Gaia Data Release 3: Astrophysical parameters inference system (Apsis) I -- methods and content overview

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

doi:10.48550/arxiv.2206.05864

Cited by 40 publications

(51 citation statements)

References 44 publications

(44 reference statements)

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“…Note that the Ca II region slightly changes after the shifting to the heliocentric frame, considering that the radial velocities of most stars lie mainly within ±50 km s −1 , corresponding to |∆λ| 0.14 nm at 866.5 nm. Furthermore, the wings of the Ca II lines are better modeled than their central parts (Creevey et al 2022;Recio-Blanco et al 2022). Thus, our masked region can properly prevent the contamination with the Ca II residuals and consequently the λ864.8 profile can be fitted well.…”

Section: Methodsmentioning

confidence: 87%

“…The Gaia-RVS spectra have a wavelength coverage of [846 − 870] nm and a medium resolution of R ∼ 11 500 (Cropper et al 2018). The stellar parameters and chemical abundances, including effective temperature (T eff ), surface gravity (log g), mean metallicity ([M/H]), and individual abundances of up to 13 chemical species, are derived by the General Stellar Parametrizer from spectroscopy (GSP-Spec) module of the Astrophysical parameters inference system (Apsis, Creevey et al 2022;Recio-Blanco et al 2022). We refer to Recio-Blanco et al (2022) for detailed descriptions of the parametrization and a validation of the measurement of λ862 in individual RVS spectra.…”

Section: Datamentioning

confidence: 99%

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A solid confirmation of the broad DIB around 864.8 nm using stacked Gaia-RVS spectra

Zhao¹,

Schultheis²,

Zwitter³

et al. 2022

Preprint

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Context. Studies on the correlation between different diffuse interstellar bands (DIBs) are important for exploring their origins. However, the Gaia-RVS spectral window between 846 and 870 nm has few DIBs, the strong DIB at 862 nm being the only convincingly confirmed one.Aims. Here we attempt to confirm the existence of a broad DIB around 864.8 nm and estimate its characteristics using the stacked Gaia-RVS spectra of a large number of stars. We study the correlations between the two DIBs at 862 nm (λ862) and 864.8 nm (λ864.8), as well as the interstellar extinction. Methods. We obtain spectra of the interstellar medium (ISM) absorption by subtracting the stellar components using templates constructed from real spectra at high Galactic latitudes with low extinctions. We then stack the ISM spectra in Galactic coordinates ( , b), pixelized by the HEALPix scheme, to measure the DIBs. The stacked spectrum is modeled by the profiles of the two DIBs, Gaussian for λ862 and Lorentzian for λ864.8, and a linear continuum. We report the fitted central depth (CD), central wavelength, equivalent width (EW), and their uncertainties for the two DIBs. Results. We obtain 8458 stacked spectra in total, of which 1103 (13%) have reliable fitting results after applying numerous conservative filters. This work is the first one to fit and measure λ862 and λ864.8 simultaneously in cool-star spectra. Based on these measurements, we find that the EWs and CDs of λ862 and λ864.8 are well-correlated with each other, with Pearson coefficients (r p ) of 0.78 and 0.87, respectively. The full width at half maximum (FWHM) of λ864.8 is estimated as 1.62 ± 0.33 nm which compares to 0.55 ± 0.06 nm for λ862. We also measure the vacuum rest-frame wavelength of λ864.8 to be λ 0 = 864.53 ± 0.14 nm, smaller than previous estimates. Conclusions. We make a solid confirmation of the existence of the DIB around 864.8 nm by exploring its correlation with λ862 and estimating its FWHM. λ864.8 is a very broad and shallow DIB. λ862 correlates better with E(BP − RP) than λ864.8. The profiles of the two DIBs could be strongly overlapped with each other, which contributes to the skew of the λ862 profile.

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Section: Methodsmentioning

confidence: 87%

Section: Datamentioning

confidence: 99%

A solid confirmation of the broad DIB around 864.8 nm using stacked Gaia-RVS spectra

Zhao¹,

Schultheis²,

Zwitter³

et al. 2022

Preprint

Self Cite

View full text Add to dashboard Cite

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“…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

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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.

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“…With the release of Gaia DR3, astrophysical parameters have become available; these are derived from RVS spectra and/or from low-resolution (R ∼ 40) BP/RP prism spectra (Creevey et al 2022). Astrophysical parameters determined from forward-modeling the BP/RP spectra (GSP-Phot, 470 million; Andrae et al 2022) outnumber those obtained from combined RVS spectra of single stars (GSP-Spec, 6 million; Recio-Blanco et al 2022), which come with more precise and detailed information on individual chemical abundances.…”

Section: Gaia Edr3 and Dr3 Datamentioning

confidence: 99%

Dynamical Origin for the Collinder 132–Gulliver 21 Stream: A Mixture of Three Comoving Populations with an Age Difference of 250 Myr

Pang

Tang

et al. 2022

ApJL

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We use Gaia DR3 data to study the Collinder 132–Gulliver 21 region via the machine-learning algorithm StarGO and find eight subgroups of stars (ASCC 32, Collinder 132 gp 1–6, Gulliver 21) located in close proximity. Three comoving populations were identified among these eight subgroups: (i) a coeval 25 Myr old moving group (Collinder 132), (ii) an intermediate-age (50–100 Myr) group, and (iii) the 275 Myr old dissolving cluster Gulliver 21. These three populations form parallel diagonal stripe-shape overdensities in the U–V distribution, which differ from open clusters and stellar groups in the solar neighborhood. We name this kinematic structure the Collinder 132–Gulliver 21 stream, as it extends over 270 pc in the 3D space. The oldest population, Gulliver 21, is spatially surrounded by the Collinder 132 moving group and the intermediate-age group. Stars in the Collinder 132–Gulliver 21 stream have an age difference up to 250 Myr. Metallicity information shows a variation of 0.3 dex between the youngest and oldest populations. The formation of the Collinder 132–Gulliver 21 stream involves both star formation and dynamical heating. The youngest population (Collinder 132 moving group) with homogeneous metallicity is probably formed through filamentary star formation. The intermediate-age and oldest populations were then scattered by the Galactic bar or spiral structure resonance to intercept Collinder 132's orbit. Without mutual interaction between each population, the three populations are flying by each other currently and will become three distinct groups again in ∼50 Myr.

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Gaia Data Release 3: Astrophysical parameters inference system (Apsis) I -- methods and content overview

Cited by 40 publications

References 44 publications

A solid confirmation of the broad DIB around 864.8 nm using stacked Gaia-RVS spectra

A solid confirmation of the broad DIB around 864.8 nm using stacked Gaia-RVS spectra

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

Dynamical Origin for the Collinder 132–Gulliver 21 Stream: A Mixture of Three Comoving Populations with an Age Difference of 250 Myr

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