Reliable stellar abundances of individual stars with the MUSE integral-field spectrograph

Author:

Wang (王梓先) Zixian12ORCID,Hayden Michael R12,Sharma Sanjib12ORCID,Xiang (向茂盛) Maosheng3,Ting (丁源森) Yuan-Sen45678,Bland-Hawthorn Joss129ORCID,Chen Boquan12ORCID

Affiliation:

1. Sydney Institute for Astronomy, School of Physics , A28, The University of Sydney, NSW, 2006, Australia

2. ARC Centre of Excellence for All Sky Astrophysics in Three Dimensions (ASTRO-3D)

3. Max-Planck Institute for Astronomy , Königstuhl 17, D-69117 Heidelberg, Germany

4. Research School of Computer Science, Australian National University , Acton ACT 2601, Australia

5. Research School of Astronomy and Astrophysics, Australian National University , ACT 2611, Australia

6. Institute for Advanced Study , 1 Einstein Drive, Princeton, NJ 08540, USA

7. Department of Astrophysical Sciences, Princeton University , Princeton, NJ 08544, USA

8. Observatories of the Carnegie Institution of Washington , 813 Santa Barbara Street, Pasadena, CA 91101, USA

9. Miller Professor, Miller Institute , UC Berkeley, Berkeley CA 94720, USA

Abstract

ABSTRACT We present a novel approach to deriving stellar labels for stars observed in MUSE fields making use of data-driven machine learning methods. Taking advantage of the comparable spectral properties (resolution and wavelength coverage) of the LAMOST and MUSE instruments, we adopt the data-driven Payne (DD-Payne) model used on LAMOST observations and apply it to stars observed in MUSE fields. Remarkably, in spite of instrumental differences, according to the cross-validation of 27 LAMOST-MUSE common stars, we are able to determine stellar labels with precision better than 75K in Teff, 0.15 dex in log g, and 0.1 dex in abundances of [Fe/H], [Mg/Fe], [Si/Fe], [Ti/Fe], [C/Fe], [Ni/Fe], and [Cr/Fe] for current MUSE observations over a parameter range of 3800 < Teff < 7000 K, −1.5 < [Fe/H] < 0.5 dex. To date, MUSE has been used to target 13 000 fields across the southern sky since it was first commissioned 6 yr ago and it is unique in its ability to study dense star fields such as globular clusters or the Milky Way bulge. Our method will enable the automated determination of stellar parameters for all stars in these fields. Additionally, it opens the door for applications to data collected by other spectrographs having resolution similar to LAMOST. With the upcoming BlueMUSE and MAVIS, we will gain access to a whole new range of chemical abundances with higher precision, especially critical s-process elements, such as [Y/Fe] and [Ba/Fe], that provide key age diagnostics for stellar targets.

Funder

ESO

MUSE

Chinese Academy of Sciences

Publisher

Oxford University Press (OUP)

Subject

Space and Planetary Science,Astronomy and Astrophysics

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