The first CCD photometric study of the open cluster
NGC 2126

Gáspár, András; Kiss, L. L.; Bedding, Timothy R.; Derekas, A.; Kaspi, S.; Kiss, Cs.; Sárneczky, K.; Szabó, Gy. M.; Váradi, Mihály

doi:10.1051/0004-6361:20031311

Cited by 8 publications

(23 citation statements)

References 21 publications

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“…Based on the PDM code, we derive a probable period to be 0.0827 d which is close to the f 1 , and the amplitude is 0.104 mag, very low. Combining the results of Gáspár (2003) and of this paper, V5 may be confirmed to be δ Scuti star. V6: Gáspár (2003) showed that V6 was an eclipsing binary system with a δ Sct-type pulsating with P pul = 0.129 d and P orb = 1.1732 d, and it might have f pul : f orb = 1 : 9 resonance between the orbital motion and pulsation.…”

Section: The Known Variables In Ngc 2126supporting

confidence: 73%

“…Combining the results of Gáspár (2003) and of this paper, V5 may be confirmed to be δ Scuti star. V6: Gáspár (2003) showed that V6 was an eclipsing binary system with a δ Sct-type pulsating with P pul = 0.129 d and P orb = 1.1732 d, and it might have f pul : f orb = 1 : 9 resonance between the orbital motion and pulsation. Our results of P pul = 0.12957 d and P orb = 1.1732 d are consistent with Gáspár (2003).…”

Section: The Known Variables In Ngc 2126supporting

confidence: 73%

“…V2: It was discovered by Gáspár (2003), and the periods around 0.5 d and 1 d were given, however neither period cannot give a continuous phase diagram with no gap. So, Gáspár (2003) did not determine the cause of the low-amplitude. In this paper, its spectral type is decided to be A-type.…”

Section: The Known Variables In Ngc 2126mentioning

confidence: 99%

“…V4: It is an Algol-type eclipsing binary. Gáspár (2003) observed only one minimum of this star and failed to determine its period. During our observations, we recorded three eclipse events.…”

Section: The Known Variables In Ngc 2126mentioning

confidence: 99%

“…V6: Gáspár (2003) showed that V6 was an eclipsing binary system with a δ Sct-type pulsating with P pul = 0.129 d and P orb = 1.1732 d, and it might have f pul : f orb = 1 : 9 resonance between the orbital motion and pulsation. Our results of P pul = 0.12957 d and P orb = 1.1732 d are consistent with Gáspár (2003). Considering its spectral type of F-type determined in this paper, V6 may be a δ Scuti star in an eclipsing binary.…”

Section: The Known Variables In Ngc 2126mentioning

confidence: 99%

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Variable stars in the field of open cluster NGC 2126

Liu

Zhang

et al. 2009

Res. Astron. Astrophys.

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We report the results of a time-series CCD photometric survey of variable stars in the field of the open cluster NGC 2126. In about one square degree field covering the cluster, a total number of 21 variable candidates are detected during this survey, of which 16 are newly found. The periods, classifications and spectral types of 14 newly discovered variables are discussed, which consist of six eclipsing binaries systems, three pulsating variable stars, three long period variables, one RS CVn star, and one W UMa or δ Scuti star. In addition, there are two variable candidates, the properties of which cannot be determined in this paper. By a method based on fitting spectral energy distributions(SEDs) of stars with theoretical ones, the membership probabilities and the fundamental parameters of this cluster are determined.As a result, five variables are probably members of NGC 2126. The fundamental parameters of the this cluster are determined as: the metallicity to be 0.008 Z ⊙ , the age log(t)= 8.95, the distance modulus (m − M ) 0 = 10.34 and the reddening value E(B − V )=0.55 mag.

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Section: The Known Variables In Ngc 2126supporting

confidence: 73%

Section: The Known Variables In Ngc 2126supporting

confidence: 73%

Section: The Known Variables In Ngc 2126mentioning

confidence: 99%

Section: The Known Variables In Ngc 2126mentioning

confidence: 99%

Section: The Known Variables In Ngc 2126mentioning

confidence: 99%

See 3 more Smart Citations

Variable stars in the field of open cluster NGC 2126

Liu

Zhang

et al. 2009

Res. Astron. Astrophys.

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HD 172189: an eclipsing and spectroscopic binary with aδ Sct-type pulsating component in an open cluster

Mart́ın-Rúız¹,

Amado

Suárez³

et al. 2005

A&A

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Abstract. We present a study based on more than 2500 uvby-measurements collected on HD 172189, a new eclipsing binary system with a δ Sct-type pulsating component that belongs to the open cluster IC 4756. The great interest of this object lies in that three important characteristics coexist: cluster membership, binarity and pulsation. Its binarity and the δ Sct-type pulsations of one component were detected in the course of several Strömgren photometric campaigns. The frequency analysis of all the uvby out-of-eclipse data reveals a clear frequency of 19.5974 cd −1 as well as the existence of other high values in the range 18-20 cd −1 . We have also carried out a first evaluation of the binary parameters and determined a value of 5.702 d for the orbital period. An additional potential interest of HD 172189 resides in its location in the field of view of the COROT mission and, therefore, this star is an excellent candidate for becoming a target for asteroseismology.

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Exploring FSR open cluster candidates within $\sf |\Delta\ell|=20^\circ$ of the Galactic anticentre

Bonatto

Bica

2008

A&A

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Context. We investigate the nature of a sample of star cluster candidates detected as stellar overdensities towards the Galactic anticentre. Aims. Taken from the catalogue of Froebrich, Scholz, and Raftery (FSR), the sample contains 28 star cluster candidates located within |Δ | = 20• of the anticentre. These are all the candidates in that sector classified by FSR with a high probability of being star clusters. Our main goals are to determine the fraction of such candidates that are unknown star clusters, to derive their astrophysical parameters, and to investigate the relationship of cluster parameters with position in the Galaxy. Methods. Properties of the star cluster candidates are investigated with field-star decontaminated 2MASS colour-magnitude diagrams and stellar radial density profiles. Results. All candidates present significant excesses in the radial density profiles, consistent with the method from which they were originally selected. Of the 28 candidates, 7 are previously known open clusters, 2 have been recently identified, and 6 are new ones with ages from 30 Myr to 1 Gyr. Among the remaining 13 candidates, 6 are uncertain cases that require deeper observations, while 7 appear to be important field fluctuations. The structure of part of the newly identified open clusters appears to be affected by interaction with giant molecular clouds in the Local and Perseus arms. Conclusions. When photometric and radial distribution properties are considered together, an important fraction of the stellar overdensities with a fluctuation level > ∼ 3σ are shown to be star clusters. Thus, catalogues of star cluster candidates, coupled to the present kind of study, are an important source for identifying unknown open clusters. Such efforts affect the understanding of the star-formation rate, cluster dynamical evolution, and Galactic structure, among others.

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The first CCD photometric study of the open cluster NGC 2126

Cited by 8 publications

References 21 publications

Variable stars in the field of open cluster NGC 2126

Variable stars in the field of open cluster NGC 2126

HD 172189: an eclipsing and spectroscopic binary with aδ Sct-type pulsating component in an open cluster

Exploring FSR open cluster candidates within $\sf |\Delta\ell|=20^\circ$ of the Galactic anticentre

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