BV CCD photometry of the old open cluster NGC 2243

Bergbusch, Peter A.; VandenBerg, Don A.; Infante, L.

doi:10.1086/115832

Cited by 25 publications

(23 citation statements)

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“…For NGC 2243, the previous results were not available in electronic form. However, we could rather easily find the color index for the TOP for the cluster from the published figures in Bonifazi et al (1990) and Bergbusch, Vandenberg, & Infante (1991), both consistent with (BÀV ) TOP = 0.45. Our average (BÀV ) TOP = 0.445 is in excellent agreement with these results.…”

Section: Photometric Calibrationsupporting

confidence: 72%

Open Cluster LW 55 in the Large Magellanic Cloud

Kałużny¹,

Ruciński²

2003

Astron J

162

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The field of the moderately old open cluster LW 55 in the outer parts of the Large Magellanic Cloud disk was monitored for detection of short-period variable stars over two nights. Eight variables were found; all but one (a detached eclipsing binary) are small-amplitude (DV 0.1 mag) pulsating stars of the Scuti, SX Phoenicis, or Doradus type. The BV color-magnitude diagram extends down to the solar-type stars at V = 24 (M V ' 5.2). The cluster age is estimated at 1.5 Gyr for Z = 0.004 ([Fe/H] = À0.67); the surrounding stellar field is older, with an age greater than 4 Gyr.

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Section: Photometric Calibrationsupporting

confidence: 72%

Open Cluster LW 55 in the Large Magellanic Cloud

Kałużny¹,

Ruciński²

2003

Astron J

162

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“…The noteworthy variations of the width of the cluster MS along the T 1 magnitude are mainly due both to evolutionary effects and to the presence of binaries. We identified gaps of stars centred at (T 1 , C − T 1 ) ≈ (15.8, 0.85), (16, 1.25) and (17.2, 1.65), some of which have also been detected in other intermediate-age and old open clusters (see, e.g., Bonifazi et al 1990;Bergbusch et al 1991;Park & Lee 1999). Although there is not yet any satisfactory explanation for these gaps, they seem to be related to the existence of convective overshooting in the core of moderate mass stars before and during the hydrogen exhaustion phase (Crowe & Mitalas 1982;Lee 1997).…”

Section: Cluster Fundamental Parametersmentioning

confidence: 64%

Improvements on the fundamental parameters of the open cluster Tombaugh 1 through Washington system photometry

Piatti

Clariá

Ahumada

2004

A&A

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Abstract. We present CCD photometry in the Washington system C and T 1 passbands down to T 1 ∼ 18.5 mag in the field of Tombaugh 1, a little studied open cluster located in the third Galactic quadrant. We measured T 1 magnitudes and C − T 1 colours for a total of 1351 stars distributed throughout an area of 13. 6 × 13. 6. A cluster radius of 4. 3 ± 0. 3 was estimated from star counts in 100-pixel a side boxes distributed throughout the entire observed field. Based on the best fits of isochrones computed by the Geneva group for Z = 0.008 to the T 1 vs. C − T 1 colour-magnitude diagram, we derive a colour excess E(C − T 1 ) = 0.55 ± 0.10, equivalent to E(B − V) = 0.30 ± 0.05, a distance of (2.2 ± 0.5) kpc from the Sun and an age of 1.3The latter value is in good agreement with that derived from the independent metallicity δT 1 index defined in Geisler et al. (1997( , AJ, 114, 1920). An independent metallicity estimation using the [M T 1 , (C − T 1 ) 0 ] plane with the standard giant branches of Geisler & Sarajedini (1999, AJ, 117, 308)

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“…Variables V 1 , V 2 and V 6 correspond to stars #235, #258 and #368 in Bergbush et al (1991). The remaining variables are located outside the field observed by these authors.…”

Section: The Search For Variablesmentioning

confidence: 68%

Variable stars in the field of the old open cluster NGC 2243

Kałużny

Krzemiński

Mazur

1996

Astron. Astrophys. Suppl. Ser.

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Abstract. -We report results of photometric monitoring of the NGC 2243 field in V and I filters. Two W UMatype systems and three detached eclipsing binaries were discovered. Both contact systems are likely members of the cluster. One of the detached binaries -variable V1 -has a period P=1.188 day. This variable is located at the cluster's turnoff in the color-magnitude diagram. Determination of parameters for components of V1 can provide direct information about properties of turnoff stars in NGC 2243 as well as to allow direct determination of cluster's distance. A background RR Lyr variable was found in the monitored field. The reddening of NGC 2243 is estimated at E(V − I) = 0.10 ± 0.04 based on the V −I color exhibited by this star at minimum light. The observed distribution of colors for the background halo stars shows a cutoff at (V − I) ≈ 0.60 what implies E(V − I) ≤ 0.12 for the cluster.

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BV CCD photometry of the old open cluster NGC 2243

Cited by 25 publications

References 0 publications

Open Cluster LW 55 in the Large Magellanic Cloud

Open Cluster LW 55 in the Large Magellanic Cloud

Improvements on the fundamental parameters of the open cluster Tombaugh 1 through Washington system photometry

Variable stars in the field of the old open cluster NGC 2243

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