<i>Gaia</i>Data Release 3

Fouesneau, M.; Frémat, Y.; Andrae, R.; Korn, A. J.; Soubiran, C.; Kordopatis, G.; Vallenari, A.; Heiter, U.; Creevey, O.; Sarro, L. M.; Laverny, P. de; Lanzafame, A. C.; Lobel, A.; Sordo, R.; Rybizki, J.; Slezak, I.; Álvarez, M. A.; Drimmel, R.; Garabato, D.

doi:10.1051/0004-6361/202243919

Cited by 76 publications

(34 citation statements)

References 121 publications

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“…Validation of these values indicates a systematic offset on the order of 0.3 with respect to external catalogues for main sequence stars; see e.g. Creevey et al (2022); Fouesneau et al (2022); Recio-Blanco & et al (2022). We therefore removed log g when log g > 4.0 in order to retain a 'gold' status, and kept all of the other parameters.…”

Section: Filtering Of Flame Gsp-spec and Esp-hs Parameters In Samples...mentioning

confidence: 87%

“…Creevey et al (2022) present an overview of the processing, the architecture, and the modules of Apsis, along with a summary of the data products. Fouesneau et al (2022) focus on the stellar content, its description, and quality assessments, and Delchambre et al (2022) detail the non-stellar content, in particular object classification, extinction, and extragalactic objects.…”

Section: Data Descriptionmentioning

confidence: 99%

“…misclassified cool objects, white dwarfs, etc.) are included when the astrometry is less reliable (Fouesneau et al 2022). To exclude a significant fraction of these, we removed all targets based on the signal-tonoise ratio (S/N) of the parallax parallax_over_error ≤ 15, as illustrated in Fig.…”

Section: Sample Selectionmentioning

confidence: 99%

“…We retained sources whose parameters are within the FGKM regime: T eff < 7500 K, M G < 12, R < 100 R , and had a log posterior > −4000 (goodness-of-fit indicator). We also retained sources with [M/H] > -0.8 which excludes lowmetallicity sources with unreliable metallicities (Andrae et al 2022;Creevey et al 2022;Fouesneau et al 2022).…”

Section: Gsp-phot Sample Selectionmentioning

confidence: 99%

“…Gaia DR3 contains a wealth of new data products. In particular, it provides us with stellar parameters derived from the analysis of the Gaia RVS spectra (Sartoretti et al 2018), the low-resolution spectra produced by the Blue Photometer (BP) and the Red Photometer (RP) (Carrasco et al 2021;De Angeli et al 2022), astrometry (Lindegren et al 2021c), and integrated photometry (Riello et al 2021a) for up to 470 million stars (Andrae et al 2022;Creevey et al 2022;Fouesneau et al 2022;Lanzafame et al 2022;Recio-Blanco & et al 2022). As expected, the accuracy and precision of these parameters with brightness, distance, stellar type and the number of observations.…”

Section: Introductionmentioning

confidence: 99%

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GaiaData Release 3

Creevey¹,

Sarro²,

Lobel³

et al. 2023

A&A

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Context. Gaia Data Release 3 (DR3) provides a wealth of new data products for the astronomical community to exploit, including astrophysical parameters for half a billion stars. In this work, we demonstrate the high quality of these data products and illustrate their use in different astrophysical contexts. Aims. We produce homogeneous samples of stars with high-quality astrophysical parameters by exploiting Gaia DR3, while focusing on many regimes across the Hertzsprung-Russell (HR) diagram; spectral types OBA, FGKM, and ultracool dwarfs (UCDs). We also focus on specific subsamples of particular interest to the community: solar analogues, carbon stars, and the Gaia spectrophotometric standard stars (SPSS). Methods. We query the astrophysical parameter tables along with other tables in Gaia DR3 to derive the samples of the stars of interest. We validate our results using the Gaia catalogue itself and by comparison with external data. Results. We produced six homogeneous samples of stars with high-quality astrophysical parameters across the HR diagram for the community to exploit. We first focus on three samples that span a large parameter space: young massive disc stars (OBA; about 3 Million ), FGKM spectral type stars (about 3 Million), and UCDs (about 20 000). We provide these sources along with additional information (either a flag or complementary parameters) as tables that are made available in the Gaia archive. We also identify 15 740 bone fide carbon stars and 5 863 solar analogues, and provide the first homogeneous set of stellar parameters of the SPSS sample. We demonstrate some applications of these samples in different astrophysical contexts. We use a subset of the OBA sample to illustrate its usefulness in analysing the Milky Way rotation curve. We then use the properties of the FGKM stars to analyse known exoplanet systems. We also analyse the ages of some unseen UCD-companions to the FGKM stars. We additionally predict the colours of the Sun in various passbands (Gaia, 2MASS, WISE) using the solar-analogue sample. Conclusions. Gaia DR3 contains a wealth of new high-quality astrophysical parameters for the community to exploit.

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Section: Filtering Of Flame Gsp-spec and Esp-hs Parameters In Samples...mentioning

confidence: 87%

Section: Data Descriptionmentioning

confidence: 99%

Section: Sample Selectionmentioning

confidence: 99%

Section: Gsp-phot Sample Selectionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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GaiaData Release 3

Creevey¹,

Sarro²,

Lobel³

et al. 2023

A&A

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Stellar occultations by trans-Neptunian objects

Sicardy,

Braga-Ribas,

Buie

et al. 2024

Astron Astrophys Rev

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The PL diagram for δ Sct stars: back in business as distance estimators

Garca Hernández,

Pascual-Granado,

Lares-Martiz

et al. 2022

Proc. IAU

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In this work, we focus on the period-luminosity relation (PLR) of δ Sct stars, in which mode excitation and selection mechanisms are still poorly constrained, and whose structure and oscillations are affected by rotation. We review the PLRs in the recent literature, and add a new inference from a large sample of δ Sct. We highlight the difficulty in identifying the fundamental mode and show that rotation-induced surface effects can impact the measured luminosities, explaining the broadening of the PLR. We derive a tight relation between the low-order large separation and the fundamental radial mode frequency (F0) that holds for rotating stars, thus paving the way towards mode identification. We show that the PLRs we obtain for different samples are compatible with each other and with the recent literature, and with most observed δ Sct stars when taking rotation effects into account. We also find that the highest-amplitude peak in the frequency spectrum corresponds to the fundamental modein most δ Sct, thus shedding some light on their elusive mode selection mechanism.

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GaiaData Release 3

Cited by 76 publications

References 121 publications

GaiaData Release 3

GaiaData Release 3

Stellar occultations by trans-Neptunian objects

The PL diagram for δ Sct stars: back in business as distance estimators

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