Mapping Interstellar Ice Inventory toward Class 0 Protostars in Star-forming Region Orion A with JWST Data: Laboratory ice analogue IR spectra
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2026
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| _version_ | 1866902307716726784 |
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| author | Petrashkevich, Igor Pavlyuchenkov, Yaroslav Punanova, Anna Ozhiganov, Maksim Nakibov, Ruslan Karteyeva, Varvara Salii, Svetlana Sobolev, Andrey Medvedev, Mikhail Vasyunin, Anton |
| author_facet | Petrashkevich, Igor Pavlyuchenkov, Yaroslav Punanova, Anna Ozhiganov, Maksim Nakibov, Ruslan Karteyeva, Varvara Salii, Svetlana Sobolev, Andrey Medvedev, Mikhail Vasyunin, Anton |
| contents | <p>The laboratory spectra of CH3OH (at 10~K) and NH4+OCN- (at 10 K and 120 K) obtained with the ISEAge using transmission method (Ozhiganov et al. 2024).<br><br>The pure CH3OH was deposited at a rate of 1.43×10^13 molecules cm^−2 s^−1 for 60 minutes onto a germanium substrate cooled to 10 K, resulting in a total column density of 5.15×10^16 cm−2. Following the deposition, the IR spectrum of the CH3OH ice was recorded with 128 scans. The spectra of the NH4+ OCN− salt (the product of the NH3 + HNCO = NH4+ OCN− reaction) were obtained by co-depositing ammonia (NH3) and HNCO onto a 10 K substrate. Deposition rates were 5.50×10^13 molecules cm−2 s−1 for NH3 and 2.37×10^13 molecules cm^−2 s^−1 for HNCO, supported for 30 minutes. The resulting ice contained NH3, HNCO, and NH4+ OCN− in a molecular ratio of 6:1:3, determined from the NH3 umbrella band (with the band strength of A’=1.95×10^−17 cm, Hudson et al. 2022), the HNCO band (A’=1.29×10^−16 cm, Hudson et al. 2024), and the OCN− band (A’=1.5×10^−16 cm, Gerakines et al. 2025). Subsequently, we heated the ice at a rate of 5 K min−1 to 200 K while continuously collecting IR spectra with 32 scans per spectrum, which corresponds to an averaging of 45 seconds.</p> |
| format | Recurso digital |
| id | zenodo_https___doi_org_10_5281_zenodo_20346324 |
| institution | Zenodo |
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| publishDate | 2026 |
| publisher | Zenodo |
| record_format | zenodo |
| spellingShingle | Mapping Interstellar Ice Inventory toward Class 0 Protostars in Star-forming Region Orion A with JWST Data: Laboratory ice analogue IR spectra Petrashkevich, Igor Pavlyuchenkov, Yaroslav Punanova, Anna Ozhiganov, Maksim Nakibov, Ruslan Karteyeva, Varvara Salii, Svetlana Sobolev, Andrey Medvedev, Mikhail Vasyunin, Anton <p>The laboratory spectra of CH3OH (at 10~K) and NH4+OCN- (at 10 K and 120 K) obtained with the ISEAge using transmission method (Ozhiganov et al. 2024).<br><br>The pure CH3OH was deposited at a rate of 1.43×10^13 molecules cm^−2 s^−1 for 60 minutes onto a germanium substrate cooled to 10 K, resulting in a total column density of 5.15×10^16 cm−2. Following the deposition, the IR spectrum of the CH3OH ice was recorded with 128 scans. The spectra of the NH4+ OCN− salt (the product of the NH3 + HNCO = NH4+ OCN− reaction) were obtained by co-depositing ammonia (NH3) and HNCO onto a 10 K substrate. Deposition rates were 5.50×10^13 molecules cm−2 s−1 for NH3 and 2.37×10^13 molecules cm^−2 s^−1 for HNCO, supported for 30 minutes. The resulting ice contained NH3, HNCO, and NH4+ OCN− in a molecular ratio of 6:1:3, determined from the NH3 umbrella band (with the band strength of A’=1.95×10^−17 cm, Hudson et al. 2022), the HNCO band (A’=1.29×10^−16 cm, Hudson et al. 2024), and the OCN− band (A’=1.5×10^−16 cm, Gerakines et al. 2025). Subsequently, we heated the ice at a rate of 5 K min−1 to 200 K while continuously collecting IR spectra with 32 scans per spectrum, which corresponds to an averaging of 45 seconds.</p> |
| title | Mapping Interstellar Ice Inventory toward Class 0 Protostars in Star-forming Region Orion A with JWST Data: Laboratory ice analogue IR spectra |
| url | https://doi.org/10.5281/zenodo.20346324 |