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The first spectroscopically confirmed brown dwarfs in NGC 2264
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dc.contributor.author | Pearson, Samuel | |
dc.contributor.author | Scholz, Aleks | |
dc.contributor.author | Teixeira, Paula S | |
dc.contributor.author | Mužić, Koraljka | |
dc.contributor.author | Almendros-Abad, Víctor | |
dc.date.accessioned | 2021-09-24T11:30:03Z | |
dc.date.available | 2021-09-24T11:30:03Z | |
dc.date.issued | 2021-11 | |
dc.identifier | 275628998 | |
dc.identifier | daa8dce6-9064-48b4-aef8-be45bbe84d48 | |
dc.identifier | 85117198077 | |
dc.identifier | 000708848000065 | |
dc.identifier.citation | Pearson , S , Scholz , A , Teixeira , P S , Mužić , K & Almendros-Abad , V 2021 , ' The first spectroscopically confirmed brown dwarfs in NGC 2264 ' , Monthly Notices of the Royal Astronomical Society , vol. 507 , no. 3 , pp. 4074–4085 . https://doi.org/10.1093/mnras/stab2394 | en |
dc.identifier.issn | 0035-8711 | |
dc.identifier.other | Bibtex: 10.1093/mnras/stab2394 | |
dc.identifier.other | ORCID: /0000-0002-3665-5784/work/100549756 | |
dc.identifier.uri | https://hdl.handle.net/10023/24020 | |
dc.description | Support from STFC through grant number ST/R000824/1. K.M. acknowledges funding by the Science and Technology Foundation of Portugal (FCT), grants No. IF/00194/2015, PTDC/FISAST/28731/2017 and UIDB/00099/2020. | en |
dc.description.abstract | We present spectroscopic follow-up observations of 68 red, faint candidates from our multi-epoch, multi-wavelength, previously published survey of NGC 2264. Using near-infrared spectra from VLT/KMOS, we measure spectral types and extinction for 32 young low-mass sources. We confirm 13 as brown dwarfs in NGC 2264, with spectral types between M6 and M8, corresponding to masses between 0.02 and 0.08 M⊙. These are the first spectroscopically confirmed brown dwarfs in this benchmark cluster. 19 more objects are found to be young M-type stars of NGC 2264 with masses of 0.08 to 0.3 M⊙. 7 of the confirmed brown dwarfs as well as 15 of the M-stars have IR excess caused by a disc. Comparing with isochrones, the typical age of the confirmed brown dwarfs is <0.5 to 5 Myr. More than half of the newly identified brown dwarfs and very low mass stars have ages <0.5 Myr, significantly younger than the bulk of the known cluster population. Based on the success rate of our spectroscopic follow-up, we estimate that NGC 2264 hosts 200-600 brown dwarfs in total (in the given mass range). This would correspond to a star-to-brown dwarf ratio between 2.5:1 and 7.5:1. We determine the slope of the substellar mass function as α=0.43+0.41−0.56, these values are consistent with those measured for other young clusters. This points to a uniform substellar mass function across all star forming environments. | |
dc.format.extent | 7990394 | |
dc.language.iso | eng | |
dc.relation.ispartof | Monthly Notices of the Royal Astronomical Society | en |
dc.subject | Brown dwardfs | en |
dc.subject | Stars: low-mass | en |
dc.subject | Catalogues | en |
dc.subject | Surveys | en |
dc.subject | QB Astronomy | en |
dc.subject | QC Physics | en |
dc.subject | DAS | en |
dc.subject.lcc | QB | en |
dc.subject.lcc | QC | en |
dc.title | The first spectroscopically confirmed brown dwarfs in NGC 2264 | en |
dc.type | Journal article | en |
dc.contributor.sponsor | Science & Technology Facilities Council | en |
dc.contributor.institution | University of St Andrews. School of Physics and Astronomy | en |
dc.contributor.institution | University of St Andrews. St Andrews Centre for Exoplanet Science | en |
dc.identifier.doi | 10.1093/mnras/stab2394 | |
dc.description.status | Peer reviewed | en |
dc.identifier.grantnumber | ST/R00824/1 | en |
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