Kinematics of the Open Cluster System in the Galaxy

Zhao, Jing; Chen, Li; Zu, Zhongliang

doi:10.1088/1009-9271/6/3/03

Cited by 3 publications

(2 citation statements)

References 8 publications

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“…The kinematical parameters determined from these clusters can be used to represent the kinematic properties of thin-disk objects in the vicinity of the Sun. Thus, we deduced the following Galactic parameters: (i) the mean heliocentric velocity of the OC system, (u1, u2, u3) = (−16.1 ± 1.0, −7.9 ± 0.4, −10.4 ± 1.5) km s −1 , (ii) the characteristic velocity dispersions, (σ 1 , σ 2 , σ 3 ) = (17.0 ± 0.7, 12.2 ± 0.9, 8.0 ± 1.3) km s −1 , (iii) the Oort constants, (A, B) = (14.8 ± 1.0, −13.0 ± 2.7) km s −1 kpc −1 , and (iv) the radial motion parameters, (C, D) = (1.5 ± 0.7, −1.2 ± 1.5) km s −1 kpc −1 (Zhao et al 2006). The parameters determined from these clusters have accuracies significantly better than those obtained from the other groups of clusters.…”

Section: Spatial and Kinematic Properties Of Galactic Open Clustersmentioning

confidence: 99%

Open clusters: their kinematics and metallicities

et al. 2007

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Abstract. We review our work on Galactic open clusters in recent years, and introduce our proposed large program for the LOCS (LAMOST Open Cluster Survey). First, based on the most complete open clusters sample with metallicity, age and distance data as well as kinematic information, some preliminary statistical analysis regarding the spatial and metallicity distributions is presented. In particular, a radial abundance gradient of −0.058± 0.006 dex kpc −1 is derived. By dividing clusters into the age groups we show that the disk abundance gradient was steeper in the past. Secondly, proper motions, membership probabilities, and velocity dis- The open cluster system and the observational databaseOpen clusters (OCs) are considered excellent laboratories for studies of stellar evolution. Studies in the research area dealing with OCs show a rapid growth in 1990's and this area continues to develop vigorously. There may be several reasons for this recent growth of OC studies. New techniques are greatly beneficial to the OC observations, including, for example, the application of wide-field, high quality CCD cameras and, more recently, multi-object spectrographs. In addition, OC studies play a very important and unique role in determining the structure and evolution of the Galactic disk.OCs have long been used to trace the structure and evolution of the Galactic disk. From the observational point of view, there are some important advantages of using OCs as opposed to field stars. In OCs, we deal with groups of stars of nearly the same age, a similar composition and at a similar distance. We can observe OCs to large distances, and the photometric distances to most of the OC sample have already been derived. In particular, OCs have a relatively stable orbital motion, which can be used as a better tracer of the Galactic disk structure. OCs also have a wide range of ages, so that -combined with their spatial distribution and kinematic information -we can study the effects of dynamical evolution. Very young OCs are ideal objects for studies of the stellar initial mass function. Furthermore, when combined with abundance data, we can 433 at https://www.cambridge.org/core/terms. https://doi

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Section: Spatial and Kinematic Properties Of Galactic Open Clustersmentioning

confidence: 99%

Open clusters: their kinematics and metallicities

et al. 2007

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“…The kinematical parameters determined from these clusters can be used to represent the kinematic properties of thin-disk objects in the vicinity of the Sun. Thus, we deduced the Galactic components of (i) the mean heliocentric velocity of the OC system, (u1, u2, u3) = (−16.1 ± 1.0, −7.9 ± 0.4, −10.4 ± 1.5) km s −1 , (ii) the characteristic velocity dispersions, (σ 1 , σ 2 , σ 3 ) = (17.0 ± 0.7, 12.2 ± 0.9, 8.0 ± 1.3) km s −1 , (iii) the Oort constants, (A, B) = (14.8 ± 1.0, −13.0 ± 2.7) km s −1 kpc −1 , and (iv) the radial motion parameters, (C, D) = (1.5 ± 0.7, −1.2 ± 1.5) km s −1 kpc −1 (Zhao et al 2006). The parameters determined from these clusters have accuracies significantly greater than those obtained from other groups of clusters.…”

Section: Spatial and Kinematic Properties Of Galactic Open Clustersmentioning

confidence: 99%

Open clusters: their kinematics and metellicities

Chen,

Hou,

Zhao

et al. 2007

Preprint

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We review our work on Galactic open clusters in recent years, and introduce our proposed large program for the LOCS (LAMOST Open Cluster Survey). First, based on the most complete open clusters sample with metallicity, age and distance data as well as kinematic information, some preliminary statistical analysis regarding the spatial and metallicity distributions is presented. In particular, a radial abundance gradient of -0.058± 0.006 dex kpc −1 was derived, and by dividing clusters into age groups we show that the disk abundance gradient was steeper in the past. Secondly, proper motions, membership probabilities, and velocity dispersions of stars in the regions of two very young open clusters are derived. Both clusters show clear evidence of mass segregation, which provides support for the "primordial" mass segregation scenarios. Based on the great advantages of the forthcoming LAMOST facility, we have proposed a detailed open cluster survey with LAMOST (the LOCS). The aim, feasibility, and the present development of the LOCS are briefly summarized.

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A Kinematical Calibration of the Galactocentric Distance

Shen

Zhu

2007

Chin. J. Astron. Astrophys.

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Kinematics of the Open Cluster System in the Galaxy

Cited by 3 publications

References 8 publications

Open clusters: their kinematics and metallicities

Open clusters: their kinematics and metallicities

Open clusters: their kinematics and metellicities

A Kinematical Calibration of the Galactocentric Distance

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