white dwarfs in the gaia era - sciencesconf.org · non-relativistic relativistic mass (mʘ) (r ʘ)...
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White dwarfs in the Gaia era
Pier-Emmanuel TremblayNicola Gentile Fusillo (Warwick), Stefan Jordan (Heidelberg), Boris Gänsicke (Warwick)
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1 MWD ~ 1 Mʘ
log g = 7-9Teff = 3000 – 100 000 K
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Probing the history of the Milky Way
Present day population
Constant formation for 10 Gyr
1.5 Mʘ 2.5 Mʘ 5 Mʘ
0.6 Mʘ WDs 0.7 Mʘ WDs 1.0 Mʘ WDs
WDs provide
• Calibration of the mass loss in stellar evolution (Casewell et al. 2009, Kalirai et al. 2014)
• Precise star formation history and IMF for the disk, halo, and clusters of the Milky Way(Tremblay et al. 2014)
• History and fate of planetary systems (metal pollution, Zuckerman et al. 2007)
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non-relativistic
relativistic
Mass (Mʘ)
Rad
ius
(Rʘ)
Gaia parallaxand coloursgives Teff and R
White dwarf Mass-Radius relation
mass-radiusrelation
total agewith evolutionmodels
Spectroscopic follow-ups for more precision, subtypes, and internal check of models
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White dwarfs in Gaia DR1 (Tremblay et al. 2017)
• Only 6 white dwarfs directly observed• 46 in wide binaries, 32 in unresolved binaries (S. Joyce talk)• Gaia parallaxes and G-band magnitudes agree with WD models at the 0.5% level!• There are a few outliers! (e.g. 2 new suspected double degenerates)
distance modulus from spectroscopic parameters and Gaia G-band
Pure-hydrogen Gaia DR1 WDs in wide binarieswith high S/N optical spectroscopy
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Gaia DR2 white dwarf populationAbout 300000 WDs / ~10-25 white dwarfs per deg2
+20◦
-20◦
per
deg
2
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300000 white dwarfs Gaia DR2predicted HR diagram with Gaia errors
White dwarfs: Tremblay et al. simulation (this conference)
GUMSl=180° b=45°
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final DR will improve by ~ √2
100 pc sample (10 000 white dwarfs)
WDs in Gaia DR2parallax accuracy
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Stellar parameters from Gaia only data(parallax, G, GP, RP)
does not include double white dwarfs!
WDs in Gaia DR2stellar parameters
1) All 300 000 WDs
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Stellar parameters from Gaia only data(parallax, G, GP, RP)
does not include double white dwarfs!
WDs in Gaia DR2stellar parameters
2) 100 pc sampleσπ/π < 0.01(same number of WDs on plot)
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Agecluster
Weideman 1980, Kalirai et al. 2009, Williams et al. 2009, Dobbie et al. 2012
Initial-final mass relation
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Input SFH (20 pc sample; Tremblay et al. 2014) Gaia 40 pc (1000 white dwarfs) – G, Bp, Rp only
> 12 Gyr
Galactic archeology with white dwarfs 1) Gaia parameters only
Minimum we can do (direct method)
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Input SFH (Tremblay et al. 2014) Gaia 40 pc – S/N > 30 spectro
Galactic archeology with white dwarfs 2) Gaia + follow-up spectroscopy
> 12 Gyr
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• Up to 3x105 new white dwarfs
• Spectroscopic follow-ups necessary for precise stellar parameters
• medium-resolution (380-520 nm) -> relatively small cost to include WDs!
• White dwarfs are excellent flux / telluric calibrators
Outcomes
• Stellar formation history in the disk / initial mass function
• Ages in wide binaries, clusters / mass loss in AGB
• 6D phase-space: up to 3000 halo white dwarfs, streams
• Chemical abundances: Galactic evolution of planetary systems
Long term: halo stellar formation history with Euclid+LSST
Conclusion: White dwarfs in Gaia/WEAVE/4MOST