The open-cluster initial--final mass relationship and the high-mass tail of the white dwarf distribution

Ferrario, Lilia; Wickramasinghe, D. T.; Liebert, James; Williams, Kurtis A.

doi:10.1111/j.1365-2966.2005.09244.x

Cited by 121 publications

(245 citation statements)

References 27 publications

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“…The cluster data for NGC 3532 are from Koester & Reimers (1993), although we have used the latest results of Koester & Reimers (1996) and those reported in Ferrario et al (2005). According to Ferrario et al (2005) the age of this cluster is 300±150, and the metallicity is [Fe/H]= −0.022 (Twarog et al 1997) or [Fe/H]= −0.02 (Chen et al 2003), so we have used the tracks corresponding to Z = 0.019.…”

Section: Other Available Datamentioning

confidence: 99%

“…According to Ferrario et al (2005) the age of this cluster is 300±150, and the metallicity is [Fe/H]= −0.022 (Twarog et al 1997) or [Fe/H]= −0.02 (Chen et al 2003), so we have used the tracks corresponding to Z = 0.019. We have also included the data for the three white dwarfs reported in Reimers & Koester (1989), although the resolution is lower.…”

Section: Other Available Datamentioning

confidence: 99%

“…For white dwarfs LAWDS2 and LAWDS27 we have used the atmospheric parameters reported in Ferrario et al (2005) corresponding to new data. As can be seen in Table 4.4, the white dwarfs of this cluster are more massive than those of M37.…”

Section: Ngc2168 (M35)mentioning

confidence: 99%

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Testing the Initial–Final Mass Relationship of White Dwarfs

Catalán

Isern

Garcı́a–Berro

et al. 2010

Astrophysics and Space Science Proceedings

113

184

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A mis padres y hermana AgraïmentsEn primer lloc vull agrair als meus directors de tesi, Jordi Isern i Enrique García-Berro, que em donessin l'oportunitat de realitzar el doctorat a l'IEEC (al CSIC i a la UPC), així com que em proporcionessin tot el suport necessari. Crec que he après moltes coses importants en aquestsúltims anys, no només en la part científica, i això en partés una conseqüència d'haver treballat amb ells. Els vull donar les gràcies també pel suport i la confiança dipositada en mi, especialment durant aquestúltim any de feina.Durant tota aquestaèpoca he tingut la sort de tenir uns companys fantàstics que m'han fet molt més fàcil la feina. Primer vaig conèixer l'Alina, la meva companya de "fatigas" i després el Jose, el Pep i el Miquel. Més tard s'hi van afegir l'Ignasi, la Violeta, l'Anna C., l'Anna A., el Carlo, el Moi, el Nil, l'Anaïs. . . Tots els moments que hem compartit dins i fora de l'IEEC han estat molt importants per a mi i m'emporto un gran record de tota aquestaèpoca, primer al Nexus, després a la UAB i finalment a l'ETSE. Ara que tinc la oportunitat, els hi vull agrair als meus companys, o més ben dit, amics, tots elsànims i suport que m'han donat. També els hi vull donar les gràcies al personal d'administració i a la resta de companys que he tingut durant aquests anys.En especial, l'Ignasi es mereix un gran gràcies. . . Primer de tot, per venir a l'IEEC en un moment en que la meva feina necessitava d'un observador amb experiència. Per tenir la generositat de compartir els seus coneixements amb mi durant aquests anys, per acompanyar-me en les observacions, per tenir sempre tanta confiança en mi, molta més que jo mateixa i per ajudar-me sempre que se li presentés la oportunitat. Els seusànims i el seu suport han estat essencials per a que arribés aquest moment i per tant, només em queda donar-li el meu agraïment més sincer.También le debo un agradecimiento especial a Carlos Allende Prieto, que sin ni siquiera conocerme en persona aceptó acompañarme a observar al McDonald Observatory durante 10 días. Su ayuda y dedicación en la distancia, especialmente en el análisis de las compañeras de las enanas blancas, han sido también vitales para el desarrollo de esta tesis.Durante mi doctorado he tenido la oportunidad de disfrutar de estancias en otros centros. Le quiero dar las gracias a Inma Domínguez, Carlos Abia y Olga Zamora de la Universidad de Granada por la atención que me dispensaron cuando estuve allí. También quisiera dar las gracias a Roberto Silvotti y Juan Alcalá por la ayuda y el buen trato que me dieron durante el tiempo que pasé en el Osservatorio Astronomico di Capodimonte. Gracias también al resto de personas que trabajan en el Osservatorio y que hicieron mi estancia muy agradable.A mi profesor Manolo Segura le quiero agredecer que en su día me hiciera creer en mis posibilidades y despertara mi afán por intentar superarme poco a poco. Muchas gracias también por la "contingencia" y por la confianza dipositada en mí.En un momento para mí tan importante comoéste no me puedo olvi...

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Section: Other Available Datamentioning

confidence: 99%

Section: Other Available Datamentioning

confidence: 99%

See 1 more Smart Citation

Testing the Initial–Final Mass Relationship of White Dwarfs

Catalán

Isern

Garcı́a–Berro

et al. 2010

Astrophysics and Space Science Proceedings

113

184

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“…This yielded a value of M MS = 3.8 ± 0.5 M . Alternatively, we used the IFMR determined by Ferrario et al (2005) based on white dwarfs observed in open clusters (see in particular their Fig. 1).…”

Section: The Optical Spectrum Of Hip 96515 B: Observations and Modelingmentioning

confidence: 99%

The triple system HIP 96515: a low-mass eclipsing binary with a DB white dwarf companion

Huélamo¹,

Vaz

Torres

et al. 2009

A&A

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Context. HIP 96515 A is a double-lined spectroscopic binary included in the SACY catalog as a potential young star. It has a visual companion (CCDM 19371-5134 B, HIP 96515 B) at 8. 6. If bound to the primary, the optical and infrared colors of this wide companion are consistent with those of a white dwarf. Aims. We attempt to characterize the system HIP 96515 A&B by studying each of its components. Methods. We analyzed spectroscopic and photometric observations of HIP 96515 A and its visual companion, HIP 96515 B. To confirm the system as a common proper-motion pair, we analyzed the astrometry of the components using high-angular resolution infrared observations obtained within a time span of two years, and archival astrometry. Results. The high-resolution optical spectrum of HIP 96515 A was used to derive a mass ratio, M 2 /M 1 , close to 0.9. The optical lightcurve of HIP 96515 A shows periodic variations with P orbital = 2.3456 days, revealing that HIP 96515 A is an eclipsing binary with preliminary orbital parameters of i = 89.• 0 ± 0.• 2, and M 1 = 0.59 ± 0.03 M and M 2 = 0.54 ± 0.03 M , for the primary and secondary, respectively, at an estimated distance of 42 ± 3 pc. This is a new eclipsing binary with component masses below 0.6 M . Multi-epoch observations of HIP 96515 A&B show that the system is a common proper-motion pair. The optical spectrum of HIP 96515 B is consistent with a pure helium atmosphere (DB) white dwarf. The comparison with evolutionary cooling sequence models provides T eff,WD = 19 126 ± 195 K, log g WD = 8.08, M WD /M = 0.6, and a distance of ∼46 pc. The estimated WD cooling age is ∼100 Myr and the total age of the object (including the main-sequence phase) is ∼400 Myr. Finally, if HIP 96515 A&B are coeval, and assuming a common age of ∼400 Myr, the comparison of the masses of the eclipsing binary members with evolutionary tracks shows that they are underestimated by ∼15% and 10%, for the primary and secondary, respectively.

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“…assessment of cluster's age and metallicity, amount of convective overshooting, thickness of the white dwarf H/He layers, The IFMR of Single CO White Dwarfs 37 Figure 1. Semi-empirical IFMR based on the compilation by Ferrario et al (2005), Kalirai et al (2008), andCatalán et al (2008). Solid lines are linear fits provided by various authors quoted in the plot.…”

Section: Introductionmentioning

confidence: 99%

Asymptotic Giant Branch Evolution and the Initial-Final Mass Relation of Single CO White Dwarfs

Marigo¹

2011

Proc. IAU

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Abstract. Combining recent mass determinations of Galactic CO white dwarfs and their progenitors with the latest evolutionary models for Asymptotic Giant Branch (AGB) stars, I review the initial-final mass relation (IFMR) of low-and intermediate-mass stars. In particular, I analyze the impact on the IFMR produced by a few critical processes characterizing the AGB phase, namely: the second and third dredge-up events, hot-bottom burning, and mass loss. Their dependence on metallicity and related theoretical uncertainties are briefly discussed.

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The open-cluster initial--final mass relationship and the high-mass tail of the white dwarf distribution

Cited by 121 publications

References 27 publications

Testing the Initial–Final Mass Relationship of White Dwarfs

Testing the Initial–Final Mass Relationship of White Dwarfs

The triple system HIP 96515: a low-mass eclipsing binary with a DB white dwarf companion

Asymptotic Giant Branch Evolution and the Initial-Final Mass Relation of Single CO White Dwarfs

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