ICCD speckle observations of binary stars. IX - A duplicity survey of the Pleiades, Praesepe, and IC 4665 clusters

Mason, Brian D.; Hartkopf, William I.; McAlister, Harold A.; Sowell, James R.

doi:10.1086/116669

Cited by 37 publications

(56 citation statements)

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“…No binarity was reported by Abt et al (1965) in their spectroscopic binary survey. Further negative binarity detections were reported in the following works: LO observation by McGraw et al (1974), HIPPARCOS and the post-mission compilation of the Tycho Double Star Catalogue (Fabricius et al 2002), and deep ICCD observations by Mason et al (1993). We note also that HD 23632 was employed by Eisner et al (2010Eisner et al ( , 2009 as calibrator for the Keck Interferometer, attaining a spatial resolution of ≈1 mas.…”

Section: Resultssupporting

confidence: 65%

An investigation of binary stars in the Pleiades with high contrast and spatial resolution

Richichi

Chen

Cusano

et al. 2012

A&A

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Context. It is widely recognized that binarity is a very common feature during star formation; however, different regions and clusters display significantly different binary fractions. This appears to be related to the initial density of the star forming region. The Pleiades cluster has been shown to have a binary fraction similar to that of field stars in the solar neighborhood. Aims. We have taken advantage of a passage of the Moon over the Pleiades cluster, to investigate at high angular resolution two small but similar and consistent samples of cluster members and field stars. Methods. We have employed the technique of lunar occultations (LO). Although LO in the Pleiades have been reported several times in the past, we have for the first time employed the superior performance of the VLT, achieving about 1 milliarcsecond (mas) resolution and detecting sources as faint as K ≈ 12 mag. Results. We have recorded 17 LO light curves of stars recognized as cluster members, and 17 of field stars. The average magnitude was K ≈ 8.5 mag and the average limiting resolution ≈0. 002, for both samples. We detect 5 binaries among the cluster members, and 2 among the sample of field stars. Three systems are new detections, while two were previously only suspected to be binaries. The projected separations are in the range 0. 017 to 0. 642 and the brightness ratios in the range 1 to 90. One more star is suspected to have a companion. Conclusions. Although the fraction of binary detections appears higher among the members than among the non-members, the two samples are too small to draw firm conclusions. Our observations show that, in spite of extensive investigations carried out previously in the Pleiades cluster, the binarity census is not yet complete. We have detected significant orbital motion in four binary systems, which stand up as candidates for dynamical mass estimations.

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Section: Resultssupporting

confidence: 65%

An investigation of binary stars in the Pleiades with high contrast and spatial resolution

Richichi

Chen

Cusano

et al. 2012

A&A

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“…For Coma and Praesepe, binaries are initially identified from radial velocity and speckle measurements. The papers consulted for those data include Mason et al (1993), Abt & Willmarth (1999), Mayor (1999), andBouvier et al (2001). Data for binaries identified from those papers are retained in the temperature catalogs for Coma and Praesepe only if the binaries fall within the main sequence scatter in the colormagnitude diagrams of those clusters.…”

Section: Binariesmentioning

confidence: 99%

Cousins Photometry and Temperatures for the Hyades, Coma, NGC 752, Praesepe, and M67

Taylor

Joner

Jeffery

2008

ASTROPHYS J SUPPL S

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In this paper, new Cousins VRI data are presented for NGC 752 and Praesepe, and new and extant data are combined into an augmented database for M67. For those three clusters, catalogs containing Cousins VRI photometry, reddening-corrected values of (V À K ) J , and temperatures are produced. The same is done for Coma by using both previously published and newly derived Cousins photometry. An extant set of catalogs for the Hyades is updated to include V magnitudes and values of (R À I ) C that were published after the original catalogs appeared. Finally, M67 V magnitudes published previously by Sandquist are corrected for an effect that depends on location on the face of the cluster. The corrected data and values of (V À I ) C given by Sandquist are then set out in a supplementary catalog. Data files containing all of these catalogs are deposited in the CDS archives. To assess the quality of the data in the catalogs, the consistency of extant Cousins VRI databases is tested by performing analyses with the following features: (1) quantities as small as a few millimags are regarded as meaningful; (2) statistical analysis is applied; (3) no use is made of data other than VRI measurements and comparable results; (4) no inferences are drawn from colormagnitude comparisons; (5) pertinent data that have not been included previously are analyzed; and (6) results based on direct comparisons of stellar groups at the telescope are featured. In this way, it is found that our updated M67 color data and those of Sandquist are on the E region zero point. In contrast, values of (V À I ) C from Montgomery and collaborators are found to be too red by 27 AE 3 mmag, with an even larger offset being likely for unpublished data from Richer and his collaborators. Zero-point tests of our Cousins VRI colors for Coma, Praesepe, and NGC 752 are also satisfactory. Scale factor tests of the M67 colors are performed, and a likely scale factor error in the Montgomery et al. colors is found. However, it appears at present that the scale factors of our M67 colors and those of Sandquist are satisfactory. For the most part, zero-point tests of the assembled V magnitudes are also satisfactory, although it is found that further work on the V magnitudes for Praesepe and M67 would be useful. To put these results in perspective, it is pointed out that photometric tests that are satisfactory at the few-millimag level have been published for some two decades and so are not appearing for the first time in this paper.

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“…We have not found short amplitude variations of KW 284 in short time scales, although the variability reported by Rolland et al (1991) is unquestionable. More, KW 284 has been found, by the speckle observations (Mason et al 1993;McAlister et al 1989), as an occultation binary system. However, this binarity cannot account for the variations found.…”

Section: Resultsmentioning

confidence: 94%

“…The same aim was pursued by Hambly et al (1995) extended to low mass main sequence membership. ICCD speckle observations of binary stars in Praesepe has been done recently by Mason et al (1993). They listed one new binary star, KW 212, out of over 54 potentially short period stars and three more: KW 203, KW 265 and KW 284, that were discovered before.…”

Section: Generalities Of Praesepementioning

confidence: 99%

Photoelectric photometry and period analysis of selected Delta Scuti stars in Praesepe

Peña¹,

Peniche²,

Hobart³

et al. 1998

Astron. Astrophys. Suppl. Ser.

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Abstract. Photoelectric photometry of seven Delta Scuti stars in Praesepe was secured. Three of them were observed simultaneously at observatories located at different longitudes. Period analysis has been carried out for each star with different computing packages and the results compared to those in the literature. Their physical characteristics have been determined from the Strömgren photometry and theoretical and empirical calibrations.

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ICCD speckle observations of binary stars. IX - A duplicity survey of the Pleiades, Praesepe, and IC 4665 clusters

Cited by 37 publications

References 1 publication

An investigation of binary stars in the Pleiades with high contrast and spatial resolution

An investigation of binary stars in the Pleiades with high contrast and spatial resolution

Cousins Photometry and Temperatures for the Hyades, Coma, NGC 752, Praesepe, and M67

Photoelectric photometry and period analysis of selected Delta Scuti stars in Praesepe

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