@Article{LeewenVJLBPBBBBBEEJKLLMPPRSSSVWAACDHKLOGHHPPBCCCCAFGHJMMMNOPPRRSTTTEGCGLMAAABBBBBCCCCCCDRTDDDFGGHHHHHHHHJJKKLMMMOPPPRRSSSSSTVVAAAAAAAÁAAAAAAAABBBBBBBNBBBBBBBBBBBBBBBBBBBBBBBBBBBBBCCCCCCCCCCCCCCCCCCCDDDDDCFLLMMSDDDDDDDDDDDDDEEEEFFFFFFFFFFFFFFFFFFGGGGGGGGGGGGGGGGGGGGGGGGHHHHHHHHHHHIIJJJJJKKKKKKKKKKKBLLLLLLLLLLLLLLLLLLLLLMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMMNNNNOOOPPPPPPPPPPPPPPPPPRRRRRRRRRRRRRRRRRRRSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSSTTTTTTTTTUUVVVVVVVVVVVVVWWWWWYZZZZAAAAAAABBBBBBBBBBBBBBBCCCCCDBTZDDDFFFFFGGGGGGGGHHIIJJJKKKKKKKKKLLLLMMMMMMMMNNOOOOOOOPPPPPPPPPPPRRRRRRRSSSSSSSSSSTTTTTTTVVVVVVWWWZZ:2017:OpClAs,
author = "Leewen, F. van and Vallenari, A. and Jordi, C. and Lindegren, L.
and Bastian, U. and Prusti, T. and De Bruijne, J. H. J. and Brown,
A. G. A. and Babusiaux, C. and Bailer-Jones, C. A. L. and
Biermann, M. and Evans, D. W. and Eyer, L. and Jansen, F. and
Klioner, S. A. and Lammers, U. and Luri, X. and Mignard, F. and
Panem, C. and Pourbaix, D. and Randich, S. and Sartoretti, P. and
Siddiqui, H. I. and Soubiran, C. and Valette, V. and Walton, N. A.
and Aerts, C. and Arenou, F. and Cropper, M. and Drimmel, R. and
Høg, E. and Katz, D. and Lattanzi, M. G. and O'Mullane, W. and
Grebel, E. K. and Holland, A. D. and Huc, C. and Passot, X. and
Perryman, M. and Bramante, L. and Cacciari, C. and Castañeda, J.
and Chaoul, L. and Cheek, N. and De Angeli, F. and Fabricius, C.
and Guerra, R. and Hern{\'a}ndez, J. and Jean-Antoine-Piccolo, A.
and Masana, E. and Messineo, R. and Mowlavi, N. and Nienartowicz,
K. and Ord{\'o}ñez-Blanco, D. and Panuzzo, P. and Portell, J. and
Richards, P. J. and Riello, M. and Seabroke, G. M. and Tanga, P.
and Th{\'e}venin, F. and Torra, J. and Els, S. G. and
Gracia-Abril, G. and Comoretto, G. and Garcia-Reinaldos, M. and
Lock, T. and Mercier, E. and Altmann, M. and Andrae, R. and
Astraatmadja, T. L. and Bellas-Velidis, I. and Benson, K. and
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Cuypers, J. and Davidson, M. and De Ridder, J. and De Torres, A.
and Delchambre, L. and Dell'oro, A. and Ducourant, C. and
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Wilkinson, M. I. and Ziaeepour, H. and Zschocke, S.",
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and {} and {Instituto Nacional de Pesquisas Espaciais (INPE)}",
title = "Gaia Data Release 1: Open cluster astrometry: Performance,
limitations, and future prospects",
journal = "Astronomy \& Astrophysics",
year = "2017",
volume = "601",
month = "May",
keywords = "Astrometry Open clusters and associations: general.",
abstract = "Context. The first Gaia Data Release contains the Tycho-Gaia
Astrometric Solution (TGAS). This is a subset of about 2 million
stars for which, besides the position and photometry, the proper
motion and parallax are calculated using Hipparcos and Tycho-2
positions in 1991.25 as prior information. Aims. We investigate
the scientific potential and limitations of the TGAS component by
means of the astrometric data for open clusters. Methods. Mean
cluster parallax and proper motion values are derived taking into
account the error correlations within the astrometric solutions
for individual stars, an estimate of the internal velocity
dispersion in the cluster, and, where relevant, the effects of the
depth of the cluster along the line of sight. Internal consistency
of the TGAS data is assessed. Results. Values given for standard
uncertainties are still inaccurate and may lead to unrealistic
unit-weight standard deviations of least squares solutions for
cluster parameters. Reconstructed mean cluster parallax and proper
motion values are generally in very good agreement with earlier
Hipparcos-based determination, although the Gaia mean parallax for
the Pleiades is a significant exception. We have no current
explanation for that discrepancy. Most clusters are observed to
extend to nearly 15 pc from the cluster centre, and it will be up
to future Gaia releases to establish whether those potential
cluster-member stars are still dynamically bound to the clusters.
Conclusions. The Gaia DR1 provides the means to examine open
clusters far beyond their more easily visible cores, and can
provide membership assessments based on proper motions and
parallaxes. A combined HR diagram shows the same features as
observed before using the Hipparcos data, with clearly increased
luminosities for older A and F dwarfs.",
doi = "10.1051/0004-6361/201730552",
url = "http://dx.doi.org/10.1051/0004-6361/201730552",
issn = "0004-6361 and 1432-0746",
language = "en",
urlaccessdate = "27 abr. 2024"
}