2MASS photometry and kinematical studies of open cluster NGC 188

Elsanhoury, W. H.; Haroon, A. A.; Чупина, Н. В.; Верещагин, С. В.; Sariya, Devesh P.; Yadav, R. K. S.; Jiang, Ing-Guey

doi:10.1016/j.newast.2016.06.002

Cited by 17 publications

(8 citation statements)

References 37 publications

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“…This method has been used and discussed for the kinematics of Ursa Major kinematic stream (Chupina et al 2001(Chupina et al , 2006. This method is also used to study the Hyades (Vereshchagin et al 2008), Orion Sword region (Vereshchagin & Chupina 2010), Praesepe (Vereshchagin & Chupina 2013), M 67 (Vereshchagin et al 2014), Castor moving group (Vereshchagin & Chupina 2015), and recently, NGC 188 (Elsanhoury et al 2016).…”

Section: The Ad-chart Methodsmentioning

confidence: 99%

The Pleiades apex and its kinematical structure

Elsanhoury¹,

Postnikova²,

Чупина³

et al. 2018

Astrophys Space Sci

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A study of cluster characteristics and internal kinematical structure of the middle-aged Pleiades open star cluster is presented. The individual star apexes and various cluster kinematical parameters including the velocity ellipsoid parameters are determined using both Hipparcos and Gaia data. Modern astrometric parameters were taken from the Gaia Data Release 1 (DR1) in combination with the Radial Velocity Experiment Fifth Data Release (DR5). The necessary set of parameters including parallaxes, proper motions and radial velocities are used for n=17 stars from Gaia DR1+RAVE DR5 and for n=19 stars from the Hipparcos catalog using SIMBAD data base. Single stars are used to improve accuracy by eliminating orbital movements. RAVE DR5 measurements were taken only for the stars with the radial velocity errors not exceeding 2 km/s. For the Pleiades stars taken from Gaia, we found mean heliocentric distance as 136.8 ± 6.4 pc, and the apex position is calculated as: A CP = 92 • .52 ± 1 • .72, D CP = −42 • .28 ± 2 • .56 by the convergent point method and A 0 = 95 • .59 ± 2 • .30 and D 0 = −50 • .90 ± 2 • .04 using AD-diagram method (n=17 in both cases). The results are compared with those obtained historically before the Gaia mission era.

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Section: The Ad-chart Methodsmentioning

confidence: 99%

The Pleiades apex and its kinematical structure

Elsanhoury¹,

Postnikova²,

Чупина³

et al. 2018

Astrophys Space Sci

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“…It is known that a moving cluster is a group of stars whose parallel motions on the celestial sphere and its direction of proper motion will direct towards a virtual point called convergent point or apex of this group. This method has been used by our group to determine apex and other kinematical parameters for open clusters M67, NGC 188 and Pleiades (Vereshchagin et al 2014, Elsanhoury et al 2016, 2018.…”

Section: Apex (Vertex Position) Of the Clustermentioning

confidence: 99%

“…Data for the cluster and the stream's stars can be found in Table 1 and Table 2, respectively. We will use these parameters to determine apex positions (example, Vereshchagin et al 2014;Elsanhoury et al 2016Elsanhoury et al , 2018 for the cluster and the stream using both convergent point method (CP) and AD-diagram method. We also study the space motion, the velocity ellipsoids, the shape in the space and birthplaces for both cluster and the stream.…”

Section: Introductionmentioning

confidence: 99%

The kinematical and space structures of IC 2391 open cluster and moving group with Gaia-DR2

Postnikova

Elsanhoury

Sariya

et al. 2020

Res. Astron. Astrophys.

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The kinematical parameters, spatial shape and structure of the open cluster IC 2391 and the associated stellar stream are studied here using Gaia-DR2 (GDR2) astrometry data. The apex positions are determined for the open cluster IC 2391 (data taken from Cantat-Gaudin et al.) and for the kinematical stream's stars mentioned in Montes et al. using both convergent point and AD-diagram methods. The values of apex coordinates are: (A, D) CP =(6. h 17 ± 0. h 004, −6. • 88 ± 0. • 381; for cluster) & (6. h 07 ± 0. h 007, −5. • 00 ± 0. • 447; stream) and (A 0 , D 0 )= (6. h 12 ± 0. h 004, −3. • 4 ± 0. • 3; cluster) & (6. h 21 ± 0. h 007, −11. • 895 ± 0. • 290; stream). The results are in good agreement with the previously calculated values. The positions of the stars in the disk and the spatial dispersion velocities are determined. The paths of cluster and associated stream are traced in the disk by orbit calculation back in time to their places of formation. A possible genetic relationship between the cluster and the stream has been detected. The approximation of the spatial and kinematical shape of the stream and the cluster is made. According to this study, even though currently the cluster and the stream seem to have spatial difference in their locations but they appear to have formed in the same region of the Galactic disk.

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“…NGC 188 serves as a test case because it is old (and therefore it exhibits a clear radial density profile) and it is located far above the Galactic plane (with little contamination by field stars). NGC 188 has been extensively studied and it has relatively well-determined physical parameters (see Table 1 in Elsanhoury et al 2016, for a summary of some published parameters). Regarding the cluster size, the radius reported in Dias et al (2002) for NGC 188 is 8.5 arcmin, which is the value given in the WEBDA database (Mermilliod 1995) Elsanhoury et al (2016).…”

Section: Test On Ngc 188mentioning

confidence: 99%

“…NGC 188 has been extensively studied and it has relatively well-determined physical parameters (see Table 1 in Elsanhoury et al 2016, for a summary of some published parameters). Regarding the cluster size, the radius reported in Dias et al (2002) for NGC 188 is 8.5 arcmin, which is the value given in the WEBDA database (Mermilliod 1995) Elsanhoury et al (2016). These dissimilar values serve to exemplify the necessity of alternative approaches such as the one proposed here.…”

Section: Test On Ngc 188mentioning

confidence: 99%

A method for determining the radius of an open cluster from stellar proper motions

Sánchez

Alfaro

López-Martínez

2018

Monthly Notices of the Royal Astronomical Society

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We propose a method for calculating the radius of an open cluster in an objective way from an astrometric catalogue containing, at least, positions and proper motions. It uses the minimum spanning tree (hereinafter MST) in the proper motion space to discriminate cluster stars from field stars and it quantifies the strength of the clusterfield separation by means of a statistical parameter defined for the first time in this paper. This is done for a range of different sampling radii from where the cluster radius is obtained as the size at which the best cluster-field separation is achieved. The novelty of this strategy is that the cluster radius is obtained independently of how its stars are spatially distributed. We test the reliability and robustness of the method with both simulated and real data from a well-studied open cluster (NGC 188), and apply it to UCAC4 data for five other open clusters with different catalogued radius values. NGC 188, NGC 1647, NGC 6603 and Ruprecht 155 yielded unambiguous radius values of 15.2 ± 1.8, 29.4 ± 3.4, 4.2 ± 1.7 and 7.0 ± 0.3 arcmin, respectively. ASCC 19 and Collinder 471 showed more than one possible solution but it is not possible to know whether this is due to the involved uncertainties or to the presence of complex patterns in their proper motion distributions, something that could be inherent to the physical object or due to the way in which the catalogue was sampled.

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2MASS photometry and kinematical studies of open cluster NGC 188

Cited by 17 publications

References 37 publications

The Pleiades apex and its kinematical structure

The Pleiades apex and its kinematical structure

The kinematical and space structures of IC 2391 open cluster and moving group with Gaia-DR2

A method for determining the radius of an open cluster from stellar proper motions

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