ApJ

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“…We have adopted the electric dipole moment µ CH + = 1.68 Debye (Cheng et al 2007) and note that a nearly identical value µ13 CH + = 1.7 Debye was reported for the heavier isotopologue (Follmeg et al 1987). For the sulfanylium ion we have adopted the same value µ SH + = 1.28 Debye for both isotopologues (Senekowitsch et al 1985;Cheng et al 2007).…”

Section: Laboratory Spectroscopic Datamentioning

confidence: 99%

Detection of CH⁺, SH⁺, and their ¹³C- and ³⁴S-isotopologues toward PKS 1830−211

Müller

Black

et al. 2017

A&A

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The z = 0.89 molecular absorber toward PKS 1830−211 provides us with the opportunity to probe the chemical and physical properties of the interstellar medium in the disk of a galaxy at a look-back time of half the present age of the Universe. Recent ALMA observations of hydrides have unveiled the multi-phase composition of this source's interstellar medium along two absorbing sightlines. Here, we report ALMA observations of CH + and SH + , and of their 13 C-and 34 S-isotopologues, as potential tracers of energetic processes in the interstellar medium. CH + and 13 CH + are detected toward both images of PKS 1830−211, CH + showing the deepest and broadest absorption among all species observed so far. The [CH + ]/[ 13 CH + ] abundance ratio is ∼100 in the southwest line of sight. This value is larger than any previous [ 12 CX]/[ 13 CX] ratios determined from other species toward this source and suggests either that the latter might be affected by fractionation or that CH + might be tracing a different gas component. Toward the northeast image, we find an even larger value of [CH + ]/[ 13 CH + ], 146 ± 43, although with a large uncertainty. This sightline intercepts the absorber at a larger galactocentric radius than the southwestern one, where material might be less processed in stellar nucleosynthesis. In contrast to CH + and its 13 C isotopologue, SH + and 34 SH + are only detected on the southwest sightline. These are the first detections of extragalactic SH + and interstellar 34 SH +. The spectroscopic parameters of SH + are reevaluated and improved rest frequencies of 34 SH + are obtained. The [CH + ]/[SH + ] column density ratios show a large difference between the two lines of sight: ∼25 and >600 toward the SW and NE image, respectively. We are not able to shed light on the formation process of CH + and SH + with these data, but the differences between the two sightlines toward PKS 1830−211 suggest that their absorptions arise from gas with a molecular fraction of 10%, with SH + tracing significantly higher molecular fractions than CH + .

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“…[13][14][15]. The theoretical efforts have been more extensive and have dealt with various quantum mechanical properties including potential energy curves and spectroscopic constants for the lower states, photodissociation cross sections, Franck-Condon factors, polarizabilities and radiative association rate [16][17][18][19][20][21][22][23][24][25][26][27][28]. On the other hand, CH + has been thoroughly studied astrophysically.…”

Section: Introductionmentioning

confidence: 98%