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dc.creatorGould, Andrew
dc.date.accessioned2011-01-25T16:43:04Z
dc.date.available2011-01-25T16:43:04Z
dc.date.issued2000-01-01
dc.identifier.citationAndrew Gould, "A New Kinematic Distance Estimator to the Large Magellanic Cloud ," The Astrophysical Journal 528, no. 1 (2000), doi:10.1086/308169, http://iopscience.iop.org/0004-637X/528/1/156en_US
dc.identifier.issn1538-4357
dc.identifier.urihttp://hdl.handle.net/1811/47607
dc.description.abstractThe distance to the Large Magellanic Cloud (LMC) can be directly determined by measuring three of its properties: its radial velocity field, its mean proper motion, and the position angle φph of its photometric line of nodes. Statistical errors of ~2% are feasible based on proper motions obtained with any of several proposed astrometry satellites, the earliest possibility being the Full-Sky Astrometric Mapping Explorer (FAME). The largest source of systematic error is likely to be in the determination of φph. I suggest two independent methods to measure φph, one based on counts of clump giants and the other on photometry of clump giants. I briefly discuss a variety of methods to test for other sources of systematic errors.en_US
dc.language.isoen_USen_US
dc.publisherAmerican Astronomical Societyen_US
dc.subjectastrometryen_US
dc.subjectgalaxies: distances and redshiftsen_US
dc.subjectMagellanic Cloudsen_US
dc.titleA New Kinematic Distance Estimator to the Large Magellanic Clouden_US
dc.typeArticleen_US
dc.identifier.doi10.1086/308169
dc.identifier.osuauthorgould.34


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