The GALAH survey: accurate radial velocities and library of observed stellar template spectra

Tomaž Zwitter, Janez Kos, Andrea Chiavassa, Sven Buder, Gregor Traven, Klemen Čotar, Jane Lin, Martin Asplund, Joss Bland-Hawthorn, Andrew R. Casey, Gayandhi De Silva, Ly Duong, Kenneth C. Freeman, Karin Lind, Sarah Martell, Valentina D'Orazi, Katharine J. Schlesinger, Jeffrey D. Simpson, Sanjib Sharma, Daniel B. ZuckerBorja Anguiano, Luca Casagrande, Remo Collet, Jonathan Horner, Michael J. Ireland, Prajwal R. Kafle, Geraint Lewis, Ulisse Munari, David M. Nataf, Melissa Ness, Thomas Nordlander, Dennis Stello, Yuan Sen Ting, Chris G. Tinney, Fred Watson, Rob A. Wittenmyer, Maruša Žerja

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    GALAH is a large-scale magnitude-limited southern stellar spectroscopic survey. Its second data release (GALAH DR2) provides values of stellar parameters and abundances of 23 elements for 342 682 stars (Buder et al.). Here we add a description of the public release of radial velocities with a typical accuracy of 0.1 km s-1 for 336 215 of these stars, achievable due to the large wavelength coverage, high resolving power, and good signal-to-noise ratio of the observed spectra, but also because convective motions in stellar atmosphere and gravitational redshift from the star to the observer are taken into account. In the process we derive medians of observed spectra that are nearly noiseless, as they are obtained from between 100 and 1116 observed spectra belonging to the same bin with a width of 50 K in temperature, 0.2 dex in gravity, and 0.1 dex in metallicity. Publicly released 1181 median spectra have a resolving power of 28 000 and trace the well-populated stellar types with metallicities between -0.6 and +0.3. Note that radial velocities from GALAH are an excellent match to the accuracy of velocity components along the sky plane derived by Gaia for the same stars. The level of accuracy achieved here is adequate for studies of dynamics within stellar clusters, associations, and streams in the Galaxy. So it may be relevant for studies of the distribution of dark matter.

    Original languageEnglish
    Pages (from-to)645-654
    Number of pages10
    JournalMonthly Notices of the Royal Astronomical Society
    Issue number1
    Publication statusPublished - 21 Nov 2018

    Bibliographical note

    This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society, Volume 481, Issue 1, 21 November 2018, Pages 645–654, Copyright 2018 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.


    • Methods: data analysis
    • Stars: fundamental parameters
    • Surveys
    • methods: observational


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