Characterizing the Evolved Stellar Population in the Galactic Foreground. I. Bolometric Magnitudes, Spatial Distribution and Period–Luminosity Relations
The Astrophysical Journal, vol. 904, pp. 82
Abstract
Abstract Radio campaigns using maser stellar beacons have provided crucial information to characterize Galactic stellar populations. Currently, the Bulge Asymmetries and Dynamical Evolution (BAaDE) project is surveying infrared (IR) color-selected targets for SiO masers. This provides a sample of evolved stars that can be used to study the inner, optically obscured Galaxy using line-of-sight velocities and possibly very long baseline interferometry proper motions. In order to use the BAaDE sample for kinematic studies, the stellar population should be characterized. In this study, the BAaDE targets have been cross-matched with IR (2MASS) and optical (Gaia) samples. By exploring the synergies of this cross-match together with Gaia parallaxes and extinction maps, the local (d < 2 kpc) asymptotic giant branch (AGB) stars can be characterized. We have defined a BAaDE–Gaia sample of 20,111 sources resulting from cross-matching BAaDE targets with IR and optical surveys. From this sample, a local sample of 1812 evolved stars with accurate parallax measurements, confirmed evolved stellar evolution stage, and within 2 kpc distance around the Sun was selected, for which absolute (bolometric) magnitudes are estimated. The evolved stellar population with Gaia counterparts that are variable seems to be predominantly associated with AGB stars with moderate luminosity ( <?CDATA ${1500}_{-500}^{+3000}\ {L}_{\odot }$?> ) and periods between 250 and 1250 days.
Authors 9
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Luis Henry Quiroga-Nuñez Aachen
Leiden University · University of New Mexico · National Radio Astronomy Observatory · Leiden Observatory · Joint Institute for VLBI ERIC
Affiliation as printed
Joint Institute for VLBI ERIC (JIVE), Dwingeloo, 7990AA, The Netherlands
Leiden University, Leiden Observatory, Leiden, 2300RA, The Netherlands
National Radio Astronomy Observatory, Array Operations Center, Socorro, NM 87801, USA; lquiroga@nrao.edu
University of New Mexico, Department of Physics and Astronomy, Albuquerque, NM 87131, USA
National Radio Astronomy Observatory, Array Operations Center, Socorro, NM 87801, USA
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Huib Jan van Langevelde Aachen
Leiden University · Leiden Observatory · Joint Institute for VLBI ERIC
Affiliation as printed
Joint Institute for VLBI ERIC (JIVE), Dwingeloo, 7990AA, The Netherlands
Leiden University, Leiden Observatory, Leiden, 2300RA, The Netherlands
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National Radio Astronomy Observatory
Affiliation as printed
National Radio Astronomy Observatory, Array Operations Center, Socorro, NM 87801, USA; lquiroga@nrao.edu
National Radio Astronomy Observatory, Array Operations Center, Socorro, NM 87801, USA
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Affiliation as printed
University of New Mexico, Department of Physics and Astronomy, Albuquerque, NM 87131, USA
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A. G. A. Brown Aachen
Leiden University · Leiden Observatory
Affiliation as printed
Leiden University, Leiden Observatory, Leiden, 2300RA, The Netherlands
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University of California, Los Angeles
Affiliation as printed
University of California, Department of Physics and Astronomy, Los Angeles, CA 90095, USA
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Affiliation as printed
Northwestern University, Center for Interdisciplinary Exploration and Research in Astrophysics, Evanston, IL 60201, USA
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University of New Mexico · National Radio Astronomy Observatory
Affiliation as printed
National Radio Astronomy Observatory, Array Operations Center, Socorro, NM 87801, USA; lquiroga@nrao.edu
University of New Mexico, Department of Physics and Astronomy, Albuquerque, NM 87131, USA
National Radio Astronomy Observatory, Array Operations Center, Socorro, NM 87801, USA
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Harm J. Habing Aachen
Leiden University · Leiden Observatory
Affiliation as printed
Leiden University, Leiden Observatory, Leiden, 2300RA, The Netherlands
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