Spectroscopic and photometric studies of white dwarfs in the Hyades

Tremblay, Pier-Emmanuel; Schilbach, E.; Röser, S.; Jordan, S.; Ludwig, H.‐G.; Goldman, B.

doi:10.1051/0004-6361/201220057

Cited by 20 publications

(34 citation statements)

References 77 publications

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“…Finally, we made use of the analysis by Salaris et al (2009) to assess the effect of decreasing the mass thickness of the hydrogen layers of the models by two orders of magnitude, below the standard 'thick' layers value of 10 −4 M WD . For the magnitude and colour range of our sample of Hyades WDs 3 In addition, the H and He profiles are not step function like in Salaris et al (2010) and Fontaine et al (2001) but have been shaped by atomic diffusion during the early WD phases (7) and (9) of Table 1) and the corresponding values from Tremblay et al (2012).…”

Section: Namementioning

confidence: 86%

“…In this diagram, we also show the Gaia DR2 proper motions for the 25 WD cluster member candidates defined in Table 2 of Tremblay et al (2012); only 9 out of these 25 objects are defined as members by the Gaia team. Given the large motion of the cluster, and the fact that proper motions are better constrained than parallaxes, we relax the membership selections of Gaia Collaboration et al (2018b) and arbitrarily use only proper motions as membership criterion for the 25 objects in Tremblay et al (2012) Table 2. We set the proper motion threshold for membership as large as the largest motions in the Gaia member sample, approximated to the next round number.…”

Section: Datamentioning

confidence: 99%

“…Of the 12 WD member candidates that survive this mild proper motion selection, 9 were already in the Gaia selection, and only 3 are potential additional WDs candidates. Seven of the 9 WDs surviving the Gaia selection -also included in Tremblay et al (2012) paperare 'classical' Hyades WDs as defined by Tremblay et al (2012) and previously used in IFMR determinations (see, e.g., Ferrario et al 2005;Salaris et al 2009). Two other objects (HG 7-85, and GD 52) belong to the 'new candidates' listed by Tremblay et al (2012).…”

Section: Datamentioning

confidence: 99%

“…Moreover, Gaia DR2 data will allow us to determine whether the sample of new Hyades WD candidates discussed in Tremblay et al (2012) contains truly Hyades stars.…”

Section: Introductionmentioning

confidence: 99%

“…The plan of the paper is as follows. Section 2 describes the Hyades WD sample and the membership of Tremblay et al (2012) candidates, whilst section 3 describes our derivation of the IFMR and associated errors. Section 4 Figure 1.…”

Section: Introductionmentioning

confidence: 99%

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A Gaia DR2 view of white dwarfs in the Hyades

Salaris

Bedin

2018

Monthly Notices of the Royal Astronomical Society

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We have exploited the very precise parallaxes, proper motions and photometry of Gaia Data Release 2 to study white dwarf members of the Hyades star cluster. Gaia photometry and parallaxes for the eight DA white dwarfs confirmed members have been then used to compute absolute magnitudes and colours. These were compared to three independent sets of white dwarf evolutionary tracks, to derive cooling times and white dwarf (final) masses. All sets of models provide the same mass values, with only small differences in the cooling ages. The precision in the derived masses and cooling ages is typically 1-3%. Our derived masses are generally consistent with spectroscopic estimates from the literature, whilst cooling ages are generally larger. The recent estimate of the cluster age from the Gaia Data Release 2 main sequence turn off colour-magnitude-diagram (790 Myr) has been employed to derive progenitor (initial) masses. We find a slope of the initial-final mass relation for the Hyades white dwarfs (masses between ∼0.67 and ∼ 0.84M ⊙ ) steeper than that derived for the same mass range from global estimates -averaged over the whole spectrum of white dwarf masses-irrespectively of the cooling models adopted. However, when considering the error in this age estimate ( +160 −100 Myr), a definitive conclusion on this issue cannot be reached yet. The lower limit of 690 Myr (closer to the classical Hyades age of 600-650 Myr) would provide a slope of the initial-final mass relation closer to the global determinations. We also find hints of an intrinsic spread of the cluster initial-final mass relation for the cluster.

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Section: Namementioning

confidence: 86%

Section: Datamentioning

confidence: 99%

Section: Datamentioning

confidence: 99%

“…Moreover, Gaia DR2 data will allow us to determine whether the sample of new Hyades WD candidates discussed in Tremblay et al (2012) contains truly Hyades stars.…”

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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A Gaia DR2 view of white dwarfs in the Hyades

Salaris

Bedin

2018

Monthly Notices of the Royal Astronomical Society

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Progress and Application of The Initial-Final Mass Relation

Cummings

2016

Proc. IAU

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The stellar life cycle is dominated by phases such as the hydrogen-burning stage and the remnant white dwarf cooling phase. However, between these two stages, stars dramatically transform themselves by losing the bulk of their mass. Planetary nebulae (PNe) provide a powerful clue to the processes involved in this transformation, but they are very complex. Over the past 15 years, a new wave of imaging and spectroscopy programs have uncovered the remnants of PNe, white dwarfs, in a wide range of well-measured environments. With this we can map the masses and temperatures of the stellar remnants to the properties of their progenitors. This work has now led to the first uniform mapping of the initial-final mass relation from 1.5 to 7 M⊙. The resulting relation is a fundamental input to our understanding of stellar evolution for low and intermediate-mass stars that produce PNe and has a wide range of applications.

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A 3D view of the Hyades stellar and sub-stellar population

Lodieu

Smart

Pérez‐Garrido

et al. 2019

A&A

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Aims. Our scientific goal is to provide a 3D map of the nearest open cluster to the Sun, the Hyades, combining the recent release of Gaia astrometric data, ground-based parallaxes of sub-stellar member candidates and photometric data from surveys which cover large areas of the cluster. Methods. We combined the second Gaia release with ground-based H-band parallaxes obtained with the infrared camera on the 2-m robotic Liverpool telescope to astrometrically identify stellar and sub-stellar members of the Hyades, the nearest open cluster to the Sun. Results. We find 1764 objects within 70 • radius from the cluster center from the Gaia second data release, whose kinematic properties are consistent with the Hyades. We limit our study to 30 pc from the cluster center (47.03±0.20 pc) where we identify 710 candidate members, including 85 and 385 in the core and tidal radius, respectively. We determine proper motions and parallaxes of eight candidate brown dwarf members and confirm their membership. Using the 3D positions and a model-based mass-luminosity relation we derive a luminosity and mass function in the 0.04 to 2.5 M range. We confirm evidence for mass segregation in the Hyades and find a dearth of brown dwarfs in the core of the cluster. From the white dwarf members we estimate an age of 640 +67 −49 Myr. Conclusions. We identify a list of members in the Hyades cluster from the most massive stars down to the brown dwarfs. We produce for the first time a 3D map of the Hyades cluster in the stellar and sub-stellar regimes and make available the list of candidate members.

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Spectroscopic and photometric studies of white dwarfs in the Hyades

Cited by 20 publications

References 77 publications

A Gaia DR2 view of white dwarfs in the Hyades

A Gaia DR2 view of white dwarfs in the Hyades

Progress and Application of The Initial-Final Mass Relation

A 3D view of the Hyades stellar and sub-stellar population

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