Room temperature line lists for CO{}_{2} symmetric isotopologues with ab initio computed intensities

Room temperature line lists for CO symmetric isotopologues with ab initio computed intensities

Emil J. Zak, Jonathan Tennyson111To whom correspondence should be addressed; email:, Oleg L. Polyansky, Lorenzo Lodi Nikolay F. Zobov Sergei A. Tashkun, Valery I. Perevalov Department of Physics and Astronomy, University College London,
London, WC1E 6BT, UK
Institute of Applied Physics, Russian Academy of Sciences, Ulyanov Street 46, Nizhny Novgorod 603950, Russia V.E. Zuev Institute of Atmospheric Optics, SB RAS, 1, Academician Zuev Square, Tomsk 634021, Russia
July 13, 2019

Remote sensing experiments require high-accuracy, preferably sub-percent, line intensities and in response to this need we present computed room temperature line lists for six symmetric isotopologues of carbon dioxide: CO, CO, CO, CO, CO and CO, covering the range 0-8000 cm. Our calculation scheme is based on variational nuclear motion calculations and on a reliability analysis of the generated line intensities. Rotation-vibration wavefunctions and energy levels are computed using the DVR3D software suite and a high quality semi-empirical potential energy surface (PES), followed by computation of intensities using an ab initio dipole moment surface (DMS). Four line lists are computed for each isotopologue to quantify sensitivity to minor distortions of the PES/DMS. Reliable lines are benchmarked against recent state-of-the-art measurements and against the HITRAN2012 database, supporting the claim that the majority of line intensities for strong bands are predicted with sub-percent accuracy. Accurate line positions are generated using an effective Hamiltonian. We recommend the use of these line lists for future remote sensing studies and their inclusion in databases.

1 Introduction

Remote sensing of carbon dioxide for atmospheric applications requires a detailed knowledge of the rotational-vibrational spectra of all its major isotopologues. It is commonly believed that such measurements should be supported by reference line intensities of 1 accuracy or better XOCO (). This is the main requirement for successful interpretation of data from the NASA Orbiting Carbon Observatory 2 (OCO-2) space mission, which is designed to monitor the concentration of carbon dioxide in Earth’s atmosphere. As was shown in our previous papers considering the main CO isotopologue (denoted here as 626), a fully ab initio dipole moment surface is capable of providing such a level of accuracy jt613 (); 15ZaTePo.CO2 (). The next step is to address other isotopologues, which are ubiquitous in natural samples and may interfere with spectral lines of the main isotopologue as well as other species 13GaBaCa.CO2 (); 14KaCaMo.CO2 (); 15GeVaPh.CO2 (); 11GaPaLo.CO2 (). Concentration measurements of trace compounds also require very accurate line positions, intensities and line profiles of several isotopologues at the same time.

Experimental line-intensity measurements for isotopologues other than the main 626 one are much more challenging due to their low natural abundance, which ranges from 1% for CO (636) down to 10 % for the unstable CO (646). Enriched samples feature the need for precise (a priori) knowledge of isotopologue concentration. Therefore experimental accuracies of line intensities for less abundant isotopologues of carbon dioxide are in general lower than for the main isotopologue. A comprehensive source of spectroscopic data for carbon dioxide is the HITRAN database jt557 (). The 2012 release of this database contains line lists for the CO (636), CO (727), CO (828) and CO (838) isotopologues, all featuring spectral gaps because of lack of experimental data. Line intensities included in the database have uncertainties of 5-20%, thus well above current requirements. The database comprises both semi-empirical (taken from the pre-release of the CDSD database 08PeTa.CO2 (); 15TaPeGa.CO2 ()) and purely experimental entries. Multiple data sources are reflected by discontinuities in intensity patterns of some bands 15ZaTePo.CO2 (). Several measurements have been made since the last edition of the database, to pursue the elusive naturally abundant molecules, although these studies also have uncertainties well above the desired 1% threshold. The most accurate recent experiments by Devi et al. 16DeBeSu.CO2 (), Jacquemart et al. 12JaGuLy.CO2 (); 14BoJaLy.CO2 (); 15BoJaLy.CO2 (); 15JaBoLy.CO2 (), Karlovets et al. 14KaCaMo.CO2 () and Durry et al. 10DuLiVi.CO2 () address several bands of carbon dioxide isotopologues with unprecedented, though still unsatisfactory, intensity accuracies between 1% and 20%.

Among the few theoretical attempts to model high-resolution infrared spectra of carbon dioxide, the study by Huang et al. from the NASA Ames Research Center proved to be very accurate 12HuScTa.CO2 (); 14HuGaFr.CO2 (). Line lists from Huang et al. provide both line positions and intensities covering the infrared and visible spectral region () for room temperature (296 K) and 1000 K. Line positions, derived from a variational approach and based on semi-empirical potential energy surface (PES), are accurate to 0.03 – 0.2 cm. Although the Ames-1 line lists 12HuScTa.CO2 (); 14HuGaFr.CO2 () show the best agreement with experiment among all variational calculations, semi-empirical approaches based on effective Hamiltonians can provide line positions with an accuracy at least one order of magnitude better 08PeTa.CO2 (). On the other hand, effective Hamiltonian models strongly depend on the quality of the input data, thus the accuracy and completeness of this technique are limited by experiment.

A major advantage of the use of variational nuclear motion programs is that, within the limits of the Born-Oppenheimer approximation, line intensities can be computed with the same accuracy for all isotopolgues. In the present study the computation of line intensities was based on ab initio dipole moment surfaces (DMSs), and these were preliminarily tested by several authors 15ZaTePo.CO2 (); 15TaPeGa.CO2 (); 16DeBeSu.CO2 (). Some minor inaccuracies and discontinuities were discovered; however, comparisons showed overall good agreement with experiment. A comprehensive literature review on both experimental and theoretical approaches to line positions and intensities is given in the recent work by Tashkun et al. 15TaPeGa.CO2 (). In this study the authors indicate and support the need for a unified theoretical treatment of line positions and intensities; whereas the former are largely covered by experiments facilitated by effective Hamiltonian models 08PeTa.CO2 (), the latter still await high levels of accuracy, which we target in the present study. Due to lack of experimental data, a line list for the radioactive isotopologue CO is not included in the HITRAN2012 and CDSD-296 databases. The Ames-1 line list is presently a unique source of high accuracy spectra for this species.

The unstable CO isotopologue is of particular importance because of its usage in dating of biosamples and, more recently, in monitoring emissions, migrations and sinks of fossil fuel combustion products 10ReRaPo.CO2 (); 10LeNaKr.CO2 (); 10RoSiGu.CO2 () as well as for the assessment of contamination from nuclear power plants 08ToWaTa.CO2 (). Until recently, monitoring fossil fuel emission relied mostly on -decay count measurements or mass spectrometry, both of which are high cost, invasive methods.

Despite its low natural atmospheric abundance, radiocarbon dioxide has been probed via optical spectroscopy methods 15GeVaPh.CO2 (); 11GaPaLo.CO2 (); 15GiGaMa.CO2 (); 11GaBaBo.CO2 (). Recent advances in absorption laser spectroscopy provided an unprecedented tool for detection of species containing radiocarbon of ratios C/C down to parts per quadrillion. These measurements exploit saturated-absorption cavity ring down (SCAR) spectroscopy technique 10GiBaBo.CO2 () for the strongest fundamentals of CO 11GaPaLo.CO2 (); 11GaBaBo.CO2 (). The knowledge of accurate line intensities for several isotopologues at the same time is therefore a necessity for eliminating the unwanted noise sourced in traces of different isotopic carbon dioxide representatives. For instance the line of the 00011 – 00001 band in 646, which is dedicated for radiocarbon measurements, above certain temperatures, heavily interferes with the Lorentzian tail of the line in the 05511 – 05501 band of the 636 isotopologue 13GaBaCa.CO2 (). This raises difficulties in retrieving unbiased concentrations of the radioactive isotopologue. Similar problems occurred in measurements based on the line of the band of CO 15McOgBe.CO2 (). In both cases accurate values of line intensities are required. Otherwise, as shown in 15McOgBe.CO2 (), calculation of the fraction of C in measured samples that employed a line strength taken from a theoretical approach, led to over 35 % error in retrieved concentrations (as later confirmed by alternative experiments (AMS)). These observations were explained in terms of both inaccuracies of the line intensity and drawbacks of the spectroscopic fit model used, which fuels the need for reliable line intensity sources. Another successful technique further supporting this need was recently introduced by Genoud et al. 15GeVaPh.CO2 (), cavity ring-down spectroscopy with quantum cascade laser for monitoring of emissions from nuclear power plants. High quality line intensities for CO, CO and OCO are also required for real-time detection methods based on quantum cascade lasers to monitor C/C isotope ratios in identification of bio-geo-chemical origins of carbon dioxide emissions from the soil-air interface 16GuNuCh.CO2 (). Spectra of isotopologues can be used for a variety of different tasks such as the recent suggestion that observations of absorptions by CO in breath analysis provides a non-invasive means of diagnosing gastrointestinal cancers 16KiShKo.CO2 ().

In this work we aim to provide highly accurate line intensities in the 0 – 8000 cm spectral region together with reliable semi-empirical line positions for six symmetric isotopologues of carbon dioxide; five naturally abundant: 636, 727, 737, 828, 838 and one radioactive (646). An important advantage of a first principles theoretical approach is wide spectral coverage, in contrast to limited laser tuning capability of some measurements. For this reason databases like HITRAN, containing ro-vibrational spectra of small molecules, often utilize various experimental data sources, thereby giving up consistency of entries. This is not the case for the ab initio approaches, which are believed to provide consistent accuracy of line intensities within a vibrational band jt522 ().

Another issue related to post-processing of experimental data is the functional form of the Herman-Wallis factors. These, as arbitrarily chosen and empirically fitted, can become a source of unnatural biases for high transitions 15ZaTePo.CO2 (). The theoretical model implemented here should be inherently free from this problem, as the rotational contribution to line intensities is computed directly. The only underlying source of errors within the Born-Oppenheimer approximation is potential energy surface (PES) and dipole moment surface (DMS). The quality of both surfaces is assessed here by employing the line sensitivity analysis procedure introduced by Lodi and Tennyson jt522 (), which requires computation of at least four line lists for each isotopologue. This allows us to detect resonances 15ZaTePo.CO2 (), that affect line intensities and significantly diminish the reliability of data provided.

The final results are given in the form of line lists with associated uncertainties, which are available in the supplementary materials. Uniformity of errors (except for the regions affected by resonance interactions) accompanied by the precise reproduction of observed line intensities at the sub-percent level for the majority of strong bands 15ZaTePo.CO2 () suggests our results provide a viable update to the current, 2012 version of the HITRAN database.

2 Methodology

The Lodi-Tennyson methodology presented in detail elsewhere 15ZaTePo.CO2 (); jt522 () is used to validate line lists on a purely theoretical basis. For each isotopologue four line lists were computed, based on set of two PESs and two DMSs. These surfaces come from two sources: the semi-empirical Ames-1 PES and DMS from Huang et al. 12HuScTa.CO2 (), an ab initio PES and DMS (UCL DMS) computed by us, where the former one was subsequently fitted to observed levels (called below: Fitted PES). Details of all surfaces were presented before 15ZaTePo.CO2 (). These four high-quality surfaces are used in nuclear motion calculations to obtain rotational-vibrational energy levels, wavefunctions and line intensities.

2.1 Nuclear motion calculations

The strategy for solving the nuclear-motion problem employed here is analogous to the one presented in 15ZaTePo.CO2 (). In the Born-Oppenheimer approximation the PES and DMS are isotopologue independent. Therefore the only parameters that distinguish between different isotopologues are the nuclear masses entering the expression for the kinetic energy operator (KEO) of the nuclei. Our approach is based on an exact, within the Born-Oppenheimer approximation, KEO which is used in a two step procedure jt48 (); jt66 (); jt96 () of solving the nuclear Schrödinger equation. The first step involves solving the Coriolis-decoupled ro-vibrational motion problem for every quantum number combination separately to supply a basis for the second step, where the full ro-vibrational Hamiltonian is considered. The DVR technique implemented in the DVR3D suite jt338 () is used to represent the Hamiltonian matrix. Diagonalisation of this matrix provides rotational-vibrational energy levels and wavefunctions. In the present study we used symmetrized Radau coordinates and a bisector embedding to define nuclear degrees of freedom in the body-fixed coordinate system.

Nuclear masses for isotopes of carbon and oxygen were used: 11.996709 Da (C), 13.000439 Da (C), 14.000327 Da (C), 15.990525 Da (O), 16.995245 Da (O) and 17.995275 Da (O) 95AuWa.CO2 (). In the first step of the computation (program DVR3DJZ) the Born-Oppenheimer ro-vibrational wavefunctions were expanded in Morse-like oscillator basis functions for stretching coordinates and Legendre polynomials for the bending one; symmetrised Raudau internal coordinates were used. The converged DVR basis set associated with Gauss-Legendre quadrature points contained 30 radial and 120 angular functions, respectively. In the second step (program ROTLEV3b) we employed a dependent basis set of symmetry-adapted symmetric-top rotational functions. The ranges considered were chosen to match those present in the HITRAN2012 database (see Table 1). The same set of parameters was used to evaluate ro-vibrational energies computed from Ames-1 and fitted PESs. Calculation of line strengths used the DIPOLE program and require both DMS and ro-vibrational wavefunctions as input functions. Transformation from line strengths to transition intensities included scaling by natural isotopic abundance and multiplication by the appropriate spin statistical weights. Partition functions at 296 K were taken from Huang et al. 12HuScTa.CO2 () and they agree to better than 0.1% with partition functions from the present computation based on Ames-1 PES (see Table 1). A natural-abundance weighted intensity cut-off was then set to cm/molecule. In the case of the radioactive isotopologue (646) we assumed unit abundance and increased the cut-off value to cm/molecule.

2.2 Estimation of the intensity uncertainties

The ab initio DMS is a primary source of inaccuracies in line intensities. The accuracy of the UCL DMS has been proven to be at sub-percent level for several strong bands (stronger than cm/molecule) below 8000 cmjt613 (); 15ZaTePo.CO2 (). A key feature of using an ab initio DMS with a variational nuclear motion calculation is that entire vibrational bands are reproduced with similar accuracy. The reliability of line intensities obtained theoretically is correlated with the quality of -dependent ro-vibrational wavefunctions, hence with an underlying PES. Wavefunctions play an important role in capturing the interaction between different vibrational states. Such resonance interactions can lead to intensity stealing and, particularly for so-called dark states, huge changes in transition intensities.

Indeed, the sensitivity analysis performed for 626 15ZaTePo.CO2 () indicated that certain ro-vibrational energy levels of CO are vulnerable to interactions induced by Coriolis-type terms in the Hamiltonian. These resonances may change intensities of lines, particularly for weak transitions, by several orders of magnitude. This effect manifests itself especially when the perturbing band is strong. For this reason even minor inaccuracies in the PES in regions where such interactions occur can significantly change the intensity of lines, hence not reflecting the accuracy of the DMS. Thus, it is important to filter out bands or specific transitions with perturbed intensities which should not be trusted. A few such bands have been reported for the main isotopologue of CO (626) 15ZaTePo.CO2 (); 13HuFrTa.CO2 () and other isotopologues 14KaCaMo.CO2 (); 15BoJaLy.CO2 (); 15JaBoLy.CO2 ().

Here we adopt a scheme from our previous works (15ZaTePo.CO2, ; jt522, ), where a method of locating resonances was developed and tested on HO and CO. Cross-comparison of four line lists yielded an intensity scatter factor assigned to every line, which is defined as the ratio of the strongest to the weakest transition in a set of four intensities matching the same transition line. The four line lists read: Ames-1 PES and Ames DMS (named AA), Ames-1 PES and UCL DMS (named AU), Fitted PES and Ames DMS (named FA), Fitted PES and UCL DMS (named FU). Our base model, which should on theoretical grounds be the most accurate, is AU; it is from this model that our underlying uncertainties are drawn. For transitions involved in resonance interactions, calculations with different procedures should give markedly different results. The trustworthy line intensities should be stable under minor PES/DMS modifications, hence should feature a small scatter factor. Based on the statistics of the scatter factor we established arbitrary limits on for a line to be considered stable (), intermediate () and unstable (). These values are the same for all isotopologues. We believe that this descriptor gives a robust measure of sensitivity of line intensities to small PES changes, and hence reflects the reliability of a theoretically evaluated line intensity.

2.3 Line positions

As discussed above line positions for the “recommended UCL-IAO line list” are taken from the CDSD-296 database 15TaPeGa.CO2 (). These line positions were calculated within the framework of the effective Hamiltonian approach for which the partly-reduced polyad model was used 92TeSuPe.CO2 (); 98TaPeTe.CO2 (); 00TaPeTe.CO2 (). This model takes into account the resonance anharmonic, anharmonic+l-type and Coriolis interactions. The global weighted fits of the effective Hamiltonian parameters to the observed line positions collected from the literature were performed. The observations cover the 0.7 - 13 633 cm range, but for the rare isotopologues the ranges of the observations are considerably smaller. A review of the observed line positions used is given elsewhere 15TaPeGa.CO2 (). Each isotopologue was considered separately. In the case of isotopologues for which the observed line positions are scarce the effective Hamiltonian parameters obtained from the multi-isotopologue fitting 12Ta.CO2 () were used as an initial guess for further refinement of some of the parameters by separate fitting. The fitted sets of the effective Hamiltonian parameters reproduce the observed line positions practically within their experimental uncertainties, from 10 cm to 0.01 cm. The good predictive ability of the resulting effective Hamiltonian parameters has been demonstrated many times 14KaCaMo.CO2 (); 12JaGuLy.CO2 (); 14BoJaLy.CO2 (); 15BoJaLy.CO2 (); 13KaCaMo.CO2 (); 14KaCaMoII.CO2 (). The exceptions are several bands of the asymmetric isotopologues which are perturbed by the interpolyad resonance anharmonic interactions. Some of the examples are given in Refs.14KaCaMo.CO2 (); 13KaCaMo.CO2 (); 14KaCaMoII.CO2 (). Usually these perturbed bands are very weak.

2.4 Pseudo-experimental refinements

Energy levels taken from the effective Hamiltonian (EH) are generally considered to be accurate to 0.002 cm or better, which is usually more accurate than those given by PES based studies 15TaPeGa.CO2 (). Multi-isotopologue fits allowed for completeness of EH line lists even for less abundant isotopologues 15KaPe.CO2 (). From this reason our recommended line lists include line positions from the Effective Hamiltonian calculations provided by the CDSD-296 database 15TaPeGa.CO2 (). However, the very limited experimental data for CO did not allow us to extract EH parameters for this isotopologue. Therefore an alternative source of line positions is needed here.

Comparison of DVR3D (AMES-1 PES) line positions with EH values for the CO isotopologue shows that on average agreement between the two is at the 0.02 cm level. Within one vibrational band the residuals between EH and DVR entries remain almost constant. This observation suggests the viability of correcting the DVR3D line positions with respective differences for the main isotopologue. Such an approach has recently been shown to give excellent results for HO and HO jt522 ().

Thus, an attempt to correct DVR3D line positions with the effective Hamiltonian values was made. First, energy differences between corresponding EH and DVR energy levels for the main isotopologue were taken: . Next, each energy level of a given less abundant isotopologue was refined by adding respective difference to the DVR-computed value: . These refined energy levels were then compared to EH values. Application of the above procedure to symmetric isotopologues of CO resulted however in increased deviations between DVR and EH energy levels, hence should be considered here as unsuccessful. The reason for this is not entirely clear but the cited study for water jt522 () took considerable care over the corrections to the Born-Oppenheimer approximation while the results here were based on a PES simultaneously fitted to data from several isotopologues with no allowance for the beyond Born-Oppenheimer effects. For this reason pure DVR3D line positions were used in the recommended line list for CO.

3 Results and Discussion

Below we present an overview of our line lists. The next subsection contains statistical analysis of the scatter factor for each isotopologue, which will be further used in detecting resonances in the following subsection. After that, we compare our present results to recent highly accurate measurements, which were not included in the latest release of the HITRAN database. Next, a detailed comparison with the HITRAN2012 and CDSD-296 databases is performed. Finally we discuss the radioactive 646 isotopologue in the environmental context, as one of possible applications of present results.

3.1 Overview

Table 1 contains general information about our line lists.

Isotopologue 636 646 727 737 828 838
ZPE [cm] 2483.08 2436.75 2500.75 2447.50 2469.05 2415.39
J 119 130 99 50 101 50
Spin factors (ortho:para) 2:0 7:0 15:21 30:42 1:0 2:0
Q(This work) 576.652 2033.395 10 902.24 21 758.08 323.438 644.754
Q(CDSD-296) 576.652 N/A 10 971.90 22 129.96 323.418 652.234
Q(Ames-296) 576.644 2033.353 10 971.91 22 129.96 323.424 652.242
Q(HITRAN) 578.408 N/A 11 001.67 N/A 324.211 653.756
No. lines (This work) 68 635 41 610 6530 1501 10 441 2637
No. lines (CDSD-296) 68 640 N/A 6530 1500 10 444 2635
No. lines (Ames-296) 68 739 42 072 6545 1634 10 531 3050
No. HITRAN lines 68 856 N/A 5187 N/A 7070 121
No. HITRAN matches 68 856 N/A 5187 N/A 7069 121

Zero point energy based on the Ames-1 PES; 2015 Edition of CDSD 15TaPeGa.CO2 (); 12HuScTa.CO2 (); TIPS-2011 11LaGaLa.CO2 (); HITRAN2012 abundances were taken from Ref. 12HuScTa.CO2 (); For cm/molecule intensity cut-off for the 646 isotopologues and cm/molecule after scaling for natural abundance for the other isotopologues; UCL-IAO line list with cm/molecule intensity cut-off was used in the comparison.

Table 1: General information on computed room temperature (=296 K) line lists.

Partition functions in this work were calculated using Ames-1 PES, and these are compared to HITRAN2012, Ames and CDSD-296 line lists. We can see from the Table 1 that for isotopologues: 636, 646 and 828 the agreement between Ames work and our values is at level, as expected from runs based on the same PES. Partition functions calculated by us should however be treated as provisional for the 737 and the 838 isotopologue, as -range employed here did not allow for full convergence of the partition function. On average, the computed partition functions agree excellent with CDSD-296, and are systematically shifted by - with respect to HITRAN2012. This fact must be taken into account in comparisons aimed at sub-percent accuracy of line intensities. For line intensity calculations we used Ames partition functions from Huang et al. 12HuScTa.CO2 (). The HITRAN2012 database has significant spectral gaps for less abundant isotopologues, which are all covered by our line lists. Lines present in HITRAN2012 were completely matched to our lines using the energy level comparison technique.

3.2 Scatter factor statistics

Figure 1 gives an overview of the scatter factor statistics for all isotopologues considered. It is readily seen that the majority of lines are classified as stable, that is have scatter factor less than 2.5 (marked in blue in Figure 1). For CO and CO all lines are stable. Line lists for CO and CO have 3.5% and 3.3% of unstable lines respectively, whereas the CO line list features only 0.5% of unstable lines. Whenever a line-to-line match between a Fitted PES derived line and an Ames-1 based line was impossible by our automatic procedure due to ambiguity in matching of energy levels, manual attempts were made. Nevertheless a small fraction of lines remained unmatched, resulting in ’unknown’ scatter factors; the numbers of such unmatched lines is small for all isotopologues. The blue dashed area denotes stable and strong lines ( cm/molecule), for which the most accurate HITRAN accuracy index was assigned (). The HITRAN uncertainty index value () equal to 8 corresponds to accuracy of line intensity better than 1%. Consequently, stands for 1 – 2% accuracy, stands for 2 – 5% accuracy, stands for 5 – 10% accuracy, stands for 10 – 20% accuracy and stands for line intensities accurate to 20% or worse.

Figure 1: Scatter factor statistics for six isotopologues of carbon dioxide. Respective colours denote percentages of lines classified to particular stability domain. The axis corresponds to percentage of total lines present in our line list. Black regions give percentage of stable and strong lines ( cm/molecule), for which the highest HITRAN intensity accuracy code was assigned ().

3.3 Resonances

Detailed information on the energetic distribution of the scatter factor may be extracted from a ’transition stability map’, which is a useful tool in searching for resonances, as exemplified in Figure 2, which presents an example of such a map for the 828 isotopologue. The advantage of this particular representation is that one gains a full overview of all energetic regions, where transition intensities appear to be sensitive to minor inaccuracies of the PES. These lines are marked as red dots in Figure 2.

Figure 2: Scatter factor map for the 828 isotopologue. Colour coding denotes respective classification of lines: blue stands for stable lines, orange for intermediate lines and red for unstable lines. The arrows indicate selected bands for which a -localized peak in the scatter factor is observed. The zoomed inset in right bottom corner shows the peak region of the scatter factor for the 12212 – 02201 band. Both P and R branches are affected by the interaction around .

Figure 2 also illustrates the general trend of decreasing stability of lines with increasing energy of states involved in a transition. This has been already observed for the main 626 isotopologue in 15ZaTePo.CO2 (). Sporadic red points localized in small energetic areas are indicative of -localized resonances, while long chains of unstable points suggest instability of whole bands. It is instructive to give a more detailed insight into resonances by plotting scatter factor as a function of quantum number for each band separately within a given polyad number change (). The quantum number is defined as equal to -J(lower energy level) for the P branch, J(lower energy level) for the Q branch, and J(lower energy level)+1 for the R branch. The polyad number for carbon dioxide is defined as , where are the vibrational quantum numbers of symmetric stretching, bending and asymmetric stretching, respectively.

Figure 3: Scatter factor distribution for selected bands of 828 with polyad change . Color code denotes classification of transition as stable (blue), orange (intermediate) or unstable (red), measured by the scatter factor.

In general bands with polyad number change equal to 1 () are stable. For three unstable bands were found: 23301 – 12202 , 11101 – 00001 and 11102 – 00001. The first of the three bands contain transitions for which upper energy levels (localized around a particular value) become energetically close to rotational states of some other vibrational state; in this case to levels from the 12212 state. This may lead to a strong resonance interaction between states. In the case of the last two bands, an intensity borrowing mechanism from the strong asymmetric stretching fundamental is responsible for the instability of line intensities around a particular (see Figure 3 and Figure 5). For , both 12212 – 02201 and 23301 – 02201 bands are subject to a -localized resonance, as depicted in Figure 6. This is due to mutual interaction of the upper levels of these bands, which are energetically close. For , the 22213 – 02201 band exhibits a weak -localised peak in the scatter factor around . The 31101 – 00001 band is weakly perturbed by interaction between the 31101 and 20012 states in the vicinity of . Bands with higher polyad change number () are in general less stable, following uniform distribution of the scatter factor.

Resonances occur when ro-vibrational energy levels of two or more states cross or nearly cross in the vicinity of a single value. A prominent example of near crossing situation is the 11101 – 00001 band, which is perturbed by the 00011 state (intrapolyad interaction). Because the 00011 – 00001 fundamental is very strong and the perturbed band is relatively weak, significant intensity stealing is observed. This case is depicted in Figure 4. The relative intensity representation supplied by Figure 4 leads to the immediate conclusion of unreliability on the theoretical line intensities of transitions affected by resonances.

Figure 4: Relative intensities plotted against HITRAN2012 line intensities for the 11101–00001 band for the 828 isotopologue. This is an example of a band involved in resonant Coriolis interaction. Blue, orange and red points denote stable, intermediate and unstable lines, respectively.

In Figure 4 colour coding shows the stability of the transition intensity. A J-localized resonance is visible around , clearly correlating with both high instability of lines (marked by red points) and large deviations from HITRAN2012 line intensities.

This quasi-singularity in line intensity occurs due to Coriolis interaction with the strong 00011–00001 band, which equally perturbs P and R branches of the 11101–00001 band, and manifests itself by intensity borrowing, which in turn leads to the strengthening of the P-branch and to suppression of the R-branch. This observation confirms our previous predictions for existence of such perturbation in the main isotopologue 15ZaTePo.CO2 (). For this reason, in the final recommended line list we replace line intensities perturbed by these Coriolis interactions with semi-empirical data from the CDSD-296 database.

A view of the 636 isotopologue in Figure 5 supports this thesis. Similar behaviour is observed for other isotopologues. The 636 case clearly shows that this type of interaction is branch-specific and -specific as illustrated in Figure 5.

Figure 5: Relative intensities plotted against HITRAN2012 line intensities for 11101–00001 band for the 636 isotopologue. This is an example of a band involved in resonant Coriolis interaction.

Another example of the intrapolyad interaction is the pair: 23301 (perturber) and 12212 – 02201 (perturbed band), for which we depict the intensities scheme in Figure 6.

Figure 6: Multidimensional graph characterising the 12212 – 02201 band of CO. The base plane depicts dependence of line intensities with bar height and color code measuring the value of the scatter factor. The far right plane represents dependence of energy levels of the perturbed state (12212) and perturber (23301), which happen to nearly overlap around . Left plane gives intensity ratios of lines taken from UCL-IAO line list and CDSD-296 database.

Figure 6 shows perfect correlation between line stability measured by the scatter factor and agreement with CDSD-296 line intensities, where large discrepancies surround the region of elevated scatter factor (marked with red filled triangles in Figure 6). Very similar behaviour for line positions of the 12212 – 02201 band was noted by Borkov et al. for 727 15BoJaLy.CO2 (), whose simple polynomial fit of the line positions resulted in a -localised quasi-singularity in deviation of line positions. In such cases, effective Hamiltonian calculations have proved to be very successful and should be trusted regardless of resonances 14KaCaMo.CO2 (); 15JaBoLy.CO2 ().

One would expect that at least some of the large deviations in line intensities (see Figures 5 and 6) can be assigned to the influence of a resonance. Indeed, the correlation between high deviations in intensity and high scatter factor values is strikingly high, and reliability of the data provided might be unresolvable in favor of either approach. Nevertheless, as many HITRAN2012 transitions comes from CDSD-296 semi-empirical calculations, one should expect them to be trustworthy. This behavior is common for all bands in our line lists. Therefore we may consider the scatter factors used as a legitimate measure of reliability of a theoretical line list.

In the recommended line lists given in the supplementary materials, we replace the intensities of lines identified as unstable with entries from the effective Hamiltonian calculations, which for these cases are much more reliable, being experimentally based. Line lists with ab initio intensities can be found in supplementary material in files named as ’UCL-IAO-296-isotopologue_ name.dat’.

3.4 Comparison with recent measurements

Numerous experimental line intensity data sources are available throughout the literature (see refs. 15TaPeGa.CO2 (); 11TaPe.CO2 () for a comprehensive review), of which only few have high precision. Our attention is therefore focused on the most recent and the most accurate measurements. We assume that up to 2011 all highly accurate measurements and computations are captured by the 2012 edition of HITRAN, which will be analysed below.

A notable advantage of our ab initio approach is constant accuracy of intensity of entire bands, which is also believed to be transferable between different isotopologues. This is because all line intensities are computed using the same PES and DMS. Assuming that non-Born-Oppenheimer corrections are negligible we should expect an accuracy of 1% or better for strong and stable bands of all symmetric isotopologues. These bands are defined as ones containing transitions stronger than cm/molecule at 100% abundance. For the weak stable and intermediate bands this accuracy reduces to 1 – 3%. Such levels of accuracy are generally beyond reach of current experimental techniques, especially for the less abundant species.

3.5 Isotopologue 636

Recently Devi et al. 16DeBeSu.CO2 () performed precise measurements of line intensities of the 626, 636 and 628 isotopologues of carbon dioxide in the 1.6  m region. Figure 7 compares our results and HITRAN2012 line intensities to these new experimental results. The HITRAN2012 data comes from the CDSD database. A significant systematic shift of and toward higher intensities is observed for both 30012 – 00001 and 30013 – 00001 band. An almost identical pattern is followed by our line intensities and the effective Hamiltonian calculations given under HITRAN2012 entries. Possible problems in measured line intensities were found at and . These transitions clearly stand out in the comparison pattern for both HITRAN and the present study. High tails of both bands are bent in a bow-like structure, behavior which has been already observed for the main isotopologue. We attribute such behaviour to limited flexibility of functional form assumed for the Herman-Wallis factors, when reducing the experimental data.

Less pronounced deviations in high region have been observed in the work by Benner et al. 16BeDeSu.CO2 (), where highly accurate measurements for the 2.06 m band of the main isotopologue were made. Comparison shows 0.5% agreement between the experiment and UCL-IAO line intensities for the 20013 – 00001 band for the main isotopologue 16BeDeSu.CO2 (), and systematic increase in intensity deviation from onwards to reach 1.5% deviation at . Both experiments (Devi et al. 16DeBeSu.CO2 () and Benner et al. 16BeDeSu.CO2 ()) utilized the same multispectrum nonlinear least squares curve fitting technique to retrieve line profiles and intensities. This similarity in high behaviour supports the thesis of potential problems with retrieval model used in experimental post processing.

Figure 7: Relative deviations (PS/Experiment) of line intensities from measurements by Devi et al. 16DeBeSu.CO2 () plotted against quantum number. Blue and red triangles denote the 300013 – 00001 band of the 626 isotopologue taken from HITRAN2012 and present study, respectively. Purple and green squares stand for line intensities of the 30012 – 00001 band of the 636 isotopologue taken from HITRAN2012 and present study, respectively. Orange and grey circles give the line intensities of the 30013 – 00001 band of the 636 isotopologue taken from HITRAN2012 and present study, respectively. Zero relative deviation means 100% agreement with Devi et al. 

The accuracy of the experiments by Devi et al. and the present calculations has been verified by very recent Cavity Ring-Down Spectroscopy measurements of CO lines by Kiseleva et al. 16KiMaSt.CO2 (). Their observed intensity of the P(6) line in the 30013 – 00001 band of the 636 isotopologue was found to be within 0.4% of both UCL and HITRAN line intensities. Further proof of the consistency between the experiment by Kiseleva et al. and the present study is the P(52) line of the 30014 – 00001 band of the main isotopologue (626), which was also compared and found to be only 0.17% from our predicted value. Both lines were measured with stated 1% uncertainty budget. This suggests that a similar, presumably sub-percent, accuracy for the line intensities provided here and by HITRAN2012 for the 30013 – 00001 band of the 636 isotopologue.

The 2010 experimental study by Durry et al. 10DuLiVi.CO2 () deserves special attention, as intensity uncertainties for measured bands of the 636 isotopologue are claimed at the 1% level. Figure 8 compares experimental line intensities from Durry et al. with HITRAN2004 jt350 (), HITRAN2008 jt453 () and 2008 release of the CDSD database 08PeTa.CO2 (); 11TaPe.CO2 (), as well as with our calculated values. A characteristic wave-like pattern is visible. As all four sources follow this envelope, but with different systematic shift, we conclude this pattern is an artifact of the results of Durry et al.. The points from present work are shifted toward most negative values of relative deviation, with average systematic shift of 2%. Intensity comparison for this band for the main 626 isotopologue 16BeDeSu.CO2 () supports the 1% accuracy our theoretical intensities. Therefore it would seem that the stated 1% uncertainty of Durry et al.’s measurements may be too optimistic.

Figure 8: Relative deviations of line intensities of the 20012 – 00001 band of the 636 isotopologue from measurements by Durry et al. 10DuLiVi.CO2 () plotted against quantum number for several databases. Sources considered are HITRAN2004 jt350 (), HITRAN2008 jt453 (), the 2008 release of CDSD 08PeTa.CO2 () and the present work. The 1% deviation region is represented by green edge-blurred strip.

3.6 Isotopologue 727

In recent measurements performed on O and O enriched samples, Jacquemart et al. 15JaBoLy.CO2 () measured several bands for the 727 isotopologue. The authors argue that only lines stronger than 10 cm/molecule are retrieved with ’good accuracy’ and this accuracy is also strongly dependent on the knowledge of isotopic abundances. Figure 9 compares intensities of different bands measured by Jacquemart et al. with our predictions. It is evident that lines weaker than cm/molecule give reduced accuracy, as statistical spread appears an order-of-magnitude larger than for the strong bands measured in this experiment. Hence the experimental results 15JaBoLy.CO2 () for the 30011 – 00001, 31112 – 01101 and 31113 – 01101 band should be considered with caution.

Figure 9: Relative intensities for several bands of the 727 isotopologue measured by Jacquemart et al. 15JaBoLy.CO2 ().

The intensities of the two strongest bands in the 2 m region, that is 30012 – 00001 and 30013 – 00001, are uniformly shifted by +10% with respect to experiment. As indicated by Jacquemart et al. (15JaBoLy.CO2, ), intensities of whole bands are strongly dependent on isotopologue abundance (reported as 22.27%), and this factor is considered to be the main source of possible systematic shifts with respect to other studies. Comparisons with previous measurements by Karlovets et al. 14KaCaMo.CO2 () were made, revealing the new measurements by Jacquemart et al. (15JaBoLy.CO2, ) to be on average 3 – 4% stronger. However, samples used by Karlovets et al. had very low abundance of 727 (0.04%), which resulted in large statistical error (15%) in the intensities. Therefore we conclude that with the current level of experimental control over systematic errors it is difficult to reliably refer to measurements better than 10% accuracy. Nonetheless, because theoretical line intensities have constant accuracy for whole bands (except resonances), they can be used to assess the precision of measurements. Small scatter of line intensities throughout these bands (marked red and cyan in Figure 9) confirms the claimed high precision (1%) of the measurement from Ref. (15JaBoLy.CO2, ) above cm/molecule,  2% between and ,  5% between and , and  20% below .

Figure 10: Relative intensities for several bands of the 727 isotopologue measured by Karlovets et al. 14KaCaMo.CO2 (). Intensities were scaled to unit abundance.

Figure 10 compares line intensities from the present work to the experimental data from Karlovets et al. 14KaCaMo.CO2 (). The low isotopic abundance of samples used in experiments and large stated uncertainty (15%) means that the comparison despite its large scatter is satisfactory. As for other isotopologues, the 00031 – 00001 band computed by us has an underestimated intensity (grey squares in Figure 10). Cyan and red points correspond to 30013 – 00001 and 30012 – 00001 bands, and these experimental points were used to relate the line intensities of these bands in the study by Jacquemert et al..

3.7 Isotopologue 828

Recent CW-Cavity Ring Down experiments for enriched sample of the CO isotopologue by Karlovets et al. 14KaCaMoII.CO2 () cover the spectral range of all previous measurements for transitions. The study comprises 2870 lines from 59 bands in the 5851 – 6990 cm region and was recorded for 25.45 % abundance. Crude experimental data was fitted with an effective operator model to take into account another accurate experimental dataset from Toth et al. 07ToMiBr.CO2 (), which has been also included in the 2012 release of the HITRAN database. The estimated 10% uncertainty of the line intensities is the most accurate claim up-to-date. For a detailed review of previous measurements for this isotopologue see Refs.14KaCaMoII.CO2 (); 15TaPeGa.CO2 () and references therein. Here, highly enriched sample allowed for more precise measurements than in the 727 isotopologue case. Figure 11 compares line intensities of the three strongest bands measured by Karlovets et al. to present study. The 30012 – 00001 and 30003 – 00001 bands remain within deviation range, which suggest that the stated experimental uncertainty of 10 % is actually too pessimistic. Our intensities for the 00031 – 00001 band are shifted down by 14 %, similar to other isotopologues. The recommended line list uses line intensities from CDSD-296 for this band.

Figure 11: Relative intensities for several bands of the 828 isotopologue measured by Karlovets et al. 14KaCaMoII.CO2 (). Intensities were scaled to unit abundance.

Above results for 636, 727 and 828 isotopologues are summarized in Table 2.

Iso. Band Strength acc. (%) (%) (%) Strength acc. (%)
Karlovets et al. (2013) 13KaCaMo.CO2 () UCL-IAO
727 30012–00001 64 3-20 +17 13 64 1
30013–00001 58 3-20 +13 12 58 1
Jacquemart et al. (2015) 15JaBoLy.CO2 ()
727 30012–00001 85 20 +11 2 85 1
30013–00001 93 20 +9 2 93 1
31113–01101 130 20 +17 15 130 3
Karlovets et al. (2013) 13KaCaMo.CO2 ()
828 30012–00001 64 10 -2 2 64 1
30013–00001 81 10 -2 3 81 1
00031–00001 80 10 -13 5 80 20
Devi et al. (2016) 16DeBeSu.CO2 ()
636 30012–00001 55 10 +4 3 55 1
30013–00001 47 10 +8 15 47 1
Table 2: Characterization of selected vibrational bands of three symmetric CO isotopologues. Given for each band and each reference are the number of lines in the band, accuracy declared in the reference, average systematic shift (: average residual with respect to present study), average statistical dispersion ( ) and the total band strength in cm/molecule. The last column (marked UCL-IAO) contains the data from the present study, the total number of lines in the band, suggested accuracy for the band (in %) and the total band strength in cm/molecule.

3.8 Comparison with HITRAN2012, Ames and CDSD-296

The HITRAN2012 database comprise line lists for 636, 727, 828 and 838. Uncertainty indices of the line positions range from 2 ( 0.01 cm and 0.1 cm) to 9 ( cmand cm). In general, line positions from the latest version of CDSD-296 are very close to the line positions given in HITRAN2012 and have uncertainties corresponding to indices ranging from 3 to 9 depending on spectral region and quality of underlying experimental entries. Intensities provided by the current release of HITRAN for symmetric isotopologues of carbon dioxide come from two main sources: experiment (JPL OCO line list) by Toth et al. 08ToBrMi.CO2 () and the majority of transitions from a previous version of CDSD. The estimated uncertainties for all CDSD intensities is given as 20 % or worse in HITRAN (uncertainty code 3). However, this number does not reflect the actual uncertainties of the intensities. Most of the HITRAN intensities have the uncertainties much better than 20%. More detailed information about the actual uncertainties can be found in the official release of CDSD 15TaPeGa.CO2 (), which can be used to get more realistic information about the uncertainties of the line parameters.

Intensities from Toth et al.are supposed to be accurate to better than 2% (uncertainty code 7) or 5% (code 6). As discussed elsewhere 15ZaTePo.CO2 (), the stated uncertainty estimates of all current entries are insufficiently accurate for remote sensing applications. In addition to that, several bands feature unrealistic jumps in line intensities originating from switching data sources. Therefore a unified approach giving line positions of spectroscopic quality combined with significantly more accurate transition intensities is needed. In the present paper we aim in fulfilling these requirements.

In order to relate results from the present study to data given in HITRAN we compared line intensities for matched lines between the two line lists (see Table 1). As a primary measure of relative intensity deviation from HITRAN data we used the following formula:


where stands for line intensity from UCL-IAO line list given in cm/molecule and is HITRAN2012 intensity.

This measure is adequate for small deviations but poorly illustrates highly discrepant intensities, due to its asymmetric functional form. For larger deviations, especially for line intensities weaker than HITRAN by more than 100%, the quasi-symmetry is noticeably broken, resulting in a biased picture. In such cases, for example to show graphically a general overview, we decided to use a symmetrized measure to account for proper representation of large deviations:


This measure, in turn, yields far from intuitive numbers near deviation.

3.8.1 Isotopologue 636

The HITRAN2012 line list for the second most abundant 636 isotopologue contains 68 856 lines below 8000 cm. There are two sources of line intensities: the majority of lines taken from the 2008 version of the CDSD-296 database 08PeTa.CO2 () and two bands (20012–00001 and 20013–00001) from high precision measurements by Toth et al. 08ToBrMi.CO2 (). All lines present in the HITRAN2012 database for this isotopologue were matched to our line list with a root mean squared deviation (RMSD) of 0.04 cm. Lines that lay far in intensity from our predictions (vide infra) were double checked by manual investigation.

Figure 12: Left panel represents symmetric relative deviation for the 636 isotopologue for the two different sources (Perevalov et al. 08PeTa.CO2 () and Toth et al. 08ToBrMi.CO2 ()) from the HITRAN2012 database. Right panel is a zoomed image in the region of high accuracy () measurement by Toth et al. . Dashed green line indicates 5% limit of deviation tolerance associated with . Two bands measured by Toth et al. are marked with arrow

An overview from Figure 12 reveals the rather typical situation of funnel shaped relative deviation plot. By zooming into the region of high accuracy measurement by Toth et al., one can clearly see that all lines (marked with blue filled triangles in the right panel of Figure 12) remain within the claimed 5% uncertainty, additionally exhibiting a very narrow spread.

3.8.2 Isotopologue 727

HITRAN2012 line list for the 727 isotopologue contains 5187 lines below 8000 cm, all of which were taken from the effective Hamiltonian calculations by Tashkun and Perevalov 12TaPe_dip.CO2 (). Figure 13 compares our line intensities (all stable) to HITRAN2012; we observe the majority of line intensities display a systematic shift of -6% with respect to those recommended by HITRAN. Here again, noticeable arc structures appear. Similar behaviour was observed for the main 626 isotopologue. Although most of arcs are rather flat, there are a few bands which arc structure extends over a wide deviation range. Such occurrences may be caused by insufficiently flexible functional form of the Herman-Wallis factors employed to reduce experimental data for those bands, resulting in inaccurately retrieved experimental line intensities, especially for high s. These serve as an input to the effective Hamiltonian calculations (CDSD, hence HITRAN), thus artifacts of experimental analysis are likely to be propagated within the EH approach.

We have already shown that inaccuracies of our model are largely reflected in systematic shifts of whole bands, rather than statistical scatter, which is assumed to remain almost constant as a function of . Two bands in Figure 13 lie outside the tolerance given by the HITRAN2012 uncertainty code 3. These are: the 00031 – 00001 band and the 30013 – 00001 band (both indicated with arrows in Figure 13). The discrepancy for the former band has been explained in terms of rather poor reproduction of the 3 series of bands by our DMS and needs to be replaced in our recommended line list. The behavior of the latter band however is not clearly understood at this stage and requires further investigation. Our working hypothesis is that the 6% systematic shift applies to all bands, hence the 30013 – 00001 band when shifted by +6%, should match the 20% tolerance region, which is also regarded as provisional. New measurements by Karlovets et al. 14KaCaMo.CO2 () and Jacquemart et al. 15JaBoLy.CO2 () analysed in the previous section improved the quality of the line positions and intensities for the 30013 – 00001 band.

Figure 13: Relative intensities (cf. eq. (2)) plotted against HITRAN2012 line intensities for the 727 isotopologue. Green dashed horizontal line represents deviation from HITRAN2012 data equal to %.

3.8.3 Isotopologue 828

HITRAN2012 line list for the 828 isotopologue contains 7071 lines below 8000 cm. There are three sources of line intensities: 6280 lines taken from CDSD-296 08PeTa.CO2 () with equal to 3 and 4, 722 lines taken from a 1994 update to older variational calculations 92RoHaWa.CO2 () with equal to 2, and finally 69 lines taken from measurements by Toth et al. 08ToBrMi.CO2 () with ier assigned to 3. Figure 14 compares intensities from the present study to HITRAN2012 data. Despite the low uncertainty index, line intensities originating from Rothman et al. 92RoHaWa.CO2 () agree within with our results. Transitions around 2.06 m measured by Toth et al. 08ToBrMi.CO2 () are enclosed in 10% region reflecting the ier value for this set. Data points originating from CDSD-296 are divided into two sets with differing uncertainty index. The more accurate subset (marked with orange rotated crosses) is clearly squeezed along the relative deviation axis and exhibits almost no systematic shift. In contrast, the lower accuracy subset from CDSD spreads over a large region in relative deviation space. This suggests that both sets were calculated with separate input parameters of different quality. The 30013 – 00001 band () deviates around +2% from CDSD predictions, while the relatively strong 00031 – 00001 band () lies 11% below the zero deviation line (visible in Figure 14). It should be noted that large deviations of the lower accuracy CDSD-296 data () occur for very weak lines, for each the respective experimental data to fit the effective dipole moment parameters are absent. In these cases the parameters of the principal isotopologue were used in CDSD-296.

Figure 14: Relative intensities from the present study plotted against HITRAN2012 line intensities for the 828 isotopologue. Only region is depicted. Dashed grey and green lines correspond to 10% and 20% deviation, respectively. Blue crosses correspond to a subset of lines taken from Perevalov et al. 08PeTa.CO2 () which has been assigned to . Consequently, rotated orange crosses represent from the same reference. Red filled triangles refer to Rothman et al. 92RoHaWa.CO2 (), while purple filled squares stand for the small set of lines provided by Toth et al. (08ToBrMi.CO2, ).
Figure 15: Symmetric relative intensities (cf. eq. (2)) plotted against HITRAN2012 line intensities for the 828 isotopologue. Only region is depicted. Blue crosses correspond to a subset of lines taken from Perevalov et al. 08PeTa.CO2 () which has been assigned to . Consequently, rotated orange crosses represent from the same reference. Red filled triangles refer to Rothman et al. 92RoHaWa.CO2 (), while purple filled squares stand for the small set of lines provided by Toth et al. (08ToBrMi.CO2, )
Figure 16: Symmetric relative intensities (cf. eq. (2)) plotted against CDSD-296 line intensities for the 828 isotopologue. Only region is depicted.

Figure 15 shows that all strong lines ( cm/molecule) follow funnel shape envelope, thereby reflecting the typical relation between intensity and accuracy of lines. However several weaker lines, which constitute whole bands, align in wide arc structures with large systematic shift. This is particularly visible for lowered accuracy lines from HITRAN2012 (blue crosses in Figure 15). These lines were directly incorporated from HITRAN2008. The current release of the CDSD database improved on accuracy of these weak lines. A comparison between UCL and CDSD-296 intensities is given in Figure. 16.

3.8.4 Isotopologue 838

Only limited data are available for the 838 isotopologue in the 2012 edition of HITRAN. 121 lines measured by Toth et al. 08ToBrMi.CO2 () have uncertainty flag 3 and cover three bands in the 2 m region: 20011 – 00001, 20012 – 00001 and 20013 – 0000. All lines present in this set are matched to our line list with a RMSD cm. Here, similar to the 727 case, a systematic shift of around 10% is visible. This causes three transitions to breach the stipulated accuracy tolerance. Nevertheless, this should be considered as rather illusory due to the systematic shift of lines coming from all three bands. Figure 17 shows calculated intensities relative to HITRAN2012, where all computed lines are classified as stable.

Figure 17: Relative intensities plotted against HITRAN2012 line intensities for the 838 isotopologue. The triangles represent the 121 lines measured by Toth et al. (08ToBrMi.CO2, ) and included in the current version of HITRAN.

3.8.5 Overview

A natural question to ask is if accuracy of our computational scheme based on ab initio DMS holds at the same level for all symmetric isotopologues. The current status of experimental accuracy does not give a definite answer to this question and there is a clear need for high accuracy measurements. In the meantime we formulate a weaker query: do line intensities for a chosen band maintain similar relative deviation from consistent, highly accurate experimental data source for all symmetric isotopologues? Unfortunately, HITRAN2012 contains no such band. Arguably the most important band from an astrophysical and atmospheric measurements perspective is the 20012 – 00001 band, located in the 2 m wavelength region. A comparative study for this band for different CO symmetric isotopologues is therefore given below in Figure 18.

Figure 18: Relative intensities plotted against HITRAN2012 line intensities for the 20012 – 00001 band for four symmetric isotopologues. Red filled squares represent lines (636) measured by Toth et al.08ToBrMi.CO2 () appearing with . The remaining lines have code .

It is instructive to follow changes in relative intensity deviation among different isotopologues for the selected band. Two data sources were used for this band: a small set of low lines from experiment by Toth et al. 08ToBrMi.CO2 () for the 636 isotopologue (given uncertainty index 6) and CDSD-296 for rest of the lines (). All lines compared above match the stipulated HITRAN uncertainty, that is lines with fit the 5% tolerance, and the rest of the lines are 20% or less away from HITRAN2012 values. Minor discontinuity related to change of source of data is seen for the 636 isotopologue. We conclude that the results illustrated in Figure 18 give a tentative validation of the consistency of our approach with the analysed database. Relatively good overall agreement between our line list and HITRAN2012, revealing only sporadic deviations that exceed the claimed HITRAN accuracy, but yet justified and facilitated with comparisons with recent and highly accurate measurements, allow us to draw a conclusion that replacing current HITRAN line intensities with our computed values would significantly increase the accuracy, reliability and consistency of the database.

3.8.6 Ames-1

In table LABEL:table:Ames we present comparison of root-mean-square-residuals of intensities between Ames-1 DMS, UCL DMS and CDSD-296 for 14 strongest bands of CO for six symmetric isotopologues. By looking at a given isotopologue, a general trend is that the perpendicular bands () are in worse agreement with CDSD than the parallel bands. On average, UCL-IAO based band intensities are in better agreement with CDSD than Ames for 626 and 636. the 828 isotopologue exhibits a similar level of agreement, and larger deviations for UCL-IAO bands are observed for 727, 838 and 737. This may have two causes: a) The UCL treatment does not include any beyond Born-Oppenheimer correction, which may be a source of errors for other than main isotopologue, against which the DMS was benchmarked; b) CDSD entries, as experimentally tuned, are less accurate for less abundant isotopologues, and derived uncertainties do not allow us to judge in favour of either DMS. On balance we believe the second explanation is more likely.

Table 3: DMS statistics for 14 strongest carbon dioxide bands for six symmetric isotopologues. Numbers in columns correspond to root-mean-square-deviations of band intensities from the CDSD-296 database.

3.9 Radioactive isotopologue

Due to its trace atmospheric abundance, 10LeNaKr.CO2 (), only the strongest ro-vibrational absorption lines of radiocarbon dioxide (CO, 646) are accessible to accurate measurements. There are only 36 lines (all belonging to the 00011–00001 band) which have intensities above 10 cm/molecule at room temperature, of which only line (2209.10 cm) is located in a spectral region free of major interferences from other abundant atmospheric species like HO or CH. For this reason, this line is most commonly chosen as a reference for determination of radioactive carbon concentrations. Therefore, the line of the asymmetric stretching fundamental plays a distinct role in monitoring of carbon dioxide emission caused by fossil fuel combustion.

Although knowledge of the absolute value of the line strength to obtain the C concentrations in SCAR measurements performed on fossil samples 13GaBaCa.CO2 () can be avoided by using a more convoluted experimental procedure, encouraged by a successful retrieval of natural abundance of 646 by utilizing theoretically calculated line intensity (claimed 5% accurate) by Galli et al. 11GaBaBo.CO2 (), we hope that our updated and plausibly sub-percent accurate intensities will be utilized in future experiments as a reference or calibration data. Usually, a sample to be analysed is cooled down to 195 or 170 in order to diminish interference effects from the nearby (separated by 230 MHz) line of the 636 isotopologue ( line of the 05511 – 05501 band). For this reason attention is also paid to line intensities at low temperature for this particular transition. Table 4 compares intensities of the and lines obtained from several measurements and theoretical calculations together with their respective uncertainties.

Reference Temperature Strength(uncertainty) cm/molecule
Galli et al. 11GaBaBo.CO2 () 195
Present study 195
Genoud et al. 15GeVaPh.CO2 () 295
Present study 295
Present study 170
McCartt et al. 15McOgBe.CO2 () 300
Present study 300
Table 4: Intensities of the and lines of the 00011 – 00001 band for CO taken from different experimental sources.

Both and lines are considered stable according to our sensitivity analysis (). Line intensity given by Galli et al. agree to 1% with our value for 195. Genoud et al. gives room temperature line intensity flagged with 10% uncertainty, which lies 11% below our prediction. The line is 5 times stronger than , however the latter one is located in a less crowded spectral region. From this reason McCartt et al. used the line to produce calibration curve for concentration of radioactive carbon in the SCAR technique, where reference concentrations were determined by accelerator mass spectrometry. In their spectroscopic model, McCartt et al. use a line intensity at 300 K taken from measurements by Galli et al. 11GaBaBo.CO2 () (9% above UCL-IAO intensity) and line intensities of interfering isotopologues from the HITRAN2012 database. This leads to negative concentrations resulting from fitted calibration curve. One of the possible reason for that could be inaccurate line strength used in the retrieval model. Of equal importance are however: the accuracy of C abundance in samples and the intensities of the satellite lines of other carbon dioxide isotopologues. Here we provide line intensities which are internally consistent and proved to agree within experimental uncertainty to state-of-the-art measurements. Table 4 also lists our prediction for the line intensity at 170 K, a temperature which is commonly used for intensity measurements for the line.

Vibrational assignments of the UCL line list for 646 were based on isotopic shifts of energy levels and respective assignments for the 626 and 636 isotopologues. After that, a comparison of the DVR3D line positions to experimental frequencies by Dobos et al. 89DoWiKl.CO2 () was made. The tunable diode laser measurements supplied accuracy of 0.001 cm or better in the 2229 – 2259 cm spectral range of the asymmetric stretching fundamental; this yields an RMSD cm. This result shows that calculated line positions deviate from experiment just above the stated experimental accuracy, hence may be considered as highly reliable for the 00011 – 00001 band. For this band the average deviation from the EH calculations for 5 symmetric isotopologue levels is 0.018 cm, which could probably be reduced by treatment of mass-dependent non-Born-Oppenheimer effects. A more recent study performed by Galli et al. 11GaPaLo.CO2 (), where high-resolution optical-frequency-comb-assisted cavity ring-down technique was used to measure ro-vibrational line positions in 2190 – 2250 cm region with accuracy of few MHz. Comparison with this study resulted in 0.005 cm RMSD, thereby establishing the provisional uncertainty of the DVR3D line positions to 0.005 cm for the asymmetric stretching fundamental. The study by Galli et al. awaits accurate intensity evaluation. This creates an opportunity for further utilization of our results and comparison with experiments, when done.

The 3 family of bands discussed in ref. 15ZaTePo.CO2 () and in the preceding sections of this article, has been proven to be on average 12% too weak in present calculations. For isotopologues other than the radioactive CO intensities for these bands were replaced with CDSD-296 entries. For CO these intensities were scaled by 1.12 to correct for the systematic differences known from other isotopologues.

3.10 Recommended line lists

For all six isotopologues two types of line lists were prepared. First, files named ’UCL-296-isotopologue_ name.dat’ contain line positions calculated using Ames-1 PES with DVR3D program and line intensities using UCL DMS. Each line is supplemented with the appropriate scatter factor, given in the last column (see supplementary materials). Vibrational assignments are taken from the newest version of the CDSD-296 database. The second set of line lists, called ”recommended UCL-IAO line list” borrows line positions from the effective Hamiltonian calculations (see section 2.3) whenever a match was possible between Ames-1 PES based line positions from UCL and the effective Hamiltonian values. In rare cases when such match could not be found, line positions were transferred from the CDSD-296 database. The scheme used for the line intensities is similar the one used for the main isotopologue. The bands and unstable lines were taken from the effective Hamiltonian calculations, and appropriate uncertainty indices were assigned. Intensities of stable lines belonging to bands stronger than cm/molecule (for unit abundance) were taken from UCL DMS calculations and assigned HITRAN uncertainty code 8 (i.e. accuracy of 1% or better). Stable lines belonging to parallel bands weaker than cm/molecule also come from UCL DMS computation and were given uncertainty code 7 (i.e. accuracy 1 – 3 %). Intermediate lines and stable lines belonging to perpendicular bands weaker than cm/molecule feature HITRAN uncertainty code 6 (i.e. accuracy 3 – 5%). All line positions and line intensities for which scatter factor was not assigned were taken from CDSD-296. This was the case for only 3700 weak lines in total for all isotopologues. Both types of line lists are given in the supplementary materials with appropriate explanation in text files. Abundances were taken from the HITRAN2012 database with intensity cut-off cm/molecule. For the radiocarbon isotopologue unit abundance was assumed and cm/molecule intensity cut-off cm/molecule.

4 Conclusion

In the present study we compute new line lists for six symmetric isotopologues of carbon dioxide: CO, CO, CO, CO, CO and CO. Detailed comparisons with both the theoretical and experimental works indicate the high accuracy of the line intensities resulting from our ab initio DMS. Sensitivity analysis of the line intensities performed here confirmed the existence of several resonance interactions already reported in the literature, altogether with predictions for new pairs of energy levels involved in strong interactions. We hope that the methodology presented and evaluated here will be of use in theoretical approaches to other molecules. Accurate line positions generated using an effective Hamiltonian combined with highly accurate line intensities give comprehensive line lists, which we recommend for use in remote sensing studies and inclusions in databases.

This paper completes our analysis of the transition intensities of symmetric isotopolgues of CO. We are currently analysing the transition intensities of the asymmetric isotopologues. This work raises some theoretical issues as the loss of symmetry has consequences for both the DVR3D nuclear motion calculations and the CDSD effective Hamiltonian studies. Results will be reported in the near future jtasym ().


This work is supported by the UK Natural Environment Research Council (NERC) through grant NE/J010316, the ERC under the Advanced Investigator Project 267219 and the Russian Fund for Fundamental Science. The authors acknowledge the use of the UCL Legion High Performance Computing Facility (Legion@UCL), and associated support services, in the completion of this work.


  • (1) C. E. Miller, D. Crisp, P. L. DeCola, S. C. Olsen, J. T. Randerson, A. M. Michalak, A. Alkhaled, P. Rayner, D. J. Jacob, P. Suntharalingam, D. B. A. Jones, A. S. Denning, M. E. Nicholls, S. C. Doney, S. Pawson, H. Boesch, B. J. Connor, I. Y. Fung, D. O’Brien, R. J. Salawitch, S. P. Sander, B. Sen, P. Tans, G. C. Toon, P. O. Wennberg, S. C. Wofsy, Y. L. Yung, R. M. Law, Precision requirements for space-based X-CO2 data, J. Geophys. Res. 112 (2007) D10314. doi:{10.1029/2006JD007659}.
  • (2) O. L. Polyansky, K. Bielska, M. Ghysels, L. Lodi, N. F. Zobov, J. T. Hodges, J. Tennyson, High accuracy CO line intensities determined from theory and experiment, Phys. Rev. Lett. 114 (2015) 243001. doi:10.1103/PhysRevLett.114.243001.
  • (3) E. Zak, J. Tennyson, O. L. Polyansky, L. Lodi, S. A. Tashkun, V. I. Perevalov, A room temperature CO line list with ab initio computed intensities, J. Quant. Spectrosc. Radiat. Transf. 177 (2016) 31–42. doi:10.1016/j.jqsrt.2015.12.022.
  • (4) I. Galli, S. Bartalini, P. Cancio, P. De Natale, D. Mazzotti, G. Giusfredi, M. E. Fedi, P. A. Mando, Optical detection of radiocarbon dioxide: First results and AMS intercomparison, Radiocarbon 55 (2013) 213–223.
  • (5) E. V. Karlovets, A. Campargue, D. Mondelain, S. Kassi, S. A. Tashkun, V. I. Perevalov, High sensitivity Cavity Ring Down spectroscopy of O enriched carbon dioxide between 5850 and 7000cm: Part III Analysis and theoretical modeling of the CO, OCO, OCO, OCO and OCO spectra, J. Quant. Spectrosc. Radiat. Transf. 136 (2014) 89–107. doi:10.1016/j.jqsrt.2013.11.006.
  • (6) G. Genoud, M. Vainio, H. Phillips, J. Dean, M. Merimaa, Radiocarbon dioxide detection based on cavity ring-down spectroscopy and a quantum cascade laser, Opt. Lett. 40 (2015) 1342. doi:10.1364/ol.40.001342.
  • (7) I. Galli, P. C. Pastor, G. Di Lonardo, L. Fusina, G. Giusfredi, D. Mazzotti, F. Tamassia, P. D. Natale, The band of C O molecule measured by optical-frequency-comb-assisted cavity ring-down spectroscopy, Mol. Phys. 109 (2011) 2267–2272. doi:10.1080/00268976.2011.614284.
  • (8) L. S. Rothman, I. E. Gordon, Y. Babikov, A. Barbe, D. C. Benner, P. F. Bernath, M. Birk, L. Bizzocchi, V. Boudon, L. R. Brown, A. Campargue, K. Chance, E. A. Cohen, L. H. Coudert, V. M. Devi, B. J. Drouin, A. Fayt, J.-M. Flaud, R. R. Gamache, J. J. Harrison, J.-M. Hartmann, C. Hill, J. T. Hodges, D. Jacquemart, A. Jolly, J. Lamouroux, R. J. Le Roy, G. Li, D. A. Long, O. M. Lyulin, C. J. Mackie, S. T. Massie, S. Mikhailenko, H. S. P. Müller, O. V. Naumenko, A. V. Nikitin, J. Orphal, V. Perevalov, A. Perrin, E. R. Polovtseva, C. Richard, M. A. H. Smith, E. Starikova, K. Sung, S. Tashkun, J. Tennyson, G. C. Toon, V. G. Tyuterev, G. Wagner, The HITRAN 2012 molecular spectroscopic database, J. Quant. Spectrosc. Radiat. Transf. 130 (2013) 4 – 50. doi:10.1016/jqsrt.2013.07.002.
  • (9) V. I. Perevalov, S. A. Tashkun, CDSD-296 (Carbon Dioxide Spectroscopic Databank): updated and enlarged version for atmospheric applications, Cambridge MA, USA, 2008.
  • (10) S. A. Tashkun, V. I. Perevalov, R. R. Gamache, J. Lamouroux, CDSD-296, high resolution carbon dioxide spectroscopic databank: Version for atmospheric applications, J. Quant. Spectrosc. Radiat. Transf. 152 (2015) 45–73. doi:10.1016/j.jqsrt.2014.10.017.
  • (11) V. M. Devi, D. C. Benner, K. Sung, L. R. Brown, T. J. Crawford, C. E. Miller, B. J. Drouin, V. H. Payne, S. Yu, M. A. H. Smith, A. W. Mantz, R. R. Gamache, Line parameters including temperature dependences of self- and air-broadened line shapes of CO: 1.6-m region, J. Quant. Spectrosc. Radiat. Transf. 177 (2016) 117–144. doi:10.1016/j.jqsrt.2015.12.020.
  • (12) D. Jacquemart, F. Gueye, O. M. Lyulin, E. V. Karlovets, D. Baron, V. I. Perevalov, Infrared spectroscopy of CO2 isotopologues from 2200 to 7000 cm: I—Characterizing experimental uncertainties of positions and intensities, J. Quant. Spectrosc. Radiat. Transf. 113 (2012) 961–975. doi:10.1016/j.jqsrt.2012.02.020.
  • (13) Y. G. Borkov, D. Jacquemart, O. M. Lyulin, S. A. Tashkun, V. I. Perevalov, Infrared spectroscopy of O- and O-enriched carbon dioxide: Line positions and intensities in the 3200–4700 cm region. Global modeling of the line positions of OCO and OCO, J. Quant. Spectrosc. Radiat. Transf. 137 (2014) 57–76. doi:10.1016/j.jqsrt.2013.11.008.
  • (14) Y. G. Borkov, D. Jacquemart, O. M. Lyulin, S. A. Tashkun, V. I. Perevalov, Infrared spectroscopy of O- and O-enriched carbon dioxide: Line positions and intensities in the 4681–5337 cm region, J. Quant. Spectrosc. Radiat. Transf. 159 (2015) 1–10. doi:10.1016/j.jqsrt.2015.02.019.
  • (15) D. Jacquemart, Y. Borkov, O. M. Lyulin, S. A. Tashkun, V. I. Perevalov, Fourier transform spectroscopy of CO isotopologues at 1.6m: Line positions and intensities, J. Quant. Spectrosc. Radiat. Transf. 160 (2015) 1–9. doi:10.1016/j.jqsrt.2015.03.016.
  • (16) G. Durry, J. S. Li, I. Vinogradov, A. Titov, L. Joly, J. Cousin, T. Decarpenterie, N. Amarouche, X. Liu, B. Parvitte, O. Korablev, M. Gerasimov, V. Zéninari, Near infrared diode laser spectroscopy of CH, HO, CO and their isotopologues and the application to TDLAS, a tunable diode laser spectrometer for the martian PHOBOS-GRUNT space mission, Appl. Phys. B 99 (2010) 339–351. doi:10.1007/s00340-010-3924-y.
  • (17) X. Huang, D. W. Schwenke, S. A. Tashkun, T. J. Lee, An isotopic-independent highly accurate potential energy surface for CO isotopologues and an initial CO infrared line list, J. Chem. Phys. 136 (2012) 124311. doi:10.1063/1.3697540.
  • (18) X. Huang, R. R. Gamache, R. S. Freedman, D. W. Schwenke, T. J. Lee, Reliable infrared line lists for 13 CO isotopologues up to E =18,000 cm and 1500 K, with line shape parameters, J. Quant. Spectrosc. Radiat. Transf. 147 (2014) 134–144. doi:{10.1016/j.jqsrt.2014.05.015}.
  • (19) C. H. Reick, T. Raddatz, J. Pongratz, M. Claussen, Contribution of anthropogenic land cover change emissions to pre-industrial atmospheric CO, Tellus B 62 (2010) 329–336. doi:10.1111/j.1600-0889.2010.00479.x.
  • (20) I. Levin, T. Naegler, B. Kromer, M. Diehl, R. J. Francey, A. J. Gomez-Pelaez, L. P. Steele, D. Wagenbach, R. Weller, D. E. Worthy, Observations and modelling of the global distribution and long-term trend of atmospheric CO, Tellus B 62 (2010) 26–46. doi:10.1111/j.1600-0889.2009.00446.x.
  • (21) K. A. Rose, E. L. Sikes, T. P. Guilderson, P. Shane, T. M. Hill, R. Zahn, H. J. Spero, Upper-ocean-to-atmosphere radiocarbon offsets imply fast deglacial carbon dioxide release, Nature 466 (2010) 1093–1097. doi:10.1038/nature09288.
  • (22) H. Tomita, K. Watanabe, Y. Takiguchi, J. Kawarabayashi, T. Iguchi, Radioactive carbon isotope monitoring system based on cavity ring-down laser spectroscopy for decommissioning process of nuclear facilities, J. Power Energy Systems 2 (2008) 221–228. doi:10.1299/jpes.2.221.
  • (23) G. Giusfredi, I. Galli, D. Mazzotti, P. Cancio, P. De Natale, Theory of saturated-absorption cavity ring-down: radiocarbon dioxide detection, a case study, J. Opt. Soc. Am. B 32 (2015) 2223. doi:10.1364/josab.32.002223.
  • (24) I. Galli, S. Bartalini, S. Borri, P. Cancio, D. Mazzotti, P. De Natale, G. Giusfredi, Molecular gas sensing below parts per trillion: Radiocarbon-dioxide optical detection, Phys. Rev. Lett. 107 (2011) 270802. doi:10.1103/physrevlett.107.270802.
  • (25) G. Giusfredi, S. Bartalini, S. Borri, P. Cancio, I. Galli, D. Mazzotti, P. D. Natale, Saturated-absorption cavity ring-down spectroscopy, Phys. Rev. Lett. 104 (2010) 110801. doi:10.1103/physrevlett.104.110801.
  • (26) A. McCartt, T. Ognibene, G. Bench, K. Turteltaub, Measurements of carbon-14 with cavity ring-down spectroscopy, Nuclear Instruments and Methods in Physics Research Section B: Beam Interactions with Materials and Atoms 361 (2015) 277 – 280. doi:
  • (27) C. Guimbaud, C. Noel, M. Chartier, V. Catoire, M. Blessing, J. C. Gourry, C. Robert, A quantum cascade laser infrared spectrometer for CO stable isotope analysis: Field implementation at a hydrocarbon contaminated site under bio-remediation, J. Environ. Sci. 40 (2016) 60–74. doi:10.1016/j.jes.2015.11.015.
  • (28) S. V. Kireev, S. L. Shnyrev, A. A. Kondrashov, Development of laser noninvasive on-line diagnostics of oncological diseases based on the absorption method in the 4860-4880 cm spectral range, Laser Phys. 26 (2016) 075601. doi:{10.1088/1054-660X/26/7/075601}.
  • (29) L. Lodi, J. Tennyson, Line lists for HO and HO based on empirically-adjusted line positions and ab initio intensities, J. Quant. Spectrosc. Radiat. Transf. 113 (2012) 850–858.
  • (30) J. Tennyson, TRIATOM, SELECT and ROTLEV - for the calculation of ro-vibrational levels of triatomic molecules, Comput. Phys. Commun. 42 (1986) 257–270.
  • (31) B. T. Sutcliffe, S. Miller, J. Tennyson, An effective computational approach to the calculation of vibration-rotation spectra of triatomic molecules, Comput. Phys. Commun. 51 (1988) 73–82.
  • (32) B. T. Sutcliffe, J. Tennyson, A general treatment of vibration-rotation coordinates for triatomic molecules, Intern. J. Quantum Chem. 39 (1991) 183–196.
  • (33) J. Tennyson, M. A. Kostin, P. Barletta, G. J. Harris, O. L. Polyansky, J. Ramanlal, N. F. Zobov, DVR3D: a program suite for the calculation of rotation-vibration spectra of triatomic molecules, Comput. Phys. Commun. 163 (2004) 85–116.
  • (34) G. Audi, A. H. Wapstra, The 1995 update to the atomic mass evaluation, Nucl. Phys. A 595 (1995) 409–480. doi:10.1016/0375-9474(95)00445-9.
  • (35) X. Huang, R. S. Freedman, S. A. Tashkun, D. W. Schwenke, T. J. Lee, Semi-empirical CO IR line lists for simulations up to 1500 K and 20,000 cm, J. Quant. Spectrosc. Radiat. Transf. 130 (2013) 134–146. doi:10.1016/j.jqsrt.2013.05.018.
  • (36) J. L. Teffo, O. N. Sulakshina, V. I. Perevalov, Effective Hamiltonian for rovibrational energies and line-intensities of carbon-dioxide, J. Mol. Spectrosc. 156 (1992) 48–64. doi:10.1016/0022-2852(92)90092-3.
  • (37) S. A. Tashkun, V. I. Perevalov, J. L. Teffo, L. S. Rothman, V. Tyuterev, Global fitting of CO vibrational-rotational line positions using the effective hamiltonian approach, J. Quant. Spectrosc. Radiat. Transf. 60 (1998) 785 – 801. doi:
  • (38) S. Tashkun, V. Perevalov, J.-L. Teffo, M. Lecoutre, T. Huet, A. Campargue, D. Bailly, M. Esplin, CO: Global treatment of vibrational–rotational spectra and first observation of the 21 + 53 and 1 + 22 + 53 absorption bands, J. Mol. Spectrosc. 200 (2000) 162 – 176. doi:
  • (39) S. Tashkun, Global multi-isotopologue fitting of CO vibrational-rotational line positions using a phenomenological mass dependent effective hamiltonian, Abstracts of the XVII Symposium on High Resolution Molecular Spectroscopy.Zelenogorsk, St.Petersburg region, Russia (2012) P.67.
  • (40) E. V. Karlovets, A. Campargue, D. Mondelain, S. Béguier, S. Kassi, S. A. Tashkun, V. I. Perevalov, High sensitivity cavity ring down spectroscopy of O enriched carbon dioxide between 5850 and 7000 cm: I. analysis and theoretical modeling of the OC spectrum, J. Quant. Spectrosc. Radiat. Transf. 130 (2013) 116 – 133. doi:
  • (41) E. Karlovets, A. Campargue, D. Mondelain, S. Kassi, S. Tashkun, V. Perevalov, High sensitivity Cavity Ring Down spectroscopy of 18O enriched carbon dioxide between 5850 and 7000 cm: Part II—Analysis and theoretical modeling of the CO, CO and OCO spectra, J. Quant. Spectrosc. Radiat. Transf. 136 (2014) 71 – 88. doi:
  • (42) E. V. Karlovets, V. I. Perevalov, The influence of isotopic substitution on the effective dipole moment parameters of CO molecule, Optics Spectrosc. 119 (2015) 16–21. doi:10.1134/s0030400x15070139.
  • (43) A. L. Laraia, R. R. Gamache, J. Lamouroux, I. E. Gordon, L. S. Rothman, Total internal partition sums to support planetary remote sensing, Icarus 215 (2011) 391–400. doi:10.1016/j.icarus.2011.06.004.
  • (44) S. A. Tashkun, V. I. Perevalov, CDSD-4000: High-resolution, high-temperature carbon dioxide spectroscopic databank, J. Quant. Spectrosc. Radiat. Transf. 112 (2011) 1403–1410. doi:10.1016/j.jqsrt.2011.03.005.
  • (45) D. C. Benner, V. M. Devi, K. Sung, L. R. Brown, C. E. Miller, V. H. Payne, B. J. Drouin, S. Yu, T. J. Crawford, A. W. Mantz, M. A. H. Smith, R. R. Gamache, Line parameters including temperature dependences of air- and self-broadened line shapes of CO: 2.06-m region, J. Mol. Spectrosc. 326 (2016) 21–47. doi:10.1016/j.jms.2016.02.012.
  • (46) M. Kiseleva, J. Mandon, S. Persijn, J. Petersen, L. Nielsen, F. J. M. Harren, Tractable line strength measurements of methane and carbon dioxide in the near infrared wavelength region at 1.65 m using cavity ring down spectroscopy, in: 13th ASA-HITRAN conference, Reims, 2016, pp. P1–16.
  • (47) L. S. Rothman, D. Jacquemart, A. Barbe, D. C. Benner, M. Birk, L. R. Brown, M. R. Carleer, C. Chackerian, K. Chance, L. H. Coudert, V. Dana, V. M. Devi, J.-M. Flaud, R. R. Gamache, A. Goldman, J.-M. Hartmann, K. W. Jucks, A. G. Maki, J.-Y. Mandin, S. T. Massie, J. Orphal, A. Perrin, C. P. Rinsland, M. A. H. Smith, J. Tennyson, R. N. Tolchenov, R. A. Toth, J. Vander Auwera, P. Varanasi, G. Wagner, The HITRAN 2004 molecular spectroscopic database, J. Quant. Spectrosc. Radiat. Transf. 96 (2005) 139–204.
  • (48) L. S. Rothman, I. E. Gordon, A. Barbe, D. C. Benner, P. F. Bernath, M. Birk, V. Boudon, L. R. Brown, A. Campargue, J. P. Champion, K. Chance, L. H. Coudert, V. Dana, V. M. Devi, S. Fally, J. M. Flaud, R. R. Gamache, A. Goldman, D. Jacquemart, I. Kleiner, N. Lacome, W. J. Lafferty, J. Y. Mandin, S. T. Massie, S. N. Mikhailenko, C. E. Miller, N. Moazzen-Ahmadi, O. V. Naumenko, A. V. Nikitin, J. Orphal, V. I. Perevalov, A. Perrin, A. Predoi-Cross, C. P. Rinsland, M. Rotger, M. Simeckova, M. A. H. Smith, K. Sung, S. A. Tashkun, J. Tennyson, R. A. Toth, A. C. Vandaele, J. Vander Auwera, The HITRAN 2008 molecular spectroscopic database, J. Quant. Spectrosc. Radiat. Transf. 110 (2009) 533–572.
  • (49) R. Toth, C. Miller, L. Brown, V. M. Devi, D. C. Benner, Line positions and strengths of OCO, OCO and OCO between 2200 and 7000 cm, J. Mol. Spectrosc. 243 (2007) 43–61. doi:10.1016/j.jms.2007.03.005.
  • (50) R. A. Toth, L. R. Brown, C. E. Miller, V. M. Devi, D. C. Benner, Spectroscopic database of CO line parameters: 4300–7000cm, J. Quant. Spectrosc. Radiat. Transf. 109 (2008) 906–921. doi:10.1016/j.jqsrt.2007.12.004.
  • (51) S. A. Tashkun, V. I. Perevalov, private communication: Intensities calculated using the effective dipole moment function (2012).
  • (52) L. S. Rothman, R. L. Hawkins, R. B. Wattson, R. R. Gamache, Energy levels, intensities, and linewidths of atmospheric carbon dioxide bands, J. Quant. Spectrosc. Radiat. Transf. 48 (1992) 537–566. doi:10.1016/0022-4073(92)90119-o.
  • (53) S. Dobos, G. Winnewisser, F. Kling, J. Mink, Improved spectroscopic constants for C O obtained from the band, Z. Naturforsch 44a (1989) 633–639.
  • (54) E. Zak, J. Tennyson, O. L. Polyansky, L. Lodi, N. F. Zobov, S. A. Tashkun, V. I. Perevalov, Room temperature line lists for CO asymmetric isotopologues with ab initio computed intensities, J. Quant. Spectrosc. Radiat. Transf. (2017) submitted.
Comments 0
Request Comment
You are adding the first comment!
How to quickly get a good reply:
  • Give credit where it’s due by listing out the positive aspects of a paper before getting into which changes should be made.
  • Be specific in your critique, and provide supporting evidence with appropriate references to substantiate general statements.
  • Your comment should inspire ideas to flow and help the author improves the paper.

The better we are at sharing our knowledge with each other, the faster we move forward.
The feedback must be of minimum 40 characters and the title a minimum of 5 characters
Add comment
Loading ...
This is a comment super asjknd jkasnjk adsnkj
The feedback must be of minumum 40 characters
The feedback must be of minumum 40 characters

You are asking your first question!
How to quickly get a good answer:
  • Keep your question short and to the point
  • Check for grammar or spelling errors.
  • Phrase it like a question
Test description