Gaia Data Release 2 Kinematics of globular clusters and dwarf galaxies around the Milky Way

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Gaia Data Release 2 Kinematics of globular clusters and dwarf galaxies around the Milky Way. / Gaia Collaboration.

In: Astronomy & Astrophysics, Vol. 616, 12, 10.08.2018.

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Gaia Collaboration. / Gaia Data Release 2 Kinematics of globular clusters and dwarf galaxies around the Milky Way. In: Astronomy & Astrophysics. 2018 ; Vol. 616.

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@article{46253e3925ea4a5e87fc100816afeeb3,
title = "Gaia Data Release 2 Kinematics of globular clusters and dwarf galaxies around the Milky Way",
abstract = "Aims. The goal of this paper is to demonstrate the outstanding quality of the second data release of the Gaia mission and its power for constraining many different aspects of the dynamics of the satellites of the Milky Way. We focus here on determining the proper motions of 75 Galactic globular clusters, nine dwarf spheroidal galaxies, one ultra-faint system, and the Large and Small Magellanic Clouds.Methods. Using data extracted from the Gaia archive, we derived the proper motions and parallaxes for these systems, as well as their uncertainties. We demonstrate that the errors, statistical and systematic, are relatively well understood. We integrated the orbits of these objects in three different Galactic potentials, and characterised their properties. We present the derived proper motions, space velocities, and characteristic orbital parameters in various tables to facilitate their use by the astronomical community.Results. Our limited and straightforward analyses have allowed us for example to (i) determine absolute and very precise proper motions for globular clusters; (ii) detect clear rotation signatures in the proper motions of at least five globular clusters; (iii) show that the satellites of the Milky Way are all on high-inclination orbits, but that they do not share a single plane of motion; (i v) derive a lower limit for the mass of the Milky Way of 9.1(-2.6)(+6.2) x 10(11) M-circle dot based on the assumption that the Leo I dwarf spheroidal is bound; (v) derive a rotation curve for the Large Magellanic Cloud based solely on proper motions that is competitive with line-of-sight velocity curves, now using many orders of magnitude more sources; and (v i) unveil the dynamical effect of the bar on the motions of stars in the Large Magellanic Cloud.Conclusions. All these results highlight the incredible power of the Gaia astrometric mission, and in particular of its second data release.",
keywords = "Galaxy: kinematics and dynamics, astrometry, globular clusters: general, galaxies: dwarf, Local Group, Magellanic Clouds, LARGE-MAGELLANIC-CLOUD, EXPLORING HALO SUBSTRUCTURE, VELOCITY DISPERSION PROFILE, TO-LIGHT RATIOS, PROPER MOTIONS, SPHEROIDAL GALAXY, SATELLITE GALAXIES, DARK-MATTER, SPACE VELOCITIES, GALACTIC HALO",
author = "A. Helmi and {van Leeuwen}, F. and McMillan, {P. J.} and D. Massari and T. Antoja and Robin, {A. C.} and L. Lindegren and U. Bastian and F. Arenou and C. Babusiaux and M. Biermann and Breddels, {M. A.} and D. Hobbs and C. Jordi and E. Pancino and C. Reyle and J. Veljanoski and Brown, {A. G. A.} and A. Vallenari and T. Prusti and {de Bruijne}, {J. H. J.} and Bailer-Jones, {C. A. L.} and Evans, {D. W.} and L. Eyer and F. Jansen and Klioner, {S. A.} and U. Lammers and X. Luri and F. Mignard and C. Panem and D. Pourbaix and S. Randich and P. Sartoretti and Siddiqui, {H. I.} and C. Soubiran and Walton, {N. A.} and M. Cropper and R. Drimmel and D. Katz and Lattanzi, {M. G.} and J. Bakker and C. Cacciari and J. Castaneda and L. Chaoul and N. Cheek and {De Angeli}, F. and C. Fabricius and J. Hernandez and D. Bossini and {von Essen}, C. and {Gaia Collaboration}",
year = "2018",
month = "8",
day = "10",
doi = "10.1051/0004-6361/201832698",
language = "English",
volume = "616",
journal = "Astronomy & Astrophysics",
issn = "0004-6361",
publisher = "E D P Sciences",

}

RIS

TY - JOUR

T1 - Gaia Data Release 2 Kinematics of globular clusters and dwarf galaxies around the Milky Way

AU - Helmi, A.

AU - van Leeuwen, F.

AU - McMillan, P. J.

AU - Massari, D.

AU - Antoja, T.

AU - Robin, A. C.

AU - Lindegren, L.

AU - Bastian, U.

AU - Arenou, F.

AU - Babusiaux, C.

AU - Biermann, M.

AU - Breddels, M. A.

AU - Hobbs, D.

AU - Jordi, C.

AU - Pancino, E.

AU - Reyle, C.

AU - Veljanoski, J.

AU - Brown, A. G. A.

AU - Vallenari, A.

AU - Prusti, T.

AU - de Bruijne, J. H. J.

AU - Bailer-Jones, C. A. L.

AU - Evans, D. W.

AU - Eyer, L.

AU - Jansen, F.

AU - Klioner, S. A.

AU - Lammers, U.

AU - Luri, X.

AU - Mignard, F.

AU - Panem, C.

AU - Pourbaix, D.

AU - Randich, S.

AU - Sartoretti, P.

AU - Siddiqui, H. I.

AU - Soubiran, C.

AU - Walton, N. A.

AU - Cropper, M.

AU - Drimmel, R.

AU - Katz, D.

AU - Lattanzi, M. G.

AU - Bakker, J.

AU - Cacciari, C.

AU - Castaneda, J.

AU - Chaoul, L.

AU - Cheek, N.

AU - De Angeli, F.

AU - Fabricius, C.

AU - Hernandez, J.

AU - Bossini, D.

AU - von Essen, C.

AU - Gaia Collaboration

PY - 2018/8/10

Y1 - 2018/8/10

N2 - Aims. The goal of this paper is to demonstrate the outstanding quality of the second data release of the Gaia mission and its power for constraining many different aspects of the dynamics of the satellites of the Milky Way. We focus here on determining the proper motions of 75 Galactic globular clusters, nine dwarf spheroidal galaxies, one ultra-faint system, and the Large and Small Magellanic Clouds.Methods. Using data extracted from the Gaia archive, we derived the proper motions and parallaxes for these systems, as well as their uncertainties. We demonstrate that the errors, statistical and systematic, are relatively well understood. We integrated the orbits of these objects in three different Galactic potentials, and characterised their properties. We present the derived proper motions, space velocities, and characteristic orbital parameters in various tables to facilitate their use by the astronomical community.Results. Our limited and straightforward analyses have allowed us for example to (i) determine absolute and very precise proper motions for globular clusters; (ii) detect clear rotation signatures in the proper motions of at least five globular clusters; (iii) show that the satellites of the Milky Way are all on high-inclination orbits, but that they do not share a single plane of motion; (i v) derive a lower limit for the mass of the Milky Way of 9.1(-2.6)(+6.2) x 10(11) M-circle dot based on the assumption that the Leo I dwarf spheroidal is bound; (v) derive a rotation curve for the Large Magellanic Cloud based solely on proper motions that is competitive with line-of-sight velocity curves, now using many orders of magnitude more sources; and (v i) unveil the dynamical effect of the bar on the motions of stars in the Large Magellanic Cloud.Conclusions. All these results highlight the incredible power of the Gaia astrometric mission, and in particular of its second data release.

AB - Aims. The goal of this paper is to demonstrate the outstanding quality of the second data release of the Gaia mission and its power for constraining many different aspects of the dynamics of the satellites of the Milky Way. We focus here on determining the proper motions of 75 Galactic globular clusters, nine dwarf spheroidal galaxies, one ultra-faint system, and the Large and Small Magellanic Clouds.Methods. Using data extracted from the Gaia archive, we derived the proper motions and parallaxes for these systems, as well as their uncertainties. We demonstrate that the errors, statistical and systematic, are relatively well understood. We integrated the orbits of these objects in three different Galactic potentials, and characterised their properties. We present the derived proper motions, space velocities, and characteristic orbital parameters in various tables to facilitate their use by the astronomical community.Results. Our limited and straightforward analyses have allowed us for example to (i) determine absolute and very precise proper motions for globular clusters; (ii) detect clear rotation signatures in the proper motions of at least five globular clusters; (iii) show that the satellites of the Milky Way are all on high-inclination orbits, but that they do not share a single plane of motion; (i v) derive a lower limit for the mass of the Milky Way of 9.1(-2.6)(+6.2) x 10(11) M-circle dot based on the assumption that the Leo I dwarf spheroidal is bound; (v) derive a rotation curve for the Large Magellanic Cloud based solely on proper motions that is competitive with line-of-sight velocity curves, now using many orders of magnitude more sources; and (v i) unveil the dynamical effect of the bar on the motions of stars in the Large Magellanic Cloud.Conclusions. All these results highlight the incredible power of the Gaia astrometric mission, and in particular of its second data release.

KW - Galaxy: kinematics and dynamics

KW - astrometry

KW - globular clusters: general

KW - galaxies: dwarf

KW - Local Group

KW - Magellanic Clouds

KW - LARGE-MAGELLANIC-CLOUD

KW - EXPLORING HALO SUBSTRUCTURE

KW - VELOCITY DISPERSION PROFILE

KW - TO-LIGHT RATIOS

KW - PROPER MOTIONS

KW - SPHEROIDAL GALAXY

KW - SATELLITE GALAXIES

KW - DARK-MATTER

KW - SPACE VELOCITIES

KW - GALACTIC HALO

U2 - 10.1051/0004-6361/201832698

DO - 10.1051/0004-6361/201832698

M3 - Journal article

VL - 616

JO - Astronomy & Astrophysics

JF - Astronomy & Astrophysics

SN - 0004-6361

M1 - 12

ER -