The Radial Velocity Experiment (Rave): Fifth Data Release

Kunder, Andrea; Kordopatis, G.; Steinmetz, Matthias; Zwitter, T.; McMillan, Paul J.; Casagrande, Luca; Enke, H.; Wojno, Jennifer; Valentini, M.; Chiappini, Cristina; Matijevič, G.; Siviero, A.; Laverny, P. de; Recio–Blanco, A.; Bijaoui, A.; Wyse, Rosemary F. Ġ.; Binney, James; Grebel, Eva K.; Helmi, Amina; Jofré, P.; Antoja, T.; Gilmore, G.; Siebert, A.; Famaey, Benoît; Bienaymé, O.; Gibson, Brad K.; Freeman, K. C.; Navarro, Julio F.; Munari, U.; Seabroke, G. M.; Anguiano, Borja; Žerjal, M.; Minchev, Ivan; Reid, Warren A.; Bland-Hawthorn, Joss; Kos, Janez; Sharma, Sanjib; Watson, Fred; Parker, Quentin A.; Scholz, R.‐D.; Burton, D.; Cass, Paul; Hartley, M.; Fiegert, Kristin; Stupar, M.; Ritter, Andreas; Hawkins, Keith; Gerhard, Ortwin; Chaplin, W. J.; Davies, G. R.; Elsworth, Y.; Lund, Mikkel N.; Miglio, A.; Mosser, B.

doi:10.3847/1538-3881/153/2/75

Cited by 460 publications

(432 citation statements)

References 107 publications

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“…Numerous direct analyses of such surveys (GCS (Nordström et al 2004), RAVE (Kordopatis et al 2013;Kunder et al 2017), APOGEE (Eisenstein et al 2011), Gaia-ESO (Randich et al 2013), among the largest ones) are giving outstanding contributions to theses studies, thanks to the large statistics that are possible with several hundred thousands of measurements homogeneous on the sky, in opposition to earlier studies that worked with samples of a few hundred stars at most.…”

Section: Introductionmentioning

confidence: 91%

“…The difference in gravity is not negligible, but we do not use it in the present study. The definition of our subsamples for the analysis of the observed proper motions and radial velocities is based on cuts in I magnitudes (the same magnitudes in DR4 and DR5), a cut in temperature at 5300 K, and cuts in metallicity [M/H] Kunder et al (2017). Hence, using the DR5 instead would not have introduced systematic changes in the content of our subsamples.…”

Section: Sample Selectionmentioning

confidence: 99%

“…DR5 data are improved thanks to a recalibration of the temperature, gravity, and metallicity. Figures 4-6 (Kunder et al 2017) allow us to compare the mean DR5 versus DR4 values. The difference in gravity is not negligible, but we do not use it in the present study.…”

Section: Sample Selectionmentioning

confidence: 99%

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Kinematics of the local disk from the RAVE survey and the Gaia first data release

Robin

Bienaymé

Fernández-Trincado

et al. 2017

A&A

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Aims. We attempt to constrain the kinematics of the thin and thick disks using the Besançon population synthesis model together with RAVE DR4 and Gaia first data release (TGAS). Methods. The RAVE fields were simulated by applying a detailed target selection function and the kinematics was computed using velocity ellipsoids depending on age in order to study the secular evolution. We accounted for the asymmetric drift computed from fitting a Stäckel potential to orbits. Model parameters such as velocity dispersions, mean motions, and velocity gradients were adjusted using an ABC-MCMC method. We made use of the metallicity to enhance the separation between thin and thick disks. Results. We show that this model is able to reproduce the kinematics of the local disks in great detail. The disk follows the expected secular evolution, in very good agreement with previous studies of the thin disk. The new asymmetric drift formula, fitted to our previously described Stäckel potential, fairly well reproduces the velocity distribution in a wide solar neighborhood. The U and W components of the solar motion determined with this method agree well with previous studies. However, we find a smaller V component than previously thought, essentially because we include the variation of the asymmetric drift with distance to the plane. The thick disk is represented by a long period of formation (at least 2 Gyr), during which, as we show, the mean velocity increases with time while the scale height and scale length decrease, very consistently with a collapse phase with conservation of angular momentum.Conclusions. This new Galactic dynamical model is able to reproduce the observed velocities in a wide solar neighborhood at the quality level of the TGAS-RAVE sample, allowing us to constrain the thin and thick disk dynamical evolution, as well as determining the solar motion.

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Section: Introductionmentioning

confidence: 91%

Section: Sample Selectionmentioning

confidence: 99%

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Kinematics of the local disk from the RAVE survey and the Gaia first data release

Robin

Bienaymé

Fernández-Trincado

et al. 2017

A&A

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“…fitting the Ca II triplet at ∼8,500Å, fitting the Na I doublet at ∼5,800Å or applying the cross-correlation function (see Section 5). Whilst both the cross-correlation function and the Ca II triplet fitting technique have been proven to yield precise radial velocities -see Queloz (1995) and Kunder et al (2017), respectively -the Na I doublet profile at ∼5,800 may be affected by interstellar absorption (Welsh et al 2010). In order to explore possible effects of the interstellar absorption on the measurement of Na I radial velocities, we compare in Figure 3 the Ca II absorption triplet and the Na I absorption doublet radial velocities measured from 45 LAMOST high signal-to-noise ratio spectra (>300) 4 and 24 CFHT spectra of unique objects.…”

Section: Identification Of Close Wd+fgk Binariesmentioning

confidence: 99%

The white dwarf binary pathways survey – II. Radial velocities of 1453 FGK stars with white dwarf companions from LAMOST DR 4

Rebassa‐Mansergas¹,

Ren²,

Irawati³

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We present the second paper of a series of publications aiming at obtaining a better understanding regarding the nature of type Ia supernovae (SN Ia) progenitors by studying a large sample of detached F, G and K main sequence stars in close orbits with white dwarf companions (i.e. WD+FGK binaries). We employ the LAMOST (Large Sky Area Multi-Object Fibre Spectroscopic Telescope) data release 4 spectroscopic data base together with GALEX (Galaxy Evolution Explorer) ultraviolet fluxes to identify 1,549 WD+FGK binary candidates (1,057 of which are new), thus doubling the number of known sources. We measure the radial velocities of 1,453 of these binaries from the available LAMOST spectra and/or from spectra obtained by us at a wide variety of different telescopes around the globe. The analysis of the radial velocity data allows us to identify 24 systems displaying more than 3σ radial velocity variation that we classify as close binaries. We also discuss the fraction of close binaries among WD+FGK systems, which we find to be ∼10 per cent, and demonstrate that high-resolution spectroscopy is required to efficiently identify double-degenerate SN Ia progenitor candidates.

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“…References and (where used) CDS catalogue numbers for the RV catalogues: (1) Kunder et al (2017); (2) velocity (and takes into account their covariances, which can be very large). The orbit for every surrogate is integrated through the Galactic potential and the perihelia found.…”

Section: Procedures For Finding Close Encountersmentioning

confidence: 99%

The completeness-corrected rate of stellar encounters with the Sun from the first Gaia data release

Bailer‐Jones¹

2017

A&A

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I report on close encounters of stars to the Sun found in the first Gaia data release (GDR1). Combining Gaia astrometry with radial velocities of around 320 000 stars drawn from various catalogues, I integrate orbits in a Galactic potential to identify those stars which pass within a few parsecs. Such encounters could influence the solar system, for example through gravitational perturbations of the Oort cloud. 16 stars are found to come within 2 pc (although a few of these have dubious data). This is fewer than were found in a similar study based on Hipparcos data, even though the present study has many more candidates. This is partly because I reject stars with large radial velocity uncertainties (>10 km s −1 ), and partly because of missing stars in GDR1 (especially at the bright end). The closest encounter found is Gl 710, a K dwarf long-known to come close to the Sun in about 1.3 Myr. The Gaia astrometry predict a much closer passage than pre-Gaia estimates, however: just 16 000 AU (90% confidence interval: 10 000-21 000 AU), which will bring this star well within the Oort cloud. Using a simple model for the spatial, velocity, and luminosity distributions of stars, together with an approximation of the observational selection function, I model the incompleteness of this Gaia-based search as a function of the time and distance of closest approach. Applying this to a subset of the observed encounters (excluding duplicates and stars with implausibly large velocities), I estimate the rate of stellar encounters within 5 pc averaged over the past and future 5 Myr to be 545 ± 59 Myr −1 . Assuming a quadratic scaling of the rate within some encounter distance (which my model predicts), this corresponds to 87 ± 9 Myr −1 within 2 pc. A more accurate analysis and assessment will be possible with future Gaia data releases.

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The Radial Velocity Experiment (Rave): Fifth Data Release

Cited by 460 publications

References 107 publications

Kinematics of the local disk from the RAVE survey and the Gaia first data release

Kinematics of the local disk from the RAVE survey and the Gaia first data release

The white dwarf binary pathways survey – II. Radial velocities of 1453 FGK stars with white dwarf companions from LAMOST DR 4

The completeness-corrected rate of stellar encounters with the Sun from the first Gaia data release

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