Data mining in the young open cluster IC 2391

Dodd, R. J.

doi:10.1111/j.1365-2966.2004.08378.x

Cited by 15 publications

(38 citation statements)

References 30 publications

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“…There are possibly as many as 125 members of IC 2391 (Dodd 2004). We analyze only seven of these members.…”

Section: Samplementioning

confidence: 99%

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Differential Radial Velocities and Stellar Parameters of Nearby Young Stars

Paulson¹,

Yelda

2006

PUBL ASTRON SOC PAC

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ABSTRACT. Radial velocity searches for substellar-mass companions have focused primarily on stars older than 1 Gyr. Increased levels of stellar activity in young stars hinders the detection of solar system analogs, and therefore until recently there has been a prejudice against inclusion of young stars in radial velocity surveys. Adaptive optics surveys of young stars have given us insight into the multiplicity of young stars, but only for massive, distant companions. Understanding the limit of the radial velocity technique, restricted to high-mass, close-orbiting planets and brown dwarfs, we began a survey of young stars of various ages. While the number of stars needed to carry out full analysis of the problems of planetary and brown dwarf population and evolution is large, the beginning of such a sample is included here. We report on 61 young stars ranging in age from the b Pictoris association (∼12 Myr) to the Ursa Major association (∼300 Myr). This initial search resulted in no stars showing evidence of companions larger than ∼1M Jup -2M Jup in short-period orbits at the 3 j level. We also present derived stellar parameters, as most have unpublished values. The chemical homogeneity of a cluster, and presumably of an association, may help to constrain true membership, so we present [Fe/H] abundances for the stars in our sample.

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“…There are possibly as many as 125 members of IC 2391 (Dodd 2004). We analyze only seven of these members.…”

Section: Samplementioning

confidence: 99%

“…IC 2391 is a cluster ∼30-50 Myr old (Mermilliod 1981;Barrado y Navascués et al 2004;Patten & Simon 1996) at a distance of ∼150 pc (Dodd 2004;Stauffer et al 1989). There are possibly as many as 125 members of IC 2391 (Dodd 2004).…”

Section: Samplementioning

confidence: 99%

Differential Radial Velocities and Stellar Parameters of Nearby Young Stars

Paulson¹,

Yelda

2006

PUBL ASTRON SOC PAC

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“…Because of its proximity and youth, this cluster has been subject to several studies (e.g., Barrado y Navascués et al 2004Koen & Ishihara 2006;Siegler et al 2007;Platais et al 2007). Barrado y Navascués et al (2004) and Dodd (2004) measured the MF down to the substellar limit, but the MF for confirmed member with a completeness limit at lower masses has not yet been determined.…”

Section: Introductionmentioning

confidence: 99%

A Constraint on Brown Dwarf Formation via Ejection: Radial Variation of the Stellar and Substellar Mass Function of the Young Open Cluster Ic 2391

Boudreault

Bailer‐Jones

2009

ApJ

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We present the stellar and substellar mass function (MF) of the open cluster IC 2391, plus its radial dependence, and use this to put constraints on the formation mechanism of brown dwarfs (BDs). Our multi-band optical and infrared photometric survey with spectroscopic follow-up covers 11 deg 2 , making it the largest survey of this cluster to date. We observe a radial variation in the MF over the range 0.072-0.3 M , but no significant variation in the MF below the substellar boundary at the three cluster radius intervals is analyzed. This lack of radial variation for low masses is what we would expect with the ejection scenario for BD formation, although considering that IC 2391 has an age about three times older than its crossing time, we expect that BDs with a velocity greater than the escape velocity have already escaped the cluster. Alternatively, the variation in the MF of the stellar objects could be an indication that they have undergone mass segregation via dynamical evolution. We also observe a significant variation across the cluster in the color of the (background) field star locus in colormagnitude diagrams and conclude that this is due to variable background extinction in the Galactic plane. From our preliminary spectroscopic follow-up, to confirm BD status and cluster membership, we find that all candidates are M dwarfs (in either the field or the cluster), demonstrating the efficiency of our photometric selection method in avoiding contaminants (e.g., red giants). About half of our photometric candidates for which we have spectra are spectroscopically confirmed as cluster members; two are new spectroscopically confirmed BD members of IC 2391.

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“…Because of the low precision, we were unable to calculate the probability of membership for the standard method described in Moraux et al (2003). Consequently, we only selected objects to be proper motion members if their proper motions were within 3σ of the cluster mean proper motion (pm(RA) ≈ −24 mas/yr and pm(DEC) ≈ +24 mas/yr ;Dodd 2004;Kharchenko 2001). This criterion identified only 9 proper motion member candidates out of 70.…”

Section: Selection Of Cluster Member Candidate From the Hr Diagrammentioning

confidence: 99%

“…In this cluster there are about 180 known members, with accurate proper motion determinations Based on observations carried out at the ESO/La Silla, Chile under proposal number 68.D-0541(A). (Dodd 2004;Monet al 2003;Platais et al 2007), among which a dozen are substellar objects. The only determination of the IC 2391 mass spectrum in the very low-mass regime has been presented by Barrado y Navascués et al (2004).…”

Section: Introductionmentioning

confidence: 99%

A deep multi-band investigation of IC 2391

Spezzi

Pagano²,

Marino³

et al. 2009

A&A

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Aims. We report the outcome of a deep multiwavelength study of the IC 2391 young open cluster. We attempt to uncover new lowmass and sub-stellar members of the cluster and identify new debris disk objects. Methods. We observed a 30 × 30 square arcmin area in IC 2391 using the wide-field imager at the ESO 2.2 m telescope. The completeness limits of the photometry at the 3σ level are V = 24.7, R C = 23.7, and I C = 23.0, faint enough to reveal sub-stellar members down to ∼0.03 M . Our membership criteria are based on use of our optical data in combination with JHK S magnitudes from the 2MASS catalog. We also estimate the physical parameters of the selected candidates. Debris disk candidates are identified on the basis of their infrared excess emission using near-and mid-infrared photometry from the Spitzer Space Telescope. Results. Our optical survey, which has a limiting magnitude at the 3σ level 1-2 mag fainter than previous optical surveys conducted in IC 2391, revealed 29 new low-mass member candidates of the cluster. We estimate the contamination to be at least ∼50%. We constrain the fraction of sub-stellar objects in the range 8-15% and discuss possible explanations of the deficit of brown dwarfs in this cluster. We also identify 10 candidates in the cluster showing IR excess emission consistent with the presence of debris disks.

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Data mining in the young open cluster IC 2391

Cited by 15 publications

References 30 publications

Differential Radial Velocities and Stellar Parameters of Nearby Young Stars

Differential Radial Velocities and Stellar Parameters of Nearby Young Stars

A Constraint on Brown Dwarf Formation via Ejection: Radial Variation of the Stellar and Substellar Mass Function of the Young Open Cluster Ic 2391

A deep multi-band investigation of IC 2391

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