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Phase-space Properties and Chemistry of the Sagittarius Stellar Stream Down to the Extremely Metal-poor ([Fe/H] ≲ -3) Regime

Journal Article · · The Astrophysical Journal
 [1];  [2];  [3];  [4];  [5];  [6];  [7];  [8];  [9]
  1. Univ. of Sao Paulo (Brazil); Univ. of Chicago, IL (United States)
  2. Leibniz Institute for Astrophysics Potsdam (AIP), Potsdam (Germany); Univ. of Potsdam (Germany)
  3. Univ. of Sao Paulo (Brazil); Institut d'Estudis Espacials de Catalunya (IEEC), Barcelona (Spain)
  4. Univ. of Sao Paulo (Brazil)
  5. Institut d'Estudis Espacials de Catalunya (IEEC), Barcelona (Spain); University of Central Lancashire, Preston (United Kingdom)
  6. Universidade Federal de Goiás, Goiânia (Brasil)
  7. Leibniz Institute for Astrophysics Potsdam (AIP), Potsdam (Germany); Laboratório Interinstitucional de e-Astronomia—LIneA, Rio de Janeiro (Brasil)
  8. Universidad Nacional Autónoma de México, Ensenada (Mexico)
  9. Chungnam National Univ., Daejeon (Korea, Republic of); University of Notre Dame, IN (United States)
In this work, we study the phase-space and chemical properties of the Sagittarius (Sgr) stream, the tidal tails produced by the ongoing destruction of the Sgr dwarf spheroidal (dSph) galaxy, focusing on its very metal-poor (VMP; [Fe/H] < -2) content. We combine spectroscopic and astrometric information from SEGUE and Gaia EDR3, respectively, with data products from a new large-scale run of the StarHorse spectrophotometric code. Our selection criteria yield ~1600 stream members, including >200 VMP stars. We find the leading arm (b > 0°) of the Sgr stream to be more metal-poor, by ~0.2 dex, than the trailing one (b < 0°). With a subsample of turnoff and subgiant stars, we estimate this substructure's stellar population to be ~1 Gyr older than the thick disk's. With the aid of an N-body model of the Sgr system, we verify that simulated particles stripped earlier (>2 Gyr ago) have present-day phase-space properties similar to lower metallicity stream stars. Conversely, those stripped more recently (<2 Gyr) are preferentially akin to metal-rich ([Fe/H] > -1) members of the stream. Such correlation between kinematics and chemistry can be explained by the existence of a dynamically hotter, less centrally concentrated, and more metal-poor population in Sgr dSph prior to its disruption, implying that this galaxy was able to develop a metallicity gradient before its accretion. Finally, we identified several carbon-enhanced metal-poor ([C/Fe] > +0.7 and [Fe/H] ≤ -1.5) stars in the Sgr stream, which might be in tension with current observations of its remaining core where such objects are not found.
Research Organization:
US Department of Energy (USDOE), Washington, DC (United States). Office of Science, Sloan Digital Sky Survey (SDSS)
Sponsoring Organization:
USDOE Office of Science (SC)
OSTI ID:
2425247
Journal Information:
The Astrophysical Journal, Journal Name: The Astrophysical Journal Journal Issue: 2 Vol. 946; ISSN 0004-637X
Publisher:
IOP PublishingCopyright Statement
Country of Publication:
United States
Language:
English

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