Free Access
Issue
A&A
Volume 516, June-July 2010
Article Number L3
Number of page(s) 2
Section Letters
DOI https://doi.org/10.1051/0004-6361/201014877
Published online 22 June 2010
A&A 516, L3 (2010)

LETTER TO THE EDITOR

Rotational transitions of CH$_{\sf 2}$D+ determined by high-resolution IR spectroscopy

S. Gärtner - J. Krieg - A. Klemann - O. Asvany - S. Schlemmer

I. Physikalisches Institut, Universität zu Köln, Zülpicher Str. 77, 50937 Köln, Germany

Received 28 April 2010 / Accepted 10 May 2010

Abstract
Context. Deuterated forms of CH3+ are responsible for deuterium fractionation in warmer environments. Current searches for CH2D+ are hampered by a lack of accurate laboratory data.
Aims. We demonstrate that IR spectroscopy at very high resolution can make accurate rotational predictions.
Methods. By combining a low-temperature ion trap with a narrow-bandwidth IR light source, we are able to measure vibrational transitions with high accuracy. A subsequent fit using an asymmetric rotor model allows predictions of MHz accuracy or even better.
Results. We predict rotational transitions up to 1.5 THz.

Key words: methods: laboratory - ISM: molecules - submillimeter: ISM

1 Introduction

In cold interstellar clouds, the deuterium content of some molecules is enhanced by several orders of magnitude relative to the cosmic D/H ratio of $1.5\times10^{-5}$. While gas-phase ion-molecule reactions involving H3+-isotopologues are responsible for this fractionation in the coldest regions, as proven by several detections of H2D+ (Stark et al. 1999) and a single observation of D2H+ by Vastel et al. (2004), CH3+ is assumed to mediate the fractionation in warmer (50 K) clouds (Roueff et al. 2007). This can be traced back to the exchange reactions

$\displaystyle \rm {CH}_3^+ + \rm {HD}$ $\textstyle \rightleftharpoons$ $\displaystyle \rm {CH}_2\rm {D}^+ + \rm {H}_2$ (1)
$\displaystyle \rm {CH}_2\rm {D}^+ + \rm {HD}$ $\textstyle \rightleftharpoons$ $\displaystyle \rm {CD}_2\rm {H}^+ + \rm {H}_2$ (2)
$\displaystyle \rm {CD}_2\rm {H}^+ + \rm {HD}$ $\textstyle \rightleftharpoons$ $\displaystyle \rm {CD}_3^+ \hspace{0.5cm} + \rm {H}_2,$ (3)

which are quite effective (Asvany et al. 2004) and whose relatively high exothermicity of about 370 K (Smith et al. 1982) prevents the formed deuterated species being destroyed in the warmer H2 gas. To support this CH3+ hypothesis, there are currently astronomical searches for the rotational signatures of CH2D+. Unfortunately, these searches have been hampered by the lack of accurate laboratory data of the rotational transitions, only measurements of the IR vibrational transitions being available to date (Jagod et al. 1992; Rösslein et al. 1991). Jagod et al. (1992) recorded some hundred lines of the $\nu_1$ and $\nu _4$ IR bands of CH2D+ and the $\nu_1$band of CD2H+, and a subsequent fit yielded molecular constants of the molecular ground state, in particular predictions of the rotational transitions. The IR spectroscopic techniques 20 years ago permitted predictions with uncertainties up to $\sim$10 MHz for the range 200-600 GHz, as documented currently in the Cologne Database for Molecular Spectroscopy (CDMS, Müller et al. 2005).

Submm-spectroscopy of carbon-containing species remains a challenge. To support future laboratory and astronomical searches for rotational transitions of CH2D+, as a first step, we revisit the IR spectroscopy of CH2D+at very high resolution. We achieve this by applying a low temperature ion trap combined with a narrow-bandwidth IR source, permitting us to push the predictions into the sub-MHz domain. A full experimental account will be given elsewhere, but the predictions for the astronomically important rotational transitions can be found at the end of this letter.

2 Laboratory methods

We recorded the $\nu_1$ and $\nu _4$ IR-active bands of CH2D+by applying the method of laser-induced reactions (LIR, Schlemmer et al. 1999; Asvany et al. 2007,2008,2005; Schlemmer et al. 2005). In brief, typically 3000 CH2D+ ions were stored and cooled in a low-temperature 22-pole ion trap (Gerlich 1995) held at 14 K and subject to cold hydrogen gas. The IR light traversing the trap was then able to induce the reaction in Eq. (1) in the backward direction. Thus, by counting the laser-induced reaction products CH3+ as a function of the laser frequency, we were able to record a spectrum. As the IR light source we used a home-made optical parametric oscillator (OPO), characterized by high power up to 1 W, a narrow bandwidth ($\sim$100 kHz), and a tunability between 2500 and 4000 cm-1. The relative frequency measurement has been achieved with a commercial wavemeter, and placed on an absolute basis with a calibration gas contained in a multipass reflection cell. Because of the high accuracy requirements, only lines of OCS (Guelachvili & Rao 1993; Saupe et al. 1996, NIST[*]) and H2O (Toth 1993) known with better accuracy than 1 MHz have been used as reference. In summary, because of the cold ions, the vanishing linewidth of the laser, and use of accurate calibration gases, the center frequencies of the measured transitions were able to be determined with high accuracy of typically 3 MHz. We checked this by comparing combination differences in the ground and excited states.

3 Results and predicted rotational spectra

\begin{figure}
\par\includegraphics[width=8.5cm,clip]{14877fig1.eps}
\end{figure} Figure 1:

Four lines of the the $\nu _4$ vibrational band of CH2D+. The strongest one is the transition $3_{03} \leftarrow 3_{12}$ at $(3091.24687 \pm 0.0001)$ cm-1.

Open with DEXTER

We measured in total 112 lines in the two bands, some coinciding with those of Jagod et al. (1992). As an example, Fig. 1 shows four lines of the $\nu _4$ vibrational band. An asymmetric rotor model was fitted to the lines using SPFIT (Pickett 1991) and PGOPHER[*] with our data only, our data and those of Jagod et al. (1992), and our 61 ground state combination differences. All fits show consistent results, as long as sextic distortion constants are included. As expected, the average deviation of our IR data from the fit is about 4 MHz. The ground state molecular constants based on our lines alone are summarized in Table 1 and the resulting predictions for the rotational transitions are collected in Table 2. They are given up to to 1.5 THz for potential high-frequency searches (APEX, Herschel). A comparison to the values of Rösslein et al. (1991) and CDMS (essentially a re-fit of the lines of Jagod et al. 1992), shows that the predictions are in very good agreement, and are substantially refined by this work. Further improvements of the presented high resolution IR technique will thus aid laboratory and astronomical searches of species whose pure rotational spectra are difficult to measure.

During the review process we learned that Amano had submitted a paper on the pure rotational lines of CH2D+, also published in this volume. The predicted frequencies based on both works will be available at CDMS.

Table 1:   Best-fit parameters in the ground state of CH2D+given in MHz. For the sextic distortion constants on the right, only those of statistical significance are given.

Table 2:   Prediction of low-lying (J<6) rotational transitions (in MHz) of CH2D+ up to 1.5 THz.

Acknowledgements
The authors thank Holger Müller and Evelyne Roueff for discussions, as well as Colin Western for assistance with PGOPHER.

References

Footnotes

... NIST[*]
Wavenumbers for Calibration of IR Spectrometers, data taken from http://www.nist.gov/physlab/data/wavenum/
... PGOPHER[*]
PGOPHER, a Program for Simulating Rotational Structure, C. M. Western, University of Bristol, http://pgopher.chm.bris.ac.uk

All Tables

Table 1:   Best-fit parameters in the ground state of CH2D+given in MHz. For the sextic distortion constants on the right, only those of statistical significance are given.

Table 2:   Prediction of low-lying (J<6) rotational transitions (in MHz) of CH2D+ up to 1.5 THz.

All Figures

  \begin{figure}
\par\includegraphics[width=8.5cm,clip]{14877fig1.eps}
\end{figure} Figure 1:

Four lines of the the $\nu _4$ vibrational band of CH2D+. The strongest one is the transition $3_{03} \leftarrow 3_{12}$ at $(3091.24687 \pm 0.0001)$ cm-1.

Open with DEXTER
In the text

Copyright ESO 2010

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