Stellar ages, masses, extinctions and orbital parameters based on spectroscopic parameters of Gaia DR3

Kordopatis, G.; Schultheis, M.; McMillan, P. J.; Palicio, P. A.; Laverny, P. de; Recio-Blanco, A.; Creevey, O.; Álvarez, M. A.; Andrae, R.; Poggio, E.; Spitoni, E.; Contursi, G.; Zhao, H.; Oreshina-Slezak, I.; Ordenovic, C.; Bijaoui, A.

doi:10.48550/arxiv.2206.07937

Cited by 3 publications

(3 citation statements)

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“…To select the candidate low-mass objects for spectroscopic follow up, we use the photometric and astrometric data from Gaia DR3 (Gaia Collaboration et al 2016;Gaia Collaboration 2022). We extract the Gaia DR3 data for our survey area (∼21′ × 21′) and for those sources in our WIRCam data with counterparts in Gaia DR3 we apply the following astrometric quality conditions: (1) renormalized unit weight error (RUWE) < 1.4 -sources with higher values can possibly have unreliable astrometric solutions (Fabricius et al 2021;Manara et al 2021;Kordopatis et al 2022;Stoop et al 2022) and (2) σ π /π <0.1, where π is the parallax and σ π is the uncertainty in the parallax (Esplin & Luhman 2022;Penoyre et al 2022). We then selected for follow-up spectroscopy 11sources lying along the PMS branch in the Gaia G -J versus absolute Gaia G CMD.…”

Section: Member Selection Using Gaia Dr3mentioning

confidence: 99%

A Novel Survey for Young Substellar Objects with the W-band Filter. VI. Spectroscopic Census of Substellar Members and the IMF of the σ Orionis Cluster

Damian

Jose

Biller

et al. 2023

ApJ

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Low-mass stars and substellar objects are essential in tracing the initial mass function (IMF). We study the nearby young σ Orionis cluster (d ∼ 408 pc, age ∼ 1.8 Myr) using deep near-infrared (NIR) photometric data in the J, W, and H bands from WIRCam on the Canada–France–Hawaii Telescope. We use the water absorption feature to select brown dwarfs photometrically and confirm their nature spectroscopically with IRTF-SpeX. Additionally we select candidate low-mass stars for spectroscopy and analyze their membership and those of literature sources using astrometry from Gaia DR3. We obtain NIR spectra for 28 very-low-mass stars and brown dwarfs and estimate their spectral type between M3 and M8.5 (masses ranging between 0.3 and 0.01 M ⊙). Apart from these, we also identify five new planetary-mass candidates which require further spectroscopic confirmation of youth. We compile a comprehensive catalog of 170 spectroscopically confirmed members in the central region of the cluster, for a wide mass range of ∼19–0.004 M ☉. We estimate the star-to-brown-dwarf ratio to be ∼4, within the range reported for other nearby star-forming regions. With the updated catalog of members we trace the IMF down to 4 M Jup and we find that a two-segment power law fits the substellar IMF better than a log-normal distribution.

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Section: Member Selection Using Gaia Dr3mentioning

confidence: 99%

A Novel Survey for Young Substellar Objects with the W-band Filter. VI. Spectroscopic Census of Substellar Members and the IMF of the σ Orionis Cluster

Damian

Jose

Biller

et al. 2023

ApJ

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“…In order to propagate the errors, we considered the correlations between the astrometric parameters. Motivated by the approach of Gaia Collaboration (2022b) and Kordopatis et al (2022), we modelled the distribution of the errors of the geometric distances with a broken Gaussian distribution parameterised by the input confidence intervals (i.e. r lo and r hi in Bailer-Jones et al 2021).…”

Section: Gaia Data and Selection Criteriamentioning

confidence: 99%

Spiral-like features in the disc revealed by Gaia DR3 radial actions

Palicio

Recio–Blanco

Poggio

et al. 2023

A&A

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Context. The so-called action variables are specific functions of the positions and velocities that remain constant along the stellar orbit. The astrometry provided by Gaia Early Data Release 3 (EDR3), combined with the velocities inferred from the Radial Velocity Spectrograph (RVS) spectra of Gaia DR3, allows for the estimation of these actions for the largest volume of stars to date. Aims. We explore such actions with the aim of locating structures in the Galactic disc. Methods. We computed the actions and the orbital parameters of the Gaia DR3 stars, assuming an axisymmetric model for the Milky Way. Using Gaia DR3 photometric data, we also selected a subset of giant stars with better astrometry as a control sample. Results. We find that the maps of the percentiles of the radial action JR reveal arc-like segments. We found a high JR region centered at R ≈ 10.5 kpc of 1 kpc width, as well as three arc-shape regions dominated by circular orbits at inner radii. We also identified the spiral arms in the overdensities of the giant population. Conclusions. For Galactic coordinates (X, Y, Z), we find good agreement with the literature in the innermost region for the Scutum-Sagittarius spiral arms. At larger radii, the low JR structure tracks the Local arm at negative X, while for the Perseus arm, the agreement is restricted to the X < 2 kpc region, with a displacement with respect to the literature at more negative longitudes. We detected a high JR area at a Galactocentric radii of ∼10.5 kpc, consistent with some estimations of the Outer Lindblad Resonance location. We conclude that the pattern in the dynamics of the old stars is consistent in several places with the spatial distribution of the spiral arms traced by young populations, with small potential contributions from the moving groups.

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“…More recently, Gaia DR3 data present the latest general stellar information, including around 1.5 billion sources with full astrometric solution (e.g., Gaia Collaboration et al 2021;Gaia Collaboration et al 2023a;Kordopatis et al 2022), and it helps us to better hunt and/or reidentify possible OCs. In this study, we revisit 77 special OC candidates with multiple main sequences (MSs) using Gaia DR3 from LISC catalog.…”

Section: Introductionmentioning

confidence: 99%

Revisit of 77 Clusters Candidates with Multiple Main Sequences using Gaia DR3

Chen,

Li,

Zhang

et al. 2024

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Gaia DR3 data provide the latest and full astrometric data for more than 1.5 billion sources, and these allow us to revisit the 77 special open cluster candidates collected from LISC star cluster catalog. According to their unclear color–magnitude-diagram (CMD) morphology, they are difficult to be ensured as real open clusters (OCs), and their cluster properties are still poorly known. We perform a cluster census by reidentification for these clusters using pyUPMASK based on the photometric and astrometric stellar information. We have redetected these 77 objects and they should be real OCs, of which five clusters are potential binary clusters. Their basic parameters are obtained by fitting isochrones to observed CMDs. Our results show that their CMDs display more clean main sequences (MSs) and less member stars lying on the right of lower MSs relative to most of clusters in our initial sample, but broad MSs have not changed significantly. We suggest that efficient clustering algorithm combined with precision data can only partly reduce some stars lying on the right of lower MSs, and a simple stellar population of binary and rotating stars can partly reproduce multiple MS phenomena, including split and broad MSs.

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Stellar ages, masses, extinctions and orbital parameters based on spectroscopic parameters of Gaia DR3

Cited by 3 publications

References 0 publications

A Novel Survey for Young Substellar Objects with the W-band Filter. VI. Spectroscopic Census of Substellar Members and the IMF of the σ Orionis Cluster

A Novel Survey for Young Substellar Objects with the W-band Filter. VI. Spectroscopic Census of Substellar Members and the IMF of the σ Orionis Cluster

Spiral-like features in the disc revealed by Gaia DR3 radial actions

Revisit of 77 Clusters Candidates with Multiple Main Sequences using Gaia DR3

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