Protoplanetary disk masses in the young NGC 2024 cluster

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DOIResolve DOI: http://doi.org/10.1088/0004-637X/802/2/77
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TypeArticle
Journal titleThe Astrophysical Journal
ISSN0004-637X
Volume802
Issue2
Article number77
AbstractWe present the results from a Submillimeter Array survey of the 887 μm continuum emission from the protoplanetary disks around 95 young stars in the young cluster NGC 2024. Emission was detected from 22 infrared sources, with flux densities from ∼5 to 330 mJy; upper limits (at 3σ) for the other 73 sources range from 3 to 24 mJy. For standard assumptions, the corresponding disk masses range from ∼0.003 to 0.2 M⊙, with upper limits at 0.002-0.01 M⊙. The NGC 2024 sample has a slightly more populated tail at the high end of its disk mass distribution compared to other clusters, but without more information on the nature of the sample hosts it remains unclear if this difference is statistically significant or a superficial selection effect. Unlike in the Orion Trapezium, there is no evidence for a disk mass dependence on the (projected) separation from the massive star IRS 2b in the NGC 2024 cluster. We suggest that this is due to either the cluster youth or a comparatively weaker photoionizing radiation field.
Publication date
PublisherIOP Science
LanguageEnglish
AffiliationNational Research Council Canada; National Science Infrastructure
Peer reviewedYes
NPARC number21275698
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Record identifierbee8632f-52dd-46b6-b432-4b9c48cce949
Record created2015-07-14
Record modified2016-07-18
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