The Astrophysical Journal (Jan 2025)

GD-1 Stellar Stream and Cocoon in the DESI Early Data Release

  • M. Valluri,
  • P. Fagrelius,
  • S. E. Koposov,
  • T. S. Li,
  • Oleg Y. Gnedin,
  • E. F. Bell,
  • R. G. Carlberg,
  • A. P. Cooper,
  • J. Aguilar,
  • S. Ahlen,
  • C. Allende Prieto,
  • V. Belokurov,
  • L. Beraldo e Silva,
  • D. Brooks,
  • A. Byström,
  • T. Claybaugh,
  • K. Dawson,
  • A. Dey,
  • P. Doel,
  • J. E. Forero-Romero,
  • E. Gaztañaga,
  • S. Gontcho A Gontcho,
  • J. Han,
  • K. Honscheid,
  • T. Kisner,
  • A. Kremin,
  • A. Lambert,
  • M. Landriau,
  • L. Le Guillou,
  • M. E. Levi,
  • A. de la Macorra,
  • M. Manera,
  • P. Martini,
  • G. E. Medina,
  • A. Meisner,
  • R. Miquel,
  • J. Moustakas,
  • A. D. Myers,
  • J. Najita,
  • C. Poppett,
  • F. Prada,
  • M. Rezaie,
  • G. Rossi,
  • A. H. Riley,
  • E. Sanchez,
  • D. Schlegel,
  • M. Schubnell,
  • D. Sprayberry,
  • G. Tarlé,
  • G. Thomas,
  • B. A. Weaver,
  • R. H. Wechsler,
  • R. Zhou,
  • H. Zou

DOI
https://doi.org/10.3847/1538-4357/ada690
Journal volume & issue
Vol. 980, no. 1
p. 71

Abstract

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We present ∼115 new spectroscopically identified members of the GD-1 tidal stream observed with the 5000-fiber Dark Energy Spectroscopic Instrument (DESI). We confirm the existence of a “cocoon,” which is a broad (FWHM ∼ 2 $\mathop{.}\limits^{\unicode{x000b0}}$ 932 ∼ 460 pc) and kinematically hot (velocity dispersion, σ ∼ 5–8 km s ^−1 ) component that surrounds a narrower (FWHM ∼ 0 $\mathop{.}\limits^{\unicode{x000b0}}$ 353 ∼ 55 pc) and colder [( σ = 3.09 ± 0.76 km s ^−1 )] thin stream component (based on a median per star velocity precision of 2.7 km s ^−1 ). The cocoon extends over at least a 30 ^∘ segment of the stream observed by DESI. The thin and cocoon components have similar mean values of [Fe/H]: −2.54 ± 0.04 dex and −2.47 ± 0.06 dex, suggestive of a common origin. The data are consistent with the following scenarios for the origin of the cocoon. The progenitor of the GD-1 stream was an accreted globular cluster (GC) and: (a) the cocoon was produced by pre-accretion tidal stripping of the GC while it was still inside its parent dwarf galaxy; (b) the cocoon comprises debris from the parent dwarf galaxy; (c) an initially thin GC tidal stream was heated by impacts from dark subhalos in the Milky Way; (d) an initially thin GC stream was heated by a massive Sagittarius dwarf galaxy; or a combination of some of these. Future DESI spectroscopy and detailed modeling may enable us to distinguish between these possible origins.

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