The extended ‘stellar halo’ of the Ursa Minor dwarf galaxy

Sestito, Federico; Zaremba, Daria; Venn, Kim A; D’Aoust, Lina; Hayes, Christian; Jensen, Jaclyn; Navarro, Julio F; Jablonka, Pascale; Fernández-Alvar, Emma; Glover, Jennifer; McConnachie, Alan W; Chené, André-Nicolas

doi:10.1093/mnras/stad2427

The extended ‘stellar halo’ of the Ursa Minor dwarf galaxy

Journal Article · Wed Aug 16 00:00:00 EDT 2023 · Monthly Notices of the Royal Astronomical Society

DOI:https://doi.org/10.1093/mnras/stad2427· OSTI ID:2425402

^[1]; Zaremba, Daria ^[2]; ^[1]; D’Aoust, Lina ^[1]; Hayes, Christian ^[3]; Jensen, Jaclyn ^[1]; Navarro, Julio F ^[1]; Jablonka, Pascale ^[4]; Fernández-Alvar, Emma ^[5]; Glover, Jennifer ^[1]; McConnachie, Alan W ^[6]; Chené, André-Nicolas ^[7]

Univ. of Victoria, BC (Canada)
Univ. of Victoria, BC (Canada); National University of Kyiv-Mohyla Academy (Ukraine)
NRC Herzberg Astronomy & Astrophysics, Victoria, BC (Canada)
Ecole Polytechnique Federale Lausanne (EPFL) (Switzerland); PSL Univ. (France); Centre National de la Recherche Scientifique (CNRS) (France)
Institute of Astrophysics of the Canary Islands (Spain); University of La Laguna (Spain)
Univ. of Victoria, BC (Canada); NRC Herzberg Astronomy&nbsp;&amp; Astrophysics, Victoria (Canada)
National Optical-Infrared Astronomy Research Laboratory (NOIRLab), Hilo, HI (United States). Gemini Observatory

Stellar candidates in the Ursa Minor (UMi) dwarf galaxy have been found using a new Bayesian algorithm applied to Gaia EDR3 data. Five of these targets are located in the extreme outskirts of UMi, from ∼5 to 12 elliptical half-light radii (r_h), where r_h(UMi) = 17.32 ± 0.11 arcmin, and have been observed with the high-resolution Gemini Remote Access to CFHT ESPaDOnS Spectrograph at the Gemini North telescope. Precise radial velocities (σ_RV < 2 km s⁻¹) and metallicities (σ_[Fe/H] < 0.2 dex) confirm their memberships of UMi. Detailed analysis of the brightest and outermost star (Target 1, at ∼12r_h), yields precision chemical abundances for the α (Mg, Ca, and Ti), odd-Z (Na, K, and Sc), Fe-peak (Fe, Ni, and Cr), and neutron-capture (Ba) elements. With data from the literature and APOGEE data release 17, we find the chemical patterns in UMi are consistent with an outside-in star-formation history that includes yields from core-collapse supernovae, asymptotic giant branch stars, and Type Ia supernovae. Evidence for a knee in the [α/Fe] ratios near [Fe/H] ∼ −2.1 indicates a low star-formation efficiency similar to that in other dwarf galaxies. Detailed analysis of the surface number density profile shows evidence that UMi’s outskirts have been populated by tidal effects, likely as a result of completing multiple orbits around the Galaxy.

View Accepted Manuscript (DOE)

Research Organization:: US Department of Energy (USDOE), Washington, DC (United States). Office of Science, Sloan Digital Sky Survey (SDSS)

Sponsoring Organization:: Natural Sciences and Engineering Research Council of Canada; USDOE Office of Science (SC)

OSTI ID:: 2425402

Journal Information:: Monthly Notices of the Royal Astronomical Society, Journal Name: Monthly Notices of the Royal Astronomical Society Journal Issue: 2 Vol. 525; ISSN 0035-8711; ISSN 1365-2966

Publisher:: Oxford University PressCopyright Statement

Country of Publication:: United States

Language:: English

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