The motion of the Magellanic clouds, origin of the Magellanic Stream, and the mass of the Milky Way

Lin, Da-Bin; Jones, B. F.; Klemola, A. R.

doi:10.1086/175205

Cited by 149 publications

(174 citation statements)

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“…The corresponding mass limit becomes M in > 1:7 ; 10 11 M . This limit is consistent with previous estimates of Kochanek (1996) and others (van der Marel 2002; Wilkinson & Evans 1999;Lin et al 1995).…”

Section: The Orbit Of the Large Magellanic Cloudsupporting

confidence: 93%

Orbits in Extended Mass Distributions: General Results and the Spirographic Approximation

Adams

Bloch

2005

ApJ

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This paper explores orbits in extended mass distributions and develops an analytic approximation scheme based on epicycloids (spirograph patterns). We focus on the Hernquist potential ¼ 1/(1 þ ), which provides a good model for many astrophysical systems, including elliptical galaxies (with an R 1/4 law), dark matter halos (where N-body simulations indicate a nearly universal density profile), and young embedded star clusters (with gas density $ À1 ). For a given potential, one can readily calculate orbital solutions as a function of energy and angular momentum using numerical methods. In contrast, this paper presents a number of analytic results for the Hernquist potential and proves a series of general constraints showing that orbits have similar properties for any extended mass distribution (including, e.g., the NFW profile). We discuss circular orbits, radial orbits, zero-energy orbits, different definitions of eccentricity, analogs of Kepler's law, the definition of orbital elements, and the relation of these orbits to spirograph patterns (epicycloids). Over a large portion of parameter space, the orbits can be adequately described (with accuracy better than 10%) using the parametric equations of epicycloids, thereby providing an analytic description of the orbits. As an application of this formal development, we find a solution for the orbit of the Large Magellanic Cloud in the potential of our Galaxy.

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Section: The Orbit Of the Large Magellanic Cloudsupporting

confidence: 93%

Orbits in Extended Mass Distributions: General Results and the Spirographic Approximation

Adams

Bloch

2005

ApJ

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“…Similar results were found by Sakamoto et al (2003) from the kinematics of Galactic satellites, halo globular clusters, and horizontal branch stars. Lin et al (1995) obtained M tot r < 100 kpc = 5 × 10 11 M from the dynamics of the Magellanic Clouds, Vallenari et al (2004) found M tot r < 100 kpc = 8. Xue et al (2008) have found M tot r < 60 kpc ≈ 4.0 × 10 11 M .…”

Section: Milky Way Modelmentioning

confidence: 99%

Orbital evolution of the Carina dwarf galaxy and self-consistent determination of star formation history

Pasetto

Grebel

Berczik

et al. 2010

A&A

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We present a new study of the evolution of the Carina dwarf galaxy that includes a simultaneous derivation of its orbit and star formation history. The structure of the galaxy is constrained through orbital parameters derived from the observed distance, proper motions, radial velocity, and star formation history. The different orbits admitted by the large proper motion errors are investigated in relation to the tidal force exerted by an external potential representing the Milky Way. Our analysis is performed with the aid of fully consistent N-body simulations that are able to follow the dynamics and the stellar evolution of the dwarf system in order to determine the star formation history of Carina self-consistently. We also find a star formation history characterized by several bursts, partially matching the observational expectation. We find also compatible results between dynamical projected quantities and the observational constraints. The possibility of a past interaction between Carina and the Magellanic Clouds is also separately considered and deemed unlikely.

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“…From his Figure 7 we extracted for the mass inside 100 kpc M R<100kpc = 7.5 ± 2 × 10 11 M⊙. For comparison, by modelling the dynamics of the Magellanic Clouds and Stream Lin, Jones & Klemola (1995) found that M R<100kpc = 5.5 ± 1 × 10 11 M⊙. Clearly, the uncertainties here are dominated by systematic errors, so we allow for a generous error bound on our adopted constraint, which is M R<100kpc = (7 ± 2.5) × 10 11 M⊙.…”

Section: Oort's Constantsmentioning

confidence: 99%

Mass models of the Milky Way

Dehnen

Binney

1998

Monthly Notices RAS

516

734

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A parameterized model of the mass distribution within the Milky Way is fitted to the available observational constraints. The most important single parameter is the ratio of the scale length R d, * of the stellar disk to R 0 . The disk and bulge dominate v c (R) at R < ∼ R 0 only for R d, * /R 0 < ∼ 0.3. Since the only knowledge we have of the halo derives from studies like the present one, we allow it to contribute to the density at all radii. When allowed this freedom, however, the halo causes changes in assumptions relating to R ≪ R 0 to affect profoundly the structure of the best-fitting model at R ≫ R 0 . For example, changing the disk slightly from an exponential surface-density profile significantly changes the form of v c (R) at R ≫ R 0 , where the disk makes a negligible contribution to v c . Moreover, minor changes in the constraints can cause the halo to develop a deep hole at its centre that is not physically plausible. These problems call into question the proposition that flat rotation curves arise because galaxies have physically distinct halos rather than outwards-increasing mass-to-light ratios.The mass distribution of the Galaxy and the relative importance of its various components will remain very uncertain until more observational data can be used to constrain mass models. Data that constrain the Galactic force field at z > ∼ R and at R > R 0 are especially important.

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The motion of the Magellanic clouds, origin of the Magellanic Stream, and the mass of the Milky Way

Cited by 149 publications

References 0 publications

Orbits in Extended Mass Distributions: General Results and the Spirographic Approximation

Orbits in Extended Mass Distributions: General Results and the Spirographic Approximation

Orbital evolution of the Carina dwarf galaxy and self-consistent determination of star formation history

Mass models of the Milky Way

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