Volume 559, November 2013
|Number of page(s)||9|
|Section||Atomic, molecular, and nuclear data|
|Published online||26 November 2013|
The rotational spectrum of 12C2HD in the ground and excited bending states: an improved ro-vibrational global analysis
1 Dipartimento di Chimica “Giacomo Ciamician”Università di Bologna, via F. Selmi 2, 40126 Bologna, Italy
e-mail: email@example.com; firstname.lastname@example.org
2 Dipartimento di Chimica Industriale “Toso Montanari”, Università di Bologna, viale del Risorgimento 4, 40136 Bologna, Italy
e-mail: email@example.com; firstname.lastname@example.org
Received: 26 July 2013
Accepted: 11 October 2013
Rotational transitions of 12C2HD were recorded in the range 100–700 GHz for the vibrational ground state and for the bending states v4 = 1 (Π), v5 = 1 (Π), v4 = 2 (Σ+ and Δ), v5 = 2 (Σ+ and Δ), v4 = v5 = 1 (Σ−, Σ+ and Δ), v4 = 3 (Π and Φ) and v5 = 3 (Π and Φ). The transition frequencies measured in this work were fitted together with all the infrared ro-vibrational transitions involving the same bending states available in the literature. The global fit allowed a very accurate determination of the vibrational, rotational, and ℓ-type interaction parameters for the bending states up to v4 + v5 = 3 of this molecule. The results reported in this paper provide a set of information very useful for undertaking astronomical searches in both the mm−wave and the infrared spectral regions. The parameters from the global fit can be used to calculate accurate rest frequencies for rotational transitions in the ground state or in excited vibrational states involving the bending modes. Pure rotational transition frequencies up to 1 THz are listed.
Key words: molecular data / methods: laboratory: molecular / techniques: spectroscopic / catalogs
© ESO, 2013
Acetylene can be found in several astronomical environments: in molecular clouds (Lacy et al. 1989), in massive young stellar objects and planet forming zones (Lahuis & van Dishoeck 2000; Bast et al. 2013), in circumstellar envelopes of AGB stars (Ridgway et al. 1976; Matsuura et al. 2006; Fonfría et al. 2008), and it has been identified in cometary comae (Mumma et al. 2003) as well. This unsaturated hydrocarbon may react with radicals – atomic C, CN, and CH – to form complex molecules in starless cores (Herbst 2005), it plays a key role in the formation of circumstellar carbon chain molecules (Cherchneff & Glassgold 1993) and it is even a possible precursor of benzene in a carbon-rich PPN (Woods et al. 2002).
However, 12C2H2 does not have a permanent dipole moment and cannot be detected by (sub-)millimetre telescopes, therefore interstellar acetylene has been detected by observing its vibration-rotation bands. The only detectable sub-millimetre features could be those due to some P-branch high-J transitions of the ν5 ← ν4 difference band in the THz region (Yu et al. 2009). On the other hand, non-centrosymmetric isotopologues of acetylene, such as the subject of this paper 12C2HD, do have a small permanent electric dipole moment. The first astronomical detection of 12C2HD is recent, namely it has been observed in Titan’s atmosphere through the Composite InfraRed Spectrometer (CIRS) mounted on the Cassini spacecraft (Coustenis et al. 2008). From these observations it was possible to derive the D/H ratio on Titan, which was previously determined only through the transitions of the CH4/CH3D pair.
Molecules containing less abundant isotopes are very relevant from an astrophysical point of view. Several species containing D, 13C, 15N, 18O, among the most important, provide a tool to assess isotopic ratios in several astronomical environments (see for instance Herbst 2003; Caselli & Ceccarelli 2012; Bézard 2009). The D/H isotopic ratio is of particular interest for several reasons. It is an important experimental constraint on the Big Bang models, as deuterium was formed in abundance only in this event. It can also provide key information on the chemical processes that lead to the formation of complex organic molecules (Sandford et al. 2001). Although the cosmic D/H ratio is of the order of magnitude of 10-5, abundances of a few percent with respect to their parent species can be produced in the interstellar medium through isotopic fractionation mechanisms (Herbst 2003). It is known that in cold dense interstellar clouds D-enrichment proceeds through gas phase ion-molecule exothermic reactions, but also through gas-grain chemistry (Sandford et al. 2001). Alternative routes for achieving D-H fractionation in more energetic environments and of interest for complex molecules are: a) gas phase unimolecolar photodissociation; and b) ultraviolet photolysis in D-enriched ice mantles (Sandford et al. 2001).
Laboratory rotational spectra have been observed in the past for several monodeuterated species of acetylene, including also 13C containing isotopologues (Wlodarczak et al. 1989; Matsumura et al. 1980; Cazzoli et al. 2008; Degli Esposti et al. 2013). Rotational transitions of 12C2HD were measured up to 418 GHz for the ground vibrational state (GS) and for the v4 = 1 and v5 = 1 excited states, ν4 and ν5 being the trans and cis bending modes, respectively (Wlodarczak et al. 1989). Pure rotational transitions in the GS up to J′′ = 10, around 650 GHz, were observed for 12C2HD, H12C13CD and H13C12CD (Cazzoli et al. 2008). In the same study, ab initio calculations were performed at various levels in order to predict the electric dipole moment for these species and the equilibrium structure of acetylene. The calculated dipole moment does not show sizable variations upon isotopic substitution of one carbon atom, and is approximately 0.01 D for all monodeuterated isotopologues in the GS. The ν5 ← ν4 difference band and associated hot bands for 12C2HD have been recorded recently in the far-infrared (FIR) region, between 60 and 360 cm-1, using the synchrotron radiation at the Canadian Light Source (Predoi-Cross et al. 2011). The same band for the H12C13CD and H13C12CD isotopologues was also detected and analysed.
As far as the infrared (IR) region is concerned, several papers have been published on 12C2HD. The most recent are the investigations of the bending states up to v4 + v5 = 3 (Fusina et al. 2005a) and of the stretching-bending bands in the 1800–4700 cm-1 spectral region (Fusina et al. 2005b). In both cases the spectra were recorded by Fourier transform infrared spectroscopy (FTIR). A study of the integrated band intensities in the 25–2.5 μm window was also published (Jolly et al. 2008).
In the present paper we report on the observation of the pure rotational transitions of 12C2HD up to 657 GHz, that is in bands 3, 6, 7, 8 and 9 of the Atacama Large Millimeter Array (ALMA). A total of 168 transitions were assigned in the GS and in various excited vibrational bending states. The rotational lines detected in this work were fitted together with the FIR (Predoi-Cross et al. 2011) and IR lines (Fusina et al. 2005a). The spectroscopic parameters obtained from the final global fit are determined with an excellent accuracy.
The high accuracy of the millimetre- and submillimetre-wave data presented in this paper, together with the increasing sensitivity of new observation systems, such as ALMA, will favour the observation of transitions belonging to this species.
It should also be stressed that the dipole moment of 12C2HD is strongly enhanced by the bending vibrations. Therefore, considering that some chemically rich regions, e.g. IRC+10216 (Cernicharo et al. 2011), show a high degree of vibrational excitation, this will facilitate the detection of emission lines in the bending states ν4 or ν5 of 12C2HD. In Sect. 3.1, the dipole moment variation in excited bending states is discussed.
The sample of 12C2HD was purchased from CDN Isotopes (98.9% purity). The rotational spectra of 12C2HD were observed in selected frequency regions between 100 and 700 GHz, using a source-modulation mm-wave spectrometer which employs Gunn oscillators (RPG Radiometer Physics GmbH and J. E. Carlstrom Co.) as main radiation sources covering the fundamental frequency range 75–124 GHz. Higher frequencies were generated using three different frequency multipliers (VDI – Virginia Diodes, Inc. and RPG). The Gunn oscillators were phase-locked to the suitable harmonic of the frequency emitted by a computer-controlled frequency synthesizer (Schomandl), referenced to an external rubidium frequency standard (SRS Stanford Research System). This guaranteed an absolute accuracy of ca. 20 Hz to the frequency scale. A liquid-helium-cooled InSb detector (QMC Instr. Ltd.) was employed. The Gunn oscillators were frequency modulated at 6 kHz, and the detected signals were demodulated by a lock-in amplifier tuned at twice the modulation frequency, so that the second derivative of the actual spectrum profile was detected by the computer-controlled acquisition system.
Transition frequencies were recovered from a line-shape analysis of the spectral profile (Dore 2003); their accuracy, estimated by repeated measurements, was in the range 5–30 kHz depending on the signal-to-noise ratio of the recorded lines.
The absorption cell was a 3.5 m long, 10 cm in diameter glass tube equipped with polyethylene windows. A double pass arrangement based on a wire grid polarizer and a roof mirror (Ziurys et al. 1994; Dore et al. 1999) was employed to increase the absorption path. Sample pressures of a few tens of mTorr were employed during the measurements.
The J = 5 ← 4 transition of 12C2HD in the v5 = 1, ground, and v4 = 1 vibrational states. The low-frequency components of each ℓ-doublet are displayed. Fourteen scans are co-added, the total integration time is 850 s.
|Open with DEXTER|
Dipole moments, vibrational term values, populations and intensity calculations for several excited vibrational bending states of 12C2HD.
The very small dipole moment of 12C2HD was first determined by Matsumura et al. (1980), who performed Stark-effect measurements on the J = 2 ← 1 rotational transition of 12C2HD in the v4 = 1,3 and v5 = 1,3 states. The obtained dipole moment values are: − 0.02359(5) D for v4 = 1, 0.05601(9) D for v5 = 1, − 0.09077(26) D for v4 = 3 and 0.1472(21) D for v5 = 3. These experimental values led to extrapolate a GS moment of 0.01001(15) D, since the dipole moments of the v4 = 1 and v4 = 3 states have opposite sign with respect to that of the GS. The increase of the dipole moment values due to vibrational excitation causes a considerable intensity enhancement of the excited state rotational lines, so that their detection is much easier than expected from an evaluation of the population factors. At room temperature (kT = 207 cm-1), the population factors are N4/N0 = exp ( − 518/kT) = 0.0819 and N5/N0 = exp ( − 677/kT) = 0.0378, which should reduce the intensity of the rotational lines by a factor of 12 for v4 = 1 and of 26 for v5 = 1. It should be noticed that the bending states are doubly degenerate. However, the factor 2, which doubles the population of v4 = 1 and v5 = 1, has no effect on the intensity of the rotational lines. In fact, the ℓ-type doubling removes the degeneracy of the levels and rotational transitions are allowed only within each set. On the other hand, from the experimental μ values one can calculate the following ratios: (μ4/μ0)2 ≃ 5.6 and (μ5/μ0)2 ≃ 31, which partly compensate the unfavourable population factors of the excited states. The intensity ratio between rotational lines in the excited bending states and in the GS can be calculated as (1)The rotational transitions in v4 = 1 are expected to be less intense than those of the GS by only a factor 12/5.6 ≃ 2, whereas the lines in v5 = 1 should be even stronger than those in the GS by a factor 31/26 ≃ 1.2. Figure 1 shows a 250 MHz frequency scan in which the J = 5 ← 4 transitions of v5 = 1, ground, and v4 = 1 states are simultaneously present. The experimental intensity ratios nicely agree with the predicted ones. Anyway, for any combination of bending vibrational quanta, the dipole moment can be calculated by applying the usual expression for the vibrational dependence (2)as reported in Eq. (11) of Matsumura et al. (1980). The values of the parameters δμi are: δμ4 = − 0.03360(13) D and δμ5 = 0.04600(17) D, as given in Table 3 of the same reference. For mixed excitations of ν4 and ν5 there is a less significant enhancement on the dipole moment, and therefore on the intensity, since δμ4 and δμ5 have opposite sign and comparable magnitude. Indeed, only transitions in the combination v4 + v5 could be detected, whereas in higher-order mixed vibrational excitations they were too weak to be observed.
A summary of the intensity predictions at 300 K and 500 K for rotational lines of some vibrationally excited bending states is reported in Table 1. It is evident a large temperature effect, therefore at 500 K the transitions in vibrational states up to the doubly excited ν4 and ν5 are stronger than the ground-state ones.
A very limited number of excited-state transitions of 12C2HD have previously been observed only for v4 = 1,3 (Π) and v5 = 1,3 (Π) (Wlodarczak et al. 1989; Matsumura et al. 1980). We have considerably enlarged the previous data-set by measuring more than 150 new line frequencies, spanning J values from 1 to 10, corresponding to transitions in the ground state, in the first excited vibrational bending states v4 = 1 and v5 = 1 (Π), in the doubly excited v4 = 2 and v5 = 2 states (Σ+ and Δ), in the combination state v4 = v5 = 1 (Σ−, Σ+ and Δ) and in the triply excited v4 = 3 and v5 = 3 states (Π and Φ). The search of the rotational lines was guided by predictions based on the spectroscopic constants determined in a previous analysis of 4888 IR and FIR data and 21 rotational transitions available at that time (Predoi-Cross et al. 2011). On average, the newly observed lines were found some hundreds of kHz away from the initial predictions. The measured transition frequencies are listed in Table 2, along with predictions of unobserved low-J transitions and of the ones occurring at higher frequency up to 1 THz.
The term values of the observed rotational levels in the ground and excited vibrational states are in the range 2 − 2140 cm-1. With the exception of the ground state, multiplets of rotational lines were always observed for each J + 1 ← J transition, because of ℓ-type resonance effects. Before performing the final ro-vibrational global analysis (see Sect. 3.2), a series of state-by-state least-squares fits were done to check the consistency of the MW measurements. The pure rotational spectra have been analysed using the formalism originally developed by Yamada et al. (1985) and already employed to fit the excited-state rotational spectra of a large number of linear carbon chains (see for example Bizzocchi & Degli Esposti 2008, and references therein). The model is slightly different from the one used to perform the global ro-vibrational analysis (see Sect. 3.2 for a detailed description), because the vibrational dependence of the various parameters is neglected, so that effective constants for each vibrational state were determined by these preliminary fits. Briefly, rotational and vibrational ℓ-type resonance effects have been treated by diagonalization of ro-vibrational matrices with off-diagonal elements which include qt, , rtt′ and spectroscopic parameters (t and t′ being equal to 4 or 5). The vibrational energy differences between the interacting ℓ sublevels (Δℓt = ± 2) of each doubly or triply excited vibrational state have been expressed through the effective values of the constants g44, g55 and g45, which produce ℓ-dependent energy contributions. In addition, the ℓ-dependence of rotational and quartic centrifugal distortion constants have been taken into accounts trough the γtt′ and δtt′ parameters, respectively. Generally, not all of the required constants can be statistically determined from the rotational transitions of a single vibrational state, and some assumptions had to be necessarily made. The ℓ-type doubling parameters qt and were fitted for the vt = 1 (t = 4 or 5) and vt = 3 states (where degenerate ℓ = ± 1 levels do exist), but constrained to interpolated values for the vt = 2 states, in order to avoid high correlations with the g44 and g55 constants. The latter constant has a rather large value (ca. 5.2 cm-1), so that rotational ℓ-type resonance effects are weak in the v5 = 3 state, where no splitting of the | ℓ | = 3 lines could be observed. As far as the v4 = v5 = 1 combination state is concerned, where rotational and vibrational ℓ-type resonance effects are simultaneously present, qt and constants were held fixed at the values determined for the singly excited bending states, while the parameters involved in the vibrational ℓ-type resonance, namely g45, r45 and were refined. The various state-by-state fits were repeated iteratively in order to achieve full consistency of the obtained parameters. The results of the eight least-squares fits performed are collected in Tables 3 and 4.
Measured and predicteda transition frequencies (MHz) of 12C2HD in the ground and excited bending statesb.
Ro-vibrational transitions involving the vibrational states presently studied, except the v4 = 3 state (Φ), were already observed in the FIR and IR regions (Predoi-Cross et al. 2011; Fusina et al. 2005b). They have been fitted together with the rotational transitions presently measured. The model Hamiltonian adopted for the global analysis represents an extension up to three quanta of the bending excitation, i.e. v4 + v5 = 3, of the Hamiltonian for a molecule with two bending vibrations which has been described in detail by Herman et al. (1991). It was already used for 13C2HD (Degli Esposti et al. 2013) and 12C2HD (Fusina et al. 2005a) itself. The term values of the ro-vibrational levels of the transitions were obtained by diagonalizing the appropriate energy matrix containing the following vibrational (G0) and rotational (F) diagonal contributions: with M = J(J + 1) and k = ℓ4 + ℓ5.
Effective spectroscopic constants determined from state-by-state fits of the rotational transitions measured for the ground and v4 = 1, v5 = 1, v4 = v5 = 1 states of 12C2HDa.
Effective spectroscopic constants determined from state-by-state fits of the rotational transitions measured for the v4 = 2, v4 = 3, v5 = 2 and v5 = 3 states of 12C2HDa.
Vibrational and rotational ℓ-type resonances are expressed by off-diagonal matrix elements (Herman et al. 1991) containing the following parameters: The global fit included 5317 IR and 168 MW transitions. Overlapping lines were given zero weight. The uncertainty for the FIR and IR data was in the range 5.0 × 10-5 − 2.0 × 10-4 cm-1, and 1.0 × 10-7 cm-1 for the MW data. The MW blended lines were given an uncertainty of . Finally, 489 IR transitions, 9.2%, were excluded in the final fit because they were overlapping (271) or their observed-calculated values (218) were larger than 5 times their estimated experimental uncertainty.
For the 3ν4(Φ) state, the J′′ = 3 e/f components were not resolved. For the 3ν5(Φ) state, all the e/f components of the rotational lines were not resolved. The couples of overlapping lines were identified by the same frequency (see Table 2) and their observed-calculated values were derived from the comparison of the experimental frequency with the average of the frequencies calculated for the two components. Sixty nine statistically well determined parameters, which are collected in Table 5, were refined with a final rms value of 3.06 × 10-4 cm-1 for the IR data and 19 kHz for the MW data. A few parameters in the model not reported in Table 5 were nevertheless allowed to vary during the fitting procedure but they resulted statistically undetermined and were constrained to zero. Some of the parameters are highly correlated, i.e. , and y444, and , γ44 and . The results in Table 5 can be compared with those obtained from the previous analysis, see Table 2 of Predoi-Cross et al. (2011). Sixty two parameters are common to both sets. The inclusion of the MW data allowed the determination of 7 additional constants. Three of these are related to the ν4 bending states, partly because experimental data for the v4 = 3(Φ) state have been obtained for the first time. Values and signs of all the common parameters are consistent in both sets: the differences between new and old values being in the range 0–1% (31 parameters), 1–10% (18 parameters), 10–50% (7 parameters), 50–100% (5 parameters) and 1 parameter, h4, differs by 306%. The inclusion of the MW data also yields a significant improvement of the precision of the main constants which contribute to the rotational energy. For example, the values of B0, αt, and constants are ca. 5 times more precise than those determined previously (Predoi-Cross et al. 2011). It should be pointed out that in the present global analysis 60 additional IR transitions were discarded in the final fit, compared with the previous fit (Predoi-Cross et al. 2011), adopting the same rejection limits. The discarded lines are scattered over most of the bands. Considering the high accuracy of the assigned MW transitions, this result is particularly pleasing since it confirms the validity of the calibration of the IR data, which span a wide wavenumber range, from about 90 to 2100 cm-1.
Spectroscopic parameters (in cm-1) for the bending states of 12C2HD resulting from the simultaneous fit of all rovibrational and rotational transitions involving levels up to v4 + v5 = 3a.
Rotational lines of 12C2HD were detected in the range 100–700 GHz. They were analysed together with the IR transitions reported in the literature in a global fit. Sixty nine parameters (rotational, vibrational, ro-vibrational, and ℓ-type interaction) were determined with high precision. The analysis of the ℓ-type resonances which affect the pure rotational spectra allows the determination of the small vibrational energy differences ΔG between different ℓ-sublevels of a given vibrational state, which can be directly calculated using the effective values of the fitted gtt′, r45 and Bv constants in Tables 3 and 4.
Vibrational energy differences ( cm-1) between ℓ-sublevels of doubly and triply excited bending states of 12C2HD, as resulting from the rotational analysis and the global rovibrational analysis.
The reliability of these results can be checked by comparison with the corresponding values from the global analysis. Table 6 shows that the agreement between the two sets of ΔG values is very good, differences being mostly less than one percent, thus confirming that an accurate treatment of ℓ-type resonances in the pure rotational spectra can provide precise information on the vibrational energy. The set of spectroscopic constants determined in this work is the most accurate and consistent available in the literature. From these constants it is possible to derive very accurate predictions for IR and MW spectra useful for astronomical searches. An extensive list of rotational frequencies up to 1 THz is reported in Table 2 for all the observed vibrational states, whose energies are reported in Table 1. The line strength of each transition can be calculated by the simple formula (Lafferty & Lovas 1978): (3)
The authors acknowledge the Università di Bologna and the Ministero della Ricerca e dell’Università for financial support under the grant PRIN09 “High-resolution Spectroscopy for Atmospherical and Astrochemical Research: Experiment, Theory and Applications”. The authors also thank Prof. G. Di Lonardo for helping the analysis of the infrared spectra.
- Bast, J. E., Lahuis, F., van Dishoeck, E. F., & Tielens, A. G. G. M. 2013, A&A, 551, A118 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
- Bézard, B. 2009, Phil. Trans. Roy. S. London, Ser. A, 367, 683 [Google Scholar]
- Bizzocchi, L., & Degli Esposti, C. 2008, Chem. Phys., 346, 139 [NASA ADS] [CrossRef] [Google Scholar]
- Caselli, P., & Ceccarelli, C. 2012, A&AR, 20, 56 [NASA ADS] [CrossRef] [MathSciNet] [Google Scholar]
- Cazzoli, G., Puzzarini, C., Fusina, L., & Tamassia, F. 2008, J. Mol. Spectr., 247, 115 [NASA ADS] [CrossRef] [Google Scholar]
- Cernicharo, J., Agúndez, M., Kahane, C., et al. 2011, A&A, 529, L3 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
- Cherchneff, I., & Glassgold, A. E. 1993, ApJ, 419, L41 [NASA ADS] [CrossRef] [Google Scholar]
- Coustenis, A., Jennings, D. E., Jolly, A., et al. 2008, Icarus, 197, 539 [NASA ADS] [CrossRef] [Google Scholar]
- Degli Esposti, C., Dore, L., Fusina, L., & Tamassia, F. 2013, Mol. Phys., 111, 896 [NASA ADS] [CrossRef] [Google Scholar]
- Dore, L. 2003, J. Mol. Spectr., 221, 93 [NASA ADS] [CrossRef] [Google Scholar]
- Dore, L., Degli Esposti, C., Mazzavillani, A., & Cazzoli, G. 1999, Chem. Phys. Lett., 300, 489 [NASA ADS] [CrossRef] [Google Scholar]
- Fonfría, J. P., Cernicharo, J., Richter, M. J., & Lacy, J. H. 2008, ApJ, 673, 445 [NASA ADS] [CrossRef] [Google Scholar]
- Fusina, L., Canè, E., Tamassia, F., & Lonardo, G. D. 2005a, Mol. Phys., 103, 3263 [NASA ADS] [CrossRef] [Google Scholar]
- Fusina, L., Tamassia, F., & Lonardo, G. D. 2005b, Mol. Phys., 103, 2613 [NASA ADS] [CrossRef] [Google Scholar]
- Herbst, E. 2003, Space Sci. Rev., 106, 293 [NASA ADS] [CrossRef] [Google Scholar]
- Herbst, E. 2005, J. Phys. Chem. A, 109, 4017 [CrossRef] [PubMed] [Google Scholar]
- Herman, M., Huet, T., Kabbadj, Y., & Auwera, J. V. 1991, Mol. Phys., 72, 75 [NASA ADS] [CrossRef] [Google Scholar]
- Jolly, A., Benilan, Y., Canè, E., et al. 2008, J. Quant. Spectr. Rad. Transf., 109, 2846 [NASA ADS] [CrossRef] [Google Scholar]
- Lacy, J. H., Evans, II, N. J., Achtermann, J. M., et al. 1989, ApJ, 342, L43 [NASA ADS] [CrossRef] [Google Scholar]
- Lafferty, W. J., & Lovas, F. J. 1978, J. Phys. Chem. Ref. Data, 7, 441 [NASA ADS] [CrossRef] [Google Scholar]
- Lahuis, F., & van Dishoeck, E. F. 2000, A&A, 355, 699 [NASA ADS] [Google Scholar]
- Matsumura, K., Tanaka, T., Endo, Y., Saito, S., & Hirota, E. 1980, J. Phys. Chem., 84, 1793 [CrossRef] [Google Scholar]
- Matsuura, M., Wood, P. R., Sloan, G. C., et al. 2006, MNRAS, 371, 415 [NASA ADS] [CrossRef] [Google Scholar]
- Mumma, M., DiSanti, M., Russo, N. D., et al. 2003, Adv. Space Res., 31, 2563 [NASA ADS] [CrossRef] [Google Scholar]
- Predoi-Cross, A., Herman, M., Fusina, L., & Lonardo, G. D. 2011, Mol. Phys., 109, 559 [NASA ADS] [CrossRef] [Google Scholar]
- Ridgway, S. T., Hall, D. N. B., Wojslaw, R. S., Kleinmann, S. G., & Weinberger, D. A. 1976, Nature, 264, 345 [NASA ADS] [CrossRef] [Google Scholar]
- Sandford, S. A., Bernstein, M. P., & Dworkin, J. P. 2001, MAPS, 36, 1117 [NASA ADS] [CrossRef] [Google Scholar]
- Wlodarczak, G., Demaison, J., Burie, J., & Lasne, M. C. 1989, Mol. Phys., 66, 669 [NASA ADS] [CrossRef] [Google Scholar]
- Woods, P. M., Millar, T. J., Zijlstra, A. A., & Herbst, E. 2002, ApJ, 574, L167 [NASA ADS] [CrossRef] [Google Scholar]
- Yamada, K. M., Birss, F., & Aliev, M. 1985, J. Mol. Spectr., 112, 347 [NASA ADS] [CrossRef] [Google Scholar]
- Yu, S., Drouin, B. J., & Pearson, J. C. 2009, ApJ, 705, 786 [NASA ADS] [CrossRef] [Google Scholar]
- Ziurys, L., Jr., W. B., Anderson, M., Fletcher, D., & Lamb, J. 1994, Rev. Sci. Instrum., 65, 1517 [NASA ADS] [CrossRef] [Google Scholar]
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.