Free Access
Volume 657, January 2022
Article Number L4
Number of page(s) 6
Section Letters to the Editor
Published online 07 January 2022

© ESO 2022

1. Introduction

The cold dark cloud TMC-1 shows a rich and complex chemistry, and it is known to contain a variety of protonated species of abundant neutral molecules. In addition to the widespread ions HCO+ and N2H+, the polyatomic cations detected in TMC-1 are HCS+ (Irvine et al. 1983), HCNH+ (Schilke et al. 1991), HC3NH+ (Kawaguchi et al. 1994), HCO (Turner et al. 1999), NCCNH+ (Agúndez et al. 2015), HC5NH+ (Marcelino et al. 2020), HC3O+ (Cernicharo et al. 2020), HC3S+ (Cernicharo et al. 2021a), and CH3CO+ (Cernicharo et al. 2021b). The abundance ratio between a protonated molecule and its neutral counterpart, MH+/M, is sensitive to the degree of ionization and to the formation and destruction rates of the cation (Agúndez et al. 2015). The main formation route to the cation is usually the proton transfer to the neutral, while its main destruction process is the dissociative recombination with electrons. It is interesting to note that both chemical models and observations suggest a trend in which the abundance ratio MH+/M increases with increasing proton affinity of M (Agúndez et al. 2015). Thus, protonated species of abundant molecules with high proton affinities are good candidates for detection.

The number of sulfur-bearing species detected to date in TMC-1 is small compared to oxygen- and nitrogen-bearing species (see e.g. McGuire et al. 2019). However, the most recent discoveries have revealed that TMC-1 is also a source rich in sulfur-bearing molecules (Cernicharo et al. 2021a,c,d). The carbon chains CCS and CCCS are particularly abundant in this cloud (Saito et al. 1987; Yamamoto et al. 1987). The protonated form of the CCCS molecule, HC3S+, was discovered in TMC-1 and confirmed in the laboratory by Cernicharo et al. (2021a). The protonated form of CCS, HCCS+, has not been detected in space so far, but it is considered a promising candidate to be observed (Agúndez et al. 2015) given that CCS is even more abundant than CCCS, CCS/CCCS ∼4.2, it has a high calculated proton affinity, between 869.6 (Maclagan & Sudkeaw 1992) and 901.2 kJ mol−1 (Barrientos & Largo 1991), and chemical models predict HCCS+ to be just a few times less abundant than CCS (Agúndez et al. 2015). However, the lack of laboratory data for HCCS+ has hampered its detection.

High resolution line surveys can be used to conduct molecular spectroscopy in space; they are an invaluable alternative that can be used to overcome the lack of laboratory experimental data. Some examples of these kinds of identifications carried out by our group are C5H (Cernicharo et al. 1986), C5N (Cernicharo et al. 2008), MgC3N and MgC4H (Cernicharo et al. 2019), HC5NH+ (Marcelino et al. 2020), MgC5N and MgC6H (Pardo et al. 2021), and H2NC (Cabezas et al. 2021). If the source displays narrow lines and spectral resolution is sufficiently high, it is possible to resolve the hyperfine structure and derive very precise spectroscopic parameters (Cabezas et al. 2021). Here we present a new case of molecular spectroscopy done in space. Thanks to the sensitivity of our QUIJOTE1 line survey of TMC-1 (Cernicharo et al. 2021e) we have detected various groups of unidentified lines, revealing a characteristic fine and hyperfine structure, which we confidently assign to HCCS+ based on our quantum chemical calculations.

2. Observations

The observations in the Q band are part of the QUIJOTE spectral line survey, carried out towards TMC-1 (αJ2000 = 4h41m41.9s and ) with the Yebes 40 m radio telescope. The QUIJOTE data currently available were taken during various observing sessions between November 2019 and April 2021. These observations were carried out using the frequency-switching technique with a frequency throw of 10 MHz during the first observing runs and of 8 MHz in the later ones. Different frequency coverages were observed, 31.08–49.52 GHz and 31.98–50.42 GHz, which permitted us to verify that no spurious ghosts were produced in the down-conversion chain. In this process, the signal coming from the receiver is down-converted to 1–19.5 GHz and then split into eight bands, each with a coverage of 2.5 GHz, which are analysed by the fast Fourier transform (FFT) spectrometers.

Data in the 3 mm band come from a spectral line survey performed towards TMC-1 and B1-b using the IRAM 30 m telescope (Marcelino et al. 2007; Cernicharo et al. 2012). Additional data were gathered in September and October 2021. For these observations the 3 mm EMIR receiver was used connected to a FFT spectrometer, providing a spectral resolution of 48.84 kHz. We observed two setups at slightly different central frequencies in order to check for spurious signals, line emission from the image band, and other technical artefacts. The observations were performed in the frequency-switching observing mode with a frequency throw of 18 MHz. System temperatures varied between 80 and 130 K, and the final rms for the line studied in this work is between 1.1 and 3 mK.

The intensity scale used for the Yebes 40 m and IRAM 30 m observations, the antenna temperature , was calibrated using two absorbers at different temperatures and the atmospheric transmission model ATM (Cernicharo 1985; Pardo et al. 2001). Calibration uncertainties were adopted to be 10%. All data were analysed using the GILDAS package2.

3. Results and discussion

3.1. Discovery of HCCS+

The ion HCCS+ is predicted to be an abundant interstellar species (Agúndez et al. 2015). This open-shell cation was investigated by Puzzarini (2008) using high level quantum chemical calculations. In this work, the equilibrium geometry and energy for HCCS+ are presented at different levels of theory. Using the best estimated equilibrium structure for HCCS+ in its 3Σ ground electronic state, we calculate a B rotational constant of 6048 MHz. This value has been used in the past to make frequency predictions and search for this species towards TMC-1 (Cernicharo et al. 2021a), with a 3σ upper limit to its column density of 9 × 1011 cm−2 obtained. However, due to the 3Σ ground state for HCCS+, its rotational spectral pattern is not as simple as that of other closed-shell species. The prediction of this spectral pattern requires knowing not only the rotational constant, but also additional spectroscopic parameters, such as the spin-spin interaction constant, λ, the spin-rotation interaction constant, γ, and the hydrogen nuclei hyperfine constants bF and c. For our predictions we calculated all these molecular parameters (see Sect. 3.2) except λ, for which we adopted the value derived for the CCS (3Σ) radical (Yamamoto et al. 1990), which is isoelectronic to HCCS+. These predictions have very large uncertainties, and the search was unsuccessful even for the J = N lines, which could appear at harmonically related frequencies. Moreover, the expected intensity variation in the lines was also an important unknown, and a handicap, because the J = N + 1 levels are significantly lower in energy than those with J = N and J = N − 1 (see Sect. 3.3). Hence, the three rotational lines arising from a given N could have very different intensities in a cold dark cloud such as TMC-1.

In a new attempt, we followed a different strategy to find lines that could be attributable to HCCS+. The expected pattern for the most intense lines (J = N + 1) consists in doublets of lines with a separation of a few megahertz. We searched for these doublets in a very wide region and found a couple of very strong unidentified lines (the strongest among our U-lines) at 32.11 GHz, which is 350 MHz lower to the initially predicted frequency. A second pair of lines with similar intensity was found at 43.03 GHz. For a 3Σ molecule the transitions J = N follow a very good harmonic relation with a very small error. However, the energy terms for the levels J = N − 1 and J = N + 1 contain contributions from λ and γ, and the frequency ratio between subsequent transitions deviates from the ratio of the J values. The frequency ratio between the two observed doublets is near 4/3, with an error of a few per cent, which is in agreement with the expected ratio for the J = N + 1 transitions. Hence, these two doublets, shown in Fig. 1, can be assigned to the NJ = 23 − 12 and 34 − 23 transitions of HCCS+. Using this near-harmonic relation, we predicted the frequencies of the next doublets of lines within our data at 3 mm and found three additional doublets that can be assigned to the NJ = 67 − 56, 78 − 67, and 89 − 78 transitions. As expected, the separation between the two components of each doublet decreases with N (see Fig. 1). These five pairs of lines can be fitted with a standard Hamiltonian for a 3Σ molecule (see Sect. 3.2). New frequency predictions, improved by the assigned transitions, were used to search for the J = N and J = N − 1 transitions. Three of them, the NJ = 33 − 22, 43 − 32, and 44 − 33, were easily found in the QUIJOTE line survey (see Fig. 1). Once merged with the previous lines, the predictions for additional lines at 3 mm permitted four additional doublets corresponding to the NJ = 77 − 66, 88 − 77, 76 − 65, and 87 − 76 transitions to be detected. The final set of twenty-six hyperfine components includes two weak components from the NJ = 23 − 12 and 34 − 23 transitions. The derived line parameters are given in Table A.1. The energy levels associated with the observed rotational transitions are shown in Fig. 2 (see Sect. 3.3).

thumbnail Fig. 1.

Spectra of the observed transitions of HCCS+ in TMC-1. The abscissa corresponds to the rest frequency assuming a local standard of rest velocity of 5.83 km s−1. The ordinate is antenna temperature in millikelvin. Blanked channels correspond to negative features produced in the folding of the frequency-switching data. The red lines correspond to the synthetic spectra calculated for a column density of 1.1 × 1012 cm−2 and a rotational temperature of 7.0 K for Nu ≤ 4 and 4.5 K for higher Nu values (see Sect. 3.3).

3.2. Rotational analysis of HCCS+

All the observed hyperfine components were analysed with the SPFIT program (Pickett 1991) using a Hamiltonian for a linear molecule in a 3Σ electronic state. Since HCCS+ contains one nucleus with a non-zero nuclear spin, the appropriate Hamiltonian to describe the rotational levels can be written as follows:


where Hrot, Hss, and Hsr denote the rotational, spin-spin, and spin-rotation terms, respectively, and Hmhf represents the magnetic hyperfine coupling interaction term due to the hydrogen nucleus. The coupling scheme used is J = N + S, F = J + I(H).

The molecular constants determined from the fit are given in Table 1 together with those predicted by ab initio calculations (Frisch et al. 2016; Werner et al. 2020) and those for the CCS radical. All the constants are very well determined, indicating that the fine and hyperfine structures are well described by the employed Hamiltonian. The identification of HCCS+ as the carrier of the observed lines is unequivocal. The rotational constant B obtained by us through ab initio calculations (RCCSD(T)-F12/cc-pCVTZ-F12; Knizia et al. 2009; Hill et al. 2010) is 6042.5 MHz, which is similar to that calculated by Puzzarini (2008) and deviates from the value derived from TMC-1 data by just 0.3%. This difference decreases down to 0.01% when the theoretical value is scaled using the experimental/theoretical ratio of the isoelectronic CCS radical. The B value obtained for CCS at the same level of theory is 6500.7 MHz. The value derived for D is also in good agreement with that predicted at the MP2/cc-pVTZ level of theory (Møller & Plesset 1934; Woon & Dunning 1993). The values for the spin-spin interaction constant and its centrifugal distortion constant, λ and λD, cannot be estimated using quantum chemical calculations. However, their values are similar to those found for the isoelectronic CCS radical, as expected. The value for the spin-rotation constant, γ, is significantly different from that predicted by ab initio calculations (Møller & Plesset 1934; Woon & Dunning 1993). For the CCS radical, the predicted value for γ at the same level of theory is −110.2 MHz, quite different from the experimental value as well. The accuracy of the prediction of γ is much smaller than that of other molecular constants. For the hyperfine constants, the agreement with the theoretical values is disparate. The derived value for the Fermi contact constant, bF, agrees well with the predicted value (QCISD/cc-pVTZ; Pople et al. 1987; Woon & Dunning 1993). However, for the dipole-dipole constant, c, the discrepancy is very large. This is very surprising because the prediction of hyperfine constants at the employed level of theory usually gives satisfactory results. In order to get some insight into this, we calculated the c constant for the other 3Σ molecule, HCCN, and we found the same behaviour. The predicted value, at the same level of theory, for the c constant is 52.8 MHz, while the experimental one is 32.91(18) MHz (Endo & Oshima 1993). The prediction of the c constant for 3Σ molecules may not be as accurate as expected.

Table 1.

Spectroscopic parameters of HCCS+, in MHz.

3.3. The abundance and excitation of HCCS+ in TMC-1

The scheme of rotational energy levels of a 3Σ molecule has a peculiar pattern, as shown in Fig. 2 for HCCS+. Since the λ value is rather large, similar to that of CCS, the J = N + 1 ladder of levels is always below the J = N − 1 and J = N ladders, the latter being the highest in energy. For a cloud with a kinetic temperature of 10 K, the energy difference between these three ladders affects the intensity of the rotational transitions. As shown in Fig. 1, the J = N + 1 lines are very strong, but their intensity declines for high N values. The upper level energy of the highest N transition in our data, 89 − 78, is ∼24 K. If we assume thermalization at 10 K and optically thin emission, this line should be as strong as the 34 − 23 one, but this is not the case. Hence, the rotational levels of HCCS+ are not thermalized. This is in fact indicated by a rotation diagram constructed with the lines observed, where two different rotational temperatures are seen. The lines observed with QUIJOTE are reproduced with a rotational temperature of 7.0 ± 1.5 K and a column density of (1.1 ± 0.2)×1012 cm−2, while the lines observed at 3 mm, which correspond to transitions involving higher level energies, are reproduced with the same column density but a rotational temperature of 4.5 ± 1.0 K.

thumbnail Fig. 2.

Energy levels of HCCS+ organized by N and J values. The observed transitions are indicated by green arrows.

In order to evaluate possible excitation effects in the different lines of HCCS+, we used the MADEX code to perform a large velocity gradient calculation (MADEX follows the formalism described by Goldreich & Kwan 1974). The hyperfine structure was neglected in these calculations. For this purpose, we adopted, as done by Cernicharo et al. (2021f) for CCO, the collisional rates of OCS (Green & Chapman 1978) and the infinite-order sudden approximation for a 3Σ molecule (Alexander & Dagdigian 1983; Corey & McCourt 1983; Fuente et al. 1990). For a volume density of H2 of 4 × 104 cm−3 (Cernicharo & Guélin 1987), the excitation temperatures obtained using this approach are ∼7–10 K for the lines observed in the Q band. However, the excitation temperature decreases to 5.7 K for Nu = 6 and to 4.5 K for Nu = 8. We explored the effect of n(H2) on the excitation temperatures of HCCS+. For n(H2) ≥ 104 cm−3, the N = 2 and 3 (J = N + 1) lines have an excitation temperature close to TK. However, the lines associated with upper levels with N ≥ 6 show a sharp dependence of Texc with density. The best fit to the observations is obtained for n(H2) = 2 − 4 × 104 cm−3 and N(HCCS+) = (1.1 ± 0.2) × 1012 cm−2. We adopted Trot = 7.0 K for Nu≤4 and 4.5 K for higher Nu values and a source radius of 40″ (Fossé et al. 2001). The match between the observations is rather good despite the uncertainty in the collisional rates (see Fig. 1). The derived column density is only 20% larger than the previous 3σ limit reported by Cernicharo et al. (2021a).

3.4. The chemistry of HCCS+

Adopting the column density of CCS derived by Cernicharo et al. (2021a) of (5.5 ± 0.6)×1013 cm−2, the abundance ratio between CCS and its protonated form is 50 ± 10. This ratio is very similar to that obtained by those authors for CS and HCS+ (35 ± 8) and for CCCS and HCCCS+ (65 ± 20). In order to get insight into the chemistry of HCCS+ in TMC-1, we constructed a pseudo-time-dependent gas-phase chemical model with parameters typical of cold dark clouds (see Cernicharo et al. 2021a for details and Agúndez et al. 2015 for further details on the adopted physical conditions). We adopted the chemical network kida.uva.2014 from the KIDA database (Wakelam et al. 2015).

The calculated abundances of CCS and HCCS+ are shown in the bottom panel of Fig. 3, with the calculated abundance ratio CCS/HCCS+ shown in the top panel of the same figure. If we first focus on the neutral-to-protonated ratio, we see that the calculated value at steady state is pretty small, ∼3 (solid orange curve in the top panel of Fig. 3), in agreement with the prediction by Agúndez et al. (2015). However, steady state may not be a good choice for TMC-1. Instead, the so-called early time (105–106 yr) may better represent the state of TMC-1 since at this time calculated and observed abundances show the best overall agreement (see e.g. Agúndez & Wakelam 2013). At a time of (2–3) × 105 yr, the calculated CCS/HCCS+ ratio agrees very well with the observed value. However, the fractional abundance of HCCS+ is below the observed value by about two orders of magnitude. According to the chemical model, HCCS+ is mostly destroyed through dissociative recombination with electrons, as usual for cations. On the other hand, the formation of HCCS+ is mostly driven by ion-neutral reactions, such as S+ + C2H2, S + C2, and S + C2, rather than by reactions of proton transfer to CCS from HCO+, H3O+, and . This occurs because the chemical model severely underestimates the abundance of CCS, by two to three orders of magnitude (see the solid blue curve in the bottom panel of Fig. 3). This has been already noticed by Cernicharo et al. (2021a) and points to an inadequate description of the chemistry of CCS.

thumbnail Fig. 3.

Calculated abundances of CCS and HCCS+ (bottom) and abundance ratio CCS/HCCS+ (top) as a function of time. Dashed lines correspond to a chemical model in which the reaction O + CCS is removed from the chemical network. Observed values are indicated by horizontal dotted lines.

The kida.uva.2014 network includes a very efficient process of destruction of CCS through reaction with O atoms. The rate coefficient for this reaction has been estimated by Loison et al. (2012) to be as high as 10−10 cm3 s−1. If we remove this reaction from the chemical network, the calculated abundance of CCS at early time agrees much better with the observed value (dashed blue curve in the bottom panel of Fig. 3), and the abundance of protonated CCS is also enhanced because the reactions of proton transfer to CCS become the dominant routes to HCCS+. In this case, the calculated abundance of HCCS+ at early time is closer to the observed value, while the neutral-to-protonated ratio is still of the order of the value observed. It would therefore be interesting to study the reaction O + CCS and evaluate how rapid it could be at low temperatures. Whatever the failure in the description of the chemistry of CCS, it seems clear that proton transfer to CCS should be the main pathway to HCCS+. In such a case, the neutral-to-protonated abundance ratio can be evaluated through the expression (Agúndez et al. 2015)


where kDR and kPT are the rate coefficients for dissociative recombination of HCCS+ and proton transfer to CCS, respectively, while [e] and [XH+] are the abundances of electrons and proton donors, respectively. Assuming to a first order that [XH+] = [e], and adopting kDR(10 K) = 1.6 × 10−6 cm3 s−1 and kPT(10 K) = 1.6 × 10−8 cm3 s−1, as given in the kida.uva.2014 network, the predicted CCS/HCCS+ ratio is 100, which is only a factor of two higher than the value derived from the observations. This supports the idea that HCCS+ is mainly formed by proton transfer to CCS from the most abundant proton donors.

4. Conclusions

We observed a total of 26 unidentified lines in the cold dark cloud TMC-1, which we confidently assign to the cation HCCS+ based on high level ab initio calculations. The astronomical lines are used to precisely characterize the rotational spectrum of HCCS+ for the first time. The analysis of the line intensities considering possible excitation effects provides a column density for HCCS+ of (1.1 ± 0.2)×1012 cm−2 with rotational temperatures of 7.0 ± 1.5 K and 4.5 ± 1.0 K for the transitions observed in the Q band and at 3 mm, respectively. According to our chemical modelling calculations, in TMC-1 the cation HCCS+ is most likely formed through proton transfer to CCS from the most abundant proton donors, such as HCO+, H3O+, and .


Q-band Ultrasensitive Inspection Journey to the Obscure TMC-1 Environment


This research has been funded by ERC through grant ERC-2013-Syg-610256-NANOCOSMOS. Authors also thank Ministerio de Ciencia e Innovación for funding support through projects PID2019-106235GB-I00 and PID2019-107115GB-C21/AEI/10.13039/501100011033. MA thanks Ministerio de Ciencia e Innovación for grant RyC-2014-16277.


  1. Agúndez, M., & Wakelam, V. 2013, Chem. Rev., 113, 8710 [Google Scholar]
  2. Agúndez, M., Cernicharo, J., de Vicente, P., et al. 2015, A&A, 579, L10 [Google Scholar]
  3. Alexander, M. H., & Dagdigian, P. J. 1983, J. Chem. Phys., 79, 302 [NASA ADS] [CrossRef] [Google Scholar]
  4. Barrientos, C., & Largo, A. 1991, Chem. Phys. Lett., 184, 168 [NASA ADS] [CrossRef] [Google Scholar]
  5. Cabezas, C., Agúndez, M., Marcelino, N., et al. 2021, A&A, 654, A45 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  6. Cernicharo, J. 1985, Internal IRAM Report (Granada: IRAM) [Google Scholar]
  7. Cernicharo, J., & Guélin, M. 1987, A&A, 176, 299 [Google Scholar]
  8. Cernicharo, J., Kahane, C., Gómez-González, J., & Guélin, M. 1986, A&A, 167, L5 [NASA ADS] [Google Scholar]
  9. Cernicharo, J., Guélin, M., Agúndez, M., et al. 2008, ApJ, 688, L83 [NASA ADS] [CrossRef] [Google Scholar]
  10. Cernicharo, J., Marcelino, N., Rouef, E., et al. 2012, ApJ, 759, L43 [Google Scholar]
  11. Cernicharo, J., Cabezas, C., Pardo, J. R., et al. 2019, A&A, 630, L2 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  12. Cernicharo, J., Marcelino, N., Agúndez, M., et al. 2020, A&A, 642, L17 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  13. Cernicharo, J., Cabezas, C., Endo, Y., et al. 2021a, A&A, 646, L3 [EDP Sciences] [Google Scholar]
  14. Cernicharo, J., Cabezas, C., Bailleux, S., et al. 2021b, A&A, 646, L7 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  15. Cernicharo, J., Cabezas, C., Agúndez, M., et al. 2021c, A&A, 648, L3 [EDP Sciences] [Google Scholar]
  16. Cernicharo, J., Cabezas, C., Endo, Y., et al. 2021d, A&A, 650, L14 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  17. Cernicharo, J., Agúndez, M., Kaiser, R., et al. 2021e, A&A, 652, L9 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  18. Cernicharo, J., Agúndez, M., Cabezas, C., et al. 2021f, A&A, 656, L21 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  19. Corey, G. C., & McCourt, F. R. 1983, J. Chem. Phys., 87, 2723 [Google Scholar]
  20. Endo, Y., & Oshima, Y. 1993, J. Chem. Phys., 98, 6618 [NASA ADS] [CrossRef] [Google Scholar]
  21. Fossé, D., Cernicharo, J., Gerin, M., & Cox, P. 2001, ApJ, 552, 168 [Google Scholar]
  22. Frisch, M. J., Trucks, G. W., Schlegel, H. B., et al. 2016, Gaussian 16 Revision A.03 [Google Scholar]
  23. Fuente, A., Cernicharo, J., Barcia, A., & Gómez-González, J. 1990, A&A, 231, 151 [Google Scholar]
  24. Goldreich, P., & Kwan, J. 1974, ApJ, 189, 441 [CrossRef] [Google Scholar]
  25. Green, S., & Chapman, S. 1978, ApJS, 37, 169 [Google Scholar]
  26. Hill, J. G., Mazumder, S., & Peterson, K. A. 2010, J. Chem. Phys., 132, 054108 [Google Scholar]
  27. Irvine, W. M., Good, J. C., & Schloerb, F. P. 1983, A&A, 127, L10 [NASA ADS] [Google Scholar]
  28. Kawaguchi, K., Kasai, Y., Ishikawa, S., et al. 1994, ApJ, 420, L95 [NASA ADS] [CrossRef] [Google Scholar]
  29. Knizia, G., Adler, T. B., & Werner, H.-J. 2009, J. Chem. Phys., 130, 054104 [Google Scholar]
  30. Loison, J.-C., Halvick, P., Bergeat, A., et al. 2012, MNRAS, 421, 1476 [Google Scholar]
  31. Maclagan, R. G. A. R., & Sudkeaw, P. 1992, Chem. Phys. Lett., 194, 147 [NASA ADS] [CrossRef] [Google Scholar]
  32. Marcelino, N., Cernicharo, J., Agúndez, M., et al. 2007, ApJ, 665, L127 [Google Scholar]
  33. Marcelino, N., Agúndez, M., Tercero, B., et al. 2020, A&A, 643, L6 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  34. McGuire, B. A., Shingledecker, C. N., Willis, E. R., et al. 2019, ApJ, 883, 201 [NASA ADS] [CrossRef] [Google Scholar]
  35. Møller, C., & Plesset, M. S. 1934, Phys. Rev., 46, 618 [Google Scholar]
  36. Pardo, J. R., Cernicharo, J., & Serabyn, E. 2001, IEEE Trans. Antennas Propag., 49, 12 [Google Scholar]
  37. Pardo, J. R., Cabezas, C., Fonfría, J. P., et al. 2021, A&A, 652, L13 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  38. Pickett, H. M. 1991, J. Mol. Spectr., 148, 371 [Google Scholar]
  39. Pople, J. A., Head-Gordon, M., & Raghavachari, K. 1987, J. Chem. Phys., 87, 5968 [NASA ADS] [CrossRef] [Google Scholar]
  40. Puzzarini, C. 2008, Chem. Phys., 346, 45 [Google Scholar]
  41. Saito, S., Kawaguchi, K., Yamamoto, S., et al. 1987, ApJ, 317, L115 [NASA ADS] [CrossRef] [Google Scholar]
  42. Schilke, P., Walmsley, C. M., Millar, T. J., & Henkel, C. 1991, A&A, 247, 487 [Google Scholar]
  43. Turner, B. E., Terzieva, R., & Herbst, E. 1999, ApJ, 518, 699 [NASA ADS] [CrossRef] [Google Scholar]
  44. Wakelam, V., Loison, J.-C., Herbst, E., et al. 2015, ApJS, 217, 20 [Google Scholar]
  45. Werner, H. J., Knowles, P. J., Knizia, G., et al. 2020, MOLPRO, version 2020.2 [Google Scholar]
  46. Woon, D. E., & Dunning, T. H., Jr 1993, J. Chem. Phys., 98, 1358 [NASA ADS] [CrossRef] [Google Scholar]
  47. Yamamoto, S., Saito, S., Kawaguchi, K., et al. 1987, ApJ, 317, L119 [Google Scholar]
  48. Yamamoto, S., Saito, S., Kawaguchi, K., et al. 1990, ApJ, 361, 318 [Google Scholar]

Appendix A: Transition frequencies and line parameters for HCCS+ towards TMC-1

Line parameters were derived from a Gaussian fit to the observed lines using GILDAS. Observed frequencies were derived assuming a local standard of rest velocity of 5.83 km s−1.

Table A.1.

Observed lines of HCCS+ towards TMC-1.

All Tables

Table 1.

Spectroscopic parameters of HCCS+, in MHz.

Table A.1.

Observed lines of HCCS+ towards TMC-1.

All Figures

thumbnail Fig. 1.

Spectra of the observed transitions of HCCS+ in TMC-1. The abscissa corresponds to the rest frequency assuming a local standard of rest velocity of 5.83 km s−1. The ordinate is antenna temperature in millikelvin. Blanked channels correspond to negative features produced in the folding of the frequency-switching data. The red lines correspond to the synthetic spectra calculated for a column density of 1.1 × 1012 cm−2 and a rotational temperature of 7.0 K for Nu ≤ 4 and 4.5 K for higher Nu values (see Sect. 3.3).

In the text
thumbnail Fig. 2.

Energy levels of HCCS+ organized by N and J values. The observed transitions are indicated by green arrows.

In the text
thumbnail Fig. 3.

Calculated abundances of CCS and HCCS+ (bottom) and abundance ratio CCS/HCCS+ (top) as a function of time. Dashed lines correspond to a chemical model in which the reaction O + CCS is removed from the chemical network. Observed values are indicated by horizontal dotted lines.

In the text

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