A search for white dwarfs in the Galactic plane: the field and the open cluster population

Raddi, R.; Catalán, S.; Gänsicke, B. T.; Hermes, J. J.; Napiwotzki, R.; Koester, D.; Tremblay, Pier-Emmanuel; Barentsen, Geert; Farnhill, H. J.; Mohr-Smith, M.; Drew, J. E.; Groot, P.; Guzmán-Ramírez, L.; Parker, Quentin A.; Steeghs, D.; Zijlstra, A. A.

doi:10.1093/mnras/stw042

Cited by 20 publications

(14 citation statements)

References 97 publications

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“…We note that observations of ultra-massive 20 white dwarfs are particularly difficult due to their relative scarcity, inherently low luminosity due to more compact nature, as well as more rapid cooling (Althaus et al, 2007). Recent works by Cummings et al (2016a,b) and Raddi et al (2016) have derived semi-empirical initial-final mass relations for ultramassive WDs using observations from young open clusters. However, the procedure to derive an initial-final mass relation is quite involved and is affected by quite a range of uncertainties.…”

Section: Low Mass Channelmentioning

confidence: 94%

Super-AGB Stars and their Role as Electron Capture Supernova Progenitors

Doherty

Gil‐Pons

Siess

et al. 2017

Publ. Astron. Soc. Aust.

161

193

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We review the lives, deaths and nucleosynthetic signatures of intermediate-mass stars in the range ≈6-12 M , which form super-AGB stars near the end of their lives. The critical mass boundaries both between different types of massive white dwarfs (CO, CO-Ne, ONe), and between white dwarfs and supernovae, are examined along with the relative fraction of super-AGB stars that end life either as an ONe white dwarf or as a neutron star (or an ONeFe white dwarf), after undergoing an electron capture supernova event. The contribution of the other potential single-star channel to electroncapture supernovae, that of the failed massive stars, is also discussed. The factors that influence these different final fates and mass limits, such as composition, rotation, the efficiency of convection, the nuclear reaction rates, mass-loss rates, and third dredge-up efficiency, are described. We stress the importance of the binary evolution channels for producing electron-capture supernovae. Recent nucleosynthesis calculations and elemental yield results are discussed and a new set of s-process heavy element yields is presented. The contribution of super-AGB star nucleosynthesis is assessed within a Galactic perspective, and the (super-)AGB scenario is considered in the context of the multiple stellar populations seen in globular clusters. A brief summary of recent works on dust production is included. Last, we conclude with a discussion of the observational constraints and potential future advances for study into these stars on the low mass/high mass star boundary.

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Section: Low Mass Channelmentioning

confidence: 94%

Super-AGB Stars and their Role as Electron Capture Supernova Progenitors

Doherty

Gil‐Pons

Siess

et al. 2017

Publ. Astron. Soc. Aust.

161

193

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“…Reimers & Koester (1989) discovered seven white dwarf candidates on photographic plates of which three could be verified spectroscopically (Koester & Reimers 1993). More recently Dobbie et al (2009Dobbie et al ( , 2012 have confirmed further white dwarfs and Raddi et al (2016) have discovered an additional candidate. Having seven confirmed white dwarf members makes NGC 3532 a rich source for degenerate objects among Galactic open clusters (Dobbie et al 2012), further testifying to its value for studies of stellar evolution.…”

Section: Introductionmentioning

confidence: 95%

Spectroscopic membership for the populous 300 Myr-old open cluster NGC 3532

Fritzewski

Barnes

James

et al. 2019

A&A

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Context. NGC 3532 is an extremely rich open cluster embedded in the Galactic disc, hitherto lacking a comprehensive, documented membership list. Aims. We provide membership probabilities from new radial velocity observations of solar-type and low-mass stars in NGC 3532, in part as a prelude to a subsequent study of stellar rotation in the cluster. Methods. Using extant optical and infra-red photometry we constructed a preliminary photometric membership catalogue, consisting of 2230 dwarf and turn-off stars. We selected 1060 of these for observation with the AAOmega spectrograph at the 3.9 m-Anglo-Australian Telescope and 391 stars for observations with the Hydra-South spectrograph at the 4 m Victor Blanco Telescope, obtaining spectroscopic observations over a decade for 145 stars. We measured radial velocities for our targets through cross-correlation with model spectra and standard stars, and supplemented them with radial velocities for 433 additional stars from the literature. We also measured log g, T eff , and [Fe/H] from the AAOmega spectra. Results. The radial velocity distribution emerging from the observations is centred at 5.43 ± 0.04 km s −1 and has a width (standard deviation) of 1.46 km s −1 . Together with proper motions from Gaia DR2 we find 660 exclusive members, of which five are likely binary members. The members are distributed across the whole cluster sequence, from giant stars to M dwarfs, making NGC 3532 one of the richest Galactic open clusters known to date, on par with the Pleiades. From further spectroscopic analysis of 153 dwarf members we find the metallicity to be marginally sub-solar, with [Fe/H] = −0.07 ± 0.10. We confirm the extremely low reddening of the cluster, E B−V = 0.034 ± 0.012 mag, despite its location near the Galactic plane. Exploiting trigonometric parallax measurements from Gaia DR2 we find a distance of 484 +35 −30 pc [(m − M) 0 = 8.42 ± 0.14 mag]. Based on the membership we provide an empirical cluster sequence in multiple photometric passbands. A comparison of the photometry of the measured cluster members with several recent model isochrones enables us to confirm the 300 Myr cluster age. However, all of the models evince departures from the cluster sequence in particular regions, especially in the lower mass range.

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“…Within the past 10 years, the increasing availability of both widefield imagers and spectrographs on large telescopes has led to a significantly increased number of known white dwarfs in star clusters. This includes the work of Kalirai et al (2005Kalirai et al ( , 2008Kalirai et al ( , 2009), Williams et al (2009), Casewell et al (2009, Dobbie et al (2009Dobbie et al ( , 2012, Cummings et al (2015Cummings et al ( , 2016aCummings et al ( , 2016b hereafter Papers I, II, and III, respectively), and Raddi et al (2016).…”

Section: Introductionmentioning

confidence: 99%

The White Dwarf Initial–Final Mass Relation for Progenitor Stars from 0.85 to 7.5 M _⊙

Cummings

Kalirai

Tremblay

et al. 2018

ApJ

Self Cite

314

369

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We present the initial-final mass relation (IFMR) based on the self-consistent analysis of Sirius B and 79 white dwarfs from 13 star clusters. We have also acquired additional signal on eight white dwarfs previously analyzed in the NGC 2099 cluster field, four of which are consistent with membership. These reobserved white dwarfs have masses ranging from 0.72 to 0.97 M ⊙ , with initial masses from 3.0 to 3.65 M ⊙ , where the IFMR has an important change in slope that these new data help to observationally confirm. In total, this directly measured IFMR has small scatter (σ = 0.06 M ⊙ ) and spans from progenitors of 0.85 to 7.5 M ⊙ . Applying two different stellar evolutionary models to infer two different sets of white dwarf progenitor masses shows that when the same model is also used to derive the cluster ages, the resulting IFMR has weak sensitivity to the adopted model at all but the highest initial masses (>5.5 M ⊙ ). The non-linearity of the IFMR is also clearly observed with moderate slopes at lower masses (0.08 M final /M initial ) and higher masses (0.11 M final /M initial ) that are broken up by a steep slope (0.19 M final /M initial ) between progenitors from 2.85 to 3.6 M ⊙ . This IFMR shows total stellar mass loss ranges from 33% of M initial at 0.83 M ⊙ to 83% of M initial at 7.5 M ⊙ . Testing this total mass loss for dependence on progenitor metallicity, however, finds no detectable sensitivity across the moderate range of -0.15 < [Fe/H] < +0.15.

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A search for white dwarfs in the Galactic plane: the field and the open cluster population

Cited by 20 publications

References 97 publications

Super-AGB Stars and their Role as Electron Capture Supernova Progenitors

Super-AGB Stars and their Role as Electron Capture Supernova Progenitors

Spectroscopic membership for the populous 300 Myr-old open cluster NGC 3532

The White Dwarf Initial–Final Mass Relation for Progenitor Stars from 0.85 to 7.5 M _⊙

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A search for white dwarfs in the Galactic plane: the field and the open cluster population

Cited by 20 publications

References 97 publications

Super-AGB Stars and their Role as Electron Capture Supernova Progenitors

Super-AGB Stars and their Role as Electron Capture Supernova Progenitors

Spectroscopic membership for the populous 300 Myr-old open cluster NGC 3532

The White Dwarf Initial–Final Mass Relation for Progenitor Stars from 0.85 to 7.5 M ⊙

Contact Info

Product

Resources

About

The White Dwarf Initial–Final Mass Relation for Progenitor Stars from 0.85 to 7.5 M _⊙