Table · dataset · 2024
SOMA carbon-chain chemistry of IM protostars
Listed in IVOA Registry (Virtual Observatory)
Evidence for similar chemical characteristics around low- and high-mass protostars has been found: in particular, a variety of carbon-chain species and complex organic molecules (COMs) are formed around them.
Description
On the other hand, the chemical compositions around intermediate-mass (IM) protostars (2M_{sun}_<m*<8M_{sun}_) protostars have not been studied with large samples. In particular, it is unclear the extent to which carbon-chain species are formed around them.
We aim to obtain the chemical compositions, particularly focusing on carbon-chain species, towards a sample of IM protostars. Another purpose is deriving the rotational temperatures of HC5N to confirm whether carbon-chain species are formed in the warm gas around these stars. We have conducted Q-band (31.5-50GHz) line survey observations towards eleven mainly intermediate-mass protostars with the Yebes 40m radio telescope.
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The target protostars were selected from a sub-sample of the source list of the SOFIA Massive (SOMA) Star Formation project. Assuming local thermodynamic equilibrium (LTE), we have derived column densities of the detected molecules and rotational temperatures of HC_5_N and CH_3_OH. Nine carbon-chain species (HC_3_N, HC_5_N, C_3_H, C_4_H, linear-H_2_CCC, cyclic-C_3_H_2_, CCS, C_3_S, and CH__3CCH), three COMs (CH_3_OH, CH_3_CHO, and CH_3_CN), H_2_CCO, HNCO, and four simple sulfur (S)-bearing species (^13^CS, C^34^S, HCS+, H_2_CS) have been detected.
The rotational temperatures of HC_5_N are derived to be ~20-30K in three IM protostars (Cepheus E, HH288, and IRAS 20293+3952). The rotational temperatures of CH_3_OH are derived in five IM sources and found to be similar to those of HC_5_N. The rotational temperatures of HC_5_N around the three IM protostars are very similar compared to those around low- and high-mass protostars.
These results indicate that carbon-chain molecules are formed in lukewarm (~20-30K) gas around the IM protostars by the Warm Carbon-Chain Chemistry (WCCC) process. Thus, carbon-chain formation occurs ubiquitously in the warm gas around protostars across a wide range of stellar masses. Carbon-chain molecules and COMs coexist around most of the target IM protostars, which is similar to the situation in low- and high-mass protostars.
In summary, the chemical characteristics around protostars are common in the low-, intermediate- and high-mass regimes.
Links
Where it is published
- Reference page cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/692/A65 ↗
landing page · from IVOA Registry
Documentation and papers
- ADS 2024A&A...692A..65T ui.adsabs.harvard.edu/abs/2024A%26A...692A..65T ↗
publication · from IVOA Registry
Catalogue records · 2
- VOResource record dc.g-vo.org/oai.xml?verb=GetRecord&metadataPrefix=ivo_vor&identifier=ivo%3… ↗
metadata API · from IVOA Registry
- Registry record (GAVO) dc.g-vo.org/I/cds.vizier/j/a%2Ba/692/a65 ↗
catalogue entry · from IVOA Registry
Topics
- Stated by source
- Radio
- From keywords
- Astronomy & Astrophysics
Provenance · 1 source records, 8 field assertions
| Source | Key | Last seen | Raw |
|---|---|---|---|
| IVOA Registry (Virtual Observatory) | ivo://cds.vizier/j/a+a/692/a65 | 14 d ago | JSON v1 |
| Field | Assertion | Extractor | Evidence |
|---|---|---|---|
| access_level | source · IVOA Registry | connector:ivoa_registry@1.0.0 | |
| concepts[field].local:field:astronomy | mapping · IVOA Registry | connector:ivoa_registry@1.0.0 | |
| concepts[modality].ivoa_waveband:radio | source · IVOA Registry | connector:ivoa_registry@1.0.0 | |
| description | source · IVOA Registry | connector:ivoa_registry@1.0.0 | rr.resource.res_description |
| license_text | source · IVOA Registry | connector:ivoa_registry@1.0.0 | |
| publication_date | source · IVOA Registry | connector:ivoa_registry@1.0.0 | |
| title | source · IVOA Registry | connector:ivoa_registry@1.0.0 | rr.resource.res_title |
| updated_date | source · IVOA Registry | connector:ivoa_registry@1.0.0 |