Gaia Data Release 3: Apsis II -- Stellar Parameters

Fouesneau, M.; Frémat, Y.; Andrae, R.; Korn, A. J.; Soubiran, C.; Kordopatis, G.; Vallenari, A.; Heiter, U.; Creevey, O. L.; Sarro, L. M.; Laverny, P. de; Lanzafame, A. C.; Lobel, A.; Sordo, R.; Rybizki, J.; Slezak, I.; Álvarez, M. A.; Drimmel, R.; Garabato, D.; Delchambre, L.; Bailer-Jones, C. A. L.; Hatzidimitriou, D.; Lorca, A.; Fustec, Y. Le; Pailler, F.; Mary, N.; Robin, C.; Utrilla, E.; Aramburu, A. Abreu; Bakker, J.; Bellas-Velidis, I.; Bijaoui, A.; Blomme, R.; Bouret, J. -C.; Brouillet, N.; Brugaletta, E.; Burlacu, A.; Carballo, R.; Casamiquela, L.; Chaoul, L.; Chiavassa, A.; Contursi, G.; Cooper, W. J.; Dafonte, C.; Demouchy, C.; Dharmawardena, T. E.; García-Lario, P.; García-Torres, M.; Gomez, A.; González-Santamaría, I.; Piccolo, A. Jean-Antoine; Kontizas, M.; Lebreton, Y.; Licata, E. L.; Lindstrøm, H. E. P.; Livanou, E.; Romeo, A. Magdaleno; Manteiga, M.; Marocco, F.; Martayan, C.; Marshall, D. J.; Nicolas, C.; Ordenovic, C.; Palicio, P. A.; Pallas-Quintela, L.; Pichon, B.; Poggio, E.; Recio-Blanco, A.; Riclet, F.; Santoveña, R.; Schultheis, M.; Segol, M.; Silvelo, A.; Smart, R. L.; Süveges, M.; Thévenin, F.; Elipe, G. Torralba; Ulla, A.; Dillen, E. van; Zhao, H.; Zorec, J.

doi:10.48550/arxiv.2206.05992

Cited by 30 publications

(39 citation statements)

References 69 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The goal of the present paper is to describe the production and content of the CU8 data products available in the Gaia DR3 archive. More details on the validation and use of the stellar and non-stellar products can be found in the accompanying papers II (Fouesneau et al 2022) and III (Delchambre et al 2022), respectively. More complete descriptions of specific products and methods can be found in the following papers: Delchambre (2018), Andrae et al (2022), Lanzafame et al (2022) and Recio-Blanco et al (2022), and the official online documentation 1 .…”

Section: Introductionmentioning

confidence: 99%

GaiaData Release 3

Creevey¹,

Sordo²,

Pailler³

2023

A&A

Self Cite

112

View full text Add to dashboard Cite

Gaia Data Release 3 contains a wealth of new data products for the community. Astrophysical parameters are a major component of this release, and were produced by the Astrophysical parameters inference system (Apsis) within the Gaia Data Processing and Analysis Consortium (DPAC). The aim of this paper is to describe the overall content of the astrophysical parameters in Gaia DR3 and how they were produced. In Apsis, we use the mean BP/RP and mean RVS spectra along with astrometry and photometry, and we derive the following parameters: source classification and probabilities for 1.6 billion objects; interstellar medium characterisation and distances for up to 470 million sources, including a 2D total Galactic extinction map; 6 million redshifts of quasar candidates; 1.4 million redshifts of galaxy candidates; and an analysis of 50 million outlier sources through an unsupervised classification. The astrophysical parameters also include many stellar spectroscopic and evolutionary parameters for up to 470 million sources. These comprise T eff , log g, and [M/H] (470 million using BP/RP, 6 million using RVS), radius (470 million), mass (140 million), age (120 million), chemical abundances (up to 5 million), diffuse interstellar band analysis (0.5 million), activity indices (2 million), Hα equivalent widths (200 million), and further classification of spectral types (220 million) and emission-line stars (50 000). This paper is the first in a series of three papers, and focusses on describing the global content of the parameters in Gaia DR3. The accompanying papers II and III focus on the validation and use of the stellar and non-stellar products, respectively. This catalogue is the most extensive homogeneous database of astrophysical parameters to date, and is based uniquely on Gaia data. It will only be superseded by Gaia Data Release 4, and will therefore remain a key reference over the next four years, providing astrophysical parameters independent of other ground-and space-based data.

show abstract

Section: Introductionmentioning

confidence: 99%

GaiaData Release 3

Creevey¹,

Sordo²,

Pailler³

2023

A&A

Self Cite

112

View full text Add to dashboard Cite

show abstract

“…16), using integrated photometry in the G, G BP , and G RP bands (Riello et al 2021). For more than half the sample, extinction parameters are available from the Apsis pipeline (Creevey et al 2022;Fouesneau et al 2022;Andrae et al 2022). The absorption in the G band, A G , and the G BP − G RP colour excess, E(G BP − G RP ), are taken from ESP-HS (Creevey et al 2022) for hot stars (T eff > 7500 K, ag_esphs, ebpminrp_esphs) and from GSP-Phot for cooler ones (ag_gspphot, ebpminrp_gspphot).…”

Section: Discussionmentioning

confidence: 99%

“…It is published in Gaia DR3 as vsini_esphs (in the astrophysical_parameters table) and is an intermediate result of the analysis of the RVS and BP/RP data when the astrophysical parameters of stars with T eff > 7500 K are derived. A discussion of vsini_esphs and a comparison with the vbroad measurements described in the present paper is given in the online documentation (Section 11.4.4, Korn et al 2022) and in Fouesneau et al (2022). In this work, we provide more information about the line-broadening parameter for the Gaia DR3 catalogue user as it is derived from the spectra obtained by the Gaia Radial Velocity Spectrometer (RVS) and derived by the spectroscopic pipeline.…”

Section: Introductionmentioning

confidence: 99%

GaiaData Release 3

Frémat¹,

Royer²,

Marchal³

et al. 2023

A&A

View full text Add to dashboard Cite

Context. The third release of the Gaia catalogue contains radial velocities for 33 812 183 stars with effective temperatures ranging from 3100 K to 14 500 K. The measurements are based on the comparison of the spectra observed with the Radial Velocity Spectrometer (RVS; wavelength coverage: 846–870 nm, median resolving power: 11 500) to synthetic data broadened to the adequate along-scan line spread function. The additional line-broadening, fitted as it would only be due to axial rotation, is also produced by the pipeline and is available in the catalogue (field name vbroad). Aims. We describe the properties of the line-broadening information extracted from the RVS and published in the catalogue, and analyse the limitations imposed by the adopted method, wavelength range, and instrument. Methods. We used simulations to express the link between the line-broadening measurement provided in Gaia Data Release 3 and V sin i. We then compared the observed values to the measurements published by various catalogues and surveys (GALAH, APOGEE, LAMOST, etc.). Results. While we recommend caution in the interpretation of the vbroad measurement, we also find a reasonable general agreement of the Gaia Data Release 3 line-broadening values and values in other catalogues. We discuss and establish the validity domain of the published vbroad values. The estimate tends to be overestimated at the lower V sin i end, and at Teff > 7500 K its quality and significance degrade rapidly when GRVS > 10. Despite all the known and reported limitations, the Gaia Data Release 3 line-broadening catalogue contains measurements obtained for 3 524 677 stars with Teff ranging from 3500 to 14 500 K, and GRVS < 12. It gathers the largest stellar sample ever considered for the purpose, and allows a first mapping of the Gaia line-broadening parameter across the Hertzsprung-Russel diagram.

show abstract

“…Nevertheless, the large luminosities of giant stars can hide even potentially massive, non-degenerate companions (El-Badry et al 2022b). We therefore select for only dwarf stars by first removing any stars with a log g < 3.6 (if the stars have a log g measured by Apsis, the Gaia team's astrophysical parameters inference system; Creevey et al 2022;Fouesneau et al 2022) and second making a cut in the color-magnitude diagram:…”

Section: Sample Selectionmentioning

confidence: 99%

A Sample of Neutron Star and Black Hole Binaries Detected through Gaia DR3 Astrometry

Andrews¹,

Taggart²,

Foley³

2022

Preprint

View full text Add to dashboard Cite

With its exquisite astrometric precision, the latest Gaia data release includes ∼10 5 astrometric binaries, each of which have measured orbital periods, eccentricities, and the Thiele-Innes orbital parameters. Using these and an estimate of the luminous stars' masses, we derive the companion stars' masses, from which we identify a sample of 24 binaries in long period orbits (P orb ∼ yrs) with a high probability of hosting a massive (>1.4 M ), dark companion: a neutron star (NS) or black hole (BH). The luminous stars in these binaries tend to be F-, G-, and K-dwarfs with the notable exception of one hot subdwarf. Follow-up spectroscopy of eight of these stars shows no evidence for contamination by white dwarfs or other luminous stars. The dark companions in these binaries span a mass range of 1.35-2.7 M and therefore likely includes both NSs and BHs without a significant mass gap in between. Furthermore, the masses of several of these objects are 1.7 M , similar to the mass of at least one of the merging compact objects in GW190425. Given that these orbits are too wide for significant mass accretion to have occurred, this sample implies that some NSs are born heavy ( 1.5 M ). Additionally, the low orbital velocities ( 20 km s −1 ) of these binaries requires that at least some heavy NSs receive low natal kicks, otherwise they would have been disrupted during core collapse. Although none will become gravitational wave sources within a Hubble time, these systems will be exceptionally useful for testing binary evolution theory.

show abstract

Gaia Data Release 3: Apsis II -- Stellar Parameters

Cited by 30 publications

References 69 publications

GaiaData Release 3

GaiaData Release 3

GaiaData Release 3

A Sample of Neutron Star and Black Hole Binaries Detected through Gaia DR3 Astrometry

Contact Info

Product

Resources

About