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

Erkal, Denis, 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, Allam, S, Annis, J, Avila, S, Bertin, E, Brooks, D, Buckley-Geer, E, Burke, D L, Rosell, A Carnero, Kind, M Carrasco, Carretero, J, D’Andrea, C B, da Costa, L N, Davis, C, De Vicente, J, Doel, P, Eifler, T F, Evrard, A E, Flaugher, B, Frieman, J, García-Bellido, J, Gaztanaga, E, Gerdes, D W, Gruen, D, Gruendl, R A, Gschwend, J, Gutierrez, G, Hartley, W G, Hollowood, D L, Honscheid, K, James, D J, Krause, E, Maia, M A G, March, M, Menanteau, F, Miquel, R, Ogando, R L C, Plazas, A A, Sanchez, E, Santiago, B, Scarpine, V, Schindler, R, Sevilla-Noarbe, I, Smith, M, Smith, R C, Soares-Santos, M, Sobreira, F, Suchyta, E, Swanson, M E C, Tarle, G, Tucker, D L and Walker, A R (2018) Modelling the Tucana III stream - a close passage with the LMC Monthly Notices of the Royal Astronomical Society, 481 (3). pp. 3148-3159.

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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. 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.

Item Type: Article
Divisions : Faculty of Engineering and Physical Sciences > Physics
Authors :
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
Allam, S
Annis, J
Avila, S
Bertin, E
Brooks, D
Buckley-Geer, E
Burke, D L
Rosell, A Carnero
Kind, M Carrasco
Carretero, J
D’Andrea, C B
da Costa, L N
Davis, C
De Vicente, J
Doel, P
Eifler, T F
Evrard, A E
Flaugher, B
Frieman, J
García-Bellido, J
Gaztanaga, E
Gerdes, D W
Gruen, D
Gruendl, R A
Gschwend, J
Gutierrez, G
Hartley, W G
Hollowood, D L
Honscheid, K
James, D J
Krause, E
Maia, M A G
March, M
Menanteau, F
Miquel, R
Ogando, R L C
Plazas, A A
Sanchez, E
Santiago, B
Scarpine, V
Schindler, R
Sevilla-Noarbe, I
Smith, M
Smith, R C
Soares-Santos, M
Sobreira, F
Suchyta, E
Swanson, M E C
Tarle, G
Tucker, D L
Walker, A R
Date : 14 September 2018
Funders : Science and Technology Facilities Council (STFC)
DOI : 10.1093/mnras/sty2518
Copyright Disclaimer : © 2018 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (
Uncontrolled Keywords : Galaxy: kinematics and dynamics; Galaxy:evolution; Galaxies: dwarf
Depositing User : Clive Harris
Date Deposited : 20 Sep 2018 12:42
Last Modified : 27 Nov 2018 15:15

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