A Constraint on the Formation Timescale of the Young Open Cluster NGC 2264: Lithium Abundance of Pre-Main Sequence Stars

Lim, Beomdu; Sung, Hwankyung; Kim, Jinyoung Serena; Bessell, M. S.; Hwang, Narae; Park, Byeong-Gon

doi:10.3847/0004-637x/831/2/116

Cited by 18 publications

(15 citation statements)

References 85 publications

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“…The numbers (median ages) reported in Table 2 suggest that a spread of 4-5 Myr exists among cluster members (see also Getman et al 2014). This is compatible with the age spread estimated by Lim et al (2016) from the Li abundances of NGC 2264 PMS objects (although Bouvier et al 2016 examined the dispersion of EW(Li) for K4-M0 WTTS in NGC 2264 from GESiDR4 data and concluded that this scatter is likely not caused by an age spread).…”

Section: Regionsupporting

confidence: 71%

The Gaia-ESO Survey and CSI 2264: Substructures, disks, and sequential star formation in the young open cluster NGC 2264

Venuti

Prisinzano

Sacco

et al. 2017

A&A

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Context. Reconstructing the structure and history of young clusters is pivotal to understanding the mechanisms and timescales of early stellar evolution and planet formation. Recent studies suggest that star clusters often exhibit a hierarchical structure, possibly resulting from several star formation episodes occurring sequentially rather than a monolithic cloud collapse. Aims. We aim to explore the structure of the open cluster and star-forming region NGC 2264 ("3 Myr), which is one of the youngest, richest and most accessible star clusters in the local spiral arm of our Galaxy; we link the spatial distribution of cluster members to other stellar properties such as age and evolutionary stage to probe the star formation history within the region. Methods. We combined spectroscopic data obtained as part of the Gaia-ESO Survey (GES) with multi-wavelength photometric data from the Coordinated Synoptic Investigation of NGC 2264 (CSI 2264) campaign. We examined a sample of 655 cluster members, with masses between 0.2 and 1.8 M d and including both disk-bearing and disk-free young stars. We used T eff estimates from GES and g, r, i photometry from CSI 2264 to derive individual extinction and stellar parameters. Results. We find a significant age spread of 4-5 Myr among cluster members. Disk-bearing objects are statistically associated with younger isochronal ages than disk-free sources. The cluster has a hierarchical structure, with two main blocks along its latitudinal extension. The northern half develops around the O-type binary star S Mon; the southern half, close to the tip of the Cone Nebula, contains the most embedded regions of NGC 2264, populated mainly by objects with disks and ongoing accretion. The median ages of objects at different locations within the cluster, and the spatial distribution of disked and non-disked sources, suggest that star formation began in the north of the cluster, over 5 Myr ago, and was ignited in its southern region a few Myr later. Star formation is likely still ongoing in the most embedded regions of the cluster, while the outer regions host a widespread population of more evolved objects; these may be the result of an earlier star formation episode followed by outward migration on timescales of a few Myr. We find a detectable lag between the typical age of disk-bearing objects and that of accreting objects in the inner regions of NGC 2264: the first tend to be older than the second, but younger than disk-free sources at similar locations within the cluster. This supports earlier findings that the characteristic timescales of disk accretion are shorter than those of disk dispersal, and smaller than the average age of NGC 2264 (i.e., À3 Myr). At the same time, we note that disks in the north of the cluster tend to be shorter-lived ("2.5 Myr) than elsewhere; this may reflect the impact of massive stars within the region (notably S Mon), that trigger rapid disk dispersal. Conclusions. Our results, consistent with earlier studies on NGC 2264 and other young clusters, suppor...

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Section: Regionsupporting

confidence: 71%

The Gaia-ESO Survey and CSI 2264: Substructures, disks, and sequential star formation in the young open cluster NGC 2264

Venuti

Prisinzano

Sacco

et al. 2017

A&A

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“…The mean age and age spread of Stock 8 is 6.5 ± 0.2 dex or 3.16 (+1.85 -1.16) Myr. The contribution from the true age spread due to star formation history of the cluster is comparable to other star forming regions such as W3-main (2-3 Myr;Bik et al 2012) andNGC2264 (3-4 Myr;Lim et al 2016). The luminosity spread corresponding to the 1σ observed age spread at V − I= 2.5 mag is 0.24 dex.…”

Section: Probable Causes Of the Apparent Age Spreadsupporting

confidence: 49%

The Low-mass Population in the Young Cluster Stock 8: Stellar Properties and Initial Mass Function

Jose

Herczeg

Samal

et al. 2017

ApJ

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The evolution of Hii regions/supershells can trigger a new generation of stars/clusters at their peripheries, with environmental conditions that may affect the initial mass function, disk evolution and star formation efficiency. In this paper we study the stellar content and star formation processes in the young cluster Stock 8, which itself is thought to be formed during the expansion of a supershell. We present deep optical photometry along with JHK and 3.6, 4.5 µm photometry from UKIDSS and Spitzer-IRAC. We use multi-color criteria to identify the candidate young stellar objects in the region. Using evolutionary models, we obtain a median log(age) of ∼6.5 (∼3.0 Myr) with an observed age spread of ∼0.25 dex for the cluster. Monte Carlo simulations of the population of Stock 8, based on estimates for the photometric uncertainty, differential reddening, binarity, and variability, indicate that these uncertainties introduce an age spread of ∼0.15 dex. The intrinsic age spread in the cluster is ∼0.2 dex. The fraction of young stellar objects surrounded by disk is ∼35%. The K-band luminosity function of Stock 8 is similar to that of the Trapezium cluster. The IMF of Stock 8 has a Salpeterlike slope at > 0.5 M ⊙ and the IMF flattens and peaks at ∼0.4 M ⊙ , below which declines into the substellar regime. Although Stock 8 is surrounded by several massive stars, there seems to be no severe environmental effect in the form of IMF due to the proximity of massive stars around the cluster.

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“…KH 15D is a pre-main sequence (PMS) spectroscopic binary (A+B) with near-equal-mass components (0.715M ⊙ for Star A and 0.74M ⊙ for Star B), high eccentricity (e ≈ 0.6), a semi-major axis of ∼0.25 au, and a period of 48.37 days Winn et al 2006;Aronow et al 2018). It is a member of the NGC 2264 cluster which is at ∼ 750 pc, based on the members from Venuti et al 2018 and Gaia Data Release 2 parallaxes, and the cluster is about ∼2-6 Myr old (Naylor 2009;Lim et al 2016). KH 15D exhibits unique and dramatic long and short term photometric variability (e.g., Capelo et al 2012).…”

Section: Introductionmentioning

confidence: 99%

Double-peaked [O i] Profile: A Likely Signature of the Gaseous Ring around KH 15D

Fang

Pascucci

Kim

et al. 2019

ApJL

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KH 15D is a well-known spectroscopic binary because of its unique and dramatic photometric variability. The variability is explained by a circumbinary dust ring but the ring itself was never directly detected. We present a new interpretation of the double-peaked [O I] λ6300 profiles as originating from the hot disk surface of KH 15D. By modeling these profiles, we measure emitting radii between ∼0.5-5 au, basically a gaseous ring very similar in radial extent to the dust ring inferred from modeling the system's photometric variability. We also discuss the possibility that external photoevaporation driven by UV photons from the nearby massive star HD 47887 has truncated the outer edge of the disk to the observed value.

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A Constraint on the Formation Timescale of the Young Open Cluster NGC 2264: Lithium Abundance of Pre-Main Sequence Stars

Cited by 18 publications

References 85 publications

The Gaia-ESO Survey and CSI 2264: Substructures, disks, and sequential star formation in the young open cluster NGC 2264

The Gaia-ESO Survey and CSI 2264: Substructures, disks, and sequential star formation in the young open cluster NGC 2264

The Low-mass Population in the Young Cluster Stock 8: Stellar Properties and Initial Mass Function

Double-peaked [O i] Profile: A Likely Signature of the Gaseous Ring around KH 15D

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