Gaia Data Release 3 Properties and validation of the radial velocities

Katz, David; Sartoretti, Paola; Cropper, Mark; Panuzzo, P.; Seabroke, G. M.; Viala, Y.; Benson, K.; Blomme, R.; Jasniewicz, G.; Jean-Antoine, A.; Huckle, H. E.; Smith, M.; Baker, S. G.; Crifo, F.; Damerdji, Y.; David, M.; Dolding, C.; Frémat, Y.; Gosset, Éric; Guerrier, A.; Guy, L. P.; Haigron, R.; Janßen, K.; Marchal, Olivier; Plum, G.; Soubiran, C.; Thévenin, F.; Ajaj, M.; Prieto, C. Allende; Babusiaux, C.; Boudreault, S.; Chemin, L.; Luche, C. Delle; Fabre, C.; Gueguen, A.; Hambly, N. C.; Lasne, Y.; Meynadier, Frédéric; Pailler, F.; Panem, C.; Royer, F.; Tauran, G.; Zurbach, C.; Zwitter, T.; Arenou, Frédéric; Bossini, D.; Gómez, A.; Lemaı̂tre, V.; Leclerc, Nicolas; Morel, Thierry; Munari, U.; Turon, C.; Vallenari, A.; Žerjal, M.

doi:10.48550/arxiv.2206.05902

Cited by 62 publications

(89 citation statements)

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“…For fainter stars (12 < 𝐺 RVS 14), radial velocities are instead the combinations of the epoch cross-correlation functions. The quoted radial velocity errors reflect the adopted method (Zucker 2003;Katz et al 2022).…”

Section: Introductionmentioning

confidence: 67%

“…The exquisite quality of the data produced by the European Space Agency (ESA) satellite Gaia is revolutionizing our knowledge of the Milky Way, allowing us to resolve and characterize its stellar populations to an unprecedented level of detail (Gaia Collaboration et al 2016). The third data release (DR3), out on June 13th, 2022 (Gaia Collaboration et al 2022a;Babusiaux et al 2022), provides a massive amount of new information, including (but not limited to) ∼ 220 million low-resolution spectra (De Angeli et al 2022;Montegriffo et al 2022), astrophysical parameters for ∼ 470 million stars (Creevey et al 2022), ∼ 34 million radial velocities (Katz et al 2022), and catalogues for 10 million variable stars (Eyer et al 2022) and ∼ 800 000 binaries (Damerdji et al 2022;Holl et al 2022;Siopis et al 2022). The Gaia DR3 catalogue spans 34 months of observations, and, combined with the astrometry already provided by the early third Gaia data release (EDR3, Gaia Collaboration et al 2021) for ∼ 1.5 billion stars 1 , is the largest stellar dataset ever ★ E-mail:tommaso.marchetti@eso.org 1 Since Gaia EDR3 astrometry and photometry are part of Gaia DR3 (they share the same list of sources), in this work we will always refer to Gaia DR3 when discussing these quantities.…”

Section: Introductionmentioning

confidence: 99%

“…Gaia DR3 radial velocities are obtained by the Radial Velocity Spectrometer (RVS) (Katz et al 2022;Blomme et al 2022), which takes spectra spanning a range of wavelengths between 847 nm and 874 nm near the Ca triplet (Cropper et al 2018). Gaia DR3 radial velocities are determined using two different methods depending on 𝐺 RVS , the apparent magnitude of a star in the RVS band (Sartoretti et al 2022).…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Gaia DR3 in 6D: The search for fast hypervelocity stars and constraints on the Galactic Centre environment

Marchetti,

Evans,

Rossi

2022

Preprint

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The third data release (DR3) of the European Space Agency satellite Gaia provides coordinates, parallaxes, proper motions, and radial velocities for a sample of ∼ 34 million stars. We use the combined 6-dimensional phase space information to search for hypervelocity stars (HVSs), unbound stars accelerated by dynamical processes happening in the Galactic Centre. By looking at the kinematics of Gaia DR3 stars in Galactocentric coordinates and by integrating their orbits in the Galactic potential, we do not identify any HVS candidates with a velocity higher than 700 km s −1 and robustly observed kinematics. Assuming a scenario wherein the interaction between a stellar binary and the massive black hole Sgr A * is responsible for HVS ejections from the Galactic Centre, we derive degenerate limits on the ejection rate of HVSs and the slope of the initial mass function of the primary star among binaries in the Galactic Centre. Our results indicate that the HVS ejection rate is 8 × 10 −5 yr −1 assuming a Salpeter mass function, and this upper limit becomes progressively smaller for an increasingly topheavy mass distribution. A fiducial HVS ejection rate of 10 −4 yr −1 prefers a mass function slope −2.35, disfavouring previously claimed top-heavy initial mass functions among stars in the Galactic Centre.

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Section: Introductionmentioning

confidence: 67%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Gaia DR3 in 6D: The search for fast hypervelocity stars and constraints on the Galactic Centre environment

Marchetti,

Evans,

Rossi

2022

Preprint

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“…• The pair is separated by at least 5 arcsec, to minimize the effects of blending on the RVs (Katz et al 2022). The median projected physical separation of the sample is 6,000 AU, corresponding to a typical orbital RV difference of order 0.5 km s −1 (with no preferred sign).…”

Section: Methodsmentioning

confidence: 99%

The Gravitational Redshift of Solar-type Stars from Gaia DR3 Wide Binaries

El-Badry¹

2022

Res. Notes AAS

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Light escaping from a gravitational potential suffers a redshift with magnitude proportional to the depth of the potential. This “gravitational redshift” is easily measurable in dense stars such as white dwarfs, but is much weaker and has evaded unambiguous detection in main-sequence stars. I show that the effect is directly measurable in the Gaia DR3 radial velocities (RVs) of the components of wide binary stars. In a sample of ∼500 wide binaries containing a solar-type main-sequence star and a red giant or red clump companion, the apparent RV of the giant is on average 0.49 ± 0.02 km s−1 lower than that of the main-sequence star. This owes primarily to the giants’ weaker gravitational fields and is in reasonably good agreement with the value expected from general relativity.

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“…Among other data products, it includes 186,905 orbital solutions for spectroscopic binaries, representing more than an order of magnitude increase in sample size over all previous studies. These solutions are obtained by fitting multi-epoch spectra from the Radial Veloc-★ E-mail: kareem.el-badry@cfa.harvard.edu ity Spectrometer (RVS) instrument (Cropper et al 2018;Katz et al 2022), which covers the wavelength range of 846-870 nm with spectral resolution 𝑅 ≈ 11, 500 and ≈ 20 epochs for typical binaries. Both single-lined ("SB1") and double-lined ("SB2") solutions are included in DR3 (Gaia Collaboration et al 2022a).…”

Section: Introductionmentioning

confidence: 99%

What are the spectroscopic binaries with high mass functions near the Gaia DR3 main sequence?

El-Badry,

Rix

2022

Preprint

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The 3rd data release of the Gaia mission includes orbital solutions for > 10 5 single-lined spectroscopic binaries, representing more than an order of magnitude increase in sample size over all previous studies. This dataset is a treasure trove for searches for quiescent black hole + normal star binaries. We investigate one population of black hole candidate binaries highlighted in the data release: sources near the main sequence in the color-magnitude diagram (CMD) with dynamically-inferred companion masses 𝑀 2 larger than the CMD-inferred mass of the luminous star. We model light curves, spectral energy distributions, and archival spectra of the 14 such objects in DR3 with high-significance orbital solutions and inferred 𝑀 2 > 3 𝑀 . We find that 100% of these sources are mass-transfer binaries containing a highly stripped lower giant donor (0.2 𝑀/𝑀 0.4) and much more massive (2 𝑀/𝑀 2.5) main-sequence accretor. The Gaia orbital solutions are for the donors, which contribute about half the light in the Gaia RVS bandpass but only 20% in the 𝑔−band. The accretors' broad spectral features likely prevented the sources from being classified as double-lined. The donors are all close to Roche lobe-filling (𝑅/𝑅 Roche lobe > 0.8), but modeling suggests that a majority are detached (𝑅/𝑅 Roche lobe < 1). Binary evolution models predict that these systems will soon become detached helium white dwarf + main sequence "EL CVn" binaries. Our investigation highlights both the power of Gaia data for selecting interesting sub-populations of binaries and the ways in which binary evolution can bamboozle standard CMD-based stellar mass estimates.

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Gaia Data Release 3 Properties and validation of the radial velocities

Cited by 62 publications

References 1 publication

Gaia DR3 in 6D: The search for fast hypervelocity stars and constraints on the Galactic Centre environment

Gaia DR3 in 6D: The search for fast hypervelocity stars and constraints on the Galactic Centre environment

The Gravitational Redshift of Solar-type Stars from Gaia DR3 Wide Binaries

What are the spectroscopic binaries with high mass functions near the Gaia DR3 main sequence?

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