scholarly journals IC 361, a distant intermediate-age cluster in Camelopardalis

2009 ◽  
Vol 5 (S266) ◽  
pp. 557-560
Author(s):  
Justas Zdanavičius ◽  
Richard P. Boyle ◽  
Frederick J. Vrba ◽  
Kazimieras Zdanavičius ◽  
Stanislava Bartašiūtė
Keyword(s):  
Open Cluster ◽  
Interstellar Extinction ◽  
Distance Modulus ◽  
Ccd Photometry ◽  
True Distance ◽  
Individual Stars ◽  
Cluster Distance ◽  
Spiral Arm

AbstractWe have undertaken CCD photometry in the eight-color Vilnius + I system for the open cluster IC 361 (l = 147.5°, b = 5.7°) located in the constellation of Camelopardalis. Based on multicolor data, estimates of distance moduli, foreground reddening and metallicity have been obtained for individual stars measured in the field of the cluster. This allowed us to eliminate most of the field stars and to identify the probable cluster members, from which we derived the true distance modulus (m − M)0 = 12.7 mag and metallicity [Fe/H] = −0.3 dex. The interstellar extinction is found to be nonuniform across the field, with values of AV ranging from 1.9 to 2.6 mag. A comparison of the color–magnitude diagrams with Padova isochrones yields (m − M)0 = 12.6 mag, or a cluster distance of 3.3 kpc, and an age of 1.0 Gyr. Therefore, IC 361 appears to be a mildly metal-deficient cluster of intermediate age, located as far as, or just beyond, the Perseus spiral arm.

scholarly journals The Young Open Cluster NGC 2384

1984 ◽  
Vol 78 ◽  
pp. 295-299
Author(s):  
S.M. Hassan
Keyword(s):  
Spectral Type ◽  
Open Cluster ◽  
Apparent Distance ◽  
Distance Modulus ◽  
Colour Excess ◽  
Young Open Cluster ◽  
Ubv Photometry ◽  
Spiral Arm

AbstractCombined photoelectric – photographic UBV-photometry for NGC 2384 is discussed. The results achieved so far are summarized and indicate that this cluster is young enough to be used as spiral arm tracer out to a distance of 3.27 kpc. The colour excess E(B-V) is 0.31, the apparent distance modulus is 13m.50 and its earliest spectral type is BO.

scholarly journals Investigation of contact binaries in the field of NGC 6811

2020 ◽  
Vol 72 (4) ◽  
Author(s):  
Xu-Zhi Li ◽  
Liang Liu ◽  
Xu-Dong Zhang
Keyword(s):  
Binary Systems ◽  
Open Cluster ◽  
Interstellar Extinction ◽  
Cluster Center ◽  
Strong Interactions ◽  
Cluster Distance ◽  
Metal Abundance ◽  
Contact Binaries ◽  
Contact Binary ◽  
Distance Data

Abstract Contact binary systems are very important for studying physical processes such as strong interactions between stars, mass transfer, and stellar merger. Further, the members of an open cluster have the same age, metal abundance, and interstellar extinction conditions. Therefore, we can conduct a comparative study on the different binary systems of the same open cluster. NGC 6811 is an observed intermediate-aged, slightly reddened open cluster in the Kepler field of view; we conducted a corresponding study on the contact binary systems in this cluster. We analyzed six suspected targets and found a total of five EW-type binary systems within a field of 40′ radius of the NGC 6811 cluster center. These targets were analyzed base on the Kepler data, and the corresponding system parameters were obtained by using the latest version of the Wilson–Devinney code. Further, we also used Gaia DR2 data and the cluster distance data to estimate the absolute parameters of these targets to determine whether they are members of the cluster. Finally, we determined that two targets (KIC 9470175 and KIC 9533706) are most likely cluster members; KIC 9957411 and KIC 9776718 are definitely not members of the cluster, just background stars.

Multicolor CCD Photometry of the Open Cluster IC 361

2010 ◽  
Vol 19 (1-2) ◽  
Author(s):  
J. Zdanavičius ◽  
S. Bartašiūtė ◽  
R. P. Boyle ◽  
F. J. Vrba ◽  
K. Zdanavičius
Keyword(s):  
Open Cluster ◽  
Interstellar Extinction ◽  
Ccd Photometry ◽  
Color Indices ◽  
Absolute Magnitudes

AbstractCCD photometry in the eight-color Vilnius + I system for 7250 stars down to I =19.6 mag has been obtained in the 20′ × 26′ field of the open cluster IC 361 in Camelopardalis. The catalog of 1420 stars down to V ~ 18.5 mag is presented. It contains the coordinates, V magnitudes and seven color indices, quantitative photometric spectral types, absolute magnitudes and distances. The interstellar extinction is found to be non-uniform across the field, with the values of A

scholarly journals CCD Photometry of NGC 2453

1993 ◽  
Vol 155 ◽  
pp. 182-182
Author(s):  
D.C.V. Mallik ◽  
Ram Sager ◽  
A.K. Pati
Keyword(s):  
Open Cluster ◽  
Core Region ◽  
Distance Modulus ◽  
Photometric Study ◽  
Ccd Photometry ◽  
Image Frame ◽  
Standard Practice ◽  
The Core ◽  
Flat Field

We have undertaken a detailed photometric study of the open cluster NGC 2453 in Puppis with a view to determining accurately its distance modulus and to investigate its possible association with the PN NGC 2452. We have observed the core region of the cluster in V and I photometric bands using a Thomson-CSF TH 7882 CCD chip with the format 384×576 pixels, at the f/13 cassegrain focus of the 102-cm telescope at Vainu Bappu Observatory, Kavalur, India. Each image frame covers a field of 2′.3 × 3′.4 of the sky. Bias frames and flat field exposures on the twilight sky were obtained as per standard practice.

scholarly journals Young open cluster IC 4996 and its vicinity: multicolor photometry and Gaia DR2 astrometry

2019 ◽  
Vol 623 ◽  
pp. A22 ◽  
Author(s):  
V. Straižys ◽  
R. P. Boyle ◽  
K. Milašius ◽  
K. Černis ◽  
M. Macijauskas ◽  
...  
Keyword(s):  
Open Cluster ◽  
Interstellar Extinction ◽  
Mean Value ◽  
Photometric System ◽  
B Stars ◽  
Dust Clouds ◽  
Wide Range ◽  
Cluster Distance ◽  
Young Open Cluster ◽  
Similar Distance

The open cluster IC 4996 in Cygnus and its vicinity are investigated by applying a two-dimensional photometric classification of stars measured in the Vilnius seven-color photometric system. Cluster members are identified by applying distances based on the Gaia DR2 parallaxes and the point vector diagram of the Gaia DR2 proper motions. For some B-type stars, spectroscopic MK types are also obtained from the Asiago spectra and collected from the literature. New parameters of the cluster are derived. The interstellar extinction AV covers a wide range of values, from 1.3 to 2.4 mag; the mean value in the central part of the cluster is 1.8 mag. The cluster distance is 1915 ± 110 pc, and its age is within 8–10 Myr. The cluster exhibits a long sequence from early-B to G stars, where stars cooler than B8 are in the pre-main-sequence stage. The plot of extinction versus distance shows a steep rise of AV up to 1.6 mag at 700–800 pc, which is probably related to dust clouds at the edge of the Great Cygnus Rift. The next increase in extinction by an additional 0.8 mag at d ≥ 1.7 kpc is probably related to the associations Cyg OB1 and Cyg OB3. The cluster IC 4996 does not belong to the Cyg OB1 association, which is located closer to the Sun, at 1682 ± 116 pc. It seems likely that the cluster and the surrounding O-B stars have a common origin with the nearby association Cyg OB3 since Gaia data show that these stellar groups are located at a similar distance.

scholarly journals A revised moving cluster distance to the Pleiades open cluster

2017 ◽  
Vol 598 ◽  
pp. A48 ◽  
Author(s):  
P. A. B. Galli ◽  
E. Moraux ◽  
H. Bouy ◽  
J. Bouvier ◽  
J. Olivares ◽  
...  
Keyword(s):  
Open Cluster ◽  
Space Mission ◽  
Cluster Method ◽  
Individual Stars ◽  
Long Baseline ◽  
Cluster Distance ◽  
Trigonometric Parallaxes ◽  
Point Search ◽  
Good Agreement

Context. The distance to the Pleiades open cluster has been extensively debated in the literature over several decades. Although different methods point to a discrepancy in the trigonometric parallaxes produced by the Hipparcos mission, the number of individual stars with known distances is still small compared to the number of cluster members to help solve this problem. Aims. We provide a new distance estimate for the Pleiades based on the moving cluster method, which will be useful to further discuss the so-called Pleiades distance controversy and compare it with the very precise parallaxes from the Gaia space mission. Methods. We apply a refurbished implementation of the convergent point search method to an updated census of Pleiades stars to calculate the convergent point position of the cluster from stellar proper motions. Then, we derive individual parallaxes for 64 cluster members using radial velocities compiled from the literature, and approximate parallaxes for another 1146 stars based on the spatial velocity of the cluster. This represents the largest sample of Pleiades stars with individual distances to date. Results. The parallaxes derived in this work are in good agreement with previous results obtained in different studies (excluding Hipparcos) for individual stars in the cluster. We report a mean parallax of 7.44 ± 0.08 mas and distance of 134.4+2.9-2.8 pc that is consistent with the weighted mean of 135.0 ± 0.6 pc obtained from the non-Hipparcos results in the literature. Conclusions. Our result for the distance to the Pleiades open cluster is not consistent with the Hipparcos catalog, but favors the recent and more precise distance determination of 136.2 ± 1.2 pc obtained from Very Long Baseline Interferometry observations. It is also in good agreement with the mean distance of 133 ± 5 pc obtained from the first trigonometric parallaxes delivered by the Gaia satellite for the brightest cluster members in common with our sample.

scholarly journals The young open cluster NGC 7067 using Strömgren photometry

2016 ◽  
Vol 466 (3) ◽  
pp. 3636-3647 ◽  
Author(s):  
M Monguió ◽  
I Negueruela ◽  
A Marco ◽  
C González-Fernández ◽  
J Alonso-Santiago ◽  
...  
Keyword(s):  
Spectroscopic Data ◽  
Milky Way ◽  
Open Cluster ◽  
Physical Parameters ◽  
Wide Field ◽  
Isaac Newton ◽  
Cluster Distance ◽  
Young Open Cluster ◽  
Isaac Newton Telescope ◽  
Spiral Arm

Abstract NGC 7067 is a young open cluster located in the direction between the first and the second Galactic quadrants and close to the Perseus spiral arm. This makes it useful for studies of the nature of the Milky Way spiral arms. Strömgren photometry taken with the Wide Field Camera at the Isaac Newton Telescope allowed us to compute individual physical parameters for the observed stars and hence to derive the cluster's physical parameters. Spectra from the 1.93-m telescope at the Observatoire de Haute-Provence helped to check and improve the results. We obtained photometry for 1233 stars, individual physical parameters for 515 and spectra for 9 of them. The 139 selected cluster members lead to a cluster distance of 4.4 ± 0.4 kpc, with an age below log10(t(yr)) = 7.3 and a present mass of 1260 ± 160 M⊙. The morphology of the data reveals that the centre of the cluster is at (α, δ) = (21: 24: 13.69, +48: 00: 39.2) J2000, with a radius of 6.1 arcmin. Strömgren and spectroscopic data allowed us to improve the previous parameters available for the cluster in the literature.

scholarly journals Multicolor CCD photometry of the open cluster NGC 752

2009 ◽  
Vol 5 (S266) ◽  
pp. 361-364
Author(s):  
Stanislava Bartašiūtė ◽  
Robert Janusz ◽  
Richard P. Boyle ◽  
A. G. Davis Philip ◽  
Viktoras Deveikis
Keyword(s):  
Main Sequence ◽  
Open Cluster ◽  
Ccd Camera ◽  
Advanced Technology ◽  
Ccd Photometry ◽  
Intermediate Band ◽  
Individual Stars ◽  
Ccd Observations ◽  
Low Mass

AbstractWe obtained CCD observations of the open cluster NGC 752 with the 1.8m Vatican Advanced Technology Telescope (Mt. Graham, Arizona) with a 4K CCD camera and eight intermediate-band filters of the Stromvil (Strömgren + Vilnius) system. Four 12′ × 12′ fields were observed, covering the central part of the cluster. The good-quality multicolor data made it possible to obtain precise estimates of distance moduli, metallicity and foreground reddening for individual stars down to the limiting magnitude, V = 17.5, enabling photometric identification of faint cluster members. The new observations provide an extension of the lower main sequence to three magnitudes beyond the previous (photographic) limit. A relatively small number of photometric members identified at fainter magnitudes seems to be indicative of actual dissolution of the cluster from the low-mass end.

scholarly journals Refining the true parameters of the open cluster NGC 4852

2009 ◽  
Vol 5 (S266) ◽  
pp. 539-539
Author(s):  
Gladys Solivella ◽  
Edgard Giorg ◽  
Rubén Vázquez ◽  
Giovanni Carraro
Keyword(s):  
Emission Line ◽  
Open Cluster ◽  
Open Clusters ◽  
Occurrence Rate ◽  
Hot Stars ◽  
Cluster Area ◽  
Young Object ◽  
Cluster Distance ◽  
Be Star ◽  
Compact Cluster

AbstractNGC 4852 is a moderately compact cluster centered at α2000 = 13 : 00 : 09; δ = −59 : 36 : 48, located near the center of an Hα superring. This cluster forms part of an extended region including young stellar aggregates inside a circle with a radius of 3 degrees, where many show an abundance of emission line stars. In the field of this cluster, two stars of known type exist: Wray 15–1039 (emission-line object) and CD −58:4845 (emission-line star). We do not yet know whether the Be phase is transient or whether it is just what randomly happens in some hot stars. It appears that Be star may be found even in clusters as old as 70 Myr with a high occurrence rate in clusters of 25–27 Myr old. A recent photometric survey in NGC 4852 down to V = 22 – 23 mag established that NGC 4852 is about 200 – 250 Myr old, located at 1.1 kpc from the Sun and with a mean E(B − V) = 0.45 mag. Since the presence of potential Be-type stars in the cluster area suggests it may be a very young object instead of moderately old, we decided to carry out spectroscopy for 33 selected stars and CCD UBVI photometry for the bright objects in the cluster area. This way, we attempt to clarify their evolutionary state and include them in the framework of emission-line stars and open clusters. From our analysis, we agree with the cluster distance and reddening determined by earlier studies, but we derive that the age of NGC 4852 is younger than 40 Myr.

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