Membership, fundamental parameters and luminosity function of the open cluster NGC 5662

Clariá, J. J.; Lapasset, E.; Bosio, Martín

doi:10.1093/mnras/249.2.193

Cited by 19 publications

(41 citation statements)

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“…The averaged external mean errors are smaller than 0.015 mag for the V magnitude and the (B − V) and (U − B) colours. All these errors are nearly similar to those in previous papers (e.g., Clariá et al 1991). No evidence of systematic differences either in the V magnitude or in the colours among the stars measured in LCO and CTIO was detected.…”

Section: Observations and Reductionssupporting

confidence: 90%

IC 2395 and BH 47: Only one open cluster in the Vela constellation

Clariá¹,

Lapasset²,

Piatti³

et al. 2003

A&A

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Abstract. We report UBV photoelectric photometry for 273 stars in the fields of the open clusters IC 2395 and BH 47. Our postulate is that, rather than two different clusters in this region of Vela, there is only one, which we call IC 2395 = BH 47. The cluster is centered at about α = 8 h 42. m 5, δ = −48• 06. 8 (2000), its angular diameter being ∼19 . The analysis of the photometric data yields 61 probable cluster members and 16 possible members. Photometric membership probabilities show good agreement with those obtained from a proper motion study for 21 stars in common. The reddening across the cluster appears to be uniform, the mean E(B − V) value being 0.09 ± 0.02. The true distance modulus is (V − M V ) 0 = 9.52 ± 0.10, corresponding to a distance from the Sun of (800 ± 40) pc and 48 pc below the Galactic plane. The cluster age, determined by fitting isochrones with core overshooting, turns out to be (6 ± 2) Myr. There is a strong likelihood that IC 2395 = BH 47 is physically connected to the Vela OB1C association.

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Section: Observations and Reductionssupporting

confidence: 90%

IC 2395 and BH 47: Only one open cluster in the Vela constellation

Clariá¹,

Lapasset²,

Piatti³

et al. 2003

A&A

Self Cite

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“…The average external mean errors are smaller than 0.015 mag for the V magnitude and the (B − V) and (U − B) colours. All these errors are nearly similar to those in previous papers (e.g., Clariá et al 1991). Table 1 presents the results of our photometry for the stars numbered in Fig.…”

Section: Photometric Datasupporting

confidence: 88%

Multicolour photometry and Coravel observations of stars in the southern open cluster IC 2488

Clariá¹,

Piatti²,

Lapasset³

et al. 2003

A&A

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Abstract. We present new UBV photoelectric observations of 119 stars in the field of the southern open cluster IC 2488, supplemented by DDO and Washington photometry and Coravel radial velocities for a sample of red giant candidates. Nearly 50% of the stars sampled -including three red giants and one blue straggler -are found to be probable cluster members. Photometric membership probabilities of the red giant candidates show good agreement with those obtained from Coravel data. A mean radial velocity of (−2.63 ± 0.06) km s −1 is derived for the cluster giants. The reddening across the cluster is found to be uniform, the mean value being E(B − V) = 0.24 ± 0.04. IC 2488, located at a distance of (1250 ± 120) pc from the Sun and 96 pc below the Galactic plane, is most probably not related to the planetary nebula ESO 166-PN21. A metal abundance [Fe/H] = 0.10 ± 0.06 relative to the Sun is determined from DDO data of the red giant members, in good agreement with the [Fe/H] values derived from five independent Washington abundance indices. An age of 180 Myr is determined from the fitting of isochrones computed with convective overshooting for Z = 0.019. The isochrone for log t = 8.25 reproduces remarkably well not only the morphology of the upper main sequence but also the observed red giant pattern.

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“…Mean extinction coefficients at both observatories were employed and nightly observations of about 13-17 standard stars taken from the lists of Cousins (1973Cousins ( , 1974, Landolt (1973) and Graham (1982) were used to transform instrumental magnitudes into the UBV standard system. External and internal mean errors are nearly similar to those in previous papers (e.g., Clariá et al 1991). Typically σV ≤ 0.014 mag, σB − V ≤ 0.010 mag and σU − B ≤ 0.017 mag for V < 12 mag, increasing to 0.018, 0.022 and 0.027 for V > 12 mag, respectively.…”

Section: Observations and Reductionssupporting

confidence: 86%

Photometric study of the open cluster NGC 2323

Clariá

Piatti

Lapasset

1998

Astron. Astrophys. Suppl. Ser.

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Abstract. UBV photoelectric photometry for 175 stars in the field of the southern open cluster NGC 2323, supplemented by DDO photometry of 5 probable giants, is presented. The analysis of the photometric data yields 109 probable members; one of them being a red giant, and 3 possible members. The reddening across the cluster is slightly variable and the mean value E(B − V ) = 0.25. The apparent cluster distance modulus is 10.62, corresponding to a distance of 940 pc. The age, determined by fitting isochrones with core overshooting, turns out to be 100 ± 20 Myr. Other fundamental cluster parameters are also determined. NGC 2323 appears not to be physically connected to the CMa OB1 association.

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Membership, fundamental parameters and luminosity function of the open cluster NGC 5662

Cited by 19 publications

References 0 publications

IC 2395 and BH 47: Only one open cluster in the Vela constellation

IC 2395 and BH 47: Only one open cluster in the Vela constellation

Multicolour photometry and Coravel observations of stars in the southern open cluster IC 2488

Photometric study of the open cluster NGC 2323

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