Proper motions and membership probabilities of stars in the region of open cluster NGC 3766

Yadav, R. K. S.; Sariya, Devesh P.; Sagar, Ram

doi:10.1093/mnras/stt136

Cited by 56 publications

(49 citation statements)

References 23 publications

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“…In addition, the MF values of brighter members of the system is too low for it to be an OC. The typical MF value for brighter members of any OC reported is much lower than our value (Lata et al 2014;Joshi et al 2014;Glushkova et al 2013;Yadav et al 2013;Tadross et al 2012;Tadross 2011;Bhatt, Sagar, & Pandey 2012;Sharma et al 2008). There is also a possibility that the lighter members of this system has already evaporated from its central region as expected by the phenomenon of mass segregation.…”

Section: Discussioncontrasting

confidence: 76%

Complex Stellar System ESO65SC03: Open Cluster or Remnant?

Joshi

Joshi²,

Joshi³

et al. 2015

Publ. Astron. Soc. Aust.

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We present a complete spatial and dynamical study of the poorly populated stellar system ESO65SC03. The radial distribution of the system gives a core and cluster radii of 1.10 ± 0.63 and 5.36 ± 0.24 arcmin, respectively. The SNDP does not show any clear enhancement of the surface stellar number density between the stars of the system and the field regions. We derive the optimum isochrone solution for a particular grid size in the CMD using the statistical cleaning procedure. Using the statistically cleaned CMDs, we find the distance modulus, (m − M) 0 , and reddening, E(B − V ), of the system to be 11.8 ± 0.2 and 0.45 mag, respectively. The mean proper motion of this system is −5.37 ± 0.81 mas yr −1 and 0.31 ± 0.40 in RA and DEC directions, respectively. The mean proper motion of this system is found to be almost similar to the field region. The mass function for the brighter stars is found to be too high for the system to be an open cluster. These combined results place constraints on whether stellar system ESO65SC03 is a POCR or an Asterism. Our understanding is that the ESO65SC03 is in a stage of POCR by losing their main-sequence stars in the dynamic evolution processes.

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Section: Discussioncontrasting

confidence: 76%

Complex Stellar System ESO65SC03: Open Cluster or Remnant?

Joshi

Joshi²,

Joshi³

et al. 2015

Publ. Astron. Soc. Aust.

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“…The major difficulty in determination of the cluster parameters using isochrone fitting is contamination by the field stars. The proper motions based vector point diagram is very effective in separating field stars from the member stars of a cluster (Yadav et al 2013;Straižys et al 2019). With the availability of the Gaia DR2 catalog with unprecedented astrometric precision, kinematic study of the OCs has become more reliable (Cantat-Gaudin et al 2018;Castro-Ginard et al 2018Liu & Pang 2019;Joshi et al 2020).…”

Section: Proper Motion Membershipmentioning

confidence: 99%

Photometric and kinematic study of the three intermediate age open clusters NGC 381, NGC 2360, and Berkeley 68

Maurya

Joshi

2020

Monthly Notices of the Royal Astronomical Society

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We present UBVR c I c photometric study of three intermediate age open star clusters NGC 381, NGC 2360, and Berkeley 68 (Be 68). We examine the cluster membership of stars using recently released Gaia DR2 proper motions and obtain a total of 116, 332, and 264 member stars in these three clusters. The mean reddening of E(B − V) = 0.36±0.04, 0.08±0.03, and 0.52±0.04 mag are found in the direction of these clusters where we observe an anomalous reddening towards NGC 381. We fitted the solar metallicity isochrones to determine age and distance of the clusters which are found to be log(Age) = 8.65±0.05, 8.95±0.05, and 9.25±0.05 yr with the respective distance of 957±152, 982±132, and 2554±387 pc for the clusters NGC 381, NGC 2360, and Be 68. A two-stage power law in the mass function (MF) slope is observed in the cluster NGC 381, however, we observe only a single MF slope in the clusters NGC 2360 and Be68. To study a possible spatial variation in the slope of MF we estimate slopes separately in the inner and the outer regions of these clusters and notice a steeper slope in outer region. The dynamic study of these clusters reveals deficiency of lowmass stars in their inner regions suggesting the mass segregation process in all these clusters. The relaxation times of 48.5, 78.9, and 87.6 Myr are obtained for the clusters NGC 381, NGC 2360, and Be 68, respectively which are well below to their respective ages. This suggests that all the clusters are dynamically relaxed.

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“…In the present work, we followed the method described in Balaguer-Núñez et al (1998). This is the same method that we used for NGC 6809 (Sariya et al 2012) and NGC 3766 (Yadav et al 2013). According to this method, the frequency distribution functions of cluster stars (φ ν c ) and field stars (φ ν f ) are constructed for the ith star using the equations…”

Section: Membership Probabilitiesmentioning

confidence: 99%

“…Therefore, a catalogue with membership information covering a wide field centered on the cluster is very much needed. The archival data taken with the WFI at the 2.2 m ESO telescope enable us to derive proper motions by using an epoch gap of only a few years, deeper by several magnitudes, and covering a larger region (Anderson et al 2006;Yadav et al 2008Yadav et al , 2013Bellini et al 2009;Sariya et al 2012). We selected the WFI at the 2.2 m ESO telescope because it is one of the first wide-field cameras available, thus it has a long time baseline in its public archive.…”

Section: Introductionmentioning

confidence: 99%

Proper motions and membership probabilities of stars in the region of globular cluster NGC 6366

Sariya

Yadav

2015

A&A

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Context. NGC 6366 is a metal-rich globular cluster that is relatively unstudied. It is a kinematically interesting cluster, reported as belonging to the slowly rotating halo system, which is unusual given its metallicity and spatial location in the Galaxy. Aims. The purpose of this research is to determine the relative proper motion and membership probability of the stars in the region of globular cluster NGC 6366. To target cluster members reliably during spectroscopic surveys without including field stars, a good proper motion and membership probability catalogue of NGC 6366 is needed. Methods. To derive relative proper motions, the archival data from the Wide Field Imager mounted on the ESO 2.2 m telescope have been reduced using a high precision astrometric software. The images used are in the B, V, and I photometric bands with an epoch gap of ∼3.2 yr. The calibrated BV I magnitudes have been determined using recent data for secondary standard stars. Results. We determined relative proper motions and cluster membership probabilities for 2530 stars in the field of globular cluster NGC 6366. The median proper motion rms errors for stars brighter than V ∼ 18 mag is ∼2 mas yr −1 , which gradually increases to ∼5 mas yr −1 for stars having magnitudes V ∼ 20 mag. Based on the membership catalogue, we checked the membership status of the X-ray sources and variable stars of NGC 6366 mentioned in the literature. We also provide the astronomical community with an electronic catalogue that includes B, V, and I magnitudes; relative proper motions; and membership probabilities of the stars in the region of NGC 6366.

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Proper motions and membership probabilities of stars in the region of open cluster NGC 3766

Cited by 56 publications

References 23 publications

Complex Stellar System ESO65SC03: Open Cluster or Remnant?

Complex Stellar System ESO65SC03: Open Cluster or Remnant?

Photometric and kinematic study of the three intermediate age open clusters NGC 381, NGC 2360, and Berkeley 68

Proper motions and membership probabilities of stars in the region of globular cluster NGC 6366

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