Observational bias and young massive cluster characterization − II. Can Gaia accurately observe young clusters and associations?
dc.contributor.author | Buckner, ASM | |
dc.contributor.author | Naylor, T | |
dc.contributor.author | Dobbs, CL | |
dc.contributor.author | Rieder, S | |
dc.contributor.author | Bending, TJR | |
dc.date.accessioned | 2024-05-23T13:23:02Z | |
dc.date.issued | 2023-11-03 | |
dc.date.updated | 2024-05-23T11:20:34Z | |
dc.description.abstract | Observations of clusters suffer from issues such as completeness, projection effects, resolving individual stars, and extinction. As such, how accurate measurements and conclusions are likely to be? Here, we take cluster simulations (Westerlund2-and Orion-Type), synthetically observe them to obtain luminosities, accounting for extinction, and the inherent limits of Gaia, then place them within the real Gaia DR3 catalogue. We then attempt to rediscover the clusters at distances of between 500 and 4300 pc. We show the spatial and kinematic criteria that are best able to pick out the simulated clusters, maximizing completeness, and minimizing contamination. We then compare the properties of the 'observed' clusters with the original simulations. We looked at the degree of clustering, the identification of clusters and subclusters within the data sets, and whether the clusters are expanding or contracting. Even with a high level of incompleteness (e.g. stellar members identified), similar qualitative conclusions tend to be reached compared to the original data set, but most quantitative conclusions are likely to be inaccurate. Accurate determination of the number, stellar membership, and kinematic properties of subclusters are the most problematic to correctly determine, particularly at larger distances due to the disappearance of cluster substructure as the data become more incomplete, but also at smaller distances where the misidentification of asterisms as true structure can be problematic. Unsurprisingly, we tend to obtain better quantitative agreement of properties for our more massive Westerlund2-Type cluster. We also make optical style images of the clusters over our range of distances. | en_GB |
dc.description.sponsorship | European Union Horizon 2020 | en_GB |
dc.format.extent | 5448-5463 | |
dc.identifier.citation | Vol. 527(3), pp. 5448-5463 | en_GB |
dc.identifier.doi | https://doi.org/10.1093/mnras/stad3367 | |
dc.identifier.grantnumber | 818940 | en_GB |
dc.identifier.grantnumber | 833925 | en_GB |
dc.identifier.uri | http://hdl.handle.net/10871/136023 | |
dc.identifier | ORCID: 0000-0002-0506-8501 (Naylor, Tim) | |
dc.identifier | ORCID: 0000-0002-4578-297X (Dobbs, Clare L) | |
dc.identifier | ResearcherID: K-8649-2014 (Dobbs, Clare L) | |
dc.language.iso | en | en_GB |
dc.publisher | Oxford University Press (OUP) / Royal Astronomical Society | en_GB |
dc.relation.url | https://zenodo.org/records/10053996 | en_GB |
dc.rights | © The Author(s) 2023. Published by Oxford University Press on behalf of Royal Astronomical Society. This is an Open Access article distributed under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited. | en_GB |
dc.subject | methods: data analysis | en_GB |
dc.subject | methods: numerical | en_GB |
dc.subject | methods: observational | en_GB |
dc.subject | methods: statistical | en_GB |
dc.subject | stars: statistics | en_GB |
dc.subject | open clusters and associations: general | en_GB |
dc.title | Observational bias and young massive cluster characterization − II. Can Gaia accurately observe young clusters and associations? | en_GB |
dc.type | Article | en_GB |
dc.date.available | 2024-05-23T13:23:02Z | |
dc.identifier.issn | 0035-8711 | |
dc.description | This is the final version. Available on open access from Oxford University Press via the DOI in this record | en_GB |
dc.description | Data availability: The final stage field-of-view files, from which stellar members are selected, at 500, 2500, and 4300 pc for all three clusters are available to download from the Zenodo repository at https://zenodo.org/records/10053996. Additional distances and analysis data underlying this article will be shared on reasonable request to the corresponding author. The simulation data underlying this article were provided by CLD by permission, which will be shared on request to the corresponding author with permission of CLD. | en_GB |
dc.identifier.eissn | 1365-2966 | |
dc.identifier.journal | Monthly Notices of the Royal Astronomical Society | en_GB |
dc.relation.ispartof | Monthly Notices of the Royal Astronomical Society, 527(3) | |
dc.rights.uri | https://creativecommons.org/licenses/by/4.0/ | en_GB |
dcterms.dateAccepted | 2023-10-26 | |
rioxxterms.version | VoR | en_GB |
rioxxterms.licenseref.startdate | 2023-11-03 | |
rioxxterms.type | Journal Article/Review | en_GB |
refterms.dateFCD | 2024-05-23T13:20:38Z | |
refterms.versionFCD | VoR | |
refterms.dateFOA | 2024-05-23T13:24:00Z | |
refterms.panel | B | en_GB |
refterms.dateFirstOnline | 2023-11-03 |
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Except where otherwise noted, this item's licence is described as © The Author(s) 2023. Published by Oxford University Press on behalf of Royal Astronomical Society. This is an Open Access article distributed under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited.