TY - JOUR
T1 - A Chemical and Kinematical Analysis of the Intermediate-age Open Cluster IC 166 from APOGEE and Gaia DR2
AU - Schiappacasse-Ulloa, J.
AU - Tang, B.
AU - Fernández-Trincado, J. G.
AU - Zamora, O.
AU - Geisler, D.
AU - Frinchaboy, P.
AU - Schultheis, M.
AU - Dell'Agli, F.
AU - Villanova, S.
AU - Masseron, T.
AU - Mészáros, Sz
AU - Souto, D.
AU - Hasselquist, S.
AU - Cunha, K.
AU - Smith, V. V.
AU - García-Hernández, D. A.
AU - Vieira, K.
AU - Robin, A. C.
AU - Minniti, D.
AU - Zasowski, G.
AU - Moreno, E.
AU - Pérez-Villegas, A.
AU - Lane, R. R.
AU - Ivans, I. I.
AU - Pan, K.
AU - Nitschelm, C.
AU - Santana, F. A.
AU - Carrera, R.
AU - Roman-Lopes, A.
N1 - Funding Information:
We would like to thank John Donor for helpful comments in the manuscript. We are grateful to the referee for a prompt and constructive report. J.G.F.-T. is supported by FONDECYT No. 3180210. J.S.-U. and D.G. gratefully acknowledge support from the Chilean BASAL Centro de Excelencia en Astrofísica y Tecnologías Afines (CATA) grant PFB-06/2007. B.T. acknowledges support from the one-hundred-talent project of Sun Yat-Sen University. S.V. gratefully acknowledges the support provided by Fondecyt reg n. 1170518. D.M. is supported by the BASAL Center for Astrophysics and Associated Technologies (CATA) through grant PFB-06, by the Ministry for the Economy, Development and Tourism, Programa Iniciativa Científica Milenio grant IC120009, awarded to the Millennium Institute of Astrophysics (MAS), and by FONDECYT Regular grant No. 1170121. Sz.M. has been supported by the Premium Postdoctoral Research Program of the Hungarian Academy of Sciences, and by the Hungarian NKFI Grants K-119517 of the Hungarian National Research, Development and Innovation Office. P.M.F. acknowledges support by an National Science Foundation AAG grants AST-1311835 & AST-1715662. V.V.S. and K.C. acknowledge support from NASA grant NNX17AB64G. O.Z., F.D., T.M., and D.A.G.H. acknowledge support provided by the Spanish Ministry of Economy and Competitiveness (MINECO) under grant AYA-2014-58082-P.
Funding Information:
Funding for the Sloan Digital Sky Survey IV (SDSS-IV) has been provided by the Alfred P. Sloan Foundation, the US Department of Energy Office of Science, and the Participating Institutions. SDSS-IV acknowledges support and resources from the Center for High-Performance Computing at the University of Utah. The SDSS website ishttp://www.sdss.org.
Funding Information:
Funding for the GravPot16 software has been provided by the Centre national d’études spatiales (CNES) through grant 0101973 and UTINAM Institute of the Université de Franche-Comté supported by the Région de Franche-Comté and Institut des Sciences de l’Univers (INSU). Simulations have been executed on computers from the Utinam Institute of the Université de Franche-Comté supported by the Région de Franche-Comté and Institut des Sciences de l’Univers (INSU), and on the supercomputer facilities of the Mésocentre de calcul de Franche-Comté.
Publisher Copyright:
© 2018. The American Astronomical Society.
PY - 2018/9/1
Y1 - 2018/9/1
N2 - IC 166 is an intermediate-age open cluster (OC) (∼1 Gyr) that lies in the transition zone of the metallicity gradient in the outer disk. Its location, combined with our very limited knowledge of its salient features, make it an interesting object of study. We present the first high-resolution spectroscopic and precise kinematical analysis of IC 166, which lies in the outer disk with R GC ∼ 12.7 kpc. High-resolution H-band spectra were analyzed using observations from the SDSS-IV Apache Point Observatory Galactic Evolution Experiment survey. We made use of the Brussels Automatic Stellar Parameter code to provide chemical abundances based on a line-by-line approach for up to eight chemical elements (Mg, Si, Ca, Ti, Al, K, Mn, and Fe). The α-element (Mg, Si, Ca, and whenever available Ti) abundances, and their trends with Fe abundances have been analyzed for a total of 13 high-likelihood cluster members. No significant abundance scatter was found in any of the chemical species studied. Combining the positional, heliocentric distance, and kinematic information, we derive, for the first time, the probable orbit of IC 166 within a Galactic model including a rotating boxy bar, and found that it is likely that IC 166 formed in the Galactic disk, supporting its nature as an unremarkable Galactic OC with an orbit bound to the Galactic plane.
AB - IC 166 is an intermediate-age open cluster (OC) (∼1 Gyr) that lies in the transition zone of the metallicity gradient in the outer disk. Its location, combined with our very limited knowledge of its salient features, make it an interesting object of study. We present the first high-resolution spectroscopic and precise kinematical analysis of IC 166, which lies in the outer disk with R GC ∼ 12.7 kpc. High-resolution H-band spectra were analyzed using observations from the SDSS-IV Apache Point Observatory Galactic Evolution Experiment survey. We made use of the Brussels Automatic Stellar Parameter code to provide chemical abundances based on a line-by-line approach for up to eight chemical elements (Mg, Si, Ca, Ti, Al, K, Mn, and Fe). The α-element (Mg, Si, Ca, and whenever available Ti) abundances, and their trends with Fe abundances have been analyzed for a total of 13 high-likelihood cluster members. No significant abundance scatter was found in any of the chemical species studied. Combining the positional, heliocentric distance, and kinematic information, we derive, for the first time, the probable orbit of IC 166 within a Galactic model including a rotating boxy bar, and found that it is likely that IC 166 formed in the Galactic disk, supporting its nature as an unremarkable Galactic OC with an orbit bound to the Galactic plane.
KW - Galaxy: abundances
KW - Galaxy: kinematics and dynamics
KW - open clusters and associations: individual (IC 166)
UR - http://www.scopus.com/inward/record.url?scp=85053124009&partnerID=8YFLogxK
U2 - 10.3847/1538-3881/aad048
DO - 10.3847/1538-3881/aad048
M3 - Article
AN - SCOPUS:85053124009
SN - 0004-6256
VL - 156
JO - Astronomical Journal
JF - Astronomical Journal
IS - 3
M1 - 94
ER -