| Download | - View final version: An ALMA search for substructure and fragmentation in starless cores in Orion B North (PDF, 5.6 MiB)
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| DOI | Resolve DOI: https://doi.org/10.3847/1538-4357/ad3d56 |
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| Author | Search for: Fielder, Samuel D.ORCID identifier: https://orcid.org/0009-0001-8625-505X; Search for: Kirk, Helen1ORCID identifier: https://orcid.org/0000-0002-5779-8549; Search for: Dunham, Michael M.ORCID identifier: https://orcid.org/0000-0003-0749-9505; Search for: Offner, Stella S. R.ORCID identifier: https://orcid.org/0000-0003-1252-9916 |
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| Affiliation | - National Research Council of Canada. Herzberg Astronomy and Astrophysics
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| Funder | Search for: Natural Sciences and Engineering Research Council of Canada |
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| Format | Text, Article |
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| Subject | star formation; molecular clouds; collapsing clouds; star forming regions; radio interferometry; millimeter astronomy; submillimeter astronomy; dust continuum emission |
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| Abstract | We present Atacama Large Millimeter/submillimeter Array (ALMA) Cycle 3 observations of 73 starless and protostellar cores in the Orion B North molecular cloud. We detect a total of 34 continuum sources at 106 GHz, and after comparisons with other data, four of these sources appear to be starless. Three of the four sources are located near groupings of protostellar sources, while one source is an isolated detection. We use synthetic observations of a simulation modeling a collapsing turbulent, magnetized core to compute the expected number of starless cores that should be detectable with our ALMA observations and find at least two (1.52) starless cores should be detectable (at 5σ), consistent with our data. We run a simple virial analysis of the cores to put the Orion B North observations into context with similar previous ALMA surveys of cores in Chamaeleon I and Ophiuchus. We conclude that the Chamaeleon I starless core population is characteristically less bounded than the other two populations, along with external pressure contributions dominating the binding energy of the cores. These differences may explain why the Chamaeleon I cores do not follow turbulent model predictions, while the Ophiuchus and Orion B North cores are consistent with the model. |
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| Publication date | 2024-06-04 |
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| Publisher | American Astronomical Society |
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| Licence | |
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| Language | English |
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| Peer reviewed | Yes |
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| Export citation | Export as RIS |
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| Report a correction | Report a correction (opens in a new tab) |
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| Record identifier | c3fce224-e6e8-4495-9257-cf0593b6dbfa |
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| Record created | 2024-09-06 |
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| Record modified | 2024-09-06 |
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