$S^5$: The Orbital and Chemical Properties of One Dozen Stellar Streams. (arXiv:2110.06950v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Li_T/0/1/0/all/0/1">Ting S. Li</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ji_A/0/1/0/all/0/1">Alexander P. Ji</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pace_A/0/1/0/all/0/1">Andrew B. Pace</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Erkal_D/0/1/0/all/0/1">Denis Erkal</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Koposov_S/0/1/0/all/0/1">Sergey E. Koposov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shipp_N/0/1/0/all/0/1">Nora Shipp</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Costa_G/0/1/0/all/0/1">Gary S. Da Costa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cullinane_L/0/1/0/all/0/1">Lara R. Cullinane</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kuehn_K/0/1/0/all/0/1">Kyler Kuehn</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lewis_G/0/1/0/all/0/1">Geraint F. Lewis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mackey_D/0/1/0/all/0/1">Dougal Mackey</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Simpson_J/0/1/0/all/0/1">Jeffrey D. Simpson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zucker_D/0/1/0/all/0/1">Daniel B. Zucker</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ferguson_P/0/1/0/all/0/1">Peter S. Ferguson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Martell_S/0/1/0/all/0/1">Sarah L. Martell</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bland_Hawthorn_J/0/1/0/all/0/1">Joss Bland-Hawthorn</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Balbinot_E/0/1/0/all/0/1">Eduardo Balbinot</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tavangar_K/0/1/0/all/0/1">Kiyan Tavangar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Drlica_Wagner_A/0/1/0/all/0/1">Alex Drlica-Wagner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Silva1_G/0/1/0/all/0/1">Gayandhi M. De Silva1</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Simon_J/0/1/0/all/0/1">Joshua D. Simon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Collaboration_S5/0/1/0/all/0/1">S5 Collaboration</a>

We report the kinematic, orbital, and chemical properties of 12 stellar
streams with no evident progenitors, using line-of-sight velocities and
metallicities from the Southern Stellar Stream Spectroscopic Survey ($S^5$),
proper motions from Gaia EDR3, and distances derived from distance tracers or
the literature. This data set provides the largest homogeneously analyzed set
of streams with full 6D kinematics and metallicities. All streams have
heliocentric distances between ${sim}10-50$ kpc. The velocity and metallicity
dispersions show that half of the stream progenitors were dwarf galaxies (DGs),
while the other half originated from disrupted globular clusters (GCs). Based
on the mean metallicities of the streams and the mass-metallicity relation, the
luminosities of the progenitors of the DG streams range between Ursa Major I
and Carina ($-9.5lesssim M_Vlesssim-5.5$). Four of the six GC streams have
mean metallicities of [Fe/H] $< -2$, more metal-poor than typical Milky Way
(MW) GCs at similar distances. Interestingly, the 300S and Jet GC streams are
the only streams on retrograde orbits in our dozen stream sample. Finally, we
compare the orbital properties of the streams with known DGs and GCs in the MW,
finding several possible associations. Some streams appear to have been
accreted with the recently discovered Gaia-Enceladus-Sausage system, and others
suggest that GCs were formed in and accreted together with the progenitors of
DG streams whose stellar masses are similar to Draco to Carina ($sim10^5-10^6
M_odot$).

We report the kinematic, orbital, and chemical properties of 12 stellar
streams with no evident progenitors, using line-of-sight velocities and
metallicities from the Southern Stellar Stream Spectroscopic Survey ($S^5$),
proper motions from Gaia EDR3, and distances derived from distance tracers or
the literature. This data set provides the largest homogeneously analyzed set
of streams with full 6D kinematics and metallicities. All streams have
heliocentric distances between ${sim}10-50$ kpc. The velocity and metallicity
dispersions show that half of the stream progenitors were dwarf galaxies (DGs),
while the other half originated from disrupted globular clusters (GCs). Based
on the mean metallicities of the streams and the mass-metallicity relation, the
luminosities of the progenitors of the DG streams range between Ursa Major I
and Carina ($-9.5lesssim M_Vlesssim-5.5$). Four of the six GC streams have
mean metallicities of [Fe/H] $< -2$, more metal-poor than typical Milky Way
(MW) GCs at similar distances. Interestingly, the 300S and Jet GC streams are
the only streams on retrograde orbits in our dozen stream sample. Finally, we
compare the orbital properties of the streams with known DGs and GCs in the MW,
finding several possible associations. Some streams appear to have been
accreted with the recently discovered Gaia-Enceladus-Sausage system, and others
suggest that GCs were formed in and accreted together with the progenitors of
DG streams whose stellar masses are similar to Draco to Carina ($sim10^5-10^6
M_odot$).

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