Erratum: Gas phase SiO in the circumstellar environment of the recurrent nova T Coronae Borealis (Monthly Notices of the Royal Astronomical Society DOI: 10.1093/mnras/stz1071)

A. Evans, Ya V. Pavlenko, D. P.K. Banerjee, U. Munari, R. D. Gehrz, C. E. Woodward, S. Starrfield, L. A. Helton, M. Shahbandeh, S. Davis, S. Dallaporta, G. Cherini

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In Evans et al. ( 2019 ), we reported the disco v ery of gas-phase SiO in the wind of the red giant component of the recurrent nova T CrB. This conclusion, which we now consider to be incorrect, was based on the Spitzer Space Telescope IRS spectrum of T CrB. This has an absorption feature at 8 μm, attribted to the SiO fundamental transition. An attempt to fit this feature with a model atmosphere revealed that an additional component was needed, which was attributed to a contribution to the absorption feature from SiO in the wind from the red giant component of T CrB. The fit of the 8 μm feature by Evans et al. included the contribution of the 28 SiO isotopologue only. Ho we ver when the isotopic ratios for Si reported by Pavlenko et al. ( 2020 ) are included in the analysis, the photospheric model matches the observed SiO feature well, without the need for a wind. The reason for the present result is that absorption in the 28 SiO fundamental is saturated. If only the 28 SiO isotopologue is included in the model atmosphere calculation, as in Evans et al. ( 2019 ), an additional component from 28 SiO in the red giant wind is needed to match the observed absorption. Ho we ver the addition of even small amounts of the (unsaturated) 29 SiO and 30 SiO isotopologues, corresponding to the Si isotopic ratios reported in Pavlenko et al. ( 2020 ), makes up the difference between theory and observation. The need for the wind is therefore remo v ed. The revised fit is shown in Fig. 1, which assumes (as in Evans et al. 2019 ), an ef fecti ve temperature T eff = 3600 K, gravity log g = 1 and microturbulent velocity V t = 2 km s -1 for the red giant. Clearly the photospheric model, with the added SiO isotopologues, fits the data well. {Graph presented} The same considerations apply to the fit of the CO fundamental and the SiO first o v ertone, shown in fig. 6 of Evans et al. ( 2019 ). Note that the Spitzer IRS data reach only as far as the red wing of the observed absorption feature. The fit with the less abundant Si and C isotopes is shown in Fig. 2 . {Graph presented} DATA AVAILABILITY The data in this paper are available from the Spitzer Space Telescope Archive.

Original languageEnglish (US)
Pages (from-to)56-57
Number of pages2
JournalMonthly Notices of the Royal Astronomical Society
Issue number1
StatePublished - May 1 2022

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