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Chemical abundances in a high-velocity RR Lyrae star near the bulge

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Chemical abundances in a high-velocity RR Lyrae star near the bulge. / Hansen, C. J.; Rich, R. M.; Koch, A. et al.
In: Astronomy and Astrophysics, Vol. 590, A39, 01.06.2016.

Research output: Contribution to Journal/MagazineJournal articlepeer-review

Harvard

Hansen, CJ, Rich, RM, Koch, A, Xu, S, Kunder, A & Ludwig, H-G 2016, 'Chemical abundances in a high-velocity RR Lyrae star near the bulge', Astronomy and Astrophysics, vol. 590, A39. https://doi.org/10.1051/0004-6361/201628279

APA

Hansen, C. J., Rich, R. M., Koch, A., Xu, S., Kunder, A., & Ludwig, H-G. (2016). Chemical abundances in a high-velocity RR Lyrae star near the bulge. Astronomy and Astrophysics, 590, Article A39. https://doi.org/10.1051/0004-6361/201628279

Vancouver

Hansen CJ, Rich RM, Koch A, Xu S, Kunder A, Ludwig H-G. Chemical abundances in a high-velocity RR Lyrae star near the bulge. Astronomy and Astrophysics. 2016 Jun 1;590:A39. Epub 2016 May 4. doi: 10.1051/0004-6361/201628279

Author

Hansen, C. J. ; Rich, R. M. ; Koch, A. et al. / Chemical abundances in a high-velocity RR Lyrae star near the bulge. In: Astronomy and Astrophysics. 2016 ; Vol. 590.

Bibtex

@article{3b585aa821d0400aa2b7913032be07a3,
title = "Chemical abundances in a high-velocity RR Lyrae star near the bulge",
abstract = "Low-mass variable high-velocity stars are interesting study cases for many aspects of Galactic structure and evolution. Until recently, the only known high- or hyper-velocity stars were young stars thought to originate from the Galactic center. Wide-area surveys such as APOGEE and BRAVA have found several low-mass stars in the bulge with Galactic rest-frame velocities higher than 350 km s-1. In this study we present the first abundance analysis of a low-mass RR Lyrae star that is located close to the Galactic bulge, with a space motion of ~–400 km s-1. Using medium-resolution spectra, we derived abundances (including upper limits) of 11 elements. These allowed us to chemically tag the star and discuss its origin, although our derived abundances and metallicity, at [Fe/H] =−0.9 dex, do not point toward one unambiguous answer. Based on the chemical tagging, we cannot exclude that it originated in the bulge. However, its retrograde orbit and the derived abundances combined suggest that the star was accelerated from the outskirts of the inner (or even outer) halo during many-body interactions. Other possible origins include the bulge itself, or the star might have been stripped from a stellar cluster or the Sagittarius dwarf galaxy when it merged with the Milky Way.",
keywords = "stars: abundances , stars: variables: RR Lyrae, stars: Population II, stars: kinematics and dynamics, Galaxy: bulge, Galaxy: halo",
author = "Hansen, {C. J.} and Rich, {R. M.} and A. Koch and S. Xu and A. Kunder and H.-G. Ludwig",
year = "2016",
month = jun,
day = "1",
doi = "10.1051/0004-6361/201628279",
language = "English",
volume = "590",
journal = "Astronomy and Astrophysics",
issn = "0004-6361",
publisher = "EDP Sciences",

}

RIS

TY - JOUR

T1 - Chemical abundances in a high-velocity RR Lyrae star near the bulge

AU - Hansen, C. J.

AU - Rich, R. M.

AU - Koch, A.

AU - Xu, S.

AU - Kunder, A.

AU - Ludwig, H.-G.

PY - 2016/6/1

Y1 - 2016/6/1

N2 - Low-mass variable high-velocity stars are interesting study cases for many aspects of Galactic structure and evolution. Until recently, the only known high- or hyper-velocity stars were young stars thought to originate from the Galactic center. Wide-area surveys such as APOGEE and BRAVA have found several low-mass stars in the bulge with Galactic rest-frame velocities higher than 350 km s-1. In this study we present the first abundance analysis of a low-mass RR Lyrae star that is located close to the Galactic bulge, with a space motion of ~–400 km s-1. Using medium-resolution spectra, we derived abundances (including upper limits) of 11 elements. These allowed us to chemically tag the star and discuss its origin, although our derived abundances and metallicity, at [Fe/H] =−0.9 dex, do not point toward one unambiguous answer. Based on the chemical tagging, we cannot exclude that it originated in the bulge. However, its retrograde orbit and the derived abundances combined suggest that the star was accelerated from the outskirts of the inner (or even outer) halo during many-body interactions. Other possible origins include the bulge itself, or the star might have been stripped from a stellar cluster or the Sagittarius dwarf galaxy when it merged with the Milky Way.

AB - Low-mass variable high-velocity stars are interesting study cases for many aspects of Galactic structure and evolution. Until recently, the only known high- or hyper-velocity stars were young stars thought to originate from the Galactic center. Wide-area surveys such as APOGEE and BRAVA have found several low-mass stars in the bulge with Galactic rest-frame velocities higher than 350 km s-1. In this study we present the first abundance analysis of a low-mass RR Lyrae star that is located close to the Galactic bulge, with a space motion of ~–400 km s-1. Using medium-resolution spectra, we derived abundances (including upper limits) of 11 elements. These allowed us to chemically tag the star and discuss its origin, although our derived abundances and metallicity, at [Fe/H] =−0.9 dex, do not point toward one unambiguous answer. Based on the chemical tagging, we cannot exclude that it originated in the bulge. However, its retrograde orbit and the derived abundances combined suggest that the star was accelerated from the outskirts of the inner (or even outer) halo during many-body interactions. Other possible origins include the bulge itself, or the star might have been stripped from a stellar cluster or the Sagittarius dwarf galaxy when it merged with the Milky Way.

KW - stars: abundances

KW - stars: variables: RR Lyrae

KW - stars: Population II

KW - stars: kinematics and dynamics

KW - Galaxy: bulge

KW - Galaxy: halo

U2 - 10.1051/0004-6361/201628279

DO - 10.1051/0004-6361/201628279

M3 - Journal article

VL - 590

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

SN - 0004-6361

M1 - A39

ER -