Modelling the Tucana III stream - a close passage with the LMC

D. Erkal; T. S. Li; S. E. Koposov; V. Belokurov; E. Balbinot; K. Bechtol; B. Buncher; A. Drlica-Wagner; K. Kuehn; J. L. Marshall; C. E. Martínez-Vázquez; A. B. Pace; N. Shipp; J. D. Simon; K. M. Stringer; A. K. Vivas; R. H. Wechsler; B. Yanny; F. B. Abdalla; S. Allam; J. Annis; S. Avila; E. Bertin; D. Brooks; E. Buckley-Geer; D. L. Burke; A. Carnero Rosell; M. Carrasco Kind; J. Carretero; C. B. D'Andrea; L. N. da Costa; C. Davis; J. De Vicente; P. Doel; T. F. Eifler; A. E. Evrard; B. Flaugher; J. Frieman; J. García-Bellido; E. Gaztanaga; D. W. Gerdes; D. Gruen; R. A. Gruendl; J. Gschwend; G. Gutierrez; W. G. Hartley; D. L. Hollowood; K. Honscheid; D. J. James; E. Krause; M. A.G. Maia; M. March; F. Menanteau; R. Miquel; R. L.C. Ogando; A. A. Plazas; E. Sanchez; B. Santiago; V. Scarpine; R. Schindler; I. Sevilla-Noarbe; M. Smith; R. C. Smith; M. Soares-Santos; F. Sobreira; E. Suchyta; M. E.C. Swanson; G. Tarle; D. L. Tucker; A. R. Walker

doi:10.1093/mnras/sty2518

Modelling the Tucana III stream - a close passage with the LMC

D. Erkal, T. S. Li, S. E. Koposov, V. Belokurov, E. Balbinot, K. Bechtol, B. Buncher, A. Drlica-Wagner, K. Kuehn, J. L. Marshall, C. E. Martínez-Vázquez, A. B. Pace, N. Shipp, J. D. Simon, K. M. Stringer, A. K. Vivas, R. H. Wechsler, B. Yanny, F. B. Abdalla, S. AllamJ. Annis, S. Avila, E. Bertin, D. Brooks, E. Buckley-Geer, D. L. Burke, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, C. B. D'Andrea, L. N. da Costa, C. Davis, J. De Vicente, P. Doel, T. F. Eifler, A. E. Evrard, B. Flaugher, J. Frieman, J. García-Bellido, E. Gaztanaga, D. W. Gerdes, D. Gruen, R. A. Gruendl, J. Gschwend, G. Gutierrez, W. G. Hartley, D. L. Hollowood, K. Honscheid, D. J. James, E. Krause, M. A.G. Maia, M. March, F. Menanteau, R. Miquel, R. L.C. Ogando, A. A. Plazas, E. Sanchez, B. Santiago, V. Scarpine, R. Schindler, I. Sevilla-Noarbe, M. Smith, R. C. Smith, M. Soares-Santos, F. Sobreira, E. Suchyta, M. E.C. Swanson, G. Tarle, D. L. Tucker, A. R. Walker

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Abstract

We present results of the first dynamical stream fits to the recently discovered Tucana III stream. These fits assume a fixed Milky Way potential and give proper motion predictions, which can be tested with the upcoming Gaia Data Release 2 (DR2). These fits reveal that Tucana III is on an eccentric orbit around the Milky Way and, more interestingly, that Tucana III passed within 15 kpc of the Large Magellanic Cloud (LMC) approximately 75 Myr ago. Given this close passage, we fit the Tucana III stream in the combined presence of the Milky Way and the LMC. We find that the predicted proper motions depend on the assumed mass of the LMC and that the LMC can induce a substantial proper motion perpendicular to the stream track. A detection of this misalignment will directly probe the extent of the LMC's influence on our Galaxy, and has implications for nearly all methods which attempt to constraint the Milky Way potential. Such a measurement will be possible with the upcoming Gaia DR2, allowing for a measurement of the LMC's mass.

Original language	English
Pages (from-to)	3148-3159
Number of pages	12
Journal	Monthly Notices of the Royal Astronomical Society
Volume	481
Issue number	3
DOIs	https://doi.org/10.1093/mnras/sty2518
State	Published - Dec 11 2018

Funding

The DES data management system is supported by the National Science Foundation under grant numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2015-71825, ESP2015-66861, FPA2015-68048, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAAS-TRO), through project number CE110001020, and the Brazilian In-stituto Nacional de Ciência e Tecnologia (INCT) e-Universe (CNPq grant 465376/2014-2). Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundac¸ão Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desen-volvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovac¸ão, the Deutsche Forschungsgemeinschaft, and the Collaborating Institutions in the DES. DE thanks Jorge Peñarrubia for insightful discussions on the LMC and Victor Debattista for helpful discussions on the bar. DE and VB acknowledge that the research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Programme (FP/2007-2013)/ERC grant agreement no. 308024. SK is supported by National Science Foundation grant AST-1813881. EB acknowledges financial support from the European Research Council (StG-335936). ABP acknowledges generous support from the George P. and Cynthia Woods Institute for Fundamental Physics and Astronomy at Texas A&M University. We thank the anonymous referee for useful comments which improved the clarity of this work. DE thanks Jorge Peñarrubia for insightful discussions on the LMC and Victor Debattista for helpful discussions on the bar. DE and VB acknowledge that the research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Programme (FP/2007-2013)/ERC grant agreement no. 308024. SK is supported by National Science Foundation grant AST-1813881. EB acknowledges financial support from the European Research Council (StG-335936). ABP acknowledges generous support from the George P. and Cynthia Woods Institute for Fundamental Physics and Astronomy at Texas A&M University.We thank the anonymous referee for useful comments which improved the clarity of this work. This paper has gone through internal review by the DES collaboration. Based on data obtained at the Australian Astronomical Telescope via program A/2016A/26. We acknowledge the traditional owners of the land on which the AAT stands, the Gamilaraay people, and pay our respects to elders past and present. Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, theMinistry of Science and Education of Spain, the Science and Technology FacilitiesCouncil of theUnitedKingdom, theHigher Education Funding Council for England, theNationalCenter for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft, and the Collaborating Institutions in the DES. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciències de l'Espai (IEEC/CSIC), the Institut de Física d'Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universit ät München and the associated Excellence Cluster Universe, the University of Michigan, the National Optical Astronomy Observatory, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, TexasA&MUniversity, and the OzDESMembership Consortium. Based in part on observations at Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES data management system is supported by the National Science Foundation under grant numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2015-71825, ESP2015-66861, FPA2015-68048, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Program (FP7/2007-2013) includingERCgrant agreements 240672, 291329, and 306478.We acknowledge support from the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020, and the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) e-Universe (CNPq grant 465376/2014-2). This manuscript has been authored by Fermi Research Alliance, LLC under contract no. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics. TheUnited StatesGovernment retains and the publisher, by accepting the article for publication, acknowledges that the United States Government retains a non-exclusive, paid-up, irrevocable, world-wide license to publish or reproduce the published form of this manuscript, or allow others to do so, for United States Government purposes. This manuscript has been authored by Fermi Research Alliance, LLC under contract no. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics. The United States Government retains and the publisher, by accepting the article for publication, acknowledges that the United States Government retains a non-exclusive, paid-up, irrevocable, world-wide license to publish or reproduce the published form of this manuscript, or allow others to do so, for United States Government purposes.

Funders	Funder number
Australian Research Council Centre of Excellence for All-sky Astrophysics
CAAS-TRO	CE110001020
Conselho Nacional de Desen-volvimento Científico e Tecnológico
European Union’s Seventh Framework Program
FP7/2007
Fermi Research Alliance, LLC	DE-AC02-07CH11359
INCT
Kavli Institute of Cosmological Physics at the University of Chicago
Ministry of Science and Education of Spain
Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University
National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign
U.S. National Science Foundation
National Science Foundation	StG-335936, 1813881, AST-1138766, AST-1813881, AST-1536171
U.S. Department of Energy
Office of Science
High Energy Physics
Seventh Framework Programme	308024, 1138766, 240672, 306478, 335936, 291329
Higher Education Funding Council for England
Center for Cosmology and Astroparticle Physics, Ohio State University
Instituto Nacional de Ciência e Tecnologia Midas
Science and Technology Facilities Council
European Commission
European Research Council
Deutsche Forschungsgemeinschaft
Generalitat de Catalunya
Ministerio de Economía y Competitividad	SEV-2016-0588, SEV-2016-0597, ESP2015-66861, MDM-2015-0509, FPA2015-68048, AYA2015-71825
Conselho Nacional de Desenvolvimento Científico e Tecnológico	465376/2014-2
Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro
Financiadora de Estudos e Projetos
Seventh Framework Programme	FP/2007-2013
Ministério da Ciência e Tecnologia
European Regional Development Fund
National Science Foundation	1536171

Keywords

Galaxies: dwarf
Galaxy: evolution
Galaxy: kinematics and dynamics

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10.1093/mnras/sty2518

Cite this

Erkal, D., Li, T. S., Koposov, S. E., Belokurov, V., Balbinot, E., Bechtol, K., Buncher, B., Drlica-Wagner, A., Kuehn, K., Marshall, J. L., Martínez-Vázquez, C. E., Pace, A. B., Shipp, N., Simon, J. D., Stringer, K. M., Vivas, A. K., Wechsler, R. H., Yanny, B., Abdalla, F. B., ... Walker, A. R. (2018). Modelling the Tucana III stream - a close passage with the LMC. Monthly Notices of the Royal Astronomical Society, 481(3), 3148-3159. https://doi.org/10.1093/mnras/sty2518

@article{63e4473dc6a044a6acceb60a92ba1b57,

title = "Modelling the Tucana III stream - a close passage with the LMC",

abstract = "We present results of the first dynamical stream fits to the recently discovered Tucana III stream. These fits assume a fixed Milky Way potential and give proper motion predictions, which can be tested with the upcoming Gaia Data Release 2 (DR2). These fits reveal that Tucana III is on an eccentric orbit around the Milky Way and, more interestingly, that Tucana III passed within 15 kpc of the Large Magellanic Cloud (LMC) approximately 75 Myr ago. Given this close passage, we fit the Tucana III stream in the combined presence of the Milky Way and the LMC. We find that the predicted proper motions depend on the assumed mass of the LMC and that the LMC can induce a substantial proper motion perpendicular to the stream track. A detection of this misalignment will directly probe the extent of the LMC's influence on our Galaxy, and has implications for nearly all methods which attempt to constraint the Milky Way potential. Such a measurement will be possible with the upcoming Gaia DR2, allowing for a measurement of the LMC's mass.",

keywords = "Galaxies: dwarf, Galaxy: evolution, Galaxy: kinematics and dynamics",

author = "D. Erkal and Li, {T. S.} and Koposov, {S. E.} and V. Belokurov and E. Balbinot and K. Bechtol and B. Buncher and A. Drlica-Wagner and K. Kuehn and Marshall, {J. L.} and Mart{\'i}nez-V{\'a}zquez, {C. E.} and Pace, {A. B.} and N. Shipp and Simon, {J. D.} and Stringer, {K. M.} and Vivas, {A. K.} and Wechsler, {R. H.} and B. Yanny and Abdalla, {F. B.} and S. Allam and J. Annis and S. Avila and E. Bertin and D. Brooks and E. Buckley-Geer and Burke, {D. L.} and Rosell, {A. Carnero} and Kind, {M. Carrasco} and J. Carretero and D'Andrea, {C. B.} and {da Costa}, {L. N.} and C. Davis and {De Vicente}, J. and P. Doel and Eifler, {T. F.} and Evrard, {A. E.} and B. Flaugher and J. Frieman and J. Garc{\'i}a-Bellido and E. Gaztanaga and Gerdes, {D. W.} and D. Gruen and Gruendl, {R. A.} and J. Gschwend and G. Gutierrez and Hartley, {W. G.} and Hollowood, {D. L.} and K. Honscheid and James, {D. J.} and E. Krause and Maia, {M. A.G.} and M. March and F. Menanteau and R. Miquel and Ogando, {R. L.C.} and Plazas, {A. A.} and E. Sanchez and B. Santiago and V. Scarpine and R. Schindler and I. Sevilla-Noarbe and M. Smith and Smith, {R. C.} and M. Soares-Santos and F. Sobreira and E. Suchyta and Swanson, {M. E.C.} and G. Tarle and Tucker, {D. L.} and Walker, {A. R.}",

note = "Publisher Copyright: {\textcopyright} 2018 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society.",

year = "2018",

month = dec,

day = "11",

doi = "10.1093/mnras/sty2518",

language = "English",

volume = "481",

pages = "3148--3159",

journal = "Monthly Notices of the Royal Astronomical Society",

issn = "0035-8711",

publisher = "Oxford University Press",

number = "3",

}

Erkal, D, Li, TS, Koposov, SE, Belokurov, V, Balbinot, E, Bechtol, K, Buncher, B, Drlica-Wagner, A, Kuehn, K, Marshall, JL, Martínez-Vázquez, CE, Pace, AB, Shipp, N, Simon, JD, Stringer, KM, Vivas, AK, Wechsler, RH, Yanny, B, Abdalla, FB, Allam, S, Annis, J, Avila, S, Bertin, E, Brooks, D, Buckley-Geer, E, Burke, DL, Rosell, AC, Kind, MC, Carretero, J, D'Andrea, CB, da Costa, LN, Davis, C, De Vicente, J, Doel, P, Eifler, TF, Evrard, AE, Flaugher, B, Frieman, J, García-Bellido, J, Gaztanaga, E, Gerdes, DW, Gruen, D, Gruendl, RA, Gschwend, J, Gutierrez, G, Hartley, WG, Hollowood, DL, Honscheid, K, James, DJ, Krause, E, Maia, MAG, March, M, Menanteau, F, Miquel, R, Ogando, RLC, Plazas, AA, Sanchez, E, Santiago, B, Scarpine, V, Schindler, R, Sevilla-Noarbe, I, Smith, M, Smith, RC, Soares-Santos, M, Sobreira, F, Suchyta, E, Swanson, MEC, Tarle, G, Tucker, DL & Walker, AR 2018, 'Modelling the Tucana III stream - a close passage with the LMC', Monthly Notices of the Royal Astronomical Society, vol. 481, no. 3, pp. 3148-3159. https://doi.org/10.1093/mnras/sty2518

TY - JOUR

T1 - Modelling the Tucana III stream - a close passage with the LMC

AU - Erkal, D.

AU - Li, T. S.

AU - Koposov, S. E.

AU - Belokurov, V.

AU - Balbinot, E.

AU - Bechtol, K.

AU - Buncher, B.

AU - Drlica-Wagner, A.

AU - Kuehn, K.

AU - Marshall, J. L.

AU - Martínez-Vázquez, C. E.

AU - Pace, A. B.

AU - Shipp, N.

AU - Simon, J. D.

AU - Stringer, K. M.

AU - Vivas, A. K.

AU - Wechsler, R. H.

AU - Yanny, B.

AU - Abdalla, F. B.

AU - Allam, S.

AU - Annis, J.

AU - Avila, S.

AU - Bertin, E.

AU - Brooks, D.

AU - Buckley-Geer, E.

AU - Burke, D. L.

AU - Rosell, A. Carnero

AU - Kind, M. Carrasco

AU - Carretero, J.

AU - D'Andrea, C. B.

AU - da Costa, L. N.

AU - Davis, C.

AU - De Vicente, J.

AU - Doel, P.

AU - Eifler, T. F.

AU - Evrard, A. E.

AU - Flaugher, B.

AU - Frieman, J.

AU - García-Bellido, J.

AU - Gaztanaga, E.

AU - Gerdes, D. W.

AU - Gruen, D.

AU - Gruendl, R. A.

AU - Gschwend, J.

AU - Gutierrez, G.

AU - Hartley, W. G.

AU - Hollowood, D. L.

AU - Honscheid, K.

AU - James, D. J.

AU - Krause, E.

AU - Maia, M. A.G.

AU - March, M.

AU - Menanteau, F.

AU - Miquel, R.

AU - Ogando, R. L.C.

AU - Plazas, A. A.

AU - Sanchez, E.

AU - Santiago, B.

AU - Scarpine, V.

AU - Schindler, R.

AU - Sevilla-Noarbe, I.

AU - Smith, M.

AU - Smith, R. C.

AU - Soares-Santos, M.

AU - Sobreira, F.

AU - Suchyta, E.

AU - Swanson, M. E.C.

AU - Tarle, G.

AU - Tucker, D. L.

AU - Walker, A. R.

PY - 2018/12/11

Y1 - 2018/12/11

N2 - We present results of the first dynamical stream fits to the recently discovered Tucana III stream. These fits assume a fixed Milky Way potential and give proper motion predictions, which can be tested with the upcoming Gaia Data Release 2 (DR2). These fits reveal that Tucana III is on an eccentric orbit around the Milky Way and, more interestingly, that Tucana III passed within 15 kpc of the Large Magellanic Cloud (LMC) approximately 75 Myr ago. Given this close passage, we fit the Tucana III stream in the combined presence of the Milky Way and the LMC. We find that the predicted proper motions depend on the assumed mass of the LMC and that the LMC can induce a substantial proper motion perpendicular to the stream track. A detection of this misalignment will directly probe the extent of the LMC's influence on our Galaxy, and has implications for nearly all methods which attempt to constraint the Milky Way potential. Such a measurement will be possible with the upcoming Gaia DR2, allowing for a measurement of the LMC's mass.

AB - We present results of the first dynamical stream fits to the recently discovered Tucana III stream. These fits assume a fixed Milky Way potential and give proper motion predictions, which can be tested with the upcoming Gaia Data Release 2 (DR2). These fits reveal that Tucana III is on an eccentric orbit around the Milky Way and, more interestingly, that Tucana III passed within 15 kpc of the Large Magellanic Cloud (LMC) approximately 75 Myr ago. Given this close passage, we fit the Tucana III stream in the combined presence of the Milky Way and the LMC. We find that the predicted proper motions depend on the assumed mass of the LMC and that the LMC can induce a substantial proper motion perpendicular to the stream track. A detection of this misalignment will directly probe the extent of the LMC's influence on our Galaxy, and has implications for nearly all methods which attempt to constraint the Milky Way potential. Such a measurement will be possible with the upcoming Gaia DR2, allowing for a measurement of the LMC's mass.

KW - Galaxies: dwarf

KW - Galaxy: evolution

KW - Galaxy: kinematics and dynamics

UR - http://www.scopus.com/inward/record.url?scp=85054220967&partnerID=8YFLogxK

U2 - 10.1093/mnras/sty2518

DO - 10.1093/mnras/sty2518

M3 - Article

AN - SCOPUS:85054220967

SN - 0035-8711

VL - 481

SP - 3148

EP - 3159

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

IS - 3

ER -

Modelling the Tucana III stream - a close passage with the LMC

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