<i>Gaia</i>Data Release 3

Babusiaux, C.; Fabricius, C.; Khanna, Shourya; Muraveva, T.; Reylé, C.; Spoto, F.; Vallenari, A.

doi:10.1051/0004-6361/202243790

Cited by 109 publications

(43 citation statements)

References 79 publications

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“…The median simulated grvs_mag starts to deviate from the true magnitude and become systematically brighter (by about 0.015 mag) at G true RVS = 13.4, reaching an offset of ∼ 0.14 mag at G true RVS =14.0. A similar magnitude term is reported in Babusiaux et al (2022).…”

Section: Underestimate Of Grvs_mag At Faint Magnitudessupporting

confidence: 81%

“…1, the primary product of the RVS pipeline is the radial_velocity, and all filters applied to nullify spurious radial velocity measurements were applied to all pipeline products, including grvs_mag. The radial_velocity filter criteria are listed in the online documentation (Sartoretti et al 2022, section 6.5.2.1) and described in detail in Katz et al (2022) and Babusiaux et al (2022). Most radial_velocity filters were beneficial also for grvs_mag, leading to the removal of many spurious grvs_mag measurements contaminated by nearby relatively bright sources located also outside the contamination area considered in the pipeline (Sect.…”

Section: Validation Filtering Of Grvs_magmentioning

confidence: 99%

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GaiaData Release 3

Sartoretti¹,

Marchal²,

Babusiaux³

et al. 2023

A&A

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Context. Gaia Data Release 3 (DR3) contains the first release of magnitudes estimated from the integration of Radial Velocity Spectrometer (RVS) spectra for a sample of about 32.2 million stars brighter than G RVS ∼ 14 mag (or G ∼ 15 mag). Aims. In this paper, we describe the data used and the approach adopted to derive and validate the G RVS magnitudes published in DR3. We also provide estimates of the G RVS passband and associated G RVS zero-point. Methods. We derived G RVS photometry from the integration of RVS spectra over the wavelength range from 846 to 870 nm. We processed these spectra following a procedure similar to that used for DR2, but incorporating several improvements that allow a better estimation of G RVS . These improvements pertain to the stray-light background estimation, the line spread function calibration, and the detection of spectra contaminated by nearby relatively bright sources. We calibrated the G RVS zero-point every 30 hours based on the reference magnitudes of constant stars from the Hipparcos catalogue, and used them to transform the integrated flux of the cleaned and calibrated spectra into epoch magnitudes. The G RVS magnitude of a star published in DR3 is the median of the epoch magnitudes for that star. We estimated the G RVS passband by comparing the RVS spectra of 108 bright stars with their flux-calibrated spectra from external spectrophotometric libraries.Results. The G RVS magnitude provides information that is complementary to that obtained from the G, G BP , and G RP magnitudes, which is useful for constraining stellar metallicity and interstellar extinction. The median precision of G RVS measurements ranges from about 0.006 mag for the brighter stars (i.e. with 3.5 ∼ < G RVS ∼ < 6.5 mag) to 0.125 mag at the faint end. The derived G RVS passband shows that the effective transmittance of the RVS is approximately 1.23 times better than the pre-launch estimate.

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Section: Underestimate Of Grvs_mag At Faint Magnitudessupporting

confidence: 81%

Section: Validation Filtering Of Grvs_magmentioning

confidence: 99%

GaiaData Release 3

Sartoretti¹,

Marchal²,

Babusiaux³

et al. 2023

A&A

Self Cite

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“…( − ∆ )/ σ 2 parallax + σ 2 sys ≥ 5, where σ parallax is parallax_error, and σ sys is the systematic uncertainty on the zero-point, which we take to be 0.015 mas (Lindegren et al 2021). Furthermore, we select stars with RUWE < 1.4 and σ(V los ) < 20 km/s, after applying the correction to radial_velocity_error recommended by Babusiaux, C. et al (2022). We also follow these authors and remove 3 stars with (G RVS − G) < −3.…”

Section: Datamentioning

confidence: 99%

The Gaia DR3 view of dynamical substructure in the stellar halo near the Sun

Dodd¹,

Callingham²,

Helmi³

et al. 2022

Preprint

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Context. The debris from past merger events is expected and, to some extent, known to populate the stellar halo near the Sun. Aims. We aim to identify and characterise such merger debris using Gaia DR3 data supplemented by metallicity and chemical abundance information from LAMOST LRS and APOGEE for halo stars within 2.5 kpc from the Sun. Methods. We utilise a single linkage-based clustering algorithm to identify over-densities in Integrals of Motion space that could be due to merger debris. Combined with metallicity information and chemical abundances, we characterise these statistically significant over-densities. Results. We find that the local stellar halo contains 8 main dynamical groups, some of in-situ and some of accreted origin, most of which are already known. We report the discovery of a new substructure, which we name ED-1. In addition, we find evidence for 9 independent smaller clumps, 4 of which are new: ED-2, 3, 4 and 5 are typically rather tight dynamically, depict a small range of metallicities, and their abundances when available, as well as their location in Integrals of Motion space suggest an accreted origin. Conclusions. The local halo contains an important amount of substructure, of both in-situ and accreted origin.

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“…In the selection process, we removed events located towards and close to the Galactic Bulge, within 20 deg in Galactic longitude. Despite having the highest sky-density of events, the Gaia astrometric data in that part of the sky are likely to suffer from multiple errors, often unaccounted for in the Gaia data processing, caused by crowding and source confusion (Gaia Collaboration 2021; Babusiaux et al 2022;Lindegren et al 2021).…”

Section: Selectionmentioning

confidence: 99%

A possible nearby microlensing stellar remnant hiding in Gaia DR3 astrometry

Jabłońska

Wyrzykowski

Rybicki

et al. 2022

A&A

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Massive galactic lenses with large Einstein Radii should cause a measurable astrometric microlensing effect, that is, a light centroid shift due to the motion of the two images. Such a shift in the position of a background star due to microlensing was not included in the Gaia astrometric model, and therefore significant deviation should cause Gaia’s astrometric parameters to be determined incorrectly. Here we study one of the photometric microlensing events reported in the Gaia Data Release 3, GaiaDR3-ULENS-001, for which a poor goodness of Gaia fit and erroneous parallax could indicate the presence of an astrometric microlensing signal. Based on the photometric microlensing model, we simulated Gaia astrometric time series with the astrometric microlensing effect added. We find that including microlensing with an angular Einstein radius of θE = 2.60−0.24+0.21 mas (2.47−0.24+0.28 mas) assuming a positive (negative) impact parameter, u0, reproduces the astrometric quantities reported by Gaia well. We estimate the mass of the lens to be 1.00−0.18+0.23 M⊙ (0.70−0.13+0.17 M⊙) and its distance 0.90−0.11+0.14 kpc (0.69−0.09+0.13 kpc), proposing the lens could be a nearby isolated white dwarf.

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GaiaData Release 3

Cited by 109 publications

References 79 publications

GaiaData Release 3

GaiaData Release 3

The Gaia DR3 view of dynamical substructure in the stellar halo near the Sun

A possible nearby microlensing stellar remnant hiding in Gaia DR3 astrometry

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