Kinematic structure of the corona of the Ursa Major flow 
found using proper motions and radial velocities of single stars

Чупина, Н. В.; Reva, V. G.; Верещагин, С. В.

doi:10.1051/0004-6361:20054009

Cited by 28 publications

(10 citation statements)

References 11 publications

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“…The formulae to construct the AD-diagram can be seen in Chupina et al (2001Chupina et al ( , 2006. The value of the apex coordinates for the IC 2391 cluster using data from Table 1 is (A 0 , D 0 ) = (6. h 12 ± 0. h 004, −3.…”

Section: The Ad-diagram Methodsmentioning

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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Section: The Ad-diagram Methodsmentioning

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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“…We can identify the group of stars having common space motions using this method. This method is described in good details by Chupina et al (2006). In the AD-diagram the positions of the apexes of the individual stars are calculated in equatorial coordinates.…”

Section: Apex Of the Clustersmentioning

confidence: 99%

Photometric and Kinematic study of the open clusters SAI 44 and SAI 45

Maurya¹,

C.²,

Elsanhoury³

et al. 2021

Preprint

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We carry out detailed photometric and kinematic study of the poorly studied sparse open clusters SAI 44 and SAI 45 using ground based BVR c I c data supplemented by archival data from Gaia eDR3 and Pan-STARRS. The stellar membership are determined using a statistical method based on Gaia eDR3 kinematic data and we found 204 members in SAI 44 while only 74 members are identified in SAI 45. The average distances to SAI 44 and SAI 45 are calculated as 3670±184 and 1668±47 pc. The logarithmic age of the clusters are determined as 8.82±0.10 and 9.07±0.10 years for SAI 44 and SAI 45, respectively. The color-magnitude diagram of SAI 45 hosts an extended main-sequence turn-off (eMSTO) which may be originated through differential rotation rates of member stars. The mass function slopes are obtained as -1.75±0.72 and -2.58±3.20 in the mass rages 2.426-0.990 M and 2.167-1.202 M for SAI 44 and SAI 45, respectively. SAI 44 exhibit the signature of mass segregation while we found a weak evidence of the mass segregation in SAI 45 possibly due to tidal striping. The dynamical relaxation times of these clusters indicate that both the clusters are in dynamically relaxed state. Using AD-diagram method, the apex coordinates are found to be (69. • 79 ± 0. • 11, -30. • 82 ± 0. • 15) for SAI 44 and (-56. • 22 ± 0. • 13, -56. • 62 ± 0. • 13) for SAI 45. The average space velocity components of the clusters SAI 44 and SAI 45 are calculated in units of km s −1

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“…The AD-diagram is discussed in detail by Chupina et al (2001Chupina et al ( , 2006; Vereshchagin et al (2014) and Elsanhoury et al (2018Elsanhoury et al ( , 2019. In stellar apex method, (A, D) of individual stars give the positions of those stars as a function of space velocity vectors (V x , V y , V z ).…”

Section: The Apex Of the Clustermentioning

confidence: 99%

An investigation of poorly studied open cluster NGC 4337 using multi-color photometric and Gaia DR2 astrometric data

Bisht,

Elsanhoury,

Zhu

et al. 2020

Preprint

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We present a comprehensive analysis (photometric and kinematical) of poorly studied open cluster NGC 4337 using 2MASS, WISE, APASS, and Gaia DR2 database. By determining the membership probabilities of stars, we identified 624 most probable members with membership probability higher than 50% by using proper motion and parallax data taken from Gaia DR2. The mean proper motion of the cluster is obtained as µ x = −8.83 ± 0.01 and µ y = 1.49 ± 0.006 mas yr −1 . We find the normal interstellar extinction towards the cluster region. The radial distribution of members provides a cluster radius of 7.75 arcmin (5.63 pc). The estimated age of 1600 ± 180 Myr indicates that NGC 4337 is an old open cluster with a bunch of red giant stars. The overall mass function slope for main-sequence stars is found as 1.46 ± 0.18 within the mass range 0.75−2.0 M ⊙ , which is in fair agreement with Salpeter's value (x=1.35) within uncertainty. The present study demonstrates that NGC 4337 is a dynamically relaxed open cluster. Using the Galactic potential model, Galactic orbits are obtained for NGC 4337. We found that this object follows a circular path around the Galactic center. Under the kinematical analysis, we compute the apex coordinates (A, D) by using two methods: (i) the classical convergent point method and (ii) the AD-diagram method. The obtained coordinates are: (A conv , D conv ) = (96 o .27 ± 0 o .10, 13 o .14 ± 0 o .27) & (A • , D • ) = (100 o .282 ± 0 o .10, 9 o .577 ± 0 o .323) respectively. We also computed the Velocity Ellipsoid Parameters (VEPs), matrix elements (µ ij ), direction cosines (l j , m j , n j ) and the Galactic longitude of the vertex (l 2 ).

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Kinematic structure of the corona of the Ursa Major flow found using proper motions and radial velocities of single stars

Cited by 28 publications

References 11 publications

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

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

Photometric and Kinematic study of the open clusters SAI 44 and SAI 45

An investigation of poorly studied open cluster NGC 4337 using multi-color photometric and Gaia DR2 astrometric data

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