The Proper Motion of the Large Magellanic Cloud Using<i>HST</i>

Kallivayalil, Nitya; Marel, Roeland P. van der; Alcock, C.; Axelrod, T. S.; Cook, K. H.; Drake, A. J.; Geha, Marla

doi:10.1086/498972

Cited by 305 publications

(312 citation statements)

References 27 publications

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“…2) Next, the LMC proper motions of Table 4 are replaced by (µ α cos δ, µ δ ) = (+1.94±0.29, −0.14±0.36) mas yr −1 (Kroupa & Bastian 1997) to explore their influence on the outcome. Edelmann et al (2005); (b) Przybilla et al (2008); (c) Brown et al (2010); (d) van der Marel et al (2002); (e) Freedman et al (2001); ( f ) Kallivayalil et al (2006).…”

Section: The Hypervelocity Star He 0437-5439 Revisitedmentioning

confidence: 99%

Milky Way mass models for orbit calculations

Irrgang

Wilcox

Tucker

et al. 2013

A&A

227

339

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Context. Studying the trajectories of objects like stars, globular clusters, or satellite galaxies in the Milky Way allows the dark matter halo to be traced but requires reliable models of its gravitational potential. Aims. Realistic, yet simple and fully analytical, models have already been presented in the past. However, improved, as well as new, observational constraints have become available in the meantime, calling for a recalibration of the respective model parameters. Methods. Three widely used model potentials are revisited. By a simultaneous least-squares fit to the observed rotation curve, in-plane proper motion of Sgr A*, local mass/surface density, and the velocity dispersion in Baade's window, parameters of the potentials are brought up-to-date. The mass at large radii -in particular, that of the dark matter halo -is hereby constrained by requiring that the most extreme known halo, blue horizontal-branch star has to be bound to the Milky Way. Results. The Galactic mass models are tuned to yield a very good match to recent observations. The mass of the dark matter halo is -within the limitations of the applied models -estimated in a fully consistent way. As a first application, the trajectory of the hypervelocity star HE 0437-5439 is investigated again to check its suggested origin in the Large Magellanic Cloud (LMC). Conclusions. Despite their simplicity, the presented Milky Way mass models are very able to reproduce all observational constraints. Their analytical and simple form makes them ideally suited for fast and accurate orbit calculations. The LMC cannot be ruled out as HE 0437-5439's birthplace.

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Section: The Hypervelocity Star He 0437-5439 Revisitedmentioning

confidence: 99%

Milky Way mass models for orbit calculations

Irrgang

Wilcox

Tucker

et al. 2013

A&A

227

339

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“…Our proper motion for the SMC Red is dominated by stars in the red clump and RGB phases which typically have ages between 1 Gyr and a few Gyr. On the other hand, HST observations are dominated by main-sequence stars with a small number of SGB, red clump and RGB stars (Kallivayalil et al 2006;Piatek et al 2008).…”

Section: Comparison To Previous Measurementsmentioning

confidence: 99%

The VMC survey

Cioni

Bekki

Girardi

et al. 2016

A&A

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Aims. In this study we use multi-epoch near-infrared observations from the VISTA survey of the Magellanic Cloud system (VMC) to measure the proper motions of different stellar populations in a tile of 1.5 deg 2 in size in the direction of the Galactic globular cluster 47 Tuc. We obtain the proper motion of the cluster itself, of the Small Magellanic Cloud (SMC), and of the field Milky Way stars. Methods. Stars of the three main stellar components are selected according to their spatial distributions and their distributions in colour−magnitude diagrams. Their average coordinate displacement is computed from the difference between multiple K s -band observations for stars as faint as K s = 19 mag. Proper motions are derived from the slope of the best-fitting line among ten VMC epochs over a time baseline of ∼1 yr. Background galaxies are used to calibrate the absolute astrometric reference frame. Results. The resulting absolute proper motion of 47 Tuc is (μ α cos(δ), μ δ ) = (+7.26 ± 0.03, −1.25 ± 0.03) mas yr −1 . This measurement refers to about 35 000 sources distributed between 10 and 60 from the cluster centre. For the SMC we obtain (μ α cos(δ), μ δ ) = (+1.16 ± 0.07, −0.81 ± 0.07) mas yr −1 from about 5250 red clump and red giant branch stars. The absolute proper motion of the Milky Way population in the line of sight (l = 305.9, b = −44.9) of this VISTA tile is (μ α cos(δ), μ δ ) = (+10.22 ± 0.14, −1.27 ± 0.12) mas yr −1 and has been calculated from about 4000 sources. Systematic uncertainties associated with the astrometric reference system are 0.18 mas yr −1 . Thanks to the proper motion we detect 47 Tuc stars beyond its tidal radius.

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“…Peñarrubia et al (2008), Klimentowski et al (2009) andŁokas et al (2010), they all rely on the dSphs plunging to pericentres that are a factor of three or four nearer the Milky Way (≈20 kpc) than their current positions and observed proper motions allow (Piatek et al 2006(Piatek et al , 2007(Piatek et al , 2008. Given the observed disk of satellites (Kroupa et al 2005) and that the Magellanic Clouds are not bound to the Milky Way (Kallivayalil et al 2006b,a) these orbits are improbable, so other mechanisms should be investigated.…”

Section: Mondmentioning

confidence: 99%

Implications for dwarf spheroidal mass content from interloper removal

Serra

Angus

Diaferio

2010

A&A

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Using the caustic method, we identify the member stars of five dwarf spheroidal (dSph) galaxies of the Milky Way, the smallest dark matter (DM) dominated systems in the Universe. After our interloper rejection, we compute line-of-sight velocity dispersion profiles that are substantially smoother than previous results. Moreover, two dSphs have line-of-sight velocity dispersions 20% smaller than previous calculations suggested. Our Jeans modelling confirms that the DM content interior to 300 pc is roughly constant with satellite luminosity. Finally, if we assume that MOND provides the true law of gravity, our identification of interlopers implies that four dSphs have mass-to-light ratios in agreement with stellar population synthesis models, whereas Carina still has a mass-to-light ratio a factor of two too large and remains a problem for MOND.

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The Proper Motion of the Large Magellanic Cloud UsingHST

Cited by 305 publications

References 27 publications

Milky Way mass models for orbit calculations

Milky Way mass models for orbit calculations

The VMC survey

Implications for dwarf spheroidal mass content from interloper removal

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