A Catalog of 120 NGC Open Star Clusters

Tadross, A. L.

doi:10.5303/jkas.2011.44.1.1

Cited by 43 publications

(63 citation statements)

References 35 publications

(26 reference statements)

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“…Taking advantage of more data becoming available, refined and homogeneous determinations of spatial, structural, kinematic, and astrophysical parameters for poorly studied clusters have been published (e.g. Bonatto et al 2006;Piskunov et al 2006;Kharchenko et al 2009, Bukowiecki et al 2011Tadross et al 2011;Kharchenko et al 2013;Dias et al 2014), and a number of clusters shown to be nonexistent have been removed from the catalogues. It is important to mention that distinguishing between true gravitationally bound, physical associations from chance aggregates on the sky requires in-depth follow-up for individual cluster candidates.…”

Section: Cataloguesmentioning

confidence: 99%

Open clusters and associations in the Gaia era

Moraux

2016

EAS Publications Series

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Abstract. Open clusters and associations are groups of young stars, respectively bound and unbound, that share the same origin and disperse over time into the galactic field. As such, their formation and evolution are the key to understand the origin and properties of galactic stellar populations. Moreover, since their members have about the same age, they are ideal laboratories to study the properties of young stars and constrain stellar evolution theories.In this contribution, I present our current knowledge on open clusters and associations. I focus on the methods used to derive the statistical properties (IMF, spatial distribution, IMF) of young stars and briefly discuss how they depend on the environment. I then describe how open clusters can be used as probes to investigate the structure, dynamics and chemical composition of the Milky Way. I conclude by presenting the Gaia mission and discuss how it will revolutionize this field of research.

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Section: Cataloguesmentioning

confidence: 99%

Open clusters and associations in the Gaia era

Moraux

2016

EAS Publications Series

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“…We have estimated the value of distance modulus for DOLIDZE 14 as 11.12±0.18 mag while it turns out to be 10.57±0.28 mag for NGC 110. The distance is then obtained as 1.29±0.22 kpc for NGC 110 which is close to 1150±53 pc as calculated by Tadross (2011) while the same for the DOLIDZE 14 comes out to be 1.67±0.14 kpc. In addition, the best fit of Marigo isochrones further leads to the log(age) of NGC 110 as 9.0 (equivalent to 1 Gyr) which is close to the value 0.9±0.04 Gyr as estimated by Tadross (2011).…”

Section: Colour-magnitude Diagrams: Distance Age and Colour-excessmentioning

confidence: 99%

“…Further, the Wide-field Infrared Survey Explorer (WISE; Wright et al (2010)) operating in the mid-IR is a NASA Medium Class Explorer mission which conducted a digital imaging survey of the entire sky in the 3.4, 4.6, 12 and 22 µm (referred as W 1 , W 2 , W 3 and W 4 passbands, respectively) and has produced a reliable Source Catalog containing accurate photometry and astrometry of more than 300 million stellar objects. The cluster NGC 110 is previously studied by Tadross (2011), while DOLIDZE 14 has been termed as an OCL in a catalogue provided by Alter et al (1970) but have not been studied so far. In the present paper, we have determined various physical parameters of these OCLs in Sec.…”

Section: Introductionmentioning

confidence: 99%

Basic parameters of open star clusters DOLIDZE 14 and NGC 110 in infrared bands

Joshi

et al. 2015

New Astronomy

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The basic physical parameters of a poorly studied open cluster NGC 110 and an unstudied open cluster DOLIDZE 14 are estimated in the present study using the archival P P MXL and W ISE catalogues. The radius of both the clusters are estimated by fitting the modified King's empirical model on their stellar density profiles. The other basic parameters of the clusters such as distance, reddening, and age are obtained by visual fitting of the Marigo's solar metallicity isochrone on their IR colour-magnitude diagrams (CMDs). The mean-proper motion of the clusters are estimated through the individual proper motion of probable members identified through the dynamical and statistical methods. The archival catalogues (JHKW 1 W 2 ) are constructed for both the clusters by compiling the extracted data from the P P MXL and W ISE catalogues. The various colour-excesses, such as E(J −H), E(H −K) and E(W 1 − W 2 ), are estimated using the best fit theoretical isochrone on the (J − H) − H, (H − K) − H and (W 1 − W 2 ) − H CMDs, respectively. The ratios of various infrared colours of the clusters are obtained through their two-colour diagrams. We also identify the most probable members in these clusters by estimating spatial, kinematic and spatio-kinematic probabilities of stars within the cluster. A correlation between the E(H −K) and E(W 1 −W 2 ) is also established.

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“…Furthermore, this catalogue is a homogeneous database which allows us to observe young clusters in their dusty environments and reach out to their outer regions which is dominated by low-mass stars (Tadross 2011). The WISE (Wright et al 2010) is a NASA Medium Class Explorer mission that conducted a digital imaging survey of the entire sky in the mid-IR bands.…”

Section: Joshi Et Almentioning

confidence: 99%

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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A Catalog of 120 NGC Open Star Clusters

Cited by 43 publications

References 35 publications

Open clusters and associations in the Gaia era

Open clusters and associations in the Gaia era

Basic parameters of open star clusters DOLIDZE 14 and NGC 110 in infrared bands

Complex Stellar System ESO65SC03: Open Cluster or Remnant?

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