Central Stars of Planetary Nebulae in Galactic Open Clusters: Providing additional data for the White Dwarf Initial-to-Final-Mass Relation

Fragkou, Vasiliki; Parker, Quentin A.; Zijlstra, A. A.; Shaw, Richard A.; Lykou, Foteini

doi:10.1017/s1743921318005641

Cited by 5 publications

(6 citation statements)

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“…The case of vd Bergh-Hagen 144 is interesting because its estimated metallicity of [Fe/H] = −0.53 −0.55 −0.48 is well below the expected solar value at that distance (R GC ∼ 8.5 kpc). There are two other articles where a similar markedly sub-solar metallicity was found for this cluster: Frinchaboy et al (2006b) and Fragkou et al (2019). In these studies the reported metallicity values are [Fe/H] = −0.51 ± 0.3 (spectroscopic metallicity from two stars) and [Fe/H] ≈ −0.40 (photometric estimate) 7 for Frinchaboy et al (2004) and Fragkou et al (2019), respectively.…”

Section: Resultssupporting

confidence: 66%

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An analysis of the most distant cataloged open clusters

Perren

Pera

Navone

et al. 2022

A&A

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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 then employed in larger scale analyses, for example the structure of the Galaxy’s spiral arms. The distance is one of the most 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 kiloparsecs away. Aims. We cross-matched several published catalogs and selected the 25 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 the catalogs and our estimates. Methods. Photometric and astrometric data from the Gaia EDR3 survey was employed. The data were processed with our own membership analysis code, pyUPMASK, and our package for the automatic estimation of fundamental cluster parameters, ASteCA. Results. We find differences in the estimated distances of up to several kiloparsecs between our results and those cataloged, even for the catalogs 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 cataloged to date. Conclusions. Caution is thus strongly recommended when using cataloged parameters of open clusters to infer large-scale properties of the Galaxy, particularly for those located more than a few kiloparsecs away.

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Section: Resultssupporting

confidence: 66%

“…Both age and distance values for these two articles are very close to ours. Recently Fragkou et al (2019) suggested a slightly larger distance of ∼ 12 kpc, the value present in OC02 and WEBDA, and an age of about 0.66 Gyr.…”

Section: Discussionmentioning

confidence: 82%

An analysis of the most distant cataloged open clusters

Perren

Pera

Navone

et al. 2022

A&A

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“…Frinchaboy et al (2004b) andFragkou et al (2019). In these studies the reported metallicity values are [Fe/H]=-0.51±0.3 (spectroscopic metallicity from 2 stars) and [Fe/H]≈-0.40 (photometric estimate) 7 , forFrinchaboy et al and Fragkou et al respectively.…”

mentioning

confidence: 84%

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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“…Nevertheless, the confirmation of a PN associated to an open cluster, has a direct implication on the upper limit on the progenitor's mass. Fragkou et al (2019a) and Fragkou et al (2019b) have proved that the PNe PHR 1315−6555 and BMP J1613−5406 are physically linked to an open cluster. Consequently we have, for the first time, observational evidence that the upper limit of the initial stellar mass for the formation of a PN can be as high as M * 5.0 M ⊙ .…”

Section: Introductionmentioning

confidence: 99%

Catalogue of central stars of planetary nebulae: Expanded edition

Weidmann,

Mari,

Schmidt

et al. 2020

Preprint

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Planetary nebulae represent a potential late stage of stellar evolution, however the central stars (CSPNe) are relatively faint and therefore pertinent information is merely available for <20% of the Galactic sample. Consequently, the literature was surveyed to construct a new catalogue of 620 CSPNe featuring important spectral classifications and information. The catalogue supersedes the existing iteration by 25%, and includes physical parameters such as luminosity, surface gravity, temperature, magnitude estimates, and references for published spectra. The marked statistical improvement enabled the following pertinent conclusions to be determined: the H-rich/H-poor ratio is 2:1, there is a deficiency of CSPNe with types [WC 5-6], and nearly 80% of binary central stars belong to the H-rich group. The last finding suggests that evolutionary scenarios leading to the formation of binary central stars interfere with the conditions required for the formation of H-poor CSPN. Approximately 50% of the sample with derived values of log L, log T eff , and log g, exhibit masses and ages consistent with single stellar evolutionary models. The implication is that single stars are indeed able to form planetary nebulae. Moreover, it is shown that H-poor CSPNe are formed by higher mass progenitors. The catalogue is available through the Vizier database.

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Central Stars of Planetary Nebulae in Galactic Open Clusters: Providing additional data for the White Dwarf Initial-to-Final-Mass Relation

Cited by 5 publications

References 4 publications

An analysis of the most distant cataloged open clusters

An analysis of the most distant cataloged open clusters

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

Catalogue of central stars of planetary nebulae: Expanded edition

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