Stellar streams around the Magellanic Clouds in 4D

Navarrete, C.; Belokurov, Vasily; Catelan, M.; Jethwa, Prashin; Koposov, S. E.; Carballo‐Bello, J. A.; Jofré, P.; Erkal, Denis; Duffau, S.; Corral-Santana, J. M.

doi:10.1093/mnras/sty3347

Cited by 11 publications

(12 citation statements)

References 66 publications

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“…This difference is to be expected, as each of the above methods provides the total infall mass of the LMC, including its dark halo. In contrast, the MagES field considered here, despite being at a greater distance from the LMC COM than most previous kinematic estimates, is still located well within the LMC dark halo: studies such as Navarrete et al (2019) or Munoz et al (2006) have found likely LMC-associated stars at distances almost three times greater than field 18. As such, the enclosed mass derived simply does not capture a significant fraction of the total LMC mass.…”

Section: Lmc Mass Estimatecontrasting

confidence: 66%

“…As such, the enclosed mass derived simply does not capture a significant fraction of the total LMC mass. If, however, the assumption is made that the LMC rotation curve remains flat out to 29kpc (the furthest distance LMC-associated stars have been found to date as per Navarrete et al 2019), and that the LMC is embedded in a typical dark matter halo, the inferred LMC enclosed mass would be (1.1±0.2)×10 11 M , which is more in line with total infall mass estimates, and the mass calculated under similar assumptions in Wan et al (2020). In this scenario, the implied M/L ratio of the LMC rises to 58.2±6.8 M /L .…”

Section: Lmc Mass Estimatementioning

confidence: 99%

“…SMC debris has been found in not only the bridge region between the Clouds (e.g. Carrera et al 2017), but also at large distances from the Clouds (Navarrete et al 2019), and even within the LMC itself (Olsen et al 2011).…”

Section: Introductionmentioning

confidence: 99%

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The Magellanic Edges Survey I: Description and first results

Cullinane

Mackey

Costa

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We present an overview of, and first science results from, the Magellanic Edges Survey (MagES), an ongoing spectroscopic survey mapping the kinematics of red clump and red giant branch stars in the highly substructured periphery of the Magellanic Clouds. In conjunction with Gaia astrometry, MagES yields a sample of ~7000 stars with individual 3D velocities that probes larger galactocentric radii than most previous studies. We outline our target selection, observation strategy, data reduction and analysis procedures, and present results for two fields in the northern outskirts (>10○ on-sky from the centre) of the Large Magellanic Cloud (LMC). One field, located in the vicinity of an arm-like overdensity, displays apparent signatures of perturbation away from an equilibrium disk model. This includes a large radial velocity dispersion in the LMC disk plane, and an asymmetric line-of-sight velocity distribution indicative of motions vertically out of the disk plane for some stars. The second field reveals 3D kinematics consistent with an equilibrium disk, and yields Vcirc = 87.7 ± 8.0km s−1 at a radial distance of ~10.5kpc from the LMC centre. This leads to an enclosed mass estimate for the LMC at this radius of (1.8 ± 0.3) × 1010M⊙.

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Section: Lmc Mass Estimatecontrasting

confidence: 66%

Section: Lmc Mass Estimatementioning

confidence: 99%

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The Magellanic Edges Survey I: Description and first results

Cullinane

Mackey

Costa

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…This mass agrees with other estimations based on stellar dynamics, e.g., van der Marel & Kallivayalil (2014); van der Marel et al (2002). van der Marel & Kallivayalil (2014) estimated the tidal radius to be 22.3±5.2 kpc, whilst Navarrete et al (2019) found stars that match the expected velocity gradient for the LMC halo extending up to 29 kpc away from the LMC centre. If we assume that the circular velocity remains constant out to 30 kpc, the mass within tidal radius is (1.06±0.32)×10 11 M .…”

Section: Massmentioning

confidence: 93%

A SkyMapper view of the Large Magellanic Cloud: the dynamics of stellar populations

Wan

Guglielmo

Lewis

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We present the first SkyMapper stellar population analysis of the Large Magellanic Cloud (hereafter LMC),including the identification of 3578 candidate Carbon Stars through their extremely red g − r colours. Coupled with Gaia astrometry, we analyse the distribution and kinematics of this Carbon Star population, finding the LMC to be centred at (R.A., Dec.) = (80.90 • ±0.29, −68.74 • ±0.12), with a bulk proper motion of (µ α , µ δ ) = (1.878 ± 0.007, 0.293 ± 0.018) mas yr −1 and a disk inclination of i = 25.6 • ± 1.1 at position angle θ = 135.6 • ± 3.3 • . We complement this study with the identification and analysis of additional stellar populations, finding that the dynamical centre for Red Giant Branch (RGB) stars is similar to that seen for the Carbon Stars, whereas for young stars the dynamical centre is significantly offset from the older populations. This potentially indicates that the young stars were formed as a consequence of a strong tidal interaction, probably with the Small Magellanic Cloud (SMC). In terms of internal dynamics, the tangential velocity profile increases linearly within ∼ 3 kpc, after which it maintains an approximately constant value of V rot = 83.6 ± 1.7 km s −1 until ∼ 7 kpc. With an asymmetric drift correction, we estimate the mass within 7 kpc to be M LMC (< 7 kpc) = (2.5±0.1)×10 10 M and within the tidal radius (∼ 30 kpc) to be M LMC (< 30 kpc) = (1.06 ± 0.32) × 10 11 M , consistent with other recent measurements.

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“…We fit Sersic profiles to the Hα, Hγ and Hβ Balmer lines (see Navarrete et al 2019 eqn. 1), and the radial velocities are calculated by fitting all 3 lines simultaneously.…”

Section: Radial Velocities and A-type Star Classificationmentioning

confidence: 99%

The Pisces Plume and the Magellanic wake

Belokurov

Deason

Erkal

et al. 2019

Monthly Notices of the Royal Astronomical Society: Letters

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Using RR Lyrae stars in the Gaia Data Release 2 and Pan-STARRS1 we study the properties of the Pisces Overdensity, a diffuse sub-structure in the outer halo of the Milky Way. We show that along the line of sight, Pisces appears as a broad and long plume of stars stretching from 40 to 110 kpc with a steep distance gradient. On the sky Pisces's elongated shape is aligned with the Magellanic Stream. Using follow-up VLT FORS2 spectroscopy, we have measured the velocity distribution of the Pisces candidate member stars and have shown it to be as broad as that of the Galactic halo but offset to negative velocities. Using a suite of numerical simulations, we demonstrate that the structure has many properties in common with the predicted behaviour of the Magellanic wake, i.e. the Galactic halo overdensity induced by the in-fall of the Magellanic Clouds.

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Stellar streams around the Magellanic Clouds in 4D

Cited by 11 publications

References 66 publications

The Magellanic Edges Survey I: Description and first results

The Magellanic Edges Survey I: Description and first results

A SkyMapper view of the Large Magellanic Cloud: the dynamics of stellar populations

The Pisces Plume and the Magellanic wake

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