Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 471, Issue 1, Pages 770-791Publisher
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stx1433
Keywords
circumstellar matter; stars: fundamental parameters; Hertzsprung; Russell and colour; magnitude diagrams; stars: mass-loss; solar neighbourhood; infrared: stars
Categories
Funding
- UK Science and Technology Facility Council [ST/L000768/1]
- Alfred P. Sloan Foundation
- US Department of Energy Office of Science
- Center for High-Performance Computing at the University of Utah
- SCIENCE plan of the European Commission
- HCM plan of the European Commission [CT920791, CT940627]
- INSU in France
- MEN in France
- CNRS in France
- State of Baden-Wurttemberg in Germany
- DGICYT in Spain
- CNR in Italy
- FFwFBWF in Austria
- FAPESP in Brazil
- OTKA in Hungary [F-4239, F-013990]
- ESO CEE [A-04-046]
- National Aeronautics and Space Administration
- National Science Foundation
- Ballistic Missile Defense Organization
- NASA Office of Space Science
- ESA
- NASA
- STFC [ST/P000649/1] Funding Source: UKRI
- Science and Technology Facilities Council [ST/P000649/1] Funding Source: researchfish
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Effective temperatures and luminosities are calculated for 1475 921 Tycho-2 and 107 145 Hipparcos stars, based on distances from Gaia Data Release 1. Parameters are derived by comparing multi-wavelength archival photometry to BT-SETTL model atmospheres. The 1 sigma uncertainties for the Tycho-2 and Hipparcos stars are +/- 137 and +/- 125 K in temperature and +/- 35 and +/- 19 per cent in luminosity. The luminosity uncertainty is dominated by that of the Gaia parallax. Evidence for infrared excess between 4.6 and 25 mu m is found for 4256 stars, of which 1883 are strong candidates. These include asymptotic giant branch (AGB) stars, Cepheids, Herbig Ae/Be stars, young stellar objects and other sources. We briefly demonstrate the capabilities of this data set by exploring local interstellar extinction, the onset of dust production in AGB stars, the age and metallicity gradients of the solar neighbourhood and structure within the Gould Belt. We close by discussing the potential impact of future Gaia data releases.
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