Small silicon carbide (SiC) clusters are hypothesized to be an integral step in the process that begins with the nucleosynthesis of carbon and silicon in small, carbonaceous asymptotic giant branch (AGB) stars and leads to the formation of SiC dust grains found in the interstellar medium (ISM) (Mélinon et al., 2007). Several steps along the process of formation from the atomic level to fractal aggregate dust grain structures are not entirely known (Matthews et al., 2007), but their aggregation is thought to have a direct impact on protoplanetary disk formation. Understanding the composition of stellar atmospheres and nebulae may lead to newfound insight into these processes of dust formation.

The only direct way to study interstellar dust grains is through chemical inspection of primitive chondrite meteorites which accreted before the formation of our Solar System. A chemical isolation technique for SiC dust grains found on primitive chondrite meteorites has long been established (Bernatowicz and Fraundorf., 1987; Nittler and Alexander, 2003) and has shown that SiC dust grains are prevalent in proto-planetary dust clouds. The prevalence of these grains on chondrite meteorites may indicate that SiC species should be targeted for observation in the unidentified infrared/microwave spectra of the interstellar medium.

In addition to terrestrial identification from meteorites containing proto-solar SiC dust grains, some SiC clusters have been accurately identified in stellar environments of carbonaceous AGB stars. The diatomic radical, SiC (Cernicharo and Gottlieb., 1989) along with the triatomic radical (Thaddeus et al., 1984) and closed-shell (Prieto et al., 2015) species of SiC₂ and Si₂C (Cernicharo et al., 2015), have all been identified in the circumstellar envelope of IRC+10216 (CW Leo). The only cyclic tetra-atomic species identified to date in the ISM is SiC₃ (Apponi and McCarthy., 1999a), which was also detected in the aforementioned star IRC+10216. These species have all been detected with rotational spectroscopy. Such observations suggest that the SiC chemistry of these astronomical regions may be richer than has been observed to date. However, the observations so far have been limited to molecules with permanent dipole moments allowing for their detection via rotational spectroscopy. With the new JWST, similar molecules without dipole moments, such as some tetra-atomic silicon carbide clusters (TASCCs), may now be observable by infrared spectroscopy, but the data needed to elucidate such spectra first need to be generated here on Earth.

To that end, the spectral data for the pure carbon cluster, rhomboidal (r-)C₄, has been extensively studied both experimentally (Algranati et al., 1989; Blanksby et al., 2000) as well as theoretically (Martin et al., 1996; Martin and Taylor, 1996; Varandas and Rocha, 2018; Wang and Whithey, 2018) at many different levels of theory including at the CCSD(T)/cc-pCV5Z level of theory by Wang and Bowman in 2013 (Wang and Bowman, 2013). In stepping into the silicon analogues of this molecule, cyclic SiC₃ includes two C _2v isomers, one exhibiting a transannular C-C bond and the other a transannular Si-C bond. The former will be referred to as diamond SiC₃, or d-SiC₃ hereafter. The d-SiC₃ isomer, in particular has been a focus of previous theoretical and experimental work as it is currently the only cyclic tetra-atomic species identified in the ISM (Apponi and McCarthy., 1999a). Thus, previous theoretical (Linguerri et al., 2006), experimental microwave spectroscopy (Apponi and McCarthy., 1999b; McCarthy et al., 2019), and astronomically-observed (Apponi and McCarthy., 1999a; McCarthy et al., 2019) spectral data are available. The isomer of SiC₃ with a transannular Si-C bond, which will be referred to as r-SiC₃ hereafter, has been previously studied theoretically (Linguerri et al., 2006) and experimentally (McCarthy et al., 1999). While some spectral data do exist, the complete set of spectral data have yet to be produced especially for vibrational spectra of these SiC₃ isomers. As such, the existing experimental data for these molecules will serve to benchmark the computations performed herein, but new data will also be provided beyond these benchmarks.

Two isomers of Si₂C₂, a rhomboidal D _2h structure with a transannular C-C bond and a C _s trapezoidal isomer with a transannular Si-C bond, have been studied experimentally (Presilla-Márquez et al., 1995) using vibrational spectroscopy. The r-Si₂C₂ species with a C-C transannular bond has also been theoretically studied using density functional theory (DFT) at the B3LYP/6-311G(3df) level of theory (Yadav et al., 2006). Trapezoidal (t-)Si₂C₂ and r-Si₂C₂ isomers with transannular Si-Si bonds have only been studied theoretically at the MP2/6-31G* level (Lammertsma and Güner, 1988). A higher level of theory could be useful in corroborating these early computations making more modern computations on these structures necessary.

Two isomers of Si₃C are studied in this work. Like with the SiC₃ isomers, r-Si₃C exhibits a transannular Si-C bond, while d-Si₃C possesses a transannular Si-Si bond. The r-Si₃C isomer has been studied in the laboratory via vibrational spectroscopy (Presilla-Márquez and Graham, 1992; Stanton et al., 2005; Truong et al., 2015). Both isomers have only been theoretically studied in regards to their spectroscopic constants (Rittby, 1992) more than 30 years ago at the Hartree-Fock level of theory. Lastly, only the r-Si₄ cation has been both theoretically and experimentally studied (Savoca et al., 2012). Conversely, theoretical spectral data are currently unavailable for the neutral species of r-Si₄ leaving the door open for a more complete theoretical analysis and spectroscopic characterization of these structures.

Despite all the previous work discussed previously, high level theoretical methods have only been applied to three of the nine TASCCs with various levels of spectral completeness reported. Additionally, one experimental study has investigated the spectral data of heteroatomic TASCCs (Babin et al., 2021), while another study has undertaken DFT analysis with the 6-311G* basis set for various TASCC cations (Lavendy et al., 1997). The current work applies recent advancements in modern approaches to all nine TASCCs herein including the first high-level computations for the remaining six species. By covering every combination of Si and C in a tetra-atomic molecule, this work will examine the effect of silicon doping on the IR emission bands for carbide clusters, which previously has only been briefly studied (Inostroza et al., 2008; Savoca et al., 2013), and no work has studied this effect on TASCCs.

In light of a need for modern approaches, this work utilizes quartic force field (QFF) methods to produce highly-accurate, explicit anharmonic vibrational frequencies, rotational constants, and other spectroscopic constants for each of the molecules studied herein. A QFF is a fourth-order Taylor series expansion of the potential portion of the internuclear Watson Hamiltonian (Fortenberry and Lee, 2019). Previous work has shown that QFF techniques produce fundamental anharmonic frequencies that are accurate to within 5–7 cm⁻¹ of gas-phase vibrational frequencies and within about 20 MHz of experimental rotational constants (Huang and Lee, 2008, 2009; Huang et al., 2011; Fortenberry et al., 2012; Huang et al., 2013; Fortenberry et al., 2014a, 2015; Zhao et al., 2014; Kitchens and Fortenberry, 2016; Bizzocchi et al., 2017; Fortenberry et al., 2018a; Valiev et al., 2020; Gardner et al., 2021). These constants may be used to aid in determination of the molecules responsible for unidentified peaks in the infrared and microwave spectra in nebulae, gas clouds, circumstellar envelopes, or other astronomical environments. Accurate characterization of these environments may lead to a more complete understanding of the processes that lead to their evolution possibly including dust nucleation and planet formation. Vibrational observation may be promising for the novel molecules studied herein as JWST’s MIRI instrument can resolve spectra at frequencies down to roughly 350 cm⁻¹ (28 μm).

The present QFFs are computed at two different levels of theory for each TASCC. Both methods use coupled cluster theory at the singles, doubles, and perturbative triples level (Raghavachari et al., 1989) within the explicitly correlated F12b formalism, or CCSD(T)-F12b (Adler et al., 2007; Peterson et al., 2008; Knizia et al., 2009; Huang et al., 2010). The first QFF method utilizes the cc-pVTZ-F12 basis set alone, and this combination will henceforth be abbreviated as “F12-TZ”. F12-TZ has been shown to yield accurate results for vibrational frequencies, within 5–7 cm⁻¹ compared to gas-phase experiment, and it still exhibits far greater time savings than previously used composite, coupled cluster methods (Agbaglo et al., 2019; Agbaglo and Fortenberry, 2019a,b; Gardner et al., 2021). The second QFF method employs the cc-pCVTZ-F12 (Hill and Peterson, 2010) basis set to include the effects from core electron correlation (cC) with additional corrections for scalar relativity (R). This composite method is hereafter abbreviated “F12-TZ-cCR” (Watrous et al., 2021). In addition to including core correlation in the computation, the F12-TZ-cCR method utilizes Douglas-Kroll scalar relativistic corrections (Douglas and Kroll, 1974) in its single-point energy computations at the CCSD(T)/cc-pVTZ-DK level of theory to produce a more accurate description of the potential energy surface for an increased computational cost relative to F12-TZ that is still far less than the composite methods used previously.

All of the QFFs reported in this work are computed in the same, general manner beginning with the optimization of the molecular geometry with the CCSD(T)-F12b method whether excluding (F12-TZ) or including (F12-TZ-cCR) core electron correlation in the computation. All also utilize the MOLPRO 2020.1 quantum chemical program (Werner et al., 2020). The resulting optimized geometry serves as a reference point from which the INTDER program (Allen., 2005) displaces bond lengths and angles/torsions by 0.005 Å and radians, respectively (Huang and Lee, 2008). For the tetra-atomic D_4h and D_2h molecules, such as rhomboidal C₄ and Si₄ and the rhomboidal and diamond isomers of Si₂C₂, 233 displacement points are required utilizing the following symmetry-internal coordinates (SICs) with atomic labels, as shown in Figure 1. QFFs of this connectivity have previously employed such a coordinate system (Westbrook and Fortenberry, 2020). S 1 a g = 1 2 r Si 1 − Si 4 + r C 2 − C 3 (1) S 2 a g = 1 2 r Si 1 − Si 4 − r C 2 − C 3 (2) S 3 b 3 g = 1 2 r Si 1 − C 2 − r Si 1 − C 3 − r C 2 − Si 4 + r C 3 − Si 4 (3) S 4 b 3 u = τ Si 4 − C 3 − C 2 − Si 1 (4) S 5 b 1 u = 1 2 r Si 1 − C 2 + r Si 1 − C 3 − r C 2 − Si 4 − r C 3 − Si 4 (5) S 6 b 2 u = 1 2 r Si 1 − C 2 − r Si 1 − C 3 + r C 2 − Si 4 − r C 3 − Si 4 (6)

Differently, 413 displacement points, as employed previously (Fortenberry et al., 2013; Bassett and Fortenberry, 2018), are computed for the cyclic C_2v molecules (r-Si₃C and d-SiC₃) incorporating the following SICs with atom labels given in Figure 1. S 1 a 1 = r Si 1 − C 2 (7) S 2 a 1 = 1 2 r C 2 − C 3 + r C 2 − C 4 (8) S 3 a 1 = 1 2 ∠ Si 1 − C 2 − C 3 + ∠ Si 1 − C 2 − C 4 (9) S 4 b 2 = 1 2 r C 2 − C 3 − r C 2 − C 4 (10) S 5 b 2 = 1 2 ∠ Si 1 − C 2 − C 3 − ∠ Si 1 − C 2 − C 4 (11) S 6 b 1 = τ Si 1 − C 2 − C 3 − C 4 (12)

Furthermore, 665 points are used for the C _s molecule in this study (d-Si₃C) with the following SICs from earlier work (Fortenberry et al., 2018b, 2019; Fortenberry, 2019) with atomic labels, shown in Figure 1. S 1 a 1 = r Si 1 − C 2 (13) S 2 a 1 = 1 2 r C 2 − Si 3 + r C 2 − Si 4 (14) S 3 b 2 = 1 2 ∠ Si 1 − C 2 − Si 3 + ∠ Si 1 − C 2 − Si 4 (15) S 4 b 2 = ∠ Si 3 − C 2 − Si 4 (16) S 5 a 1 = 1 2 r C 2 − Si 3 − r C 2 − Si 4 (17) S 6 b 1 = 1 2 ∠ Si 1 − C 2 − Si 3 − ∠ Si 1 − C 2 − Si 4 (18)

Finally, 743 symmetry-unique (for a total of 805) points, as incorporated in previous work (Fortenberry et al., 2011, 2012, 2020), are used for the planar C _s molecule in this study (t-Si₂C₂). The SICs for such a connectivity are labeled as shown in Figure 1. S 1 a ′ = r C 1 − C 2 (19) S 2 a ′ = r C 2 − Si 3 (20) S 3 a ′ = r Si 3 − Si 4 (21) S 4 a ′ = ∠ C 1 − C 2 − Si 3 (22) S 5 a ′ = ∠ C 2 − Si 3 − Si 4 (23) S 6 a ″ = τ Si 4 − Si 3 − C 2 − C 1 (24)

Regardless of the number of displacements, single-point energy computations are conducted at both levels of theory for each of the molecules analyzed in this work. Once the single-point energy computations finish, their relative energies are fit to a potential function by a least squares procedure with sums of squared residual values of better than 10^–16 a. u.², excluding d-Si₃C, r-SiC₃, and t-Si₂C₂/d-SiC₃ which have slightly higher residuals of 10^–13, 10^–14, and 10^–15 a. u.², respectively. The QFF is then refit including corrections from the initial fitting to produce the final equilibrium geometry and zero-gradient force constants. The INTDER program (Allen., 2005) then converts the force constants from SICs into Cartesian coordinates. The Cartesian force constants provide greater flexibility for use in the SPECTRO program (Gaw et al., 1991), which utilizes second-order rotational and vibrational perturbation theory (Mills, 1972; Watson, 1977; Papousek and Aliev, 1982) (VPT2) to produce highly-accurate rovibrational constants and fundamental vibrational frequencies. SPECTRO also incorporates Fermi resonances as well as resonance polyads (Martin and Taylor, 1997), of the Supplementary Material, to increase the accuracy of the computed fundamental anharmonic vibrational frequencies and rotational constants. Coriolis resonances are included in the rotational constant computations, as well.

Additionally, the Gaussian16 (Frisch et al., 2016) program is used to compute transition intensities for each anharmonic vibrational frequency at the MP2/cc-pVDZ level of theory. This method has been shown to produce semi-quantitative accuracy for anharmonic infrared intensities at a low computational cost (Fortenberry et al., 2014b). Finally, dipole moments for each molecule are computed using the Molpro 2020.1 quantum chemical program (Werner et al.,2020).

The fundamental anharmonic frequencies for r-C₄ from a CCSD(T)/cc-pCV5Z semi-global potential energy surface within a variational approach (Wang and Bowman, 2013) compare well with the QFF VPT2 current data provided in Table 1. In each of these tables, ω represents the harmonic values of the vibrational frequencies, ν represents the anharmonic values, and the description of the modes (Desc.) is given in terms of the SICs from the previous section. These values all fall within 3.6 cm⁻¹ (ν ₂) and 1.00% (ν ₆) of the F12-TZ-cCR data in this work while averaging a 1.8 cm⁻¹ (0.32%) difference. Such correlation suggests that the F12-TZ-cCR QFF VPT2 treatment is handling the system well. In contrast, the F12-TZ values do not compare as well as the F12-TZ-cCR data to the previously determined CCSD(T)/cc-pCV5Z data. The ν ₂ frequency has the largest absolute difference of 10.7 cm⁻¹ (0.85%), and the difference for the total set averages 4.6 cm⁻¹ (0.46%). Thus, the F12-TZ-cCR method may come at the optimal ratio of accuracy and computational efficiency for chemical systems of the current nature. Equilibrium ( _e ), vibrationally-averaged (₀), and singly-vibrationally excited ( _n>0) rotational constants for r-C₄ can be found in Table 2, along with the quartic (Δ and δ) and sextic (Φ and ϕ) distortion coefficients in the Watson A-reduced Hamiltonian and the dipole moment (μ), which by symmetry is zero in this case. The vibrational frequency at 1315.1 cm⁻¹ (ν ₁) is the best candidate for potential vibrational observation as the frequency is above the ∼ 350 cm⁻¹ cutoff for JWST’s MIRI, and the intensity is notable with a value of 159 km mol⁻¹. The antisymmetric stretch of water, used here as a familiar basis for comparison, has an intensity of 70 km mol⁻¹ implying that this frequency in r-C₄ has a higher oscillator strength by more than a factor of two.

The d-SiC₃ structure is found to be the lowest energy cyclic isomer for the first silicon replacement analogue. It lies approximately 6.1 kcal mol⁻¹ below r-SiC₃. The d-SiC₃ F12-TZ-cCR rotational constants compare well with previously determined experimental values by McCarthy et al. (McCarthy et al., 2019). The experimental and present theoretical F12-TZ-cCR spectroscopic constants found in Table 3 differ by just 0.20% for A ₀, 0.04% for B ₀, and 0.02% for C ₀, suggesting high-accuracy for the current method. The dipole moment of d-SiC₃ is computed to be 4.03 D, comparing well with previous work (Alberts et al., 1990) which determined the dipole moment to be 4.2 D. This large dipole moment is likely the cause of d-SiC₃’s previous detection in the ISM. F12-TZ-cCR rotational constants for r-SiC₃ compare well with experimental values determined by McCarthy et al. (McCarthy et al., 1999), with the A ₀, B ₀, and C ₀ constants displaying differences of 0.08%, 0.02%, and 0.02%, respectively. The r-SiC₃ isomer is shown to have a dipole moment of 2.07 D, also comparing well with a previous 2.2 D value (Alberts et al., 1990). The strength of the dipole moment for r-SiC₃ may also lead to its radioastronomical detection. However, the slightly higher relative energy of this isomer and roughly half dipolar strength of the d isomer imply that the r isomer will likely have a notably smaller emission profile.

Differently, all harmonic frequencies reported for d-SiC₃ and r-SiC₃, found in Table 4, at the F12-TZ-cCR level provided herein exhibit notable deviations from previous theoretical work done by Linguerri et al. (2006) at the CCSD(T)/cc-pVQZ level of theory. The largest differences are 16.2 cm⁻¹ (ω ₃ from d-SiC₃; 1.64%) and 11.4 cm⁻¹ (ω ₂ from r-SiC₃; 1.01%). Linguerri et al. (2006) also report fundamental anharmonic frequencies using VSCF for both cyclic isomers of SiC₃. These values compare poorly for both isomers with fundamental frequencies differing by up to 16.3 cm⁻¹ (ν ₅; 3.98%) and 27.2 cm⁻¹ (ν ₃; 3.31%) for the presently analyzed d-SiC₃ and r-SiC₃ isomers’ F12-TZ-cCR data, respectively. Such poor comparison of the anharmonic frequencies is to be expected for the relatively poor agreement in the harmonic frequencies. The most obvious difference between the present and previous studies is the inclusion of core electron correlation (or lack thereof). As a result, the present F12-TZ-cCR results should be producing more accurate data for subsequent experimental or observational comparison. Additionally, potentially observable fundamental frequencies for r-SiC₃ include ν ₁ at 1525.5 cm⁻¹ and ν ₃ at 793.8 cm⁻¹ with intensities of 77 and 54 km mol⁻¹, respectively, given favorable ISM conditions.

With the accuracy of the current methods benchmarked on the aforementioned species, this work presents the first high level theoretical data for the remaining isomers herein. Relative energies computed at the F12-TZ-cCR level for the three cyclic Si₂C₂ isomers determine that r-Si₂C₂ with the transannular C-C bond is the lowest energy isomer, followed by t-Si₂C₂, which is 7.5 kcal mol⁻¹ higher in energy, and, lastly, the other d-Si₂C₂ isomer with the transannular Si-Si bond resides 83.8 kcal mol⁻¹ higher in energy. Experimental matrix studies are available for ν ₂, shown to be 988.1 cm⁻¹ in this work, and ν ₅, 383.0 cm⁻¹ here, for r-Si₂C₂ with a transannular C-C bond (Presilla-Márquez et al., 1995). These values are determined to be about 5.2 (0.53%) and 0.8 cm⁻¹ (0.21%) lower than the F12-TZ-cCR data found in Table 5, respectively. This agreement is relatively good, especially for ν ₅ which suggests the accuracy of both the experiment and computations. Matrix studies performed by Presilla-Márquez et al. (Presilla-Márquez et al., 1995) considered ν ₁ and ν ₃ as potential candidates for accurately observed vibrational frequencies of t-Si₂C₂, and the current work shows values for these modes differing by only 0.4 cm⁻¹ (0.03%) for ν ₁ at 1537.6 cm⁻¹ and 4.9 cm⁻¹ (0.78%) for ν ₃ at 636.9 cm⁻¹ for the F12-TZ-cCR computations found in Table 5. This may be promising for the vibrational observation of ν ₃ for t-Si₂C₂ in the ISM as the intensity is determined to be 63 km mol⁻¹. The lowest energy isomer of cyclic Si₂C₂ is found to have an anharmonic vibrational intensity of 247 km mol⁻¹ for ν ₂ at 988.1 cm⁻¹, which is over three times more intense than that of the aforementioned antisymmetric stretch of water. Also, t-Si₂C₂ is found to have a strong dipole moment of 2.90 D given in Table 6, which suggests the molecule may be rotationally observable if present in high concentrations. This may be likely given the prevalence of SiC dust on chondrite meteorites and in the observed ISM.

The d-Si₂C₂ isomer with the transannular Si-Si bond displays a strong pseudo-Jahn Teller type-2 distortion effect in the potential energy surface of the molecule (Mintz and Crawford, 2010; Bersuker, 2021). Such behavior causes overlap in the surfaces between this isomer and r-Si₂C₂. This negates the computation for all of the fundamental vibrational frequencies, but the five that can be determined are reported in Table 5. The one that is missing involves the out-of-plane bend. The coordinates for this motion cause the orbital occupations to collapse to that of the r-Si₂C₂ isomer where the C _s symmetry is too low to distinguish the wavefunctions in the reference. Even so, the fundamentals reported herein should serve as estimates for any subsequent analysis. Intensities for d-Si₂C₂ are not computed due to the complexity of the type 2 pseudo-Jahn Teller distortion.

The current work presents the only spectroscopic constants computed at a high level of theory for cyclic Si₃C isomers. The r-Si₃C species is found to be the lowest energy isomer residing 49.6 kcal mol⁻¹ below d-Si₃C. Anharmonic vibrational modes of r-Si₃C, found in Table 7, computed at the F12-TZ-cCR level compare well with previous experimental matrix studies performed by Presilla-Márquez and Graham (1992) differing by 5.8 cm⁻¹ (1.62%) for ν ₄ and 5.4 cm⁻¹ (1.06%) for ν ₃. Similarly, ν ₂ shows a maximum difference of 3.2 cm⁻¹ (0.49%). Table 8 displays the rotational constants for both isomers. The d-Si₃C species may be rotationally observable as the dipole moment for this molecule is determined to be 2.64 D. The d-Si₃C isomer has no observable vibrational modes, meaning no modes above JWST’s high resolution cutoff of 350 cm⁻¹ have an intensity near the anti-symmetric stretch of water, or 70 km mol⁻¹. However, ν ₁ of r-Si₃C has a higher intensity at 80 km mol⁻¹. This may lead to the vibrational observation of this species in the ISM if found in sufficient quantities relative to adjacent molecular species.

Similarly to the previous isomers, this work provides the first high level theoretical spectral data for neutral r-Si₄. Computed spectral data for r-Si₄ are presented in Tables 9 and 10. The anharmonic frequency ν ₁ may be observable experimentally, as it is shown to have a reasonable intensity of 41 km mol⁻¹.

As silicon composition increases with each TASCC, the current data sheds some light on the effects of silicon doping on the spectral frequencies of tetra-atomic carbon clusters. This is possible due to a similar connectivity between r-C₄, r-Si₂C₂ with a transannular C-C bond, and r-Si₄. Tables 1, 5, and 9 and Figure 2 demonstrate that the addition of silicon to carbon clusters causes a redshift in each of the vibrational frequencies, agreeing with the work done on larger silicon clusters by Savoca et al. (2013). This can be seen with ν ₁ for each species with r-C₄ coming at 1315.1 cm⁻¹, C-C r-Si₂C₂ falling to 1069.7 cm⁻¹, and r-Si₄ coming down to 505.9 cm⁻¹. While such a relationship is expected for heavier atoms, quantification of this relationship may aid in accurately identifying the silicon composition in stellar atmospheres of large carbonaceous stars, or subsequent novae and nebulae. Identifying the molecular framework and elemental ratios in these environments may lead to a more holistic understanding of their processes of formation, i.e. novae processes and the formation of the first interstellar dust grains. With SiC dust making up a large portion of the available cosmic dust for research on chondrite meteorites, characterization of carbon to silicon ratios in various astronomical environments may lead to a better understanding of the ISM and the processes that lead to its formation but only if data such as those provided herein can be utilized to detect more SiC molecules and clusters.

The most promising anharmonic fundamental frequency for astronomical vibrational detection for these silicon carbide clusters is the ν ₂ frequency at 988.1 cm⁻¹ (10.1 μm) of r-Si₂C₂ with a transannular C-C bond displaying a very large intensity of 247 km mol⁻¹. This frequency may be a distinct feature in the unidentified IR spectrum and would be a likely candidate for observation if found in sufficient concentrations. Other notable IR features for possible observation include ν ₁ of r-C₄ (1315.1 cm⁻¹; 7.6 μm) with an intensity of 159 km mol⁻¹, ν ₁ of d-SiC₃ (1339.4 cm⁻¹; 7.5 μm) with an intensity of 128 km mol⁻¹, ν ₁ of r-Si₃C (1100.3 cm⁻¹; 9.1 μm) with an intensity of 80 km mol⁻¹, and ν ₁ of r-SiC₃ (1525.5 cm⁻¹; 6.6 μm) with an intensity of 77 km mol⁻¹. Each of these anharmonic frequencies are good candidates for observation with the recently operational MIRI instrument aboard the JWST between 9.09 μm and 6.56 μm. Finally, rotational observation may be possible for t-Si₂C₂, d-Si₃C, and r-SiC₃ due to dipole moments of 2.90, 2.63, and 2.07 D, respectively. Because of this, the prevalence of SiC dust in the ISM, and the known observation of the related d-SiC₃, these molecules are strong candidates for radioastronomical observation.