TY - JOUR
T1 - A new method to identify subclasses among AGB stars using Gaia and 2MASS photometry
AU - Lebzelter, T.
AU - Mowlavi, N.
AU - Marigo, P.
AU - Pastorelli, G.
AU - Trabucchi, M.
AU - Wood, P. R.
AU - Lecoeur-Taibi, I.
N1 - Publisher Copyright:
© ESO 2018
PY - 2018
Y1 - 2018
N2 - 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 WRP,BP−RP and WKs,J−Ks in the Gaia BP, RP, and 2MASS J, Ks spectral ranges, respectively, and use a new diagram, (WRP,BP−RP − WKs,J−Ks) versus Ks, 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.
AB - 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 WRP,BP−RP and WKs,J−Ks in the Gaia BP, RP, and 2MASS J, Ks spectral ranges, respectively, and use a new diagram, (WRP,BP−RP − WKs,J−Ks) versus Ks, 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.
KW - Magellanic clouds
KW - Stars: AGB and post-AGB
KW - Stars: Evolution
KW - Stars: Variables: General
UR - http://www.scopus.com/inward/record.url?scp=85061096971&partnerID=8YFLogxK
U2 - 10.1051/0004-6361/201833615
DO - 10.1051/0004-6361/201833615
M3 - Article
SN - 0004-6361
VL - 616
JO - Astronomy and Astrophysics
JF - Astronomy and Astrophysics
M1 - L13
ER -