Measurement of the Absolute Proper Motions of the Magellanic Clouds

Tucholke, H. J.; Hiesgen, M.

doi:10.1007/978-94-011-3432-3_134

Cited by 3 publications

(2 citation statements)

References 4 publications

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“…The transverse motion of the Large Magellanic Cloud (LMC) has recently been measured by Jones et al (1991) and Tucholke & Hiesgen (1991). These authors have compared the present day positions of stars with old photographic plate measurements to infer the proper motion of the LMC.…”

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confidence: 99%

The origin of the Magellanic Stream

Moore¹,

Davis²

1994

Monthly Notices of the Royal Astronomical Society

201

184

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Recent measurements of the proper motion of the Large Magellanic Cloud (LMC)show it to be moving in a nearly circular orbit around the Milky Way and to be leading the Magellanic Stream which stretches in a well-confined arc 100 • behind it. We present numerical investigations designed to critically test models of the origin of the Magellanic Stream. The most developed model is the tidal model which fails to reproduce several of its characteristic properties: (i) High resolution numerical simulations of tidal stripping show that stripped material from the LMC would retain the internal velocities of the LMC and would define a thick plane surrounding the Milky Way, not the tightly confined wake actually observed. (ii) There is no leading stream as would be expected if it were tidally produced. (iii) The observed radial velocity along the Stream is inconsistent with the observed orbital parameters of the Magellanic Clouds. (iv) The uniform variation in column density along the Stream cannot be reproduced by tidal forces. (v) No stars have been observed within the Stream, but stars should be tidally stripped from the LMC as easily as gas.

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mentioning

confidence: 99%

The origin of the Magellanic Stream

Moore¹,

Davis²

1994

Monthly Notices of the Royal Astronomical Society

201

184

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“…Unfortunately, the angular density of galaxies and QSOs on the sky is small enough that this technique has been difficult to apply. Scholz (1990) and Tucholke and Hiesgen ( 1991 ) attempted to overcome this difficulty by using large area, Schmidt plates for studies of Ml3 and the LMC, respectively, but with a commensurate loss of astrometric precision due to poorer scale. Majewski (1992) demonstrated another approach to the problem in his study of proper motions of field stars.…”

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confidence: 99%

Absolute proper motions of distant Galactic satellites

Majewski¹,

Cudworth²

1993

PASP

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We describe the motivation for a new program to determine the absolute proper motions (transverse velocities) for distant Galactic globular clusters and satellite dwarf spheroidal galaxies. The topic of globular-cluster proper motions is reviewed with emphasis on the correction from relative to absolute proper motions. Our project relies on astrometry from deep ( 21), 2-5 m prime focus plates which contain images of numerous faint galaxies which are used to set a precise extragalactic reference frame. We discuss first results from the survey, determinations of the space motions for the clusters Palomar 5 and Palomar 3, at distances of 21 and 88 kpc, respectively.

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Proper-Motion Study of the Magellanic Clouds Using SPM Material

Vieira

Girard

Altena

et al. 2010

The Astronomical Journal

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-Absolute proper motions are determined for stars and galaxies to V=17.5 over a 450 square-degree area that encloses both Magellanic Clouds. The proper motions are based on photographic and CCD observations of the Yale/San Juan Southern Proper Motion program, which span over a baseline of 40 years. Multiple, local relative proper motion measures are combined in an overlap solution using photometrically selected Galactic Disk stars to define a global relative system that is then transformed to absolute using external galaxies and Hipparcos stars to tie into the ICRS. The resulting catalog of 1.4 million objects is used to derive the mean absolute proper motions of the Large Magellanic Cloud and the Small Magellanic Cloud; (µ α cos δ, µ δ ) LM C = (1.89, +0.39) ± (0.27, 0.27) mas yr −1 and (µ α cos δ, µ δ ) SM C = (0.98, −1.01) ± (0.30, 0.29) mas yr −1 . These mean motions are based on best-measured samples of 3822 LMC stars and 964 SMC stars. A dominant portion (0.25 mas yr −1 ) of the formal errors is due to the estimated uncertainty in the inertial system of the Hipparcos Catalog stars used to anchor the bright end of our proper motion measures. A more precise determination can be made for the proper motion of the SMC relative to the LMC; (µ α cos δ , µ δ ) SM C−LM C = (−0.91, −1.49) ± (0.16, 0.15) mas yr −1 . This differential value is combined with measurements of the proper motion of the LMC taken from the literature to produce new absolute proper-motion determinations for the SMC, as well as an estimate of the total velocity difference of the two clouds to within ±54 kms −1 . The absolute proper motion results are consistent with the Clouds' orbits being marginally bound to the Milky Way, albeit on an elongated orbit. The inferred relative velocity between the Clouds places them near their binding energy limit and, thus, no definitive conclusion can be made as to whether or not the Clouds are bound to one another.

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Measurement of the Absolute Proper Motions of the Magellanic Clouds

Cited by 3 publications

References 4 publications

The origin of the Magellanic Stream

The origin of the Magellanic Stream

Absolute proper motions of distant Galactic satellites

Proper-Motion Study of the Magellanic Clouds Using SPM Material

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