Properties of the Old Open Cluster Czernik 30

Hayes, Christian R.; Friel, Eileen D.; Slack, Taleah J.; Boberg, Owen M.

doi:10.1088/0004-6256/150/6/200

Cited by 8 publications

(11 citation statements)

References 22 publications

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“…Our analysis results in a distance of 6.5 kpc and an age of 3.6 Gyr. These values are in good agreement with those of Dias et al (2021) (5.9 kpc, 3 Gyr), but the distance strongly differs with the one found in Hayes et al (2015). Hayes et al determined 9.12 kpc and 2.8 Gyr for the distance and age, respectively, meaning that they have overestimated the cluster distance.…”

Section: Clustersupporting

confidence: 78%

“…The situation is not much better for the older OCs which do not have very luminous stars in the main sequence, although they do in the giant branch. Stars in the lower part of the main sequences, as well as those belonging to the giant branch, share similar photometric characteristics with field stars making it rather difficult to unravel to which population each star belongs (Hayes et al 2015). The situation worsens as the distance to the older OCs increases because the limiting magnitude increases, which results in only a small portion of the lower part being visible.…”

Section: Introductionmentioning

confidence: 99%

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An analysis of the most distant catalogued open clusters -- Re-assessing fundamental parameters with Gaia EDR3 and $\texttt{ASteCA}$

Perren,

Pera,

Navone

et al. 2022

Preprint

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Context. Several studies have been presented in the last few years applying some kind of automatic processing of data to estimate the fundamental parameters of open clusters. These parameters are later on employed in larger scale analyses, for example the structure of the Galaxy's spiral arms. The distance is one of the more straightforward parameters to estimate, yet enormous differences can still be found among published data. This is particularly true for open clusters located more than a few kpc away. Aims. We cross-matched several published catalogues and selected the twenty-five most distant open clusters (>9000 pc). We then performed a detailed analysis of their fundamental parameters, with emphasis on their distances, to determine the agreement between catalogues and our estimates. Methods. Photometric and astrometric data from the Gaia EDR3 survey was employed. The data was processed with our own membership analysis code (pyUPMASK), and our package for automatic fundamental cluster's parameters estimation (ASteCA). Results. We find differences in the estimated distances of up to several kpc between our results and those catalogued, even for the catalogues that show the best matches with ASteCA values. Large differences are also found for the age estimates. As a by-product of the analysis we find that vd Bergh-Hagen 176 could be the open cluster with the largest heliocentric distance catalogued to date. Conclusions. Caution is thus strongly recommended when using catalogued parameters of open clusters to infer large-scale properties of the Galaxy, particularly for those located more than a few kpc away.

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Section: Clustersupporting

confidence: 78%

Section: Introductionmentioning

confidence: 99%

An analysis of the most distant catalogued open clusters -- Re-assessing fundamental parameters with Gaia EDR3 and $\texttt{ASteCA}$

Perren,

Pera,

Navone

et al. 2022

Preprint

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“…In fact, offsets from isochrones have been noticed both in metal-poor globular clusters (e.g., Brasseur et al 2010;Cohen et al 2015) and metal-rich bulge stars (Ness et al 2013). Additionally, work on open clusters has indicated that, depending on the choice of models, isochrones can be too blue in some bands and too red in others (see e.g., Hayes et al 2015). However, because each of these regimes is usually analyzed individually, using each author's choice of models and colors, this likely made it more difficult to identify a systematic offset between the models and the data.…”

Section: Why Was This Not Noticed Before?mentioning

confidence: 99%

The Correlation between Mixing Length and Metallicity on the Giant Branch: Implications for Ages in the Gaia Era

Tayar

Somers

Pinsonneault

et al. 2017

ApJ

109

105

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In the updated APOGEE-Kepler catalog, we have asteroseismic and spectroscopic data for over 3000 first ascent red giants. Given the size and accuracy of this sample, these data offer an unprecedented test of the accuracy of stellar models on the post-main-sequence. When we compare these data to theoretical predictions, we find a metallicity dependent temperature offset with a slope of around 100 K per dex in metallicity. We find that this effect is present in all model grids tested, and that theoretical uncertainties in the models, correlated spectroscopic errors, and shifts in the asteroseismic mass scale are insufficient to explain this effect. Stellar models can be brought into agreement with the data if a metallicity-dependent convective mixing length is used, with Δα ML, YREC ∼0.2 per dex in metallicity, a trend inconsistent with the predictions of three-dimensional stellar convection simulations. If this effect is not taken into account, isochrone ages for red giants from the Gaia data will be off by as much as a factor of two even at modest deviations from solar metallicity ([Fe/H]=−0.5).

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“…However, CMDs can be contaminated severely by the field population along the line of sight (e.g., Sung & Bessell 2010;Da Rio et al 2010;Chauhan et al 2011;Sung et al 2013;Pandey et al 2013b). The cluster population can be distinguished from the general Galactic population along the line of sight through a comparison of the CMDs of the cluster region and the control field (e.g., Brandner et al 2008;Sharma et al 2008;Gennaro et al 2011;Hayes et al 2015). In Fig 2a and 2b, we show the V vs. (V -I) CMDs for the stars in the cluster region and control field, respectively.…”

Section: Identification Of Pms Members Of the Clustermentioning

confidence: 99%

Young Cluster Berkeley 59: Properties, Evolution, and Star Formation

Panwar

Pandey

Samal

et al. 2018

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Berkeley 59 is a nearby (∼1 kpc) young cluster associated with the Sh2-171 Hii region. We present deep optical observations of the central ∼ 2.5 × 2.5 pc 2 area of the cluster, obtained with the 3.58-m Telescopio Nazionale Galileo. The V /(V -I) color-magnitude diagram manifests a clear pre-mainsequence (PMS) population down to ∼ 0.2 M . Using the near-infrared and optical colors of the low-mass PMS members we derive a global extinction of A V = 4 mag and a mean age of ∼ 1.8 Myr, respectively, for the cluster. We constructed the initial mass function and found that its global slopes in the mass ranges of 0.2 -28 M and 0.2 -1.5 M are -1.33 and -1.23, respectively, in good agreement with the Salpeter value in the solar neighborhood. We looked for the radial variation of the mass function and found that the slope is flatter in the inner region than in the outer region, indicating mass segregation. The dynamical status of the cluster suggests that the mass segregation is likely primordial. The age distribution of the PMS sources reveals that the younger sources appear to concentrate close to the inner region compared to the outer region of the cluster, a phenomenon possibly linked to the time evolution of star-forming clouds is discussed. Within the observed area, we derive a total mass of ∼10 3 M for the cluster. Comparing the properties of Berkeley 59 with other young clusters, we suggest it resembles more to the Trapezium cluster.

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Properties of the Old Open Cluster Czernik 30

Cited by 8 publications

References 22 publications

An analysis of the most distant catalogued open clusters -- Re-assessing fundamental parameters with Gaia EDR3 and $\texttt{ASteCA}$

An analysis of the most distant catalogued open clusters -- Re-assessing fundamental parameters with Gaia EDR3 and $\texttt{ASteCA}$

The Correlation between Mixing Length and Metallicity on the Giant Branch: Implications for Ages in the Gaia Era

Young Cluster Berkeley 59: Properties, Evolution, and Star Formation

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