A<i>Gaia</i>Data Release 2 catalogue of white dwarfs and a comparison with SDSS

Fusillo, N. P. Gentile; Tremblay, Pier-Emmanuel; Gänsicke, B. T.; Manser, Christopher J.; Cunningham, Tim; Cukanovaite, E.; Hollands, Mark; Marsh, T. R.; Raddi, R.; Jordan, S.; Toonen, Silvia; Geier, S.; Barstow, M. A.; Cummings, Jeffrey D.

doi:10.1093/mnras/sty3016

Cited by 392 publications

(313 citation statements)

References 150 publications

(208 reference statements)

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“…The blue BP-RP color indicates that it is white dwarf companion. This is further confirmed by the analysis of Gentile Fusillo et al [70]. Therefore, this star is a new Sirius-like system.…”

Section: Id Plx (Mas) Rho ( ) Ecc a (Au) A Crit (Au) Msupporting

confidence: 61%

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Frequency of Planets in Binaries

Bonavita

Desidera

2020

Galaxies

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The frequency of planets in binaries is an important issue in the field of extrasolar planet studies because of its relevance in the estimation of the global planet population of our galaxy and the clues it can give to our understanding of planet formation and evolution. Multiple stars have often been excluded from exoplanet searches, especially those performed using the radial velocity technique, due to the technical challenges posed by such targets. As a consequence and despite recent efforts, our knowledge of the frequency of planets in multiple stellar systems is still rather incomplete. On the other hand, the lack of knowledge about the binarity at the time of the compilation of the target samples means that our estimate of the planet frequency around single stars could be tainted by the presence of unknown binaries, especially if these objects have a different behavior in terms of planet occurrence. In a previous work we investigated the binarity of the objects included in the Uniform Detectability sample defined by Fisher and Valenti (2005), showing how more than 20% of their targets were, in fact, not single stars. Here, we present an update of this census, made possible mainly by the information now available thanks to the second Gaia Data Release. The new binary sample includes a total of 313 systems, of which 114 were added through this work. We were also able to significantly improve the estimates of masses and orbital parameters for most of the pairs in the original list, especially those at close separations. A few new systems with white dwarf companions were also identified. The results of the new analysis are in good agreement with the findings of our previous work, confirming the lack of difference in the overall planet frequency between binaries and single stars but suggesting a decrease in the planet frequency for very close pairs. Galaxies 2020, 8, 16 G (1) Mass(J) = 3.95501 − 2.87761 * M J + 1.58846 * M 2 J − 0.568685 * M 3 J + 0.125674 * M 4 J −0.0169899 * M 5 J + 0.00136157 * M 6 J − 5.91812e − 05 * M 7 J + 1.07257e − 06 * M 8 J (2) Mass(K)

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“…The blue BP-RP color indicates that it is white dwarf companion. This is further confirmed by the analysis of Gentile Fusillo et al [70]. Therefore, this star is a new Sirius-like system.…”

Section: Id Plx (Mas) Rho ( ) Ecc a (Au) A Crit (Au) Msupporting

confidence: 61%

“…HD 139323: The secondary (HD 139341) is a close visual and spectroscopic binary. HD 140901: The companion is a WD [70]. HD 145825: New binary from the RV orbital solution [38], with mass in the stellar regime.…”

Section: Id Plx (Mas) Rho ( ) Ecc a (Au) A Crit (Au) Mmentioning

confidence: 99%

Frequency of Planets in Binaries

Bonavita

Desidera

2020

Galaxies

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“…Besides their high magnetic fields, most of them have been shown to be massive, and responsible for the high-mass peak at 1 M of the WD mass distribution; for instance: REJ 0317-853 has M ≈ 1.35 M and B ≈ (1.7-6.6) × 10 8 G ( Barstow et al 1995;Külebi et al 2010); PG 1658+441 has M ≈ 1.31 M and B ≈ 2.3 × 10 6 G (Liebert et al 1983;Schmidt et al 1992); and PG 1031+234 has the highest magnetic field B ≈ 10 9 G (Schmidt et al 1986;Külebi et al 2009). The existence of ultra-massive WDs has been revealed in several studies (see e.g., Castanheira et al 2013;Hermes et al 2013;Curd et al 2017;Camisassa et al 2019;Gentile Fusillo et al 2018;Jiménez-Esteban et al 2018).…”

Section: Introductionmentioning

confidence: 99%

Gravitational waves from fast-spinning white dwarfs

Sousa

Coelho

2020

Monthly Notices of the Royal Astronomical Society

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Two mechanisms of gravitational waves (GWs) emission in fast-spinning white dwarfs (WDs) are investigated: accretion of matter and magnetic deformation. In both cases, the GW emission is generated by an asymmetry around the rotation axis of the star. However, in the first case, the asymmetry is due to the amount of accreted matter on the magnetic poles, while in the second case it is due to the intense magnetic field. We have estimated the GW amplitude and luminosity for three binary systems that have a fast-spinning magnetized WD, namely, AE Aquarii, AR Scorpii and RX J0648.0-4418. We find that, for the first mechanism, the systems AE Aquarii and RX J0648.0-4418 can be observed by the space detectors BBO and DECIGO if they have an amount of accreted mass of δm ≥ 10 −5 M . For the second mechanism, the three systems studied require that the WD have a magnetic field above ∼ 10 9 G to emit GWs that can be detected by BBO. We also verified that, in both mechanisms, the gravitational luminosity has an irrelevant contribution to the spindown luminosity of these three systems. Therefore, other mechanisms of energy emission are needed to explain the spindown of these objects.

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“…We follow Bergeron et al (1997) to perform our SED analysis (also see Gentile Fusillo et al 2019). We first construct the SED of the white dwarf using photometry from Gaia DR2, PS1, and the UKIDSS Hemisphere Survey (Table 1), and convert magnitudes into fluxes using zero-point fluxes from Evans et al (2018), Tonry et al (2012), and Lawrence et al (2007), respectively.…”

Section: The White Dwarf Primarymentioning

confidence: 99%

COol Companions ON Ultrawide orbiTS (COCONUTS). I. A High-gravity T4 Benchmark around an Old White Dwarf and a Re-examination of the Surface-gravity Dependence of the L/T Transition

Zhang

Liu

Hermes

et al. 2020

ApJ

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We present the first discovery from the COol Companions ON Ultrawide orbiTS (COCONUTS) program, a large-scale survey for wide-orbit planetary and substellar companions. We have discovered a co-moving system COCONUTS-1, composed of a hydrogen-dominated white dwarf (PSO J058.9855 + 45.4184; d = 31.5 pc) and a T4 companion (PSO J058.9869 + 45.4296) at a 40.6 (1280 au) projected separation. We derive physical properties for COCONUTS-1B from (1) its near-infrared spectrum using cloudless Sonora atmospheric models, and (2) its luminosity and the white dwarf's age (7.3 +2.8 −1.6 Gyr) using Sonora evolutionary models. The two methods give consistent temperatures and radii, but atmospheric models infer a lower surface gravity and therefore an unphysically young age. Assuming evolutionary model parameters (T eff = 1255 +6 −8 K, log g = 5.44 +0.02 −0.03 dex, R = 0.789 +0.011 −0.005 R Jup ), we find cloudless model atmospheres have brighter Y -and J-band fluxes than the data, suggesting condensate clouds have not fully dispersed around 1300 K. The W2 flux (4.6 µm) of COCONUTS-1B is fainter than models, suggesting non-equilibrium mixing of CO. To investigate the gravity dependence of the L/T transition, we compile all 60 known L6−T6 benchmarks and derive a homogeneous set of temperatures, surface gravities, and masses. As is wellknown, young, low-gravity late-L dwarfs have significantly fainter, redder near-infrared photometry and ≈ 200 − 300 K cooler temperatures than old, high-gravity objects. Our sample now reveals such gravity dependence becomes weaker for T dwarfs, with young objects having comparable near-infrared photometry and ≈ 100 K cooler temperatures compared to old objects. Finally, we find that young objects have a larger amplitude J-band brightening than old objects, and also brighten at H band as they cross the L/T transition.

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AGaiaData Release 2 catalogue of white dwarfs and a comparison with SDSS

Abstract: Please refer to published version for the most recent bibliographic citation information. If a published version is known of, the repository item page linked to above, will contain details on accessing it.

Cited by 392 publications

References 150 publications

Frequency of Planets in Binaries

Frequency of Planets in Binaries

Gravitational waves from fast-spinning white dwarfs

COol Companions ON Ultrawide orbiTS (COCONUTS). I. A High-gravity T4 Benchmark around an Old White Dwarf and a Re-examination of the Surface-gravity Dependence of the L/T Transition

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