Detection of chloronium and measurement of the35Cl/37Cl isotopic ratio atz= 0.89 toward PKS 1830–211

Müller, S.; Black, J. H.; Guèlin, M.; Henkel, C.; Combes, F.; Gérin, M.; Aalto, S.; Beelen, A.; Darling, Jeremy; Horellou, C.; Martín, S.; Menten, K. M.; V-Trung, Dinh

doi:10.1051/0004-6361/201423947

Cited by 37 publications

(46 citation statements)

References 34 publications

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“…The detection of the para-H 2 Cl + 1 11 -0 00 line along both the SW and NE lines of sight has already been reported by Muller et al (2014a). Assuming for each sightline that 3/4 is contributed by the ortho H 2 Cl + and 1/4 by the para H 2 Cl + , they estimated total H 2 Cl + column densities of 1.4 ×10 13 cm −2 in the SW line of sight, and 4 ×10 12 cm −2 in the NE line of sight.…”

Section: Observed Absorption Spectrasupporting

confidence: 54%

“…Molecules tracing gas with a low fraction of molecular hydrogen ( f H 2 ) preferentially, such as ArH + , OH + , H 2 O + , and H 2 Cl + , are found to have enhanced abundances along the NE line of sight relative to the SW one (Muller et al 2014a;Müller et al 2015;Muller et al 2016a). Among other evidence, this observation suggests that the absorbing gas in the NE line of sight is more diffuse.…”

Section: Description Of the Sourcementioning

confidence: 99%

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The ortho-to-para ratio of H₂Cl⁺: Quasi-classical trajectory calculations and new simulations in light of new observations

Gal

Xie

Herbst

et al. 2017

A&A

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Multi-hydrogenated species with proper symmetry properties can present different spin configurations, and thus exist under different spin symmetry forms, labeled as para and ortho for two-hydrogen molecules. We investigated here the ortho-to-para ratio (OPR) of H 2 Cl + in the light of new observations performed in the z=0.89 absorber toward the lensed quasar PKS 1830−211 with the Atacama Large Millimeter/submillimeter Array (ALMA). Two independent lines of sight were observed, to the southwest (SW) and northeast (NE) images of the quasar, with OPR values found to be 3.15±0.13 and 3.1±0.5 in each region, respectively, in agreement with a spin statistical weight of 3:1. An OPR of 3:1 for a molecule containing two identical hydrogen nuclei can refer to either a statistical result or a high-temperature limit depending on the reaction mechanism leading to its formation. It is thus crucial to identify rigorously how OPRs are produced in order to constrain the information that these probes can provide. To understand the production of the H 2 Cl + OPR, we undertook a careful theoretical study of the reaction mechanisms involved with the aid of quasi-classical trajectory calculations on a new global potential energy surface fit to a large number of high-level ab initio data. Our study shows that the major formation reaction for H 2 Cl + produces this ion via a hydrogen abstraction rather than a scrambling mechanism. Such a mechanism leads to a 3:1 OPR, which is not changed by destruction and possible thermalization reactions for H 2 Cl + and is thus likely to be the cause of observed 3:1 OPR ratios, contrary to the normal assumption of scrambling.

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Section: Observed Absorption Spectrasupporting

confidence: 54%

Section: Description Of the Sourcementioning

confidence: 99%

The ortho-to-para ratio of H₂Cl⁺: Quasi-classical trajectory calculations and new simulations in light of new observations

Gal

Xie

Herbst

et al. 2017

A&A

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“…Muller et al (2014a) found a similar ratio of ∼3 for H 2 Cl + . In contrast, the H 2 column density, estimated from proxies such as CH, is about one order of magnitude higher toward SW (Muller et al 2014b).…”

Section: Column Densities and Abundancesmentioning

confidence: 72%

Detection of extragalactic argonium, ArH⁺, toward PKS 1830−211

Müller

Schilke

et al. 2015

A&A

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Context. Argonium has recently been detected as a ubiquitous molecule in our Galaxy. Model calculations indicate that its abundance peaks at molecular fractions in the range of 10 −4 to 10 −3 and that the observed column densities require high values of the cosmic ray ionization rate. Therefore, this molecular cation may serve as an excellent tracer of the very diffuse interstellar medium (ISM), as well as an indicator of the cosmic ray ionization rate. Aims. We attempted to detect ArH + in extragalactic sources to evaluate its diagnostic power as a tracer of the almost purely atomic ISM in distant galaxies. Methods. We obtained ALMA observations of a foreground galaxy at z = 0.89 in the direction of the lensed blazar PKS 1830−211. Results. Two isotopologs of argonium, 36 ArH + and 38 ArH + , were detected in absorption along two different lines of sight toward PKS 1830−211, known as the SW and NE images of the background blazar. The argonium absorption is clearly enhanced on the more diffuse line of sight (NE) compared to other molecular species. The isotopic ratio 36 Ar/ 38 Ar is 3.46 ± 0.16 toward the SW image, i.e., significantly lower than the solar value of 5.5.Conclusions. Our results demonstrate the suitability of argonium as a tracer of the almost purely atomic, diffuse ISM in high-redshift sources. The evolution of the isotopic ratio with redshift may help to constrain nucleosynthetic scenarios in the early Universe.

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“…These estimates were consistent with the hightemperature LTE value of 3, but had very large error bars. Most recently, extragalactic chloronium has been detected in the z = 0.89 absorber in front of the lensed blazar PKS 1830-211 (Muller et al 2014), again through observations of the 1 0 11 00 -transition, redshifted now to ∼257 GHz.…”

Section: Introductionmentioning

confidence: 93%

HERSCHELOBSERVATIONS OF INTERSTELLAR CHLORONIUM. II. DETECTIONS TOWARD G29.96-0.02, W49N, W51, AND W3(OH), AND DETERMINATIONS OF THE ORTHO-TO-PARA AND³⁵Cl/³⁷Cl ISOTOPIC RATIOS

Neufeld

Black

Gérin

et al. 2015

ApJ

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We report additional detections of the chloronium molecular ion, H 2 Cl + , toward four bright submillimeter continuum sources: G29.96-0.02, W49N, W51, and W3(OH). With the use of the HIFI instrument on board the Herschel Space Observatory, we observed the 2 1 Cl + column density ratios that are consistent with the solar system 35 Cl/ 37 Cl isotopic ratio of 3.1, and chloronium ortho-to-para ratios consistent with 3, the ratio of spin statistical weights.

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Detection of chloronium and measurement of the³⁵Cl/³⁷Cl isotopic ratio atz= 0.89 toward PKS 1830–211

Cited by 37 publications

References 34 publications

The ortho-to-para ratio of H₂Cl⁺: Quasi-classical trajectory calculations and new simulations in light of new observations

The ortho-to-para ratio of H₂Cl⁺: Quasi-classical trajectory calculations and new simulations in light of new observations

Detection of extragalactic argonium, ArH⁺, toward PKS 1830−211

HERSCHELOBSERVATIONS OF INTERSTELLAR CHLORONIUM. II. DETECTIONS TOWARD G29.96-0.02, W49N, W51, AND W3(OH), AND DETERMINATIONS OF THE ORTHO-TO-PARA AND³⁵Cl/³⁷Cl ISOTOPIC RATIOS

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Detection of chloronium and measurement of the35Cl/37Cl isotopic ratio atz= 0.89 toward PKS 1830–211

Cited by 37 publications

References 34 publications

The ortho-to-para ratio of H2Cl+: Quasi-classical trajectory calculations and new simulations in light of new observations

The ortho-to-para ratio of H2Cl+: Quasi-classical trajectory calculations and new simulations in light of new observations

Detection of extragalactic argonium, ArH+, toward PKS 1830−211

HERSCHELOBSERVATIONS OF INTERSTELLAR CHLORONIUM. II. DETECTIONS TOWARD G29.96-0.02, W49N, W51, AND W3(OH), AND DETERMINATIONS OF THE ORTHO-TO-PARA AND35Cl/37Cl ISOTOPIC RATIOS

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Detection of chloronium and measurement of the³⁵Cl/³⁷Cl isotopic ratio atz= 0.89 toward PKS 1830–211

The ortho-to-para ratio of H₂Cl⁺: Quasi-classical trajectory calculations and new simulations in light of new observations

The ortho-to-para ratio of H₂Cl⁺: Quasi-classical trajectory calculations and new simulations in light of new observations

Detection of extragalactic argonium, ArH⁺, toward PKS 1830−211

HERSCHELOBSERVATIONS OF INTERSTELLAR CHLORONIUM. II. DETECTIONS TOWARD G29.96-0.02, W49N, W51, AND W3(OH), AND DETERMINATIONS OF THE ORTHO-TO-PARA AND³⁵Cl/³⁷Cl ISOTOPIC RATIOS