A deep, wide-field search for substellar members in NGC 2264

Kendall, T. R.; Bouvier, J.; Moraux, E.; James, D. J.; Ménard, F.

doi:10.1051/0004-6361:20042164

Cited by 8 publications

(10 citation statements)

References 36 publications

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“…Three of the YBDCs in Table 3 (C33215 = 2MASS J06405674+0938101, C35463 = J06410604+0949232, and C20186 = J06401789+0941546) are in common with the YBDCs listed by Kendall et al (2005). Another object (2MASS J06402759+0945464) could be a YBCD because the star is within the PMS locus of both CMDs and R−Hα is very similar to that of weak line T Tauri stars with X-ray emission.…”

Section: Young Brown Dwarf Candidatesmentioning

confidence: 95%

“…Another object (2MASS J06402759+0945464) could be a YBCD because the star is within the PMS locus of both CMDs and R−Hα is very similar to that of weak line T Tauri stars with X-ray emission. The other 6 YBDCs in Kendall et al (2005) may not be members of NGC 2264 -Three objects (2MASS J06395722+0941011, J06400642+0944197, J06411281+0945529) are fainter than the lower boundary of PMS locus of NGC 2264 (Sung et al 2008). Two (J06401053+0939557, J06413132+0935120) are within the PMS locus in the (I, V − I) diagram, but are below the lower boundary of the PMS locus in the (I, R − I) diagram.…”

Section: Young Brown Dwarf Candidatesmentioning

confidence: 97%

“…The YBDCs in NGC 2264 are therefore still very bright and their photometric characteristics are very similar to those of young low-mass stars. Kendall et al (2005) tried to find the YBDCs in NGC 2264 using deep Iz photometry with CFH12K. Although they tried to find YBDCs in various color-color diagrams and CMDs and through the help of recent model atmospheres, they were unable to find YBDCs confidently due to a lack of reliable membership selection criteria.…”

Section: Young Brown Dwarf Candidatesmentioning

confidence: 99%

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The Initial Mass Function and Young Brown Dwarf Candidates in NGC 2264. Iv. The Initial Mass Function and Star Formation History

Sung

Bessell

2010

The Astronomical Journal

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We have studied the star formation history and the initial mass function (IMF) using the age and mass derived from spectral energy distribution (SED) fitting and from color-magnitude diagrams. We also examined the physical and structural parameters of more than 1,000 pre-main sequence stars in NGC 2264 using the on-line SED fitting tool (SED fitter) of Robitaille et al.We have compared the physical parameters of central stars from SED fitter and other methods. The temperature of the central star is, in many cases, much higher than that expected from its spectral type. The mass and age from SED fitter are not well matched with those from color-magnitude diagrams. We have made some suggestions to improve the accuracy of temperature estimates in SED fitter.In most cases these parameters of individual stars from SED fitter in a star forming region (SFR) or in the whole cluster showed nearly no systematic variation with age or with any other relevant parameter. On the other hand, the median properties of stars in NGC 2264 SFRs showed an evident evolutionary Subject headings: open clusters and associations: individual (NGC 2264) -stars: luminosity function, mass function

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Section: Young Brown Dwarf Candidatesmentioning

confidence: 95%

Section: Young Brown Dwarf Candidatesmentioning

confidence: 97%

Section: Young Brown Dwarf Candidatesmentioning

confidence: 99%

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The Initial Mass Function and Young Brown Dwarf Candidates in NGC 2264. Iv. The Initial Mass Function and Star Formation History

Sung

Bessell

2010

The Astronomical Journal

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“…The substellar population of NGC 2264 remains relatively unexplored given the distance of the cluster. Several deep imaging surveys have been conducted of the region, including that of Sung et al (2004) and Kendall et al (2005). Sung et al (2004) observed NGC 2264 with the CFHT 12K array in the broadband V RI filters and a narrowband Hα filter.…”

Section: The Substellar Population Of Ngc 2264mentioning

confidence: 99%

The Young Cluster and Star Forming Region NGC 2264

Dahm

2008

Preprint

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NGC 2264 is a young Galactic cluster and the dominant component of the Mon OB1 association lying approximately 760 pc distant within the local spiral arm. The cluster is hierarchically structured, with subclusters of suspected members spread across several parsecs. Associated with the cluster is an extensive molecular cloud complex spanning more than two degrees on the sky. The combined mass of the remaining molecular cloud cores upon which the cluster is superposed is estimated to be at least ∼3.7×10 4 M ⊙ . Star formation is ongoing within the region as evidenced by the presence of numerous embedded clusters of protostars, molecular outflows, and Herbig-Haro objects. The stellar population of NGC 2264 is dominated by the O7 V multiple star, S Mon, and several dozen B-type zero-age main sequence stars. X-ray imaging surveys, Hα emission surveys, and photometric variability studies have identified more than 600 intermediate and low-mass members distributed throughout the molecular cloud complex, but concentrated within two densely populated areas between S Mon and the Cone Nebula. Estimates for the total stellar population of the cluster range as high as 1000 members and limited deep photometric surveys have identified ∼230 substellar mass candidates. The median age of NGC 2264 is estimated to be ∼3 Myr by fitting various pre-main sequence isochrones to the low-mass stellar population, but an apparent age dispersion of at least ∼5 Myr can be inferred from the broadened sequence of suspected members. Infrared and millimeter observations of the cluster have identified two prominent sites of star formation activity centered near NGC 2264 IRS1, a deeply embedded early-type (B2-B5) star, and IRS2, a star forming core and associated protostellar cluster. NGC 2264 and its associated molecular clouds have been extensively examined at all wavelengths, from the centimeter regime to X-rays. Given its relative proximity, well-defined stellar population, and low foreground extinction, the cluster will remain a prime candidate for star formation studies throughout the foreseeable future.

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“…NGC 2264 is a diverse star forming region that has the potential to provide this large sample, but currently lacks the spectroscopic observations needed for detailed characterisation. Several purely photometric surveys have probed the substellar domain, including Lamm et al (2004); Kendall et al (2005); Sung & Bessell (2010). We have recently published the first photometric study identifying brown dwarf candidates down to estimated masses of 0.02 ⊙ , using multi-epoch, multiwavelength data from CTIO/Blanco, KPNO/FLAMINGOS, and Spitzer/IRAC (Pearson et al 2020).…”

Section: Introductionmentioning

confidence: 99%

The first spectroscopically confirmed brown dwarfs in NGC 2264

Pearson,

Scholz,

Teixeira

et al. 2021

Preprint

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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 ⊙ . 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 ⊙ . 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 = 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.

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A deep, wide-field search for substellar members in NGC 2264

Cited by 8 publications

References 36 publications

The Initial Mass Function and Young Brown Dwarf Candidates in NGC 2264. Iv. The Initial Mass Function and Star Formation History

The Initial Mass Function and Young Brown Dwarf Candidates in NGC 2264. Iv. The Initial Mass Function and Star Formation History

The Young Cluster and Star Forming Region NGC 2264

The first spectroscopically confirmed brown dwarfs in NGC 2264

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