The rotational spectrum of protonated sulfur dioxide, HOSO<sup>+</sup>

Lattanzi, Valerio; Gottlieb, C. A.; Thaddeus, P.; Thorwirth, Sven; McCarthy, Michael

doi:10.1051/0004-6361/201117753

Cited by 9 publications

(8 citation statements)

References 24 publications

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“…This level of agreement is similar to that obtained with the same level of theory (CcCR QFF) recently reported for HOCO + (Bizzocchi et al 2017). For example, the experimental D J fourth-order distortion constant differs by 2.5% from the ab-initio values; recent studies on rigid molecules with two to three heavy atoms showed that this parameter, when calculated at a high level of theory, is usually accurate to about 3% or better (Lattanzi et al 2011;Spezzano et al 2012). In Table 1 the HSCO + spectroscopic parameters are also compared with those derived by Brünken et al (2009) for HSCN.…”

Section: Discussionsupporting

confidence: 88%

HSCO⁺ and DSCO⁺: a multi-technique approach in the laboratory for the spectroscopy of interstellar ions

Lattanzi

Spezzano

Laas

et al. 2018

A&A

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Context. Protonated molecular species have been proven to be abundant in the interstellar gas. This class of molecules is also pivotal for the determination of important physical parameters for the ISM evolution (e.g. gas ionisation fraction) or as tracers of non-polar, hence not directly observable, species. The identification of these molecular species through radioastronomical observations is directly linked to a precise laboratory spectral characterisation. Aims. The goal of the present work is to extend the laboratory measurements of the pure rotational spectrum of the ground electronic state of protonated carbonyl sulfide (HSCO + ) and its deuterium substituted isotopomer (DSCO + ). At the same time, we show how implementing different laboratory techniques allows the determination of different spectroscopical properties of asymmetric-top protonated species. Methods. Three different high-resolution experiments were involved to detected for the first time the b−type rotational spectrum of HSCO + , and to extend, well into the sub-millimeter region, the a−type spectrum of the same molecular species and DSCO + . The electronic ground-state of both ions have been investigated in the 273-405 GHz frequency range, allowing the detection of 60 and 50 new rotational transitions for HSCO + and DSCO + , respectively. Results. The combination of our new measurements with the three rotational transitions previously observed in the microwave region permits the rest frequencies of the astronomically most relevant transitions to be predicted to better than 100 kHz for both HSCO + and DSCO + up to 500 GHz, equivalent to better than 60 m/s in terms of equivalent radial velocity. Conclusions. The present work illustrates the importance of using different laboratory techniques to spectroscopically characterise a protonated species at high frequency. Each instruments addressed complementary part of the same spectroscopic challenge, showing that a similar approach can be adopted in the future when dealing with similar reactive species.

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Section: Discussionsupporting

confidence: 88%

HSCO⁺ and DSCO⁺: a multi-technique approach in the laboratory for the spectroscopy of interstellar ions

Lattanzi

Spezzano

Laas

et al. 2018

A&A

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“…These include H 2 O + , SH + , SO + , HCS + , CO + , HOCO + , and NNH + . In addition to these, the HOSO + ion recently measured in the laboratory may also be a plausible species in VY CMa (Lattanzi et al 2011). We were unable to identify any of the positive molecular ions referred to -26here in our survey, nevertheless this band appears well suited for future searches for new molecular ions in this source.…”

Section: Molecular Ions and Recombination Linesmentioning

confidence: 69%

AN INTERFEROMETRIC SPECTRAL LINE AND IMAGING SURVEY OF VY CANIS MAJORIS IN THE 345 GHz BAND

Kamiński

Gottlieb

Young

et al. 2013

ApJS

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A spectral line survey of the oxygen-rich red supergiant VY Canis Majoris was made between 279 and 355 GHz with the Submillimeter Array. Two hundred twenty three spectral features from 19 molecules (not counting isotopic species of some of them) were observed, including the rotational spectra of TiO, TiO 2 , and AlCl for the first time in this source. The parameters and an atlas of all spectral features is presented. Observations of each line with a synthesized beam of ∼0. ′′ 9, reveal the complex kinematics and morphology of the nebula surrounding VY CMa. Many of the molecules are observed in high lying rotational levels or in excited vibrational levels. From these, it was established that the main source of the submillimeter-wave continuum (dust) and the high excitation molecular gas (the star) are separated by about 0. ′′ 15. Apparent coincidences between the molecular gas observed with the SMA, and some of the arcs and knots observed at infrared wavelengths and in the optical scattered light by the Hubble Space Telescope are identified. The observations presented here provide important constraints on the molecular chemistry in oxygen-dominated circumstellar environments and a deeper picture of the complex circumstellar environment of VY CMa.-4according to morphological type (Sect. 3.3); and discusses the continuum and location of the centers of molecular emission with respect to the peak of the continuum (Sect. 3.4). From an analysis of population diagrams, approximate rotational temperatures and column densities of eleven molecules were derived (Appendix B). A detailed discussion of the chemistry in the circumstellar gas and the structure of the outflow of VY CMa will be presented elsewhere. Observations and data reductionThe survey of VY CMa was obtained together with an AGB star IK Tau, whose observations will be presented elsewhere. The observations of VY CMa were made with the SMA in its extended configuration over ten nights during January and February of 2010 (see Table 1). In that configuration, unprojected baselines range in length from 44 to 226 m producing a synthesized beam with a full width at half maximum (FWHM) of typically 0. ′′ 9. On each night, observing began around 03:30 UT; IK Tau was observed for about two hours until VY CMa rose, at which time observations of IK Tau and VY CMa were interleaved for five hours until IK Tau set. After that, VY CMa was observed alone for two more hours. The phase center for IK Tau was α(2000) = 03 h 53 m 28.866 s , δ(2000) = 11 • 24 ′ 22.29. ′′ 2; for VY CMa α(2000) = 07 h 22 m 58.332 s , δ(2000) = −25 • 46 ′ 03.17. ′′ 2 was used. The online software Doppler-tracked VY CMa during the entire observation, the frequency scale for the IK Tau data was corrected offline to compensate for that. Nearby quasars were observed every 20 min for gain calibration. The quasar 0423-013 was used to calibrate IK Tau data, and 0730-116 was used for VY CMa. Titan was observed for flux calibration on the nights when it was separated from Saturn by several arcmin. On other night...

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“…[1a] It appearst hat, despite the presence of thesen eutral and ionic species in severala strophysicale nvironments, there is an unexpected lack of both experimental and computational studies of their reactivity.I ni ts neutral (SO 2 )a nd cationic state (SO 2 · + )t he simplest, most fundamental and widespread reactions with ag eneral compound RÀHi nvolvep roton transfer (PT) from RÀH 0/ + to SO 2 and hydrogen atom transfer (HAT) from RÀHt oS O 2 · + ,b oth leading to the same ionic product, HSO 2 + . [8] Although the protonated sulfur dioxide has not yet been detected in space,t he growing field of interstellar ion chemistrya nd the rotationals pectra data collected in the laboratory [9] will probably help identifying this ion. Hence, reactions that produce HSO 2 + and the kinetic trend of the reaction with the temperature are relevant to understanding the reactiven etwork of sulfur-containing compounds.…”

Section: Introductionmentioning

confidence: 99%

HSO₂⁺ Formation from Ion‐Molecule Reactions of SO₂^⋅+ with Water and Methane: Two Fast Reactions with Reverse Temperature‐Dependent Kinetic Trend

Cartoni

Catone

Bolognesi

et al. 2017

Chemistry A European J

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In this work an experimental and theoretical study on the formation of HSO ion from the SO +CH and SO +H O ion-molecule reactions at different temperatures is reported. Tunable synchrotron radiation was used to produce the SO ion in excited ro-vibrational levels of the ionic ground state X A and mass spectrometry was employed to identify the product ions. Calculations in the frame of the density functional theory and variational transition state theory were combined to explore the dynamics of the reactions. The experimental results show that HSO is the only product in both reactions. Its yield decreases monotonically with photon energy in the SO +H O reaction, while it decreases at first and then increases in the SO +CH reaction. Theory confirms this trend by calculating the rate constants at different temperatures and explains the results by means of the polar, spin and charge effects as well as structural reorganization occurring in the reaction coordinate. The dynamic behavior observed in these two reactions is of general and fundamental interest. It can also provide some insights on the role of these reactions in astrochemistry as well as in their use as models for bond-activation reactions.

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The rotational spectrum of protonated sulfur dioxide, HOSO⁺

Cited by 9 publications

References 24 publications

HSCO⁺ and DSCO⁺: a multi-technique approach in the laboratory for the spectroscopy of interstellar ions

HSCO⁺ and DSCO⁺: a multi-technique approach in the laboratory for the spectroscopy of interstellar ions

AN INTERFEROMETRIC SPECTRAL LINE AND IMAGING SURVEY OF VY CANIS MAJORIS IN THE 345 GHz BAND

HSO₂⁺ Formation from Ion‐Molecule Reactions of SO₂^⋅+ with Water and Methane: Two Fast Reactions with Reverse Temperature‐Dependent Kinetic Trend

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The rotational spectrum of protonated sulfur dioxide, HOSO+

Cited by 9 publications

References 24 publications

HSCO+ and DSCO+: a multi-technique approach in the laboratory for the spectroscopy of interstellar ions

HSCO+ and DSCO+: a multi-technique approach in the laboratory for the spectroscopy of interstellar ions

AN INTERFEROMETRIC SPECTRAL LINE AND IMAGING SURVEY OF VY CANIS MAJORIS IN THE 345 GHz BAND

HSO2+ Formation from Ion‐Molecule Reactions of SO2⋅+ with Water and Methane: Two Fast Reactions with Reverse Temperature‐Dependent Kinetic Trend

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The rotational spectrum of protonated sulfur dioxide, HOSO⁺

HSCO⁺ and DSCO⁺: a multi-technique approach in the laboratory for the spectroscopy of interstellar ions

HSCO⁺ and DSCO⁺: a multi-technique approach in the laboratory for the spectroscopy of interstellar ions

HSO₂⁺ Formation from Ion‐Molecule Reactions of SO₂^⋅+ with Water and Methane: Two Fast Reactions with Reverse Temperature‐Dependent Kinetic Trend