Mapping the asymmetric disc of the Milky Way

被引：62

作者：

Drimmel, R. ^{[1
]}

Romero-Gomez, M. ^{[2
]}

Chemin, L. ^{[3
]}

Ramos, P. ^{[2
,4
]}

Poggio, E. ^{[1
,5
]}

Ripepi, V. ^{[6
]}

Andrae, R. ^{[7
]}

Blomme, R. ^{[8
]}

Cantat-Gaudin, T. ^{[2
,7
]}

Castro-Ginard, A. ^{[9
]}

Clementini, G. ^{[10
]}

Figueras, F. ^{[2
]}

Fouesneau, M. ^{[7
]}

Fremat, Y. ^{[8
]}

Jardine, K. ^{[11
]}

Khanna, S. ^{[1
,12
]}

Lobel, A. ^{[8
]}

Marshall, D. J. ^{[13
]}

Muraveva, T. ^{[10
]}

Brown, A. G. A. ^{[9
]}

Vallenari, A. ^{[14
]}

Prusti, T. ^{[15
]}

de Bruijne, J. H. J. ^{[15
]}

Arenou, F. ^{[16
]}

Babusiaux, C. ^{[16
,17
]}

Biermann, M. ^{[18
]}

Creevey, O. L. ^{[5
]}

Ducourant, C. ^{[19
]}

Evans, D. W. ^{[20
]}

Eyer, L. ^{[21
]}

Guerra, R. ^{[22
]}

Hutton, A. ^{[23
]}

Jordi, C. ^{[2
]}

Klioner, S. A. ^{[24
]}

Lammers, U. L. ^{[22
]}

Lindegren, L. ^{[25
]}

Luri, X. ^{[2
]}

Mignard, F. ^{[5
]}

Panem, C. ^{[26
]}

Pourbaix, D. ^{[27
,28
]}

Randich, S. ^{[29
]}

Sartoretti, P. ^{[16
]}

Soubiran, C. ^{[19
]}

Tanga, P. ^{[5
]}

Walton, N. A. ^{[20
]}

Bailer-Jones, C. A. L. ^{[7
]}

Bastian, U. ^{[18
]}

Jansen, F. ^{[30
]}

Katz, D. ^{[16
]}

Lattanzi, M. G. ^{[1
,31
]}

机构：

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

[2] Univ Barcelona IEEC UB, Inst Ciencies Cosmos ICCUB, Marti & Franques 1, Barcelona 08028, Spain

[3] Univ Antofagasta, Ctr Astron CITEVA, Ave Angamos 601, Antofagasta 1270300, Chile

[4] Univ Strasbourg, CNRS, Observ Astron Strasbourg, UMR 7550, 11 Rue Univ, F-67000 Strasbourg, France

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

[6] INAF Osservatorio Astron Capodimonte, Via Moiariello 16, I-80131 Naples, Italy

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

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

[9] Leiden Univ, Leiden Observ, Niels Bohrweg 2, NL-2333 CA Leiden, Netherlands

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

[11] Radagast Solut, Simon Vestdijkpad 24, NL-2321 WD Leiden, Netherlands

[12] Univ Groningen, Kapteyn Astron Inst, Landleven 12, NL-9747 AD Groningen, Netherlands

[13] Univ Toulouse, CNRS, IRAP, UPS,CNES, 9 Av Colonel Roche,BP 44346, F-31028 Toulouse 4, France

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

[15] European Space Agcy ESA, European Space Res & Technol Ctr ESTEC, Keplerlaan 1, NL-2201 AZ Noordwijk, Netherlands

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

[17] Univ Grenoble Alpes, CNRS, IPAG, F-38000 Grenoble, France

[18] Heidelberg Univ, Astron Rechen Inst, Zentrum Astron, Monchhofstr 12-14, D-69120 Heidelberg, Germany

[19] Univ Bordeaux, CNRS, Lab Astrophys Bordeaux, B18N,Allee Geoffroy St Hilaire, F-33615 Pessac, France

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

[21] Univ Geneva, Dept Astron, Chemin Pegasi 51, CH-1290 Versoix, Switzerland

[22] European Space Agcy ESA, European Space Astron Ctr ESAC, Camino Bajo Castillo S-N, Madrid 28692, Spain

[23] Aurora Technol European Space Agcy ESA, Camino Bajo Castillo S-N, Madrid 28692, Spain

[24] Tech Univ Dresden, Lohrmann Observ, Mommsenstr 13, D-01062 Dresden, Germany

[25] Lund Univ, Dept Astron & Theoret Phys, Lund Observ, Box 43, S-22100 Lund, Sweden

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

[27] Univ Libre Bruxelles, Inst Astron & Astrophys, CP 226,Blvd Triomphe, B-1050 Brussels, Belgium

[28] FRS FNRS, Rue Egmont 5, B-1000 Brussels, Belgium

[29] INAF Osservatorio Astrofis Arcetri, Largo Enrico Fermi 5, I-50125 Florence, Italy

[30] European Space Agcy ESA, Noordwijk, Netherlands

[31] Univ Turin, Dept Phys, Via Pietro Giuria 1, I-10125 Turin, Italy

[32] Univ Barcelona IEEC UB, DAPCOM Inst Ciencies Cosmos ICCUB, Marti & Franques 1, Barcelona 08028, Spain

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

[34] ALTEC Spa, Corso Marche 79, I-10146 Turin, Italy

[35] Sednai Sarl, Geneva, Switzerland

[36] Univ Geneva, Dept Astron, Chemin Ecogia 16, CH-1290 Versoix, Switzerland

[37] Univ Coll London, Mullard Space Sci Lab, Holmbury St Mary, Dorking RH5 6NT, Surrey, England

[38] ESAC, Gaia DPAC Project ffice, Camino Bajo Castillo S-N, Madrid 28692, Spain

[39] Telespazio UK SL European Space Agcy ESA, Camino Bajo Castillo S-N, Madrid 28692, Spain

[40] Sorbonne Univ, Univ PSL, CNRS, SYRTE,Observ Paris,LNE, 61 Ave Observ, F-75014 Paris, France

[41] Natl Observ Athens, Athens 15236, Greece

[42] Univ Lille, Sorbonne Univ, Univ PSL, IMCCE,CNRS,Observ Paris, 77 Denfert Rochereau, F-75014 Paris, France

[43] Serco Gest Negocios European Space Agcy ESA, Camino Bajo Castillo S-N, Madrid 28692, Spain

[44] Univ Liege, Inst Astrophys & Geophys, 19c,Allee 6 Aout, B-4000 Liege, Belgium

[45] CRAAG Ctr Rech Astron Astrophys & Geophys, Route Observ Bp 63 Bouzareah, Algiers 16340, Algeria

[46] Univ Edinburgh, Inst Astron, Royal Observ, Blackford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland

[47] RHEA European Space Agcy ESA, Camino Bajo Castillo S-N, Madrid 28692, Spain

[48] ATG Europe European Space Agcy ESA, Camino Bajo Castillo S-N, Madrid 28692, Spain

[49] Univ A Coruna, CIGUS CITIC Dept Comp Sci & Informat Technol, Campus Elvina S-N, La Coruna 15071, Spain

[50] Kavli Inst Cosmol Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England

来源：

ASTRONOMY & ASTROPHYSICS | 2023年 / 674卷

关键词：

Galaxy: kinematics and dynamics; Galaxy: structure; Galaxy: disk; Galaxy: bulge; catalogs; DIGITAL SKY SURVEY; GAIA DR2 LINKING; DATA RELEASE; CLASSICAL CEPHEIDS; PERIOD-LUMINOSITY; VERTICAL WAVES; GALACTIC DISC; GALAH SURVEY; VELOCITY FLUCTUATIONS; MASS-DISTRIBUTION;

D O I：

10.1051/0004-6361/202243797

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. With the most recent Gaia data release, the number of sources with complete 6D phase space information (position and velocity) has increased to well over 33 million stars, while stellar astrophysical parameters are provided for more than 470 million sources, and more than 11 million variable stars are identified. Aims. Using the astrophysical parameters and variability classifications provided in Gaia DR3, we selected various stellar populations to explore and identify non-axisymmetric features in the disc of the Milky Way in configuration and velocity space. Methods. Using more about 580 000 sources identified as hot OB stars, together with 988 known open clusters younger than 100 Myr, we mapped the spiral structure associated with star formation 4-5 kpc from the Sun. We selected over 2800 Classical Cepheids younger than 200 Myr that show spiral features extending as far as 10 kpc from the Sun in the outer disc. We also identified more than 8.7 million sources on the red giant branch (RGB), of which 5.7 million have line-of-sight velocities. This later sample allows the velocity field of the Milky Way to be mapped as far as 8 kpc from the Sun, including the inner disc. Results. The spiral structure revealed by the young populations is consistent with recent results using Gaia EDR3 astrometry and source lists based on near-infrared photometry, showing the Local (Orion) Arm to be at least 8 kpc long, and an outer arm consistent with what is seen in HI surveys, which seems to be a continuation of the Perseus arm into the third quadrant. The subset of RGB stars with velocities clearly reveals the large-scale kinematic signature of the bar in the inner disc, as well as evidence of streaming motions in the outer disc that might be associated with spiral arms or bar resonances. A local comparison of the velocity field of the OB stars reveals similarities and di fferences with the RGB sample. Conclusions. This cursory study of Gaia DR3 data shows there is a rich bounty of kinematic information to be explored more deeply, which will undoubtedly lead us to a clearer understanding of the dynamical nature of the non-axisymmetric structures of the Milky Way.

引用

页数：35

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