2018/08/01 by T. Lebzelter, N. Mowlavi, N. Mowlavï +9 · 1 citation
Mathematics · Physics and Astronomy · #Astronomy #Astronomy and Astrophysical Research #Astrophysics #Astrophysics and Star Formation Studies #Asymptotic giant branch #Diagram #Large Magellanic Cloud #Mathematics #Photometry (optics) #Physics #Population #Stars #Statistics #Stellar classification #Stellar, planetary, and galactic studies #astro-ph.SR
paper · pdf · doi:10.1051/0004-6361/201833615
published as A&A 616, L13 (2018) · accepted for publication in A&A Letters; 7 figures, 2 appendices
openalex publication_date 2018/08/01 · arxiv created 2018/08/10 · openalex created_date 2018/08/22 · arxiv updated 2018/08/29 · openalex updated_date 2026/08/05
Aims . We explore the wealth of high-quality photometric data provided by data release 2 (DR2) of the Gaia mission for long-period variables (LPVs) in the Large Magellanic Cloud (LMC). Our goal is to identify stars of various types and masses along the asymptotic giant branch. Methods . For this endeavour, we developed a new multi-band approach combining Wesenheit functions W RP,BP−RP and W K s , J − K s in the Gaia BP, RP, and 2MASS J, K s spectral ranges, respectively, and use a new diagram, ( W RP,BP−RP − W K s , J − K s ) versus K s , to distinguish between different kinds of stars in our sample of LPVs. We used stellar population synthesis models to validate our approach. Results . We demonstrate the ability of the new diagram to discriminate between O- and C-rich objects, and to identify low-mass, intermediate-mass, and massive O-rich red giants, as well as extreme C-rich stars. Stellar evolution and population synthesis models guide the interpretation of the results, highlighting the diagnostic power of the new tool to discriminate between stellar initial masses, chemical properties, and evolutionary stages.