Apex determination and detection of stellar clumps in the open cluster M 67

Верещагин, С. В.; Чупина, Н. В.; Sariya, Devesh P.; Yadav, R. K. S.; Kumar, Brijesh

doi:10.1016/j.newast.2014.02.008

Cited by 20 publications

(14 citation statements)

References 24 publications

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“…According to Yadav et al (2008), this F9V MS star has a membership probability of 97% and a proper motion shorter than 6 mas/yr with respect to the average. Vereshchagin et al (2014) revised the membership list of Yadav et al (2008) and expressed doubts about the cluster membership for YBP401. However, the RV value considered for YBP401 in Vereshchagin et al (2014) has an uncertainty of σ = 130 m s −1 and is not consistent with our measurements by more than 1σ.…”

Section: Observations and Orbital Solutionsmentioning

confidence: 99%

“…Vereshchagin et al (2014) revised the membership list of Yadav et al (2008) and expressed doubts about the cluster membership for YBP401. However, the RV value considered for YBP401 in Vereshchagin et al (2014) has an uncertainty of σ = 130 m s −1 and is not consistent with our measurements by more than 1σ. Recently, Geller et al (2015) for the individual RV values.…”

Section: Observations and Orbital Solutionsmentioning

confidence: 99%

See 1 more Smart Citation

Search for giant planets in M67

Brucalassi

Pasquini

Saglia

et al. 2016

A&A

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Since 2008 we used high-precision radial velocity (RV) measurements obtained with different telescopes to detect signatures of massive planets around main-sequence and evolved stars of the open cluster (OC) M67. We aimed to perform a long-term study on giant planet formation in open clusters and determine how this formation depends on stellar mass and chemical composition. A new hot Jupiter (HJ) around the main-sequence star YBP401 is reported in this work. An update of the RV measurements for the two HJ host-stars YBP1194 and YBP1514 is also discussed. Our sample of 66 main-sequence and turnoff stars includes 3 HJs, which indicates a high rate of HJs in this cluster (5.6 +5.4 −2.6 % for single stars and 4.5% +4.5 −2.5 % for the full sample). This rate is much higher than what has been discovered in the field, either with RV surveys or by transits. High metallicity is not a cause for the excess of HJs in M67, nor can the excess be attributed to high stellar masses. When combining this rate with the non-zero eccentricity of the orbits, our results are qualitatively consistent with a HJ formation scenario dominated by strong encounters with other stars or binary companions and subsequent planet-planet scattering, as predicted by N-body simulations.

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Section: Observations and Orbital Solutionsmentioning

confidence: 99%

Section: Observations and Orbital Solutionsmentioning

confidence: 99%

Search for giant planets in M67

Brucalassi

Pasquini

Saglia

et al. 2016

A&A

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“…The details of the AD-method can be found in Chupina (2006). We used this method to study the kinematics of various open clusters, namely M 67 (Vereshchagin et al 2014), Pleiades (Elsanhoury et al 2018), IC 2391 (Postnikova et al 2020) and NGC 2158 (Sariya et al 2021a).…”

Section: The Apex Of King 11mentioning

confidence: 99%

A Gaia based photometric and kinematic analysis of the old open cluster King 11

Sariya,

Jiang,

Bisht

et al. 2021

Preprint

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This paper presents an investigation of an old age open cluster King 11 using Gaia's Early Data Release 3 (EDR3) data. Considering the stars with membership probability (P µ ) > 90%, we identified 676 most probable cluster members within the cluster's limiting radius. The mean proper motion (PM) for King 11 is determined as: µ x = −3.391 ± 0.006 and µ y = −0.660 ± 0.004 mas yr −1 . The blue straggler stars (BSS) of King 11 show a centrally concentrated radial distribution. The values of limiting radius, age, and distance are determined as 18.51 arcmin, 3.63±0.42 Gyr and 3.33 ± 0.15 kpc, respectively. The cluster's apex coordinates (A = 267.84 • ± 1.01 • , D = −27.48 • ± 1.03 • ) are determined using the apex diagram (AD) method and verified using the (µ U ,µ T ) diagram. We also obtained the orbit that the cluster follows in the Galaxy and estimated its tentative birthplace in the disk. The resulting spatial velocity of King 11 is 60.2 ± 2.16 km s −1 . A significant oscillation along the Z-coordinate up to 0.556±0.022 kpc is determined.

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“…We aim to derive apex coordinates (A, D) of the cluster on the celestial sphere (Vereshchagin et al 2014, Postnikova et al 2020 based on 2MASS and Gaia DR2 catalogs. The apex demonstrates the actual direction where the object moves.…”

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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Apex determination and detection of stellar clumps in the open cluster M 67

Cited by 20 publications

References 24 publications

Search for giant planets in M67

Search for giant planets in M67

A Gaia based photometric and kinematic analysis of the old open cluster King 11

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

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