Gaia Data Release 2 Observational Hertzsprung-Russell diagrams

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Gaia Data Release 2 Observational Hertzsprung-Russell diagrams. / Gaia Collaboration.

In: Astronomy & Astrophysics, Vol. 616, 10, 10.08.2018.

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Gaia Collaboration. / Gaia Data Release 2 Observational Hertzsprung-Russell diagrams. In: Astronomy & Astrophysics. 2018 ; Vol. 616.

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@article{e086c2d3fe9d4164b0d7bbe88f7f8f40,
title = "Gaia Data Release 2 Observational Hertzsprung-Russell diagrams",
abstract = "Context. Gaia Data Release 2 provides high-precision astrometry and three-band photometry for about 1.3 billion sources over the full sky. The precision, accuracy, and homogeneity of both astrometry and photometry are unprecedented.Aims. We highlight the power of the Gaia DR2 in studying many fine structures of the Hertzsprung-Russell diagram (HRD). Gaia allows us to present many different HRDs, depending in particular on stellar population selections. We do not aim here for completeness in terms of types of stars or stellar evolutionary aspects. Instead, we have chosen several illustrative examples.Methods. We describe some of the selections that can be made in Gaia DR2 to highlight the main structures of the Gaia HRDs. We select both field and cluster (open and globular) stars, compare the observations with previous classifications and with stellar evolutionary tracks, and we present variations of the Gaia HRD with age, metallicity, and kinematics. Late stages of stellar evolution such as hot subdwarfs, post-AGB stars, planetary nebulae, and white dwarfs are also analysed, as well as low-mass brown dwarf objects.Results. The Gaia HRDs are unprecedented in both precision and coverage of the various Milky Way stellar populations and stellar evolutionary phases. Many fine structures of the HRDs are presented. The clear split of the white dwarf sequence into hydrogen and helium white dwarfs is presented for the first time in an HRD. The relation between kinematics and the HRD is nicely illustrated. Two different populations in a classical kinematic selection of the halo are unambiguously identified in the HRD. Membership and mean parameters for a selected list of open clusters are provided. They allow drawing very detailed cluster sequences, highlighting fine structures, and providing extremely precise empirical isochrones that will lead to more insight in stellar physics.Conclusions. Gaia DR2 demonstrates the potential of combining precise astrometry and photometry for large samples for studies in stellar evolution and stellar population and opens an entire new area for HRD-based studies.",
keywords = "parallaxes, Hertzsprung-Russell and C-M diagrams, solar neighborhood, stars: evolution, COLOR-MAGNITUDE DIAGRAMS, MASS-RADIUS RELATION, GLOBULAR-CLUSTER SYSTEM, WHITE-DWARFS, PROPER MOTIONS, MILKY-WAY, T DWARFS, HORIZONTAL-BRANCH, STAR-CLUSTERS, SKY SURVEY",
author = "C. Babusiaux and {van Leeuwen}, F. and Barstow, {M. A.} and C. Jordi and A. Vallenari and D. Bossini and A. Bressan and T. Cantat-Gaudin and {van Leeuwen}, M. and Brown, {A. G. A.} and T. Prusti and {de Bruijne}, {J. H. J.} and Bailer-Jones, {C. A. L.} and M. Biermann and Evans, {D. W.} and L. Eyer and F. Jansen and Klioner, {S. A.} and U. Lammers and L. Lindegren 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 F. Arenou and U. Bastian 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 R. Guerra and B. Holl and E. Masana and R. Messineo and N. Mowlavi and K. Nienartowicz and P. Panuzzo and {von Essen}, C. and {Gaia Collaboration}",
year = "2018",
month = "8",
day = "10",
doi = "10.1051/0004-6361/201832843",
language = "English",
volume = "616",
journal = "Astronomy & Astrophysics",
issn = "0004-6361",
publisher = "E D P Sciences",

}

RIS

TY - JOUR

T1 - Gaia Data Release 2 Observational Hertzsprung-Russell diagrams

AU - Babusiaux, C.

AU - van Leeuwen, F.

AU - Barstow, M. A.

AU - Jordi, C.

AU - Vallenari, A.

AU - Bossini, D.

AU - Bressan, A.

AU - Cantat-Gaudin, T.

AU - van Leeuwen, M.

AU - Brown, A. G. A.

AU - Prusti, T.

AU - de Bruijne, J. H. J.

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

AU - Biermann, M.

AU - Evans, D. W.

AU - Eyer, L.

AU - Jansen, F.

AU - Klioner, S. A.

AU - Lammers, U.

AU - Lindegren, L.

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 - Arenou, F.

AU - Bastian, U.

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 - Guerra, R.

AU - Holl, B.

AU - Masana, E.

AU - Messineo, R.

AU - Mowlavi, N.

AU - Nienartowicz, K.

AU - Panuzzo, P.

AU - von Essen, C.

AU - Gaia Collaboration

PY - 2018/8/10

Y1 - 2018/8/10

N2 - Context. Gaia Data Release 2 provides high-precision astrometry and three-band photometry for about 1.3 billion sources over the full sky. The precision, accuracy, and homogeneity of both astrometry and photometry are unprecedented.Aims. We highlight the power of the Gaia DR2 in studying many fine structures of the Hertzsprung-Russell diagram (HRD). Gaia allows us to present many different HRDs, depending in particular on stellar population selections. We do not aim here for completeness in terms of types of stars or stellar evolutionary aspects. Instead, we have chosen several illustrative examples.Methods. We describe some of the selections that can be made in Gaia DR2 to highlight the main structures of the Gaia HRDs. We select both field and cluster (open and globular) stars, compare the observations with previous classifications and with stellar evolutionary tracks, and we present variations of the Gaia HRD with age, metallicity, and kinematics. Late stages of stellar evolution such as hot subdwarfs, post-AGB stars, planetary nebulae, and white dwarfs are also analysed, as well as low-mass brown dwarf objects.Results. The Gaia HRDs are unprecedented in both precision and coverage of the various Milky Way stellar populations and stellar evolutionary phases. Many fine structures of the HRDs are presented. The clear split of the white dwarf sequence into hydrogen and helium white dwarfs is presented for the first time in an HRD. The relation between kinematics and the HRD is nicely illustrated. Two different populations in a classical kinematic selection of the halo are unambiguously identified in the HRD. Membership and mean parameters for a selected list of open clusters are provided. They allow drawing very detailed cluster sequences, highlighting fine structures, and providing extremely precise empirical isochrones that will lead to more insight in stellar physics.Conclusions. Gaia DR2 demonstrates the potential of combining precise astrometry and photometry for large samples for studies in stellar evolution and stellar population and opens an entire new area for HRD-based studies.

AB - Context. Gaia Data Release 2 provides high-precision astrometry and three-band photometry for about 1.3 billion sources over the full sky. The precision, accuracy, and homogeneity of both astrometry and photometry are unprecedented.Aims. We highlight the power of the Gaia DR2 in studying many fine structures of the Hertzsprung-Russell diagram (HRD). Gaia allows us to present many different HRDs, depending in particular on stellar population selections. We do not aim here for completeness in terms of types of stars or stellar evolutionary aspects. Instead, we have chosen several illustrative examples.Methods. We describe some of the selections that can be made in Gaia DR2 to highlight the main structures of the Gaia HRDs. We select both field and cluster (open and globular) stars, compare the observations with previous classifications and with stellar evolutionary tracks, and we present variations of the Gaia HRD with age, metallicity, and kinematics. Late stages of stellar evolution such as hot subdwarfs, post-AGB stars, planetary nebulae, and white dwarfs are also analysed, as well as low-mass brown dwarf objects.Results. The Gaia HRDs are unprecedented in both precision and coverage of the various Milky Way stellar populations and stellar evolutionary phases. Many fine structures of the HRDs are presented. The clear split of the white dwarf sequence into hydrogen and helium white dwarfs is presented for the first time in an HRD. The relation between kinematics and the HRD is nicely illustrated. Two different populations in a classical kinematic selection of the halo are unambiguously identified in the HRD. Membership and mean parameters for a selected list of open clusters are provided. They allow drawing very detailed cluster sequences, highlighting fine structures, and providing extremely precise empirical isochrones that will lead to more insight in stellar physics.Conclusions. Gaia DR2 demonstrates the potential of combining precise astrometry and photometry for large samples for studies in stellar evolution and stellar population and opens an entire new area for HRD-based studies.

KW - parallaxes

KW - Hertzsprung-Russell and C-M diagrams

KW - solar neighborhood

KW - stars: evolution

KW - COLOR-MAGNITUDE DIAGRAMS

KW - MASS-RADIUS RELATION

KW - GLOBULAR-CLUSTER SYSTEM

KW - WHITE-DWARFS

KW - PROPER MOTIONS

KW - MILKY-WAY

KW - T DWARFS

KW - HORIZONTAL-BRANCH

KW - STAR-CLUSTERS

KW - SKY SURVEY

U2 - 10.1051/0004-6361/201832843

DO - 10.1051/0004-6361/201832843

M3 - Journal article

VL - 616

JO - Astronomy & Astrophysics

JF - Astronomy & Astrophysics

SN - 0004-6361

M1 - 10

ER -