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

AbstractAccurate (< 10%) distances of Galactic star clusters allow a precise estimation of the physical parameters of any physically associated Planetary Nebula (PN) and also that of its central star (CSPN) and its progenitor. The progenitor’s mass can be related to the PN’s chemical characteristics and, furthermore, provides additional data for the widely used white dwarf (WD) initial-to-final mass relation (IFMR) that is crucial for tracing the development of both carbon and nitrogen in entire galaxies. To date, there is only one PN (PHR1315- 6555) confirmed to be physically associated with a Galactic open cluster (ESO 96 -SC04) that has a turn-off mass ∼2Mʘ. Our deep HST photometry was used for the search of the CSPN of this currently unique PN. In this work, we present our results.

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What we can say about PN if their luminosity function distances are correct

Symposium - International Astronomical Union ◽

10.1017/s0074180900131705 ◽

1997 ◽

Vol 180 ◽

pp. 448-459

Author(s):

George H. Jacoby

Keyword(s):

Ionizing Radiation ◽

Luminosity Function ◽

High Reliability ◽

Central Star ◽

Nitrogen Enrichment ◽

Mass Relation ◽

Final Mass ◽

Method Agreement ◽

Central Stars ◽

Better Than

I review the arguments favoring the high reliability of the PNLF method. Agreement with Cepheid distances is better than 8%, and consistency for multiple PNLF distances within clusters is even better. Agreement between Cepheid distances to spirals and PNLF distances to ellipticals within the same cluster also is excellent. In order for the PNLF method to work despite the vast diversity of properties seen among PN, several factors must operate. Most importantly, the progenitors of the bright extragalactic PN probably have ages less than ∼10 Gyrs. Also, very young PN must either be absent from the bright extragalactic samples or must have lower luminosities than suggested by their predicted central star masses. The latter may be due to internal dust, nitrogen enrichment that competes with oxygen for ionizing photons, and/or a tendency for massive PN to be optically thin to ionizing radiation. In addition, models that reproduce observed PNLFs rely on theoretical evolutionary tracks of central stars, and so these tracks also must be reasonably correct. PNLF observations suggest, however, that the slope of the initial-to-final mass relation is shallower than the Weidemann (1987) relation.

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Constraining axion-like particles using the white dwarf initial-final mass relation

Journal of Cosmology and Astroparticle Physics ◽

10.1088/1475-7516/2021/09/010 ◽

2021 ◽

Vol 2021 (09) ◽

pp. 010 ◽

Cited By ~ 1

Author(s):

Matthew J. Dolan ◽

Frederick J. Hiskens ◽

Raymond R. Volkas

Keyword(s):

White Dwarf ◽

Mass Relation ◽

Final Mass

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Ensemble evolutionary studies of white dwarfs in open star clusters

Proceedings of the International Astronomical Union ◽

10.1017/s1743921320000848 ◽

2019 ◽

Vol 15 (S357) ◽

pp. 179-183

Author(s):

Kurtis A Williams

Keyword(s):

White Dwarfs ◽

Binary Star ◽

Open Cluster ◽

Star Clusters ◽

Mass Relation ◽

Correlated Errors ◽

Open Star Clusters ◽

Open Star ◽

Final Mass ◽

Evolutionary Studies

AbstractWhite dwarfs (WDs) in open star clusters are a highly useful ensemble of stars. While numerous researchers use open cluster WDs to study the initial-final mass relation, numerous other evolutionary studies are also enabled by this sample of stars, including searches for stochastic mass loss, studies of binary star evolution, and measurements of metallicity impacts on WD formation and evolution. However, it is crucial to use astrometric data such as proper motions to remove contaminating field WDs from open cluster samples; multi-epoch ground based imaging is needed for most open cluster WDs. Also, the strongly correlated errors in the initial mass - final mass plane must be considered; we illustrate the importance of this consideration using a large open cluster WD sample and Monte Carlo techniques.

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THE WHITE DWARF POPULATION IN NGC 1039 (M34) AND THE WHITE DWARF INITIAL-FINAL MASS RELATION

The Astronomical Journal ◽

10.1088/0004-6256/135/6/2163 ◽

2008 ◽

Vol 135 (6) ◽

pp. 2163-2176 ◽

Cited By ~ 25

Author(s):

Kate H. R. Rubin ◽

Kurtis A. Williams ◽

M. Bolte ◽

Detlev Koester

Keyword(s):

White Dwarf ◽

Mass Relation ◽

Final Mass

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An imaging and spectroscopic survey of the Abell Planetary Nebulae

Symposium - International Astronomical Union ◽

10.1017/s0074180900131043 ◽

1997 ◽

Vol 180 ◽

pp. 287-287

Author(s):

N. A. Walton ◽

J. R. Walsh ◽

G. Dudziak

Keyword(s):

White Dwarf ◽

Surface Brightness ◽

Planetary Nebulae ◽

Central Star ◽

Large Size ◽

Low Surface Brightness ◽

Thermal Pulses ◽

Central Stars

The Abell catalogue of planetary nebulae (PN) are distinguished by their large size, low surface brightness and generally faint central stars. They are thought to be old PN approaching the White Dwarf cooling track. A number have evidence for late thermal pulses (H-poor ejecta near the central star, e.g. A78) and binary central stars.

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The nature of the NGC 2546: Not one but two open clusters

Astronomy and Astrophysics ◽

10.1051/0004-6361/201936294 ◽

2020 ◽

Vol 633 ◽

pp. A146 ◽

Cited By ~ 1

Author(s):

A. D. Alejo ◽

J. F. González ◽

M. E. Veramendi

Keyword(s):

Radial Velocity ◽

Binary Stars ◽

Open Cluster ◽

Open Clusters ◽

Spectroscopic Binaries ◽

Physical Parameters ◽

Distance Modulus ◽

Cluster Membership ◽

Spectroscopic Observations ◽

Astrometric Data

Context. As part of a broader project on the role of binary stars in clusters, we present a spectroscopic study of the open cluster NGC 2546, which is a large cluster lacking previous spectroscopic analysis. Aims. We report the finding of two open clusters in the region of NGC 2546. For the two star groups, we determine radial velocity, parallax, proper motion, reddening, distance modulus, and age, using our spectroscopic observations and available photometric and astrometric data, mainly from the second Gaia data release (Gaia-DR2). We also determine the orbit of four spectroscopic binaries in these open clusters. Methods. From mid-resolution spectroscopic observations for 28 stars in the NGC 2546 region, we determined radial velocities and evaluate velocity variability. To analyze double-lined spectroscopic binaries, we used a spectral separation technique and fit the spectroscopic orbits using a least-squares code. The presence of two stellar groups is suggested by the radial velocity distribution and confirmed by available photometric and astrometric data. We applied a multi-criteria analysis to determine cluster membership, and obtained kinematic and physical parameters of the clusters. Results. NGC 2546 is actually two clusters, NGC 2546A and NGC 2546B, which are not physically related to each other. NGC 2546A has an age of about 180 Myr and a distance of 950 pc. It has a half-number radius of 8 pc and contains about 480 members brighter than G = 18 mag. NGC 2546B is a very young cluster (<10 Myr) located at a distance of 1450 pc. It is a small cluster with 80 members and a half-number radius of 1.6 pc. Stars less massive than 2.5 M⊙ in this cluster would be pre-main-sequence objects. We detected four spectroscopic binaries and determined their orbits. The two binaries of NGC 2546A contain chemically peculiar components: HD 68693 is composed of two mercury-manganese stars and HD 68624 has a Bp silicon secondary. Among the most massive objects of NGC 2546B, there are two binary stars: HD 68572, with P = 124.2 d, and CD -37 4344 with P = 10.4 d.

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The Initial–Final Mass Relationship of White Dwarfs in Common Proper Motion Pairs and Open Clusters

Proceedings of the International Astronomical Union ◽

10.1017/s1743921307004322 ◽

2006 ◽

Vol 2 (S240) ◽

pp. 380-382

Author(s):

S. Catalán ◽

I. Ribas ◽

J. Isern ◽

E. García–Berro ◽

C. Allende Prieto

Keyword(s):

White Dwarf ◽

Proper Motion ◽

White Dwarfs ◽

Open Clusters ◽

Type Star ◽

Spectroscopic Observations ◽

Final Mass ◽

Semi Empirical ◽

Relationship Of

AbstractWe have studied white dwarfs in common proper motion pairs (CPMPs) to improve the semi-empirical initial–final mass relationship of white dwarfs. In this contribution, we report new results obtained from spectroscopic observations of both members of several CPMPs composed of an F, G or K type star and a DA white dwarf.

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Constraints on stellar evolution by observation of white dwarfs

Symposium - International Astronomical Union ◽

10.1017/s0074180900030953 ◽

1984 ◽

Vol 105 ◽

pp. 229-230 ◽

Cited By ~ 1

Author(s):

V. Weidemann

Keyword(s):

White Dwarfs ◽

Recent Observation ◽

Open Cluster ◽

High Mass ◽

Mass Relation ◽

List Type ◽

Intermediate Mass Stars ◽

Final Mass ◽

Star Production ◽

The Rich

The recent observation of white dwarfs in the open cluster NGC 2516 and the determination of their surface gravity and effective temperatures (Reimers and Koester, 1982) has enabled the establishment of the initial-final mass relation for low and intermediate mass stars which was published a few months ago and is presented here (Fig. 1 of Weidemann and Koester, 1983a). The most important conclusions drawn are: 1.The limiting mass for white dwarf progenitors is 8–9 M⊙ rather than 5–6 M⊙, with supernova production beyond;2.The rather flat run of the initial-final mass relation in the main range of star production, 1–5 M⊙, explains the observed narrow mass distribution of white dwarfs and central stars of planetary nebulae around 0.6 M⊙;3.High mass white dwarfs exist, as shown in the rich, young cluster NGC 2516, but are extremely rare in general.

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Testing white dwarf cosmochronology using wide double white dwarfs

Proceedings of the International Astronomical Union ◽

10.1017/s1743921320000782 ◽

2019 ◽

Vol 15 (S357) ◽

pp. 197-201

Author(s):

Tyler Heintz ◽

JJ Hermes

Keyword(s):

White Dwarf ◽

White Dwarfs ◽

Mass Relation ◽

Final Mass ◽

Gaia Dr2

AbstractWe present a sample of nearly 650 widely separated double white dwarf binaries found using Gaia DR2 astrometry. We derive preliminary total ages for each white dwarf in our sample using Gaia photometry and compare the total ages of both components of each binary in our sample. We find agreement within 3 sigma between the two ages ∼85% of the time with median age uncertainties of ∼3.5 Gyr depending on which initial-final mass relation is used. When a subsample with the most precise ages is used, the agreement within 3 sigma drops to ∼70% with median age uncertainties of 300-600 Myr.

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