Masses of the Planetary Nebula Central Stars in the Galactic Globular Cluster System from HST Imaging and Spectroscopy<sup>∗</sup>

Jacoby, George H.; Marco, Orsola De; Davies, James E.; Lotarevich, I.; Bond, Howard E.; Harrington, J. P.; Lanz, T.

doi:10.3847/1538-4357/836/1/93

Cited by 17 publications

(21 citation statements)

References 79 publications

(116 reference statements)

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“…Hence, if it is possible to determine the progenitor mass of a PN that is physically linked to a globular cluster, this will be a good estimation for M χ . Jacoby et al (2017) showed that the progenitor mass of the PN JaFu 1 (planetary nebulae linked to the globular cluster Pal 6) is 0.8 M .…”

Section: Review Of Stellar Evolutionmentioning

confidence: 99%

Catalogue of the central stars of planetary nebulae

Weidmann

Mari

Schmidt

et al. 2020

A&A

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Planetary nebulae represent a potential late stage of stellar evolution, however, their central stars (CSPNe) are relatively faint and, therefore, pertinent information is available for merely < 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 Teff, 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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Section: Review Of Stellar Evolutionmentioning

confidence: 99%

Catalogue of the central stars of planetary nebulae

Weidmann

Mari

Schmidt

et al. 2020

A&A

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“…Also, five objects from the Milky Way bulge with the parameters derived by Hultzsch et al (2007) are displayed (diamonds). The position of K648 in M 15 is based on the recent study of Jacoby et al (2017).…”

Section: The Milky Way Bulgementioning

confidence: 99%

“…Its effective temperature is well known (e.g. 39 000 K, Rauch et al 2002), and after careful evaluation of the distance to M 15, Jacoby et al (2017) determined recently a luminosity of 4000 L only for the central star of Ps 1.…”

Section: The Case Of K648 In M15mentioning

confidence: 99%

Expansion patterns and parallaxes for planetary nebulae

Schönberner

Balick

Jacob

2018

A&A

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Aims. We aim to determine individual distances to a small number of rather round, quite regularly shaped planetary nebulae by combining their angular expansion in the plane of the sky with a spectroscopically measured expansion along the line of sight. Methods. We combined up to three epochs of Hubble Space Telescope imaging data and determined the angular proper motions of rim and shell edges and of other features. These results are combined with measured expansion speeds to determine individual distances by assuming that line of sight and sky-plane expansions are equal. We employed 1D radiation-hydrodynamics simulations of nebular evolution to correct for the difference between the spectroscopically measured expansion velocities of rim and shell and of their respective shock fronts. Results. Rim and shell are two independently expanding entities, driven by different physical mechanisms, although their model-based expansion timescales are quite similar. We derive good individual distances for 15 objects, and the main results are as follows: (i) distances derived from rim and shell agree well; (ii) comparison with the statistical distances in the literature gives reasonable agreement; (iii) our distances disagree with those derived by spectroscopic methods; (iv) central-star “plateau” luminosities range from about 2000 L⊙ to well below 10 000 L⊙, with a mean value at about 5000 L⊙, in excellent agreement with other samples of known distance (Galactic bulge, Magellanic Clouds, and K648 in the globular cluster M 15); (v) the central-star mass range is rather restricted: from about 0.53 to about 0.56 M⊙, with a mean value of 0.55 M⊙. Conclusions. The expansion measurements of nebular rim and shell edges confirm the predictions of radiation-hydrodynamics simulations and offer a reliable method for the evaluation of distances to suited objects.

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“…On the other hand, the low-mass CSs of an old population are intrinsically unable to generate any PNe. However, Jacoby et al (2017) completed a full HST survey of all PNe in Galactic GCs and they found only the CS of Ps 1 is higher than the predicted white dwarf mass, thus requiring a history of mass augmentation (the CS of JaFu 1 shows compact and bright [Oiii] and Hα emission, suggesting a binary companion).…”

Section: Expected Value For αmentioning

confidence: 99%

The Next Generation Virgo Cluster Survey. XVII. A Search for Planetary Nebulae in Virgo Cluster Globular Clusters

Sun

Peng

et al. 2019

ApJ

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The occurrence of planetary nebulae (PNe) in globular clusters (GCs) provides an excellent chance to study low-mass stellar evolution in a special (low-metallicity, high stellar density) environment. We report a systematic spectroscopic survey for the [Oiii] 5007Å emission line of PNe in 1469 Virgo GCs and 121 Virgo ultra-compact dwarfs (UCDs), mainly hosted in the giant elliptical galaxies M87, M49, M86, and M84. We detected zero PNe in our UCD sample and discovered one PN (M 5007 = −4.1 mag) associated with an M87 GC. We used the [Oiii] detection limit for each GC to estimate the luminosityspecific frequency of PNe, α, and measured α in the Virgo cluster GCs to be α ∼ 3.9 +5.2 −0.7 ×10 −8 PN/L . α in Virgo GCs is among the lowest values reported in any environment, due in part to the large sample size, and is 5-6 times lower than that for the Galactic GCs. We suggest that α decreases towards brighter and more massive clusters, sharing a similar trend as the binary fraction, and the discrepancy between the Virgo and Galactic GCs can be explained by the observational bias in extragalactic surveys toward brighter GCs. This low but non-zero efficiency in forming PNe may highlight the important role played by binary interactions in forming PNe in GCs. We argue that a future survey of less massive Virgo GCs will be able to determine whether PN production in Virgo GCs is governed by internal process (mass, density, binary fraction), or is largely regulated by external environment.

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Masses of the Planetary Nebula Central Stars in the Galactic Globular Cluster System from HST Imaging and Spectroscopy^∗

Cited by 17 publications

References 79 publications

Catalogue of the central stars of planetary nebulae

Catalogue of the central stars of planetary nebulae

Expansion patterns and parallaxes for planetary nebulae

The Next Generation Virgo Cluster Survey. XVII. A Search for Planetary Nebulae in Virgo Cluster Globular Clusters

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Masses of the Planetary Nebula Central Stars in the Galactic Globular Cluster System from HST Imaging and Spectroscopy∗

Cited by 17 publications

References 79 publications

Catalogue of the central stars of planetary nebulae

Catalogue of the central stars of planetary nebulae

Expansion patterns and parallaxes for planetary nebulae

The Next Generation Virgo Cluster Survey. XVII. A Search for Planetary Nebulae in Virgo Cluster Globular Clusters

Contact Info

Product

Resources

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Masses of the Planetary Nebula Central Stars in the Galactic Globular Cluster System from HST Imaging and Spectroscopy^∗