Deep CCD Photometry of Open Clusters Containing Cepheid Variables

1988 ◽  
Vol 100 ◽  
pp. 1222
Author(s):  
M. Mateo ◽  
B. Madore
Keyword(s):  
Open Clusters ◽  
Ccd Photometry ◽  
Cepheid Variables

scholarly journals Astronomy in Uzbekistan

2001 ◽  
Vol 24 (3) ◽  
pp. 231-232
Author(s):  
Sabit P. Ilyasov
Keyword(s):  
Star Formation ◽  
Binary Stars ◽  
Solar Physics ◽  
Open Clusters ◽  
Image Motion ◽  
Close Binary ◽  
Atmospheric Conditions ◽  
Ccd Photometry ◽  
Close Binary Stars ◽  
Star Formation Regions

Ulugh Beg Astronomical Institute (UBAI) of the Uzbek Academy of Sciences is one of the oldest scientific institutions not only in Uzbekistan, but in the whole of Central Asia as well. There are five departments in the institute. The main directions of research are solar physics, young non-stationary and close binary stars in star formation regions, satellite geodynamics, non-linear and non-stationary evolution of galaxies. Helioseismology studies carried out in the frame of the IRIS (International Research on the Interior of the Sun) and TON (Taiwan Oscillation Network) projects. Astrophysical programmes such as a search for periodicity in star-formation regions, study of close binary stars in the same regions, as well as in open clusters, CCD photometry of extra-galactic objects as gravitation lenses have been made at the Maidanak Observatory, which is located in the south-east of Uzbekistan. Monitoring of the seeing at Mt. Maidanak from 1996 to 1999, using ESO Differential Image Motion Monitor, showed that its atmospheric conditions are comparable with the best international observatories. The present status of the main fields of research and prospects are discussed. (Co-author is Shurat A. Ehgamberdiev, Uzbekistan.)

Cepheid Variables in the Large Magellanic Cloud Cluster NGC 1866. I. New BVRI CCD Photometry

2000 ◽  
Vol 129 (1) ◽  
pp. 111-121 ◽  
Author(s):  
Wolfgang P. Gieren ◽  
Matias Gomez ◽  
Jesper Storm ◽  
Thomas J. Moffett ◽  
L. Infante ◽  
...  
Keyword(s):  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Ccd Photometry ◽  
Cloud Cluster ◽  
Cepheid Variables

scholarly journals Abundances of Be Stars in Very Young Open Clusters

2000 ◽  
Vol 175 ◽  
pp. 59-62 ◽  
Author(s):  
A. Marco ◽  
G. Bernabeu ◽  
J.M. Torrejón ◽  
J.J. Rodes ◽  
J. Fabregat
Keyword(s):  
Open Clusters ◽  
Be Stars ◽  
Ccd Photometry ◽  
The Galaxy

AbstractWe present here standard uvbyβ CCD photometry for five open clusters of the Galaxy in order to determine abundances of Be stars, as a function of age.

scholarly journals UBV I CCD PHOTOMETRY OF THE OPEN CLUSTERS NGC 4609 AND HOGG 15

2010 ◽  
Vol 43 (5) ◽  
pp. 141-152 ◽  
Author(s):  
Seung-Hwa Kook ◽  
Hwan-Kyung Sung ◽  
M.S. Bessell
Keyword(s):  
Open Clusters ◽  
Ccd Photometry

scholarly journals Multicolour CCD photometry of old open clusters:

2001 ◽  
Vol 372 (1) ◽  
pp. 71-84 ◽  
Author(s):  
A. K. Durgapal ◽  
A. K. Pandey ◽  
V. Mohan
Keyword(s):  
Open Clusters ◽  
Ccd Photometry

scholarly journals The rotation period distribution of the rich Pleiades-age southern open cluster NGC 2516

2020 ◽  
Vol 641 ◽  
pp. A51 ◽  
Author(s):  
D. J. Fritzewski ◽  
S. A. Barnes ◽  
D. J. James ◽  
K. G. Strassmeier
Keyword(s):  
Time Series ◽  
Open Cluster ◽  
Rotation Period ◽  
Open Clusters ◽  
Ccd Photometry ◽  
Activity Diagram ◽  
Cool Star ◽  
Period Distribution ◽  
Rotational Distribution ◽  
Star Rotation

Aims. We wish to measure the cool star rotation period distribution for the Pleiades-age rich open cluster NGC 2516 and use it to determine whether cluster-to-cluster variations exist in otherwise identical open clusters. Methods. We obtained 42 d-long time-series CCD photometry of NGC 2516 in the V and Ic filters using the Yale 1 m telescope at CTIO and performed a number of related analyses, including PSF-based time-series photometry. Our data are complemented with additional information from several photometric datasets, literature radial velocities, and Gaia DR2 astrometry. All available data are used to construct an integrated membership list for NGC 2516, containing 844 stars in our ≈1° field of view. Results. We derived 308 rotation periods for late-F to mid-M cluster members from our photometry. We identified an additional 247 periodic M dwarf stars from a prior study as cluster members, and used these to construct a 555-star rotation period distribution for NGC 2516. The colour-period diagram (in multiple colours) has almost no outliers and exhibits the anticipated triangular shape, with a diagonal slow rotator sequence that is preferentially occupied by the warmer stars along with a flat fast rotator sequence that is preferentially populated by the cooler cluster members. We also find a group of extremely slowly rotating M dwarfs (10 d ≲ Prot ≲ 23 d), forming a branch in the colour-period diagram which we call the “extended slow rotator sequence”. This, and other features of the rotational distribution can also be found in the Pleiades, making the colour-period diagrams of the two clusters nearly indistinguishable. A comparison with the well-studied (and similarly aged) open cluster M 35 indicates that the cluster’s rotational distribution is also similarly indistinguishable from that of NGC 2516. Those for the open clusters M 50 and Blanco 1 are similar, but data issues for those clusters make the comparisons somewhat more ambiguous. Nevertheless, we demonstrate the existence of a representative zero-age main sequence rotational distribution and provide a simple colour-independent way to represent it. We perform a detailed comparison of the NGC 2516 rotation period data with a number of recent rotational evolution models. Using X-ray data from the literature, we also construct the first rotation-activity diagram for solar-type stars in NGC 2516, one that we find is essentially indistinguishable from those for the Pleiades and Blanco 1. Conclusions. The two clusters NGC 2516 and Pleiades can be considered twins in terms of stellar rotation and related properties (and M 35, M 50, and Blanco 1 are similar), suggesting that otherwise identical open clusters also have intrinsically similar cool star rotation and activity distributions.

Deep CCD Photometry of Old Open Clusters

1997 ◽  
Vol 113 ◽  
pp. 1723 ◽  
Author(s):  
Marc Kassis ◽  
Kenneth A. Janes ◽  
Eileen D. Friel ◽  
Randy L. Phelps
Keyword(s):  
Open Clusters ◽  
Ccd Photometry
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