S5: The Orbital and Chemical Properties of One Dozen Stellar Streams

S5 Collaboration; Ting S. Li; Alexander P. Ji; Andrew B. Pace; Denis Erkal; Sergey E. Koposov; Nora Shipp; Gary S.  Da Costa; Lara R. Cullinane; Kyler Kuehn; Geraint F Lewis; Dougal Mackey; Jeffrey D. Simpson; Daniel B. Zucker; Peter S. Ferguson; Sarah L. Martell; Joss Bland-Hawthorn; Eduardo Balbinot; Kiyan Tavangar; Alex Drlica-Wagner; Gayandhi M. De Silva; Joshua D. Simon

doi:10.3847/1538-4357/ac46d3

S5: The Orbital and Chemical Properties of One Dozen Stellar Streams

S5 Collaboration, Ting S. Li^*, Alexander P. Ji, Andrew B. Pace, Denis Erkal, Sergey E. Koposov, Nora Shipp, Gary S. Da Costa, Lara R. Cullinane, Kyler Kuehn, Geraint F Lewis, Dougal Mackey, Jeffrey D. Simpson, Daniel B. Zucker, Peter S. Ferguson, Sarah L. Martell, Joss Bland-Hawthorn, Eduardo Balbinot, Kiyan Tavangar, Alex Drlica-WagnerGayandhi M. De Silva, Joshua D. Simon

^*Corresponding author for this work

School of Physics and Astronomy

Research output: Contribution to journal › Article › peer-review

Abstract / Description of output

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 (S5), 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 ~10 - 50 kpc. The velocity and metallicity dispersions show that half of the stream progenitors were disrupted dwarf galaxies (DGs), while the other half originated from disrupted globular clusters (GCs), hereafter referred to as DG and GC streams. Based on the mean metallicities of the streams and the mass-metallicity
relation, the luminosities of the progenitors of the DG streams range between Carina and Ursa Major I (-9.5 ≤ MV≤ - 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 (~ 105 - 106M).

Original language	English
Article number	30
Pages (from-to)	1-18
Number of pages	18
Journal	Astrophysical Journal
Volume	928
Issue number	1
DOIs	https://doi.org/10.3847/1538-4357/ac46d3
Publication status	Published - 24 Mar 2022

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S5 Collaboration, Li, T. S., Ji, A. P., Pace, A. B., Erkal, D., Koposov, S. E., Shipp, N., Da Costa, G. S., Cullinane, L. R., Kuehn, K., Lewis, G. F., Mackey, D., Simpson, J. D., Zucker, D. B., Ferguson, P. S., Martell, S. L., Bland-Hawthorn, J., Balbinot, E., Tavangar, K., ... Simon, J. D. (2022). S5: The Orbital and Chemical Properties of One Dozen Stellar Streams. Astrophysical Journal, 928(1), 1-18. Article 30. https://doi.org/10.3847/1538-4357/ac46d3

@article{c1f6829123d64016babb8a50ed647731,

title = "S5: The Orbital and Chemical Properties of One Dozen Stellar Streams",

abstract = "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 (S5), 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 ~10 - 50 kpc. The velocity and metallicity dispersions show that half of the stream progenitors were disrupted dwarf galaxies (DGs), while the other half originated from disrupted globular clusters (GCs), hereafter referred to as DG and GC streams. Based on the mean metallicities of the streams and the mass-metallicityrelation, the luminosities of the progenitors of the DG streams range between Carina and Ursa Major I (-9.5 ≤ MV≤ - 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 (~ 105 - 106M).",

author = "{S5 Collaboration} and Li, {Ting S.} and Ji, {Alexander P.} and Pace, {Andrew B.} and Denis Erkal and Koposov, {Sergey E.} and Nora Shipp and {Da Costa}, {Gary S.} and Cullinane, {Lara R.} and Kyler Kuehn and Lewis, {Geraint F} and Dougal Mackey and Simpson, {Jeffrey D.} and Zucker, {Daniel B.} and Ferguson, {Peter S.} and Martell, {Sarah L.} and Joss Bland-Hawthorn and Eduardo Balbinot and Kiyan Tavangar and Alex Drlica-Wagner and {De Silva}, {Gayandhi M.} and Simon, {Joshua D.}",

note = "Funding Information: The authors would like to thank the referee for detailed comments that helped clarify the paper. T.S.L. would like to thank Ray Carlberg, Rohan Naidu, Ted Mackereth, Zhen Yuan, Nondh Panithanpaisal, and Robyn Sanderson for helpful discussion. T.S.L. also would like to thank Jiang Chang for sharing his Cetus model for comparison with our Palca data. T.S.L. is supported by NASA through Hubble Fellowship grant HST-HF2-51439.001 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. A.B.P. is supported by NSF grant AST-1813881. S.L.M., J.D.S., and D.B.Z. acknowledge the support of the Australian Research Council through Discovery Project grant DP180101791, and this research has also been supported in part by the Australian Research Council Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), through project number CE170100013. S.L.M. and J.D.S. are supported by the UNSW Scientia Fellowship program. EB acknowledges support from a Vici grant from the Netherlands Organization for Scientific Research (NWO). A.P.J. acknowledges a Carnegie Fellowship and support from the Thacher Research Award in Astronomy. Funding Information: This paper made use of the Whole Sky Database (wsdb) created by Sergey Koposov and maintained at the Institute of Astronomy, Cambridge by Sergey Koposov, Vasily Belokurov, and Wyn Evans with financial support from the Science & Technology Facilities Council (STFC) and the European Research Council (ERC). Funding Information: This work has made use of data from the European Space Agency (ESA) mission Gaia ( https://www.cosmos.esa.int/gaia ), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium ). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. Publisher Copyright: {\textcopyright} 2022. The Author(s). Published by the American Astronomical Society.",

year = "2022",

month = mar,

day = "24",

doi = "10.3847/1538-4357/ac46d3",

language = "English",

volume = "928",

pages = "1--18",

journal = "Astrophysical Journal",

issn = "0004-637X",

publisher = "IOP Publishing",

number = "1",

}

S5 Collaboration, Li, TS, Ji, AP, Pace, AB, Erkal, D, Koposov, SE, Shipp, N, Da Costa, GS, Cullinane, LR, Kuehn, K, Lewis, GF, Mackey, D, Simpson, JD, Zucker, DB, Ferguson, PS, Martell, SL, Bland-Hawthorn, J, Balbinot, E, Tavangar, K, Drlica-Wagner, A, De Silva, GM & Simon, JD 2022, 'S5: The Orbital and Chemical Properties of One Dozen Stellar Streams', Astrophysical Journal, vol. 928, no. 1, 30, pp. 1-18. https://doi.org/10.3847/1538-4357/ac46d3

TY - JOUR

T1 - S5: The Orbital and Chemical Properties of One Dozen Stellar Streams

AU - S5 Collaboration

AU - Li, Ting S.

AU - Ji, Alexander P.

AU - Pace, Andrew B.

AU - Erkal, Denis

AU - Koposov, Sergey E.

AU - Shipp, Nora

AU - Da Costa, Gary S.

AU - Cullinane, Lara R.

AU - Kuehn, Kyler

AU - Lewis, Geraint F

AU - Mackey, Dougal

AU - Simpson, Jeffrey D.

AU - Zucker, Daniel B.

AU - Ferguson, Peter S.

AU - Martell, Sarah L.

AU - Bland-Hawthorn, Joss

AU - Balbinot, Eduardo

AU - Tavangar, Kiyan

AU - Drlica-Wagner, Alex

AU - De Silva, Gayandhi M.

AU - Simon, Joshua D.

N1 - Funding Information: The authors would like to thank the referee for detailed comments that helped clarify the paper. T.S.L. would like to thank Ray Carlberg, Rohan Naidu, Ted Mackereth, Zhen Yuan, Nondh Panithanpaisal, and Robyn Sanderson for helpful discussion. T.S.L. also would like to thank Jiang Chang for sharing his Cetus model for comparison with our Palca data. T.S.L. is supported by NASA through Hubble Fellowship grant HST-HF2-51439.001 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. A.B.P. is supported by NSF grant AST-1813881. S.L.M., J.D.S., and D.B.Z. acknowledge the support of the Australian Research Council through Discovery Project grant DP180101791, and this research has also been supported in part by the Australian Research Council Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), through project number CE170100013. S.L.M. and J.D.S. are supported by the UNSW Scientia Fellowship program. EB acknowledges support from a Vici grant from the Netherlands Organization for Scientific Research (NWO). A.P.J. acknowledges a Carnegie Fellowship and support from the Thacher Research Award in Astronomy. Funding Information: This paper made use of the Whole Sky Database (wsdb) created by Sergey Koposov and maintained at the Institute of Astronomy, Cambridge by Sergey Koposov, Vasily Belokurov, and Wyn Evans with financial support from the Science & Technology Facilities Council (STFC) and the European Research Council (ERC). Funding Information: This work has made use of data from the European Space Agency (ESA) mission Gaia ( https://www.cosmos.esa.int/gaia ), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium ). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. Publisher Copyright: © 2022. The Author(s). Published by the American Astronomical Society.

PY - 2022/3/24

Y1 - 2022/3/24

N2 - 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 (S5), 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 ~10 - 50 kpc. The velocity and metallicity dispersions show that half of the stream progenitors were disrupted dwarf galaxies (DGs), while the other half originated from disrupted globular clusters (GCs), hereafter referred to as DG and GC streams. Based on the mean metallicities of the streams and the mass-metallicityrelation, the luminosities of the progenitors of the DG streams range between Carina and Ursa Major I (-9.5 ≤ MV≤ - 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 (~ 105 - 106M).

AB - 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 (S5), 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 ~10 - 50 kpc. The velocity and metallicity dispersions show that half of the stream progenitors were disrupted dwarf galaxies (DGs), while the other half originated from disrupted globular clusters (GCs), hereafter referred to as DG and GC streams. Based on the mean metallicities of the streams and the mass-metallicityrelation, the luminosities of the progenitors of the DG streams range between Carina and Ursa Major I (-9.5 ≤ MV≤ - 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 (~ 105 - 106M).

U2 - 10.3847/1538-4357/ac46d3

DO - 10.3847/1538-4357/ac46d3

M3 - Article

SN - 0004-637X

VL - 928

SP - 1

EP - 18

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 1

M1 - 30

ER -

S5: The Orbital and Chemical Properties of One Dozen Stellar Streams

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