First Detection of
 13
 CH
 +
 (
 J
  = 1-0)

Falgarone, É.; Phillips, T. G.; Pearson, John C.

doi:10.1086/499047

Cited by 31 publications

(27 citation statements)

References 34 publications

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“…Velocities obtained by the empirical model agree well with the velocities where deep HCO + (1-0) (Keene et al 1999;Godard et al 2010), p-H 2 O and HF (Neufeld et al 2010) and HI Fish et al (2003) absorptions are detected. It is remarkable that one of the strongest OH + absorption features at V LSR ∼ 7 km s −1 coincides with a strong dip in the HI profile that has no counterpart in CO emission Falgarone et al (2005). Overall, the velocities of the OH + and H 2 O + velocity components agree well.…”

Section: Resultsmentioning

confidence: 67%

“…The molecular cloud surrounding the star-forming complex shows evidence of continuing accretion onto the embedded stars (Keto & Wood 2006;Sollins & Ho 2005). As discussed by Neufeld et al (2010), line absorption by foreground gas has been detected from [OI] (Keene et al 1999), 13 CH + (Falgarone et al 2005), HCO + , HCN, HNC, CN (Godard et al 2010), and atomic hydrogen (Fish et al 2003). While the gas associated directly with G10.6−0.4 is detected in the velocity range −5 to +5 km s −1 , the A&A 518, L110 (2010) foreground gas along the line of sight is confined to the velocity interval from ∼5 to 45 km s −1 .…”

Section: Introductionmentioning

confidence: 97%

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Interstellar OH⁺, H₂O⁺and H₃O⁺along the sight-line to G10.6–0.4

Gérin¹,

Luca²,

Black

et al. 2010

A&A

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159

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We report the detection of absorption lines by the reactive ions OH + , H 2 O + and H 3 O + along the line of sight to the submillimeter continuum source G10.6−0.4 (W31C). We used the Herschel HIFI instrument in dual beam switch mode to observe the ground state rotational transitions of OH + at 971 GHz, H 2 O + at 1115 and 607 GHz, and H 3 O + at 984 GHz. The resultant spectra show deep absorption over a broad velocity range that originates in the interstellar matter along the line of sight to G10.6−0.4 as well as in the molecular gas directly associated with that source. The OH + spectrum reaches saturation over most velocities corresponding to the foreground gas, while the opacity of the H 2 O + lines remains lower than 1 in the same velocity range, and the H 3 O + line shows only weak absorption. For LSR velocities between 7 and 50 km s −1 we estimate total column densities of N(OH + ) ≥ 2.5 × 10 14 cm −2 , N(H 2 O + ) ∼6 × 10 13 cm −2 and N(H 3 O + ) ∼4.0 × 10 13 cm −2 . These detections confirm the role of O + and OH + in initiating the oxygen chemistry in diffuse molecular gas and strengthen our understanding of the gas phase production of water. The high ratio of the OH + by the H 2 O + column density implies that these species predominantly trace low-density gas with a small fraction of hydrogen in molecular form.

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Section: Resultsmentioning

confidence: 67%

Section: Introductionmentioning

confidence: 97%

Interstellar OH⁺, H₂O⁺and H₃O⁺along the sight-line to G10.6–0.4

Gérin¹,

Luca²,

Black

et al. 2010

A&A

Self Cite

159

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“…The lowest rotational transitions in the submillimeter and far-infrared band are blocked from the earth's atmosphere and therefore difficult to observe with ground-based telescopes. A tentative detection of the J = 1 → 0 transition of the isotope 13 CH + has been reported recently by Falgarone et al (2005). Cernicharo et al (1997) reported the first emission lines of the J = 2 → 1, 3 → 2 and 4 → 3 rotational transitions detected with the Infrared Space Observatory.…”

Section: Introductionmentioning

confidence: 85%

Rotational excitation of methylidynium (CH⁺) by a helium atom at high temperature

Hammami

Owono

Stäuber

2009

A&A

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Context. The Herschel Space Observatory with its high-resolution instrument HIFI on board will observe the CH + 1 → 0 and 2 → 1 rotational transitions in a wide range of gas temperatures up to 1000 K. Collisional parameters for such temperatures are thus welcome. Aims. We aim to obtain accurate rate coefficients for the collisional excitation of CH + by He for high gas temperatures. Methods. The ab initio coupled-cluster [CCSD(T)] approximation was used to compute the interaction potential energy. Cross sections are then derived in the close coupling (CC) approach and rate coefficients inferred by averaging these cross sections over a Maxwell-Boltzmann distribution of kinetic energies. Results. Cross sections are calculated up to 10 000 cm −1 for J ranging from 0 to 10. Rate coefficients are obtained at high temperatures up to 2000 K.

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“…Because G10.6-0.4 shows a large continuum flux at infrared and radio wavelengths, this sight-line has proven one of the most valuable in the Galaxy for the study of interstellar gas by absorption line spectroscopy. Indeed, line absorption by foreground gas has been detected over three and onehalf decades in wavelength, from species as diverse as atomic oxygen (at 63 μm, Keene et al 1999), 13 CH + (J = 1−0 at 361 μm, Falgarone et al 2005), HCO + (J = 1−0 at 3.36 mm, Keene et al 1999;Godard et al 2010), and atomic hydrogen (at 21 cm, Fish et al 2003).…”

Section: Introductionmentioning

confidence: 99%

Strong absorption by interstellar hydrogen fluoride:Herschel/HIFI observations of the sight-line to G10.6–0.4 (W31C)

Neufeld¹,

Sonnentrucker²,

Phillips

et al. 2010

A&A

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We report the detection of strong absorption by interstellar hydrogen fluoride along the sight-line to the submillimeter continuum source G10.6-0.4 (W31C). We have used Herschel's HIFI instrument, in dual beam switch mode, to observe the 1232.4763 GHz J = 1−0 HF transition in the upper sideband of the Band 5a receiver. The resultant spectrum shows weak HF emission from G10.6-0.4 at LSR velocities in the range -10 to -3 km s −1 , accompanied by strong absorption by foreground material at LSR velocities in the range 15 to 50 km s −1 . The spectrum is similar to that of the 1113.3430 GHz 1 11 −0 00 transition of para-water, although at some frequencies the HF (hydrogen fluoride) optical depth clearly exceeds that of para-H 2 O. The optically-thick HF absorption that we have observed places a conservative lower limit of 1.6 × 10 14 cm −2 on the HF column density along the sight-line to G10.6-0.4. Our lower limit on the HF abundance, 6 × 10 −9 relative to hydrogen nuclei, implies that hydrogen fluoride accounts for between ∼30% and 100% of the fluorine nuclei in the gas phase along this sight-line. This observation corroborates theoretical predictions that -because the unique thermochemistry of fluorine permits the exothermic reaction of F atoms with molecular hydrogen -HF will be the dominant reservoir of interstellar fluorine under a wide range of conditions.

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First Detection of ¹³ CH ⁺ ( J = 1-0)

Abstract: We report the probable detection of the (1-0) line in absorption against the dust continuum emission of 13 ϩ CH a bright star-forming region, G10.6Ϫ0.4. If the line velocity centroid is that of the H i gas seen in absorption, 13 ϩ

Cited by 31 publications

References 34 publications

Interstellar OH⁺, H₂O⁺and H₃O⁺along the sight-line to G10.6–0.4

Interstellar OH⁺, H₂O⁺and H₃O⁺along the sight-line to G10.6–0.4

Rotational excitation of methylidynium (CH⁺) by a helium atom at high temperature

Strong absorption by interstellar hydrogen fluoride:Herschel/HIFI observations of the sight-line to G10.6–0.4 (W31C)

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First Detection of 13 CH + ( J = 1-0)

Abstract: We report the probable detection of the (1-0) line in absorption against the dust continuum emission of 13 ϩ CH a bright star-forming region, G10.6Ϫ0.4. If the line velocity centroid is that of the H i gas seen in absorption, 13 ϩ

Cited by 31 publications

References 34 publications

Interstellar OH+, H2O+and H3O+along the sight-line to G10.6–0.4

Interstellar OH+, H2O+and H3O+along the sight-line to G10.6–0.4

Rotational excitation of methylidynium (CH+) by a helium atom at high temperature

Strong absorption by interstellar hydrogen fluoride:Herschel/HIFI observations of the sight-line to G10.6–0.4 (W31C)

Contact Info

Product

Resources

About

First Detection of ¹³ CH ⁺ ( J = 1-0)

Interstellar OH⁺, H₂O⁺and H₃O⁺along the sight-line to G10.6–0.4

Interstellar OH⁺, H₂O⁺and H₃O⁺along the sight-line to G10.6–0.4

Rotational excitation of methylidynium (CH⁺) by a helium atom at high temperature