Ultracool dwarfs in Gaia DR3☆

被引：11

作者：

Sarro, L. M. ^{[1
]}

Berihuete, A. ^{[28
]}

Smart, R. L. ^{[2
]}

Reyle, C. ^{[27
]}

Barrado, D. ^{[26
]}

Garcia-Torres, M. ^{[19
]}

Cooper, W. J. ^{[2
,17
]}

Jones, H. R. A. ^{[17
]}

Marocco, F. ^{[24
]}

Creevey, O. L. ^{[3
]}

Sordo, R. ^{[4
]}

Bailer-Jones, C. A. L. ^{[8
]}

Montegriffo, P. ^{[13
]}

Carballo, R. ^{[15
]}

Andrae, R. ^{[8
]}

Fouesneau, M. ^{[8
]}

Lanzafame, A. C. ^{[9
,21
]}

Pailler, F. ^{[5
]}

Thevenin, F. ^{[3
]}

Lobel, A. ^{[6
]}

Delchambre, L. ^{[11
]}

Korn, A. J. ^{[7
]}

Recio-Blanco, A. ^{[3
]}

Schultheis, M. S. ^{[3
]}

De Angeli, F. ^{[12
]}

Brouillet, N. ^{[14
]}

Casamiquela, L. ^{[14
,16
]}

Contursi, G. ^{[3
]}

de Laverny, P. ^{[3
]}

Garcia-Lario, P. ^{[18
]}

Kordopatis, G. ^{[3
]}

Lebreton, Y. ^{[22
,23
]}

Livanou, E. ^{[20
]}

Lorca, A. ^{[10
]}

Palicio, P. A. ^{[3
]}

Slezak-Oreshina, I. ^{[3
]}

Soubiran, C. ^{[14
]}

Ulla, A. ^{[25
]}

Zhao, H. ^{[3
]}

机构：

[1] UNED, Dept Inteligencia Artificial, C Juan Rosal 16, Madrid 28040, Spain

[2] INAF Osservatorio Astrofis Torino, Via Osservatorio 20, I-10025 Pino Torinese, TO, Italy

[3] Univ Cote Azur, Observ Cote Azur, CNRS, Lab Lagrange, Bd Observ,CS 34229, F-06304 Nice 4, France

[4] INAF Osservatorio Astron Padova, Vicolo Osservatorio 5, I-35122 Padua, Italy

[5] CNES Ctr Spatial Toulouse, 18 Ave Edouard Belin, F-31401 Toulouse 9, France

[6] Royal Observ Belgium, Ringlaan 3, B-1180 Brussels, Belgium

[7] Uppsala Univ, Dept Phys & Astron, Div Astron & Space Phys, Observat Astrophys, Box 516, S-75120 Uppsala, Sweden

[8] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany

[9] INAF Osservatorio Astrofis Catania, Via S Sofia 78, I-95123 Catania, Italy

[10] Aurora Technol European Space Agcy ESA, Camino Bajo Castillo S-N, Villanueva De La Canada 28692, Madrid, Spain

[11] Univ Liege, Inst Astrophys & Geophys, 19c Allee Six Aout, B-4000 Liege, Belgium

[12] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England

[13] INAF Osservatorio Astrofis & Sci Spazio Bologna, Via Piero Gobetti 93-3, I-40129 Bologna, Italy

[14] Univ Bordeaux, Lab Astrophys Bordeaux, CNRS, B18,Allee Geoffroy St Hilaire, F-33615 Pessac, France

[15] Univ Cantabria, Dept Matemat Aplicada & Ciencias Comp, ETS Ingn Caminos Canales & Puertos, Ave Castros S-N, Santander 39005, Spain

[16] Univ PSL, GEPI, Observ Paris, CNRS, 5 Pl Jules Janssen, F-92190 Meudon, France

[17] Univ Hertfordshire, Ctr Astrophys Res, Coll Lane, Hatfield AL10 9AB, England

[18] European Space Agcy ESA, European Space Astron Ctr ESAC, Camino Bajo Castillo S-N, Villanueva De La Canada 28692, Madrid, Spain

[19] Pablo De Olavide Univ, Data Sci & Big Data Lab, Seville 41013, Spain

[20] Natl & Kapodistrian Univ Athens, Dept Astrophys Astron & Mech, Athens 15783, Greece

[21] Univ Catania, Dipartimento Fis & Astron Ettore Majorana, Via S Sofia 64, I-95123 Catania, Italy

[22] Univ Paris, Univ PSL, Sorbonne Univ, LESIA,CNRS,Observ Paris, 5 Pl Jules Janssen, F-92190 Meudon, France

[23] Univ Rennes, IPR Inst Phys Rennes, CNRS, UMR 6251, F-35000 Rennes, France

[24] CALTECH, IPAC, Mail Code 100-22,1200 E Calif Blvd, Pasadena, CA 91125 USA

[25] Univ Vigo, Appl Phys Dept, Vigo 36310, Spain

[26] Ctr Astrobiol CSIC INTA, Dept Astrofis, ESA ESAC, Camino Bajo Castillo S-N, Villanueva De La Canada 28692, Madrid, Spain

[27] Univ Bourgogne Franche Comte, Inst UTINAM, UMR 6213, CNRS,OSU THETA Franche Comte Bourgogne,Observ Bes, BP1615, F-25010 Besancon, France

[28] Univ Cadiz, Dept Estadist & Invest Operat, Avda Republ Saharaui S-N, Puerto Real 11510, Cadiz, Spain

来源：

ASTRONOMY & ASTROPHYSICS | 2023年 / 669卷

关键词：

brown dwarfs; stars; low-mass; late-type; methods; statistical; Hertzsprung-Russell and C-M diagrams; pre-main sequence; PROPER-MOTION SURVEY; LOW-MASS STARS; BROWN DWARFS; T-DWARFS; SKY SURVEY; COOL NEIGHBORS; CANDIDATE BINARIES; SPEX SPECTROSCOPY; NORTHERN STARS; DISCOVERY;

D O I：

10.1051/0004-6361/202244507

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. Previous Gaia data releases offered the opportunity to uncover ultracool dwarfs (UCDs) through astrometric, rather than purely photometric, selection. The most recent, the third data release (DR3), offers in addition the opportunity to use low-resolution spectra to refine and widen the selection.Aims. In this work we use the Gaia DR3 set of UCD candidates and complement the Gaia spectrophotometry with additional photometry in order to characterise the global properties of the set. This includes the inference of the distances, their locus in the Gaia colour-absolute magnitude diagram, and the (biased through selection) luminosity function at the faint end of the main sequence. We study the overall changes in the Gaia RP spectra as a function of spectral type. We study the UCDs in binary systems, we attempt to identify low-mass members of nearby young associations, star-forming regions, and clusters, and we analyse their variability properties.Methods. We used a forward model and the Bayesian inference framework to produce posterior probabilities for the distribution parameters and a calibration of the colour index as a function of the absolute magnitude in the form of a Gaussian process. Additionally, we applied the hierarchical mode association clustering (HMAC) unsupervised classification algorithm for the detection and characterisation of overdensities in the space of celestial coordinates, projected velocities, and parallaxes.Results. We detect 57 young, kinematically homogeneous groups, some of which are identified as well-known star-forming regions, associations, and clusters of different ages. We find that the primary members of the 880 binary systems with a UCD belong to the thin and thick disc components of the Milky Way. We identify 1109 variable UCDs using the variability tables in the Gaia archive, 728 of which belong to the star-forming regions defined by HMAC. We define two groups of variable UCDs with extreme bright or faint outliers.Conclusions. The set of sources identified as UCDs in the Gaia archive contains a wealth of information that will require focused follow-up studies and observations. It will help advance our understanding of the nature of the faint end of the main sequence and the stellar-substellar transition.

引用

页数：25

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